paper_id string | title string | authors list | abstract string | latex list | bibtex list |
|---|---|---|---|---|---|
astro-ph0002001 | QSO Absorption Line Constraints on Intragroup High--Velocity Clouds | [
{
"author": "Jane~C.~Charlton\\altaffilmark{1}"
},
{
"author": "Christopher~W.~Churchill"
},
{
"author": "and Jane~R.~Rigby"
}
] | We show that the number statistics of moderate redshift {\MgII} and Lyman limit absorbers may rule out the hypothesis that high velocity clouds are infalling intragroup material. | [
{
"name": "astro-ph0002001.tex",
"string": "\\documentstyle[emulateapj,rotate,times]{article}\n%\\documentstyle[11pt,rotate,aaspp4]{article}\n%\\documentstyle[12pt,aasms4]{article}\n \n% this is the modification \n \n%-----------------------------------------------------------------------------\n%\n% perso... | [
{
"name": "astro-ph0002001.extracted_bib",
"string": "\\begin{thebibliography}{XXX}\n\n\\bibitem[Bergeron \\& Boiss\\'e 1991]{bb91}\nBergeron, J., \\& Boiss\\'e, P. 1991, A\\&A, 243, 344\n\n\\bibitem[Bergeron \\etal 1992]{bergeron92}\nBergeron, J., Cristiani, S., \\& Shaver, P. A. 1992, A\\&A, 257, 417\n\n\... |
astro-ph0002002 | Point source models for the gravitational lens B1608+656: Indeterminacy in the prediction of the Hubble constant | [
{
"author": "Gabriela Surpi and Roger Blandford"
}
] | We apply elliptical isothermal mass models to reproduce the point source properties, i.e. image positions, flux density ratios and time delay ratios, of the quadruple lens B1608+656. A wide set of suitable solutions is found, showing that models that only fit the properties of point sources are under-constrained and can lead to a large uncertainty in the prediction of H$_\circ$. We present two examples of models predicting H$_\circ\!=\!100{km\,s^{\!-\!1}Mpc^{\!-\!1}}$ ($\chi^2\!=\!4$) and H$_\circ\!=\!69{km\,s^{\!-\!1}Mpc^{\!-\!1}}$ ($\chi^2\!=\!24$). | [
{
"name": "gsurpi.tex",
"string": "\\documentstyle[11pt,paspconf,epsf]{article}\n\n\\begin{document}\n\\title{Point source models for the gravitational lens B1608+656:\nIndeterminacy in the prediction of the Hubble constant}\n\n\\author{Gabriela Surpi and Roger Blandford}\n\\affil{California Institute of Te... | [] |
astro-ph0002003 | Compact Stellar Systems in the Fornax Cluster: Super-massive Star Clusters or Extremely Compact Dwarf Galaxies? | [
{
"author": "M. J. Drinkwater$^{1}$"
},
{
"author": "J. B. Jones$^{2}$"
},
{
"author": "M. D. Gregg$^{3}$"
},
{
"author": "S. Phillipps$^{4}$"
}
] | and % | [
{
"name": "fss4.tex",
"string": "%\n% LaTeX template file for\n% Publications of the Astronomical Society of Australia.\n% Version 2.4 - 28 April 1997\n%\n%\\documentstyle[12pt,psfig]{article}\n\\documentstyle[11pt,psfig]{article}\n%\n% Baselineskip may be altered if desired.\n%\n\\baselineskip=2em\n%\n% A ... | [] |
astro-ph0002004 | Extracting Energy from a Black Hole through Its Disk | [
{
"author": "Li-Xin Li"
}
] | When some magnetic field lines connect a Kerr black hole with a disk rotating around it, energy and angular momentum are transferred between them. If the black hole rotates faster than the disk, $ca/GM_H>0.36$ for a thin Keplerian disk, then energy and angular momentum are extracted from the black hole and transferred to the disk ($M_H$ is the mass and $a M_H$ is the angular momentum of the black hole). This way the energy originating in the black hole may be radiated away by the disk. The total amount of energy that can be extracted from the black hole spun down from $ca/GM_H = 0.998$ to $ca/GM_H = 0.36$ by a thin Keplerian disk is $\approx 0.15 M_Hc^2$. This is larger than $\approx 0.09 M_Hc^2$ which can be extracted by the Blandford-Znajek mechanism. | [
{
"name": "bh_disk.tex",
"string": "% bh_disk.tex for ApJ Letters\n\n\\documentstyle[12pt,aaspp4]{article}\n\\begin{document}\n\n\\title{Extracting Energy from a Black Hole through Its Disk}\n\n\\author{Li-Xin Li}\n\\affil{Princeton University Observatory, Princeton, NJ 08544--1001, USA}\n\\affil{E-mail: lx... | [] |
astro-ph0002005 | A Comparison of Ultraviolet, Optical, and X-Ray Imagery of Selected Fields in the Cygnus Loop | [
{
"author": "\\sc Charles W.\\ Danforth\\altaffilmark{1}"
},
{
"author": "Robert H.\\ Cornett\\altaffilmark{2}"
},
{
"author": "N. A. Levenson\\altaffilmark{1}"
},
{
"author": "William P.\\ Blair\\altaffilmark{1}"
},
{
"author": "Theodore P.\\ Stecher\\altaffilmark{3}"
}
] | During the Astro-1 and Astro-2 Space Shuttle missions in 1990 and 1995, far ultraviolet (FUV) images of five 40\arcmin\ diameter fields around the rim of the Cygnus Loop supernova remnant were observed with the Ultraviolet Imaging Telescope (UIT). These fields sampled a broad range of conditions including both radiative and nonradiative shocks in various geometries and physical scales. In these shocks, the UIT B5 band samples predominantly \ion{C}{4} $\lambda$1550 and the hydrogen two-photon recombination continuum. Smaller contributions are made by emission lines of \ion{He}{2} $\lambda$1640 and \ion{O}{3}] $\lambda$1665. We present these new FUV images and compare them with optical \Ha\ and [\ion{O}{3}], and ROSAT HRI X-ray images. Comparing the UIT images with those from the other bands provides new insights into the spatial variations and locations of these different types of emission. By comparing against shock model calculations and published FUV spectroscopy at select locations, we surmise that resonance scattering in the strong FUV permitted lines is widespread in the Cygnus Loop, especially in the bright optical filaments typically selected for observation in most previous studies. | [
{
"name": "psfig.tex",
"string": "% Psfig/TeX Release 1.2\n% dvips version\n%\n% All software, documentation, and related files in this distribution of\n% psfig/tex are Copyright 1987, 1988 Trevor J. Darrell\n%\n% Permission is granted for use and non-profit distribution of psfig/tex \n% providing that this... | [
{
"name": "astro-ph0002005.extracted_bib",
"string": "\\begin{thebibliography}{Danforth00}\n\\bibitem[Arendt, Dwek, \\& Leisawitz 1992]{Arendt92}\nArendt, R.G., Dwek, E., \\& Leisawitz, D. 1992, \\apj, 400, 562\n\\bibitem[Bedogni \\& Woodward (1990)]{Bedogni90}\nBedogni, R. \\& Woodward, P. R. 1990, \\aap, ... |
astro-ph0002006 | ULTRA HIGH ENERGY COSMIC RAYS: the theoretical challenge | [
{
"author": "A. V. Olinto\\thanksref{corr}"
}
] | "The origin of the highest-energy cosmic rays remains a mystery. The lack of a high energy cutoff in(...TRUNCATED) | [{"name":"physrepf.tex","string":"\\def\\la{\\hbox{{\\lower -2.5pt\\hbox{$<$}}\\hskip -8pt\\raise\n-(...TRUNCATED) | [{"name":"astro-ph0002006.extracted_bib","string":"\\begin{thebibliography}{9}\n\n\\bibitem{watson99(...TRUNCATED) |
astro-ph0002007 | [] | [{"name":"astro-ph0002007.tex","string":"\\documentstyle[12pt]{article}\n\\textheight 9in\n\\textwid(...TRUNCATED) | [{"name":"astro-ph0002007.extracted_bib","string":"\\begin{thebibliography}{99}\n\\bibitem{alcock} A(...TRUNCATED) | ||
astro-ph0002008 | "ISO-SWS spectroscopy of NGC 1068 \\footnote{Based on observations with ISO, an ESA project with ins(...TRUNCATED) | [{"author":"D.~Lutz\\footnote{Max-Planck-Institut f\\\"ur extraterrestrische Physik, Postfach 1603, (...TRUNCATED) | "We present ISO-SWS spectroscopy of NGC 1068 for the complete wavelength range 2.4 to 45$\\mu$m at r(...TRUNCATED) | [{"name":"obspaper.tex","string":"%\\documentstyle[12pt,aasms4]{article}\n\\documentstyle[11pt,aaspp(...TRUNCATED) | [{"name":"astro-ph0002008.extracted_bib","string":"\\begin{thebibliography}{}\n\\bibitem[Alexander e(...TRUNCATED) |
astro-ph0002009 | The giant radio galaxy 8C\,0821+695 and its environment | [{"author":"L. Lara\\inst{1}"},{"author":"K.-H. Mack\\inst{2,3}"},{"author":"M. Lacy\\inst{4}"},{"au(...TRUNCATED) | "We present new VLA and Effelsberg observations of the radio galaxy 8C\\,0821+695. We have obtained (...TRUNCATED) | [{"name":"lara.tex","string":"%----------------------------------------------%\n% REFERENCES \n%----(...TRUNCATED) | [{"name":"astro-ph0002009.extracted_bib","string":"\\begin{thebibliography}{}\n\n\\bibitem[1977]{baa(...TRUNCATED) |
astro-ph0002010 | RADIATION SPECTRA FROM \\ADVECTION-DOMINATED ACCRETION FLOWS \\IN A GLOBAL MAGNETIC FIELD | [
{
"author": "MOTOKI KINO$^{1}$"
},
{
"author": "OSAMU KABURAKI and NAOHIRO YAMAZAKI"
}
] | "We calculate the radiation spectra from advection-dominated accretion flows (ADAFs), taking into ac(...TRUNCATED) | [{"name":"ms.tex","string":" \n%--------------------------------------------------------------------(...TRUNCATED) | [] |
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