| Title | Resolved [C II] Emission from z > 6 Quasar Host-Companion Galaxy Pairs |
| Authors | Neeleman, Marcel Banados, Eduardo Walter, Fabian Decarli, Roberto Venemans, Bram P. Carilli, Chris L. Fan, Xiaohui Farina, Emanuele P. Mazzucchelli, Chiara Novak, Mladen Riechers, Dominik A. Rix, Hans-Walter Wang, Ran |
| Affiliation | Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany Natl Radio Astron Observ, Socorro, NM 87801 USA INAF Osservatorio Astrofis & Sci Spazio Bol, Via Gobetti 93-3, I-40129 Bologna, Italy Univ Cambridge, Cavendish Astrophys Grp, Cambridge CB3 0HE, England Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany European Southern Observ, Alonso de Cordova 3107, Vitacura, Region Metropol, Chile Cornell Univ, Space Sci Bldg, Ithaca, NY 14853 USA Peking Univ, Kavli Inst Astron & Astrophys, 5 Yiheyuan Rd, Beijing 100871, Peoples R China |
| Keywords | galaxies: high-redshift galaxies: interactions galaxies: ISM galaxies: kinematics and dynamics quasars: emission lines submillimeter: galaxies |
| Issue Date | 2019 |
| Publisher | ASTROPHYSICAL JOURNAL |
| Abstract | We report on approximate to 0 ''.135 (approximate to 2kpc) resolution observations of the [C II] and dust continuum emission from five z > 6 quasar host companion galaxy pairs obtained with the Atacama Large Millimeter/submillimeter Array. The [C II] emission is resolved in all galaxies, with physical extents of 3.2-5.4 kpc. The dust continuum is on-average 40% more compact, which results in larger [C II] deficits in the center of the galaxies. However, the measured [C II] deficits are fully consistent with those found at lower redshifts. Four of the galaxies show [C II] velocity fields that are consistent with ordered rotation, while the remaining six galaxies show no clear velocity gradient. All galaxies have high (-80 -200 km s(-1)) velocity dispersions, consistent with the interpretation that the interstellar medium (ISM) of these highredshift galaxies is turbulent. By fitting the galaxies with kinematic models, we estimate the dynamical mass of these systems, which ranges between (0.3- >5.4) x 10(10) M-circle dot. For the three closest-separation galaxy pairs, we observe dust and [C II] emission from gas in between and surrounding the galaxies, which is an indication that tidal interactions are disturbing the gas in these systems. Although gas exchange in these tidal interactions could power luminous quasars, the existence of quasars in host galaxies without nearby companions suggests that tidal interactions are not the only viable method for fueling their active centers. These observations corroborate the assertion that accreting supermassive black holes do not substantially contribute to the [C II] and dust continuum emission of the quasar host galaxies, and showcase the diverse ISM properties of galaxies when the universe was less than one billion years old. |
| URI | http://hdl.handle.net/20.500.11897/545523 |
| ISSN | 0004-637X |
| DOI | 10.3847/1538-4357/ab2ed3 |
| Indexed | SCI(E) EI |
| Appears in Collections: | 科维理天文与天体物理研究所 |
