The multiphase absorption systems toward PG 1206+459

Jie Ding, Jane C. Charlton, Christopher W. Churchill, Christopher Palma

Research output: Contribution to journalArticle

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Abstract

A high-resolution (R = 30,000) ultraviolet spectrum is presented, which covers Lyα and many low-, intermediate-, and high-ionization transitions in the three Mg II-selected absorption systems toward the quasar PG 1206+459. Three systems (A, B, and C), which are clustered within 1500 km s-1 at z ∼ 0.93, were originally identified in a spectrum obtained with the High Resolution Spectrograph (HIRES) on the Keck I Telescope. A WIYN (Wisconsin-Indiana-Yale-NOAO) Gunn i-band image of the quasar field and spectroscopy of two galaxy candidates are presented. A multiphase medium is seen in all three systems, consistent with smaller, denser clouds producing low-ionization transitions (Mg II, Fe II, and Si II) and larger, diffuse, photoionized clouds giving rise to higher ionization transitions (C IV, N V, and/or O VI). (1) System A, a multicloud, weak Mg II absorber at z = 0.9254, requires a supersolar metallicity in both low- and high-ionization phases, unless an α-group enhancement is included. The low-ionization absorption is produced in clouds with sizes of 10-70 pc, which are surrounded in velocity space by broader, high-ionization components. With the unusually complex velocity structure resolved in the N V profiles, this system is unlikely to represent a traditional galaxy disk/corona. The most likely candidate host galaxy is a ∼2L*, apparently warped, spiral at an impact parameter of 43 h-1 kpc. (2) System B, at z = 0.9276, has the strongest Mg II absorption and has an approximately solar metallicity in the low-ionization phase. The smooth, broad high-ionization profiles may indicate a coronal structure similar to that of the Milky Way. The redshift of an L* galaxy (z = 0.9289), at an impact parameter of 38 h-1 kpc, is consistent with the redshift of this system. (3) System C, at z = 0.9342, has a single component in Mg II, separated from the other two systems by ∼+1000 km s -1. The Lyα profile is not aligned with the Mg II, requiring an additional velocity component offset by -40 km s-1. System C lacks the small, low-ionization cloud characteristic of an isolated single-cloud, weak Mg II absorber. Its absorption properties are similar to the "satellite clouds" of classic strong Mg II absorbers, so this could be a high-velocity cloud in the galaxy group responsible for the systems, possibly related to a 0.2L* galaxy at an impact parameter of 43 h -1 kpc.

Original languageEnglish (US)
Pages (from-to)746-769
Number of pages24
JournalAstrophysical Journal
Volume590
Issue number2 I
DOIs
StatePublished - Jun 20 2003

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ionization
galaxies
absorbers
quasars
metallicity
profiles
galactic clusters
disk galaxies
high resolution
ultraviolet spectra
velocity structure
coronas
spectrographs
corona
spectroscopy
telescopes
augmentation
parameter

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ding, Jie ; Charlton, Jane C. ; Churchill, Christopher W. ; Palma, Christopher. / The multiphase absorption systems toward PG 1206+459. In: Astrophysical Journal. 2003 ; Vol. 590, No. 2 I. pp. 746-769.
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title = "The multiphase absorption systems toward PG 1206+459",
abstract = "A high-resolution (R = 30,000) ultraviolet spectrum is presented, which covers Lyα and many low-, intermediate-, and high-ionization transitions in the three Mg II-selected absorption systems toward the quasar PG 1206+459. Three systems (A, B, and C), which are clustered within 1500 km s-1 at z ∼ 0.93, were originally identified in a spectrum obtained with the High Resolution Spectrograph (HIRES) on the Keck I Telescope. A WIYN (Wisconsin-Indiana-Yale-NOAO) Gunn i-band image of the quasar field and spectroscopy of two galaxy candidates are presented. A multiphase medium is seen in all three systems, consistent with smaller, denser clouds producing low-ionization transitions (Mg II, Fe II, and Si II) and larger, diffuse, photoionized clouds giving rise to higher ionization transitions (C IV, N V, and/or O VI). (1) System A, a multicloud, weak Mg II absorber at z = 0.9254, requires a supersolar metallicity in both low- and high-ionization phases, unless an α-group enhancement is included. The low-ionization absorption is produced in clouds with sizes of 10-70 pc, which are surrounded in velocity space by broader, high-ionization components. With the unusually complex velocity structure resolved in the N V profiles, this system is unlikely to represent a traditional galaxy disk/corona. The most likely candidate host galaxy is a ∼2L*, apparently warped, spiral at an impact parameter of 43 h-1 kpc. (2) System B, at z = 0.9276, has the strongest Mg II absorption and has an approximately solar metallicity in the low-ionization phase. The smooth, broad high-ionization profiles may indicate a coronal structure similar to that of the Milky Way. The redshift of an L* galaxy (z = 0.9289), at an impact parameter of 38 h-1 kpc, is consistent with the redshift of this system. (3) System C, at z = 0.9342, has a single component in Mg II, separated from the other two systems by ∼+1000 km s -1. The Lyα profile is not aligned with the Mg II, requiring an additional velocity component offset by -40 km s-1. System C lacks the small, low-ionization cloud characteristic of an isolated single-cloud, weak Mg II absorber. Its absorption properties are similar to the {"}satellite clouds{"} of classic strong Mg II absorbers, so this could be a high-velocity cloud in the galaxy group responsible for the systems, possibly related to a 0.2L* galaxy at an impact parameter of 43 h -1 kpc.",
author = "Jie Ding and Charlton, {Jane C.} and Churchill, {Christopher W.} and Christopher Palma",
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Ding, J, Charlton, JC, Churchill, CW & Palma, C 2003, 'The multiphase absorption systems toward PG 1206+459', Astrophysical Journal, vol. 590, no. 2 I, pp. 746-769. https://doi.org/10.1086/375028

The multiphase absorption systems toward PG 1206+459. / Ding, Jie; Charlton, Jane C.; Churchill, Christopher W.; Palma, Christopher.

In: Astrophysical Journal, Vol. 590, No. 2 I, 20.06.2003, p. 746-769.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The multiphase absorption systems toward PG 1206+459

AU - Ding, Jie

AU - Charlton, Jane C.

AU - Churchill, Christopher W.

AU - Palma, Christopher

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N2 - A high-resolution (R = 30,000) ultraviolet spectrum is presented, which covers Lyα and many low-, intermediate-, and high-ionization transitions in the three Mg II-selected absorption systems toward the quasar PG 1206+459. Three systems (A, B, and C), which are clustered within 1500 km s-1 at z ∼ 0.93, were originally identified in a spectrum obtained with the High Resolution Spectrograph (HIRES) on the Keck I Telescope. A WIYN (Wisconsin-Indiana-Yale-NOAO) Gunn i-band image of the quasar field and spectroscopy of two galaxy candidates are presented. A multiphase medium is seen in all three systems, consistent with smaller, denser clouds producing low-ionization transitions (Mg II, Fe II, and Si II) and larger, diffuse, photoionized clouds giving rise to higher ionization transitions (C IV, N V, and/or O VI). (1) System A, a multicloud, weak Mg II absorber at z = 0.9254, requires a supersolar metallicity in both low- and high-ionization phases, unless an α-group enhancement is included. The low-ionization absorption is produced in clouds with sizes of 10-70 pc, which are surrounded in velocity space by broader, high-ionization components. With the unusually complex velocity structure resolved in the N V profiles, this system is unlikely to represent a traditional galaxy disk/corona. The most likely candidate host galaxy is a ∼2L*, apparently warped, spiral at an impact parameter of 43 h-1 kpc. (2) System B, at z = 0.9276, has the strongest Mg II absorption and has an approximately solar metallicity in the low-ionization phase. The smooth, broad high-ionization profiles may indicate a coronal structure similar to that of the Milky Way. The redshift of an L* galaxy (z = 0.9289), at an impact parameter of 38 h-1 kpc, is consistent with the redshift of this system. (3) System C, at z = 0.9342, has a single component in Mg II, separated from the other two systems by ∼+1000 km s -1. The Lyα profile is not aligned with the Mg II, requiring an additional velocity component offset by -40 km s-1. System C lacks the small, low-ionization cloud characteristic of an isolated single-cloud, weak Mg II absorber. Its absorption properties are similar to the "satellite clouds" of classic strong Mg II absorbers, so this could be a high-velocity cloud in the galaxy group responsible for the systems, possibly related to a 0.2L* galaxy at an impact parameter of 43 h -1 kpc.

AB - A high-resolution (R = 30,000) ultraviolet spectrum is presented, which covers Lyα and many low-, intermediate-, and high-ionization transitions in the three Mg II-selected absorption systems toward the quasar PG 1206+459. Three systems (A, B, and C), which are clustered within 1500 km s-1 at z ∼ 0.93, were originally identified in a spectrum obtained with the High Resolution Spectrograph (HIRES) on the Keck I Telescope. A WIYN (Wisconsin-Indiana-Yale-NOAO) Gunn i-band image of the quasar field and spectroscopy of two galaxy candidates are presented. A multiphase medium is seen in all three systems, consistent with smaller, denser clouds producing low-ionization transitions (Mg II, Fe II, and Si II) and larger, diffuse, photoionized clouds giving rise to higher ionization transitions (C IV, N V, and/or O VI). (1) System A, a multicloud, weak Mg II absorber at z = 0.9254, requires a supersolar metallicity in both low- and high-ionization phases, unless an α-group enhancement is included. The low-ionization absorption is produced in clouds with sizes of 10-70 pc, which are surrounded in velocity space by broader, high-ionization components. With the unusually complex velocity structure resolved in the N V profiles, this system is unlikely to represent a traditional galaxy disk/corona. The most likely candidate host galaxy is a ∼2L*, apparently warped, spiral at an impact parameter of 43 h-1 kpc. (2) System B, at z = 0.9276, has the strongest Mg II absorption and has an approximately solar metallicity in the low-ionization phase. The smooth, broad high-ionization profiles may indicate a coronal structure similar to that of the Milky Way. The redshift of an L* galaxy (z = 0.9289), at an impact parameter of 38 h-1 kpc, is consistent with the redshift of this system. (3) System C, at z = 0.9342, has a single component in Mg II, separated from the other two systems by ∼+1000 km s -1. The Lyα profile is not aligned with the Mg II, requiring an additional velocity component offset by -40 km s-1. System C lacks the small, low-ionization cloud characteristic of an isolated single-cloud, weak Mg II absorber. Its absorption properties are similar to the "satellite clouds" of classic strong Mg II absorbers, so this could be a high-velocity cloud in the galaxy group responsible for the systems, possibly related to a 0.2L* galaxy at an impact parameter of 43 h -1 kpc.

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