STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES AT z ∼ 6: NEW INSIGHTS FROM ALMA

By Ran Wang, J. Wagg, C. Carilli, F. Walter, L. Lentati, Xiaohui Fan, D. Riechers, F. Bertoldi, D. Narayanan, M. Strauss and 6 more. 2013

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We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the [C ii] 158 μm 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 × 109 to 8.7 × 109 L☉ and the [C ii]-to-FIR luminosity ratios are 2.9–5.1 × 10−4, 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 1010–1011 M☉. 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.

Subfields: Astronomy and Astrophysics, Instrumentation

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SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, unknown): “…(e.g., Kashikawa et al. 2007; Goto et al. 2009, 2012; Willott et al. 2011) or at sub-mm/radio wavelengths (e.g., Maiolino et al. 2005; Wang et al. 2007; Venemans et al. 2012, 2016; Wang et al. 2013; Willott et al. 2013, 2015), giving a unique probe of galaxies in the reionization era.”
DISCOVERY OF THREE z > 6.5 QUASARS IN THE VISTA KILO-DEGREE INFRARED GALAXY (VIKING) SURVEY (2013, background): “By studying the host galaxies, we get insight into the formation of galaxies in the early universe (e.g., Walter et al. 2009; Wang et al. 2013).”
The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “…2013; Santini et al. 2014; Bothwell et al. 2013; Genzel et al. 2010; Daddi et al. 2010; Carilli & Walter 2013), to investigate their dynamics (e.g. Wang et al. 2013; De Breuck et al. 2014; Carniani et al. 2013; Carilli et al. 2013; Willott et al. 2013, 2015) to trace obscured star formation (e.g.…”
THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE (2016, unknown): “…(29) Zeimann et al. (2011), (30) Morganson et al. (2012), (31) Venemans et al. (2012), (32) McGreer et al. (2013), (33) Venemans et al. (2013), (34) Wang et al. (2013), (35) Willott et al. (2013), (36) Bañados et al. (2014), (37) Calura et al. (2014), (38) Leipski et al. (2014), (39) Bañados et…”
Very extended cold gas, star formation and outflows in the halo of a bright QSO at z>6 (2014, methodology): “We reach a sensitivity of 0.46 mJy beam−1 in channels of 100 km s−1, which is unprecedented for IRAM PdBI observations of high redshift quasars at this frequency (Wang et al. 2013 reach a similar line sensitivity using the Atacama large millimetre/sub-millimetre array (ALMA)).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “…and radio wavelengths of gas in the host galaxy of high-redshift quasars have enabled dynamical estimates of the host galaxies up to the highest redshifts (e.g., Walter et al. 2004; Schumacher et al. 2012; Wang et al. 2013; Willott et al. 2013, 2015; Venemans et al. 2016, 2017a; Shao et al. 2017).”
Physical Properties of 15 Quasars at z ≳ 6.5 (2017, background): “Walter et al. (2009) and Wang et al. (2013) observe quasars with high LFIR, and show that they are characterized by low luminosity ratios, comparable to local ULIRGS (〈log(L[CII]/LFIR)〉 ∼ −3.5).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “Further X-ray analysis of SMGs estimate AGN fractions of 20%–29(±7)% (Laird et al., 2010), 26%±9% (Georgantopoulos et al., 2011), 14%–28% (Johnson et al., 2013) and 17(+16 −6 )% (Wang et al., 2013a).”
AN INTENSELY STAR-FORMING GALAXY AT z ∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND HST OBSERVATIONS (2013, background): “…been observed at sub-mm wavelengths to z = 6.4 − 7.1 (Maiolino et al. 2005; Iono et al. 2006; Walter et al. 2009; Venemans et al. 2012; Willott et al. 2013; Wang et al. 2013), the presence of a powerful AGN undoubtedly complicates any understanding of the physical conditions in their host galaxies.”
THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7 (2016, methodology): “…rich information about dust emission and star formation in the host galaxies (e.g., Jiang et al. 2006, 2010; Walter et al. 2009; Gallerani et al. 2010; Wang et al. 2011, 2013; Carilli & Walter 2013; Omont et al. 2013; Calura et al. 2014; Leipski et al. 2014; Bañados et al. 2015; Lyu et al. 2016).”
Evidence of patchy hydrogen reionization from an extreme Lyα trough below redshift six (2014, methodology): “For ULAS J1319+0959 we adopt zem = 6.133 based on [C ii] 158 µm measurements from Wang et al. (2013).”
BLACK HOLE MASS ESTIMATES AND EMISSION-LINE PROPERTIES OF A SAMPLE OF REDSHIFT z > 6.5 QUASARS (2013, background): “…et al. 2012), the formation and early growth of supermassive black holes (SMBHs; e.g., Volonteri 2010; Latif et al. 2013), the galaxy formation processes (e.g., Walter et al. 2009; Wang et al. 2013), and the interstellar medium chemical evolution (e.g., Jiang et al. 2007; Simcoe et al. 2011, 2012).”