DETECTION OF ATOMIC CARBON [C ii] 158 μm AND DUST EMISSION FROM A z = 7.1 QUASAR HOST GALAXY

By B. Venemans, R. McMahon, F. Walter, R. Decarli, P. Cox, R. Neri, Paul Hewett, Daniel J. Mortlock, C. Simpson, S. E. M. Heidelberg and 6 more. 2012

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Using the IRAM Plateau de Bure Interferometer, we report the detection of the 158 μm [C ii] emission line and underlying dust continuum in the host galaxy of the quasar ULAS J112001.48+064124.3 (hereafter J1120+0641) at z = 7.0842 ± 0.0004. This is the highest redshift detection of the [C ii] line to date, and allows us to put the first constraints on the physical properties of the host galaxy of J1120+0641. The [C ii] line luminosity is 1.2 ± 0.2 × 109 L☉, which is a factor ∼4 lower than observed in a luminous quasar at z = 6.42 (SDSS J1148+5251). The underlying far-infrared (FIR) continuum has a flux density of 0.61 ± 0.16 mJy, similar to the average flux density of z ∼ 6 quasars that were not individually detected in the rest-frame FIR. Assuming that the FIR luminosity of LFIR = 5.8 × 1011–1.8 × 1012 L☉ is mainly powered by star formation, we derive a star formation rate in the range 160–440 M☉ yr−1 and a total dust mass in the host galaxy of 6.7 × 107–5.7 × 108 M☉ (both numbers have significant uncertainties given the unknown nature of dust at these redshifts). The [C ii] line width of σV = 100 ± 15 km s−1 is among the smallest observed when compared to the molecular line widths detected in z ∼ 6 quasars. Both the [C ii] and dust continuum emission are spatially unresolved at the current angular resolution of 2.0 × 1.7 arcsec2 (corresponding to 10 × 9 kpc2 at the redshift of J1120+0641).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2d34d9e2c3356602525307689b3fa7e35ba77217

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Citations in the corpus

Cool Gas in High-Redshift Galaxies (2013, background): “More recently, [C II] is now being detected in quasar host galaxies, including the most distant quasar known with a spectroscopic redshift at z=7.1 (Venemans et al. 2012).”
BLACK HOLE MASS ESTIMATES AND EMISSION-LINE PROPERTIES OF A SAMPLE OF REDSHIFT z > 6.5 QUASARS (2013, background): “For high-redshift quasars, it is possible to obtain a direct estimate of the systemic redshift through the detection of cold molecular gas phase in the host galaxy (e.g., Walter et al. 2003; Wang et al. 2010; Venemans et al. 2012).”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “This suggests that the buildup of dust starts at high redshift, as suggested by observations (Bertoldi et al. 2003; Hughes, Dunlop & Rawlings 1997; Valiante et al. 2009; Venemans et al. 2012; Casey, Narayanan & Cooray 2014; Riechers et al. 2014; Watson et al. 2015).”
THE BRIGHTEST OF REIONIZING GALAXIES SURVEY: CONSTRAINTS ON THE BRIGHT END OF THE z ∼ 8 LUMINOSITY FUNCTION (2012, background): “If these candidates are spectroscopically confirmed, this would allow us to possibly extend the detection of [C ii] 158 μm, high-J CO emission lines, and perhaps dust emission as well, to z ∼ 8, after the recent record established at z = 7.1 from a QSO host galaxy (Venemans et al. 2012).”
The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “However, at z∼7, well within the re-ionization epoch, only one quasar host galaxy has been detected in [CII] and in continuum (at z=7.08, Venemans et al. 2012).”
Physical Properties of 15 Quasars at z ≳ 6.5 (2017, methodology): “This is similar to what was found by Venemans et al. (2012, 2017) for ULAS1120, and suggests that the host galaxies of these quasars are more similar to ULIRGS.”
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.”
Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era (2018, background): “In the past decade, substantial amounts of dust ranging from 106 to ☉M108 have been identified in z>7 galaxies and quasars (Venemans et al. 2012, 2017; Watson et al. 2015; Laporte et al. 2017; Hashimoto et al. 2018a), which poses a challenge to the current theory of dust formation (Michałowski…”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “…offered by the IRAM Plateau de Bure Interferometer (PdBI; now upgraded to the NOrthern Extended Millimeter Array, NOEMA; Walter et al. 2009; Venemans et al. 2012; Bañados et al. 2015; Mazzucchelli et al. 2017) and on the advent of the Atacama Large Millimeter Array (ALMA; Wang et al. 2013;…”
STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES AT z ∼ 6: NEW INSIGHTS FROM ALMA (2013, background): “…of 1.5× the FWHM major axis from the [C ii] intensity map (i.e., full width at 20% of the peak intensity for a Gaussian profile). detections in this work, J1148+5251 (Maiolino et al. 2005), CFHQS J0210−0456 at z = 6.43 (Willott et al. 2013), and ULAS J1120+0640 at z = 7.08 (Venemans et al. 2012).”
DISCOVERY OF THREE z > 6.5 QUASARS IN THE VISTA KILO-DEGREE INFRARED GALAXY (VIKING) SURVEY (2013, background): “This one z ∼ 7 quasar already provides constraints on the neutral fraction of hydrogen up to z = 7.1 (Bolton et al. 2011; Mortlock et al. 2011), on the metallicity of the IGM (Simcoe et al. 2012) and on the formation of dust and stars in the host galaxy (Venemans et al. 2012).”
THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE (2016, unknown): “…(26) De Rosa et al. (2011), (27) Mortlock et al. (2011), (28) Wang et al. (2011), (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…”
AN INTENSELY STAR-FORMING GALAXY AT z ∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND HST OBSERVATIONS (2013, background): “Although a few QSOs have 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…”