STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES AT z {approx} 6: NEW INSIGHTS FROM ALMA
- National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM 87801 (United States)
- European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19 (Chile)
- Max-Planck-Institute for Astronomy, Koenigsstuhl 17, D-69117 Heidelberg (Germany)
- Astrophysics Group, Cavendish Laboratory, JJ Thomson Avenue, Cambridge CB3 0HE (United Kingdom)
- Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)
- Astronomy Department, Cornell University, 220 Space Sciences Building, Ithaca, NY 14853 (United States)
- Argelander-Institut fuer Astronomie, University of Bonn, Auf dem Huegel 71, D-53121 Bonn (Germany)
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States)
- Institute de Radioastronomie Millimetrique, F-38406 St. Martin d'Heres (France)
- Institut d'Astrophysique de Paris, CNRS and Universite Pierre et Marie Curie, F-75014 Paris (France)
- Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 71, D-53121 Bonn (Germany)
- Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, SE-43992 Onsala (Sweden)
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1504 (United States)
We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the [C II] 158 {mu}m fine structure line and dust continuum emission from the host galaxies of five redshift 6 quasars. We also report complementary observations of 250 GHz dust continuum and CO (6-5) line emission from the z = 6.00 quasar SDSS J231038.88+185519.7 using the IRAM facilities. The ALMA observations were carried out in the extended array at 0.''7 resolution. We have detected the line and dust continuum in all five objects. The derived [C II] line luminosities are 1.6 Multiplication-Sign 10{sup 9} to 8.7 Multiplication-Sign 10{sup 9} L{sub Sun} and the [C II]-to-FIR luminosity ratios are 2.9-5.1 Multiplication-Sign 10{sup -4}, which is comparable to the values found in other high-redshift quasar-starburst systems and local ultra-luminous infrared galaxies. The sources are marginally resolved and the intrinsic source sizes (major axis FWHM) are constrained to be 0.''3-0.''6 (i.e., 1.7-3.5 kpc) for the [C II] line emission and 0.''2-0.''4 (i.e., 1.2-2.3 kpc) for the continuum. These measurements indicate that there is vigorous star formation over the central few kpc in the quasar host galaxies. The ALMA observations also constrain the dynamical properties of the star-forming gas in the nuclear region. The intensity-weighted velocity maps of three sources show clear velocity gradients. Such velocity gradients are consistent with a rotating, gravitationally bound gas component, although they are not uniquely interpreted as such. Under the simplifying assumption of rotation, the implied dynamical masses within the [C II]-emitting regions are of order 10{sup 10}-10{sup 11} M{sub Sun }. Given these estimates, the mass ratios between the supermassive black holes and the spheroidal bulge are an order of magnitude higher than the mean value found in local spheroidal galaxies, which is in agreement with results from previous CO observations of high redshift quasars.
- OSTI ID:
- 22140258
- Journal Information:
- Astrophysical Journal, Vol. 773, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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