Draft version March 10, 2021 Preprint typeset using LATEX style emulateapj v. 5/2/11 ABSORPTION-LINE DETECTIONS OF 105−6 K GAS IN SPIRAL-RICH GROUPS OF GALAXIES John T. Stocke, Brian A. Keeney, Charles W. Danforth, David Syphers, H. Yamamoto, J. Michael Shull, James C. Green & Cynthia Froning Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA;
[email protected] Blair D. Savage, Bart Wakker & Tae-Sun Kim Department of Astronomy, U of Wisconsin, Madison, WI 53706 Emma V. Ryan-Weber & Glenn G. Kacprzak Centre for Astrophysics & Supercomputing, Swinburne University of Technology, VIC 3122, Australia Draft version March 10, 2021 ABSTRACT Using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) the COS Science Team has conducted a high signal-to-noise survey of 14 bright QSOs. In a previous paper (Savage et al. 2014) these far-UV spectra were used to discover 14 “warm” (T 105 K) absorbers using a combination of broad Lyα and broad O VI absorptions. A reanalysis of a few≥ of this new class of absorbers using slightly relaxed fitting criteria finds as many as 20 warm absorbers could be present in this sample. A shallow, wide spectroscopic galaxy redshift survey has been conducted around these sightlines to investigate the warm absorber environment, which is found to be spiral-rich groups or cluster outskirts with radial velocity dispersions σ = 250-750 km s−1. While 2σ evidence is presented favoring the hypothesis that these absorptions are associated with the galaxy groups and not with the individual, nearest galaxies, this evidence has considerable systematic uncertainties and is based on a small sample size so it is not entirely conclusive.