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dc.contributor.authorKoekemoer, Antonen_US
dc.contributor.authorO'Dea, Christopheren_US
dc.contributor.authorBaum, Stefien_US
dc.contributor.authorSarazin, Craigen_US
dc.contributor.authorOwen, Frazeren_US
dc.contributor.authorLedlow, Michaelen_US
dc.date.accessioned2006-05-17T18:26:10Zen_US
dc.date.available2006-05-17T18:26:10Zen_US
dc.date.issued1998-12-01en_US
dc.identifier.citationAstrophys.J. 508 (1998) 608-620en_US
dc.identifier.issn1538-4365en_US
dc.identifier.urihttp://hdl.handle.net/1850/1812en_US
dc.description.abstractWe present results from an extensive HST spectroscopic search for UV absorption lines in the spectrum of the quasar B2 1028+313, which is associated with the central dominant galaxy in the cluster Abell 1030 (z=0.178). This is one of the brightest known UV continuum sources located in a cluster, and therefore provides an ideal opportunity to obtain stringent constraints on the column densities of any cool absorbing gas that may be associated with the intracluster medium (ICM). Our HST spectra were obtained with the FOS and GHRS, and provide continuous coverage at rest-frame wavelengths from ~975 to 4060°A, thereby allowing the investigation of many different elements and ionization levels. We utilize a new technique that involves simultaneous fitting of large numbers of different transitions for each species, thereby yielding more robust constraints on column densities than can be obtained from a single transition. This method yields upper limits of ~<10^11−10^13 cm^−2 on the column densities of a wide range of molecular, atomic and ionized species that may be associated with the ICM. We also discuss a possible Ly-alpha and C IV absorption system associated with the quasar. We discuss the implications of the upper limits on cool intracluster gas in the context of the physical properties of the ICM and its relationship to the quasar (Refer to PDF file for exact formulas).en_US
dc.description.sponsorshipWe would like to thank Tony Keyes and Chris Blades for valuable discussions during the course of this work. We are also very grateful to D. P. Schneider for kindly making available the absorption-line identification software package that is used for the HST Quasar Absorption Line Key Project and for providing vital help regarding the use of this software. We would also like to thank the anonymous referee for useful suggestions that helped to improve the paper. Support for this work was provided by NASA through grant number GO-05934.01-94A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. M. Ledlow thanks Elizabeth Rizza for her help in obtaining the APO spectra. The Apache Point Observatory is maintained and operated by the Astrophysical Research Consortium (ARC).en_US
dc.format.extent1096221 bytesen_US
dc.format.mimetypeapplication/pdfen_US
dc.language.isoen_USen_US
dc.publisherAstrophysical Journalen_US
dc.relation.ispartofseriesvol. 508en_US
dc.relation.ispartofseriesno. 2en_US
dc.subjectGalaxies - clusters - individual - A1030en_US
dc.subjectIntergalactic mediumen_US
dc.subjectQuasars - absorption linesen_US
dc.subjectQuasars - individual - B2 1028+313en_US
dc.subjectUltraviolet - galaxiesen_US
dc.titleConstraints on ultraviolet absorption in the intracluster medium of Abell 1030en_US
dc.typeArticleen_US
dc.identifier.urlhttp://dx.doi.org/10.1086/306417


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