We present Ly α , He ii , and C iv observations of seven z ∼ 2 radio-loud quasars observed using the Keck Cosmic Web Imager and compare it to observed radio jet emission using archival Very Large Array and Atacama Large Millimeter/submillimeter Array radio observations. We detect 80–120 kpc diameter Ly α and 10–40 kpc He ii and C iv emission around the targets. We find the Ly α emission to be brighter within the inner 30 kpc by factors of 2–10 compared to other literature samples. We reproduce the trend for increased total luminosity for a larger on-sky area, but find our targets tend to be brighter for a given area when compared to literature observations, even when adjusting for the observational sensitivity. We infer that the He ii and C iv is likely powered by quasar photoionization, with the ionizing radiation likely escaping along the radio jet axis, which is aligned with the He ii and C iv emission. The observations agree with a two-component model of the circumgalactic medium (CGM), where the inner CGM (<30 kpc) is directly influenced by the host galaxies, whereas gas motions in the outer CGM (>30 kpc) are governed by turbulence and the larger-scale environment.
- The Two-component Circumgalactic Medium Emission around z ∼ 2 Radio-loud Quasars
- Sanchit Sabhlok - University of ArizonaShelley A. Wright - University of California San DiegoAndrey Vayner - California Institute of TechnologyNorman Murray - University of TorontoLee Armus - California Institute of TechnologyMaren Cosens - Carnegie ObservatoriesJames Wiley - California Institute of TechnologyEileen Meyer - University of Maryland, Baltimore CountyKarthik Reddy - California Institute of TechnologyMarie Wingyee Lau - University of California, Riverside
- The Astrophysical journal, Vol.1002(2), p.170
- IOP Publishing Ltd; Bristol
- 17
- National Aeronautics and Space Administration: ALMA 2017.1.01527 W. M. Keck Foundation
The authors wish to thank Jim Lyke, Randy Campbell, Sherry Yeh, and the other SAs at the Keck Observatory for their assistance in obtaining the data presented in this work. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2017.1.01527.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
- 99385962036006570
- Department of Chemistry & Physics
- English
- Journal article