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arXiv_src_0001_001/astro-ph0001011 | What can BeppoSAX tell us about short GRBs: An update from the Subsecond GRB Project |
We present some statistical considerations on the BeppoSAX hunt for subsecond GRBs at the Scientific Operation Center. Archive analysis of a BATSE/SAX sub-sample of bursts indicates that the GRB Monitor is sensitive to short ($\le$
2 sec) events, that are in fact $\approx$ 22$\%$ of the total. The non-detection of corresponding prompt X-ray counterparts to short bursts in the Wide Field Cameras, in about 3 years of operations, is discussed: with present data no implications on the X-to-$\gamma$-ray spectra of short vs long GRBs may be inferred. Finally, the status of searching procedures at SOC is reviewed.
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"caption": "Duration distribution of short GRBs. The solid line is the common BeppoSAX/Batse Sample distribution, the dashed one is the normalized 4B Batse distribution, for comparison.",
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arXiv_src_0001_001/astro-ph0001016 | The Space Density of Primordial Gas Clouds near Galaxies and Groups and their Relation to Galactic HVCs |
The Arecibo \hi\ Strip Survey probed the halos of $\sim$300 cataloged galaxies and the environments of $\sim$14 groups with sensitivity to neutral hydrogen masses $\geq 10^{7}~\msol$. The survey detected no objects with properties resembling the High Velocity Clouds (HVCs) associated with the Milky Way or Local Group. If the HVCs were typically
$\mhi=10^{7.5}~\msol$ objects distributed throughout groups and galaxy halos at distances of $\sim$1~Mpc, the survey should have made $\sim$70 HVC detections in groups and $\sim$250 detections around galaxies. The null detection implies that HVCs are deployed at typical distances of $\leq$200~kpc from the galaxies or group barycenters. If the clouds are in virial equilibrium, their average dark matter fraction must be 98\% or higher.
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"caption": "{Top panel:} mass function of the Local Group (LG). The points show the space density of LG members containing , after correcting for incompleteness. The solid line shows the field from Zwaan et al. (1997), scaled vertically so as to fit the points. The dotted line is a with a steep upturn at the low mass end, recently proposed by Schneider et al. (1998) {Second panel:} mass functions for extragalactic HVCs. The dark histogram shows the space density of BSTHB HVCs if they are put at the critical radii for gravitational stability. The unshaded histogram shows the effect of a baryon to total mass ratio $f$ varying from cloud to cloud. The lighter shaded histogram corresponds to BB HVCs, all at the same distance of 1 Mpc. Lines are as in top panel. {Third panel:} mass function for BSTHB HVCs for different values $f$ (from right to left: $f$=0.2, 0.1, 0.05, 0.025, 0.0125). The HVC is consistent with the field if $f\\leq 0.02$ and the median distance $\\leq 200$ kpc. {Bottom panel:} Distribution of the expected detections in the for the BSTHB population. The light grey histogram corresponds to clouds surrounding galaxies, the dark grey histogram represents clouds in galaxy groups. See section 4 for explanation.",
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"caption": "Illustration of the two surveys strips and the distribution of spheres with radii of 1 Mpc around known galaxies (thin circles) and galaxy groups (thick circles). The grey areas indicate the Zone of Avoidance where $|b|<10^\\circ$. The solid horizontal lines show the paths of the Arecibo beam.",
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arXiv_src_0001_001/astro-ph0001018 | DO AGB STARS DIFFER CHEMICALLY FROM RGB STARS IN GLOBULAR CLUSTERS? | The recent improvements in globular cluster colour-magnitude diagrams, coupled with an increase in large-sample spectroscopic abundance studies of cluster giants, finally allow some attempts at a statistically meaningful comparison of the chemical compositions of red giant branch and asymptotic branch cluster stars. We review some of the extant data here, concluding that in a few clusters the AGB stars show on average smaller amounts of high-temperature proton-capture synthesis products (low oxygen, high sodium and aluminum) at their surfaces than do the first-ascent RGB stars. This suggests that those RGB stars with envelopes that have been enriched with proton-capture material also have high helium contents. Such stars after the He-flash then take up residence on the bluest parts of the HB (as a consequence of their high envelope helium), probably never to return to the AGB during subsequent evolutionary stages. | [
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"caption": "Simple boxplots illustrating CN bandstrength ranges in RGB and AGB stars of NGC 6752, M13, and M4 are shown. For all of the individual abundance boxes, the horizontal line inside a box indicates the median value of $\\delta$S(3839). The vertical boundaries of a box show the interquartile range (the middle 50% of the data). The vertical tails extending from the boxes indicate the total range of $\\delta$S(3839), excluding outliers. Mild outliers (those between 1.5 and 3 times the interquartile range) are denoted by open circles. No severe outliers (those greater than 3 times the interquartile range) are present in these data. The number of stars included in each boxplot is noted in parentheses. The basic data (estimates of CN line blocking index S(3839)) were taken from the following sources: (a) NGC6752: Norris (1981), and we have used their suggested relationship of the lower limit of S(3839) to V magnitude to compute the relative CN bandstrengths $\\delta$S(3839); (b) M13: converted photometric CN index $m$(CN) values obtained by Suntzeff (1981). We first removed the variation of the index due to position in the c-m diagram using Suntzeff's formula, and then converted the results to $\\delta$S(3839) values using the relationship we found for the NGC 6752 stars in common to the $m$(CN) values presented by Langer (1992) and the $\\delta$S(3839) values of Norris (1981). (c) M4: Norris (1981) or Suntzeff & Smith (1991), or the mean of both, using Norris' suggested relationship of the lower limit of S(3839) to V magnitude.",
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arXiv_src_0001_001/astro-ph0001034 | First Light Measurements of Capella with the Low Energy Transmission Grating Spectrometer aboard the Chandra X-ray Observatory |
We present the first X-ray spectrum obtained by the Low Energy Transmission Grating Spectrometer (LETGS) aboard the Chandra X-ray Observatory. The spectrum is of Capella and covers a wavelength range of 5--175~\AA\ (2.5--0.07~keV). The measured wavelength resolution, which is in good agreement with ground calibration, is
$\Delta \lambda \simeq$ 0.06~\AA\ (FWHM). Although in-flight calibration of the LETGS is in progress, the high spectral resolution and unique wavelength coverage of the LETGS are well demonstrated by the results from Capella, a coronal source rich in spectral emission lines. While the primary purpose of this letter is to demonstrate the spectroscopic potential of the LETGS, we also briefly present some preliminary astrophysical results. We discuss plasma parameters derived from line ratios in narrow spectral bands, such as the electron density diagnostics of the He-like triplets of carbon, nitrogen, and oxygen, as well as resonance scattering of the strong Fe~XVII line at 15.014~\AA. | [
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arXiv_src_0001_001/astro-ph0001010 | Feedback Processes in the Early Universe |
Feedback effects due to massive stars and supernovae in the first objects are shown to strongly regulate both galaxy formation/evolution and the reionization process. Here we review the most important ones in some detail. We discuss how Type II supernovae can be used as tracers of the first objects and detected with NGST, for which we predict supernova number counts including the effects of gravitational lensing. Preliminary results on the formation of dust in the ejecta of supernovae of primordial composition are also presented. We finally turn to the consideration of the process of inhomogeneous reionization due to primordial stellar sources by means of high resolution numerical simulations, allowing for a self-consistent treatment of the above feedback processes. These simulations allow us to draw conclusions on the evolution and epoch of reionization and about the fate of reionizing objects. We conclude that a large fraction ($\approx 99$\%) of collapsed objects must be dark at redshift around eight. | [
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arXiv_src_0001_001/astro-ph0001030 | A Hard Medium Survey with ASCA.III.: a Type 2 AGN revealed from X-ray spectroscopy
\thanks{Based on observations performed at the European Southern Observatory, Paranal, Chile} | In this paper we report the discovery of an hard X-ray selected Type 2 Seyfert galaxy and we present and discuss its X-ray and optical spectrum together with the radio to X-ray energy distribution. The X-ray source - AXJ2254+1146 - is part of the ASCA Hard Serendipitous Survey (HSS). What makes this discovery particularly noteworthy is the fact that the Type 2 classification of this Seyfert galaxy has resulted directly from the X-ray data and has been confirmed by optical spectroscopy only subsequently. The X-ray spectrum of AXJ2254+1146 is best described by a model consisting of an unresolved Gaussian line at $6.43\pm 0.1$ keV plus the so called ``leaky-absorber" continua having an intrinsic power law photon index of $\Gamma$ = $2.51^{2.76}_{2.17}$
(1 $\sigma$ confidence interval). The best fit values of the absorbing column density ($N_H$ =
$1.85^{2.24}_{1.47} \times 10^{23}$ cm$^{-2}$), of the line equivalent width ($0.6^{0.84}_{0.36}$ keV) and of the scattering fraction
($0.7^{1.4}_{0.1} \%$), lead us to classify it as a Type 2 AGN from an X-ray point of view. Inspection of the POSS II image reveals the presence, within the ASCA X-ray error circle, of the nearby Sbc spiral galaxy UGC 12237
($m_{B_o}=14.26$) that, even on positional ground considerations alone, is the most likely optical counterpart of AXJ2254+1146. Subsequent optical spectroscopy of UGC 12237 has confirmed its Seyfert 2 optical nature. | [
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arXiv_src_0001_001/astro-ph0001061 | OBSERVATIONAL TESTS FOR THE COSMOLOGICAL PRINCIPLE AND WORLD MODELS |
We review observational tests for the homogeneity of the Universe on large scales. Redshift and peculiar velocity surveys, radio sources, the X-Ray Background, the Lyman-$\alpha$
forest and the Cosmic Microwave Background are used to set constraints on inhomogeneous models and in particular on fractal-like models. Assuming the Cosmological Principle and the FRW metric, we estimate cosmological parameters by joint analysis of peculiar velocities, the CMB, cluster abundance, IRAS and Supernovae. Under certain assumptions the best fit density parameter is $\Omega_{m} = 1 - \lambda \approx 0.4 $. We present a new method for joint estimation by combining different data sets in a Bayesian way, and utilising `Hyper-Parameters'.
\footnote{
Review talk, to appear in the proceedings of the NATO ASI, Isaac Newton Institute, Cambridge, July 1999, ed. R. Crritenden \& N, Turok Kluwer
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"caption": "The distribution of radio source from the 87GB and PMN surveys projected on the sky. This is an Aitoff projection in Equatorial coordinates (from Baleisis et al. 1998).",
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"caption": "A compilation of density fluctuations on different scales from various observations: a galaxy survey, deep radio surveys, the X-ray Background and Cosmic Microwave Background experiments. The measurements are compared with two popular Cold Dark Matter models (with normalization $\\sigma_8=1$ and shape parameters $\\Gamma=0.2$ and $0.5$). The Figure shows mean-square density fluctuations $({ {\\delta \\rho} \\over \\rho })^2 \\propto k^3 P(k)$, where $k=1/\\lambda$ is the wavenumber and $P(k)$ is the power-spectrum of fluctuations. The open squares at small scales are estimates from the APM galaxy catalogue (Baugh & Efstathiou 1994). The elongated 'boxes' at large scales represent the COBE 4-yr (on the right) and Tenerife (on the left) CMB measurements (Gawiser & Silk 1998). The solid triangles and crosses represent amplitudes derived from the quadrupole of radio sources (Baleisis et al. 1998) and the quadrupole of the XRB (Lahav et al. 1997; Treyer et al. 1998). Each pair of estimates corresponds to assumed shape of the two CDM models. (A compilation from Wu, Lahav & Rees 1999).",
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arXiv_src_0001_001/astro-ph0001048 | The 24-Hour Night Shift:\\
Astronomy from Microlensing Monitoring Networks |
Scores of on-going microlensing events are now announced yearly by the microlensing discovery teams OGLE, MACHO and EROS. These early warning systems have allowed other international microlensing networks to focus considerable resources on intense photometric --- and occasionally spectroscopic --- monitoring of microlensing events. Early results include:
metallicity measurements of main sequence Galactic bulge stars; limb darkening determinations for stars in the Bulge and Small Magellanic Cloud; proper motion measurements that constrain microlens identity; and constraints on Jovian-mass planets orbiting (presumably stellar) lenses. These results and auxiliary science such as variable star studies and optical identification of gamma ray bursts are reviewed.
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arXiv_src_0001_001/astro-ph0001075 | The first galaxies: clues from element abundances | {} It has recently become possible to measure directly the abundances of several chemical elements in a variety of environments at redshifts up to $z \simeq 5$. In this review I summarise the latest observations of Lyman break galaxies, damped Lyman alpha systems and the Lyman alpha forest with a view to uncovering any clues which these data may offer to the first episodes of star formation. The picture which is emerging is one where the universe at $z = 3$ already included many of the components of today's galaxies---even at these early times we see evidence for Populations I and II stars, while the `smoking gun'
for Population III objects may be hidden in the chemical composition of the lowest density regions of the IGM, yet to be deciphered.
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"caption": "Emission line widths in Lyman break galaxies at $z \\simeq 3$ and in local galaxies. The horizontal bar spans the range of widths at 20% peak intensity of [O III] lines in a dozen Lyman break galaxies, while the vertical lines at each end of the bar indicate the range of luminosities sampled (Pettini {et al.} in preparation). The light-coloured triangles are the most reliable H$\\beta$ measurements for H II galaxies by Melnick, Terlevich, & Terlevich (2000), while the filled dots are [O II] measurements in a variety of nearby star forming galaxies by Kobulnicky & Gebhardt (2000). Also shown is the relation for local spirals based on H I 21cm rotation curves (broken line) and its $3 \\sigma$ limits (dotted lines - Pierce & Tully 1992). A $H_0 = 50$ km s$^{-1}$ Mpc$^{-1}$, $\\Omega = 1$ cosmology was adopted.\n",
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"caption": "C IV column density distribution in Q1422+231 at $\\langle z \\rangle \\simeq 3.15$ (reproduced from Ellison {et al.} 2000); $f$($N$) is the number of C IV systems per column density interval and per unit redshift path. The filled circles are the data grouped into bins of 0.3 in log $N$(C IV) for display purposes. The line shows the best fitting power-law slope $\\alpha = 1.44$, assuming the distribution to be of the form $f{\\rm (}N{\\rm )} dN = B N^{-\\alpha} dN$. The open circles show the values corrected for incompleteness at the low column density end; the correction factors were estimated with the aid of simulations which showed that only $\\sim 43$% and $\\sim 23$% of C IV lines with log $N$(C IV) = 12.05 and 11.75 respectively are typically recovered from the data. Once these correction factors are introduced, there is no indication of a turnover in the column density distribution down to the lowest values of $N$(C IV) reached up to now.",
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arXiv_src_0001_001/astro-ph0001083 | Observation of Microlensing towards the Galactic Spiral Arms.
{\sc EROS II} 3 year survey
\thanks{This work is based on observations made at the European Southern Observatory, La Silla, Chile.}
|
We present an analysis of the light curves of 9.1 million stars observed during three seasons by {\sc EROS} (Exp\'erience de Recherche d'Objets Sombres), in the Galactic plane away from the bulge. Seven stars exhibit luminosity variations compatible with gravitational microlensing effects due to unseen objects. The corresponding optical depth, averaged over four directions, is $\bar\tau = 0.45^{+0.24}_{-0.11} \times 10^{-6}$. While this value is compatible with expectations from simple galactic models under reasonable assumptions on the target distances, we find an excess of events with short timescale towards the direction closest to the Galactic Centre. | [
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arXiv_src_0001_001/astro-ph0001078 | Radiative Processes and Geometry of Spectral States of Black-hole Binaries |
I review radiative processes responsible for X-ray emission in the hard (low)
and soft (high) spectral states of black-hole binaries. The main process in the hard state appears to be thermal Comptonization (in a hot plasma) of blackbody photons emitted by a cold disk. This is supported by correlations between the spectral index, the strength of Compton reflection, and the peak frequencies in the power-density spectrum, as well as by the frequency-dependence of Fourier-resolved spectra. Spectral variability may then be driven by the variable truncation radius of the disk. The soft state appears to correspond to the smallest truncation radii. However, the lack of high-energy cutoffs observed in the soft state implies that its main radiative process is Compton scattering of disk photons by nonthermal electrons. The bulk-motion Comptonization model for the soft state is shown to be ruled out by the data.
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arXiv_src_0001_001/astro-ph0001087 | Testing population synthesis models with globular cluster colors | We have measured an extensive set of $UBVRIJHK$ colors for M31 globular clusters \citep{b00}. We compare the predicted simple stellar population colors of three population synthesis models to the intrinsic colors of Galactic and M31 globular clusters. The best-fitting models fit the cluster colors very well -- the weighted mean color offsets are all $<0.05$ mag. The most significant offsets between model and data are in the $U$ and
$B$ passbands; these are not unexpected and are likely due to problems with the spectral libraries used by the models. The metal-rich clusters (${\rm [Fe/H]}\gtrsim-0.8$) are best fit by young (8 Gyr) models, while the metal-poor clusters are best fit by older (12--16 Gyr) models. If this range of globular cluster ages is correct, it implies that conditions for cluster formation must have existed for a substantial fraction of the galaxies' lifetimes. | [
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arXiv_src_0001_001/astro-ph0001080 | X-ray and optical observations of three clusters of galaxies:
Abell 901, Abell 1437, and Abell 3570\thanks{Partly based on observations collected at the European Southern Observatory} |
We analyse three clusters of galaxies, Abell 901 (z=0.17), Abell 1437
(z=0.13) and Abell 3570 (z=0.037). They have low to intermediate X-ray fluxes and an irregular morphology in the ROSAT All-Sky Survey (RASS). These clusters are chosen to test the abilities and limitations of the RASS in terms of cluster fluxes and cluster morphologies. Therefore some ``worst'' cases are used here. X-ray observations with the ROSAT/HRI and optical spectroscopic observations are carried out. The ROSAT/HRI observations, which have a much better spatial resolution than the RASS, reveal in two of the three cases a significantly different morphology than seen in the RASS. The reasons are point sources which could not be resolved in the RASS and were therefore confused with the cluster emission. For A3570 we could confirm the relaxed state of the cluster by the optical determination of a small velocity dispersion. In the cluster with the lowest flux (Abell 901) the countrate measurement is strongly affected by point sources, in the two other cases the countrate measurements of the RASS are reliable, i.e. they are reproduced by the ROSAT/HRI measurement. We conclude that for clusters with a flux of a few times $10^{-12}$
erg/cm$^2$/s or smaller, which show at the same time a non-relaxed morphology, the flux measurement of the RASS can be seriously affected by fore- or background sources. We point out that an all-sky survey of a second ABRIXAS mission would provide a much clearer source distinction for low-flux clusters and thus a much improved countrate determination. \keywords{Galaxies: clusters: individual: Abell 901, Abell 1437, Abell 3570 -- intergalactic medium -- Cosmology: observations -- dark matter -- X-rays: galaxies
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arXiv_src_0001_001/astro-ph0001095 | Phase Lag and Coherence Function of X-ray emission from Black Hole Candidate XTE J1550-564 |
We report the results from measuring the phase lag and coherence function of X-ray emission from black hole candidate (BHC) XTE J1550-564. These X-ray temporal properties have been recognized to be increasingly important in providing important diagnostics of the dynamics of accretion flows around black holes. For XTE J1550-564, we found significant hard lag --- the X-ray variability in high energy bands {\em lags} behind that in low energy bands --- associated both with broad-band variability and quasi-periodic oscillation
(QPO). However, the situation is more complicated for the QPO: while hard lag was measured for the first harmonic of the signal, the fundamental component showed significant {\em soft} lag. Such behavior is remarkably similar to what was observed of microquasar GRS 1915+105. The phase lag evolved during the initial rising phase of the 1998 outburst. The magnitude of both the soft and hard lags of the QPO increases with X-ray flux, while the Fourier spectrum of the broad-band lag varies significantly in shape. The coherence function is relatively high and roughly constant at low frequencies, and begins to drop almost right after the first harmonic of the QPO. It is near unity at the beginning and decreases rapidly during the rising phase. Also observed is that the more widely separated the two energy bands are the less the coherence function between the two. It is interesting that the coherence function increases significantly at the frequencies of the QPO and its harmonics. We discuss the implications of the results on the models proposed for BHCs. | [
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arXiv_src_0001_001/astro-ph0001111 | Evidence for TeV Emission from GRB 970417a |
Milagrito, a detector sensitive to very high energy gamma rays, monitored the northern sky from February 1997 through May 1998. With a large field of view and a high duty cycle, this instrument was well suited to perform a search for TeV gamma-ray bursts (GRBs). We report on a search made for TeV counterparts to GRBs observed by BATSE. BATSE detected 54 GRBs within the field of view of Milagrito during this period. An excess of events coincident in time and space with one of these bursts, GRB 970417a, was observed by Milagrito. The excess has a chance probability of $2.8 \times 10^{-5}$ of being a fluctuation of the background. The probability for observing an excess at least this large from any of the 54 bursts is $1.5 \times 10^{-3}$. No significant correlations were detected from the other bursts.
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arXiv_src_0001_001/astro-ph0001135 | Theory and Observations of Type I X-Ray Bursts from Neutron Stars |
I review our understanding of the thermonuclear instabilities on accreting neutron stars that produce Type I X-Ray bursts. I emphasize those observational and theoretical aspects that should interest the broad audience of this meeting. The easily accessible timescales of the bursts (durations of tens of seconds and recurrence times of hours to days) allow for a very stringent comparison to theory. The largest discrepancy (which was found with {\it EXOSAT} observations) is the accretion rate dependence of the Type I burst properties. Bursts become less frequent and energetic as the global accretion rate ($\dot M$) increases, just the opposite of what the spherical theory predicts. I present a resolution of this issue by taking seriously the observed dependence of the burning area on $\dot M$, which implies that as $\dot M$ {\it increases}, the accretion rate per unit area
{\it decreases}. This resurrects the unsolved problem of knowing where the freshly accreted material accumulates on the star, equally relevant to the likely signs of rotation during the bursts summarized by Swank at this meeting. I close by highlighting the Type I bursts from GS~1826-238 that were found with {\it BeppoSAX} and {\it RXTE}. Their energetics, recurrence times and temporal profiles clearly indicate that hydrogen is being burned during these bursts, most likely by the rapid-proton (rp) process.
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arXiv_src_0001_001/astro-ph0001117 | The PSCz catalogue | We present the catalogue, mask, redshift data and selection function for the PSCz survey of 15411 IRAS galaxies across 84\% of the sky. Most of the IRAS data is taken from the Point Source Catalog, but this has been supplemented and corrected in various ways to improve the completeness and uniformity. We quantify the known imperfections in the catalogue, and we assess the overall uniformity, completeness and data quality. We find that overall the catalogue is complete and uniform to within a few percent at high latitudes and 10\% at low latitudes. Ancillary information, access details, guidelines and caveats for using the catalogue are given. {\bf Key Words:} Catalogues - surveys - galaxies: distances and redshifts, clustering - large-scale structure of the Universe | [
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arXiv_src_0001_001/astro-ph0001129 | Gravitational Waves from Low-Mass X-ray Binaries: a Status Report \thanks{ Much theoretical progress has been made in understanding GW emission from LMXBs in the six months since the Amaldi conference in July 1999. Rather than just transcribe the talk given by one of us, we review the situation as of December 1999. Because of space limitations, this review is far from complete.} |
We summarize the observations of the spin periods of rapidly accreting neutron stars. If gravitational radiation is responsible for balancing the accretion torque at the observed spin frequencies of
$\approx300$~Hz, then the brightest of these systems make excellent gravitational wave sources for LIGO-II and beyond. We review the recent theoretical progress on two mechanisms for gravitational wave emission: mass quadrupole radiation from deformed neutron star crusts and current quadrupole radiation from r-mode pulsations in neutron star cores.
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arXiv_src_0001_001/astro-ph0001146 | The modified dynamics is conducive to galactic warp formation | There is an effect in the modified dynamics (MOND)
that is conducive to formation of warps. Because of the nonlinearity of the theory the internal dynamics of a galaxy is affected by a perturber over and above possible tidal effects. For example, a relatively distant and light companion or the mean influence of a parent cluster, with negligible tidal effects, could still produce a significant warp in the outer part of a galactic disk. We present results of numerical calculations for simplified models that show, for instance, that a satellite with the (baryonic) mass and distance of the Magellanic clouds can distort the axisymmetric field of the Milky Way enough to produce a warp of the magnitude (and position) observed. Details of the warp geometry remain to be explained: we use a static configuration that can produce only warps with a straight line of nodes. In more realistic simulations one must reckon with the motion of the perturbing body, which sometimes occurs on time scales not much longer than the response time of the disk.
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arXiv_src_0001_001/astro-ph0001145 | The Lake Baikal neutrino experiment |
We review the present status of the Baikal Neutrino Project and present the results of a search for high energy neutrinos with the detector intermediate stage {\it NT-96}.
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arXiv_src_0001_001/astro-ph0001160 | The Synchrotron Spectrum of Fast Cooling Electrons Revisited |
We discuss the spectrum arising from synchrotron emission by fast cooling (FC) electrons, when fresh electrons are continually accelerated by a strong blast wave, into a power law distribution of energies. The FC spectrum was so far described by four power law segments divided by three break frequencies $\nu _{sa}<\nu _{c}<\nu _{m}$. This is valid for a homogeneous electron distribution. However, hot electrons are located right after the shock, while most electrons are farther down stream and have cooled. This spatial distribution changes the optically thick part of the spectrum, introducing a new break frequency, $\nu_{ac}<\nu_{sa}$, and a new spectral slope, $F_{\nu }\propto \nu^{11/8}$ for $\nu_{ac}<\nu
<\nu_{sa}$. The familiar $F_{\nu }\propto \nu ^{2}$ holds only for
$\nu<\nu_{ac}$. This ordering of the break frequencies is relevant for typical gamma-ray burst (GRB) afterglows in an ISM environment. Other possibilities arise for internal shocks or afterglows in dense circumstellar winds. We discuss possible implications of this spectrum for GRBs and their afterglows, in the context of the internal-external shock model. Observations of
$F_{\nu}\propto\nu^{11/8}$ would enable us to probe scales much smaller than the typical size of the system, and constrain the amount of turbulent mixing behind the shock.
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arXiv_src_0001_001/astro-ph0001166 | A Definitive Optical Detection of a Supercluster at $z \approx 0.91$ | We present the results from a multi-band optical imaging program which has definitively confirmed the existence of a supercluster at $z
\approx 0.91$. Two massive clusters of galaxies, CL1604+4304 at $z =
0.897$ and CL1604+4321 at $z = 0.924$, were originally observed in the high-redshift cluster survey of Oke, Postman \& Lubin (1998). They are separated by $4300~{\rm km~s^{-1}}$ in radial velocity and 17 arcminutes on the plane of the sky. Their physical and redshift proximity suggested a promising supercluster candidate. Deep $BRi$
imaging of the region between the two clusters indicates a large population of red galaxies. This population forms a tight, red sequence in the color--magnitude diagram at $(R-i) \approx 1.4$. The characteristic color is identical to that of the spectroscopically-confirmed early-type galaxies in the two member clusters. The red galaxies are spread throughout the $5~h^{-1}~{\rm Mpc}$ region between CL1604+4304 and CL1604+4321. Their spatial distribution delineates the entire large scale structure with high concentrations at the cluster centers. In addition, we detect a significant overdensity of red galaxies directly between CL1604+4304 and CL1604+4321 which is the signature of a third, rich cluster associated with this system. The strong sequence of red galaxies and their spatial distribution clearly indicate that we have discovered a supercluster at $z \approx 0.91$. | [
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"caption": "Histogram of the $(R-i)$ colors of all galaxies with $20 \\le i \\le 23.5$. The vast majority of galaxies belong to the field population which has an average color of $(R-i) \\approx 0.7$. The red sequence of supercluster members is defined by the narrower peak at $(R-I) \\approx 1.4$ (indicated by the arrow) and is easily distinguished from the distribution of field galaxies. Fitting two Gaussians functions to this distribution, we find that $\\sigma_1 = 0.30$ mag for the field population and $\\sigma_2 = 0.15$ mag for the red sequence.",
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arXiv_src_0001_001/astro-ph0001212 | The triple degenerate star WD\,1704+481 |
WD\,1704+481 is a visual binary in which both components are white dwarfs. We present spectra of the H$\alpha$ line of both stars which show that one component (WD\,1704+481.2 = Sanduleak~B = GR\,577) is a close binary with two white dwarf components. Thus, WD\,1704+481 is the first known triple degenerate star. From radial velocity measurements of the close binary we find an orbital period of 0.1448d, a mass ratio, $q=\frac{
M_{\rm bright}}{M_{\rm faint}}$ of
$q=0.70\pm$0.03 and a difference in the gravitational redshifts of 11.5$\pm$2.3\kms. The masses of the close pair of white dwarfs predicted by the mass ratio and gravitational redshift difference combined with theoretical cooling curves are 0.39$\pm$0.05\Msolar\ and 0.56$\pm$0.07\Msolar. WD\,1704+481 is therefore also likely to be the first example of a double degenerate in which the less massive white dwarf is composed of helium and the other white dwarf is composed of carbon and oxygen. | [
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arXiv_src_0001_001/astro-ph0001229 | Ages, Distances, and the Initial Mass Functions of Stellar Clusters | We provide a review of the current status of several topics on the ages, distances, and mass functions of open clusters, with a particular emphasis on illuminating the areas of uncertainty. Hipparcos has obtained parallaxes for nearby open clusters that have expected accuracies much better than has been previously achievable. By using the lithium depletion boundary method and isochrone fitting based on much improved new theoretical evolutionary models for low mass stars, it is arguable that we will soon have have much better age scales for clusters and star-forming regions. With improved optical and near-IR cameras, we are just now beginning to extend the mass function of open clusters like the Pleiades into the regime below the hydrogen burning mass limit. Meanwhile, observations in star-forming regions are in principle capable of identifying objects down to of order 10 Jupiter masses. | [
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arXiv_src_0001_001/astro-ph0001232 | Morphology vs. physical properties: some comments and questions |
Some of the correlations between morphological and other physical properties of planetary nebulae (PNe) are reviewed. In particular, the finding that bipolar ($b$) PNe have more massive progenitors than the other morphological classes is discussed in detail. Earlier results are confirmed; including all the various sources of uncertainty, the Galactic distribution of objects indicate that \bpn\ are formed by stars with initial masses $>1.3$~\sm\ while elliptical ($e$) PNe by progenitors with masses $<1.3$~\sm. Recent results for the chemical abundances of $b$ and $e$ PNe and their orientation within the Galaxy are also presented. Finally, the key role in the discussion of the formation of \bpn\ played by detached binary systems such as symbiotic stars is briefly discussed.
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arXiv_src_0001_001/astro-ph0001240 | Probing The Gravity Induced Bias with Weak Lensing:\\
Test of Analytical results Against Simulations |
Future weak lensing surveys will directly probe the density fluctuation in the universe. Recent studies have shown how the statistics of the weak lensing convergence field is related to the statistics of collapsed objects. Extending earlier analytical results on the probability distribution function of the convergence field we show that the bias associated with the convergence field can directly be related to the bias associated with the statistics of underlying over-dense objects. This will provide us a direct method to study the gravity induced bias in galaxy clustering. Based on our analytical results which use the hierarchical {\em ansatz} for non-linear clustering, we study how such a bias depends on the smoothing angle and the source red-shift. We compare our analytical results against ray tracing experiments through N-body simulations of four different realistic cosmological scenarios and found a very good match. Our study shows that the bias in the convergence map strongly depends on the background geometry and hence can help us in distinguishing different cosmological models in addition to improving our understanding of the gravity induced bias in galaxy clustering.
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arXiv_src_0001_001/astro-ph0001257 | Identification of the Coronal Sources of the Fast Solar Wind | The present spectroscopic study of the ultraviolet coronal emission in a polar hole, detected on April 6--9, 1996 with the Ultraviolet Coronagraph Spectrometer aboard the SOHO spacecraft, identifies the inter--plume lanes and background coronal hole regions as the channels where the fast solar wind is preferentially accelerated. In inter--plume lanes, at heliocentric distance 1.7~\rsun, the corona expands at a rate between 105~\ks\, and 150~\ks, that is, much faster than in plumes where the outflow velocity is between 0~\ks\, and 65~\ks. The wind velocity is inferred from the Doppler dimming of the O~VI $\lambda\lambda$~1032, 1037~\AA\, lines, within a range of values, whose lower and upper limit corresponds to anisotropic and isotropic velocity distribution of the oxygen coronal ions, respectively. | [
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arXiv_src_0001_001/astro-ph0001264 | The giant X-ray outbursts from nearby, {\itshape non-active} galaxies: \\
tidal disruption flares ? | One efficient method to probe the direct vicinity of SMBHs in nearby galaxies is to make use of the detection of flares from tidally disrupted stars
(e.g., Lidskii \& Ozernoi 1979, Rees 1988). The first few excellent candidates for the occurrence of this process in non-active galaxies have emerged recently. Here, we present a review of these observations, compare with variability in AGN, and discuss theoretical implications. We concentrate on the cases of NGC\,5905 and RXJ1242-1119, and report results from a systematic search for further X-ray flares from a sample of $>$100 nearby galaxies. | [
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arXiv_src_0001_001/astro-ph0001260 | \bf Evidence for Stellar Streaming in the Cores of Elliptical Galaxies: \\
A Kinematic Signature of Mergers? | We present evidence for non-Gaussian velocity fields within the cores of luminous elliptical galaxies. This evidence is based upon high signal-to-noise, medium-resolution spectroscopy of the cores of early-type members of the Virgo and Coma clusters obtained with the WIYN 3.5-m telescope. The Virgo data were acquired using an integral-field unit (DensePak) allowing the velocity field to be sampled over a variety of spatial scales. The Coma data were obtained through single, 2-arcsec diameter fibers. The cross-correlation profiles of luminous ellipticals show considerable structure, often having several features with amplitudes as high as 10\% that of the cross-correlation peak itself. This structure is most obvious within a radius of $1.5$
arcsec (at Virgo), or $\leq$ 100 pc, and is nearly undetectable when the data are binned over R $< 15$ arcsec, or $\leq$ 1 kpc. Similar features are found in the single-fiber spectra of the luminous ellipticals in the Coma Cluster suggesting they are ubiquitous to giant ellipticals. Interesting, only the most luminous elliptical galaxies show this phenomena; the central regions of lower luminosity ellipticals have regular, Gaussian-like profiles. We interpret this kinematic structure as ``stellar streaming'' and suggest that this phenomena could be a relic signature of the merger history of luminous elliptical galaxies. | [
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arXiv_src_0001_001/astro-ph0001285 | The INT Wide Field Imaging Survey(WFS) |
The 2.5m Isaac Newton Telescope(INT) is currently being used to carry out a major multi-colour, multi-epoch, CCD based wide field survey over an area of $\sim$100deg$^2$. The survey parameters have been chosen to maximise scientific return over a wide range of scientific areas and to complement other surveys being carried out elsewhere. Unique aspects of the survey is that it concentrates on regions of sky that are easily accessible from telescopes in both Northern and Southern terrestrial hemispheres and that it the first public survey to use filters similar to that being used by the Sloan Digital Sky Survey. A major aim of the the INT Wide Field Survey program is to bridge the gap between the all-sky photographic 2 and 3 band surveys such as the Palomar and UK Schmidt sky surveys and the ultra-deep keyhole surveys such as the Hubble Deep Field(Williams et al, 1996). Apart for the science that can be derived directly from the optical data, the datasets will provide ideal targets lists for multi-object followup with fibre and slit based systems(eg GMOS, 2DF, WYYFOS, FMOS)
based systems on 4m and 8m class telescopes.
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arXiv_src_0001_001/astro-ph0001263 | Warm Absorbers in Active Galactic Nuclei | We first provide a review of the properties of warm absorbers concentrating on what we have learned from {\sl ROSAT} and {\sl ASCA}. This includes dusty and dust-free warm absorbers, non-X-ray emission and absorption features of warm absorbers, and the possible warm absorber interpretation of the peculiar 1.1 keV features. We then discuss facets of warm absorbers by a more detailed investigation of individual objects:
In a first part, we discuss several candidates for dusty warm absorbers. In a second part, we review and extend our earlier study of a possible relation between warm absorber and CLR in NGC\,4051, and confirm that both components are of different origin (the {\em observed} coronal lines are {\em under}predicted by the models, the warm absorber is too highly ionized). We then suggest that a potential overprediction of these lines in more lowly ionized absorbers can be avoided if these warm absorbers are dusty. In a third part, we present first results of an analysis of a deep {\sl ROSAT} PSPC observation of the quasar MR2251--178, the first one discovered to host a warm absorber. Finally, we summarize our scrutiny under which conditions a warm absorber could account for the dramatic spectral variability of the Narrow-line Seyfert\,1 galaxy RXJ0134-4258. | [
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arXiv_src_0001_001/astro-ph0001267 | Sunyaev-Zel'dovich Surveys: Analytic treatment of cluster detection |
Thanks to advances in detector technology and observing techniques, true Sunyaev--Zel'dovich (SZ) surveys will soon become a reality. This opens up a new window into the Universe, in many ways analogous to the X--ray band and inherently well--adapted to reaching high redshifts. I discuss the nature, abundance and redshift distributions of objects detectable in ground--based searches with state--of--the--art technology. An advantage of the SZ approach is that the total SZ flux density depends only on the thermal energy of the intracluster gas and not on its spatial or temperature structure, in contrast to the X--ray luminosity. Because ground--based surveys will be characterized by arcminute angular resolution, they will resolve a large fraction of the cluster population. I quantify the resulting consequences for the cluster selection function; these include less efficient cluster detection compared to idealized point sources and corresponding steeper integrated source counts. This implies, contrary to expectations based on a point source approximation, that deep surveys are better than wide ones in terms of maximizing the number of detected objects. At a given flux density sensitivity and angular resolution, searches at millimeter wavelengths
(bolometers)
are more efficient than centimeter searches
(radio), due to the form of the SZ spectrum. Possible ground--based surveys could discover up to $\sim 100$ clusters per square degree at a wavelength of 2 mm and $\sim 10$/sq. deg. at 1 cm, modeling clusters as a simple self--similar population. \keywords{cosmic microwave background -- Cosmology: observations -- Cosmology: theory -- large--scale structure of the Universe -- Galaxies: clusters: general}
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arXiv_src_0001_001/astro-ph0001296 |
H$_2$ emission as a diagnostic of physical processes in starforming galaxies |
Observations and interpretation of extragalactic rotational and rovibrational $\Htwo$ emission are reviewed. Direct observations of
$\Htwo$ lines do not trace bulk $\Htwo$ mass, but excitation rate. As such, the $\Htwo$ lines are unique diagnostics, if the excitation mechanism can be determined, which generally requires high-quality spectroscopy and suitable additional data. The diagnostic power of the
$\Htwo$ lines is illustrated by two cases studies: $\Htwo$ purely rotational line emission from the disk of the nearby spiral galaxy
$\NGC{891}$ and high resolution imaging and spectroscopy of $\Htwo$
vibrational line emision from the luminous merger $\NGC{6240}$.
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arXiv_src_0001_001/astro-ph0001291 | CADIS deep star counts: Galactic structure and the stellar luminosity function |
In this paper we present the first results of deep star counts carried out within the \CA, CADIS \cite{meise}. Although CADIS was designed as an extragalactic survey, it also attempts to identify the stars in the fields in order to avoid confusion with quasars and compact galaxies.\\
We have identified a sample of about 300 faint stars ($15.5\la R\la 23$), which are well suited to study the structure of the Galaxy. The stars lie in two fields with central coordinates $\alpha_{2000}=16^{\rm h}
24^{\rm m} 32.^{\rm s}3$, $\delta_{2000}=55^{\circ} 44' 32''$ (Galactic coordinates: $l=85\degr$,
$b=45^\circ$) and $\alpha_{2000}=9^{\rm h} 13^{\rm m} 47.^{\rm s}5$, $\delta_{2000}=46^{\circ} 14' 20''$ ($l=175^\circ$,
$b=45^\circ$) (hereafter 16h and 9h field, respectively. The stars have been separated from galaxies by a classification scheme based on photometric spectra and morphological criteria. Distances were derived by photometric parallaxes. We are able to find stars up to distances of $\approx 25$\,kpc above the Galactic plane. The vertical density distribution of the stars shows the contribution of the thin disk, the stellar halo and the ``thick disk'' of the Galaxy. We give quantitative descriptions of the components in terms of exponential disks and a de Vaucouleurs spheroid. For the disk stars we derive the luminosity function. It is equal within the errors to the local luminosity function and continues to rise out to at least $M_V$
= 13. Implications for the mass function are briefly discussed. \keywords{Galaxy: structure -- stars: luminosity function, mass function}
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"caption": "Spatial distribution of metallicity corrected $(b-r)_{{\\rm corr}}$. The solid line represents the distance dependent upper color limit at $R=23^{mag}$, the dotted line is the lower limit due to the selection criterium of the fields (no star brighter than $R\\approx 15.5$). Since the metal-poor halo stars are intrinsically fainter, the color limits are shifted accordingly. The horizontal line denotes the cut between halo and disk stars, the dashed-dotted line indicates the cutoff at $(b-r)_{{\\rm corr}}=1.8$ due to the metallicity correction. The different symbols refer to the different fields: squares - 16h field, triangles - 9h field.",
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arXiv_src_0001_001/astro-ph0001313 | Metallicity in damped Lyman-$\alpha$ systems:
evolution or bias? | Assuming that damped Lyman-$\alpha$ (DLA) systems are galactic discs, we calculate the corresponding evolution of metal abundances. We use detailed multi-zone models of galactic chemical evolution
(reproducing successfully the observed properties of disc galaxies)
and appropriate statistics (including geometrical propability factors)
to calculate the average metallicity as a function of redshift. The results are compatible with available observations, {\it provided that observational biases are taken into account}, as suggested by Boiss\'e et al. (1998). In particular, high column density
{\it and } high metallicity systems are not detected because the light of backround quasars is severely extinguished, while low column density
{\it and } low metallicity systems are not detectable through their absorption lines by current surveys. We show that these observational constraints lead to a ``no-evolution'' picture for the DLA metallicity, which does not allow to draw strong conclusions about the nature of those systems or about their role in ``cosmic chemical evolution''. | [
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"caption": " Zn abundances vs gas column density N(HI). Observations in DLAs are from Pettini et al. (1994, 1997, 1999), Prochaska and Wolfe (1999), Boissé et al. (1998), Lu et al. (1996). Observations are apparently contained within the {shaded area}, which is limited by [Zn/H]+log(N(HI))$<$21 ({upper diagonal}) and [Zn/H]+log(N(HI))$>$18.8 ({lower diagonal}). For illustration purposes, we show the evolution of Zn vs gas column density in three different zones of a Milky Way type disc ({solid curves}, at 0.5, 2.5 and 5.5 scalelengths from the center, respectively) according to our models. The column densities correspond to our model disc seen \"face-on\". The disc evolves from the lower left to the upper right in this diagram, as can be seen from the 3 isochrones ({dashed curves}) at times T=1 Gyr, 5.5 Gyr and 13.5 Gyr, respectively; the corresponding redshifts are for a cosmological model with $H_0$=65 km/s/Mpc, $\\Omega_0$=0.3 and a galaxy formation redshift $z$=6 (i.e. the time of formation of the first stars).",
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"caption": " Evolution of Zn abundances in our models as a function of redshift $z$. Results are presented for a grid of 25 disc models, caracterised by 5 values of the disc maximal circular velocity V$_C$ (80, 150, 220, 290, 360 km/s, {from top to bottom}) and 5 values of the spin parameter $\\lambda$/$\\lambda_{MW}$ (1/3, 1, 5/3, 7/3, 3, {from left to right}) where $\\lambda_{MW}$ is the corresponding value for the Milky Way disc. For clarity, only the evolution of two \"extreme\" zones is shown for each model, at 0.5 and 5.5 scalelengths from the center ({upper and lower curve}, respectively, in each panel), which span the evolution of the whole disc. The region enclosed within {thick curves} is obtained by application of the empirical selection criterion of Fig. 1 (i.e. 18.8 $<$ [Zn/H]+log(N(HI)) $<$ 21), assuming that all discs are seen \"face-on\". It can be seen that this \"filter\" selects zones within a restricted range of [Zn/H] value (independently of redshift), and leads to a no-evolution picture. Observations (the same in all panels) are from the references listed in the legend of Fig. 1.",
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arXiv_src_0001_001/astro-ph0001301 | HEGRA Observations of Galactic Sources |
In this talk I will first give a summary of the observations of expected Galactic TeV \gr sources with the HEGRA CT-Sytem since the Kruger Park Workshop in 1997. Then I will go into some detail regarding the observations of Supernova Remnants (SNRs), especially those of Tycho's SNR and of Cas~A. The emphasis will not be on all aspects of these published data. I will rather review the selection of these observational targets, and discuss some of the physical implications of the results.
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arXiv_src_0001_001/astro-ph0001325 | Gravitational Lensing of High Redshift Sources |
The combination of deep exposures and high resolution offered by telescopes in space allows the detection of lensing over a wide range of source redshifts and lens masses. As an example, we model a lens candidate found in the southern Hubble Deep Field. The system consists of a source galaxy lensed into an arc, $0\farcs9$ from an elliptical galaxy. The photometric redshift of 0.6 for the lens galaxy implies a mass-to-light ratio of 15 in solar units, out to three effective radii. This lens system may be a preview of the large number of lensed high-redshift galaxies that will be detected with the Next Generation Space Telescope ({\it NGST}\,). When {\it NGST}\, is launched in the next decade, some of the earliest galaxies and quasars in the Universe may be observed. Popular models of structure formation imply that at a given observed flux, roughly $3\%$ of redshift $>5$ sources are multiply imaged. Thus, {\it NGST}\, should detect several lensed objects in each field of view. In addition, {\it NGST}\, will be a valuable tool for weak lensing measurements, as long as it can resolve the background galaxies. We estimate the angular size distribution of high redshift sources within hierarchical models of structure formation and find that most will be resolved by {\it NGST}\, even at $z>10$.
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arXiv_src_0001_001/astro-ph0001328 | Oxygen Absorption in Cooling Flows |
The inhomogeneous cooling flow scenario predicts the existence of large quantities of gas in massive elliptical galaxies, groups, and clusters that have cooled and dropped out of the flow. Using spatially resolved, deprojected X-ray spectra from the {\sl ROSAT} PSPC we have detected strong absorption over energies $\sim 0.4-0.8$ keV intrinsic to the central $\sim 1\arcmin$ of the galaxy, NGC 1399, the group, NGC 5044, and the cluster, A1795. These systems have amongst the largest nearby cooling flows in their respective classes and low Galactic columns. Since no excess absorption is indicated for energies below
$\sim 0.4$ keV the most reasonable model for the absorber is warm, collisionally ionized gas with $T=10^{5-6}$ K where ionized states of oxygen provide most of the absorption. Attributing the absorption only to ionized gas reconciles the large columns of cold H and He inferred from {\sl Einstein} and {\sl ASCA} with the lack of such columns inferred from {\sl ROSAT}, and also is consistent with the negligible atomic and molecular H inferred from \hi\, and CO observations of cooling flows. The prediction of warm ionized gas as the product of mass drop-out in these and other cooling flows can be verified by {\sl Chandra}, {\sl XMM}, and {\sl ASTRO-E}.
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End of preview. Expand
in Dataset Viewer.
Dataset Card for ArxivCap
Data Instances
Example-1 of single (image, caption) pairs
"......" stands for omitted parts.
{
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'arxiv_id': '2112.08947',
'title': 'Computational metrics and parameters of an injection-locked large area semiconductor laser for neural network computing',
'abstract': 'Artificial neural networks have become a staple computing technique in many fields. Yet, they present fundamental differences with classical computing hardware in the way they process information. Photonic implementations of neural network architectures potentially offer fundamental advantages over their electronic counterparts in terms of speed, processing parallelism, scalability and energy efficiency. Scalable and high performance photonic neural networks (PNNs) have been demonstrated, yet they remain scarce. In this work, we study the performance of such a scalable, fully parallel and autonomous PNN based on a large area vertical-cavity surface-emitting laser\n(LA-VCSEL). We show how the performance varies with different physical parameters, namely, injection wavelength, injection power, and bias current. Furthermore, we link these physical parameters to the general computational measures of consistency and dimensionality. We present a general method of gauging dimensionality in high dimensional nonlinear systems subject to noise, which could be applied to many systems in the context of neuromorphic computing. Our work will inform future implementations of spatially multiplexed VCSEL PNNs.\n',
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Example-2 of multiple images and subcaptions
"......" stands for omitted parts.
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'abstract': '\nWe present Monte Carlo wavefunction simulations for quantum computations employing an exchange-coupled array of quantum dots. Employing a combination of experimentally and theoretically available parameters, we find that gate fidelities greater than 98 \\% may be obtained with current experimental and technological capabilities. Application to an encoded 3 qubit\n(nine physical qubits) Deutsch-Josza computation indicates that the algorithmic fidelity is more a question of the total time to implement the gates than of the physical complexity of those gates.\n',
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]
},
......
]
}
Dataset Summary
The ArxivCap dataset consists of 6.4 million images and 3.9 million captions with 193 million words from 570k academic papers accompanied with abstracts and titles. (papers before June 2023)
Curation Process
Refer to our paper for the curation and filter process.
Dataset Structure
Data Loading
from datasets import load_dataset
dataset = load_dataset("MMInstruction/ArxivCap")
dataset["train"] # list of dictionaries
# for quick download in linux
set -e
sudo apt-get install git-lfs -y
git clone https://huggingface.co/datasets/MMInstruction/ArxivCap
cd ArxivCap/data
# then you can load the parquet files in python use something like
data = load_dataset(
"parquet",
data_files="/path/to/parquet/arXiv_src_9912_001.parquet"
)
Data Fields
One record refers to one paper:
- src: String. "<Arxiv Tar File Name>/<Folder Name in Tar File>"e.g. "arXiv_src_2112_060/2112.08947"
- arxiv_id: String. Arxiv id of the paper, e.g. "2112.08947"
- title: String. Title of the paper.
- abstract: String. Abstract of the paper.
- meta:
- meta_from_kaggle: refers to arXiv Dataset
- journey: String. Information about the journal the paper was published in.
- licence: String. License for the paper.
- categories: String. Categories / tags in the ArXiv system.
- meta_from_s2: refers to SEMANTIC SCHOLAR
- citationCount: Integer. Total number of citations S2 has found for this paper
- influentialCitationCount: Integer. Refers here
- publicationTypes: List[String]. Journal Article, Conference, Review, etc.
- meta_from_kaggle: refers to arXiv Dataset
- caption_images:
- caption: String. Main caption.
- cil_pairs:
- sub_caption: String. Subcaption for the image.
- image_file: String. Unique file name for the image.
- image: PIL.Image.Image. A PIL.Image.Image object containing the image.
- image_ocr: List[String]. OCR result for the image using PaddleOCR
import datasets
features = datasets.Features(
{
"src": datasets.Value("string"),
"arxiv_id": datasets.Value("string"),
"title": datasets.Value("string"),
"abstract": datasets.Value("string"),
"meta": {
"meta_from_kaggle": {
"journey": datasets.Value("string"),
"license": datasets.Value("string"),
"categories": datasets.Value("string"),
},
"meta_from_s2": {
"citationCount": datasets.Value("int32"),
"influentialCitationCount": datasets.Value("int32"),
"publicationTypes": [datasets.Value("string")],
}
},
"caption_images": [{
"caption": datasets.Value("string"),
"cil_pairs": [{
"sub_caption": datasets.Value("string"),
"image_file": datasets.Value("string"),
"image": datasets.Image(),
"image_ocr": [datasets.Value("string")],
}]
}]
}
)
Additional Information
Licensing Information
ArxivCap is released under CC BY-NC-SA 4.0.
Citation Information
@misc{li2024multimodal,
title={Multimodal ArXiv: A Dataset for Improving Scientific Comprehension of Large Vision-Language Models},
author={Lei Li and Yuqi Wang and Runxin Xu and Peiyi Wang and Xiachong Feng and Lingpeng Kong and Qi Liu},
year={2024},
eprint={2403.00231},
archivePrefix={arXiv},
primaryClass={cs.CV}
}
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