TY - JOUR
T1 - Quantifying the thermal Sunyaev-Zel'dovich effect and excess millimetre emission in quasar environments
AU - Hall, Kirsten R.
AU - Zakamska, Nadia L.
AU - Addison, Graeme E.
AU - Battaglia, Nicholas
AU - Crichton, Devin
AU - Devlin, Mark
AU - Dunkley, Joanna
AU - Gralla, Megan
AU - Colin Hill, J.
AU - Hilton, Matt
AU - Hubmayr, Johannes
AU - Hughes, John P.
AU - Huffenberger, Kevin M.
AU - Kosowsky, Arthur
AU - Marriage, Tobias A.
AU - Maurin, Loïc
AU - Moodley, Kavilan
AU - Niemack, Michael D.
AU - Page, Lyman A.
AU - Partridge, Bruce
AU - Planella, Rolando Dünner
AU - Schillaci, Alessandro
AU - Sifón, Cristóbal
AU - Staggs, Suzanne T.
AU - Wollack, Edward J.
AU - Xu, Zhilei
N1 - Funding Information:
DC acknowledges the financial assistance of the South African Radio Astronomy Observatory (http://www.ska.ac.za). KM acknowledges support from the National Research Foundation of South Africa. LM is funded by the Comisión Nacional de In-vestigación Científica y Tecnológica de Chile Fondo Nacional de Desarrollo Científ ico y Tecnológico. grant no. 3170846.
Funding Information:
This work was supported by the U.S. National Science Foundation through awards AST-1440226, AST-0965625 and AST-0408698 for the Atacama Cosmology Telescope project, as well as awards PHY-1214379 and PHY-0855887. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation award to the University of British Columbia. Atacama Cosmology Telescope operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile.
Publisher Copyright:
© 2019 The Author(s)
PY - 2019/12/1
Y1 - 2019/12/1
N2 - In this paper, we probe the hot, post-shock gas component of quasar-driven winds through the thermal Sunyaev-Zel'dovich (tSZ) effect. Combining data sets from the Atacama Cosmology Telescope, the Herschel Space Observatory, and the Very Large Array, we measure average spectral energy distributions of 109 829 optically selected, radio quiet quasars from 1.4 to 3000 GHz in six redshift bins between 0.3 < z < 3.5. We model the emission components in the radio and far-infrared, plus a spectral distortion from the tSZ effect. At z > 1.91, we measure the tSZ effect at 3.8σ significance with an amplitude corresponding to a total thermal energy of 3.1 × 1060 erg. If this energy is due to virialized gas, then our measurement implies quasar host halo masses are ∼6 × 1012 h−1 M☉. Alternatively, if the host dark matter halo masses are ∼2 × 1012 h−1 M☉ as some measurements suggest, then we measure a >90 per cent excess in the thermal energy over that expected due to virialization. If the measured SZ effect is primarily due to hot bubbles from quasar-driven winds, we find that (5+1.2-1.3) per cent of the quasar bolometric luminosity couples to the intergalactic medium over a fiducial quasar lifetime of 100 Myr. An additional source of tSZ may be correlated structure, and further work is required to separate the contributions. At z ≤ 1.91, we detect emission at 95 and 148 GHz that is in excess of thermal dust and optically thin synchrotron emission. We investigate potential sources of this excess emission, finding that CO line emission and an additional optically thick synchrotron component are the most viable candidates.
AB - In this paper, we probe the hot, post-shock gas component of quasar-driven winds through the thermal Sunyaev-Zel'dovich (tSZ) effect. Combining data sets from the Atacama Cosmology Telescope, the Herschel Space Observatory, and the Very Large Array, we measure average spectral energy distributions of 109 829 optically selected, radio quiet quasars from 1.4 to 3000 GHz in six redshift bins between 0.3 < z < 3.5. We model the emission components in the radio and far-infrared, plus a spectral distortion from the tSZ effect. At z > 1.91, we measure the tSZ effect at 3.8σ significance with an amplitude corresponding to a total thermal energy of 3.1 × 1060 erg. If this energy is due to virialized gas, then our measurement implies quasar host halo masses are ∼6 × 1012 h−1 M☉. Alternatively, if the host dark matter halo masses are ∼2 × 1012 h−1 M☉ as some measurements suggest, then we measure a >90 per cent excess in the thermal energy over that expected due to virialization. If the measured SZ effect is primarily due to hot bubbles from quasar-driven winds, we find that (5+1.2-1.3) per cent of the quasar bolometric luminosity couples to the intergalactic medium over a fiducial quasar lifetime of 100 Myr. An additional source of tSZ may be correlated structure, and further work is required to separate the contributions. At z ≤ 1.91, we detect emission at 95 and 148 GHz that is in excess of thermal dust and optically thin synchrotron emission. We investigate potential sources of this excess emission, finding that CO line emission and an additional optically thick synchrotron component are the most viable candidates.
KW - (Galaxies:) intergalactic medium
KW - (Galaxies:) quasars: general
KW - Galaxies: active
KW - Galaxies: evolution
UR - http://www.scopus.com/inward/record.url?scp=85079621771&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85079621771&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz2751
DO - 10.1093/mnras/stz2751
M3 - Article
AN - SCOPUS:85079621771
SN - 0035-8711
VL - 490
SP - 2315
EP - 2335
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -