A possibleChandraandHubble Space Telescopedetection of extragalactic WHIM towards PG 1116+215

Authors:
  • MBM. Bonamente
    M. Bonamente
  • JNJ. Nevalainen
    J. Nevalainen
  • ETE. Tilton
    E. Tilton
  • JLJ. Liivamägi
    J. Liivamägi
  • PHP. Heinämäki
    P. Heinämäki
  • TFT. Fang
    T. Fang
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Abstract
We have analysed Chandra low energy transmission grating and XMM–Newton Reflection Grating Spectrometer (RGS) spectra towards the z = 0.177 quasar PG 1116+215, a sightline that is rendered particularly interesting by the Hubble Space Telescope (HST) detection of several O vi and H i broad Lyman α absorption (BLA) lines that may be associated with the warm–hot intergalactic medium (WHIM). We performed a search for resonance Kα absorption lines from O vii and O viii at the redshifts of the detected far-ultraviolet lines. We detected an absorption line in the Chandra spectra at the 5.2σ confidence level at wavelengths corresponding to O viii Kα at z = 0.0911 ± 0.0004 ± 0.0005 (statistical followed by systematic error). This redshift is within 3σ of that of an H i broad Lyman α of b ≃ 130 km s−1 (corresponding to a temperature of log T(K) ≃ 6.1) at z = 0.092 79 ± 0.000 05. We have also analysed the available XMM–Newton RGS data towards PG 1116+215. Unfortunately, the XMM–Newton data are not suitable to investigate this line because of instrumental features at the wavelengths of interest. At the same redshift, the Chandra and XMM–Newton spectra have O vii Kα absorption-line features of significance 1.5σ and 1.8σ, respectively. We also analysed the available Sloan Digital Sky Survey (SDSS) spectroscopic galaxy survey data towards PG 1116+215 in the redshift range of interest. We found evidence for a galaxy filament that intersect the PG 1116+215 sightline and additional galaxy structures that may host WHIM. The H i BLA and the O viii Kα absorbers are within a few Mpc of the filament (assuming that redshifts track Hubble flow distances) or consistent with gas accreting on to the filament from either direction relative to the sightline with velocities of a few × 100 km s−1. The combination of HST, Chandra, XMM–Newton and SDSS data indicates that we have likely detected a multi-temperature WHIM at z ≃ 0.091–0.093 towards PG 1116+215. The O viii Kα absorption line indicates gas at high temperature, log T(K) ≥ 6.4, with a total column density of the order of log NH(cm2) ≥ 20 and a baryon overdensity δb ∼ 100–1000 for sightline lengths of L = 1–10 Mpc. This detection highlights the importance of BLA absorption lines as possible signposts of high-temperature WHIM filaments.
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