HST/COS detection of a Ne VIII absorber towards PG 1407+265: An unambiguous tracer of collisionally ionized hot gas?

T. Hussain, S. Muzahid, A. Narayanan, R. Srianand, B. P. Wakker, J. C. Charlton, A. Pathak

Research output: Contribution to journalArticle

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Abstract

We report the detection of Ne VIII in a zabs = 0.599 61 absorber towards the QSO PG1407+265 (zem=0.94). Besides Ne VIII, absorption from HI Lyman series lines (H I λ1025-λ915), several other low (CII, NII, OII and S II), intermediate (CIII, NIII, NIV, OIII, SIV and S V) and high (S VI, OVI and Ne VIII) ionization metal lines are detected. Disparity in the absorption line kinematics between different ions implies that the absorbing gas comprises of multiple ionization phases. The low and the intermediate ions (except S V) trace a compact (~410 pc), metal-rich (Z ~ Z⊙) and overdense (log nH ~ -2.6) photoionized region that sustained star formation for a prolonged period. The high ions, Ne VIII and OVI, can be explained as arising in a low density (-5.3 ≤ log nH = -5.0), metal-rich (Z ≳ Z⊙) and diffuse (~180 kpc) photoionized gas. The S V, SVI and C IV [detected in the Faint Object Spectrograph (FOS) spectrum] require an intermediate photoionization phase with -4.2 < log nH < -3.5. Alternatively, a pure collisional ionization model, as used to explain the previous known Ne VIII absorbers, with 5.65 < log T < 5.72, can reproduce the S VI, OVI and Ne VIII column densities simultaneously in a single phase. However, even such models require an intermediate phase to reproduce any observable S V and/or C IV. Therefore, we conclude that when multiple phases are present, the presence of Ne VIII is not necessarily an unambiguous indication of collisionally ionized hot gas.

Original languageEnglish (US)
Pages (from-to)2444-2455
Number of pages12
JournalMonthly Notices of the Royal Astronomical Society
Volume446
Issue number3
DOIs
StatePublished - Jan 1 2015

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ionized gases
high temperature gases
tracers
absorbers
ionization
tracer
ion
metal
gas
metals
faint objects
ions
gases
quasars
spectrographs
photoionization
star formation
indication
kinematics
detection

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Hussain, T. ; Muzahid, S. ; Narayanan, A. ; Srianand, R. ; Wakker, B. P. ; Charlton, J. C. ; Pathak, A. / HST/COS detection of a Ne VIII absorber towards PG 1407+265 : An unambiguous tracer of collisionally ionized hot gas?. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 446, No. 3. pp. 2444-2455.
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title = "HST/COS detection of a Ne VIII absorber towards PG 1407+265: An unambiguous tracer of collisionally ionized hot gas?",
abstract = "We report the detection of Ne VIII in a zabs = 0.599 61 absorber towards the QSO PG1407+265 (zem=0.94). Besides Ne VIII, absorption from HI Lyman series lines (H I λ1025-λ915), several other low (CII, NII, OII and S II), intermediate (CIII, NIII, NIV, OIII, SIV and S V) and high (S VI, OVI and Ne VIII) ionization metal lines are detected. Disparity in the absorption line kinematics between different ions implies that the absorbing gas comprises of multiple ionization phases. The low and the intermediate ions (except S V) trace a compact (~410 pc), metal-rich (Z ~ Z⊙) and overdense (log nH ~ -2.6) photoionized region that sustained star formation for a prolonged period. The high ions, Ne VIII and OVI, can be explained as arising in a low density (-5.3 ≤ log nH = -5.0), metal-rich (Z ≳ Z⊙) and diffuse (~180 kpc) photoionized gas. The S V, SVI and C IV [detected in the Faint Object Spectrograph (FOS) spectrum] require an intermediate photoionization phase with -4.2 < log nH < -3.5. Alternatively, a pure collisional ionization model, as used to explain the previous known Ne VIII absorbers, with 5.65 < log T < 5.72, can reproduce the S VI, OVI and Ne VIII column densities simultaneously in a single phase. However, even such models require an intermediate phase to reproduce any observable S V and/or C IV. Therefore, we conclude that when multiple phases are present, the presence of Ne VIII is not necessarily an unambiguous indication of collisionally ionized hot gas.",
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HST/COS detection of a Ne VIII absorber towards PG 1407+265 : An unambiguous tracer of collisionally ionized hot gas? / Hussain, T.; Muzahid, S.; Narayanan, A.; Srianand, R.; Wakker, B. P.; Charlton, J. C.; Pathak, A.

In: Monthly Notices of the Royal Astronomical Society, Vol. 446, No. 3, 01.01.2015, p. 2444-2455.

Research output: Contribution to journalArticle

TY - JOUR

T1 - HST/COS detection of a Ne VIII absorber towards PG 1407+265

T2 - An unambiguous tracer of collisionally ionized hot gas?

AU - Hussain, T.

AU - Muzahid, S.

AU - Narayanan, A.

AU - Srianand, R.

AU - Wakker, B. P.

AU - Charlton, J. C.

AU - Pathak, A.

PY - 2015/1/1

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N2 - We report the detection of Ne VIII in a zabs = 0.599 61 absorber towards the QSO PG1407+265 (zem=0.94). Besides Ne VIII, absorption from HI Lyman series lines (H I λ1025-λ915), several other low (CII, NII, OII and S II), intermediate (CIII, NIII, NIV, OIII, SIV and S V) and high (S VI, OVI and Ne VIII) ionization metal lines are detected. Disparity in the absorption line kinematics between different ions implies that the absorbing gas comprises of multiple ionization phases. The low and the intermediate ions (except S V) trace a compact (~410 pc), metal-rich (Z ~ Z⊙) and overdense (log nH ~ -2.6) photoionized region that sustained star formation for a prolonged period. The high ions, Ne VIII and OVI, can be explained as arising in a low density (-5.3 ≤ log nH = -5.0), metal-rich (Z ≳ Z⊙) and diffuse (~180 kpc) photoionized gas. The S V, SVI and C IV [detected in the Faint Object Spectrograph (FOS) spectrum] require an intermediate photoionization phase with -4.2 < log nH < -3.5. Alternatively, a pure collisional ionization model, as used to explain the previous known Ne VIII absorbers, with 5.65 < log T < 5.72, can reproduce the S VI, OVI and Ne VIII column densities simultaneously in a single phase. However, even such models require an intermediate phase to reproduce any observable S V and/or C IV. Therefore, we conclude that when multiple phases are present, the presence of Ne VIII is not necessarily an unambiguous indication of collisionally ionized hot gas.

AB - We report the detection of Ne VIII in a zabs = 0.599 61 absorber towards the QSO PG1407+265 (zem=0.94). Besides Ne VIII, absorption from HI Lyman series lines (H I λ1025-λ915), several other low (CII, NII, OII and S II), intermediate (CIII, NIII, NIV, OIII, SIV and S V) and high (S VI, OVI and Ne VIII) ionization metal lines are detected. Disparity in the absorption line kinematics between different ions implies that the absorbing gas comprises of multiple ionization phases. The low and the intermediate ions (except S V) trace a compact (~410 pc), metal-rich (Z ~ Z⊙) and overdense (log nH ~ -2.6) photoionized region that sustained star formation for a prolonged period. The high ions, Ne VIII and OVI, can be explained as arising in a low density (-5.3 ≤ log nH = -5.0), metal-rich (Z ≳ Z⊙) and diffuse (~180 kpc) photoionized gas. The S V, SVI and C IV [detected in the Faint Object Spectrograph (FOS) spectrum] require an intermediate photoionization phase with -4.2 < log nH < -3.5. Alternatively, a pure collisional ionization model, as used to explain the previous known Ne VIII absorbers, with 5.65 < log T < 5.72, can reproduce the S VI, OVI and Ne VIII column densities simultaneously in a single phase. However, even such models require an intermediate phase to reproduce any observable S V and/or C IV. Therefore, we conclude that when multiple phases are present, the presence of Ne VIII is not necessarily an unambiguous indication of collisionally ionized hot gas.

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