Chandra detection of X-ray absorption associated with a damped Lyα system

Research output: Contribution to journalArticle

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Abstract

We have observed three quasars, PKS 1127-145, Q1331+171, and Q0054+144, with the ACIS-S aboard the Chandra X-Ray Observatory in order to measure soft X-ray absorption associated with intervening 21 cm and damped Lyα absorbers. For PKS 1127-145, we detect absorption that, if associated with an intervening zabs = 0.312 absorber, implies a metallicity of 23% solar. If the absorption is not at zabs = 0.312, then the metallicity is still constrained to be less than 23% solar. The advantage of the X-ray measurement is that the derived metallicity is insensitive to ionization, inclusion of an atom in a molecule, or depletion onto grains. The X-ray absorption is mostly due to oxygen and is consistent with the oxygen abundance of 30% solar derived from optical nebular emission lines in a foreground galaxy at the redshift of the absorber. For Q1331+171 and Q0054+144, only upper limits were obtained, although the exposure times were intentionally short, since for these two objects we were interested primarily in measuring flux levels to plan for future observations. The imaging results are presented in a companion paper.

Original languageEnglish (US)
Pages (from-to)133-138
Number of pages6
JournalAstrophysical Journal
Volume562
Issue number1 PART I
DOIs
StatePublished - 2001

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metallicity
absorbers
x rays
oxygen
quasars
light emission
observatories
depletion
ionization
observatory
inclusions
galaxies
detection
atoms
molecules
exposure
measuring
plan

Keywords

  • Galaxies: Abundances
  • Quasars: Absorption lines
  • X-rays: ISM

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Chandra detection of X-ray absorption associated with a damped Lyα system. / Bechtold, Jill.

In: Astrophysical Journal, Vol. 562, No. 1 PART I, 2001, p. 133-138.

Research output: Contribution to journalArticle

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abstract = "We have observed three quasars, PKS 1127-145, Q1331+171, and Q0054+144, with the ACIS-S aboard the Chandra X-Ray Observatory in order to measure soft X-ray absorption associated with intervening 21 cm and damped Lyα absorbers. For PKS 1127-145, we detect absorption that, if associated with an intervening zabs = 0.312 absorber, implies a metallicity of 23{\%} solar. If the absorption is not at zabs = 0.312, then the metallicity is still constrained to be less than 23{\%} solar. The advantage of the X-ray measurement is that the derived metallicity is insensitive to ionization, inclusion of an atom in a molecule, or depletion onto grains. The X-ray absorption is mostly due to oxygen and is consistent with the oxygen abundance of 30{\%} solar derived from optical nebular emission lines in a foreground galaxy at the redshift of the absorber. For Q1331+171 and Q0054+144, only upper limits were obtained, although the exposure times were intentionally short, since for these two objects we were interested primarily in measuring flux levels to plan for future observations. The imaging results are presented in a companion paper.",
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AB - We have observed three quasars, PKS 1127-145, Q1331+171, and Q0054+144, with the ACIS-S aboard the Chandra X-Ray Observatory in order to measure soft X-ray absorption associated with intervening 21 cm and damped Lyα absorbers. For PKS 1127-145, we detect absorption that, if associated with an intervening zabs = 0.312 absorber, implies a metallicity of 23% solar. If the absorption is not at zabs = 0.312, then the metallicity is still constrained to be less than 23% solar. The advantage of the X-ray measurement is that the derived metallicity is insensitive to ionization, inclusion of an atom in a molecule, or depletion onto grains. The X-ray absorption is mostly due to oxygen and is consistent with the oxygen abundance of 30% solar derived from optical nebular emission lines in a foreground galaxy at the redshift of the absorber. For Q1331+171 and Q0054+144, only upper limits were obtained, although the exposure times were intentionally short, since for these two objects we were interested primarily in measuring flux levels to plan for future observations. The imaging results are presented in a companion paper.

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