Dust emission from the most distant quasars

By F. Bertoldi, C. Carilli, P. Cox, Xiaohui Fan, M. Strauss, A. Beelen, A. Omont, R. Zylka. 2003

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We report observations of three SDSS z>6 QSOs at 250 GHz (1.2mm) using the 117-channel Max-Planck Millimeter Bolometer (MAMBO-2) array at the IRAM 30-meter telescope. J1148+5251 (z=6.41) and J1048+4637 (z=6.23) were detected with 250 GHz flux densities of 5.0 +- 0.6 mJy and 3.0 +- 0.4 mJy, respectively. J1630+4012 (z=6.05) was not detected with a 3 sigma upper limit of 1.8 mJy. Upper flux density limits from VLA observations at 43 GHz for J1148+5251 and J1048+4637 imply steeply rising spectra, indicative of thermal infrared emission from warm dust. The far-infrared luminosities are estimated to be \\~10^13 L_sun, and the dust masses ~10^8 M_sun, assuming Galactic dust properties. The presence of large amounts of dust in the highest redshift QSOs indicates that dust formation must be rapid during the early evolution of QSO host galaxies. Dust absorption may hinder the escape of ionizing photons which reionize the intergalactic medium at this early epoch.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6516678fa99d3b049c1635276fe1a84683ea8580

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Citations in the corpus

Spitzer Quasar and ULIRG Evolution Study (QUEST). II. The Spectral Energy Distributions of Palomar-Green Quasars (2007, background): “Deep sub-mm and mm photometry has led to the detection of rest frame submm and far-infrared dust emission from radio-quiet quasars at redshifts up to 6.42 (e,g, Omont et al. 2001; Isaak et al. 2002; Bertoldi et al. 2003).”
Production of dust by massive stars at high redshift (2011, background): “…from high-z QSOs at sub-millimeter and millimeter wavelengths (e.g., Omont et al, 2001, 2003; Carilliet al, 2001b; Bertoldi and Cox, 2002) indicates far-infrared luminosities≥ 1012−13 L⊙, implying dust masses of≥ 108 M⊙ and star-formation rates up to 3000 M⊙ yr−1 (e.g., Bertoldi et al, 2003).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “Both the gas in the broad line region around the central black hole, and the interstellar medium (ISM) of their host galaxies, appear metal-enriched (e.g., Bertoldi et al. 2003a, 2003b; Walter et al. 2003; Beelen et al. 2006; De Rosa et al. 2011; Mortlock et al. 2011).”
Emission-line diagnostics of low-metallicity active galactic nuclei (2006, background): “While it is unknown whether low metallicity AGN will contain dust, the observations of dust in high-zobjects indicates that such an assumption is not unreasonable (Bertoldi et al. 2003).”
Resolved Molecular Gas in a Quasar Host Galaxy at Redshift z = 6.42 (2004, methodology): “…section) and that the gas seen in the PdBI spectrum emerges from the same region (full width at zero intensity: 560 km s−1 or vrot ∼280km s −1, Bertoldi et al. 2003b), we derive an approximate dynamical mass for J1148+5251 of ∼ 4.5 × 1010 M⊙ (or ∼ 5.5 × 1010 M⊙ if we correct for an…”
Cool Gas in High-Redshift Galaxies (2013, unknown): “…350GHz (850µm), the following relations are commonly used: LFIR[L⊙] ∼ 1.2×10 12S350GHz[mJy] (e.g. Genzel et al. 2010, Pope et al. 2006, Magnelli et al. 2010), LFIR[L⊙] ∼ 3×10 12S250GHz[mJy] (e.g. Bertoldi et al. 2003, Omont et al. 2001), with significant dependencies on the actual shape of the SED.”
Four Quasars above Redshift 6 Discovered by the Canada-France High-z Quasar Survey (2007, background): “Their properties and detection rate, as well as the CO detection in J1148+5251 (Bertoldi et al. 2003b; Walter et al. 2003, 2004), are comparable to other high-z strong starburst quasars.”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “…observations have shown that even at the highest redshifts (z > 4) galaxies can have significant reservoirs of dust (107 M or even greater, Bertoldi et al. 2003; Hughes, Dunlop & Rawlings 1997; Valiante et al. 2009; Venemans et al. 2012; Casey, Narayanan & Cooray 2014; Riechers et al.…”
Iron Emission in the z = 6.4 Quasar SDSS J114816.64+525150.3 (2003, background): “…was evidently a site of vigorous massive star formation and metal enrichment prior toz = 6.4, as demonstrated by the roughly normal equivalent width of the MgII emission line as well as the presence of submillimeter emission from 108 M of dust in the quasar host galaxy (Bertoldi et al. 2003).”
Fragmentation of star-forming clouds enriched with the first dust (2006, methodology): “…time-scales in SN ejecta provides a straightforward interpretation of the large dust masses (M dust ∼ 109 M ) inferred from mm and sub-mm observations of quasars [quasi-stellar objects (QSOs)] with redshifts 5.7 < z < E-mail: raffa@arcetri.astro.it 6.42 (Bertoldi et al. 2003; Priddey et al. 2003).”
Evidence of strong quasar feedback in the early Universe (2012, background): “The strong far-IR thermal emission inferred from (sub-)millimeter observations reveals vigorous star formation in the host galaxy, with SFR ∼ 3000 M⊙ yr−1 (Bertoldi et al. 2003a; Beelen et al. 2006).”
Dust formation and survival in supernova ejecta (2007, background): “The inferred far-IR luminosities are consistent with thermal emission from warm dust (T < 100 K), with dust masses > 108M⊙ (Bertoldi et al. 2003; Robson et al. 2004; Beelen et al. 2006; Hines et al. 2006).”
The Evolution of Dust in the Early Universe with Applications to the Galaxy SDSS J1148+5251 (2007, background): “…(IR) and submillimeter wavelengths (Hughes et al. 1998; Bertoldi et al. 2003a; Robson et al. 2004; Beelen et al. 2006) exhibit luminosities in excess of ∼ 1013 L⊙, and inferred dust masses and star formation rates in excess of ∼ 108 M⊙ and of ∼ 10 3 M⊙ yr −1, respectively (Bertoldi et al. 2003a).”
DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj (2009, background): “This comes from a variety of observations such as sub-mm and near-infrared (NIR) studies of the most distant quasars (Bertoldi et al. 2003; Maiolino et al. 2004), obscuration by dust of quasars in damped Ly-α systems (Pei et al. 1991), and measurements of metal abundances in these systems (Pettini…”
350 μm Dust Emission from High-Redshift Quasars (2006, background): “Amassive reservoir of densemolecular gas ( 2 ; 1010 M ) is implied by the observed CO emission (Walter et al. 2003; Bertoldi et al. 2003b) and the recent detection of the [C ii] emission line (Maiolino et al. 2005).”
Spitzer Quasar and ULIRG Evolution Study (QUEST). I. The Origin of the Far-Infrared Continuum of QSOs (2006, background): “Implications for High-Redshift QSOs Deep submillimeter and millimeter photometry has led to the detection of rest-frame submillimeter and FIR dust emission from radio-quiet QSOs at redshifts up to 6.42 (e.g., Omont et al. 2001; Isaak et al. 2002; Bertoldi et al. 2003).”
The transition from population III to population II-I star formation (2010, background): “None the less, the presence of large amounts of dust and heavy elements has been detected at moderately-high redshift, i.e. atz > 6, when the Universe is younger than∼ 1 Gyr (e.g. Bertoldi et al. 2003; Maiolino et al. 2004).”
Extragalactic optical-infrared background radiation, its time evolution and the cosmic photon-photon opacity (2008, methodology): “Finally, the long-wavelength portion of galaxy emission, at 350 to 1200µm, has been sampled by ground-based millimetric and sub-millimetric telescopes with sensitive bolometriccameras (SCUBA on JCMT, see e.g. Blain et al. 2002; BOLOCAM and MAMBO on IRAM, e.g. Bertoldi et al. 2003).”
The large APEX bolometer camera LABOCA (2008, background): “Carilli et al. 2001; Bertoldi et al. 2003; Wang et al. 2008), revealing star-formation rates (SFRs) that are hundreds of times higher than in the Milky Way today.”