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15,102
Swift-XRT observations of the blazar PKS 0735+178 in a flaring state
Marcos Santander (U. Alabama), Sara Buson (U. Wurzburg)
The blazar PKS 0735+178 was recently detected in a high flux state both in the optical band by MASTER (ATel #15098) and in the GeV gamma-ray band by Fermi-LAT (ATel #15099) during follow-up observations of the region around the IceCube neutrino event IC211208A (GCN #31191). PKS 0735+178 is located 2.2 deg away from the best-fit neutrino position, although outside the 90% uncertainty region reported by IceCube for this event. Target of opportunity observations of PKS 0735+178 were performed with the The Neil Gehrels Swift Observatory on 2021 December 10 UT for a total XRT exposure of approximately 2.2 ksec in photon counting mode. The data were analyzed using the Leicester XRT analysis pipeline (Evans et al. 2009, MNRAS, 397, 1177) using an absorbed power-law model, which results in an intrinsic flux in the 0.3-10 keV band of (8.4 +/- 1.3) x 10^-12 erg cm^-2 s^-1 with a photon index of 2.6 +/- 0.2 for a Galactic column density of 4.5 x 10^20 cm^-2 (Willingdale et al. 2013). This flux level is about a factor of ~6 higher than that observed by Swift XRT on the same source in previous observations taken in 2009-2011 (https://www.swift.psu.edu/monitoring/source.php?source=0735+178) and is the highest X-ray flux observed for this source during the Swift mission. This flux increase is of similar amplitude as that reported by Fermi-LAT in the GeV band. Additional Swift observations are planned during the coming week. We encourage multiwavelength observations of this source. We wish to thank the Swift Team for making these observations possible, in particular B. Sbarufatti as the Swift Observatory Duty Scientist.
2021-12-11 06:09:00
optical,x-ray,gamma ray,neutrinos,agn,blazar,request for observations
2021-12-11
06:09:00
1,631
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15,100
15,103
The Galactic center object G2/DSO
Florian Peissker, Michal Zajacek, Andreas Eckart, Basel Ali, Vladimir Karas, Nadeen B. Sabha, Rebekka Grellmann, Lucas Labadie, Banafsheh Shahzamanian
Around 10 years ago, the Galactic center object G2 was found by Gillessen et al. (2012). The object was classified as a dusty gas cloud by the authors with a mass of about 3 earth_masses. It was predicted, that the cloud gets disrupted during its periapse in 2014 resulting in increased activity by Sgr A*, the supermassive black hole in the center of our Galaxy. Nevertheless, the object continued its trajectory on a Keplerian orbit after its periapse and no firework-like event was observed. In combination with the constant L-band temperature (Witzel et al. 2017), the behavior implied already a stellar nature of G2. Here we report the result of our analysis of the SINFONI data that covers 2005-2019. We find that G2 and its tail consist of 3 individual sources (G2, OS1, OS2) that move on Keplerian orbits around Sgr A*. We also trace the K-band continuum counterpart of G2 on the same orbit as the Doppler-shifted ionized gas emission. The K-band magnitude/temperature of G2 stays constant before and after the periapse in agreement with Witzel et al. (2017). In addition, we analyze the gas distribution in the S-cluster. We come to the conclusion, that the gas which was associated with G2 was in the S-cluster before the object passed by. We inspect position-velocity diagrams and show, that the tail emission is rather an outcome of the used Gaussian filter. In Peißker et al. (2021c), we connect these three sources to the overall population of dusty gaseous emission sources in and close by the S-cluster. With over a dozen sources, G2 seems not an exception but the rule. We speculate, that the Circum Nuclear Disk (CND) may serve as a birthplace for these sources. Cloud-cloud interactions (see Moser et al. 2017; Tsuboi et al. 2017, 2021) could decrease the angular momentum resulting in an infall of the material towards Sgr A* (for simulations of this process, see also Jalali et al. 2014). The overall population implies, that objects like G2, OS1, and OS2 move in groups (see Peißker et al. 2020b; Ciurlo et al. 2020) which would serve as a tracer for the infall of molecular clouds towards Sgr A*. The paper 'The Apparent Tail of the Galactic Center Object G2/DSO' was published today at ApJ (https://iopscience.iop.org/article/10.3847/1538-4357/ac23df) and is also available at arxiv as a preprint (https://arxiv.org/abs/2112.04543). The University of Cologne issued a press release that is attached to the telegram.
2021-12-11 06:26:00
black hole,pre-main-sequence star,star,young stellar object
2021-12-11
06:26:00
2,441
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15,101
15,104
Fermi-LAT detection of enhanced gamma-ray activity from the BL Lac NVSS J142750-321515
G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the BL Lac source NVSS J142750-321515, also known as 4FGL J1427.7-3215 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 216.959 deg, Decl. = -32.255 deg (J2000; D'Abrusco R. et al., 2014, ApJS, 215, 14) and unknown redshift. Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on December 8, 2021, with a daily averaged gamma-ray flux (E>100MeV) of (0.37+/-0.17) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 70 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.2+/-0.3 and is consistent with the 4FGL value of 2.1+/-0.1 within the uncertainties. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Giovanni La Mura ( glamura AT lip DOT pt ). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-12-11 16:04:00
gamma ray,agn,blazar,transient
2021-12-11
16:04:00
1,536
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15,102
15,105
TELAMON, Metsahovi, Medicina, OVRO and RATAN-600 programs find a long-term radio flare in PKS0735+17 coincident with IceCube-211208A
Matthias Kadler (JMU Wuerzburg), Petra Benke (MPIfR), Andrea Gokus (JMU Wuerzburg & FAU Erlangen-Nuremberg), Jonas Hessdoerfer (JMU Wuerzburg), Jonas Sinapius (DESY) & Philip Weber (JMU Wuerzburg), for the TELAMON Team, Merja Tornikoski (Aalto University Metsähovi Radio Observatory), Simona Righini (INAF/IRA) and Nicola Marchili (INAF/IRA), Talvikki Hovatta (Finnish Centre for Astronomy with ESO), Anthony C. Readhead (OVRO, Caltech), Sebastian Kiehlmann (IoA FORTH, OVRO), Yuri A. Kovalev (ASC Lebedev), Alexander V. Popkov (MIPT, ASC Lebedev), Yuri Y. Kovalev (ASC Lebedev, MIPT, MPIfR)
We report on contemporary radio observations of PKS0735+17 and two other radio and gamma-bright AGN possibly associated with the recently detected high-energy neutrino IceCube-211208A (GCN#31191) on Dec 8, 2021. While several compact radio sources are listed in the rfc_2021c_catalog in the immediate vicinity of the IC211208A neutrino event, we concentrate on the three radio sources associated with 4FGL Fermi gamma-ray sources (cf. ATel#15099). We observed NVSS J073824+153839 (associated with 4FGL J0738.4+1539) on Dec 8 with the Effelsberg 100-m telescope as part of the TELAMON program at 14GHz and detected it at a faint level of about 17mJy. In the same TELAMON session, we observed TXS 0740+173 (associated with 4FGL J0743.1+1713) with broader frequency coverage and found it to show a flat spectrum between 14GHz and 36GHz at a level of about 350mJy. We note that this is near the maximum values listed in the RFC data base for this source at lower frequencies and also near its historical maximum at 15GHz based on OVRO monitoring data. PKS0735+17 is the by far brightest radio source possibly associated with IceCube-211208A. We observed it in the same session (Dec 8, only hours after the release of GCN#31191) in the TELAMON program and found a flat spectrum between 14GHz and 44GHz at a level of about 1Jy. The high brightness of PKS0735+17 at the time of the IceCube-211208A event is confirmed by independent observations within the Metsahovi and Medicina monitoring programs. From the Metsahovi program, we report a continuous rising of the flux density at 37GHz from about 0.6Jy in January 2021 to 1.1+-0.1Jy on Dec 9, 2021. With the Medicina radio telescope, we find a steady increase of the flux density of PKS0735+17 at 8.3GHz and 24GHz over the MJD interval 59297.8-59548.1 from 0.66+-0.02 Jy to 0.98+-0.02 Jy at 8.3 GHz and from 0.61+-0.05 Jy to 0.95+-0.10 Jy at 24.1 GHz. At 15GHz, the OVRO monitoring measured PKS0735+17 at a level of 630mJy in December 2020 and at 980mJy on Nov 30, 2021. With the RATAN-600 radio telescope, we find a steady and slow increase of the flux density of the flat 2.3-22 GHz spectrum of PKS 0735+17 through the whole year of 2021 in the range 0.6-0.8 Jy. Together, the radio data show that the previously reported high flux states in the optical (ATel#15098), X-Ray (ATel#15102), and gamma-ray band (ATel#15099), occured during a long-term radio flare of PKS0735+17 that started at least several months ago. The TELAMON program (Kadler et al. 2021, Proc. ICRC 2021) is using the Effelsberg 100-m telescope to monitor the radio spectra of active galactic nuclei (AGN) under scrutiny in astroparticle physics. The 14 metre radio telescope in Metsahovi is used to study the long-term variability of a set of sources at 22 and 37 GHz, and observe very large source samples at 37 GHz in order to study the high-frequency radio behaviour of various source populations. The Medicina 32 metre radio telescope, operated as a National Facility by the National Institute for Astrophysics (INAF), regularly monitors a set of blazars at 8.3 and 24.1 GHz with monthly cadence. The OVRO 40m Telescope at California Institute of Technology is used to regularly monitor a large number of AGN at 15 GHz . It is currently supported by private funding from the California Insitute of Technology and the Max Planck Institute for Radio Astronomy. The RATAN-600 program monitors 2-22 GHz broad-band spectra of a complete sample of blazars with VLBI flux density above 0.4 Jy with a cadence of four times per year.
2021-12-11 20:43:00
radio,optical,x-ray,gamma ray,neutrinos,agn,blazar
2021-12-11
20:43:00
3,547
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15,103
15,106
Search for counterpart to IceCube-211208A with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported bronze track event IceCube-211208A (GCN#31191). The reconstructed origin was about 10 degrees above the horizon for ANTARES at the time of the alert. Extending slightly the analysis to include the events just above the horizon, no muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time. A search over an extended time window of +/- 1 day also yielded no detection (41% visibility). Over this time period, and restricting the search to the periods when the source remained below the horizon, this leads to a preliminary 90% confidence level upper limit on the muon-neutrino radiant fluence from a point source of about 17 GeV.cm^-2 over the energy range 5 TeV – 5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 43 GeV.cm^-2 (1 - 500 TeV) for an E^-2.5 spectrum. ANTARES [http://antares.in2p3.fr/] is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2021-12-13 16:38:00
tev,neutrinos,transient,variables
2021-12-13
16:38:00
1,369
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15,104
15,107
New outburst of J12355222+2755559
A. Vinokurov (SAO RAS) ; A. F. Valeev (SAO RAS); K. Atapin (SAI Moscow State University, SAO RAS); Alexei V. Moiseev (SAO RAS)
We inform about a new outburst of the LBV (TCP J12355222+2755559, AT 2016blu) in NGC 4559 galaxy. The observation with 6-m telescope of SAO RAS equipped by Scorpio-2 focal reducer on 2021 December 12.05 reveals brightening of the object of 2.58 ± 0.04 mag in V band relatively our previous measurement obtained with the 2.5-m telescope of Caucasian Mountain Observatory of SAI MSU on 2021 December 03.10. The follow-up spectroscopy shows numerous bright and wide hydrogen Balmer and HeI lines with P Cyg profiles as well as weak He II 4686 and FeII emissions. We estimate terminal velocity of the envelope as 2300 km/s using peak of emission and wing of absorption components of Hβ line. The spectral and photometric monitoring of the outburst are highly encouraged.
2021-12-13 19:59:00
optical,star,transient,variables,request for observations
2021-12-13
19:59:00
766
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15,105
15,108
SRG/eROSITA observation of PKS 0735+17
S. Haemmerich (Remeis-Observatory/ECAP, FAU Erlangen), A. Zainab (Remeis-Observatory/ECAP, FAU Erlangen), A. Gokus (Remeis-Observatory/ECAP, FAU Erlangen & Uni Wuerzburg), P. Weber (Remeis-Observatory/ECAP, FAU Erlangen), I. Kreykenbohm (Remeis-Observatory/ECAP, FAU Erlangen), J. Wilms (Remeis-Observatory/ECAP, FAU Erlangen)
On 2021 December 8 20:02:51.1 UT IceCube detected a track-like neutrino event (IC211208A; Santander et al., GCN#31191). Optical follow-up observations revealed an increase in brightness of BL Lac PKS 0735+17, after the source had decayed in flux prior to the neutrino event (Zhirkov et al., ATel#15098, Zhirkov et al., ATel#15100). In early November 2021 optical activity had been reported as well (Savchenko et al., ATel #15021). PKS 0735+17 has also shown increased gamma-ray activity starting about a week before IC211208A (Garrappa et al., ATel #15099). A target-of-opportunity observation with the Neil Gehrels Swift observatory revealed an increased X-ray flux compared to archival data from 2009 - 2011 (Santander & Buson, ATel #15102). Radio observations revealed that the radio flux of PKS 0735+17 has increased since the beginning of 2021, and is exhibiting a long-term radio flare (Kadler et al., ATel #15105). We report on the recent observations of the BL Lac PKS 0735+17 by the eROSITA telescope (Predehl et al. 2021, A&A 647, A1) onboard the Russian/German Spectrum-X-Gamma mission (Sunyaev et al. 2021, arxiv:2104.1326). Its position (RA = 07:38:07.32, DEC = +17:42:13.58) was scanned multiple times during the ongoing all-sky survey. The most recent scan took place between 2021 October 22 09:02 UTC and 2021 October 26 17:02 UTC, 48 days before IC211208A. During a total exposure of 146s, 33 counts were detected. Its X-ray spectrum can be described by an absorbed power-law model, with the equivalent neutral hydrogen column density fixed to N_H=3.76x10^20 cm^-2 (HI4PI Collaboration, N. Ben Bekhti, et al., 2016, A&A 594, A116). The best fit photon index is 2.0 +/- 0.6 and the absorbed 0.3-10 keV flux is (1.1 +/- 0.4) x 10^-12 erg/cm^2/s (all following values use the same band). The average count was (0.21 +/- 0.04) counts/s. The three previous eROSITA observations of PKS 0735+17 yielded the following results: 2020 April 18/19: Flux: (1.6 +/- 0.6) x 10^-12 erg/cm^2/s Count rate: (0.17 +/- 0.04) counts/s 2020 October 21/22: Flux: (1.3 +/- 0.5) x 10^-12 erg/cm^2/s Count rate: (0.23 +/- 0.05) counts/s 2021 April 19/20: Flux: (1.2 +/- 0.4) x 10^-12 erg/cm^2/s Count rate: (0.24 +/- 0.04) counts/s The spectral shape changes between the observations, however, the uncertainties are large (photon indices: 2020 April: 1.2+/-0.6, 2020 Oct: 1.7+/-0.6, 2021 April: 2.0+/-0.5). The eROSITA data confirms the findings by Swift (Santander & Buson, ATel #15102) of PKS 0735+17 being in an enhanced state in the X-rays at the moment. Follow-up observations with other X-ray missions and multi-wavelength facilities are encouraged in order to study the source further, in order to assess the possible neutrino association and to study the currently observed X-ray enhancement on longer time scales.
2021-12-13 21:58:00
radio,optical,x-ray,gamma ray,neutrinos,agn,blazar
2021-12-13
21:58:00
2,820
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15,106
15,109
Swift monitoring of the BL Lac object PKS 0735+178 during a bright state
Filippo D'Ammando (INAF-IRA Bologna)
Following the recent strong activity observed in optical (ATel #15021) and gamma-rays (ATel #15099) from the BL Lac object PKS 0735+178, located in the vicinity of the IC211208A best-fit position, although outside the 90% uncertainty region reported by IceCube for this event, Swift target of opportunity observations were performed on 2021 December 10 (see preliminary results in ATel #15102), 12, and 13. Swift/XRT data were taken during 2021 December 10, 12, and 13 in Photon Counting mode for a net exposure of about 2.2, 1.0, and 2.7 ksec, respectively. Preliminary analysis has been performed fitting the 0.3-10 keV X-ray spectrum with an absorbed power-law with the Galactic absorption corresponding to a hydrogen column density of n_H = 3.67 x 10^20 cm^-2 (Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 2.66 +/- 0.13, 2.51 +/- 0.22, and 2.57 +/- 0.20, respectively. The corresponding unabsorbed 0.3-10 keV flux is (8.7 +/- 0.6)e-12, (5.6 +/- 0.8)e-12, and (3.1 +/- 0.4)e-12 erg cm^-2 s^-1 for 2021 December 10, 12, and 13, respectively. As a comparison, the XRT spectra collected during 2006-2012 can be well fitted by an absorbed power-law with a photon index that varies between 1.2 and 2.2. The corresponding unabsorbed 0.3-10 keV flux estimated during 2006-2012 ranges between (0.8-5.6)e-12 erg cm^-2 s^-1, indicating an increase of flux (up to a factor of 10) and a softening of the X-ray spectrum during 2021 December with respect to past Swift observations, with a decreasing flux from December 10 to 13. The X-ray fluxes observed by Swift/XRT during 2021 December are also significantly higher than the value observed by SRG/eROSITA during 2021 October 22-26 (ATel #15108). Simultaneous Swift/UVOT observations were performed on 2021 December 10, 12, and 13. UVOT found PKS 0735+178 significantly brighter in optical and UV bands with respect to previous UVOT observations, e.g. the Swift observations performed at the time of the lowest (2010 November 2) and highest (2011 October 13) X-ray flux estimated during 2006-2012 (see Table below). The peak of the activity in optical and UV has been observed on 2021 December 10, in agreement with the behaviour observed in X-rays. The observed magnitudes are: Band 2010-11-02 2011-10-13 2021-12-10 2021-12-12 2021-12-13 B 16.95 +/- 0.06 16.89 +/- 0.08 14.88 +/- 0.05 15.40 +/- 0.05 15.32 +/- 0.05 U 16.28 +/- 0.06 16.02 +/- 0.07 13.93 +/- 0.05 14.54 +/- 0.05 14.44 +/- 0.05 W1 16.35 +/- 0.07 16.21 +/- 0.05 13.87 +/- 0.06 14.48 +/- 0.06 14.38 +/- 0.06 M2 16.50 +/- 0.07 16.29 +/- 0.08 13.87 +/- 0.06 14.50 +/- 0.06 14.41 +/- 0.06 W2 16.64 +/- 0.06 16.51 +/- 0.08 13.98 +/- 0.05 14.63 +/- 0.06 14.51 +/- 0.06 In consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multi-wavelength observations. Additional Swift observations are planned. We would like to thank the Swift Team, the Swift ODS, and the PI for making these observations possible.
2021-12-14 16:07:00
optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar
2021-12-14
16:07:00
2,995
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A descriptive title
Firstname1 Lastname1 (Affil1), Firstname2 Lastname2 (Affil2)...
The Fermi Large Area Telescope (LAT) Collaboration is pleased to announce a new database of multi-cadence light curves for over 1500 variable gamma-ray sources in the 10-year Fermi LAT point source catalog (4FGL-DR2, Ballet et al. 2020). The new Light Curve Repository (LCR) contains flux calibrated light curves on 3 day, 1 week, and 1 month timescales covering the entire Fermi mission duration, consisting of over 3.7 million individual time bins. The LCR will be continually updated as new data becomes available and is intended to serve as an ongoing resource to the time-domain and multi-messenger communities. The LCR can be accessed at the following link: https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/ The LCR is currently maintained by Daniel Kocevski (NASA/MSFC), with additional support from Janeth Valverde (GSFC/CRESST), Simone Garrappa (DESY), Michela Negro (GSFC/UMBC/CRESSTII), Ari Brill (NASA/GSFC), Jean Ballet (CEA Saclay) and Benoit Lott (CNRS/IN2P3, Université de Bordeaux), on behalf of NASA and the Fermi LAT Collaboration. The development of the LCR has been funded in part through the Fermi Guest Investigator Program (NASA Research Announcements NNH19ZDA001N and NNH20ZDA001N). Please send any questions, suggestions, or bug reports to fermilcr@athena.gsfc.nasa.gov.
2021-12-15 00:18:00
gamma ray,agn,blazar,gamma-ray burst,neutron star,pulsar,quasar,star,transient,variables
2021-12-15
00:18:00
1,317
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V1405 Cas is now a faint Super-Soft Source
K. L. Page (U. Leicester), S. Starrfield (ASU) , U. Munari (INAF-Padova), C. E. Woodward (U. Minnesota) & R. M. Wagner (LBTO and OSU)
V1405 Cas (Nova Cas 2021; PNV J23244760+6111140) was discovered on 2021 March 18.4236 by Yuji Nakamura (CBET #4945), and subsequently classified as a classical nova (ATels #14471, #14472, #14478, #14476, #14482). The nova has since been monitored and detected across the electromagnetic spectrum (ATels #14577, #14614, #14615, #14622, #14665, #14731, #14794). While ATel #14530 announced an early X-ray detection by the Neil Gehrels Swift Observatory, more detailed analysis suggests this is likely an artifact caused by the optical brightness of the nova that time. The source was detected in harder X-rays by NuSTAR 2.5 days after the initial discovery, however (ATel #14530). Following the announcement by Munari et al. in ATel #15093 that V1405 Cas had ended its ~7 month optical plateau and was showing a steady fading, a Swift Target of Opportunity observation was performed on December 14 (270.7 days after the discovery), to check for softer X-ray emission. A faint X-ray source was found, at a count rate of 0.011 +0.003/-0.002 count s-1 (single pixel events only, to mitigate continuing optical loading from the still-bright optical/UV source). Too few counts were detected in this short, ~1 ks observation to perform a spectral fit, but all photons were ≲1 keV, suggesting the source is in the super-soft phase. We thank the Swift PI and deputies for approving this observation. Further monitoring is planned.
2021-12-15 02:12:00
optical,x-ray,nova
2021-12-15
02:12:00
1,422
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15,109
15,112
Baikal-GVD observation of a high-energy neutrino candidate event from the blazar PKS 0735+17 at the day of the IceCube-211208A neutrino alert from the same direction
Zh.-A. Dzhilkibaev and O. Suvorova (INR RAS, Moscow) for the Baikal-GVD collaboration
IceCube collaboration has recently reported the detection of an event IceCube-211208A with high probability (signalness 50.2%) explained by an astrophysical neutrino with estimated energy of 172 TeV (GCN #31191). A prominent radio and gamma-ray blazar PKS 0735+17 is located just outside the 90% PSF containment of the IceCube event, within the expected systematic uncertainty of the determination of the arrival direction. The blazar was found to experience a strong flare in gamma rays (ATel #15099>), X rays (ATel #15102, #15108, #15109), optical (ATel #15098, #15100) and radio (ATel #15099) bands. No additional neutrino events from the direction of the alert have been reported by IceCube (GCN #31195) and ANTARES (ATel #15106). Here we report an observation of a high-energy neutrino in coincidence with this flaring blazar and IceCube-211208A by the Baikal-GVD experiment. During the alert follow-up examination of data (for details of the procedure, see e.g. Dik et al., 2021), we found a cascade event with the estimated energy of 43 TeV, arrived 3.95 hours after the IceCube event from the direction (RA=119.44 deg, DEC=18.00 deg), that is 4.68 degrees from PKS 0735+17 and 5.30 degrees from the best-fit direction of IceCube-211208A. The Baikal-GVD PSF, estimated by Monte-Carlo simulations for the conditions of this cascade event, has 5.5 deg (50%), 8.1 deg (68%) containment. One expects only 0.0044 events per 24 h in the 5.5 deg circle around this source, and the Poisson probability of the chance coincidence is 0.0044 (2.85 sigma significance). More detailed investigation of this and other Baikal-GVD events from the same direction continues. Historically, PKS 0735+17 was observed to reach 5 Jy at centimeter wavelengths in its flaring state which makes it one of the brightest radio blazars in the sky and as such - a probable neutrino emitter according to Plavin et al. (2020). Continuing VLBI monitoring observations at 15 GHz and 43 GHz show a clear core-dominated parsec-scale jet morphology. Its RATAN-600 spectrum from 2 to 22 GHz is currently undergoing a slow flare and is observed at the level 0.6-0.9 Jy. Baikal-GVD (see e.g. Belolaptikov et al., 2021) is the largest neutrino telescope in the Northern hemisphere, operating with an effective volume of ~0.4 km3 for the cascade detection by a collaboration of more than 60 scientists from Russia, Slovakia, Czech Republic, Poland and Germany.
2021-12-15 02:44:00
radio,optical,x-ray,gamma ray,tev,neutrinos,agn,blazar
2021-12-15
02:44:00
2,424
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0.01997130922973156, -0.005121530499309301, 0.05173603817820549, 0.03493776544928551, -5.2306489806142054e-8, 0.025161482393741608, 0.06502100825309753, -0.05780428275465965, 0.018230540677905083, 0.037445418536663055, -0.07183068990707397, -0.04524955898523331, -0.0030476991087198257, -0.07372225821018219, 0.0015961152967065573, 0.041379306465387344, -0.01051235944032669, 0.009913220070302486, -0.03253369778394699, 0.02055186592042446, 0.008302608504891396, 0.012096518650650978, -0.06052052974700928, -0.014638816006481647, 0.0008995264070108533, 0.04027768224477768, -0.026103192940354347, 0.05799360200762749, -0.08615680038928986, -0.0681368038058281, 0.00974704697728157, 0.03445659577846527, 0.06694395840167999, 0.08297236263751984, -0.07975511252880096, -0.07802829146385193, -0.07087409496307373, 0.027266116812825203, -0.0506281740963459, 0.050553180277347565, 0.04061971977353096, -0.020876774564385414, -0.020863449200987816, 0.13087931275367737, 0.03633764386177063, 0.003265170380473137, -0.03516124188899994, -0.01039841491729021, 0.05020519718527794, -0.10735825449228287, -0.016342978924512863, -0.07905707508325577, -0.11876661330461502, 0.013630876317620277, 0.060908038169145584, -0.046514395624399185, -0.02917461097240448, -0.029523815959692, -0.07422597706317902, -0.03836294263601303, 0.06144307926297188, -0.019725440070033073, -0.043314509093761444, -0.05128958076238632, 0.014425022527575493, 0.03700720891356468, -0.05839639902114868, -0.1268467754125595, -0.028988530859351158 ]
15,110
15,113
NuSTAR observations of the blazar PKS 0735+178
Qi Feng (Barnard College/Columbia University), Weidong Jin (U. Alabama), Kaya Mori (Columbia University), Reshmi Mukherjee (Barnard College/Columbia University), Marcos Santander (U. Alabama), Jooyun Woo (Columbia University)
We report on the recent target-of-opportunity NuSTAR observations of the blazar PKS 0735+178, located 2.2 deg away from the best-fit position of the IceCube neutrino event IC211208A (GCN #31191). Elevated fluxes from PKS 0735+178 were recently reported in the radio band (ATel #15105), in the optical band by MASTER (ATel #15098), in the X-ray band by Swift-XRT (ATel #15102, #15109), and in the GeV gamma-ray band by Fermi-LAT (ATel #15099) as part of the follow-up observations of the region around the IceCube event. Two NuSTAR observations of PKS 0735+178 were performed: The spectra from both modules A and B were simultaneously and adequately fitted between 3 keV and 40 keV with a single power-law model, without any evidence for curvature or absorption. The best-fit models for the two NuSTAR observations yield photon indices of 1.79 +/- 0.07 and 1.64 +/- 0.08, fluxes (3 -- 40 keV) of (3.2 +/- 0.2) x 10^-12 erg cm^-2 s^-1 and (3.0 +/- 0.2) x 10^-12 erg cm^-2 s^-1, and chi-squared (degree of freedom) values of 107 (108) and 76 (92), respectively. The hard-X-ray spectrum of the source is significantly harder than the recently reported soft-X-ray spectrum, which yielded photon indices of ~2.5 -- 2.7 and uncertainties around 0.2, observed from 0.3 to 10 keV by Swift-XRT on 2021 Dec 10, 12, and 13 UT (ATel #15102, #15109). Earlier observations of the source from 0.3 keV to 10 keV between 2020 Apr and 2021 Oct by eROSITA suggested X-ray variability both in the flux and spectrum (the photon index ranging between 1.2 and 2.0; ATel #15108). The hard-X-ray flux is consistent with being constant over the two-day interval between the two NuSTAR observations. Further multi-wavelength follow-up observations are encouraged to study the variability of the source on longer timescales. We thank the NuSTAR Science Operations Center, in particular K. Forster, for making these observations possible.
2021-12-15 06:08:00
radio,optical,x-ray,gamma ray,neutrinos,agn,blazar,request for observations
2021-12-15
06:08:00
1,912
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15,111
15,114
Swift XRT/UVOT rapid follow-up of bright FRB 20211211A
Aaron Tohuvavohu (U Toronto), Jamie Kennea (PSU), Phil Evans (U Leicester), James DeLaunay (U Alabama)
The Neil Gehrels Swift Observatory responded with its newly commissioned AutoToO autonomous repoint mode, to rapidly observe the bright CHIME FRB 20211122A (event #202020046 T0: 2021-12-11T16:58:05.183768), slewing and landing on target at T0+21 minutes. The XRT field of view fully covers the 95% containment region (radius 9.7') reported by CHIME/FRB. The UVOT field of view covered ~85% of this region. Observations continued for 800 s of integrated exposure, with XRT taking data in Photon Counting (PC) mode and UVOT observing in event mode (11 ms timing) with the u filter. No new sources are found in the FRB’s localization region, down to an average 3 sigma upper limit of 1e-2 ct s-1 (0.3-10 keV) and 20.5 AB mag in the u filter. Two known X-ray sources, believed to be AGN, are detected in apparent outburst compared to previous observations, but consistent with their historical flaring behaviour. This research has made use of the CHIME/FRB VOEvent Service.
2021-12-15 09:43:00
radio,ultra-violet,x-ray,agn,fast radio burst,transient
2021-12-15
09:43:00
971
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15,112
15,115
Swift follow-up observations of AT2021afpi / MASTER OT J030227.28+191754.5
V. V. Neustroev (U. Oulu), J. P. Osborne, K. L. Page (U. Leicester)
We report the results of follow-up observations of AT2021afpi = MASTER OT J030227.28+191754.5 carried out with the Neil Gehrels Swift Observatory. The object was discovered on 2021 November 27 as a bright optical transient by MASTER (ATel #15067) as a result of follow-up observations of the IceCube neutrino alert IceCube-211125A (GCN #31126). However, it has been shown (ATel #15081) that AT2021afpi started brightening at least 8.5 hours before the IceCube-211125A trigger (November 24, 21:53 UT). Based on the large amplitude of the optical outburst (~10 mag), the transient was initially classified as a classical nova (ATel #15069). Nevertheless, the following optical spectroscopic and time-resolved photometric observations have confirmed that AT2021afpi is a very high amplitude WZ Sge-type dwarf nova (ATel #15072, #15074). Swift started monitoring AT2021afpi 3.9 days after the transient discovery. Although initially bright, with an XRT count rate ~1.1 c/s (ATel #15073, #15087), AT2021afpi has rapidly faded for ~10 days before stabilizing at ~0.02 c/s on December 4-5. On December 11, the X-ray flux dropped to the level of about ~0.005 c/s, but returned back to the level of ~0.02 c/s by the time of the next observation on December 13. However, the optical and UV light curves show only a smooth slow decline and no response to this X-ray drop. So far, the X-ray and UV flux evolution of AT2021afpi is similar to that of the superoutbursts of SSS J122221.7-311525 and GW Lib (Neustroev+18 A&A 611 13). An X-ray spectrum consisting of the data with the lowest XRT count rates < 0.03 c/s is also consistent with the outburst spectra of SSS J122221.7-311525 and GW Lib. It can be satisfactorily fitted with one optically thin emission component. However, the two first Swift/XRT observations show the presence below 0.8 keV of an additional strong soft component. Thus, 2 optically-thin components are needed for a satisfactory fit of these "higher-state" data (see also ATel #15087). We thank the Swift PI, Brad Cenko, for approving the observations, and the Swift planning and operations teams for their ongoing support.
2021-12-15 19:02:00
optical,ultra-violet,x-ray,neutrinos,cataclysmic variable,nova,transient,variables
2021-12-15
19:02:00
2,138
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-0.0017095445655286312, 0.025976713746786118, 0.02257969044148922, 0.0316496379673481, -0.06282114237546921, 0.027197010815143585, -0.05249541997909546, -0.10441616177558899, 0.003258165204897523, 0.09818074852228165, -0.0771138146519661, 0.004429358523339033, -0.025023886933922768, 0.012834320776164532, -0.11816009879112244, -0.010509531013667583, -0.05280180275440216, -0.05242130532860756, -0.0664735734462738, 0.04450496286153793, 0.12470779567956924, -0.09693672508001328, -0.11141722649335861, 0.02076307125389576 ]
15,113
15,116
A correction to ATel #15115
V. V. Neustroev (U. Oulu), J. P. Osborne, K. L. Page (U. Leicester)
We report an erratum in ATel #15115. It has been brought to our attention that the Astronomer's Telegram requires that quantitative measurements must include uncertainties, and approximate numbers are not allowed. We, therefore, update the information from ATel #15115 with error bars included: The mean XRT count rate of the first 2 ksec observation of AT2021afpi started on November 28, 19:33 UT was 0.71 +/- 0.02 c/s. After that, the transient rapidly faded before stabilizing at 0.020+/-0.004 c/s on December 4-5. On December 11, the X-ray flux dropped to the level of 0.005 +0.002/-0.001 c/s, but returned back to the level of 0.018+/-0.004 c/s by the time of the next observation on December 13.
2021-12-15 22:09:00
x-ray,cataclysmic variable,transient,variables
2021-12-15
22:09:00
702
[ -0.046966925263404846, 0.017666799947619438, 0.05170783773064613, 0.10484971851110458, 0.039478205144405365, -0.07853810489177704, -0.019939184188842773, 0.11018992960453033, 0.04710458964109421, -0.027257898822426796, 0.04889988154172897, -0.055383071303367615, 0.07955311983823776, -0.02251535654067993, -0.07147695124149323, -0.05641625076532364, -0.027706041932106018, -0.08968459814786911, -0.034501343965530396, 0.06397699564695358, -0.018043676391243935, 0.03453482687473297, -0.031265776604413986, 0.00468185730278492, 0.073804572224617, 0.002728953491896391, -0.08864390850067139, -0.12488216161727905, -0.006297524552792311, -0.05814477428793907, 0.03326424956321716, 0.06313250213861465, -0.0036906383465975523, -0.0010784456972032785, 0.03792107105255127, 0.019913731142878532, 0.0002948794572148472, 0.002954513067379594, -0.039954960346221924, -0.01316771563142538, 0.003323513315990567, -0.06661640107631683, -0.018118010833859444, 0.03137616813182831, -0.021432898938655853, 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15,114
15,117
TRAPPIST comet production rates: 6P/d'Arrest, 67P/C-G, 4P/Faye, 19P/Borrelly, 57P/D-N-D
E. Jehin, Y. Moulane, J. Manfroid, M. Vander Donckt, S. Hmiddouch, F. Pozuelos, M. Ferrais, and D. Hutsemekers (STAR Institute, University of Liege)
E. Jehin, Y. Moulane, J. Manfroid, M. Vander Donckt, S. Hmiddouch, F. Pozuelos, M. Ferrais, and D. Hutsemekers (STAR Institute, University of Liege) report that they obtained from TRAPPIST-South (code=I40, Chile) robotic telescopes (Jehin el al. 2011) observations using HB narrowband filters (Farnham et al. 2000) for the following comets and computed preliminary production rates at 10.000 km using a Haser Model (Vp=Vd=1km/s) (Haser 1957). Their dust production rates proxy A(0)f(rho) was estimated by profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). 6P/d Arrest Date UT=2021-12-02, r_h=1.60 au, Delta=1.44 au Q(OH)=(5.40+/-0.55) E27 s-1; Q(CN)=(1.53+/-0.15) E25 s-1; Q(C2)=(1.77+/-0.17) E25 s-1; Q(C3)=(4.67+/-0.27) E24 s-1 A(0)fp(RC)= 142+/-8 cm 67P/C-G Date UT=2021-12-02, r_h=1.27 au, Delta=0.43 au, DT=+30 days Q(OH)=(6.33+/-0.67) E27 s-1; Q(CN)=(1.14+/-0.10) E25 s-1; Q(C2)=(8.14+/-0.13) E24 s-1; Q(C3)=(1.34+/-0.22) E24 s-1 A(0)fp(RC)= 853+/-14 cm 4P/Faye Date UT=2021-11-30, r_h=1.82 au, Delta=0.94 au Q(CN)=(4.21+/-0.17) E24 s-1; Q(C2)=(6.29+/-0.16) E24 s-1; Q(C3)=(1.04+/-0.34) E24 s-1 A(0)fp(RC)= 565+/-18 cm 19P/Borrelly Date UT=2021-11-30, r_h=1.54 au, Delta=1.18 au Q(OH)=(9.65+/-0.47) E27 s-1; Q(CN)=(2.16+/-0.16) E25 s-1; Q(C2)=(1.56+/-0.17) E25 s-1; Q(C3)=(2.94+/-0.33) E24 s-1 A(0)fp(RC)= 1011+/-10 cm 57P/DuToit-Neujmin-Delporte Date UT=2021-11-21, r_h=1.75 au, Delta=2.10 au Q(CN)=(2.51+/-0.17) E25 s-1; Q(C2)=(1.65+/-0.19) E25 s-1 A(0)fp(R)= 1715+/-20 cm 57P is at the limit of the C-chain depleted comets based on the -0.18 limit for Log(C2/CN) from A'Hearn et al. 1995. Notations: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, NH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, GC, RC are the blue, green and red dust continuum filters (Farnham et al. 2000) Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS under grant FRFC 2.5.594.09.F. TRAPPIST-North is funded by the University of Liège, and performed in collaboration with the Cadi Ayyad University of Marrakesh. We thank NASA, David Schleicher and the Lowell Observatory for the loan of a set of HB comet filters.
2021-12-15 22:27:00
optical,comet,star
2021-12-15
22:27:00
2,268
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15,115
15,118
Fermi-LAT detection of enhanced gamma-ray activity from the radio source NVSS J121135-273615
G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the radio source NVSS J121135-273615, also known as 4FGL J1211.6-2735 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 182.899 deg, Decl. = -27.604 deg (J2000; Condon et al. 1998, AJ, 115, 1693), and unknown redshift. Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on December 14, 2021, with a daily averaged gamma-ray flux (E>100MeV) of (0.4+/-0.1) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 40 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.1+/-0.2, and is significantly smaller than the 4FGL value of 2.6+/-0.1. The light curve for this source can be accessed via the Fermi-LAT Light-Curve Repository at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.php?source_name=4FGL_J1211.6-2735. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Giovanni La Mura (glamura AT lip DOT pt). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-12-17 05:38:00
radio,gamma ray,agn,transient
2021-12-17
05:38:00
1,716
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-0.005988952703773975, 0.01455196738243103, 0.023598112165927887, 0.03581107407808304, -5.6524811498093186e-8, -0.010561970993876457, 0.07089019566774368, -0.0953943282365799, 0.03994133695960045, 0.04231557995080948, -0.07648330926895142, 0.026691880077123642, 0.0289123747497797, 0.03080039471387863, 0.020640885457396507, 0.056136202067136765, 0.04928726702928543, 0.08149364590644836, -0.06513392925262451, -0.00869041308760643, -0.020023483783006668, -0.021048488095402718, -0.07450830936431885, -0.01601422391831875, 0.021309835836291313, 0.05177340656518936, 0.03826291114091873, 0.10270542651414871, -0.008835156448185444, -0.015984129160642624, -0.010399432852864265, -0.03755000978708267, 0.057782452553510666, 0.02739797905087471, -0.12776397168636322, -0.026638412848114967, -0.027193261310458183, 0.04062597453594208, -0.09024141728878021, -0.10738521814346313, -0.05970735847949982, -0.0411229208111763, 0.0012190088164061308, 0.09294848889112473, 0.06642411649227142, -0.004923852160573006, -0.07945285737514496, 0.06987734884023666, 0.0354916974902153, -0.09198388457298279, 0.03465896472334862, -0.07812714576721191, -0.10995395481586456, 0.018535342067480087, 0.026284649968147278, -0.06221628189086914, 0.0374458022415638, -0.004836466629058123, -0.07995253056287766, -0.0611301027238369, 0.014150272123515606, 0.012082603760063648, 0.00015835027443245053, 0.00933496281504631, -0.05717378854751587, 0.029124338179826736, -0.06895165145397186, -0.10981063544750214, -0.006314629223197699 ]
15,116
15,119
Follow-Up Observations of Comet C/2021 A1 (Leonard)
M. Mugrauer
Comet C/2021 A1 (Leonard) was observed at the University Observatory Jena on 3 December 2021. In order to follow the orbital motion of the comet, to measure its apparent brightness, and to study its morphology several images of C/2021 A1 were taken in the R-band with the CCD-camera CTK-II, which is installed at the 25cm Cassegrain telescope of the observatory. During the imaging observations the comet was located next to the globular cluster M3 (angular separation of only 7arcmin). Furthermore, in the same night spectroscopic observations of the coma of the comet were carried out with the Échelle spectrograph FLECHAS, which is operated at the 90cm telescope of the observatory. In total, three spectra, each with an integration time of 900s, were taken in the 2x2 binning mode of the instrument (R~7400). Throughout the spectroscopy of C/2021 A1 the telescope was tracked on the center of the comet's coma. In the fully reduced FLECHAS spectrum of the comet in the wavelength range between 5000 and 7000Å many emission lines are detected (NH2, C2, and [OI]). The NH2 lines were used to measure the radial velocity of comet C/2021 A1 relative to the observing site, which is -58.9±1.1km/s at the mid-time of the observations (3 December 2021 03:51:29UT).
2021-12-17 05:45:00
comet,globular cluster
2021-12-17
05:45:00
1,261
[ -0.029161736369132996, 0.01437655370682478, -0.02843506634235382, -0.026945611461997032, 0.016399813815951347, -0.003494338598102331, -0.06192341446876526, 0.10847368091344833, 0.031039701774716377, 0.08589982241392136, -0.06363092362880707, -0.07722526788711548, -0.018682541325688362, -0.05009045824408531, 0.021046103909611702, -0.016326183453202248, 0.06376425176858902, -0.0715186595916748, -0.030903570353984833, -0.035816680639982224, -0.007659971714019775, -0.030016491189599037, 0.03397586941719055, -0.013395202346146107, 0.02896387130022049, 0.026610828936100006, -0.057653848081827164, -0.07902079075574875, -0.040521930903196335, -0.052108991891145706, 0.02833167463541031, 0.04062320291996002, -0.048804596066474915, 0.00011728455865522847, 0.0481368713080883, -0.029914192855358124, 0.09591325372457504, -0.038173429667949677, 0.0543525405228138, 0.04917006194591522, 0.02629193291068077, -0.0157253947108984, 0.003932152409106493, -0.05558309331536293, 0.012186584994196892, 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-0.039393097162246704, 0.025154486298561096, 0.03843284025788307, 0.0299991425126791, -0.006423264741897583, 0.015247965231537819, -0.05365161970257759, -0.066038116812706, -0.06355611234903336, -0.08302991092205048, -0.011477114632725716, -0.025825046002864838, -0.04238414391875267, -0.0913391262292862, 0.016808196902275085, -0.009870128706097603, -0.06737631559371948, -0.0665692612528801, -0.013743671588599682, 0.013979210518300533, -0.055450189858675, -0.057121049612760544, -0.09279019385576248 ]
15,117
15,120
LJT spectroscopic classification of AT 2021aghl as a relatively young Type Ia supernova
Liping Li (Yunnan University); Jujia Zhang, Qian Zhai (YNAO); Xiaofeng Wang(THU)
We report an optical spectrum of AT 2021aghl (350-870nm) that was obtained on 2021 Dec. 16.75 UT with the Lijiang 2.4-m telescope (LJT +YFOSC) at LiJiang observatory of Yunnan Observatories. The spectrum is similar to that of a type Ia supernovae at a few days before the maximum light. Cross-correlation with the library of supernova spectra using the comparison tool SNID (Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 2003du at t = -9 days. Given a redshift of 0.045 derived by narrow H-alpha emission of the host galaxy, an expansion velocity of about 13000 km/s can be deduced from the Si II 635.5 absorption minimum.
2021-12-17 09:59:00
optical,supernovae
2021-12-17
09:59:00
646
[ -0.09157560020685196, -0.07609924674034119, 0.03809863701462746, 0.026642179116606712, 0.031027106568217278, 0.03627661615610123, -0.05644392594695091, 0.02295263484120369, -0.015519724227488041, -0.031635481864213943, 0.04180828481912613, -0.04852507635951042, -0.03941863402724266, -0.04036460444331169, 0.03871941938996315, 0.016800425946712494, 0.08491942286491394, -0.12847399711608887, 0.01734349876642227, 0.0007643898716196418, 0.06640348583459854, 0.02384176291525364, -0.06549052894115448, 0.004979175981134176, 0.06296406686306, -0.05785367265343666, -0.07124011218547821, -0.051955029368400574, -0.008554894477128983, 0.05350057780742645, 0.025534169748425484, 0.04024171456694603, -0.02347644418478012, 0.05547867342829704, 0.024181872606277466, -0.07552018016576767, 0.05554670840501785, -0.023071516305208206, 0.006102885119616985, -0.03288482502102852, 0.03095225617289543, -0.0517260916531086, -0.0008411331218667328, 0.002322726184502244, 0.013210754841566086, 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15,118
15,121
Search for counterpart to IceCube-211216A with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration.
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported track event IceCube-211216A (GCN#31241). At the time of the alert, the reconstructed origin was -8.4 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible from [T-60min, T+51min] (95%). This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 16 GeV.cm^-2 over the energy range 5 TeV – 5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 49 GeV.cm^-2 (1 TeV - 450 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (41% visibility). ANTARES [http://antares.in2p3.fr/] is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2021-12-17 17:33:00
tev,neutrinos,transient
2021-12-17
17:33:00
1,259
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0.026727035641670227, -0.06931701302528381, -0.005048228893429041, -0.07833274453878403, -0.09673892706632614, 0.017375687137246132, 0.03173358738422394, -0.006209995597600937, 0.05680947005748749, -0.061545003205537796, 0.011943788267672062, -0.006593612022697926, 0.077744260430336, -0.0008440593956038356, -0.028025906533002853, -0.05756186321377754, -0.01632869616150856, 0.06617361307144165, -0.058031726628541946, -0.16339939832687378, -0.02888287976384163 ]
15,119
15,122
Search for the X-ray counterpart to IceCube-211216A event with Swift
Rukaiya Khatoon (Tezpur Univ., IUCAA, India), Raj Prince (CFT, Poland), Ranjeev Misra (IUCAA, India)
On 2021-12-16 at 07:07:38.13 UT, IceCube detected a track-like event with a moderate probability of being of astrophysical origin (GCN #31241). The event was selected by the ICECUBE_Astrotrack_Bronze alert stream. Two gamma-ray sources listed in the 4FGL Fermi-LAT catalog are located in the 90% containment region. We performed a search for the X-ray counterpart of the IceCube-211216A (GCN #31241) event. The observation in Swift was conducted for the two 4FGL sources, 4FGL J2100.0+1445 (R.A = 315.02 deg, Dec. = 14.76 deg) and 4FGL J2108.5+1434 (R.A = 317.15, Dec. = 14.58), located in the 90% containment region with their position 1.43 deg and 1.61 deg away from the best-fit IceCube-211216A event position. The observation by Swift was performed on 2021 December 16 at 15:34:03(UT) for 4FGL J2100.0+1445 (observation ID: 00014987001) and at 16:06:05(UT) for 4FGL J2108.5+1434 (observation ID: 00014988001) with an exposure of ~ 2.0 ks for each source. With the preliminary analysis results using the Swift-XRT data, we observed that the source is too faint to extract the Swift-XRT spectrum. The GCN circular (GCN #31243) has also reported that there is no gamma-ray counterpart detected using combined all-sky detectors in INTEGRAL. Further, no ongoing muon neutrino candidate events were recorded by ANTARES (ATel #15121). The Swift-UVOT observation was performed with U band filter. We do not observe any bright source at the source location. We would like to thank the Swift Team for the extremely rapid and efficient scheduling of the ToO observation.
2021-12-17 21:54:00
optical,ultra-violet,x-ray,gamma ray,neutrinos,agn,blazar
2021-12-17
21:54:00
1,567
[ -0.08093160390853882, -0.04535650461912155, -0.04679388180375099, 0.05926614627242088, 0.035107776522636414, -0.03104216232895851, 0.008692950941622257, 0.02881215140223503, 0.020489787682890892, -0.06142503395676613, -0.02597322314977646, -0.07409249991178513, 0.010709072463214397, -0.025825995951890945, -0.0007889260887168348, -0.05482703074812889, 0.029752986505627632, -0.09909633547067642, -0.058022987097501755, -0.03407908231019974, -0.04042145982384682, -0.041810765862464905, 0.014520736411213875, -0.017481883987784386, -0.022248346358537674, -0.017769204452633858, 0.014743038453161716, -0.09059382975101471, 0.01844358630478382, 0.014855950139462948, 0.0578085295855999, 0.01848754845559597, -0.06259904056787491, 0.026598967611789703, 0.033408328890800476, -0.009922115132212639, -0.02839147299528122, -0.08546660095453262, 0.016270803287625313, -0.013633858412504196, 0.019809745252132416, -0.0007535851327702403, 0.05845397338271141, 0.03431418165564537, -0.057746533304452896, 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15,120
15,123
The Type IIn 2021gpw in the errorbox of IceCube-20211216B
Irene Salmaso (Padova Univesity, INAF-OAPd), Enrico Cappellaro (INAF-OAPd), Nancy Elias-Rosa (INAF-OAPd), Achille Fiore (INAF-OAPd), Andrea Reguitti (UAB Chile, INAF-OAPd), Leonardo Tartaglia (INAF-OAPd)
Following the alert of the Ice-Cube collaboration of a (bronze) track-like event Ice-Cube 20211216B (GCN 31249, https://gcn.gsfc.nasa.gov/gcn3/31249.gcn3), we searched the SN archives for interacting SNe within the neutrino errorbox. According to Fang et al. 2020, ApJ, 904, 4, diffusive shock acceleration in interacting SNe is one of the possible sources of high-energy neutrinos up to several months after the SN explosion. We report the presence of the Type IIn SN 2021gpw (Transient Name Server, https://www.wis-tns.org/object/2021gpw) about 1.17 degrees from the reported position and hence within the 90% PSF containment. SN 2021gpw was discovered on March 20th, 2021 by ATLAS (Transient Name Server, https://www.wis-tns.org/object/2021gpw/discovery-cert) at a distance of 320 Mpc. Based on the LT spectrum reported in TSN, the SN was classified as Type IIn. The bright, slow-evolving light curve (observed by ZTF, retrieved from the Lasair broker https://lasair.roe.ac.uk/object/ZTF21aaqhqke), reached a peak magnitude of -19.90 +/- 0.06 in the r band on April 25th, 2021. The target was of magnitude r=19.79 +/- 0.20 (absolute magnitude -17.75) at the last ZTF observation (December 2nd, 2021). We planned for follow-up optical observations in the next few days.
2021-12-18 00:42:00
optical,neutrinos,supernovae,transient,a comment
2021-12-18
00:42:00
1,271
[ -0.18637119233608246, -0.05798371508717537, 0.027391506358981133, 0.12405513226985931, 0.06380672752857208, -0.013071011751890182, -0.04982128366827965, 0.09815951436758041, 0.006080991588532925, -0.039910223335027695, -0.03385943919420242, 0.0059918370097875595, 0.0009629203123040497, 0.005453411024063826, -0.02000797912478447, -0.00495401443913579, 0.027466896921396255, 0.0017526807496324182, -0.03412504121661186, 0.02923337183892727, 0.0012196173192933202, -0.02880016714334488, -0.02615603245794773, 0.054349035024642944, -0.003608475439250469, -0.05932733044028282, -0.049731623381376266, -0.0213000625371933, 0.005830180831253529, 0.0006864895112812519, 0.039148204028606415, -0.01614760234951973, -0.01904994621872902, 0.024796677753329277, 0.05233342573046684, 0.004760322161018848, 0.01609288528561592, 0.02078019455075264, 0.014901673421263695, 0.023538164794445038, 0.0757216289639473, -0.029911711812019348, -0.00988468062132597, 0.047203149646520615, 0.0329478457570076, 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15,121
15,124
The Ongoing X-Ray Flare in Markarian 501
Bidzina Kapanadze (Ilia State University, Tbilisi, Georgia; E. Kharadze National Astrophysical Observatory, Abastumani, Georgia)
In ATel#15059 (posted on 2021 November 23), we reported the onset of X-ray flare in the nearby, TeV-detected blazar Markarian 501 (z=0.034) which is a bright X-ray source and prominent with strong TeV/X-ray flares (see, e.g., Ahnen et al., 2017, A & A, 603, 31; Kapanadze et al. 2017, MNRAS, 469; 1655). Moreover, the source is undergoing variations in the baseline X-ray level on the timescales of several years, and since 2021 March, we observe a significantly enhanced X-ray activity of the source compared to the previous years (and comparable to the flaring behaviour shown in 2014 March-October; see https://www.swift.psu.edu/monitorin g/source.php?source=Mrk501 and Kapanadze B. et al. 2017), superimposed by shorter-term X-ray flares. Currently, Mrk 501 is observed with Swift-XRT in the framework of out Target of Opportunity (TOO) request Number #16518, finding the source in the further long-term increasing X-ray flaring trend: the 0.3-10 keV count rate has reached a value of 8.94+/-0.11 cts/s during the XRT observation performed on December 16 (by a factor of ~2 higher than the minimum rate recorded on 2021 November 10, before the onset of the current flare). On average, the spectral evolution is characterized by the "harder-when-brighter" trend. In the framework of one-zone SSC models, a flaring activity of Mrk 501 is also expected in the UV-radio and gamma-ray parts of the spectrum, and intensive multiwavelength observations of the source are strongly encouraged for discerning the underlying emission mechanisms and instable processes. XRT is one of the Swift instruments along with Burst Alert Telescope (BAT) and UV/Optical Telescope (UVOT). It is a JET-X Wolter I type telescope, developed jointly by Pennsylvania State University, Brera Astronomical Observatory (OAB) and University of Leicester. Thanks to the unique characteristics, good photon statistics and low background counts of this instrument (in combination with EEV CCD2 detector), we can investigate a flux variability on different time-scales from minutes to years, obtain high-quality spectra for the majority of the observations, derive different spectral parameters, and study their timing behaviour in the 0.3-10 keV range of the electromagnetic spectrum. The Swift Satellite is operated by Pennsylvania State University.
2021-12-18 04:31:00
radio,optical,x-ray,gamma ray,tev,blazar
2021-12-18
04:31:00
2,319
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-0.038006603717803955, -0.11034541577100754, 0.0403311550617218, 0.025740982964634895, -0.06834413856267929, 0.006191596854478121, -0.017248986288905144, -0.07709859311580658, 0.05742941051721573, -0.03616815805435181, 0.05723577365279198, -0.036469560116529465, 0.03345177322626114, -0.08520041406154633, -0.029129521921277046, -0.0013275936944410205, 0.005403207149356604, -0.003190212184563279, 0.055341385304927826, -0.007430928759276867, 0.05840307101607323, -0.02764669805765152, -0.09602408111095428, -0.0018279127543792129 ]
15,122
15,125
Erratum for Atel #15122
Rukaiya Khatoon (Tezpur Univ., IUCAA, India), Raj Prince (CFT, Poland), Ranjeev Misra (IUCAA, India)
The upper-limit for the flux of the two 4FGL sources, 4FGL J2100.0+1445 and 4FGL J2108.5+1434 were not added in the original telegram and are now added here. We sincerely apologize for the inconvenience. With the preliminary analysis results using the Swift-XRT data, we do not observe any significant counterparts in X-ray and estimate the 3-sigma flux upper limit in the energy range 0.3-10.0 keV is ~ 1.94 x 10^-13 erg cm^-2 s^-1 for 4FGL J2100.0+1445 and ~ 3.74 x 10^-13 erg cm^-2 s^-1 for 4FGL J2108.5+1434.
2021-12-18 06:25:00
optical,ultra-violet,x-ray,agn,blazar
2021-12-18
06:25:00
513
[ -0.03158395364880562, -0.0618419423699379, -0.008528988808393478, 0.0012656881008297205, 0.03359493240714073, -0.03280925378203392, 0.03143622353672981, 0.09074755012989044, -0.05187149718403816, -0.058661412447690964, -0.016689378768205643, -0.08870476484298706, -0.0007882338250055909, 0.017959481105208397, 0.05876605957746506, 0.04183271899819374, 0.045963939279317856, -0.04654259234666824, -0.11949155479669571, 0.01332781556993723, 0.06468566507101059, 0.04956449940800667, 0.09060771018266678, 0.030280394479632378, 0.06688027828931808, -0.08852945268154144, 0.005065727047622204, -0.1042930856347084, 0.02951228991150856, -0.02870953269302845, -0.02921435236930847, -0.01294947974383831, -0.003220193786546588, 0.0697043314576149, 0.06269572675228119, -0.0166157353669405, -0.03211568295955658, -0.019390001893043518, -0.02150951512157917, 0.0385359488427639, -0.0764138326048851, -0.004707666113972664, 0.04113585501909256, 0.038169436156749725, -0.027228083461523056, 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15,123
15,126
Fermi-LAT detection of enhanced gamma-ray activity from the Giga-Hertz Peaked Spectrum radio source OS 300
G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed remarkably enhanced gamma-ray emission from a source positionally consistent with the radio source OS 300 (B1600+335, 4C +33.38), also known as 4FGL J1602.1+3324 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 240.530 deg, Decl. = +33.448 deg (J2000; Johnston et al. 1995, AJ, 110, 880). OS 300 is best known as a Giga-Hertz Peaked Spectrum (GPS) radio source (Snellen et al. 2000 MNRAS 319, 445) with complex radio morphology (Tremblay et al. 2010 ApJ 712, 159). Its redshift was estimated photometrically as z = 1.1 (Snellen et al. 2000 MNRAS 319, 445) and is thus tentative (see Dallacasa et al. 2013 MNRAS 433, 147). Preliminary analysis indicates that this source was in a flaring state on 2021 December 16, with a daily averaged gamma-ray flux (E>100MeV) of (0.94+/-0.18) X 10^-6 photons cm^-2 s^-1 (uncertainties are statistical only), and a peak 6-hr flux of (1.6+/-0.5) X 10^-6 photons cm^-2 s^-1 from 12:00-18:00 UTC. The former corresponds to a flux increase of a factor of 200 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the third flaring episode associated with this source and the highest flux state ever observed by LAT (see ATels #13931, #14422). The daily photon index is 2.0+/-0.1, smaller than the 4FGL average value of 2.2+/-0.1. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is part of the "LAT Monitored Sources" and, consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/OS_300). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is C.C. Cheung (teddy.cheung@nrl.navy.mil). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-12-18 07:10:00
radio,gamma ray,agn,transient,request for observations
2021-12-18
07:10:00
2,218
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15,124
15,127
Search for counterpart to IceCube-211216B with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration.
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported event IceCube-211216B (GCN#31249). At the time of the alert, the reconstructed origin was -3.7 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible from [T-60min, T+22min] (68%). This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 17 GeV.cm^-2 over the energy range 5 TeV – 5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 40 GeV.cm^-2 (1 TeV - 450 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (40% visibility). ANTARES [http://antares.in2p3.fr/] is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2021-12-18 17:13:00
tev,neutrinos,transient
2021-12-18
17:13:00
1,253
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15,125
15,128
TRAPPIST C/2021 A1 (Leonard) comet production rates
E. Jehin, Y. Moulane, and J. Manfroid (STAR Institute, University of Liege)
E. Jehin, Y. Moulane, and J. Manfroid, report that they obtained on 19 December, from 00:15 to 01:15 UT, with the TRAPPIST-South (code=I40) robotic telescope (Jehin el al. 2011) located at the ESO La Silla Observatory (Chile), three sets of cometary HB narrowband filters (Farnham et al. 2000) and broad band filters (B,V,Rc,Ic) on comet C/2021 A1 (Leonard) at high airmass under photometric conditions. The comet, 15 days from perihelion, was at a heliceontric distance of 0.70 au and 0.36 au from the Earth. Preliminary production rates at 10.000 km using a Haser Model (Vp=Vd=1km/s) (Haser 1957) were computed as well as the dust production rate proxy A(0)f(rho) estimated by profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). The three sets of measurements were in very good agreement and the average value for each quantity is given below. C/2021 A1 (Leonard) Date UT=2021-12-19, r_h=0.70 au, Delta=0.36 au, DT=-15 days Q(OH)=(9.31+/-0.33) E28 s-1 Q(NH)=(5.90+/-0.20) E26 s-1 Q(CN)=(2.21+/-0.10) E26 s-1 Q(C2)=(2.61+/-0.08) E26 s-1 Q(C3)=(2.60+/-0.05) E25 s-1 A(0)fp(RC)= 975+/-52 cm A(0)fp(R)= 1087+/-30 cm From these measurements, C/2021 A1 has the composition of a typical comet with log[Q(C2)/Q(CN))]=0.07 and it has a typical dust/gas ratio with log[Afp/Q(OH)]=-25.98 (A'Hearn et al. 1995). Broad band images reveal a sharp and bright false nucleus of fwhm 5.5", R mag = 8.10+/-0.05, no peculiar coma features, and no fragment. Notations: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, NH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, GC, RC are the blue, green and red dust continuum filters (Farnham et al. 2000) Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS under grant PDR T.0120.21. We thank NASA, David Schleicher and the Lowell Observatory for the loan of a set of HB comet filters. Observations were carried on from the ESO La Silla Paranal Observatory.
2021-12-20 17:47:00
optical,comet
2021-12-20
17:47:00
2,046
[ -0.021924521774053574, 0.036535996943712234, 0.06326334923505783, -0.029866376891732216, 0.036205049604177475, -0.08844096213579178, -0.05337024852633476, 0.08325868099927902, -0.0784183144569397, 0.021447956562042236, -0.01022604014724493, -0.06613332778215408, 0.04883870854973793, -0.06665723770856857, 0.08475740253925323, 0.011866629123687744, 0.03674917295575142, -0.08473492413759232, -0.0026092410553246737, -0.07757890969514847, 0.020832184702157974, 0.01373604591935873, -0.045607250183820724, -0.053534507751464844, 0.05805361270904541, -0.008419127203524113, -0.07108946889638901, -0.10621649026870728, -0.03461353853344917, -0.05774742364883423, -0.06391111016273499, 0.016681160777807236, -0.016702324151992798, -0.060229863971471786, 0.05043542757630348, -0.03132244944572449, 0.01979670859873295, -0.027114305645227432, 0.0009517240105196834, 0.003630443010479212, -0.01616525463759899, -0.03039070963859558, -0.02383105456829071, -0.02675636112689972, -0.07131637632846832, 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15,126
15,129
Fermi-LAT observations of flaring activity from PKS 0346-27 and PKS 0735+17
G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar PKS 0346-27, also known as 4FGL J0348.5-2749 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 57.159 deg., Dec. = -27.820 deg. (J2000; Beasley et al. 2002 ApJS, 141, 13), and redshift z=0.991 (White et al. 1988 ApJ, 327, 561). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on December 19, 2021, with a daily averaged gamma-ray flux (E>100MeV) of (2.6+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). It also shows associated emission of nine high-energy (>10 GeV) photons, the most-energetic one having an estimated energy of 25 GeV. The flux increase corresponds to a factor of 60 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon index is 1.68+/-0.05, and is significantly smaller than the 4FGL value of 2.18+/-0.02. This source entered into a persistent high state on November 6, 2021 (see ATels #15020, #15092) and the current flux enhancement represents the highest flux ever observed by LAT on a daily scale. On the same day, enhanced gamma-ray activity was also observed from a source positionally consistent with the BL Lac object PKS 0735+17, also known as 4FGL J0738.1+1742 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 114.531 deg., Decl. = +17.705 deg. (J2000; Fey et al. 2015 AJ, 150, 58), and redshift z = 0.45 (Gattano et al, 2018 A&A, 618, A80). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state, with a daily averaged gamma-ray flux (E>100MeV) of (0.6+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), corresponding to a flux increase of a factor of 10 relative to the average flux reported in 4FGL. The estimated photon index is 2.0+/-0.2, and is consistent with the 4FGL value of 2.03+/-0.01 within the uncertainties. This source was also observed during a flaring state on December 8, 2021, close to the best-fit localization of the IceCube neutrino alert IC211208A (ATel #15099). The current flux is consistent within the uncertainties to the peak flux measured on December 4, representing the highest levels ever observed for this source on a daily scale. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of these sources will continue. For 4FGL J0348.5-2749, the light curve can be accessed via the Fermi-LAT Light-Curve Repository (LCR) at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/lcr/source.php?source_name=4FGL_J0348.5-2749. The Fermi-LAT contact person for this source is Bindu Rani ( binduphysics AT gmail.com ). For 4FGL J0738.1+1742, the light curve can be accessed via LCR at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/lcr/source.php?source_name=4FGL_J0738.1+1742. The Fermi-LAT contact persons are S. Garrappa (simone.garrappa AT desy.de) and S. Buson (sara.buson AT gmail.com). We encourage multifrequency observations of these sources. The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-12-21 07:34:00
radio,gamma ray,neutrinos,agn,blazar,quasar,transient,request for observations
2021-12-21
07:34:00
3,442
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15,127
15,130
Re-brightening of the BL Lac object PKS 0735+178 observed by Swift
Filippo D'Ammando (INAF-IRA Bologna)
Following the strong activity observed in radio (ATel #15105), optical (ATel #15098), X-rays (ATel #15102, #15109) and gamma-rays (ATel #15099) from the BL Lac object PKS 0735+178, as part of the follow-up observations of the region around the IceCube event IC211208A (GCN #31191), the Swift monitoring of the source has continued and further observations were performed on 2021 December 14 and 17. Swift/XRT data were taken during 2021 December 14 and 17 in Photon Counting mode for a net exposure of about 1.2 and 2.8 ksec, respectively. Preliminary analysis has been performed fitting the 0.3-10 keV X-ray spectrum with an absorbed power-law with the Galactic absorption corresponding to a hydrogen column density of n_H = 3.67 x 10^20 cm^-2 (Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 2.24 +/- 0.25 and 2.74 +/- 0.12 for 2021 December 14 and 17, respectively. The corresponding unabsorbed 0.3-10 keV flux is (3.9 +/- 0.6)e-12 and (8.2 +/- 0.5)e-12 erg cm^-2 s^-1 on December 14 and 17, respectively. The flux observed on 2021 December 17 is slightly lower than the maximum flux observed so far from this source on 2021 December 10 (ATel #15109), with a significant softening of the X-ray spectrum. This behaviour is in agreement with the enhanced gamma-ray activity observed on 2021 December 19 (ATel #15129). Simultaneous Swift/UVOT observations were performed on 2021 December 14 and 17. The observed magnitudes are: B = 15.19 +/- 0.05, U = 14.31 +/- 0.05, W1 = 14.24 +/- 0.06, M2 = 14.22 +/- 0.06, W2 = 14.34 +/- 0.05 for 2021 December 14; B = 15.32 +/- 0.05, U = 14.40 +/- 0.05, W1 = 14.37 +/- 0.06, M2 = 14.40 +/- 0.06, W2 = 14.48 +/- 0.05 for 2021 December 17. These values confirm a re-brightening of the source in optical and UV bands with respect to UVOT observations performed during 2006-2012 and marginally to the values observed on 2021 December 12 and 13 (ATel #15109), in agreement with the behaviour observed in X-rays. In consideration of the re-brightening of the source, confirmed also by the Swift observations, we encourage further multi-wavelength observations. Additional Swift observations are planned. We would like to thank the Swift Team, the Swift ODS, and the PI for making these observations possible.
2021-12-21 19:36:00
radio,optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar
2021-12-21
19:36:00
2,262
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-0.04846761003136635, -0.04762324318289757, 0.002167728031054139, 0.05032596364617348, -0.05003988370299339, 0.03039742447435856, -0.019080448895692825, -0.0736924558877945, -0.0078325429931283, 0.03911036625504494, -0.02595827542245388, -0.05064032971858978, -0.026681775227189064, -0.047801148146390915, -0.06112126260995865, 0.03578127920627594, 0.03713943064212799, -0.07423557341098785, -0.042437996715307236, 0.02972537651658058, 0.07041987031698227, -0.08279616385698318, -0.13891388475894928, -0.0065633621998131275 ]
15,128
15,131
Gaia21fji is indeed a Young Stellar Object
Ch. Adami, N. Grosso (LAM-Marseille), M. Dennefeld (IAP-Paris), St. Favard, J. Schmitt, Fr. Huppert, J. C. Brunel (OHP)
Gaia 21fji (= AT2021aftk) was alerted on Nov. 6, 2021 due to a recent brightening (Hodgkin et al., TNS Astronomical Transient Report 130737) and noted as "Candidate YSO". It had in fact been recognised as variable much earlier by the ATLAS survey (Tonry et al. 2018, PASP 130, 4505) as ATLAS 16awa. We obtained a classification spectrum on Dec. 8 with the new Mistral spectrograph mounted on the Cassegrain focus of the Haute-Provence Observatory (OHP) 1.93m telescope. The red setting was in use, covering the range from 6000 to 9800 Angstroems, at a resolution of 2.1 A per pixel and a 2" (= 4 pixels) N-S slit. The spectrum displays many strong emission lines above a red continuum: Halpha (with an EW of -114 A), the full series of Paschen lines, from PBeta to P14 (last detected line), the IR Calcium triplet and the OI line at 8446 A. Most notably, the OI 7771 line is not seen, nor any stellar absorption line. The object is therefore undoubtedly a reddened Young Stellar Object (YSO). In fact, the position measured by Gaia coincides with the pre-main-sequence star LkHalpha-324SE in the wider complex L988 discussed by Herbig & Dahm (2006 AJ, 131,1530) and is therefore not a new candidate. But we see no [OI] 6300 nor the [SII] doublet 6723 A in emission, to an upper limit of 0.5 % of Halpha, which were seen by those authors (but our slit was not oriented along the NW flow). As we have presently no measure yet of Hbeta, it cannot be decided yet if the recent increase in brightness is due simply to a decrease of obscuration, moving dust clumps in the disc or another cause. It is to be noted that the ATLAS lightcurve shows a steady increase of more than 2 magnitudes since August 25 this year, and both Gaia and ATLAS lightcurves show that similar excursions have already occured in the past: the object deserves further spectroscopic monitoring.
2021-12-21 22:13:00
optical,pre-main-sequence star,star,transient,variables,young stellar object
2021-12-21
22:13:00
1,862
[ -0.04460489749908447, -0.03711531311273575, -0.01589384488761425, 0.004240753129124641, 0.08289564400911331, -0.030260493978857994, 0.002474658889696002, 0.03469105064868927, 0.014748960733413696, -0.04909436032176018, -0.0699755921959877, -0.053052838891744614, -0.05825173109769821, -0.021243995055556297, 0.042164575308561325, -0.0077810329385101795, 0.0762440413236618, -0.12254780530929565, 0.02258259430527687, 0.04312961548566818, 0.012601933442056179, 0.06274393945932388, -0.06735312938690186, 0.021648835390806198, 0.06680059432983398, -0.03698495402932167, -0.06380816549062729, -0.0071868933737277985, 0.004247481469064951, -0.016642505303025246, 0.01793145202100277, 0.0763070285320282, -0.04827186092734337, 0.003874374320730567, 0.034632641822099686, -0.018436374142766, 0.10194814950227737, -0.03535643592476845, 0.007214562967419624, 0.07699355483055115, -0.009539074264466763, -0.07525040209293365, -0.028284763917326927, -0.005411435384303331, -0.03364601358771324, 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15,129
15,132
Optical view of neutrino emitter candidate PKS 0735 +178
Renato Falomo (INAF/OAPD), Aldo Treves (Universita dell Insubria, INAF/OABrera), Simona Paiano (INAF/OAR, INAF/IASF-PA)
PKS0735+178 is the possible counterpart of the neutrino event IceCube 211208 (GCN#31191), and a Baikal neutrino (ATEL#15112). The event corresponded too high activity of source in gamma rays (ATEL#15099), X-rays (ATEL#15102, #15108, #15109, #15113), optical (ATEL 15021), and radio (ATEL#15105). In spite of several attempts to detect intrinsic absorption and/or emission lines in the optical spectrum of PKS0735+178, no such features were detected thus a firm determination of the redshift is not available. However, since 1974 an intervening absorption system was detected (Carswell et al. 1974, ApJ,190,101) at ~3980 Ang and associated to MgII 2800 Ang doublet. This sets a firm lower limit to the redshift of z > 0.424. This absorption was confirmed in follow up spectroscopy adding other absorption features at the same redshift (Falomo and Ulrich 2000, A&A,357,91 and Rector et al 2001, AJ,122,565). The optical spectrum obtained at VLT+FORS (Landoni et al 2013, AJ,145,114) is reproduced in https://web.oapd.inaf.it/zbllac/extra/atel0735_fig.jpg. From this spectrum we can set an upper limit for the emission line of [OII] 3727 Ang in the spectral range 5300-6700 Ang (corresponding to a redshift range limit z < 0.8). No emission lines are detected in this range down to an equivalent width EWmin = 0.2 Ang. Therefore the upper limit of the line flux is F ~ 3 x 10^(-16) erg/cm2/s. This corresponds to line luminosity upper limits in the range 1.5 to 6 x 10^(41) erg/s. Various attempts were also performed to resolve the host galaxy of this source both from ground (Stickel et al 1993; Falomo & Ulrich 2000, A&A,357,91) and space using HST (Scarpa et al 2000,ApJ,544,258, Urry et al 2000,ApJ,532,816). In all cases optical imaging failed to detect the surrounding nebulosity. Assuming the host galaxy is typical of BL Lac objects (e.g. Falomo, Pian and Treves 2014,A&Av,22,73) a lower limit (z > 0.5) to the redshift was estimated from the non detection of the host (Falomo & Ulrich 2000,A&A,357,91). Deep images of the field around this source revealed a number of galaxies in the immediate environment (see Figure in https://web.oapd.inaf.it/zbllac/extra/atel0735_fig.jpg ). In particular the companion galaxy at 7" NW of the BL Lac object is at z = 0.645 corresponding to a projected distance from the target of only 50 kpc. Another fainter galaxy is found at ~ 3.5" East. If these galaxies form a small group associated to the target, a plausible redshift is z ~ 0.65.
2021-12-22 00:30:00
radio,optical,x-ray,gamma ray,neutrinos,blazar
2021-12-22
00:30:00
2,481
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15,130
15,133
eRASSU J050810.4-660653 in the LMC: Discovery of X-ray pulsations with XMM-Newton and NuSTAR
F. Haberl (MPE), A. Salganik (St. Petersburg State University, IKI), C. Maitra (MPE), V. Doroshenko, L. Ducci (IAAT Tuebingen), D. Kaltenbrunner (MPE), I. Kreykenbohm (Remeis-Observatory/ECAP, FAU Erlangen), A. Lutovinov (IKI), P. Maggi (Universite de Strasbourg), I. Mereminskiy, S. Molkov (IKI), A. Rau (MPE), A. Semena (IKI), S. Tsygankov (IKI, University of Turku), G. Vasilopoulos (Universite de Strasbourg), P. Weber, J. Wilms (Remeis-Observatory/ECAP, FAU Erlangen)
eRASSU J050810.4-660653 is a new Be/X-ray binary in the LMC, which was discovered during the beginning of the first all-sky survey of the eROSITA instrument on board the Russian/German Spektrum-Roentgen-Gamma (SRG) mission (ATel#13609). During the end of the second survey (eRASS2) the source was bright again and we triggered one of our anticipated target of opportunity (TOO) observations with XMM-Newton. The XMM-Newton observation was performed on 17 Dec, 2020 for a total exposure of about 32 ks. The derived X-ray source position of RA (J2000) = 05:08:09.99, DEC (J2000) = -66:06:51.6 with an estimated uncertainty of 0.5" radius (including systematics) is within 0.6" of the position of the proposed optical counterpart. A power spectrum of the EPIC-pn data revealed X-ray pulsations with a period of about 40.6 s, together with five harmonics. Using a Bayesian approach (Gregory & Loredo 1996) we determined the fundamental period to 40.60254(8) s. The pulse profile is characterized by a deep narrow dip which causes the large number of harmonics and a pulsed fraction of about 25%. During the ongoing all-sky survey we have detected an enhanced X-ray activity from the source with the Mikhail Pavlinsky ART-XC telescope. The source was registered on 16-17 Dec, 2021 at the level of ~2 mCrab (3×10-11 erg cm-2 s-1) in the 4-12 keV band. For LMC distance this corresponds to a luminosity of about 1037 erg s-1, that is an order of magnitude higher, than at the moment of its discovery with eROSITA in 2019 (ATel#13609). We have triggered a NuSTAR TOO observation, which allowed us to independently detect the pulse period at ~40.578 s, a value similar to that measured one year ago. The spectrum is typical for X-ray pulsars and could be described by a cutoff power-law. We are grateful to the NuSTAR team for approving and rapid scheduling of the follow-up observation.
2021-12-23 05:05:00
optical,x-ray,binary,neutron star,pulsar,star,transient
2021-12-23
05:05:00
1,878
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-0.04440097510814667, -0.03810194879770279, 0.036765530705451965, 0.0012938346480950713, 0.05167849361896515, -0.04942823573946953, -0.01086745411157608, 0.010118774138391018, 0.03410780802369118, -0.03519293665885925, -0.04705045744776726, -0.0032474875915795565, -0.11466402560472488, -0.04565249755978584, 0.02204601839184761, -0.005234020296484232, -0.006473434157669544, 0.03286366909742355, 0.05287138372659683, 0.032886989414691925, -0.0329752154648304, -0.02402857504785061, 0.011013073846697807 ]
15,131
15,134
Optical-to-X-ray Flare in Markarian 501
Bidzina Kapanadze (Ilia State University, Tbilisi, Georgia; E. Kharadze National Astrophysical Observatory, Abastumani, Georgia)
In ATel#15124 (posted on 2021 December 17), we reported the X-ray flare in the nearby, TeV-detected blazar Markarian 501 (z=0.034) which is undergoing variations in the baseline X-ray level on the timescales of several years, and since 2021 March, we observe a significantly enhanced X-ray activity of the source compared to the previous years (and comparable to the flaring behaviour shown in 2014 March-October; see Kapanadze et al. 2017, MNRAS, 469; 1655). Currently, Mrk 501 is monitored by Neil Gehrels Swift Observatory in the framework of our Target of Opportunity (TOO) request Number #16518. The Swift-XRT visit to the source on December 22 revealed a further increase in the 0.3-10 keV count rate, amounting to 13.31+/-0.13 cts/s (derived from our thorough analysis of the quick-look data published on https://swift.gsfc.nasa.gov/cgi-bin/sdc/ql) and corresponding to the unabsorbed 0.3-10 keV flux of 5.25e-10 erg/cm^2/s), which is ~50 per cent higher compared to the level recorded during the previous X-ray on December 16 (and reported in In ATel#15124). The spectrum is very hard, corresponding to the photon index at 1 keV $a$=1.76+/-0.2 which can be related to the hadronic synchrotron contribution to the 0.3-10 keV energy range (see, e.g. Kapanadze et al. 2017). In the UVOT bands, the source shows elevated optical and UV brightness levels correspond to V=13.15+/-0.03 mag, B=13.82+/-0.04 mag, U=13.45+/-0.03 mag, UVW1=13.64+/-0.04 mag, UVM2=13.54+/-0.04 mag, UVW2=13.54+/-0.03 mag. Consequently, the intense multiwavelength observations of the source are strongly encouraged for discerning the underlying emission mechanisms and instable processes. XRT is one of the Swift instruments along with Burst Alert Telescope (BAT) and UV/Optical Telescope (UVOT). It is a JET-X Wolter I type telescope, developed jointly by Pennsylvania State University, Brera Astronomical Observatory (OAB) and University of Leicester. Thanks to the unique characteristics, good photon statistics and low background counts of this instrument (in combination with EEV CCD2 detector), we can investigate a flux variability on different time-scales from minutes to years, obtain high-quality spectra for the majority of the observations, derive different spectral parameters, and study their timing behaviour in the 0.3-10 keV range of the electromagnetic spectrum. The Swift Satellite is operated by Pennsylvania State University.
2021-12-23 06:10:00
optical,ultra-violet,x-ray,tev,black hole,blazar
2021-12-23
06:10:00
2,425
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15,132
15,135
SRG/eROSITA observations of PKS 0903-57
S. Haemmerich (Remeis-Observatory/ECAP, FAU Erlangen), A. Gokus (Remeis-Observatory/ECAP, FAU Erlangen & Uni Wuerzburg), I. Kreykenbohm (Remeis-Observatory/ECAP, FAU Erlangen), P. Weber (Remeis-Observatory/ECAP, FAU Erlangen), J. Wilms (Remeis-Observatory/ECAP, FAU Erlangen), A. Zainab (Remeis-Observatory/ECAP, FAU Erlangen)
On 2021 November 19 and 20, the blazar PKS 0903-57 was reported to exhibit enhanced gamma-ray activity (Ciprini et al., ATel #15057). The source seems to have been in an enhanced state since October 2021. In the past, five flares have been reported by the Fermi/LAT collaboration. Swift follow-up observations (Mereu et al., ATel #15058) revealed that the blazar also showed increased flux in the X-ray regime. Between 2021 December 03 and 05 AGILE again reported increased activity in the gamma rays (C. Pittori et al.,ATel #15086). The source was followed up by Swift between 2021 November 28 and December 06. These findings suggest a long-term X-ray flaring of the source. Here we report on the recent observations of PKS 0903-57 by the eROSITA telescope (Predehl et al. 2021, A&A 647, A1) onboard the Russian/German Spectrum-X-Gamma mission (Sunyaev et al. 2021, arxiv:2104.1326). The position of the source (RA = 09:04:53.70, DEC = -57:35:05.86) has been scanned multiple times during the ongoing all-sky survey. The most recent observation took place between 2021 December 14 19:15 UTC and 2021 December 17 03:15 UTC. The total exposure was 448s, in which 360 counts were detected. Describing the X-ray spectrum by an absorbed power-law model, with the equivalent neutral hydrogen column density fixed to N_H=2.6x10^21 cm^-2 (HI4PI Collaboration, N. Ben Bekhti, et al., 2016, A&A 594, A116) we find a best fit photon index of 1.7 +/- 0.2 and an absorbed 0.3-10 keV flux of (6.5 +/- 0.6) x 10^-12 erg/cm^2/s (all following values use the same band). The count rate was (0.80 +/- 0.05) counts/s. The four previous eROSITA observations yielded the following results: 2019 December 09-11: Flux: (2.1 +/- 0.4) x 10^-12 erg/cm^2/s Count rate: (0.33 +/- 0.04) counts/s photon index: 2.1+/-0.4 2020 June 07-09: Flux: (3.1 +/- 0.4) x 10^-12 erg/cm^2/s Count rate: (0.39 +/- 0.03) counts/s photon index: 1.72+/-0.27 2020 December 11-13: Flux: (4.2 +/- 0.7) x 10^-12 erg/cm^2/s Count rate: (0.31 +/- 0.03) counts/s photon index: 1.6+/-0.4 2021 June 12-14: Flux: (5.3 +/- 0.9) x 10^-12 erg/cm^2/s Count rate: (0.39 +/- 0.04) counts/s photon index: 1.6+/-0.4 The eROSITA measurements in combination with the Swift results suggest that the blazar has increased in X-ray flux significantly over the past two years, therefore supporting the suggestion that the blazar is in an X-ray flaring state. The results also suggest that the spectral shape has changed, as the spectrum seems to become harder before the reported flaring activity. However, the values agree with each other within the uncertainties to some extent. Further monitoring of the source, especially with X-ray facilities, is encouraged to study the long term behavior of PKS 0903-57.
2021-12-24 00:27:00
x-ray,gamma ray,agn,blazar
2021-12-24
00:27:00
2,748
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15,133
15,136
Optical and near-infrared observations of PKS 0735+178
Elina Lindfors (FINCA), Talvikki Hovatta (FINCA), Tapio Pursimo (NOT), Viktoria Pinter (NOT), Stephen Warren (Imperial), Thomas Andradi-Brown (Imperial), Zhang-Liang Xie (MPIA), Eduardo Banados (MPIA), Dino Fugazza (INAF Brera), Emilio Molinari (INAF Cagliari)
We have performed optical and near-infrared observations of the BL Lac object PKS 0735+178 following the strong activity observed in radio (ATel #15105), optical (ATel #15098), X-rays (ATel #15102, #15109, #15130) and gamma-rays (ATel #15099, #15129), which were triggered by the source proximity to the IceCube event IC211208A (GCN #31191) and the Baikal-GVD detection of a neutrino from the same region (ATel #15112). The observations were performed between Dec 15 and 19 with the Rapid Eye Mount (REM) telescope at La Silla, Chile and the Nordic Optical Telescope (NOT) at La Palma, Spain. The NOT observations were made using NOTCam. Standard IRAF data reduction (flat field correction with twilight flats + combining dithered images) was carried out and differential photometry was performed. The brightness was estimated against three nearby 2MASS stars K-magnitudes between 10.9 and 11.9 (marked C, C1 and C2 in the finding chart available here: https://users.utu.fi/kani/1m/finding_charts/PKS_0735+178_map.html). The standard deviation of the zero point was 0.02 mag. We find that PKS 0735+17 had the following K-band magnitudes on 2021-12-16T07:20 Ks=11.57+-0.02 and on 2021-12-18T06:45 Ks=11.62+-0.03. The REM observations were made using both REMIR (K-filter) and ROS2 (g,r,i,z filters) cameras. Standard IRAF data reduction was carried out and differential photometry was performed. In K-band the brightness was estimated against the same 2MASS stars as above, but the standard deviation of the zero point was 0.06mag. In g,r,i and z filters, the brightness was estimated using three nearby Pan-STARRS stars (marked C4, B and C7 in the finding chart available here: https://users.utu.fi/kani/1m/finding_charts/PKS_0735+178_map.html). We find that PKS 0735+17 had the following magnitudes: K-band: 2021-12-15T05:50 K=11.46+-0.07 2021-12-16T05:51 K=11.50+-0.12 2021-12-17T05:51 K=11.53+-0.07 2021-12-18T05:51 K=11.58+-0.07 z-band: 2021-12-15T05:50 z=14.35+-0.04 2021-12-16T05:51 z=14.46+-0.03 2021-12-17T05:51 z=14.49+-0.07 2021-12-18T05:51 z=14.41+-0.1 2021-12-19T05:55 z=14.54+-0.1 i-band: 2021-12-15T05:50 i=14.61+-0.02 2021-12-16T05:51 i=14.50+-0.04 2021-12-17T05:51 i=14.57+-0.03 2021-12-18T05:51 i=14.56+-0.1 2021-12-19T05:55 i=14.70+-0.03 r-band: 2021-12-15T05:50 r=14.77+-0.013 2021-12-16T05:51 r=14.80+-0.02 2021-12-17T05:51 r=14.86+-0.014 2021-12-18T05:51 r=14.75+-0.03 2021-12-19T05:55 r=14.91+-0.03 g-band: 2021-12-15T05:50 g=14.98+-0.02 2021-12-16T05:51 g=14.98+-0.02 2021-12-17T05:51 g=15.19+-0.02 2021-12-18T05:51 g=15.08+-0.04 2021-12-19T05:55 g=15.16+-0.04
2021-12-24 01:02:00
radio,infra-red,optical,x-ray,gamma ray,neutrinos,agn,blazar,quasar,star
2021-12-24
01:02:00
2,583
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-0.014136112295091152, 0.06014234572649002, 0.08157405257225037, -6.36321644265081e-8, 0.03209703415632248, 0.07853485643863678, -0.08150622993707657, 0.028953230008482933, 0.006462643388658762, -0.08043784648180008, -0.05757848173379898, 0.07223106920719147, -0.023989519104361534, 0.022099046036601067, -0.005044454243034124, 0.028420301154255867, 0.03864444047212601, -0.03822392597794533, 0.04479437693953514, 0.013666176237165928, 0.0294057484716177, -0.11830797791481018, -0.007047721650451422, 0.014568054117262363, 0.046264905482530594, -0.05323838070034981, 0.03591281548142433, -0.07113409042358398, -0.04812830314040184, 0.026249274611473083, 0.011279263533651829, 0.07045139372348785, 0.10040238499641418, -0.10119359195232391, -0.016448654234409332, -0.03548344597220421, 0.019515255466103554, -0.03085697628557682, 0.08063959330320358, 0.07854987680912018, -0.13192227482795715, 0.015080130659043789, 0.09316541999578476, 0.06397514790296555, -0.012495661154389381, -0.058977484703063965, 0.0065557644702494144, 0.03926252946257591, -0.06007673218846321, 0.00612930441275239, -0.04807562008500099, -0.12535786628723145, 0.017646869644522667, 0.051190704107284546, -0.03892705962061882, -0.07089151442050934, 0.02107478491961956, -0.025299547240138054, -0.061023127287626266, 0.051042892038822174, 0.028774319216609, -0.016959525644779205, -0.02936081774532795, -0.002398210344836116, 0.08771484345197678, -0.05663466826081276, -0.11049988120794296, -0.012394558638334274 ]
15,134
15,137
Spectroscopic Classification of AT2021agid with SOAR + Goodman
K. W. Davis, K. Taggart, S. Tinyanont, R. J. Foley (UC Santa Cruz)
We report the classification of AT2021agid from spectroscopic observations with the Goodman spectrograph on the Southern Astrophysical Research (SOAR) telescope, made on 2021 Dec 18 UT. The target was supplied by ATLAS. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We measure an H-alpha absorption velocity of -6,800 km/s.
2021-12-24 05:08:00
optical,supernovae
2021-12-24
05:08:00
517
[ -0.060132551938295364, -0.07798638939857483, -0.037330109626054764, 0.043311525136232376, 0.07612617313861847, 0.044179197400808334, -0.051515642553567886, 0.018765125423669815, -0.012736768461763859, -0.013979392126202583, -0.013834946788847446, -0.046068545430898666, -0.04287128895521164, -0.04574887454509735, -0.03021448850631714, -0.0403200201690197, 0.03834818676114082, -0.09402312338352203, 0.009281542152166367, 0.03168166056275368, -0.01515041384845972, 0.09322217851877213, -0.04954695329070091, 0.09280095249414444, 0.09544786065816879, -0.043593570590019226, -0.08942022174596786, -0.08143112808465958, -0.008006684482097626, -0.023686440661549568, 0.11705024540424347, 0.051974352449178696, 0.014004848897457123, 0.06795098632574081, 0.025296904146671295, -0.04983626306056976, 0.0685979351401329, 0.01650816760957241, 0.00897157471626997, -0.037132106721401215, 0.005669774021953344, -0.062000252306461334, 0.04583163186907768, 0.03435574099421501, -0.05059415474534035, 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-0.049575161188840866, -0.03344500809907913, 0.005269715096801519, 0.03202252835035324, -0.08521249890327454, -0.05077139660716057, -0.012290078215301037, -0.05015634000301361, 0.012157754972577095, 0.04696652293205261, -0.043985188007354736, -0.011841654777526855, -0.07119965553283691, -0.025171827524900436, -0.11859587579965591, -0.019767707213759422, -0.014719169586896896, -0.07184956222772598, -0.033602118492126465, -0.027469662949442863, 0.18389002978801727, -0.04819158837199211, -0.1325538158416748, -0.019337031990289688 ]
15,135
15,138
Classification of Gaia Alerted QSO candidates
T. Pursimo (NOT-LaPalma), M. Dennefeld (IAP-Paris)
Variability is a good mean to discover new Quasars, particularly radio-quiet ones. The Gaia Alerts (Hodgkin et al. 2021, A&A 652, 76) are emitted upon photometric variations and point, under others, also to QSO candidates when the magnitude change is larger than 0.3 mag. We are following a classification program at the Nordic Optical Telescope in LaPalma with the ALFOSC spectrograph. The grating 4 is used, covering the range 350-960 nm, with a resolution of 300 and a 1.3 arcsec slit. Some first results are given below: GaiaName, TNSname, Type, Redshift, Lines seen, Gaia18dww AT2018kjg NLS1 0.2880 Halpha (1300 km/s FWHM), Hbeta, Hgamma, [OIII], FeII Gaia19abv AT2019kn QSO 0.4275 Ha (2100 km/s), Hb, [OII] Gaia20dxw AT2020fhp QSO 0.232 Ha (10650 km/s), Hb, [OIII] Gaia20efz AT2020taf QSO 0.4682 Hb (2450 km/s), [OIII], Hg, MgII Gaia21aen AT2020aeve QSO 0.3848 Ha (2000 km/s), Hb, [OIII], [NeIII], [OII], MgII Gaia16bpi AT2016anj Star 0.0 Ha, Hb (galactic emission line star)
2021-12-24 22:51:00
radio,optical,quasar,star
2021-12-24
22:51:00
981
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15,136
15,139
MAXI/GSC detection of a new bright X-ray flare from the dMe star AU Mic
J. Kohara, W. Iwakiri, Y. Okamoto, S. Nawa, N. Nemoto, Y. Tsuboi, H. Kawai, S. Kitakoga (Chuo U.), H. Negoro, M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, T. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered on the bright X-ray flare from the position consistent with the dMe type star AU Mic during a scan transit at 22:49 UT on Dec 15 2021. The estimated X-ray flux in the 2-20 keV band of this flare during this scan transit is about 9.0 (-1.6,+1.7) × 10-9 erg/cm2/s. Assuming a distance of 9.7 pc (GaiaCollaboration et al. 2020), the peak luminosity is about 1 × 1032erg/s. This is about three times brighter than the peak luminosity of the flare previously detected by MAXI on April 15, 2020(ATel #13635) and the largest ever observed by MAXI from AU Mic. In the next scan transit 00:22 UT on Dec 16 data of MAXI, the X-ray flare is still marginally detected with a significance of 3 sigma. If we assume that the flare flux decayed exponentially with time, the estimated e-folding time and the total energy in the 2 - 10 keV band of this flare are about 3000 sec and 3 × 1035erg, respectively.
2021-12-24 23:01:00
x-ray,nova,star
2021-12-24
23:01:00
931
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0.07253143191337585, 0.05719056352972984, -7.397840562362035e-8, -0.0029951187316328287, -0.04206269234418869, 0.11923161149024963, 0.0269320048391819, 0.0031776532996445894, -0.0338284932076931, -0.0011972718639299273, 0.08973407000303268, -0.007015106733888388, 0.037227604538202286, 0.06695471704006195, 0.1568264216184616, 0.029529303312301636, 0.009285827167332172, 0.0935247614979744, -0.04817117750644684, 0.06907437741756439, 0.09605716168880463, -0.08912292867898941, -0.028582297265529633, 0.02510908804833889, -0.00909498706459999, 0.03926590830087662, -0.04624341428279877, -0.008867231197655201, -0.012296975590288639, 0.03799600526690483, 0.01307662297040224, -0.02586238831281662, 0.00786656979471445, -0.00574064813554287, -0.024906830862164497, 0.06643102318048477, -0.028203178197145462, 0.011682721786201, 0.06202806904911995, -0.005798695608973503, -0.03224126249551773, -0.058074288070201874, 0.042212653905153275, -0.0956980511546135, -0.023875752463936806, -0.034760601818561554, 0.10454843193292618, 0.046292804181575775, 0.046864453703165054, -0.012290255166590214, 0.034627798944711685, 0.014752039685845375, -0.0333094447851181, -0.0062269424088299274, -0.01146030519157648, 0.025756537914276123, -0.03923770412802696, -0.04204356297850609, 0.07616709917783737, 0.0196682158857584, -0.06474968045949936, 0.007815621793270111, -0.04779663681983948, 0.029088925570249557, -0.05564125254750252, -0.010492248460650444, 0.06235533207654953 ]
15,137
15,140
LJT spectroscopic classification of AT 2021agnf as a 91bg-like Type Ia supernova
Qian Zhai, Jujia Zhang (YNAO); Xiaofeng Wang(THU)
We report an optical spectrum of AT 2021agnf (350-870nm) obtained on 2021 Dec. 24.79 UT with the Lijiang 2.4-m telescope (LJT +YFOSC) at Lijiang observatory of Yunnan Observatories. The spectrum is similar to a 91bg-like type Ia supernovae around the peak. Cross-correlation with the library of supernova spectra using the comparison tool SNID (Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches SN 1991bg at t = +3 days at the given redshift = 0.023 of the host galaxy CGCG 175-003. The expansion velocity derived from the Si II 6355 is about 9000 km/s.
2021-12-25 10:42:00
optical,supernovae
2021-12-25
10:42:00
565
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15,138
15,141
Additional Bursts from SGR 1935+2154 Seen by Swift BAT
David Palmer (LANL) on behalf of the Swift Team
The recent burst from the soft gamma repeater SGR 1935+2154, seen by AGILE and Fermi GBM at T0=2021-12-24 03:42:34 UT (Ursi et al., GCN #21296) was also detected and localized by Swift BAT, (Trigger #1090704; Burst #1) confirming the identity of the source. BAT also detected two subsequent weaker bursts at 03:48:01 (Trigger #1090705; T+327s; Burst #2) and 03:51:27 (Trigger #1090706; T+533s; Burst #3). Burst #1 had a flat-topped profile with a 0.02 s rise, a 0.9 s plateau, and a 0.3 s decay. The count rate during the plateau was 24k counts/s. (All count rates are in the full instrumental band, which extends to slightly lower energies than BAT's usually-reported 15-350 keV band.) Burst #2 had a simple rise-and-fall peak with a duration of 0.03 s and a peak of 7k counts/s. Burst #3 had a wider peak with a squarer profile, a duration of 0.10 s and a peak of 2.2k counts/s. The most recent previous activity of this source seen by BAT was a month-long sequence of 15 bursts, extending from Sept. 11 to Oct. 11 of 2021.
2021-12-25 11:22:00
x-ray,gamma ray,magnetar,soft gamma-ray repeater
2021-12-25
11:22:00
1,030
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15,139
15,142
New giant radio flare from Cygnus X-3
S. A. Trushkin, N. A. Nizhelskij, P. G. Tsybulev (SAO RAS)
During the long-term multi-frequency monitoring of the Galactic microquasars with the RATAN-600 radio telescope we have detected the giant flare at 1.2-30 GHz from the microquasar Cygnus X-3 on 31 August 2021 (ATel #14281). This flare was probably characterized a single ejection event and was over relatively soon after two weeks. But the active X-ray state continued according the Swift/BAT data at 15-50 keV, and on 18 October 2021 (MJD 59505) we have detected the very unusually long giant flare with the maximum flux about 16 Jy at 4.8 GHz (see also ATel #14989, #14509, #14518). This flare consisted of some consistent ejection events and was over after 45 days, on MJD 59550. Both the August and October flares accompanied by the Gamma-ray activity, detected by the Fermi observatory (0.1-300 GeV) and continued to MJD 59531. On 24 December 2021 (MJD 59572.48) we have detected the new giant flare with fluxes: 2.0, 7.7, 16.1, 19.1, 18.8 and 12.7 Jy at 2.3, 4.7, 8.2, 11.2, 22.3 and 30 GHz respectively (errors are within 3-4%). According to the synchrotron emission theory such spectrum is determined by optically thick and optically thin modes of the forming jets. We consider that Cygnus X-3 is in the starting of jet motion and the flare will evolve. The radio spectra during last two days are given here . The Swift/BAT data (http://swift.gsfc.nasa.gov/results/transients/CygX-3) showed the 4-fold increase of hard X-ray flux at 15-50 keV on MJD 59572. Again we can see clear association of flaring events in the radio and X-ray bands, reflecting the disk-jet coupling in the X-ray binary stars as a result of a jet production in the polar regions of accretion disk around a black hole. This giant radio flare formed just after a transition from a hyper-soft X-ray state to a soft state in Cyg X-3. Following up the VLBI mapping, mm-band, X-ray and Gamma-ray observations of Cyg X-3 could be very useful.
2021-12-25 16:30:00
radio,millimeter,sub-millimeter,x-ray,gamma ray,binary,black hole,star,transient
2021-12-25
16:30:00
1,916
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15,140
15,143
Baksan Underground Scintillation Telescope observation of a GeV neutrino candidate event at the time of a gamma-ray flare of the blazar PKS 0735+17, a possible source of coinciding IceCube and Baikal high-energy neutrinos
V. B. Petkov, Yu. F. Novoseltsev and R. V. Novoseltseva (INR RAS) for the Baksan Underground Scintillation Telescope group
PKS 0735+17 is currently experiencing a major flare, which attracted much interest because it coincides with a simultaneous detection of two rare high-energy neutrino events by IceCube (172 TeV, GCN #31191) and Baikal-GVD (43 TeV, ATel #15112). The flare was reported in gamma rays (ATel #15099, #15129), X rays (ATel #15102, #15108, #15109, #15130), optical (ATel #15098, #15100, #15136) and radio (ATel #15105) bands. The flux of the blazar in gamma rays and in the optical band hits its historical maximum. The redshift of the blazar is uncertain, z>0.424 (ATel #15132). No additional neutrino events from the direction of the alert have been reported by IceCube (GCN #31195) and ANTARES (ATel #15106) on the same day. Here we report an observation of a lower-energy neutrino candidate event in coincidence with the gamma-ray flare of the blazar, 4 days before the two high-energy neutrino events. Baksan Underground Scintillation Telescope (BUST) detected an upgoing muon consistent with a neutrino of the energy above 1 GeV from the direction of PKS 0735+17 on December 4, 2021, at 14:52:47.83 UT. The best-fit arrival direction is RA=116.5, DEC=16.6, that is 2.18 deg from the source. The event coincided with the gamma-ray flare observed by Fermi LAT and preceded the IceCube and Baikal high-energy neutrinos by 4.2 days. With the BUST angular resolution of 2.5 deg (50% PSF containment) in the mode used and the average background of 1 upgoing muon per 8 days, the quick-look estimate of the false-alarm probability of a detection of 1 event from PKS 0735+17 during a 10-day gamma-ray flare is 0.0024, corresponding to the 3-sigma detection. More detailed investigation of this and other events from the same direction continues. PKS 0735+17 is a bright radio blazar and therefore belongs to the class of probable emitters of neutrinos with energies from TeV to PeV, according to Plavin et al. (2021). The present observation of a GeV neutrino by BUST extends this energy range 3 orders of magnitude lower and gives important information about hadronic processes in blazars. BUST (see e.g. Petkov et al., 2019) is the liquid-scintillator neutrino telescope at the Baksan Neutrino Observatory of INR RAS. Operating for almost 40 years, it is best known for the detection of neutrinos from SN 1987A. The present study uses different selection criteria than those used in the supernova-neutrino search, resulting in the threshold of 1 GeV for upgoing muon neutrinos.
2021-12-26 01:21:00
radio,optical,x-ray,gamma ray,tev,neutrinos,blazar,supernovae
2021-12-26
01:21:00
2,471
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15,141
15,144
Erratum to ATel #15141 (Additional Bursts from SGR 1935+2154 Seen by Swift BAT)
David Palmer (LANL)
In ATel #15141, uncertainty values were omitted in violation of ATel editorial policy, and are given here. (Values in parenthesis are uncertainty in last digit). All absolute times are quoted for the observed start of the burst, truncated to the UT second, with typical uncertainties in the underlying measurement of approximately 10 milliseconds. Burst #1 had a flat-topped profile with a total duration of 1.30(1) s, which can be approximately divided into 0.05(1)s of early emission, 0.02(1) seconds of rapid rise, 0.92(2)s of plateau, and 0.31(2)s of irregular fall. Count rate above background during the plateau was 23.8k counts ± 0.2k statistical error in the average ± ~10% intrinsic variability in the source. Burst #2 has a duration of 0.03(1) s and a peak of 6.7(8)k counts/s measured on a 10 ms timescale. Burst #3 has a duration of 0.12(2) s and a peak of 2.5(2)k counts/s measured on a 20 ms timescale.
2021-12-26 07:30:00
x-ray,gamma ray,magnetar,soft gamma-ray repeater
2021-12-26
07:30:00
920
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15,142
15,145
Swift detection of the blazar OJ 287 in a deep UV-optical low-state in the course of the MOMO program
S. Komossa (MPIfR), D. Grupe (Morehead State University), M. Valtonen (University of Turku)
We have monitored the blazar OJ 287 densely during the last six years with the Neil Gehrels Swift observatory in the course of the project MOMO (Multi-wavelength Observations and Modelling of OJ 287; e.g. Komossa et al. 2017, 2020, 2021a,b,c). Based on our most recent observations, we report the detection of a deep UV-optical low-state in all six UVOT filters. The low-state has so far lasted for at least three weeks, between 2021 December 2-25. On 2021 December 20, we measured Swift UVOT magnitudes in the VEGA system of UVW2: 15.75+/-0.06 (15.55), UVM2: 15.63+/-0.05 (15.39), UVW1: 15.56+/-0.05 (15.39), U: 15.54+/-0.04 (15.41), B: 16.37+/-0.04 (16.26), and V: 15.83+/-0.06 (15.75), where values in brackets are corrected for Galactic extinction. A similar optical-UV faintness was last seen during the 2017 October-December deep fade and in 2020 September (ATel #14052). While the UV and optical emission is in low-state, the X-rays do not follow the deep fade but remain relatively constant within the errors. On 2021 December 20, we measured an absorption-corrected X-ray flux of f_x = 5.0+/-0.4 10^-12 ergs/s/cm^2 and a photon index Gamma_x = 2.12+/-0.20 in the 0.3-10 keV band (using a single powerlaw fit with Galactic absorption). This pattern is similar to the remarkable UV-optical deep fade seen in 2017 October-December (Komossa et al. 2020, 2021c), where the flux in the UVOT bands dropped by a factor 3 and the X-rays did not follow. (During outbursts, the UV-optical emission is closely correlated with the X-rays.) UV-optical deep fades are well suited to obtain imaging observations of the host galaxy of OJ 287 that are much more difficult to perform when the blazar emission is brighter. The blazar OJ 287 is one of the best candidates to date for hosting a binary supermassive black hole (Valtonen et al. 2016). The Swift results presented here are part of our dedicated multi-year, multi-frequency (radio--X-ray) project MOMO (e.g. Komossa et al. 2017, 2020, 2021a,b,c). We would like to thank the Swift team for carrying out the observations we proposed.
2021-12-27 04:16:00
radio,optical,ultra-violet,x-ray,agn,binary,black hole,blazar,quasar
2021-12-27
04:16:00
2,081
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-0.06759248673915863, 0.01472618617117405, -0.00038483383832499385, 0.04606595262885094, -0.012235105037689209, 0.011765554547309875, 0.04209228977560997, -0.04551755264401436, 0.006386732216924429, 0.00012327863078098744, 0.010876310057938099, -0.04533417150378227, -0.003405896248295903, 0.020228326320648193, -0.11994832754135132, -0.0029950232710689306, 0.029392007738351822, -0.13839071989059448, -0.132839635014534, -0.000395577575545758, 0.10430996865034103, -0.1056724563241005, -0.10378456860780716, 0.013617586344480515 ]
15,143
15,146
Fermi-LAT detection of flaring gamma-ray activity from the FSRQ PKS 0403-13, and continued activity in GPS radio source OS 300 (4C +33.38, B2 1600+33)
Stefano Ciprini (INFN Roma Tor Vergata, & ASI Space Science Data Center, Rome, Italy), on behalf of the the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray emission from a source positionally consistent with the flat spectrum radio quasar (FSRQ) PKS 0403-13 (also known as TXS 0403-132, OF -105, RX J0405.5-1308, and 4FGL J0405.6-1308), with radio counterpart position R.A.: 61.391680 deg, Dec.: -13.137136 deg (J2000.0, Fey et al. 2004, AJ, 127, 3587) and with redshift z=0.5706+/-0.0001 (Marziani et al. 1996, ApJS, 104, 37). Preliminary analysis indicates that on December 25, 2021, PKS 0403-13 was in a high state with a daily averaged gamma-ray flux (E>100 MeV) of (1.0+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 80 times greater than the average flux reported in the 4FGL catalog. The corresponding daily averaged spectral photon index (E>100 MeV) of 2.7+/-0.2 is greater than the fourth Fermi-LAT catalog (4FGL) value of 2.55+/-0.05. This is second time that the Fermi-LAT Collaboration has announced flaring gamma-ray activity from PKS 0403-13 (ATel#9242). The LAT has also observed continuing and increasing gamma-ray activity from a source positionally consistent with the extragalactic radio source OS 300 (also known as 4C +33.38, B2 1600+33 and 4FGL J1602.1+3324, Abdollahi, et al. 2020, ApJS, 247, 33), with radio counterpart position R.A. = 240.530 deg, Dec. = +33.448 deg (J2000; Johnston et al. 1995, AJ, 110, 880). OS 300 is a Giga-Hertz Peaked Spectrum (GPS) radio source (Snellen et al. 2000 MNRAS 319, 445) with photometric redshift estimation of z = 1.1 (Snellen et al. 2000 MNRAS 319, 445). Preliminary analysis indicates that OS 300 was in a flaring state on 2021 December 26, with a daily averaged gamma-ray flux (E>100MeV) of (1.5+/-0.1) X 10^-6 photons cm^-2 s^-1 (uncertainties are statistical only), and a peak 6-hr flux of (2.4+/-0.4) X 10^-6 photons cm^-2 s^-1 from 12:00-18:00 UTC. The former corresponds to a flux increase of a factor of about 330 relative to the average flux reported in the 4FGL catalog. This is the fourth, and largest, flaring episode associated with this source ever observed by the LAT (see ATels #13931, #14422, #15126). The daily photon index is 2.0+/-0.1, smaller than the 4FGL average value of 2.2+/-0.1. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of PKS 0403-13 and OS 300 will continue. These sources are part of the "FSSC LAT Monitored Sources" and, consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PKS_0403-13 , and at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/OS_300 , respectively. PKS 0403-13 has also an entry in the FSSC light curve repository (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.php?source_name=4FGL_J0405.6-1308). We encourage multifrequency observations of both the gamma-ray sources. For PKS 0403-13 the Fermi LAT contact person is S. Ciprini (stefano.ciprini@ssdc.asi.it). For OS 300, the Fermi-LAT contact person is C.C. Cheung (teddy.cheung@nrl.navy.mil). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-12-28 04:59:00
radio,gamma ray,agn,blazar,quasar,request for observations
2021-12-28
04:59:00
3,454
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15,144
15,147
Optical follow-up of TXS 0403-132
Roberto Nesci (INAF/IAPS)
Following the announcement of a very high Gamma-ray flare of the blazar TXS 0403-132 (ATel #15146), I observed it with the 30cm telescope of the Foligno Observatory (MPC K56) and the R(Cousins) filter on 2021-12-29T20:53 UT: bad weather prevented observations closer to the Gamma-ray flare (December 25). Aperture photometry was performed with IRAF/apall, using as comparisons the surrounding stars of the GSC2.3 catalog. The source was detected at Fmag=16.78 +/-0.11, formally equal to the value reported in the catalog. For further check we measured the magnitude of the source using the stars of the PanSTARRS DR1 catalog obtaining rmag=16.91+/-0.09, similar to the catalog value (rmag=16.76). We remark that the two catalogs report magnitudes of the source taken at several years distance, which are rather similar: the offset between the GSC2.3 and the PanSTARRS DR1 magnitudes of the stars in the field of TXS 0403-132 is just 0.17 mag, GSC2.3 being brighter. Apparently therefore the Gamma-ray flare of the blazar TXS 0403-132 produced no corresponding enhancement in the optical band.
2021-12-30 07:51:00
optical,gamma ray,agn,blazar,star
2021-12-30
07:51:00
1,092
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15,145
15,148
NIR followup of the Blazar PKS 0735+178
L. Carrasco, E. Recillas, G. Escobedo, A. Porras, V. Chavushyan, Y. D. Mayya (INAOE, Mexico)
After the report by Fermi-LAT of a Gamma-ray flaring of the Blazar PKS 0735+178 (ATel #15129) and the observations in the Ks Band (ATel #15136), we observed the object in the NIR, on December 27th,2021 (JD 2459575.8069) and found that its fluxes corresponded to J = 13.53 +/- 0.07, H = 12.74 +/- 0.03 and Ks = 12.04 +/- 0.04. The latter is to be compared with the value Ks = 11.57 +/- 0.03 reported in ATel #15136, for December 16th, 2021. Clearly we are detecting the decay of the Gamma-ray flare. Our previous NIR photometry for this object (JD2459326.6632) is J = 14.28 +/- 0.07, H = 13.73 +/- 0.04 and Ks = 12.54 +/- 0.03. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics, and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.
2021-12-31 02:36:00
infra-red,gamma ray,agn,blazar,quasar,transient
2021-12-31
02:36:00
910
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0.010671621188521385, 0.03407706320285797, -0.020460419356822968, 0.013967234641313553, -0.03043575957417488, -0.09778037667274475, -0.027143394574522972, -0.01170892920345068, -0.011409640312194824, -0.10550402104854584, -0.009762715548276901, -0.056325413286685944, -0.06496720761060715, -0.04837614670395851, 0.03250967338681221, 0.00884376559406519, 0.029132774099707603, -0.007499488536268473, 0.06624860316514969, -0.06738749146461487, -0.11861485987901688, 0.02275434136390686 ]
15,146
15,149
Fermi-LAT detection of renewed gamma-ray activity from the FSRQ B2 2308+34
B. Rani (Korea Astronomy and Space Science Institute), J. Valverde (UMBC/NASA GSFC), G. La Mura (LIP), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar B2 2308+34 (R.A. = 347.7682 deg, Decl. = +34.4223 deg, J2000; z=1.817, Wills & Wills 1976, ApJS, 31,143), also known as 4FGL J2311.0+3425 (The Fermi-LAT collaboration 2020, ApJS, 247, 33). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on December 28, 30 and 31, 2021, with a consistent daily averaged gamma-ray flux (E>100MeV) of (1.1+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 14 relative to the average flux reported in the fourth Fermi-LAT source catalog data release 2 (4FGL-DR2; Ballet et al., arXiv:2005.11208). The corresponding photon index is 2.0+/-0.1, and is smaller than the 4FGL-DR2 value of 2.35+/-0.02. The GeV gamma-ray activity of B2 2308+34 was announced previously in 2013 and in 2010, by the Fermi LAT Collaboration (ATel#5477, ATel#2783). Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. The light curve for this source can be accessed via the Fermi-LAT Light-Curve Repository at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.php?source_name=4FGL_J2311.0+3425, and via the Fermi-LAT Monitored Sources at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/B2_2308p34. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Filippo D'Ammando (dammando@ira.inaf.it). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-01-02 09:49:00
radio,gamma ray,agn,blazar,quasar,request for observations
2022-01-02
09:49:00
1,957
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15,147
15,150
Bright radio emission from Nova Cassiopeiae 2021 = V1405 Cas
Kirill Sokolovsky, Elias Aydi, Laura Chomiuk, Adam Kawash, Jay Strader (MSU), Aliya-Nur Babul, Jennifer Sokoloski (Columbia), Amy Mioduszewski, Justin Linford (NRAO), Koji Mukai (NASA/GSFC), Kwan-Lok Li (NCKU), Tim O'Brien (JBCA/Manchester), Michael Rupen (NRC)
The classical nova V1405 Cas was discovered on 2021-03-18.4236 UT by Y. Nakamura (CBET #4945, ATel #14471, #14472, #14476, #14478, #14482, #14530, #14577, #14614, #14620, #14622, #14665, #14704, #14794). For seven month V1405 Cas stayed near its peak optical brightness showing a series of flares with the brightest one reaching V=5.1 according to the AAVSO photometry. Around 2021-11-01 the nova started a steady decline (ATel #15093) and on 2021-12-14 was detected as a super-soft X-ray source (ATel #15111). We follow V1405 Cas with the Karl G. Jansky Very Large Array (VLA) from 2021-06-10 (ATel #14731), prompted by the GeV detection of the nova (ATel #14658). V1405 Cas displays an inverted radio spectrum with flux densities gradually increasing with time at all frequencies, reaching at our latest observing epoch 2021-12-20: A power law fit results in a positively defined spectral index of 1.86 +/-0.02. The source is resolved at 31.1 and 34.9 GHz according to the SNR-adjusted resolution criterion of Kovalev et al. (2005, AJ, 130, 2473) having a Gaussian FWHM size of ~0.07 arcsec. The flux densities above 10 GHz were measured by fitting a circular Gaussian (at 31.1 and 34.9 GHz) or point source model to the uv-data and applying phase-only self-calibration. No self-calibration was applied at lower frequencies (due to more stable phases, fainter target and the presence of other sources within the field of view) - the flux densities were obtained from peaks of naturally-weighted CLEAN images of the nova. We used 3C147 to set the absolute flux density scale (Perley & Butler, 2017, ApJS, 230, 7) with expected uncertainties of 15% at 35 GHz and 5% at lower frequencies. The source J2339+6010 (TXS 2336+598) was used as the phase calibrator. From the 31.1 and 34.9 GHz data we measure the position of the radio emission peak (relative to the phase calibrator) at 23:24:47.7325 +61:11:14.599 J2000. The expected uncertainty is about 0.010 arcsec dominated by the phase calibration errors. The measured flux densities make V1405 Cas one of the brightest radio novae. Among the classical novae well observed in radio only V5668 Sgr (2015), V1369 Cen (2013), V1974 Cyg (1992) and QU Vul (1984) (Chomiuk et al., 2021, ApJS, 257, 49) as well as V959 Mon (2012) (Chomiuk et al. 2014, Nature, 514, 339) reached 100 mJy above 20 GHz (all having inverted spectra). The red giant donor recurrent nova RS Oph reached ~90 mJy at both high and low frequencies during its 2021 eruption (ATel #14886), while another embedded nova V407 Cyg peaked at lower flux densities (Chomiuk et al. 2012, ApJ, 761, 173).
2022-01-02 13:45:00
radio,millimeter,optical,x-ray,nova
2022-01-02
13:45:00
2,612
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15,148
15,151
Refining the period of the cyclic positions of a morphological structure in the inner coma of Comet C/2017 K2 (PanStarrs)
Federico Manzini (Stazione Astronomica di Sozzago), Paolo Ochner (Padova University), Virginio Oldani (Stazione Astronomica di Sozzago), Luigi R. Bedin (INAF-OAPd), Andrea Reguitti (UNAB; INAF-OAPd)
Comet C/2017 K2 (PanStarrs), coming from the Oort cloud, is approaching the Earth and the Sun towards perihelion that will occur on 20 December 2022 at 1.8 AU from the Sun. Following the observation of an asymmetrical coma and of two jet-shaped structures on the nucleus of the comet on 12 September 2020 with the INAF-OAPd 1.82-m Copernico telescope (Osservatorio Astrofisico di Asiago, Italy) (ATEL #14026), and of a cyclic angular movement of the south-east structure (ATEL #14813), we analyzed the publicly released images taken by the Hubble Space Telescope (PI David Jewitt) with the WFC3 camera (F350LP broadband filter) during two additional observation sessions on 24 March and 13 June 2021, for a total of eleven sessions. During the whole observation period, from 17 March 2018 to 13 June 2021, the comet's distance from the Sun decreased from 14.33 AU to 6.13 AU, and the resolution of the images increased from 417 to 164 km/pixel. All images were cleaned of cosmic rays and defects. Spatial filters (Larson-Sekanina with alpha = 30 - 45 deg, 1/rho, and division by azimuthal median) centered on the optocenter of the comet were then applied to highlight and confirm the presence of morphological structures in the inner coma. The inner coma was characterized during the entire 39-month period by the presence of two radial structures (probably dust emissions; Jewitt 2017) located roughly south-east and west of the nucleus (Fig. 1, 2). The first of the two structures was constantly well visible in the processed images of all the observing dates, therefore it was always possible to measure its position. The western jet-shaped structure showed a more variable intensity and on some dates it appeared almost faded. The measured position angles of the SE structure showed a cyclic oscillation between PA 105 deg and PA 190 deg, with respect to its origin on the nucleus, with an estimated period of 155.5 ± 10 days (R^2 = 0.803; Figure 3). Assuming that the SE structure is related to the presence of an active source on the cometary nucleus (Sekanina, 1987), if the observed oscillation of its position is not resulting from a precession of the spin axis, its estimated period could suggest a very slow rotation of the nucleus. In the hypothesis that the nucleus is spherical, the active area would be located at mid latitude. Furthermore, if the amplitude of the observed oscillation corresponds to the extreme positions assumed by the spin axis during the rotation of the nucleus, it would be oriented approximately towards PA 145 deg. Figures captions. Figures 1 and 2. The original HST images taken on 2021.03.24 and 2021.06.13, were stacked on the optocenter of the comet C/2017 K2. The stacks were treated with a 1/rho + LS algorithm (alpha = 30 deg). The PA of the south-eastern structure was measured as described in the text. Figure 3. Plot of the measured position angles (± standard deviation) of the south-east structure over the observation period. The red dotted line is the sinusoidal best fit, showing a period of 155.5 ± 10 days (R^2=0.803). Figures are available at: https://web.oapd.inaf.it/bedin/files/PAPERs_eMATERIALs/ATel/C2017K2_III/00_C2017_K2_ATEL_3_figures.pdf
2022-01-04 20:36:00
optical,comet,cosmic rays,the sun,variables
2022-01-04
20:36:00
3,208
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-0.09536013007164001, 0.08439970761537552, 0.08901668339967728, -6.186242273997777e-8, 0.10070834308862686, -0.028702832758426666, -0.05378472059965134, 0.05620267614722252, 0.01958037167787552, -0.04355911165475845, -0.006126292981207371, 0.039349425584077835, -0.024291440844535828, -0.017502816393971443, 0.01001801062375307, 0.05474966764450073, -0.0051018609665334225, -0.06643027812242508, -0.015823114663362503, 0.03813881427049637, -0.036792609840631485, -0.07035652548074722, -0.02475244365632534, 0.05166491121053696, 0.007339294534176588, -0.02287081815302372, 0.047086212784051895, -0.053446318954229355, -0.0033142182510346174, 0.046361908316612244, -0.01357229147106409, 0.1302134394645691, -0.04084986448287964, -0.08331028372049332, -0.07744188606739044, -0.02059154398739338, 0.01585305668413639, -0.1514597237110138, -0.03951244801282883, 0.03455859422683716, -0.07097979635000229, 0.027466878294944763, 0.06027774512767792, 0.0227105300873518, 0.0057228365913033485, 0.020033687353134155, 0.031028596684336662, 0.038054849952459335, 0.008874503895640373, 0.01581505686044693, 0.03661350533366203, -0.08247128129005432, -0.07949821650981903, -0.06578713655471802, -0.0792287215590477, -0.046466581523418427, -0.008758311159908772, -0.0628373771905899, -0.08318568766117096, 0.03031868301331997, -0.008946118876338005, -0.03546576201915741, -0.02863645739853382, 0.05136613920331001, 0.029038406908512115, -0.05415946617722511, -0.08134359121322632, 0.005214662756770849 ]
15,149
15,152
Recent outbursts from Cygnus X-3 observed with the Nasu telescope array at 1.4GHz
K. Tsubono (Univ. Tokyo), K. Asuma (Asaka High School), K. Niinuma (Yamaguchi Univ.), K. Takefuji (JAXA) and T. Daishido (Waseda Univ.)
We have reported the 2021 October outburst from Cyg X-3 observed with the Nasu telescope array at 1.4GHz (ATel #14989, #15018). The observed waveform of the light curve shows rather choppy behavior among those recently obtained from Cygnus X-3. We also detected a new outburst from 2021 December 25 UT (ATel #15142). The peak flux density was 6.3+-0.03 Jy on December 28 04:45 UT at 1.4GHz. The observed waveform of the light curve was more like a simple single pulse. Cygnus X-3 light curves at 1.4GHz observed from 2021 October 14 to 2022 January 4 can be seen here. Recent Swift/BAT data (15-50 keV; http://swift.gsfc.nasa.gov/results/transients/CygX-3/ ) would suggest that Cygnus X-3 is emerging from the quenched state. It will be interesting to see if this is the end of the deep and prolonged hypersoft/quenched state of Cygnus X-3. The Nasu telescope array is a spatial fast Fourier transform (FFT) interferometer consisting of eight linearly aligned antennas with 20 m spherical dishes. This type of interferometer was developed to survey transient radio sources with an angular resolution as high as that of a 160 m dish and a field of view as wide as that of a 20 m dish. Nasu telescope array HP: https://nasu-radio-telescope.space
2022-01-06 22:30:00
radio,binary,black hole,transient
2022-01-06
22:30:00
1,248
[ -0.07958395034074783, -0.03556996211409569, 0.06828546524047852, 0.011837940663099289, -0.046735282987356186, -0.09123631566762924, -0.0942806601524353, 0.04491578787565231, -0.0513053722679615, 0.018079428002238274, -0.006060929968953133, -0.07154260575771332, 0.014722480438649654, -0.0006402538274414837, 0.06357692927122116, -0.00440590875223279, 0.0219658762216568, -0.10329639911651611, 0.01225475873798132, -0.024317268282175064, -0.004060461185872555, 0.039190661162137985, -0.0313277430832386, 0.014111656695604324, 0.08367832005023956, 0.015142302960157394, 0.009013717994093895, -0.00891359243541956, 0.009572828188538551, 0.016489000990986824, 0.01817626878619194, 0.05337266996502876, -0.06940726190805435, 0.006754073780030012, 0.08751560747623444, -0.04434778168797493, 0.03191066160798073, -0.050220243632793427, 0.023503877222537994, -0.013189343735575676, 0.0005786425899714231, -0.005749661475419998, 0.004950100090354681, 0.017574578523635864, 0.033225346356630325, 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0.0864163339138031, -0.08147776871919632, 0.025200283154845238, 0.018048472702503204, 0.024878300726413727, 0.007405256852507591, 0.10015761107206345, -0.0730389729142189, -0.10535159707069397, 0.015072760172188282, 0.01568375900387764, -0.035735227167606354, 0.012473111040890217, 0.00034074074937961996, -0.06559281051158905, 0.11139332503080368, 0.012634425424039364, -0.06490631401538849, 0.0016487283864989877, -0.013724010437726974, -0.059330184012651443, 0.02402852661907673, -0.0937982052564621, 0.0015949079534038901, 0.050850868225097656, 0.05342917889356613, -0.009713087230920792, -0.03598202019929886, -0.007275845855474472, -0.092960424721241, 0.0681043416261673, -0.012836257927119732, -0.008560548536479473, 0.06286885589361191, 0.07040601968765259, 0.03311103954911232, -0.05161534994840622, -0.054289497435092926, -0.016413314267992973, -0.02443869225680828, 0.13924852013587952, 0.05686580389738083, 0.09616436064243317, -0.009919612668454647, 0.06085224449634552, 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0.0019162994576618075, -0.04913734272122383, 0.06443695724010468, 0.02932187356054783, -6.033437216501625e-8, 0.027292201295495033, 0.0036434426438063383, -0.08529550582170486, 0.032771699130535126, 0.0705609992146492, 0.0028505143709480762, -0.042341116815805435, -0.010052850469946861, 0.05607335641980171, 0.000314504315610975, 0.10373415052890778, -0.04864354804158211, 0.01937812939286232, -0.044024184346199036, -0.005376505199819803, -0.02407047338783741, -0.054473310708999634, -0.04130793735384941, -0.017026366665959358, 0.013741524890065193, -0.038526080548763275, 0.02810710296034813, -0.024807140231132507, -0.06141392141580582, 0.04561226814985275, 0.05982843413949013, -0.022510146722197533, 0.0970253124833107, -0.03505036607384682, -0.07366558909416199, -0.008541848510503769, -0.01079750619828701, 0.030235780403017998, -0.05266011506319046, -0.03985036164522171, 0.03275449201464653, -0.09779620915651321, 0.03201131895184517, 0.07635781168937683, 0.041632767766714096, -0.0388527475297451, -0.01957792043685913, 0.05488293990492821, 0.023396894335746765, -0.06047649681568146, 0.021100874990224838, -0.0007545819389633834, -0.1227114200592041, 0.0006785209407098591, -0.045584067702293396, -0.06555948406457901, -0.016005869954824448, 0.016183342784643173, -0.06197593733668327, -0.025685038417577744, 0.020000705495476723, -0.02896287851035595, -0.07184881716966629, -0.019433729350566864, 0.0007452665013261139, 0.05550764873623848, -0.08128023147583008, -0.08233790844678879, 0.07067184150218964 ]
15,150
15,153
Discovery of 11 ASAS-SN Supernova Candidates
J. Brimacombe (Coral Towers Observatory), B. Nicholls (Mt. Vernon Obs., New Zealand), I. Cruz (Cruz Observatory), A. Gabuya (Al Sadeem Observatory), P. Vallely, K. Z. Stanek, C. S. Kochanek, C. Christy, M. Rizzo Smith, S. Bose, T. A. Thompson (Ohio State), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), M. Stritzinger (Aarhus), P. Pearl (The Gap Observatory, BOSS), R. Cornect (Moondyne Observatory)
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm telescopes "Brutus" in Haleakala, Hawaii, "Leavitt" in Fort Davis, Texas, "Payne-Gaposchkin" in Sutherland, South Africa, and "Cassius" and "Paczynski" in Cerro Tololo, Chile, we discovered several transient sources. Their properties, as well as associated finding charts showing archival imaging (left) and follow-up confirmation (right) are included below: Follow-up observations are encouraged. While we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-21xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-21xx (AT 2021xyz) to preserve, rather than anonymize, the origin of the transient. We would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grants GBMF5490 and GBMF10501, and also funded in part by the Alfred P. Sloan Foundation grant G-2021-14192. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
2022-01-07 01:44:00
optical,supernovae,transient
2022-01-07
01:44:00
1,310
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15,151
15,154
Spectroscopic Classifications of AT2021zzv with Keck I + LRIS
K. W. Davis, S. Tinyanont, R. J. Foley (UCSC)
We report the following the classification of AT2021zzv from spectroscopic observations with the LRIS spectrograph on the Keck I telescope, made on 2022 Jan 5 UT. The target was supplied by the Young Supernova Experiment (YSE). The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy.
2022-01-07 05:56:00
optical,supernovae
2022-01-07
05:56:00
463
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0.07478500157594681, -0.046536289155483246, -0.06590265780687332, 0.0656144991517067, -5.085103182977946e-8, 0.08919890224933624, 0.0330028310418129, -0.020801514387130737, 0.020322686061263084, 0.05142432451248169, -0.007023971993476152, -0.005118140485137701, 0.08375047892332077, 0.009906881488859653, 0.02367480844259262, -0.0449371263384819, -0.06419570744037628, 0.057517971843481064, -0.06448319554328918, 0.0955786481499672, -0.02724391780793667, -0.0878433957695961, 0.01637912169098854, -0.040317654609680176, 0.07808513194322586, 0.05006950721144676, 0.07069888710975647, 0.04710240289568901, -0.05545216426253319, -0.051197655498981476, -0.028311384841799736, 0.002337666228413582, 0.1347600519657135, 0.05472978949546814, -0.058939721435308456, -0.012940875254571438, -0.007783565670251846, -0.08789265900850296, -0.017212415114045143, -0.0389288067817688, 0.03558667004108429, -0.09699560701847076, 0.008843300864100456, 0.0986606776714325, 0.06157374009490013, -0.06086425110697746, -0.057109225541353226, -0.013184839859604836, 0.05911952257156372, -0.10655348002910614, -0.017108125612139702, -0.018069785088300705, -0.0719190463423729, 0.01640212908387184, 0.05852986499667168, -0.05084272846579552, 0.010224494151771069, -0.05125106871128082, -0.051423292607069016, -0.08697757869958878, -0.0004321282613091171, -0.017535187304019928, -0.0195234976708889, -0.018555160611867905, 0.0229166429489851, 0.1258343756198883, -0.02676011435687542, -0.09756241738796234, -0.026754530146718025 ]
15,152
15,155
Classification of Gaia Alerted QSO candidates
M. Dennefeld (IAP-Paris and Sorbonne University), T. Pursimo (NOT-LaPalma)
We present further classifications of Gaia Alerted (Hodgkin et al. 2021, A&A, 652, 76) QSO candidates, as described in ATel 15138. Spectra were obtained with ALFOSC at the Nordic Optical Telescope at a resolution of ~300. All lines mentioned are in emission.
2022-01-10 23:15:00
optical,quasar
2022-01-10
23:15:00
258
[ -0.08173099160194397, -0.046497736126184464, -0.07605805993080139, 0.019553031772375107, 0.04413712024688721, -0.04190388321876526, 0.04193504899740219, -0.05675823986530304, 0.0518362857401371, 0.010309567674994469, 0.031218092888593674, -0.10222233831882477, -0.02280023880302906, -0.0068159862421453, 0.008184847421944141, 0.03717672824859619, 0.040706198662519455, -0.16584239900112152, 0.08198665827512741, 0.02968435175716877, 0.02957664057612419, 0.059062693268060684, -0.06152815371751785, 0.021423256024718285, 0.018031980842351913, -0.000130560714751482, 0.03016401082277298, 0.0026107137091457844, -0.013629917986690998, -0.023097729310393333, -0.008517704904079437, 0.0780591368675232, 0.029513023793697357, -0.007383595686405897, 0.014613034203648567, -0.039169471710920334, 0.0492117777466774, -0.11050119251012802, -0.0022231540642678738, 0.015688098967075348, -0.019284097477793694, -0.0957794263958931, -0.011601298116147518, -0.06258662790060043, -0.03593031316995621, -0.03810124844312668, -0.031264498829841614, -0.049557339400053024, -0.0702052041888237, -0.038568202406167984, 0.011600237339735031, -0.06376128643751144, -0.05319814756512642, 0.013447058387100697, 0.024966148659586906, -0.035349227488040924, -0.0836973488330841, -0.09623976796865463, 0.03134504705667496, 0.04771583154797554, 0.008797349408268929, -0.02117091976106167, -0.03160446509718895, 0.012416466139256954, -0.011049550026655197, 0.030323754996061325, -0.04517809674143791, -0.10679817199707031, 0.036349330097436905, -0.028738539665937424, -0.061048198491334915, -0.018165796995162964, 0.03773573786020279, -0.01924383081495762, 0.0414884015917778, 0.13283583521842957, 0.043370623141527176, 0.007374697830528021, -0.0014343414222821593, -0.06432881206274033, 0.005166730843484402, -0.00006285365088842809, -0.03050854615867138, 0.02919408492743969, 0.05015408247709274, 0.025731276720762253, -0.05467255041003227, 0.04680671915411949, -0.047039903700351715, -0.001205311855301261, 0.06896225363016129, -0.09794889390468597, -0.021328475326299667, -0.03790721669793129, -0.014512681402266026, 0.02106703259050846, 0.03908563405275345, -0.06200067698955536, 0.047620564699172974, -0.003734861733391881, 0.04996936768293381, -0.0062227617017924786, -0.059765271842479706, 0.04695311188697815, -0.09433510899543762, 0.00020347935787867755, 0.027144823223352432, 0.053903210908174515, 0.0020592722576111555, -0.01483133900910616, -0.07224109768867493, 0.0011285888031125069, -0.029622459784150124, -0.07936067879199982, -0.08016033470630646, 0.06716518104076385, -0.0018989930395036936, 0.10746490210294724, -0.04839704930782318, 0.04291912168264389, 0.05919565632939339, -0.03742020204663277, -0.04543319717049599, 0.08227662742137909, 0.13498570024967194, 0.07558867335319519, -0.09851743280887604, 2.444403952007476e-33, 0.06885053962469101, 0.04782293364405632, -0.00439381692558527, -0.010588387958705425, -0.02222440391778946, 0.07700611650943756, -0.03873622044920921, -0.0321076363325119, -0.05610262230038643, -0.028265206143260002, -0.052219655364751816, 0.10880101472139359, -0.007331985980272293, -0.029102515429258347, 0.033056557178497314, 0.12330421805381775, -0.03457055240869522, -0.02127990499138832, -0.02637743577361107, 0.01093087438493967, -0.011724459938704967, -0.0025183733087033033, -0.03490487113595009, 0.008110089227557182, 0.07192303240299225, 0.0794566422700882, 0.02478807047009468, -0.015431405045092106, -0.06410881131887436, 0.03333640471100807, 0.047419894486665726, -0.0064718881621956825, 0.0347466915845871, -0.021439706906676292, -0.010360502637922764, -0.051849037408828735, -0.08101287484169006, 0.005105441901832819, -0.030498769134283066, -0.08455052971839905, 0.03919350355863571, 0.04403793439269066, -0.029573779553174973, 0.026424633339047432, -0.007258124183863401, -0.0004866436356678605, -0.0497620590031147, 0.029765194281935692, 0.12994267046451569, -0.020941082388162613, -0.00048440665705129504, -0.0608363077044487, -0.06842596083879471, 0.06394757330417633, 0.02720426581799984, 0.06471806019544601, 0.02092777006328106, 0.016451193019747734, -0.028213413432240486, -0.06393413245677948, -0.001968638738617301, 0.04013873264193535, 0.0997098982334137, -0.052252378314733505, -0.006948757451027632, 0.053093258291482925, 0.01739189401268959, 0.007552172057330608, -0.038534652441740036, 0.14080139994621277, -0.008096217177808285, 0.04375964403152466, 0.07108571380376816, 0.005716552957892418, -0.007082048337906599, -0.05860146880149841, 0.03766345977783203, 0.011783949099481106, 0.009929021820425987, 0.06410621851682663, -0.0610128752887249, -0.03612971678376198, 0.061118993908166885, 0.004137064330279827, -0.05309055373072624, -0.00815843790769577, -0.024294259026646614, 0.0028297866228967905, -0.03827638179063797, 0.007257419638335705, 0.04571021720767021, 0.06038101762533188, -0.02933146245777607, 0.010205036029219627, -0.14116550981998444, -3.052181918498616e-33, 0.08229850977659225, -0.0036996204871684313, 0.0013582940446212888, -0.03966876491904259, -0.08461526036262512, -0.0189178679138422, -0.030036266893148422, 0.009399253875017166, -0.016414182260632515, 0.035116806626319885, 0.09724298119544983, 0.08207433670759201, 0.02397785522043705, -0.010789286345243454, -0.02121691033244133, -0.04093023017048836, 0.026226188987493515, -0.04413539916276932, 0.04716642573475838, -0.005035810638219118, -0.011161603033542633, -0.03392701596021652, 0.07110898196697235, -0.1406414657831192, 0.01864931359887123, -0.013518053106963634, 0.04154285043478012, -0.057564735412597656, -0.10037994384765625, -0.024106061086058617, -0.09736935049295425, -0.05052193999290466, -0.006303438451141119, -0.01261280756443739, 0.02001899853348732, -0.012302890419960022, 0.08421297371387482, 0.014926528558135033, -0.06195883825421333, -0.017714042216539383, -0.056166838854551315, 0.08917475491762161, 0.07248550653457642, 0.006185145117342472, -0.01763726957142353, -0.021667884662747383, 0.05383029952645302, 0.06587536633014679, -0.05493266507983208, -0.046651776880025864, 0.05423278734087944, 0.030853083357214928, -0.02048497647047043, 0.09844958037137985, 0.04548623412847519, 0.058817822486162186, -0.005169127602130175, 0.011360685341060162, -0.05551711842417717, 0.008426055312156677, 0.015452433377504349, -0.033927712589502335, -0.07785666733980179, -0.027890024706721306, 0.060117460787296295, 0.05637079477310181, 0.029490215703845024, 0.05956582725048065, 0.014168326742947102, 0.0426359660923481, 0.08982092142105103, -0.05859198048710823, -0.09492690116167068, 0.07504930347204208, 0.048854079097509384, 0.032144926488399506, -0.06148140877485275, -0.05987082049250603, -0.021702539175748825, -0.030426690354943275, 0.009816940873861313, -0.007044741418212652, -0.0454242005944252, 0.054264266043901443, 0.04967976361513138, 0.041537199169397354, 0.00833737663924694, 0.010833446867763996, 0.06875795125961304, 0.023706814274191856, -0.007857944816350937, 0.10030186921358109, 0.038949526846408844, -0.03542231395840645, 0.028701603412628174, -4.2647982922972005e-8, -0.01847728155553341, -0.021784545853734016, -0.03253885731101036, -0.038788553327322006, 0.04944508895277977, -0.06807995587587357, 0.017612531781196594, 0.02615858055651188, -0.009168815799057484, -0.0013192167971283197, -0.0014549554325640202, -0.02639090083539486, 0.02240729331970215, -0.01336843241006136, 0.11713806539773941, -0.04750467836856842, -0.008480716496706009, -0.005854798946529627, -0.006307505536824465, 0.04522967338562012, 0.08704960346221924, 0.03802355378866196, 0.004690457601100206, -0.05260944738984108, 0.0029524746350944042, 0.0012732173781841993, 0.052393458783626556, 0.033780548721551895, -0.05008211359381676, -0.014615916647017002, -0.02034739777445793, -0.056815214455127716, 0.018972955644130707, -0.007205527275800705, -0.03243737295269966, 0.054737165570259094, -0.0636385828256607, -0.04389447346329689, 0.01066964864730835, 0.0829504132270813, -0.023410817608237267, 0.003435503225773573, -0.05316278710961342, 0.0028274650685489178, -0.022577708587050438, 0.11181072145700455, -0.007455496117472649, -0.11647098511457443, 0.028140801936388016, 0.04788268730044365, -0.014785071834921837, -0.057399481534957886, 0.05360348895192146, -0.03318381682038307, -0.09462077915668488, -0.05299215018749237, 0.10081949084997177, -0.028902601450681686, 0.014529149048030376, 0.030869556590914726, 0.1119849905371666, 0.005694749765098095, -0.060390230268239975, 0.012442833743989468 ]
15,153
15,156
Spectroscopic classification of ZTF transients
Stephanie Figuereo, Kevin McKinnon, Rafael Nunez, Stefan Kimura, Puragra Guhathakurta (UCSC), Monika Soraisam (NOIRLab), Chien-Hsiu Lee (NOIRLab)
We report the spectroscopic classification of the following transients from the SALVATION project (ATel #13952). They were flagged from the ZTF public alert stream by the ANTARES alert-broker. The spectra were obtained on 2021 December 03 UT for ZTF21acmrdga and 2021 December 04 UT for ZTF21acjniho, ZTF21acourni, and ZTF21acpfduf with the Kast double spectrograph on the Shane 3-m telescope at Lick Observatory.
2022-01-11 06:53:00
optical,supernovae,transient
2022-01-11
06:53:00
413
[ -0.06190595403313637, -0.050586339086294174, -0.031357888132333755, 0.04147738963365555, 0.034460123628377914, -0.03928130865097046, -0.03419859707355499, 0.013431725092232227, 0.011988942511379719, -0.014385265298187733, 0.012814202345907688, -0.09175673127174377, 0.04536795988678932, 0.01968967914581299, 0.0275509562343359, -0.05715436488389969, 0.018720904365181923, -0.07886459678411484, 0.024815287441015244, 0.04801251366734505, -0.018352655693888664, 0.06012371554970741, -0.0025022721383720636, -0.0014176196418702602, 0.06625453382730484, -0.00440192362293601, -0.0905371904373169, -0.0414721742272377, 0.08107414096593857, -0.010939381085336208, 0.006459998432546854, 0.10855818539857864, -0.09100084006786346, 0.0184615645557642, 0.0972653180360794, -0.05239526554942131, 0.048782214522361755, -0.01089297141879797, 0.021165402606129646, 0.005737162660807371, 0.04093065857887268, -0.03940653055906296, -0.053496602922677994, -0.05708308890461922, -0.028984352946281433, 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15,154
15,157
MeerKAT detects radio emission from 4U 1543-47 that is consistent with a black hole hard state
Xian Zhang, Wenfei Yu (Shanghai Astronomical Observatory), Rob Fender (University of Oxford), Patrick Woudt (University of Cape Town), James Miller-Jones (Curtin University), Sara Motta (INAF-OAB & University of Oxford), on behalf of the ThunderKAT collaboration
4U 1543-47, a transient black hole X-ray binary, was found in a new X-ray outburst by MAXI/GSC on June 11, 2021 (ATel #14701). After a probable hard-to-soft spectral state transition on the same day, the source had been residing in the soft spectral state (ATel #14701, #14708, #14725, #14749). As part of the ThunderKAT Large Survey Programme (Fender et al. 2017, arXiv:1711.04132), which targets on X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts, we have monitored the black hole transient 4U 1543-47 under the X-ray binary monitoring programme with MeerKAT on ~ weekly cadence since June 19, 8 days after the starting of the X-ray outburst. In each run of the monitoring observations, J1939-6342 was firstly observed, which has been used as the bandpass and absolute flux calibrator. J1501-3918, the phase calibrator, was observed before and after each of the ~ 15 min exposure on 4U 1543-47. Variations in the radio emission from the source were detected (e.g., ATel #14878), but none can be associated with the emission from a compact jet based on X-ray and radio observations. On January 3, 2022, we detected a radio component with the flux density of 0.24 +/- 0.02 mJy with radio in-band spectral index of 0.28 +/- 0.49. The position of the component is consistent with the Gaia optical position of 4U 1543-47. The hardness ratio obtained with MAXI/GSC (4-10 keV flux over 2-4 keV flux) increased significantly on December 28, 2021. Since then has remained increasing. Based on the radio and X-ray observations, we suggest 4U 1543-47 has transitioned to the hard state and the radio emission is from a compact jet. We encourage multi-wavelength observations to follow up the black hole hard state. ThunderKAT will run for 5 years and targets X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts. As part of this programme we perform weekly monitoring observations of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt. We thank Evangelia Tremou, Joe Bright, Andrew Hughes in the ThunderKAT collaboration for scheduling the observing blocks and the staff at the South African Radio Astronomy Observatory (SARAO) for their rapid scheduling of these observations. The MeerKAT telescope is operated by SARAO, which is a facility of the National Research Foundation, an agency of the Department of Science and Technology. We also thank RIKEN, JAXA and the MAXI team for making the MAXI/GSC data available.
2022-01-11 10:00:00
radio,optical,x-ray,gamma ray,binary,black hole,cataclysmic variable,gamma-ray burst,supernovae,transient,variables
2022-01-11
10:00:00
2,565
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-0.03996353596448898, -0.006260368507355452, 0.022245235741138458, -0.1133015975356102, 0.035513389855623245, -0.11155413836240768, -0.10067426413297653, 0.013633068650960922, 0.040325816720724106, 0.002272674348205328, -0.03807411342859268, 0.017229242250323296, -0.08432888239622116, 0.0010332120582461357, 0.013651658780872822, -0.014954494312405586, -0.05269022285938263, 0.0050207460299134254, -0.020083850249648094, 0.08403662592172623, -0.10375212132930756, -0.08954308182001114, -0.012460780330002308 ]
15,155
15,158
GEMINI/GMOS-N spectroscopic classification of Gaia microlensing event candidates
Gezer I., Zielinski P., Wyrzykowski L., Gromadzki M., Kruszynska K., Rybicki K. A., Ihanec N. (Warsaw University Astronomical Observatory, Poland), Zdanavicius J., Maskoliunas M., Pakstiene E. (Institute of Theoretical Physics and Astronomy, Vilnius University, Lithuania), Hodgkin S. (Institute of Astronomy, University of Cambridge)
We report on spectroscopic observations of 6 candidates for microlensing events detected by the Gaia Science Alerts program (http://gsaweb.ast.cam.ac.uk/alerts). We have obtained Gemini/GMOS long-slit spectra (GMOS; Hook et al. 2002) for 6 objects with R400 gratings which provides resolution power of R ~ 2000 and covers the wavelength range from 400 to 900 nm. The spectra are available on IAU's Transient Name Server. Notes: (1) D Na I and weak TiO bands are clearly distinguishable, continuum shape suggests that late-type star showing emission in Halpha line, very likely TTauri star . (2) showing strong molecular absorptions, M-type supergiant, very likely Mira varaibale. (3) it is A/F (or even reddened B) type-star, hydrogen absorption are strong including Paschen series, likely Be star. (4) spectra shows weak hydrogen absoption lines with molecular bands, M-type star/ULENS . (5) strong emission in Halpha, the continuum shape suggest that it is an early type star, very likely Be star. (6) D Na I and TiO bands are visible, continuum shape suggests that it is a late-type star showing emission in Halpha line, very likely TTauri star. Acknowledgments. This project has received funding from the EU Horizon 2020 research and innovation programme under grant agreement No. No 101004719, as well as Polish NCN DAINA grant 2017/27/L/ST9/03221 and Research Council of Lithuania grant No. S-LL-19-2. We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts).
2022-01-11 16:03:00
optical,microlensing event,star,transient,variables
2022-01-11
16:03:00
1,518
[ -0.06619343161582947, -0.02256491407752037, -0.013183251954615116, 0.006432820577174425, 0.01807655207812786, -0.07308164983987808, 0.0737743228673935, -0.04727001115679741, -0.017729587852954865, 0.04702567681670189, -0.062435418367385864, 0.004198530688881874, -0.04633772373199463, 0.01706024631857872, 0.07787277549505234, -0.04256550967693329, 0.062352534383535385, -0.10029041022062302, -0.05186278373003006, 0.07020781189203262, 0.0448434017598629, -0.02019197680056095, -0.08560080826282501, 0.03914113715291023, 0.007108745630830526, -0.032631512731313705, 0.030565161257982254, -0.1014101430773735, -0.003781673265621066, -0.013805803842842579, -0.003611398860812187, 0.10686604678630829, 0.0055530923418700695, 0.036956992000341415, 0.07950487732887268, -0.009565204381942749, 0.045127060264348984, -0.02622842788696289, 0.015379024669528008, -0.0239877887070179, 0.03141433373093605, -0.03454022482037544, 0.004162145312875509, -0.03210325539112091, -0.03356887772679329, 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-0.023845883086323738, -0.0009186548413708806, -0.04140837490558624, 0.05842055380344391, -0.042380210012197495, -0.042699024081230164, 0.02328653633594513, -0.03142823651432991, -0.07950350642204285, 0.07965646684169769, 0.046087946742773056, -0.009323691949248314, -0.0475023090839386, -0.03824993222951889, -0.06935335695743561, 0.05585974454879761, -0.006233118940144777, 0.036936432123184204, -0.03952762857079506, 0.00864342786371708, -0.04511637985706329, -0.04165332391858101, -0.05671197548508644, -0.01372851338237524, -0.06326532363891602, 0.04428771883249283, 0.000023808557671145536, -0.09127569198608398, -0.02981124073266983, -0.04973563179373741, 0.018135860562324524, 0.02510899305343628, 0.04719400778412819, 0.057537741959095, -0.030614977702498436, 0.02939104288816452, 0.030176764354109764, -0.09774856269359589, -0.06962232291698456, -0.027922870591282845, 0.08055909723043442, 0.0027264622040092945, 0.047027990221977234, -0.03253539279103279, 0.024754459038376808, 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15,156
15,159
The Changing Light Curve of [MA93]1640 (XMMU J010743.1-715953)
P. C. Schmidtke (Arizona State University), A. P. Cowley (Arizona State University), A. Udalski (Warsaw University Observatory)
Emission-line star [MA93]1640 is the optical counterpart of XMMU J010743.1-715953, an X-ray source that shows evidence of weak pulsations with P=153 s and has a hard spectrum typical of Be/X-ray binaries (Coe et al., 2012, MNRAS, 424, 282). The visible star is classified as type B2IV-Ve, with a variable Halpha line profile. The OGLE-III light curve has long-term brightness changes (I=16.95 to 16.45) that are superimposed by numerous sharp dips and spikes. These rapid fluctuations are most prominent when the source is faint. Coe et al. identified a possible periodicity at P=100.3 d. A light curve folded on this period (see Fig. 15 of Coe et al.) reveals a narrow dip that precedes a rapid rise to maximum light. We have analyzed 10 years (2010-2020) of OGLE-IV observations, which are shown in the top panel of the accompanying figure. The pattern of dips/spikes and the general brightening present at the end of OGLE-III continued during OGLE-IV seasons 1-2, with the star reaching I=15.8 near JD 2456100. Thereafter, the character of these variations changed substantially. As the overall system brightness declined to I=16.5 during seasons 3-5 and then rose in seasons 6-10, the fluctuations were replaced with lower-amplitude variations. To facilitate the study of this change in optical behavior, long-term trends in the observations were removed by subtracting a second-order polynomial from each season of OGLE-IV data. We refer to these detrended values as I* magnitudes. PDM analysis of I* data from seasons 1 and 2 of OGLE-IV reveals a signal at P=103.1+/-0.5 d, close to the period reported for OGLE-III observations. A plot of the folded light curve is shown in the figure, where phase zero corresponds to maximum light. Comparison of this plot with that presented by Coe et al. shows the dip that precedes maximum light has become shallower and broader. Furthermore, the peak, which is less pronounced in OGLE-IV data than in OGLE-III, is followed by large scatter at phase 0.2. The highest points near this phase were taken JD 2455445-2455459 and are readily visible in the raw light curve. The presence of this secondary brightening is difficult to reconcile with an orbital interpretation of the 103-d periodicity. To study the character of variations after JD 2456100, we calculated a periodogram of I* data from OGLE-IV seasons 3-10. As shown in the accompanying figure, the highest peak occurs at P=51.44 d, but aliases close to 0.5 and 1.0 d have nearly the same power. When folded on each trial period, the light curve is a low-amplitude sinusoid. We note the 51.44-d period is approximately half that of the 100-103 d periodicity present when the star was more active. Evidence for an orbital signature in seasons 3-10 of OGLE-IV data is weak, and the observed signal is most likely caused by nonradial pulsations (NRPs) of the star. The light curves of the 0.5 and 1.0-d aliases have shapes and amplitudes that are consistent with this interpretation, but we cannot distinguish between them using the available observations. As an example, the OGLE-IV I* light curve folded on the best-fit sine wave at P=1.0170 d is shown in the bottom panel of the figure. The apparent strength of the 51-d signal in the periodogram is likely an artifact of data sampling, detrending errors, changes in NRP amplitude, or variations in period of the NRPs. Schmidtke et al. ( 2013, MNRAS, 431, 252) demonstrated that small changes in NRP period have the effect of shifting power to a long-period alias.
2022-01-12 00:45:00
optical,x-ray,binary,star,variables
2022-01-12
00:45:00
3,518
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15,157
15,160
Radio detection of the tidal disruption event AT2021yte
Adelle J. Goodwin (ICRAR - Curtin), James C. A. Miller-Jones (ICRAR - Curtin), Kate D. Alexander (Northwestern U.), and Sjoert van Velzen (Leiden U.), on behalf of a larger collaboration
We report new radio observations of the tidal disruption event (TDE) AT2021yte taken as part of our VLA Large Program dedicated to TDEs. AT2021yte was first discovered as ZTF21acafvhf on 2021 September 12, an optical flare from the host galaxy SDSS J065504.74+123802.8 (TNS Astronomical Transient Report No. 123252 by ALeRCE). It was later classified as a TDE with broad hydrogen and He II emission lines at a redshift of z=0.053 by ZTF (TNS Classification Report No. 11136). We observed AT2021yte with NSF's Karl G. Jansky Very Large Array (VLA), on 2021 December 21 UT. The data were reduced in CASA using standard procedures. We detected radio emission consistent with the optical position, with a flux density of 184+/-4 uJy at 15 GHz. Further radio observations to constrain the broadband spectrum of the source have been scheduled with the VLA. We encourage additional multi-wavelength follow up of this interesting source. Our VLA Large Program (20B-377) began in December 2020 and will continue until 2023. We plan to target new publicly-reported TDEs discovered at z < 0.1, to determine the prevalence of radio emission in TDEs. We will report new results from this program to the community via ATels, TNS AstroNotes, and on our program website (https://sites.northwestern.edu/radiotdes/). For collaboration, or to suggest new targets, please contact the program PI (Kate Alexander, kate.alexander@northwestern.edu) or one of the program co-Is.
2022-01-12 10:52:00
radio,optical,tidal disruption event,transient
2022-01-12
10:52:00
1,455
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-0.02553209476172924, 0.011403990909457207, -0.02092018723487854, 0.009640988893806934, -0.0336311049759388, 0.0462011881172657, -0.008625579997897148, 0.0009061915334314108, 0.00437174690887332, -0.0387573167681694, -0.02591414377093315, -0.06115376576781273, -0.03787682577967644, -0.10510706156492233, -0.06197695806622505, -0.03931792080402374, -0.048177726566791534, -0.012428661808371544, -0.0017383256927132607, 0.019394582137465477, 0.08935923129320145, -0.038242124021053314, -0.07932045310735703, 0.025105997920036316 ]
15,158
15,161
First detection of very-high-energy gamma-ray emission from PKS1413+135 with the MAGIC telescopes
Oscar Blanch (Institut de Fisica d'Altes Energies, IFAE-BIST), Julian Sitarek (University of Lodz), Jelena Striskovic (University of Osijek) on behalf of the MAGIC collaboration
The MAGIC Collaboration reports the first detection of very-high-energy (VHE; E>100 GeV) gamma-ray emission from PKS1413+135 (14 15 58.82 +13 20 23.71, J2000.0). The preliminary analysis of the MAGIC data taken on 2022/01/12 resulted in the detection of PKS1413+135 with a statistical significance more than 5 standard deviations, and indicates a flux of about 15% of the flux from the Crab nebula above 150 GeV. PKS1413+135 is a blazar located at redshift estimated in the range of 0.247-0.5 (Readhead et al 2021). It is most likely located behind a Seyfert galaxy that is possibly creating millilensing effects (Peirson et al. 2022). The MAGIC observations were motivated by the enhanced GeV flux derived with a dedicated analysis pipeline on Fermi-LAT data from blazars. MAGIC observations on PKS1413+135 will continue during the next days, multiwavelength observations are encouraged. The MAGIC contact persons for these observations are O. Blanch (blanch@ifae.es) and J. Sitarek (jsitarek@uni.lodz.pl) The preliminary analysis has been performed by the Flare Advocate Jelena Striskovic (jelena.striskovic@gmail.com). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
2022-01-13 05:05:00
gamma ray,tev,vhe,blazar
2022-01-13
05:05:00
1,349
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15,159
15,162
Fermi-GBM Observations of Recent Bursting Activity from SGR J1935+2154
Oliver J. Roberts (USRA/NASA-MSFC) on behalf of the Fermi-GBM Team
Fermi-GBM has triggered on 30 bursts from the direction of SGR J1935+2154 since December 24th 2021, some of which may have been misclassified as GRBs. This list at the time of writing (including the most recent one) is: Date and Time in UTC   Fermi MET (s) 2022-01-12T19:58:04.04   663710289 2022-01-12T17:57:08.52   663703033 2022-01-12T08:39:25.34   663669570 2022-01-12T05:42:51.54   663658976 2022-01-12T04:31:20.07   663654685 2022-01-12T02:19:22.23   663646767 2022-01-12T02:05:58.27  663645963 2022-01-12T01:03:46.83   663642231 2022-01-11T21:54:01.18   663630846 2022-01-11T18:21:07.76   663618072 2022-01-11T17:05:55.66   663613560 2022-01-11T08:58:35.36   663584320 2022-01-11T07:48:21.49   663580106 2022-01-11T05:42:12.27   663572537 2022-01-10T15:55:38.32   663522943 2022-01-10T04:31:43.13   663481908 2022-01-10T02:57:16.80   663476241 2022-01-09T12:57:21.98   663425846 2022-01-09T09:28:12.79   663413297 2022-01-09T07:39:10.69   663406755 2022-01-09T04:57:16.14   663397041 2022-01-08T14:41:46.89   663345711 2022-01-06T02:36:14.05   663129379 2022-01-05T07:06:40.74   663059205 2022-01-05T06:01:31.43   663055296 2022-01-04T04:32:11.17   662963536 2021-12-29T16:41:26.20   662488891 2021-12-26T12:55:09.72   662216114 2021-12-25T22:22:20.14   662163745 2021-12-24T03:42:34.36   662010159 Fermi-GBM will not report on future triggers from this source during its current outbursting phase. We encourage multi-wavelength observations to follow-up this most recent activation. For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/”
2022-01-13 06:33:00
x-ray,gamma ray,gamma-ray burst,magnetar,neutron star,soft gamma-ray repeater,star
2022-01-13
06:33:00
1,621
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15,160
15,163
Fermi LAT detection of renewed GeV gamma-ray activity of PKS 1413+135
Federica Giacchino (INFN Roma Tor Vergata, & ASI Space Science Data Center, Roma, Italy), Stefano Ciprini (INFN Roma Tor Vergata, & ASI Space Science Data Center, Roma, Italy), on behalf of the the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed gamma-ray flaring activity from a source positionally consistent with the blazar PKS 1413+135, also known as OQ 122 and 4FGL J1416.1+1320 (Abdollahi, et al. 2020, ApJS, 247, 33), with radio coordinates R.A. = 213.9951 deg, Decl. = +=13.3399 deg (J2000; Johnston et al. 1995, AJ, 110, 880), and redshift z=0.24671+/-0.00001 (Wiklind & Combes 1997, A&A, 328, 48). Initially classified as a BL Lac, it might also be a young radio source (Perlman et al. 1996 AJ, 111, 1839; Gugliucci et al. 2005 ApJ, 622, 136). Preliminary analysis indicates that PKS 1413+135 was in an elevated gamma-ray emission state during the past days, reaching daily averaged gamma-ray fluxes (E>100MeV) of (2.2+/-0.7) X 10^-7 photons cm^-2 s^-1 and (2.0+/-0.6) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only) respectively on January 11 and January 12, 2022. These correspond to a flux increase of a factor of about 20 with respect to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon indices are 1.7+/-0.2 for each day, significantly smaller than the 4FGL value of 2.41+/-0.07. This hard-spectrum state was accompanied by the detection of several photons with probability >99% of having been emitted by the target source. The highest energy photon was observed on 11 January 2022, with an energy of about 25 GeV. This is the second time that the Fermi LAT Collaboration has reported enhanced gamma-ray activity from PKS 1413+135 (ATel#13049). The MAGIC Cherenkov telescopes have recently reported the first detection of VHE gamma-ray emission above 150 GeV from this object (ATel#15161). Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of PKS 1413+135 will continue. This source is part of the "FSSC LAT Monitored Sources" and, consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT is publicly available at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PKS_1413p135. This source has also an entry in the FSSC light curve repository (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.php?source_name=4FGL_J1416.1+1320). We encourage multifrequency observations of this gamma-ray source. For this source, the Fermi-LAT contact persons are F. Giacchino (federica.giacchino@roma2.infn.it) and C.C. Cheung (teddy.cheung@nrl.navy.mil). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-01-14 06:06:00
radio,gamma ray,vhe,agn,blazar,quasar,request for observations
2022-01-14
06:06:00
2,761
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-0.035597123205661774, 0.02916388213634491, 0.04668426513671875, -0.08421894162893295, 0.03205882012844086, -0.07672545313835144, -0.10294284671545029, 0.04201032221317291, -0.0059708040207624435, -0.03636836260557175, -0.013521947897970676, 0.016308102756738663, -0.09659630060195923, -0.07408998906612396, -0.0029780620243400335, 0.00823977217078209, -0.009175911545753479, -0.01594456285238266, -0.030669549480080605, -0.007909953594207764, -0.03872865065932274, -0.04980460926890373, -0.009663697332143784 ]
15,161
15,164
SGR/eROSITA non-detection of the tidal disruption event AT2021yte
Zhu Liu, Arne Rau, Adam Malyali, Andrea Merloni (all MPE)
We report the non-detection from SGR/eROSITA (Predehl et al. A&A 647, A1, 2021) of the tidal disruption event (TDE) AT2021yte. AT2021yte was first reported as ZTF21acafvhf on 2021 September 12 (TNS Astronomical Transient Report No. 123252 by ALeRCE), and spectroscopically classified as a TDE at a redshift of z=0.053 (TNS Classification Report No. 11136). The source is also detected in radio band by VLA (Adelle et al., ATEL #15160) on 2021 December 21. AT2021yte was in the Field-of-View of eROSITA during the fourth consecutive all-sky survey (eRASS4) on 2021 October 13, but the source was not detected (total exposure time of ~211s). Assuming an absorbed blackbody model, with temperature fixed at 80 eV and the equivalent neutral hydrogen column density fixed to N_H=1.9x10^21 cm^-2 (HI4PI Collaboration, N. Ben Bekhti, et al., 2016, A&A 594, A116), we derived a 3 (1) sigma upper limit of 1.0E-13 (3.0E-14) erg/s/cm^2 for the observed flux in the 0.2-2.3 keV energy band.
2022-01-15 00:55:00
radio,x-ray,tidal disruption event,transient
2022-01-15
00:55:00
980
[ -0.031217588111758232, -0.03481603413820267, 0.009385078214108944, 0.014584432356059551, 0.09802588820457458, -0.04905103147029877, -0.03145195171236992, 0.04131322354078293, 0.03322736173868179, 0.0026106478180736303, 0.0014055899810045958, -0.07724364846944809, 0.01884865015745163, -0.028312494978308678, 0.04297172278165817, -0.031031427904963493, 0.0031602063681930304, -0.0761629194021225, -0.07486966997385025, 0.01984582655131817, -0.058611560612916946, 0.11947961151599884, -0.07494963705539703, 0.04681447148323059, 0.02748170867562294, -0.053953319787979126, -0.053857315331697464, -0.03392425924539566, -0.03710514307022095, 0.013421524316072464, -0.0011677044676616788, 0.011950463987886906, -0.022732757031917572, 0.014704564586281776, 0.03965897485613823, 0.008631713688373566, -0.03614836931228638, -0.04645652696490288, -0.06848661601543427, -0.04609980806708336, 0.02954491786658764, -0.12481191009283066, -0.004690461326390505, -0.023026226088404655, -0.0007371961255557835, 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-0.029524758458137512, -0.020449088886380196, -0.02585815079510212, 0.004926146008074284, 0.0035625372547656298, 0.043203070759773254, 0.017423400655388832, -0.0033595801796764135, 0.031442295759916306, -0.0031192523892968893, -0.005037000402808189, -0.0663655549287796, -0.004438878037035465, -0.07872788608074188, -0.04412967339158058, -0.04635896906256676, -0.05762435495853424, -0.023867163807153702, 0.0013950836146250367, 0.05801932513713837, 0.09452793002128601, -0.06608639657497406, -0.07739570736885071, 0.01851499453186989 ]
15,162
15,165
AMON IC_HAWC NuEm-220116A: No neutrino counterpart detected with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration.
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported AMON IC-HAWC coincidence alert NuEm-220116A [https://gcn.gsfc.nasa.gov/notices_amon_nu_em/0_105322.amon]. No up-going muon neutrino candidate events were detected within 3 degrees from the coincidence coordinate over a time period [21h13 - 23h26 UT] corresponding to 34.5% of the HAWC transit time mentioned in the AMON notice, and during which the potential source remained visible in the up-going field of view of ANTARES. This leads to a preliminary 90% confidence level upper limit on the muon neutrino radiant fluence from a point source located at the coordinates of the coincidence as reported by AMON, of about 14 GeV.cm^-2 over the energy range 6 TeV - 6 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 31 GeV.cm^-2 (1 - 580 TeV) for an E^-2.5 spectrum. These indicative limits have been computed for the end of the HAWC transit time. A search over an extended time window of +/-1 day has also yielded no detection (34% visibility). ANTARES [https://antares.in2p3.fr] is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2022-01-18 15:55:00
tev,neutrinos
2022-01-18
15:55:00
1,454
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15,163
15,166
Fermi-LAT Gamma-ray Observations of IceCube-220115A and detection of a new gamma-ray source, Fermi J2350.2+2620
S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg) and J. Sinapius (DESY-Zeuthen) on behalf of the Fermi-LAT collaboration
We report an analysis of observations of the vicinity of the high-energy IC220115A neutrino event (GCN 31451) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2022-01-15 12:11:39.75 UTC (T0) with J2000 position RA = 357.45 (+1.75, -1.18) deg, Decl. = 25.28 (+1.03, -0.95) deg 90% PSF containment. No cataloged gamma-ray sources are found within the 90% IC220115A localization error (The Fourth Fermi-LAT catalog DR2; The Fermi-LAT collaboration 2020, ApJS, 247, 33). We searched for the existence of intermediate (months to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (> 100 MeV) at the the IC220115A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is < 5.6-10 ph cm^-2 s^-1 for ~13-years (2008-08-04 / 2022-01-15 UTC), < 1.1e-8 (< 5.2e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Within the 90% confidence localization of the neutrino, ~1.1 deg offset from the best-fit IC220115A position, a >4 sigma excess of gamma rays, Fermi J2350.2+2620 was detected in an analysis of the integrated LAT data (> 100 MeV) between 2008-08-04 and 2022-01-15. Assuming a power-law spectrum, the candidate gamma-ray source has best-fit localization (J2000) RA: 357.564, Dec: 26.343 (0.15 deg 99% containment, 0.07 deg 68% containment), with best-fit spectral parameters flux = (8 +/- 5)e-10 ph cm^-2 s^-1 and index = 2.0 +/- 0.2. In a preliminary analysis of the LAT data over one day and one month prior T0, Fermi J2350.2+2620 is not significantly detected in the LAT data. All values include the statistical uncertainty only. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de) and S. Buson (sara.buson at uni-wuerzburg.de). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-01-18 19:28:00
gamma ray,neutrinos,agn,blazar,transient,request for observations
2022-01-18
19:28:00
2,382
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-0.03328568488359451, 0.018579354509711266, 0.07872191071510315, -0.034748807549476624, 0.010781697928905487, -0.07276077568531036, -0.10358557850122452, 0.01929609477519989, 0.06096206605434418, -0.08350352197885513, 0.02128973789513111, -0.042485591024160385, -0.06821712106466293, -0.024804221466183662, 0.09475841373205185, -0.046081606298685074, -0.035280466079711914, -0.026241539046168327, -0.006490386091172695, 0.008766857907176018, -0.08475551009178162, -0.1534239500761032, -0.011178398504853249 ]
15,164
15,167
Discovery of 10 ASAS-SN Supernova Candidates
J. Brimacombe (Coral Towers Observatory), J. M. Fernandez (Observatory Inmaculada del Molino), G. George (MGA/WWVSH), P. Vallely, K. Z. Stanek, C. S. Kochanek, C. Christy, M. Rizzo Smith, S. Bose, T. A. Thompson (Ohio State), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), M. Stritzinger (Aarhus), P. Pearl (The Gap Observatory, BOSS)
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm "Brutus" telescope in Haleakala, Hawaii, the quadruple 14-cm "Leavitt" telescope in Fort Davis, Texas, the quadruple 14-cm "Payne-Gaposchkin" telescope in Sutherland, South Africa, and the quadruple 14-cm "Cassius" and "Paczynski" telescopes in Cerro Tololo, Chile, we discovered several new transient sources. Properties of the supernovae, as well as associated finding charts showing the archival imaging (left) and the follow-up confirmation image (right) are included in the table below: Follow-up observations are encouraged. While we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-22xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-22xx (AT 2022xyz) to preserve, rather than anonymize, the origin of the transient. We would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grants GBMF5490 and GBMF10501, and also funded in part by the Alfred P. Sloan Foundation grant G-2021-14192. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
2022-01-19 02:07:00
optical,supernovae,transient
2022-01-19
02:07:00
1,443
[ -0.04784942790865898, -0.08406559377908707, -0.013683007098734379, 0.009571676142513752, -0.03220396488904953, -0.05786791443824768, -0.12846414744853973, -0.04269595444202423, -0.06428664177656174, -0.03619898110628128, -0.01037864200770855, -0.10125075280666351, 0.00737262237817049, -0.07225804775953293, 0.03127111494541168, 0.029618574306368828, 0.08361823856830597, -0.08636584877967834, 0.008034816943109035, -0.010163591243326664, 0.009336650371551514, -0.005549663212150335, -0.05639367178082466, 0.034334924072027206, 0.05486423149704933, -0.004347836133092642, -0.08200697600841522, -0.043870631605386734, -0.0008254718850366771, -0.03145521506667137, -0.03915994614362717, 0.04990559071302414, -0.037189070135354996, 0.0017641065642237663, 0.0641011893749237, -0.0038605404552072287, 0.007192783523350954, -0.05903550609946251, -0.026699123904109, 0.006168623920530081, 0.004227285739034414, -0.04097805544734001, -0.006306953262537718, 0.021572908386588097, -0.0420677587389946, 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15,165
15,168
GBT observations of SGR J1935+2154 during its recent high-energy bursting activity phase
Yogesh Maan (NCRA, India), Samayra Straal (NYU Abu Dhabi, UAE), Joeri van Leeuwen (ASTRON, NL) and Ines Pastor-Marazuela (UvA, NL)
SGR 1935+2154 is known to produce bright radio bursts (ATel #13681, #13684), including bursts with very high, FRB-like, energies (ATel #14074, #14080). After these CHIME and STARE2 detections, FAST also reported radio bursts and pulsed periodic emission at L-band (ATel #14084). With the detection of several high-energy bursts (GCN #21296, ATel #15141, #15162), SGR 1935+2154 entered into its latest outbursting phase on December 24, 2021. To search for any radio activity in terms of bright radio bursts and/or periodic emission, we observed SGR 1935+2154 on January 05, 2022 using the Green Bank Telescope (GBT) at L-band (1.1 - 1.9 GHz) and S-band (1.6 - 2.4 GHz). The source was observed for 63 minutes at L-band starting at 2022-01-05T19:42:04.00, and 60 minutes at S-band starting at 2022-01-05T18:27:57.001 (date and time are in UTC). At both the bands, we recorded data in coherent dedispersion mode using a DM of 332.66 pc cm^-3, with 2048 channels across a bandwidth of 800 MHz and a sampling time of 40.96 us. The nearby pulsar PSR B1933+16 was also observed as a test pulsar. We first down-sampled the data to 81.92 us, and 512 frequency sub-bands and then searched for periodic emission, both completely blind and by folding the data around the known period, as well as for bright single pulses, in the DM range of 320 - 345 pc cm^-3. We do not detect any significant periodic or burst emission. After taking into account the time and frequency sections excluded due to radio frequency interference, we place an 8-sigma upper limit on the period-averaged flux density of 12.3 microJy and 12 microJy at L and S-band respectively, assuming a 10% duty cycle. For any burst-like emission, we place 8-sigma upper limits on the pulse-integrated flux density of 51 mJy and 48 mJy at L and S-band respectively, assuming a pulse width of 2 ms. We note that high-energy bursts from SGR 1935+2154 were also detected by Fermi-GBM about 12.6/11.4 hours before as well as 6.9/8.1 hours after the start of our L/S-band observations (ATel #15162). However, no high-energy burst is reported during our radio observations. We thank the Green Bank Observatory and staff for their support and the prompt scheduling of our triggered observations.
2022-01-19 13:05:00
radio,x-ray,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
2022-01-19
13:05:00
2,239
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15,166
15,169
RS Oph emerges from solar conjunction showing great changes
U. Munari (INAF Padova), P. Valisa and S. Dallaporta (ANS Collaboration)
After two months of non-observability, RS Oph has recently emerged from the Solar conjunction. We have resumed collecting photometric and spectroscopic data for the ongoing outburst (eg ATel #14834, #14840, #14844, #14855, #14864, #14886) and found RS Oph to have greatly evolved compared to mid-November when it plunged into the conjunction. RS Oph is still tracking closely the photometric evolution of the previous outburst, as shown in this comparison of the lightcurve for the 2021 (ANS Collaboration data) and 2006 outbursts (from Munari et al. 2007BaltA..16...46M). The most recent BVRI observations that we have collected with ANS Collaboration ID 0310 telescope are listed in the table below (days counted from maximum brightness on Aug 09.58 UT), where they are compared with our last measurement before the conjunction and the median values over the 2008-2020 period between the outbursts. Immediately before the conjunction, RS Oph was still bluer than in quiescence (note that the V-R color was dominated by an extremely strong Halpha), but has turned fainter and redder upon emersion: the nova ejecta that were still providing a substantial contribution to the overall brightness in mid November, have now diluted into the surrounding space. There seems to be less gas now than in quiescence for the still hot WD to ionize, as the cavity emptied by the nova ejecta may have not yet been replenished by the wind of the RG, and the accretion disk may still be reforming. Echelle spectra of RS Oph have been obtained on 2022 Jan 16.22, 18.23 and 19.21 UT with the Varese 0.84m telescope which is maintaining a tight monitoring since the onset of the outburst (Munari and Valisa 2021, arXiv 2109.01101). The spectrum for Jan 18 is compared here with one from Nov 19, our last observation before the conjunction. The ionization degree has reduced: the strong [FeXI] 7890 has disappeared, [FeX] 6375 has declined to 1/12, while [FeVII] is remaining constant. Other emission lines have reduced in intensity to about 1/3, with the exception of the broad (FWHM=1300 km/s) [OIII] and [NII] lines from the nova ejecta, that keep expanding at constant velocity after breaking free of the RG wind. The triple structure of permitted and narrow emission lines is still well visible in the Balmer lines, less so for the others as the bluer of the three components is becoming lost in the background continuum from the RG.
2022-01-20 06:32:00
optical,cataclysmic variable,nova,variables
2022-01-20
06:32:00
2,421
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0.045680638402700424, 0.0907926931977272, -0.0221263375133276, 0.040528833866119385, -0.05243996903300285, -0.10130568593740463, 0.023810844868421555, -0.02019343338906765, -0.015137068927288055, -0.04519370198249817, 0.009107199497520924, -0.02472076378762722, -0.06522832065820694, -0.09048187732696533, -0.04343493655323982, -0.04540790244936943, 0.02425834909081459, -0.01420531701296568, 0.12626785039901733, -0.010159549303352833, -0.08799459785223007, 0.02917827107012272 ]
15,167
15,170
Independent Discovery of a Slowly Brightening Possible Nova in M31
K. Hornoch, H. Kucakova (Astronomical Institute, Ondrejov, Czech Republic)
We report the independent discovery of a slowly brightening possible nova in M31 on a co-added 900-s R-band CCD frame taken on 2022 Jan. 15.717 UT with the 0.65-m telescope at Ondrejov. We found the new transient object as a faint source and postponed its announcement until we had additional images confirming the ongoing brightening of the object, supporting its possible nova nature. The object was independently discovered on Jan. 16.587 UT by M. Zhang and X. Gao and designated as PNV J00430928+4116013 = AT 2022uz. The object was designated by us as M31N 2022-01a and is located at R.A. = 0h43m09s.30, Decl. = +41o16'00".9 (equinox 2000.0), which is 281.6" east and 7.6" south of the center of M31 (see link to discovery and confirmation image below). The following R-band magnitudes were obtained using the 0.65-m telescope at Ondrejov: 2022 Jan. 2.714 UT, [20.3; 15.717, 19.5 ± 0.2; 19.709, 19.1 ± 0.15.
2022-01-20 07:27:00
optical,nova,transient
2022-01-20
07:27:00
914
[ -0.0787079855799675, 0.014951594173908234, 0.05884106457233429, 0.05717216804623604, 0.02675015851855278, -0.0557258203625679, -0.05187274143099785, 0.0427449494600296, 0.01869475468993187, -0.037137046456336975, -0.026792781427502632, -0.03522884473204613, -0.045614853501319885, -0.028433922678232193, 0.002017896855250001, -0.020111264660954475, 0.08219169825315475, -0.04291413351893425, 0.0026592870708554983, 0.04582798480987549, 0.005171228665858507, 0.06675513088703156, -0.05594322830438614, 0.04718197137117386, 0.04867037758231163, 0.04373127222061157, -0.031790077686309814, -0.042693257331848145, 0.02321414276957512, 0.004777148365974426, 0.046201687306165695, 0.05218503624200821, -0.08183038234710693, 0.039713986217975616, -0.025445738807320595, -0.02148057520389557, 0.07192354649305344, -0.010500642471015453, 0.04717974737286568, 0.008723491802811623, 0.04537120833992958, -0.03881237283349037, 0.03210803121328354, -0.010565213859081268, 0.02077176608145237, 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15,168
15,171
A possible discovery of AGN during a NuSTAR calibration observation
Aysegul Tumer (The University of Utah), Daniel R. Wik (The University of Utah), Kristin K. Madsen (NASA Goddard Space Flight Center, University of Maryland), Francesco Tombesi (University of Rome Tor Vergata), E. Nihal Ercan (Bogazici University)
During the analysis of a calibration observation (ObsID:10610035001) of The Nuclear Spectroscopic Telescope Array (NuSTAR; Harrison et al. 2013, ApJ, 770, 103) that took place on 25 April 2020 (JDM 58964), we discovered an AGN candidate. The NuSTAR J2000 coordinates of this source are (RA,Dec) = (05:34:49.20, +21:26:02.9), which will be referred to as NuSTAR J053449+2126.0 or Tumer 1. The redshift of Tumer 1 is unknown to the best of our knowledge. We extracted a 1 arcmin NuSTAR spectrum centered on the object and fitted a power-law in the 3.0-20.0 keV energy band. The resulting photon index and norm with 1 sigma errors are: Gamma = 2.46 (-0.16,+0.17) and norm = 4.31E-04 (-1.12E-04,+1.53E-04) with cstat/dof = 140.87/149. The flux in the 3.0-10.0 keV energy band is 4.2451E-13 ergs/cm^2/s. Assuming the source is at z=0.1, the 0.5-2.5 luminosity is L_X = 4.69E+42 erg/s. Assuming a Galactic origin, with a distance of 1 kpc that corresponds to z=2.36900E-07, we found 0.5-2.5 luminosity, L_X = 2.82E+31 erg/s. The redshift of the object is needed to obtain the true luminosity. We thank the NuSTAR Operations, Software and Calibration teams for scheduling and the execution of these observations. Optical follow up observations are encouraged to find the redshift of the object for luminosity calculations.
2022-01-20 10:02:00
optical,x-ray,agn
2022-01-20
10:02:00
1,315
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15,169
15,172
Parkes ultra-wideband observations of SGR 1935+2154 during recent epochs of high activity
M. E. Lower (CSIRO Space and Astronomy), R. M. Shannon (Swinburne University of Technology) and P. Kumar (Swinburne University of Technology)
Following reports of renewed high-energy activity of magnetar SGR 1935+2154 in September 2021 (GCN #30806) and January 2022 (GCN #31445), we conducted 10425 s and 9416 s target of opportunity observations of the source starting at UTC 2021-09-11-09:04:54 and UTC 2022-01-14-01:09:33 respectively, with the CSIRO Parkes 64-m radio telescope (Murriyang). We recorded pulsar search-mode data via the Medusa backend using the Ultra-Wideband Low receiver system (central frequency of 2368 MHz, 3328 MHz of bandwidth; Hobbs et al. 2020) with 0.5 MHz-wide frequency channels and 64 microsecond sampling. These data were coherently dedispersed at a DM of 332.72 pc/cc. The data were searched for single pulses and fast radio bursts using the Heimdall (Barsdell 2012) and Fetch (Agarwal et al. 2020) packages over a DM range of 100-1100 pc/cm^3, employing a tiered sub-band strategy as described in Kumar et al. (2021). No significant single-pulse candidates of astrophysical origin were identified in either observation. Hence, we constrain the the fluence of 1 ms wide single pulses down to be less than ~0.15 Jy ms for broadband (3.3 GHz bandwidth) pulses or ~1 Jy ms for narrowband (64 MHz bandwidth) pulses during our observations. We note that two high-energy bursts were recorded by Fermi Gamma-Ray Burst Monitor at UTC 2021-09-11-10:42:51.85 and UTC 2021-09-11-11:53:57.29 (GCN #30831), both of which overlap with our first Parkes observation. Neither burst appears to have been accompanied by a radio counterpart. We also searched for signs of low-level pulsed emission by folding the data at the magnetar rotation period. No evidence for a periodic signal was found in a search spanning +/- 1 ms from the nominal period of the magnetar and +/- 25 pc/cc around its previously reported dispersion measure. Using the radiometer equation with an assumed 10 percent duty cycle and limiting S/N of 7, we place upper limits on the 2368 MHz flux of SGR 1935+2154 of 4.9 uJy on 2021-09-11 and 5.2 uJy on 2022-01-14. We would like to thank the ATNF staff, in particular James Green, for allocating the observation time. References: Agarwal, D., et al., FETCH: A deep-learning based classifier for fast transient classification, MNRAS, 479, 1661 (2020) Barsdell, B. R., Advanced Architectures for Astrophysical Supercomputing PhD thesis, Swinburne Univ. Technology (2012) Hobbs, G., et al., An ultra-wide bandwidth (704 to 4032 MHz) receiver for the Parkes radio telescope, PASA, 37, e012 (2020) Kumar, P., et al., Extremely band-limited repetition from a fast radio burst source, MNRAS, 500, 2525 (2021)
2022-01-21 13:04:00
radio,gamma ray,fast radio burst,gamma-ray burst,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
2022-01-21
13:04:00
2,599
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15,170
15,173
MASTER: high amplitude OT (>6.5m) outburst and UVCet flare
P. Balanutsa, V. Lipunov, K. Zhirkov, E. Gorbovskoy, A. Kuznetsov, O. Gress, G. Antipov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Topolev, A. Chasovnikov, E. Minkina, V. Grinshpun, D. Cheryasov, Ya. Kechin, Ya. Kechin, T. Pogrosheva, V. Shumkov (Lomonosov MSU), R. Rebolo, M. Serra(IAC), D. A. H. Buckley (SAAO), N. M. Budnev (ISU, API), R. Podesta, C. Lopez, F. Podesta, C. Francile (OAFA), A. Tlatov, D. Dormidontov (KSS, Pulkovo observatory), A. Gabovich(BSPU)
MASTER OT J173432.09+191254.2 discovery - new OT, dwarf nova outburst, ampl>6.5m MASTER-Kislovodsk auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) during own survey detected new optical transient source at (R.A.,Dec 2000) = 17h 34m 32.09s +19d 12m 54.2s on 2022-01-20.14418 UT. The OT unfiltered magnitude is 15.7m (mlim=17.6m). The OT is seen in 3 images. There is no minor planet at this place. We have reference image on 2015-08-14.75668 UT with unfiltered mlim=21m. There is no known sources in VIZIER at this position. But there is non-catalogued blue OT at PanSTARR images, taking into account neighbouring faint stars with known rmag~22, the amplitude of current OT outburst is more then 6.5mag. Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/173432.09191254.2.png MASTER OT J130738.14+210242.9 discovery possible UV Ceti MASTER-Amur auto-detection system discovered the flash of OT source at (RA, Dec) = 13h 07m 38.14s +21d 02m 42.9s on 2022-01-19.67195 UT. The OT unfiltered magnitude is 15.4m (mlim=17.3m). The OT is seen in 2 images. There is no minor planet at this place. We have 1 images for this night without object 2022-01-19.66082UT with mlim=17.2m. We have also reference image on 2019-01-05.85213 UT with unfiltered mlim=17.1m, 2017-05-30 02:28:55UT with mlim=20.5m. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/MASTEROTJ130738.14+210242.9.jpg
2022-01-21 23:23:00
optical,cataclysmic variable,nova,planet,star,transient,variables,request for observations
2022-01-21
23:23:00
1,542
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15,171
15,174
Konus-Wind observations of recent SGR 1935+2154 activity
A. Ridnaia, D. Frederiks, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko (Ioffe Institute), and T. Cline
Since the beginning of January 2022 Konus-Wind triggered on thirteen bright bursts from the SGR 1935+2154.
2022-01-22 02:26:00
x-ray,gamma ray,magnetar,soft gamma-ray repeater
2022-01-22
02:26:00
106
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15,172
15,175
Spectroscopic classification of SN 2021aau with Gemini-South/GMOS
M. R. Siebert, R. J. Foley (UC Santa Cruz)
We report the classification of SN 2021aau with the GMOS spectrograph on the Gemini-South Telescope with GMOS on UT 2022 Jan 21. The target was supplied by DLT40. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The red spectrum is consistent with a SN II that suffered significant host-galaxy reddening.
2022-01-22 03:28:00
optical,supernovae,transient
2022-01-22
03:28:00
496
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15,173
15,176
Erratum to ATel #15175
M. R. Siebert, R. J. Foley (UC Santa Cruz)
In ATel #15175 SN2021aau should be SN2022aau. Below is a corrected version of ATel #15175. Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The red spectrum is consistent with a SN II that suffered significant host-galaxy reddening.
2022-01-23 02:08:00
optical,supernovae,transient
2022-01-23
02:08:00
340
[ -0.0797201618552208, -0.04029681533575058, 0.03921513259410858, 0.054248105734586716, 0.015064427629113197, 0.04255611449480057, -0.021593088284134865, 0.007617372088134289, 0.02359028346836567, -0.0605575293302536, 0.020215313881635666, -0.01458948664367199, 0.032580796629190445, -0.040355000644922256, -0.024002844467759132, -0.03681505471467972, -0.026610706001520157, -0.035290203988552094, -0.014124849811196327, -0.039235275238752365, 0.032023485749959946, 0.10201804339885712, -0.03629320487380028, 0.018602684140205383, 0.055716436356306076, -0.1034528985619545, -0.029246993362903595, -0.01956263929605484, -0.027254972606897354, -0.0525188073515892, 0.06566926836967468, 0.058614715933799744, 0.060723237693309784, 0.03605211526155472, 0.05943811684846878, -0.08172883838415146, 0.04055589810013771, -0.010517850518226624, 0.018968909978866577, -0.018039202317595482, 0.07057248055934906, -0.04020027443766594, 0.09968923777341843, 0.023167157545685768, 0.020457791164517403, 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15,174
15,177
Comet C/108P (Ciffreo) is not splitting
Federico Manzini (SAS), Paolo Ochner (University of Padova; INAF-OAPd), Virginio Oldani (SAS), Luigi R. Bedin (INAF-OAPd), Andrea Reguitti (UNAB; INAF-OAPd), Jean Gabriel Bosch, Jean François Soulier
Comet C/108P was discovered by Jacqueline Ciffreo on November 8, 1985 with the 0.9-m Schmidt telescope of CERGA-France (IAUC 4135 ). Its short-term orbit was calculated by D. Green (IAUC 4137 ). The comet was followed by our group in its current apparition since November 7, 2021, when it showed well-defined morphological structures in the inner coma. Following some alerts of a possible fragmentation of the nucleus ( https://groups.io/g/comets-ml ), an observation of the comet was scheduled on December 30, 2021 with the INAF-OAPd 1.82-m Copernico telescope (Asiago Astrophysical Observatory, Italy). On the high-resolution CCD image, the false nucleus appeared very bright, slightly elongated in PA 30°, with an average FWHM of about 1.8 arcsec (about 1,300 km at the distance of the comet). The tail was oriented towards PA 245 deg. A bright condensation, elongated in the E-W direction, was visible in the coma at PA 90 deg, which appeared detached from the nuclear region, with a center of gravity about 7 arcsec east of the optocenter (about 5,250 km at the distance of the comet) (Figure 1). A very similar morphological structure had already been observed during the comet's last orbit in December 2014, albeit with instruments of smaller diameter and lower resolution (J.G. Bosch, A. Maury, J.F. Soulier), in almost analogous geometric conditions to those of 2021 (Figure 2). Similar morphology was also observed about 1 month after the discovery of the comet, by S. M. Larson and D. Levy, who reported that CCD images obtained with 1.5-m and 0.5-m telescopes in December 1985 showed a detached dust tail extending over 20" to the north-east of the nucleus and curving in the direction of increasing position angle. The distance of the point of maximum intensity in the tail was about 6" from the nucleus (IAUC 4158 , and Bull. AAS 1986, Vol. 18, p.811). In the same IAUC A.R. Klemola (Lick Observatory) wrote that an exposure with the Crossley reflector on 1985 Dec. 17.3 UT showed a sharp stellar object separated by an almost clear gap from a diffuse coma or tail feature. The center of the diffuse feature was 5.6" to the northeast of the stellar object. A more in-depth analysis, supported by a modelling of the inner coma that takes into account the dust outflow from discrete sources on the surface of the nucleus, shows that this structure, recurrently observed during previous apparitions of the comet, may originate from a strong activity of an area in near-polar position on a nucleus with a spin axis directed approximately towards the Sun (Figure 3). The dust outflow, emitted collimated in almost sunwards direction, would be pushed back by the radiation pressure and, due to the geometry of the observation, would appear projected onto the coma, thus creating a 'clump' effect that could resemble a detached fragment which, however, is not real. Figures are available at: https://web.oapd.inaf.it/bedin/files/PAPERs_eMATERIALs/ATel/C1985P/FiguresATEL108P.PDF
2022-01-25 19:10:00
optical,comet,the sun
2022-01-25
19:10:00
2,987
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15,175
15,178
MAXI/GSC detection of an X-ray short transient event MAXI J0709-159
M. Serino (AGU), H. Negoro, M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC)
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 10:42:28 UT on 2022 January 25. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (107.280 deg, -15.923 deg) = (07 09 07, -15 55 22) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.16 deg and 0.14 deg, respectively. The roll angle of long axis from the north direction is 161.0 deg counterclockwise. Without assumptions on the source constancy, we obtain a rectangular error box for the transient source with the following corners: (R.A., Dec) = (106.814, -15.283) deg = (07 07 15, -15 16 58) (J2000) (R.A., Dec) = (106.608, -15.459) deg = (07 06 25, -15 27 32) (J2000) (R.A., Dec) = (107.823, -16.775) deg = (07 11 17, -16 46 29) (J2000) (R.A., Dec) = (108.029, -16.598) deg = (07 12 06, -16 35 52) (J2000) There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 266 +- 32 mCrab (4.0-10.0keV, 1 sigma error). There was no significant excess flux in the previous transit at 09:09 UT and in the next transit at 12:15 UT with an upper limit of 20 mCrab for each. Since the source showed a soft X-ray spectrum and the source is located at low galactic latitude at (l, b) ~ (229.1 deg, -3.4 deg), it is possible that the source is a galactic transient source. We tentatively name the source MAXI J0709-159.
2022-01-25 20:47:00
x-ray,nova,transient
2022-01-25
20:47:00
1,462
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-0.023491395637392998, -0.030075915157794952, 0.10192886739969254, 0.042825620621442795, 0.049596648663282394, 0.00500252703204751, 0.038820162415504456, 0.00833399873226881, -0.032645780593156815, -0.0014942486304789782, -0.007693314924836159, 0.016160760074853897, -0.04274668172001839, -0.04741256311535835, 0.07010330259799957, 0.016884934157133102, -0.059031419456005096, 0.015253270044922829, -0.04860688000917435, 0.03730146586894989, -0.05179888382554054, -0.010897084139287472, 0.05987350270152092 ]
15,176
15,179
Chandra spectroscopy of the TDE AT2021ehb: evidence of a relativistic outflow
J. M. Miller, M. T. Reynolds, S.-B. Yun, A. Zoghbi (Univ. of Michigan), B. Cenko (NASA/GSFC), J. J. Drake (SAO), J. A. Irwin (Univ. Alabama), C. Miller (Univ. of Maryland), R. Mushotzky (Univ. of Maryland)
Following a rise in flux that met the trigger of our approved Cycle 22 TOO program, we observed AT 2021ehb (Munoz-Arancibia et al. 2021, Yao et al. 2021) with Chandra for 50 ks, divided between two exposures obtained on 2021 Nov 29. The dispersed spectra from the LETG were read using the HRC. The most interesting result of our analysis is that a power-law continuum shaped by a moderately ionized, relativistic wind (v = -0.15c) is preferred over alternatives, including a blackbody plus power-law continuum. The Cash statistic was minimized in the fitting process, across the 5-25 Angstrom range, after binning to require a signal to noise of S/N = 3.5. A simple power-law continuum, modified by neutral absorption in the Milky Way and host galaxy, leaves emission-like residuals near to 16 A with flux decrements on either side (Gamma = 2.7). However, no single-temperature thermal plasma model significantly improves the fit to this region. The addition of a blackbody with a temperature of kT = 0.10 keV improves the fit close to 16 A, but does not fully describe the complex. Comparing this two-component model to the simple power-law using the Akaike Information Criterion gives delta(AIC) = 1.2, signaling the improvement is not significant. Instead, allowing the power-law continuum to be modified by a partially covering wind component provides the best overall description of the spectrum. Simple fits with the "zxipcf" model give a Cash statistic of 24.4 for 37 degrees of freedom and 44 bins. The column density of the absorber is N_H = 8 (+7,-2) E+22 cm^-2, the ionization parameter is log xi = 2.0+/-0.1, the covering fraction is 0.77 (+0.06,-0.09), and the wind velocity is v = -0.15 +/- 0.02 (measured relative to the host galaxy at z = 0.017). Again utilizing the AIC, we find delta(AIC) = 5, signaling an improvement. The zxipcf model samples ionization very coarsely; replacing zxipcf with alternative absorption models confirms the results obtained with zxipcf. Examining the 10 Swift/XRT monitoring spectra obtained closest to the Chandra observation, spanning October 30 - December 30 2021, we found that joint fits including a zxipcf component with a variable column density results in an improvement over a simple power-law, with delta(AIC) = 10. The jointly-determined outflow velocity is -0.24c, suggesting that the wind may be even faster on average. We caution that CCD data are ill-suited to this kind of spectral analysis. The Chandra results imply a wind with a high covering factor. However, if the wind is active for a lengthy period - as may be implied in the Swift monitoring observations - a low volume filling factor is required if the total mass outflow is not to exceed the mass available from a disrupted solar-mass star. Alternatively, the TDE may have stimulated enhanced accretion from a pre-existing accretion disk or gas reservoir around the massive black hole. This may be supported by the fact that the X-ray rise phase occurred long after the discovery of AT2021ehb (March 3, 2021; Munoz-Arancibia et al. 2021). We thank the Chandra Director, Pat Slane, the CDO, and the Mission Planning team for executing our observations, and the Neil Gehrels Swift Observatory team for monitoring AT2021ehb. Munoz-Arancibia, A., et al., 2021, TNSTR, 651, 1 Yao, Y., 2021, TNSCR, 2291, 1
2022-01-25 23:09:00
x-ray,black hole,star,tidal disruption event,transient,variables
2022-01-25
23:09:00
3,323
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15,177
15,180
MASTER OT J153539.77-461415.4 outburst detection with amplitude >5.6m in OAGH observatory
K. Zhirkov, V. Lipunov, V. Kornilov, A. Kuznetsov, E. Gorbovskoy, G. Antipov, D. Vlasenko (Lomonosov MSU), L. Carrasco, J. R.Valdes, V. Chavushyan, V. M.Patino Alvarez, J. Martinez, A. R.Corella, L. H.Rodriguez (INAOE, OAGH), P. Balanutsa, V. Senik, Ya. Kechin, Yu. Tselik, T. Pogrosheva, V. Shumkov, E. Minkina, A. Chasovnikov, V. Topolev, V. Grinshpun, D. Kuvshinov, D. Zimnukhov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, F. Podesta, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra-Ricart (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O. A. Gress, N. M. Budnev (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V. Yurkov (Blagoveschensk State Pedagogical University)
MASTER OT J153539.77-461415.4 discovery - dwarf nova outburst with amplitude >5.6m First optical transient, detected in MASTER-OAGH (INAOE, Mexico). MASTER-OAGH of Lomonosov MSU MASTER Global Robotic Net was mounted in December 2021 in Mexico, Guillermo Haro Astrophysics Observatory of the National Institute of Astrophysics, Optics and Electronics. MASTER-OAGH consists of twin 40cm telescope, equipped with BVRI,PP filters, 4-8 square degrees field of view and has own real-time reduction and auto-detection system (Lipunov et al., MASTER Global Robotic Net, Advances in Astronomy, 2010, 30L). We use the same scientific equipment at every MASTER observatory, it means the same photometry system and possibility to use own archive images since 2006y. for analysis. During Fermi trigger 664738369 (Ttrigger=2022-01-24 17:32:44.36UT, R.A.,Dec.(2000)=15h 36m 43s, -46d 38' 23", Rstat=5.08deg.) inspection MASTER-OAGH auto-detection system discovered OT source at (RA, Dec) = 15h 35m 39.77s -46d 14m 15.4s at 2022-01-25.50915 UT (the second image was at 2022-01-25.54848UT with the same m_OT). The OT unfiltered magnitude is 14.4m (mlim=17.6). Taking into account the trigger time this OT should not be connected with GRB optical counterpart. The OT is seen in 3 images. There is no minor planet at this place. We have reference images in MASTER archive at 2018-09-12.91464 UT with unfiltered mlim=17.8m, at 2021-02-03 23:14:29UT with unfiltered mlim=17.6, at 2016-07-09 18:19:42UT with mlim=19m . There is no OT sources in Gaia,USNO inside 4" (22m limit in history). There is VISTA source in 0.7". Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/MASTEROTJ153539.77-461415.4.jpg
2022-01-26 00:44:00
optical,cataclysmic variable,nova,planet,transient,variables,request for observations
2022-01-26
00:44:00
1,755
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15,178
15,181
NICER detection of the new X-ray transient MAXI J0709-159
W. Iwakiri (Chuo U.), K. Gendreau, Z. Arzoumanian (NASA/GSFC), T. Enoto, T. Mihara (RIKEN), M. Serino (AGU), H. Negoro (Nihon U.), J. Pope (KBRwyle, NASA/GSFC), A. Sanna (Univ. of Cagliari)
Following the MAXI/GSC alert of a possible new transient named MAXI J0709-159 (ATel #15178), NICER performed multiple pointings to localize the source position beginning at 2022-01-25T13:44 (UTC). Starting from the nominal coordinates reported by MAXI, NICER performed a series of offset pointings with 42 s exposure for each. A preliminary source position was obtained at R.A. = 107.392 deg Dec = -16.108 deg (J2000), with 3 arcmin radius uncertainty set by the NICER non-imaging field of view. The averaged X-ray flux is about 10 mCrab in the NICER energy band (0.2 - 12 keV). Further NICER observations of this source are underway. Additional multi-wavelength observations are strongly encouraged. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2022-01-26 02:34:00
x-ray,transient
2022-01-26
02:34:00
872
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0.02739160694181919, -0.020656470209360123, 0.05115159973502159, -0.007042384706437588, -6.309490885314517e-8, -0.04804447293281555, -0.01587577722966671, -0.0798046812415123, 0.041662272065877914, -0.00015111727407202125, -0.024467678740620613, -0.032109878957271576, 0.09330092370510101, 0.017408646643161774, -0.01816541701555252, 0.04980656877160072, -0.02475835010409355, 0.028121907263994217, -0.07664269953966141, 0.0684593990445137, -0.006471862085163593, 0.04437630623579025, -0.023177385330200195, -0.06769982725381851, 0.01529078558087349, 0.009473249316215515, -0.010866565629839897, 0.08175353705883026, -0.041524048894643784, 0.013994365930557251, 0.027713119983673096, 0.03902927413582802, 0.07946690171957016, 0.07172360271215439, -0.1212984248995781, -0.04746512323617935, 0.0017206099582836032, 0.024711109697818756, -0.011118216440081596, 0.022647162899374962, 0.04415031149983406, -0.057458654046058655, -0.004469318315386772, 0.07123465836048126, 0.018789663910865784, -0.03724529594182968, -0.04100855439901352, 0.014790671877563, 0.07243796437978745, -0.003888213774189353, 0.006345412693917751, -0.008616585284471512, -0.08368232846260071, 0.004820073489099741, -0.06497324258089066, -0.004474738147109747, 0.03644276410341263, 0.022429004311561584, -0.0999465063214302, 0.021344734355807304, 0.026374490931630135, 0.03423656150698662, -0.07571850717067719, 0.027704134583473206, 0.04549827054142952, 0.039035484194755554, 0.02963477000594139, -0.1990073025226593, 0.016171317547559738 ]
15,179
15,182
Fermi-LAT detection of a new potential gamma-ray source associated with the radio source NVSS J161018+414653
G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed gamma-ray emission from a source positionally consistent with the radio source NVSS J161018+414653, also known as WISEA J161018.20+414654.0 / 87GB 160837.0+415405, with coordinates R.A. = 242.5759 deg, Decl. = +41.7816 deg (J2000; Condon et al., 1998, AJ, 115, 1693), and unknown redshift. This source is not in any published LAT catalog and was not detected by AGILE or EGRET. Preliminary analysis indicates that this source was significantly detected (>5 sigma) in a high gamma-ray state on January 24, 2022, with a daily averaged gamma-ray flux (E>100MeV) of (0.3+/-0.1) X 10^-6 photons cm^-2 s^-1 and a single power-law photon index of 2.2+/-0.3 (statistical uncertainties only). The best fit gamma-ray position was located at R.A. = 242.361 deg, Decl. = +41.925 deg, with a 68% confidence radius of 0.243 deg and an angular separation of 0.215 deg from the proposed counterpart. The suggested association is based on the inclusion of the radio source in the JVAS/CLASS catalog of flat-spectrum radio sources (Jackson et al., 2007, MNRAS, 376, 371), where it is listed as GB6 161018+414636. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Giovanni La Mura (glamura AT lip DOT pt). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-01-26 22:18:00
radio,gamma ray,agn,transient,request for observations
2022-01-26
22:18:00
1,751
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15,180
15,183
LJT spectroscopic classification of AT 2022ajw as a young Type Ia supernova
Qian Zhai, Jujia Zhang(YNAO); Liping Li (Yunnan University); Xiaofeng Wang(THU)
We report an optical spectrum of AT 2022ajw (350-870nm) obtained on 2022 Jan. 26.67 UT with the Lijiang 2.4-m telescope (LJT +YFOSC) at LiJiang observatory of Yunnan Observatories. The spectrum is similar to a Type Ia supernovae at a relatively early phase. Cross-correlation with the library of supernova spectra using the comparison tool Gelato (Harutyunyan et al. 2008, A&A, 488, 383) shows matches with SN 2003kf at t = -6 to -8 days. An expansion velocity of about 13000 km/s can be deduced from the Si II 6355 absorption minimum considering the redshift of 0.0489 for the host galaxy.
2022-01-27 09:12:00
optical,supernovae
2022-01-27
09:12:00
590
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15,181
15,184
Spectroscopic Classifications of Optical Transients with the Lick Shane telescope
K. Taggart, K. C. Loertscher, R. J. Foley (UCSC)
We report the following classifications of optical transients from spectroscopic observations with the Kast spectrograph on the Shane telescope. The targets were supplied by the Young Supernova Experiment and ATLAS. All observations were made on 2022 Jan 26 UT. Classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) Blue continuum, H-alpha at z=0 and a point source in Legacy Survey images are consistent with a CV. (2) We measure a Si II 6355 velocity of -11,500 km/s.
2022-01-27 11:41:00
optical,supernovae,transient
2022-01-27
11:41:00
653
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-0.0062146722339093685, -0.028533201664686203, -0.0312936007976532, 0.05454929918050766, -5.2511087034190496e-8, 0.03501269221305847, 0.050716761499643326, -0.07183526456356049, 0.060163527727127075, 0.012623707763850689, -0.024362197145819664, -0.016275852918624878, 0.04714418947696686, 0.019717374816536903, -0.04045819863677025, 0.007574167568236589, -0.06166938319802284, 0.017720576375722885, -0.0353156141936779, 0.0663413256406784, -0.030071627348661423, -0.003208302892744541, -0.008413142524659634, -0.05100167915225029, 0.0543840229511261, 0.03331928700208664, 0.07810265570878983, 0.04421413689851761, -0.06381513178348541, -0.007096387445926666, 0.026134373620152473, -0.025422852486371994, 0.12493771314620972, 0.04389829933643341, -0.062090400606393814, 0.05492003634572029, -0.03037085197865963, -0.01633136160671711, -0.02665494568645954, -0.011132706888020039, 0.01600896567106247, -0.11457046866416931, 0.07339012622833252, 0.10974812507629395, 0.06872397661209106, -0.07871635258197784, -0.029920153319835663, -0.04720310494303703, 0.03912021592259407, -0.08375633507966995, 0.0070226918905973434, -0.053953904658555984, -0.05735202878713608, -0.024202371016144753, 0.0637955591082573, -0.048856817185878754, 0.025889718905091286, -0.026095310226082802, -0.026652690023183823, -0.08600804954767227, -0.013561301864683628, 0.014805322512984276, -0.06500747054815292, -0.036962442100048065, -0.024006247520446777, 0.14533689618110657, -0.030120551586151123, -0.10116489976644516, 0.007497487589716911 ]
15,182
15,185
Spectroscopic Classification of AT2021aemn with the SOAR and Lick Shane telescopes
K. Taggart, K. W. Davis, M. J. Bustamante-Rosell, K. C. Loertscher, R. J. Foley (UCSC)
We report the following the classification of AT2021aemn from spectroscopic observations with the Goodman spectrograph on SOAR made on 2022 Jan 19 UT and with the Kast spectrograph on the Shane telescope on 2022 Jan 26 UT. The target was supplied by ZTF and the classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We measure an H-alpha absorption velocity of -6,500 km/s from the Lick spectrum. We thank the Director Jay Elias and staff at the SOAR and Lick observatories for their assistance in acquiring these observations.
2022-01-27 11:52:00
optical,supernovae
2022-01-27
11:52:00
710
[ -0.07906054705381393, -0.08921676129102707, -0.057040996849536896, 0.01622823067009449, 0.006874582264572382, 0.03776427358388901, -0.023239977657794952, 0.020125728100538254, -0.009358064271509647, -0.029539648443460464, -0.0031499499455094337, -0.07022211700677872, -0.03025083616375923, -0.04302045702934265, 0.015171036124229431, -0.04159994423389435, 0.055592045187950134, -0.09644297510385513, 0.0021726044360548258, 0.007648954167962074, 0.018013833090662956, 0.07057145237922668, 0.005922846961766481, 0.04852553457021713, 0.04873449727892876, -0.06196192279458046, -0.06732470542192459, -0.08124040067195892, 0.010979220271110535, -0.03362598270177841, 0.11108911037445068, 0.04994034767150879, -0.0074697681702673435, 0.08053100109100342, 0.036587540060281754, -0.06418069452047348, 0.023415349423885345, -0.011513231322169304, 0.03170829266309738, -0.014691471122205257, 0.052750710397958755, -0.04646355286240578, 0.026968367397785187, 0.025089962407946587, -0.004990100394934416, 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-0.03575016185641289, -0.04499698430299759, -0.0011962618445977569, 0.05415094643831253, -0.07862637937068939, -0.05034177377820015, -0.03764445707201958, -0.0779811292886734, 0.010015232488512993, 0.03718673810362816, -0.05049300938844681, 0.017234325408935547, -0.04369735345244408, -0.06656967103481293, -0.13452653586864471, -0.031215611845254898, -0.009129009209573269, -0.0765971690416336, -0.06311584264039993, 0.010124431923031807, 0.17576123774051666, -0.05927766114473343, -0.13203471899032593, 0.01641012728214264 ]
15,183
15,186
TRAPPIST comet production rates: 19P/Borrelly, 67P/C-G, 104P/Kowal 2, C/2019 L3 (ATLAS), and C/2021 A1 (Leonard)
E. Jehin, Y. Moulane, J. Manfroid, M. Vander Donckt, F. Pozuelos, M. Ferrais, D. Hutsemekers (STAR Institute, University of Liege)
E. Jehin, Y. Moulane, J. Manfroid, M. Vander Donckt, F. Pozuelos, M. Ferrais, and D. Hutsemekers (STAR Institute, University of Liege) report that they obtained from TRAPPIST-North (code=Z53, Morocco) and TRAPPIST-South (code=I40, Chile) robotic telescopes (Jehin el al. 2011) recent observations using cometary HB narrowband filters (Farnham et al. 2000) for the following comets and computed preliminary production rates at 10.000 km using a Haser Model (Vp=Vd=1km/s) (Haser 1957). The dust production rates proxy A(0)f(rho) was estimated by profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). 19P/Borrelly Date UT=2022-01-17, r_h=1.32 au, Delta=1.22 au, DT=-7 days Q(OH)=(2.76+/-0.41) E28 s-1; Q(NH)=(1.44+/-0.10) E26 s-1; Q(CN)=(5.75+/-0.65) E25 s-1; Q(C2)=(3.83+/-0.08) E25 s-1; Q(C3)=(6.74+/-0.22) E24 s-1 A(0)fp(BC)= 1847+/-35 cm 67P/C-G Date UT=2022-01-21, r_h=1.55 au, Delta=0.58 au, DT=+70 day Q(OH)=(2.16+/-0.24) E27 s-1; Q(NH)=(2.67+/-0.55) E25 s-1; Q(CN)=(6.10+/-0.56) E24 s-1; Q(C2)=(6.55+/-0.55) E24 s-1; Q(C3)=(4.38+/-2.30) E23 s-1 A(0)fp(BC)= 365+/-10 cm 104P/Kowal 2 Date UT=2022-01-18, r_h=1.08 au, Delta=0.65 au, DT=+10 day Q(OH)=(5.05+/-0.22) E27 s-1; Q(NH)=(4.12+/-0.39) E25 s-1; Q(CN)=(1.34+/-0.15) E25 s-1; Q(C2)=(1.40+/-0.16) E25 s-1; Q(C3)=(2.92+/-0.18) E24 s-1 A(0)fp(RC)= 100+/-10 cm C/2019 L3 (ATLAS) Date UT=2022-01-19, r_h=3.56 au, Delta=2.61 au, DT=+12 day Q(CN)=(1.26+/-0.10) E26 s-1; Q(C2)=(1.19+/-0.11) E26 s-1; Q(C3)=(5.16+/-0.49) E24 s-1 A(0)fp(BC)= 24710+/-125 cm With a dust/gas ratio of Log[A(0)fp(BC)/Q(CN)]=-21.71, C/2019 L3 appears as a very dusty comet, compared to the ratio of -23.30+/-0.32 for typical comets (A'Hearn et al. 1995). C/2021 A1 (Leonard) Date UT=202-01-22, r_h=0.64 au, Delta=1.17 au, DT=+18 days Q(OH)=(5.78+/-0.41) E28 s-1; Q(NH)=(1.61+/-0.15) E26 s-1; Q(CN)=(4.75+/-0.10) E25 s-1; Q(C2)=(6.70+/-0.13) E25 s-1; Q(C3)=(4.33+/-0.20) E24 s-1 Afp(BC)= 2597+/-46 cm Notations: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, NH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, GC, RC are the blue, green and red dust continuum filters (Farnham et al. 2000) Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS under grant PDR T.0120.21. TRAPPIST-North is funded by the University of Liège, and performed in collaboration with the Cadi Ayyad University of Marrakesh. Observations were carried on from the ESO La Silla Paranal Observatory. We thank NASA, David Schleicher and the Lowell Observatory for the loan of the HB comet filters. https://www.trappist.uliege.be/
2022-01-27 16:36:00
optical,comet,star
2022-01-27
16:36:00
2,688
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15,184
15,187
Radio Observations of SN 2022aau
S. D. Ryder (Macquarie University), E. Kundu (Michigan State University), L. Marnoch (Macquarie University), R. Z. E. Alsaberi (Western Sydney University), M. D. Filipovic (Western Sydney University), G. Anderson (ICRAR/Curtin University), C. Stockdale (Marquette University), K. Maeda (Kyoto University), M. Renaud (LUPM, CNRS/IN2P3), R. Kotak (University of Turku)
The young core-collapse supernova SN 2022aau (=DLT22b) in NGC 1672, classified as a type II event (ATel #15176), has been observed with the Australia Telescope Compact Array (ATCA) at 5.5 and 9.0 GHz on 25 Jan 2022 11:00-16:00 UT. No radio emission was detected to 3-sigma upper limits on the flux density of 0.22 mJy and 0.15 mJy at 5.5 GHz and 9.0 GHz, respectively, with the SN location close to the circumnuclear star-forming ring (Diaz et al. 1999, ApJ, 512, 623) making any detection more challenging. Adopting a host galaxy distance of ~15 Mpc from the NASA Extragalactic Database (NED) this implies an upper limit on the 5.5 GHz GHz luminosity within 6 days of explosion of 6.0E+25 erg/sec/Hz. We would like to extend our thanks to the ATCA staff for enabling these observations. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We acknowledge the Gomeroi people as the traditional owners of the Observatory site.
2022-01-27 18:08:00
radio,star,supernovae
2022-01-27
18:08:00
1,038
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-0.01701807789504528, -0.012068421579897404, 0.015048496425151825, 0.047903873026371, -5.7434746736362285e-8, 0.0005596864502876997, 0.06695879995822906, -0.08690483123064041, 0.04134238138794899, 0.021500784903764725, -0.057371195405721664, -0.01277067605406046, 0.024337489157915115, 0.09579320251941681, 0.05715663358569145, -0.10263856500387192, -0.10250554233789444, -0.0031923032365739346, -0.05447776988148689, 0.0690847709774971, -0.056979287415742874, -0.010383646935224533, -0.03409448638558388, -0.0654364600777626, 0.025106169283390045, 0.04670713096857071, 0.004873789846897125, 0.0427827425301075, -0.03983338922262192, 0.0061857691034674644, -0.011828064918518066, 0.0037917946465313435, 0.12136846035718918, 0.003049644874408841, -0.053143735975027084, -0.09732493758201599, -0.0045832302421331406, -0.04379821568727493, -0.056728001683950424, -0.10832102596759796, 0.03770677000284195, 0.048191510140895844, -0.021608974784612656, 0.08693520724773407, 0.0672890692949295, 0.024874238297343254, -0.03524167463183403, -0.00866964552551508, 0.03605830296874046, -0.03345241770148277, 0.01634812168776989, 0.009656306356191635, -0.012805799953639507, -0.0047501758672297, -0.030567066743969917, -0.06767965853214264, -0.01420640293508768, -0.05726751685142517, -0.11277149617671967, -0.05146035552024841, 0.013976948335766792, -0.04686775803565979, -0.01970423385500908, 0.00547599233686924, 0.0034846626222133636, 0.08666214346885681, -0.07922284305095673, -0.1263904869556427, -0.000943272840231657 ]
15,185
15,188
MAXI observations of two bright X-ray flares from MAXI J0709-159
K. Kobayashi, H. Negoro (Nihon U.), S. Sugita, M. Serino (AGU), T. Mihara (RIKEN), W. Iwakiri (Chuo U.), M. Nakajima, K. Asakura, K. Seino (Nihon U.), T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), Y. Tsuboi, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, T. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
We further report on MAXI observations of MAXI J0709-159 discovered by MAXI/GSC on 2022 January 25 (Serino et al. ATel #15178). Using the source position determined by NICER (Iwakiri et al. ATel #15181), we reconstructed light curves of MAXI/GSC, and found that the X-ray enhancement at 10:42 UT was not a short burst-like event, but a long-lasting flaring event continuing longer than the MAXI scan for about 50 s. Furthermore, we found another flaring event from the source at 13:48 UT on January 25, about 6 min before the NICER detection during the raster scan observations. Rapid time variations on timescales of seconds are observed in both flares, though it is not statistically confirmed, yet. The GSC energy spectrum of the first flaring event is well represented by an absorbed power-law model with a photon index of 1.9 (+0.6/-0.5) and an equivalent hydrogen column density nH of 3.0 (+5.2/-3.0) e22 cm-2, or a single blackbody model with a temperature of 1.6 +/- 0.2 keV. 2-10 keV fluxes using these models are 5.2 (+0.8/-0.7) e-9 erg/cm2/s and 5.4 +/-0.8 e-9 erg/cm2/s, respectively. An unabsorbed 2-10 keV flux of the power-law model is 6.2 (+2.7/-1.6) e-9 erg/cm2/s. On the other hand, the energy spectrum of the second flaring event is heavily absorbed. An absorbed power-law model fit gives a photon index of 2.5 (+1.1/-1.0) and nH = 5.4 (+3.9/-2.8) e23 cm-2, and an absorbed blackbody model fit a temperature of 2.3 (+0.8/-0.5) keV and nH = 2.3 (+2.8/-1.9) e23 cm-2. Absorbed 2-10 keV fluxes are 3.0 (+0.7/-0.6) e-9 erg/cm2/s and 3.2 (+0.7/-0.6) e-9 erg/cm2/s, respectively, and unabsorbed 2-10 keV fluxes are 16 (+41/-10) e-9 erg/cm2/s and 5.3 (+4.1/-2.0) e-9 erg/cm2/s, respectively. We note that the shape and fluxes of the two energy spectra above 5 keV are very similar. The observed energy spectra are similar to those of low-mass X-ray binaries hosting a neutron star in the hard state rather than those of X-ray binary pulsars. We note that the Be star HD 54786 is located in the error region obtained by NICER (ATel #15178). If HD 54786 is a companion star of MAXI J0709-159, the observed rapid variability suggests that the source is a kind of Super-giant Fast X-ray Transients (SFXTs), or a Cir X-1-like object. Further followup observations with multi-wavelengths are encouraged.
2022-01-27 22:27:00
x-ray,binary,black hole,neutron star,pulsar,star,transient
2022-01-27
22:27:00
2,309
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15,186
15,189
Outburst of comet C/2021 A1 (Leonard) on January 7, 2021
E. Jehin, Y. Moulane, J. Manfroid, M. Vander Donckt, F. Pozuelos, M. Ferrais, D. Hutsemekers (STAR Institute, University of Liege)
We report about an outburst of comet C/2021 A1 (Leonard) that happened between January 6 and 8, 00:00 UT 2021. Observations were carried on with TRAPPIST-South (code=I40, Chile) robotic telescopes about every night since Dec 20 until Jan 25, using broad band and cometary HB narrowband filters (Jehin el al. 2011). The production rates are computed at 10.000 km using a Haser Model (Vp=Vd=1km/s) (Haser 1957) and the dust production rates proxy A(0)f(rho) are estimated by profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). After five days around perihelion (Jan 3, 2022) of continuous decrease of the fluxes, there was a quick increase of about 1.5 magnitude in R band measured in an aperture of 5" centered on the nucleus on the images obtained on Jan 8, 00:15 UT (R=8.9+/-0.07) compared to those of Jan 6, 00:15 UT (R=10.5+/-0.08). The production rates of all the species were multiplied by about a factor of 4 with respect to Jan 6, as well as the A(0)fp. All the values peaked on Jan 9 UT and are reported below, with a Q(H2O) close to 2.5E29 s-1, the highest value measured on the whole period. The flux started to drop again on Jan 10, UT. C/2021 A1 (Leonard) Date UT=2022-01-09, r_h=0.63 au, Delta=1.12 au, DT=+6 days Q(OH)=(2.37+/-0.42) E29 s-1 Q(NH)=(1.07+/-0.35) E27 s-1 Q(CN)=(3.86+/-0.49) E26 s-1 Q(C2)=(4.41+/-0.61) E26 s-1 A(0)fp(BC)=9053+/-85 cm A(0)fp(RC)=12915+/-54 cm Notations: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, NH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, GC, RC are the blue, green and red dust continuum filters (Farnham et al. 2000). Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS under grant PDR T.0120.21. TRAPPIST-North is funded by the University of Liege, and performed in collaboration with the Cadi Ayyad University of Marrakesh. Observations were carried on from the ESO La Silla Paranal Observatory. We thank NASA, David Schleicher and the Lowell Observatory for the loan of the HB comet filters.
2022-01-28 03:50:00
optical,comet
2022-01-28
03:50:00
2,120
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15,187
15,190
Burst detection from FRB 20201124A using the Westerbork-RT1 25-m telescope
O. S. Ould-Boukattine (UvA), F. Kirsten (ASTRON, Chalmers), K. Nimmo (ASTRON, UvA), M. P. Snelders (UvA), J. W.T. Hessels (ASTRON, UvA), R. Blaauw (ASTRON), M. Gawronski (NCU, Torun), J. J. Sluman (ASTRON)
We report the detection of a fast radio burst from FRB 20201124A using the Westerbork-RT1 25-m telescope. Observations were done at a central frequency of 1323.49 MHz using a bandwidth of 128 MHz. We use a DM of 410.775 pc cm^-3, as determined in our analysis of bursts discovered using the Onsala telescope (ATel #14605, Kirsten et al., in prep.). Fluence: 32 +/- 3 Jy ms Arrival Time (MJD): 59602.992809162 at infinite frequency at the solar system barycentre (in TDB) using a DM of 410.775 pc cm^-3 and DM constant 4.14880568679703 GHz^2 cm^3 pc^-1 ms. FRB 20201124A has been described as one of the most active FRB sources to date, having burst rates as high as ~45 bursts/hour (Lee et al. 2021). The source entered a period of high activity in February-April 2021 (Lanman et al. 2021), and multiple studies have already been published, including a host galaxy association (Fong et al. 2021; Ravi et al. 2021), milliarcsecond localization (Nimmo et al. 2021, arXiv:2111.01600) and studies of polarization in the bursts (Hilmarsson et al. 2021; Kumar et al. 2021). Later in September 2021, multiple bursts were reported by CHIME/FRB and Effelsberg, possibly indicating the start of a new activity phase (ATel #14933). The detection of a new burst from FRB 20201124A with Westerbork-RT1 at 1323.49 MHz could indicate that the source is again starting a new activity cycle. We therefore encourage follow-up observations at all wavelengths. The observation reported here is part of a high-cadence multi-wavelength observation campaign of FRB 20201124A using multiple, 25-30-m dishes that are also part of the European VLBI Network (EVN). Our observing strategy has been described earlier in ATel #14605 and further details about our burst search pipeline can be found in Kirsten et al. (2021, DOI: 10.1038/s41550-020-01246-3). A detailed analysis of this burst and others detected in this campaign (ATel #14605) will be presented in a forthcoming paper (Kirsten et al., in prep.).
2022-01-29 05:39:00
radio,fast radio burst
2022-01-29
05:39:00
1,980
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0.006178517825901508, 0.03267735242843628, -0.07509499788284302, 0.008574388921260834, -0.0028434081468731165, -0.016930507495999336, -0.0010379436425864697, -0.05438249558210373, -0.04125324264168739, 0.019111504778265953, 0.018406350165605545, -0.11656598746776581, -0.08607321232557297, 0.045494649559259415, -0.0616711750626564, -0.09492156654596329, -0.05532553419470787, 0.0006972057744860649, 0.03659136965870857, -0.0388728603720665, -0.11218734085559845, -0.0013500300701707602 ]
15,188
15,191
VLT/X-Shooter spectroscopic observation of microlensing event ASASSN-22av/Gaia22ahy/AT2022aib
L. Wyrzykowski, P. Zielinski, M. Gromadzki, K. Kruszynska, K. A. Rybicki, N. Ihanec (Astronomical Observatory, University of Warsaw), S. T. Hodgkin (IoA Cambridge), I. Gezer (Konkoly Observatory), J. Corral-Santana (ESO), E. Bachelet (LCO)
We report on the spectroscopic observations of ASASSN-22av/Gaia22ahy/AT2022aib bright Galactic transient found by the All Sky Automated Survey for SuperNovae ASAS-SN (see Shappee et al. 2014) and independently discovered also by Gaia Science Alerts (Hodgkin et al. 2021), https://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia22ahy . Spectra were obtained on the night of 2022 January 26th with the ESO/VLT/X-Shooter instrument with slit widths 1.0'', 0.7'', 0.6'' yielding resolutions of 6000, 10500, 8000 in UBV, VIS and NIR, respectively. Spectrum shows clear absorption features corresponding to K3III star. This confirms the transient is a microlensing event. The visual arm of the spectrum and additional details can be obtained from the IAU Transient Name Server (TNS), https://www.wis-tns.org/object/2022aib . We thank ESO/VLT staff for support. Observations were carried out under ESO programme 108.22JZ, PI: Wyrzykowski.
2022-01-29 16:31:00
infra-red,optical,microlensing event,star,supernovae,transient
2022-01-29
16:31:00
922
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15,189
15,192
Subsequent detection of three more bursts from FRB 20201124A using the Westerbork-RT1 25-m telescope
O. S. Ould-Boukattine (UvA), F. Kirsten (ASTRON, Chalmers), K. Nimmo (ASTRON, UvA), M. P. Snelders (UvA), J. W.T. Hessels (ASTRON, UvA), R. Blaauw (ASTRON), M. Gawronski (NCU, Torun), R. J. van Ruiten (UvA), J. J. Sluman (ASTRON)
Following ATel #15190, we report the subsequent detection of three additional bursts from FRB 20201124A using the Westerbork-RT1 25-m telescope. Observations were done at a central frequency of 1323.49 MHz using a bandwidth of 128 MHz. We use a DM of 410.775 pc cm^-3, as determined in our analysis of bursts discovered using the Onsala telescope (ATel #14605, Kirsten et al., in prep.). Burst 1: Fluence: 58 +/- 5 Jy ms Arrival Time (MJD): 59603.754507227 Burst 2: Fluence: 37 +/- 5 Jy ms Arrival Time (MJD): 59603.799227754 Burst 3: Fluence: >771 +/- 70 Jy ms Arrival time (MJD): 59605.835730597 Arrival times are referenced to infinite frequency at the solar system barycentre (in TDB) using a DM of 410.775 pc cm^-3 and DM constant 4.14880568679703 GHz^2 cm^3 pc^-1 ms. The fluence of Burst 3 is only a lower limit as we are recording raw voltage data with 2-bit quantisation. This introduces quantisation noise lowering the measured value compared to the real fluence. This will be corrected for in a forthcoming paper. Likewise, a full spectro-polarimetric analysis at microsecond-resolution will be presented elsewhere. Bursts 1 and 2 are separated by roughly 1.07 hours in time. Burst 3 was detected in observations taken two days later. We spent 2.5 hours on source in each run, implying burst rates of ~1/hour above our detection limit of ~10 Jy ms. The subsequent detection of three additional bursts from FRB 20201124A, combined with the single detection on MJD 59602 (ATel #15190), strongly suggests that the source has started a new activity cycle. We therefore encourage follow-up observations at all wavelengths.
2022-01-29 21:22:00
radio,fast radio burst
2022-01-29
21:22:00
1,628
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15,190
15,193
NuSTAR identified MAXI J0709-159 as a Be X-ray binary with LY CMa
H. Negoro (Nihon U.), T. Mihara (RIKEN), S. Pike, B. Grefenstette (Caltech), W. Iwakiri (Chuo, U.), M. Nakajima (Nihon U.), and K. Gendreau (NASA/GSFC)
NuSTAR ToO observations of MAXI J0709-159 (ATel #15178, #15181, #15188) were performed from 00:21 to 11:21 UT on 2022 January 29 about 4 days after the MAXI detection of two bright flares. NuSTAR successfully detected the source at the position consistent with that of the Be star HD 54786 (aka LY CMa) within the systematic uncertainty of the NuSTAR position accuracy (~12", Lansbury et al. 2017, ApJ, 836, 99). The FPMA and FPMB spectra are well represented by an absorbed power-law model with a photon index of 2.0 +/- 0.3 and a equivalent hydrogen column density of 4.5 (+13.7/-4.5) e22. The unabsorbed 2-10 keV flux is 5 +/- 1 e-13 erg/cm2/s, corresponding to 2.5e33 erg/s taking account of the 6.4 kpc distance to HD 54786. NICER also observed the source quasi-simultaneously. The source count rate was consistent with background as was expected from the above NuSTAR result. The observed flux is lower than those of the two flares detected by MAXI by about four orders of magnitude. The decay timescale is faster than those of SFXTs, which typically decay by 2 to 3 orders of magnitudes a week (e.g., Romano et al. 2013, AdSpR, 52, 1593). The source has not been listed in any X-ray source catalog (e.g., The Swift-XRT point source catalog 1SXPS (Evans et al. 2014, ApJ, 210, 8), and The 7-year MAXI/GSC source catalog 3MAXI (Hori et al. 2018, ApJS, 235, 7)). Thus, these results imply that we have observed new SFXT-like activity in the MAXI J0709-159 and HD 54786 system. We also note that the power-law energy spectrum with a photon index of about 2 at a luminosity of about 1e33 erg/s is consistent with that of Be neutron star binaries in a quescent state (e.g., Mukherjee & Paul, 2005, A&A, 431, 667). Pulsations have not yet been detected from the source. Further followup observations are encouraged. We would like to thank the NuSTAR team for organizing the prompt observations.
2022-02-01 10:00:00
x-ray,binary,neutron star,star,transient
2022-02-01
10:00:00
1,894
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15,191
15,194
Optical follow-up of MAXI J0709-159
Roberto Nesci (INAF/IAPS-Roma)
In the announcement of two X-ray flares detected by MAXI (ATel #15181, #15188) of the source MAXI J0709-159, the star HD 54786 was indicated as a possible optical counterpart. I made therefore V,R,I (Cousins filters) imaging of the star on 2022-01-28, as well as a slitless spectrum at very low resolution (R=50) with the 30cm telescope of the Foligno Observatory (K56). Aperture photometry was made with IRAF apphot, using four nearby stars as comparisons, taken from the UCAC4 catalog. The star was at V=8.92+/-0.06; R=8.96+/-0.03; I=8.79+/-0.02. Noticeably, the star was about 0.5 mag brighter that the catalog values in all three bands. Optical V-band observations by Gerard Samolyk (AAVSO public lightcurve) performed one year ago (2021-01-15) showed a possible periodic variation with mean value V=9.05, peak to peak amplitude of 0.3 mag and 3 hours time scale. His mean value is in very good agreement with my finding. My (very poor) spectrum shows clearly an H-alpha emission line, as expected from its B1/2 Ie spectral type, with 23 A equivalent width. The identification of the optical counterpart of the X-ray source was confirmed by a NuSTAR observation in ATel 15193. Intranight optical follow-up to check a possible source periodicity is encouraged.
2022-02-01 16:42:00
optical,x-ray,binary,neutron star,star,transient
2022-02-01
16:42:00
1,263
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15,192
15,195
BAT/Scorpio-2 spectroscopic classification of Gaia microlensing event candidates
Zielinski P. (Institute of Astronomy, Nicolaus Copernicus University in Torun, Poland), Grokhovskaya A., (Special Astrophysical Observatory & Institute of Applied Astronomy, Russian Academy of Sciences, Russia), Shablovinskaya E., Moiseev A. (Special Astrophysical Observatory, Russian Academy of Sciences, Russia), Gromadzki M., Wyrzykowski L., Ihanec N., Gezer I., Jablonska, M., Kruszynska K., Rybicki K. A., Mikolajczyk P. (Warsaw University Astronomical Observatory, Poland), Maskoliunas M., Pakstiene E., Zdanavicius J. (Institute of Theoretical Physics and Astronomy, Vilnius University, Lithuania)
We report on spectroscopic observations of 4 candidates for microlensing events detected by the Gaia Science Alerts program (http://gsaweb.ast.cam.ac.uk/alerts). The spectroscopic data were collected by 6-m BAT telescope (https://relay.sao.ru/Doc-en/Telescopes/bta/descrip.html) equipped with Scorpio-2 and E2V261-84 CCD detector (Afanasiev & Moiseev, 2011). The observations were carried out in long-slit mode with diffraction grating VPHG940 at 600 nm and LP425 filter (wavelength range 425 – 850 nm for Gaia18arn, Gaia19flk, Gaia21eob) and VPHG1200 at 540 nm (spectral range 365 – 725 nm for Gaia19dqe) which provides resolution power of R~800-1000. Based on that, none of these targets was classified as microlensing event. The spectra are available on IAU's Transient Name Server. Notes: (1) strong Halpha emission, reddened Be star. (2) core emission in Halpha visible, probably Be star. (3) Balmer series in absorption, but Halpha line exhibits core emission, early-type continuum shape, Be star. (4) emission in the cores of Balmer lines visible, reddened Be star or YSO. Acknowledgments. Observations with the SAO RAS telescopes are supported by the Ministry of Science and Higher Education of the Russian Federation (including agreement No05.619.21.0016, project ID RFMEFI61919X0016). This project has received funding from the EU Horizon 2020 research and innovation programme under grant agreement No. 101004719, as well as Polish NCN DAINA grant 2017/27/L/ST9/03221 and Research Council of Lithuania grant No. S-LL-19-2. We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts).
2022-02-02 02:01:00
optical,microlensing event,star,transient,variables,young stellar object
2022-02-02
02:01:00
1,647
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15,193
15,196
Fermi LAT Detection of a New Gamma-ray Transient in the Galactic Plane: Fermi J0614+1713
I. Mereu (INFN Perugia), C. C. Cheung (NRL), on behalf of the Fermi-LAT collaboration
On Jan 31, 2022, the Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, observed gamma-ray emission from a new transient source, Fermi J0614+1713. Preliminary analysis indicates that this source was in an elevated gamma-ray emission state with a daily averaged gamma-ray flux (E >100 MeV) of (1.2 +/- 0.3) x 10^-6 ph cm^-2 s^-1, and a photon index, Gamma = 2.2 +/- 0.2. The best-fit location of this gamma-ray source (RA = 93.63 deg, Decl. = 17.23 deg; J2000) has a 95% containment radius of 0.26 deg (errors are statistical only). This source is located near the Galactic plane (l, b = 193.46 deg, -0.07 deg), and is not in any published LAT catalog and in the past has not been detected by AGILE or EGRET. There is no clear counterpart to the LAT transient: the known Swift-BAT source, Swift J0614.0+1709, is located within the LAT 95% confidence localization region but is identified as a magnetic CV (Halpern & Thorstensen 2015 AJ, 150, 170) and thus unlikely to be related. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Isabella Mereu (mereuisabella at gmail.com). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-02-02 11:06:00
gamma ray,transient,request for observations
2022-02-02
11:06:00
1,570
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15,194
15,197
Detection of two bright bursts from FRB20201124A with Apertif at the Westerbork Synthesis Radio Telescope.
Pikky Atri (ASTRON), Anna Bilous (ASTRON), Joeri van Leeuwen (ASTRON), Yogesh Maan (NCRA), Ines Pastor-Marazuela (UvA, ASTRON), Emily Petroff (UvA, McGill) and Samayra Straal (NYUAD), on behalf of the ARTS and Apertif Teams
The ALERT survey for Fast Radio Bursts using the Apertif system on WSRT (Maan & van Leeuwen 2017, Oostrum et al. 2020) targets both new and known-FRB fields (Pastor-Marazuela et al. 2021). During a 3-hr pointing including the location of FRB20201124A (ATel #14497) starting Feb 1, 19:55:55 UTC, the ARTS real-time detection system (van Leeuwen et al. 2022) blindly detected two bright bursts. The bursts agreed with the position, dispersion measure, and recent activity (see, e.g. ATel #15192) of FRB20201124A; no other FRBs were found in this observation. The burst that occurred at MJD 59611.83542063 (barycentric) had a fluence of 156 +/- 31 Jy ms. The burst at MJD 59611.91172950 had a fluence of 35 +/- 7 Jy ms. Both bursts consist of ~4 major components, and display rich spectro-temporal structure that best aligns at a dispersion measure of 410.9 +/- 0.2 pc/cm^3. The components drift downward in frequency, through the entire 300 MHz bandwidth centered on 1370 MHz. Interstellar scintillation is evident and consistent with bursts previously seen from this source (Main et al. 2021). After this week Apertif will cease operations. van Leeuwen, J., et al. 2022, Astronomy & Astrophysics, in prep. Maan, Y., & van Leeuwen, J. 2017, Proc. URSI GASS, arXiv:1709.06104 Main, R. A., et al. 2021, arXiv:2107.14339 Oostrum, L. C., et al. 2020, Astronomy & Astrophysics, 635, A61 Pastor-Marazuela, I., et al. 2021, Nature, 596, 505
2022-02-03 23:09:00
radio,fast radio burst
2022-02-03
23:09:00
1,431
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15,195
15,198
H-alpha observations of M31 nova candidates AT2022alr and AT2022uz
A. Valcheva (Sofia University, Bulgaria), M. Minev (Sofia University; IA with NAO, BAS, Bulgaria), I. Dimitrova (Sofia University; IA with NAO, BAS, Bulgaria), E. Ovcharov (Sofia Univeristy, Bulgaria), P. Nedialkov (Sofia University, Bulgaria)
We report H-alpha photometry of two recent nova candidates in M31 - AT 2022alr (= PNV J00424699+4115532) and AT 2022uz (= XM63MZ)(= PNV J00430928+4116013). The observations in narrowband H-alpha (FWHM of 30Å) were performed with the FoReRo2 focal reducer at the 2m RCC telescope at the NAO Rozhen, Bulgaria on 2022 Jan 31.712 UT under nonphotometric weather conditions (FWHM ~ 3 arcsec). Photometric magnitudes were obtained from 5x300 sec co-added frames (H-alpha image can be found here). Additional B-magnitudes are also available. AT 2022alr was discovered by Jiangao Ruan, Mi Zhang and Xing Gao (Xingming Obs) on 2022 Jan 25.556 UT very close at 30.1" east and 15.3" south of the center of M31. Our observations show that the transient is very bright in H-alpha with a magnitude of 14.89±0.03 and this confirms the object classification as a nova. B-magnitude of the nova is 17.27±0.03 mag (5x300 sec; 2022 Jan 31.712 UT). We have also detected the transient AT 2022uz discovered on 2022 Jan 16.587 UT by M. Zhang and X. Gao. Independent discovery was reported by Hornoch et al. (ATel #15170) who designated the slowly brightening transient as M31N 2022-01a. AT 2022uz is visible in H-alpha and have a magnitude of 17.66 ±0.08 mag. Obtained B-magnitude is 18.46 ±0.02 mag (5x300 sec; 2022 Jan 31.712 UT).
2022-02-04 04:40:00
optical,nova,transient
2022-02-04
04:40:00
1,311
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15,196
15,199
Improved Localization of the Fermi-LAT Gamma-ray Transient in the Galactic Plane: Fermi J0614+1713
I. Mereu (INFN Perugia), C. C. Cheung (NRL), S. Ciprini (ASI Space Science Data Center, Roma, & INFN Roma Tor Vergata), on behalf of the Fermi-LAT collaboration
ATel #15196 reported the Fermi-LAT detection of Fermi J0614+1713, a new gamma-ray transient in the Galactic plane on Jan 31, 2022. Preliminary follow-up analysis of earlier LAT data from Jan 27-30 indicates this source was detected at >3-sigma significance in 1-day intervals on Jan 29 and 30, and in the last 6 hr interval of Jan 28 (18:00-24:00). The source was not significantly detected after the initially reported detection in 1-day intervals (i.e., on Feb 1, 2 and 3). Summing the detections from the 3.25 days beginning on the last 6 hr interval of Jan 28 resulted in an improved localization for the gamma-ray source, with a best-fit (J2000) position of RA = 93.48 deg, Decl. = 17.18 deg (Galactic coordinates: l, b = 193.43 deg, -0.22 deg), with a 95% containment radius of 0.17 deg (errors are statistical only). The averaged gamma-ray flux (E >100 MeV) was (8.7 +/- 1.8) x 10^-7 ph cm^-2 s^-1, with a photon index, Gamma = 2.28 +/- 0.13. The magnetic CV, Swift J0614.0+1709, noted in ATel #15196 remains located within the improved LAT localization. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Isabella Mereu (mereuisabella at gmail.com). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2022-02-04 23:27:00
gamma ray,transient,request for observations
2022-02-04
23:27:00
1,609
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-0.06024761125445366, 0.053449664264917374, 0.0041796681471168995, -5.722600349145068e-8, -0.036141395568847656, 0.022468864917755127, -0.06101430207490921, 0.05901084467768669, 0.054965391755104065, -0.07685604691505432, -0.03075704723596573, 0.03826422616839409, -0.01871267706155777, -0.00015928540960885584, 0.03526974469423294, 0.054826121777296066, 0.06496536731719971, -0.11804479360580444, -0.00035526632564142346, -0.026075419038534164, -0.016340799629688263, -0.03706302121281624, -0.035508062690496445, 0.03917607665061951, 0.09823407977819443, 0.03317562863230705, 0.09347186982631683, 0.0034999370109289885, -0.0017739747418090701, -0.004487651865929365, -0.06773582100868225, 0.08746329694986343, 0.009110926650464535, -0.11420360952615738, -0.01945548504590988, 0.007486018817871809, 0.014979248866438866, -0.05988393723964691, -0.07617606967687607, 0.013164261355996132, -0.017583584412932396, -0.022369783371686935, 0.10106638073921204, 0.08545820415019989, -0.010571975260972977, -0.028586259111762047, 0.011801399290561676, 0.02009059116244316, -0.08679548650979996, 0.004910858813673258, -0.01485874317586422, -0.08976487070322037, -0.0057374257594347, -0.02085205353796482, -0.03677735477685928, -0.02390507236123085, -0.030605515465140343, -0.09682321548461914, -0.015581757761538029, -0.02144204080104828, -0.027407601475715637, -0.02472020871937275, 0.02876218967139721, -0.026027966290712357, 0.028053440153598785, -0.08565724641084671, -0.14375047385692596, -0.028544330969452858 ]
15,197
15,200
Observations of the new gamma-ray transient Fermi J0614+1713 with VERITAS
John Quinn (University College Dublin) for the VERITAS Collaboration
The VERITAS Collaboration reports upper limits from 4 hours of observations of the new gamma-ray transient Fermi J0614+1713 announced in ATel #15196. VERITAS observations started on February 2 at 02:50 UTC and continued until 07:00 UTC. Preliminary analysis of the VERITAS data at the best-fit position reported by the Fermi-LAT collaboration in the follow-up ATel #15199 (RA = 93.48 deg., Decl. = 17.18 deg.; J2000) results in no detection, corresponding to a flux upper limit at 99% confidence level of F(> 200 GeV) < 4.2 × 10-12 cm-2 s-1, or 2% of the Crab Nebula flux. Additionally, no very high-energy gamma-ray source is detected in the 0.17 deg. radius error circle (95%) of Fermi J0614+1713. Questions regarding the VERITAS observations should be directed to John Quinn (john.quinn@ucd.ie). VERITAS (the Very Energetic Radiation Imaging Telescope Array System) is located at the Fred Lawrence Whipple Observatory in southern Arizona, USA, and is most sensitive to gamma rays between ∼85 GeV and ∼30 TeV. For further information see the VERITAS web site.
2022-02-05 02:58:00
gamma ray,tev,vhe,transient
2022-02-05
02:58:00
1,062
[ -0.022407934069633484, -0.03657899051904678, 0.018108783289790154, -0.027100978419184685, 0.0567009411752224, -0.0593000091612339, -0.03159583732485771, 0.09331704676151276, -0.04510147124528885, -0.05146054923534393, 0.001601159106940031, -0.03187775984406471, 0.08313288539648056, -0.0008801555377431214, -0.009020188823342323, -0.046221066266298294, 0.11026491224765778, -0.06404420733451843, 0.042286135256290436, 0.07036430388689041, -0.05002759024500847, 0.07690539211034775, -0.012693138793110847, -0.044153470546007156, 0.07740926742553711, 0.0006379047990776598, 0.02042020484805107, -0.034016795456409454, -0.019861940294504166, -0.03156813234090805, -0.019631240516901016, 0.030198203399777412, -0.06668325513601303, 0.020939642563462257, 0.016697129234671593, 0.01153641939163208, 0.004348906688392162, 0.004650878254324198, -0.02107798308134079, -0.012694727629423141, -0.027394207194447517, 0.020849812775850296, 0.0005227061337791383, 0.007069671992212534, 0.00467708520591259, 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15,198
15,201
No bright optical counterpart to the GeV transient Fermi J0614+1713
Kirill Sokolovsky (MSU/SAI MSU), Olga Smolyankina (Observatory of Omsk CPCT), Stanislav Korotkiy (Ka-Dar Obs./Astrovert), Elias Aydi, Laura Chomiuk, Adam Kawash, Jay Strader (MSU)
The new Galactic plane gamma-ray transient Fermi J0614+1713 was observed with Fermi/LAT between 2022-01-28 and 2022-01-31 (ATel #15196, #15199, #15200). We imaged the field of Fermi J0614+1713 with the NMW wide-field optical camera ( http://scan.sai.msu.ru/nmw/ ) between 2022-02-03 17:37 and 22:47 UTC obtaining 14x20sec exposures. We found no new source brighter than V~15 in the vicinity of the LAT error circle after comparing the NMW stack to the archival DSS-II Red image. We also imaged the field of Fermi J0614+1713 with the 4.1m SOAR telescope between 2022-02-02 05:31 and 05:45. Unfortunately, the mosaicing was interrupted by passing clouds when only a quarter of the improved Fermi error circle was covered. No new source was found in the covered region down to V~19. The hard X-ray emitting intermediate polar candidate Swift J0614.0+1709 (Halpern & Thorstensen, 2015, AJ,150, 170) is outside the area imaged with SOAR and below the NMW image limit.
2022-02-05 16:24:00
optical,x-ray,gamma ray,transient
2022-02-05
16:24:00
963
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