Star Formation and ISM Properties in the Host Galaxies of Three Far-infrared Luminous Quasars at z ∼ 6

Shao, Yali; Wang, Ran; Carilli, C. L.; Wagg, Jeff; Walter, Fabian; Li, Jianan; Fan, Xiaohui; Jiang, Linhua; Riechers, Dominik A.; Bertoldi, F.; Strauss, Michael A.; Cox, P.; Omont, A.; Menten, K. M.

doi:10.3847/1538-4357/ab133d

Cited by 47 publications

(96 citation statements)

References 84 publications

(121 reference statements)

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“…In fact, the dust masses and continuum sizes of our AGN host galaxies provide τ ν > 0.5 at ν obs > 300 GHz, thus making the optically thin approximation not valid at higher frequencies. For comparison in Appendix B we report the best-fitting results in the optical thin assumptions, which are in agreement with those reported by previous studies (Wang et al 2013;Shao et al 2019).…”

Section: Fir Luminositiessupporting

confidence: 87%

Constraints on high-J CO emission lines in z ∼ 6 quasars

Carniani

Gallerani

Vallini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimiter/submillimiter Array (ALMA) observations of eight highly excited CO (J up > 8) lines and continuum emission in two z ∼ 6 quasars: SDSS J231038.88+185519.7 (hereafter J2310), for which CO(8-7), CO(9-8), and CO(17-16) lines have been observed, and ULAS J131911.29+095951.4 (J1319), observed in the CO(14-13), CO(17-16) and CO(19-18) lines. The continuum emission of both quasars arises from a compact region (< 0.9 kpc). By assuming a modified black-body law, we estimate dust masses of Log(M dust /M ) = 8.75 ± 0.07 and Log(M dust /M ) = 8.8 ± 0.2 and dust temperatures of T dust = 76 ± 3 K and T dust = 66 +15 −10 K, respectively for J2310 and J1319. Only CO(8-7) and CO(9-8) in J2310 are detected, while 3σ upper limits on luminosities are reported for the other lines of both quasars. The CO line luminosities and upper limits measured in J2310 and J1319 are consistent with those observed in local AGN and starburst galaxies, and other z ∼ 6 quasars, except for SDSS J1148+5251 (J1148), the only quasar at z = 6.4 with a previous CO(17-16) line detection. By computing the CO SLEDs normalised to the CO(6-5) line and FIR luminosities for J2310, J1319, and J1149, we conclude that different gas heating mechanisms (X-ray radiation and/or shocks) may explain the different CO luminosities observed in these z ∼ 6 quasar. Future J up > 8 CO observations will be crucial to understand the processes responsible for molecular gas excitation in luminous high-z quasars.

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Section: Fir Luminositiessupporting

confidence: 87%

Constraints on high-J CO emission lines in z ∼ 6 quasars

Carniani

Gallerani

Vallini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…With the short dust-growth timescale considered here, the average rate in MCs may be high enough to account for the large dust masses reported in galaxies as early as at redshifts z ∼ 7 − 8 (see, e.g., Watson et al 2015;Shao et al 2019), even without a large net production of dust from SNe. The latter is important, since there are reasons to believe that much of the dust formed at early stages in SN remnants, will not survive the passage of the reverse shock formed when the blast wave hits the circumstellar and interstellar medium (see, e.g., Bianchi & Schneider 2007;Nozawa et al 2007;Kirchschlager et al 2019), although the efficiency of grain destruction depends a lot on the shock velocity and the type of dust (Silvia et al 2010).…”

Section: Discussionmentioning

confidence: 93%

Galactic dust evolution with rapid dust formation in the interstellar medium due to hypersonic turbulence

Mattsson

2019

Monthly Notices of the Royal Astronomical Society

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Turbulence can significantly accelerate the growth of dust grains by accretion of molecules. For dust dynamically coupled to the gas, the growth rate scales with the square of the Mach number, which means that the growth timescale can easily be reduced by more than an order of magnitude. The limiting timescale is therefore rather the rate of molecular cloud formation, which means that dust production in the ISM can rapidly reach the levels needed to explain the dust masses observed at high redshifts. Thus, turbulence may be the solution to the replenishment problem in models of dust evolution in high-redshift galaxies and explain the dust masses seen at z = 7 − 8. A simple analytic galactic dust-evolution model is presented, where grain growth nicely compensates for the expected higher rate of dust destruction by supernova shocks. This model is simpler, relies on fewer assumptions and seems to yields a better fit to data derived from observations, compared to previous models of the same type.

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“…We also compare positions of the ALMA and the SDSS optical images (c.f., Shao et al 2019;Wang et al 2019). To do so, we first recalibrate astrometry of the SDSS zband image (Eisenstein et al 2011) where the quasars are detected.…”

Section: Astrometrymentioning

confidence: 99%

“…Recently,Shao et al (2019) have performed detailed multi-wavelength SED analyses in J2310+1855.Figure 4in the study shows that star formation activity may be a dominant source for the FIR dust continuum emission in J2310+1855.…”

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confidence: 99%

Detections of [O iii] 88 μm in two quasars in the reionization epoch

Hashimoto

Inoue

Tamura

et al. 2019

Publications of the Astronomical Society of Japan

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With the Atacama Large Millimeter/sub-millimeter Array (ALMA), we report detections of the far-infrared (FIR) [Oiii] 88 µm line and the underlying dust continuum in the two quasars in the reionization epoch, J205406.48-000514.8 (hereafter J2054-0005) at z = 6.0391 ± 0.0002 and J231038.88+185519.7 (hereafter J2310+1855) at z = 6.0035 ± 0.0007. The [Oiii] luminosity of J2054-0005 and J2310+1855 are L [OIII] = (6.8±0.6)×10 9 and (2.4±0.6)×10 9 L ⊙ , corresponding to ≈ 0.05% and 0.01% of the total infrared luminosity, L TIR , respectively. Combining these [Oiii] luminosities with [Cii] 158 µm luminosities in the literature, we find that J2054-0005 and J2310+1855 have the [Oiii]-to-[Cii] luminosity ratio of 2.1 ± 0.4 and 0.3 ± 0.1, respectively, the latter of which is the lowest among objects so far reported at z > 6. Combining [Oiii] observations at z ≈ 6 − 9 from our study and the literature, we identify the [Oiii] line deficit: objects with larger L TIR have lower L [OIII] -to-L TIR ratios. Furthermore, we also find that the anti-correlation is shifted toward higher L TIR value when compared to the local [Oiii] line deficit.

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Star Formation and ISM Properties in the Host Galaxies of Three Far-infrared Luminous Quasars at z ∼ 6

Abstract: We present Karl G. Jansky Very Large Array (VLA) observations of the CO

Cited by 47 publications

References 84 publications

Constraints on high-J CO emission lines in z ∼ 6 quasars

Constraints on high-J CO emission lines in z ∼ 6 quasars

Galactic dust evolution with rapid dust formation in the interstellar medium due to hypersonic turbulence

Detections of [O iii] 88 μm in two quasars in the reionization epoch

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