350 μm Dust Emission from High‐Redshift Quasars

Beelen, A.; Cox, P.; Benford, Dominic J.; Dowell, C. D.; Kovács, A.; Bertoldi, F.; Omont, A.; Carilli, C. L.

doi:10.1086/500636

Cited by 336 publications

(563 citation statements)

References 46 publications

(88 reference statements)

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“…It was detected as a bright quasar at a redshift of 6.42 in SDSS . The source is bright in submm wavelengths with a far-infrared luminosity of a HyLIRG with value ∼ 2 × 10 13 L (Beelen et al, 2006) and a SFR in excess of 3000 M yr −1 . It is also gas rich with a total molecular gas mass of ∼ 2.5 × 10 10 M distributed over a diameter of 5 kpc (Walter et al, 2003).…”

Section: J1148+5251mentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: J1148+5251mentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…While the uncertainties for the SFRs are inhomogeneously determined and perhaps underestimated, if we trust those uncertainties and calculate weightedaverage properties of the two populations, we find t =  17 1 Myr for AGN host galaxies, t =  20 1 Myr for SMGs, and t =  18.4 0.9 Myr for both populations combined. Mid-IR excesses are known to arise in the dusty tori of AGNs (e.g., Weiß et al 2003;Beelen et al 2006), and it is plausible that highly obscured AGNs would have some FIR emission that does Figure 9. Redshift (top left), dust temperature (top right), CO(3-2) line FWHM (bottom left), and dust-to-gas ratio (bottom right) as afunction of r 3,1 for the complete sample of SMGs (blue circles) and AGNs (red squares).…”

Section: Excitation Dependence Of Galaxies' Star-formation Propertiesmentioning

confidence: 99%

“…The higher SFEs appearto be due to larger average FIR luminosities for the AGN host galaxies over the same range of molecular gas masses in the SMGs, which may be due to a dusty torus contribution to the FIR luminosity that is not actually tracing star formation (e.g., Weiß et al 2003;Beelen et al 2006;Leipski et al 2013;Kirkpatrick et al 2015). If we force the linear fit between the FIR and CO luminosities in the Schmidt-Kennicutt relation to have the same index (N = 1) for both SMGs and AGN host galaxies (in order to control for additional uncertainties in the index of the power law), the difference between the offsets measures the fraction of the FIR luminosity for the AGN host galaxies that is in excess of what would be predicted for pure starburst systems (the SMGs).…”

Section: Excitation and Evidence For An Smg-quasar Transitionmentioning

confidence: 99%

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Sharon

Riechers

Hodge

et al. 2016

ApJ

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130

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We present CO(1-0) observations obtained at the Karl G. Jansky Very Large Array for 14z 2 galaxies with existing CO(3-2) measurements, including 11 galaxies thatcontain active galactic nuclei (AGNs) and three submillimeter galaxies (SMGs). We combine this sample with an additional 15z 2 galaxies from the literature that have both CO(1-0) and CO(3-2) measurements in order to evaluate differences in CO excitation between SMGs and AGN host galaxies, tomeasure the effects of CO excitation on the derived molecular gas properties of these populations, and to look for correlations between the molecular gas excitation and other physical parameters. With our expanded sample of CO(3-2)/CO(1-0) line ratio measurements, we do not find a statistically significant difference in the mean line ratio between SMGs and AGN host galaxies as can be found in the literature; we instead find =  r 1.03 0. for both populations combined). We also do not measure a statistically significant difference between the distributions of the line ratios for these populations at the p=0.05 level, although this result is less robust. We find no excitation dependence on the index or offset of the integrated Schmidt-Kennicutt relation for the two CO lines, and weobtain indices consistent with N=1 for the various subpopulations. However, including low-z "normal" galaxies increases our best-fit Schmidt-Kennicutt index toÑ 1.2. While we do not reproduce correlations between the CO line width and luminosity, we do reproduce correlations between CO excitation and star-formation efficiency.

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“…Yet the typical dust temperature at ultra-luminous infrared galaxies (ULIRGs) can be as low as 25-35 K (Hwang et al 2010). Thus, the FIR dust temperature is allowed to vary from 10 to 60 K. The initial temperature is set to be 44 K, the mean FIR dust temperature of the high-z quasars (Beelen et al 2006;Leipski et al 2013). To achieve a reliable temperature, the FIR data should be sampled around the peak of the SED at FIR.…”

Section: Fir Dust Temperaturementioning

confidence: 99%

“…It might be due to the fact that we exclude AGN contribution at the FIR. Beelen et al (2006) detected six high-redshift (1.8 z 6.4) optically luminous radio-quiet quasars at 350 μm using the SHARC-II bolometer camera at the Caltech Submillimeter Observatory. They found the mean value of the graybody temperature was 47 ± 3 K with a dust emissivity index of β = 1.6 ± 0.1.…”

Section: Fir Dust Temperaturementioning

confidence: 99%

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

2016

ApJ

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In this work, we present a study of 207 quasars selected from the Sloan Digital Sky Survey quasar catalogs and the Herschel Stripe 82 survey. Quasars within this sample are high-luminosity quasars with a mean bolometric luminosity of 10 46.4 erg s −1 . The redshift range of this sample is within z < 4, with a mean value of 1.5 ± 0.78. Because we only selected quasars that have been detected in all three Herschel-SPIRE bands, the quasar sample is complete yet highly biased. Based on the multi-wavelength photometric observation data, we conducted a spectral energy distribution (SED) fitting through UV to FIR. Parameters such as active galactic nucleus (AGN) luminosity, far-IR (FIR) luminosity, stellar mass, as well as many other AGN and galaxy properties are deduced from the SED fitting results. The mean star formation rate (SFR) of the sample is 419 M e yr −1 and the mean gas mass is ∼10 11.3 M e . All of these results point to an IR luminous quasar system. Compared with star formation main sequence (MS) galaxies, at least 80 out of 207 quasars are hosted by starburst galaxies. This supports the statement that luminous AGNs are more likely to be associated with major mergers. The SFR increases with the redshift up to z = 2. It is correlated with the AGN bolometric luminosity, where µ  L L FIR Bol 0.46 0.03 . The AGN bolometric luminosity is also correlated with the host galaxy mass and gas mass. Yet the correlation between L FIR and L Bol has higher significant level, implies that the link between AGN accretion and the SFR is more primal. The M BH /M * ratio of our sample is 0.02, higher than the value 0.005 in the local universe. It might indicate an evolutionary trend of the M BH -M * scaling relation.

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350 μm Dust Emission from High‐Redshift Quasars

Cited by 336 publications

References 46 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

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