Constraining the Ism Properties of the Cloverleaf Quasar Host Galaxy With Herschel Spectroscopy

Uzgil, Bade; Bradford, C. M.; Hailey-Dunsheath, S.; Maloney, Philip R.; Aguirre, James E.

doi:10.3847/0004-637x/832/2/209

Cited by 33 publications

(35 citation statements)

References 74 publications

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“…Such problems can be avoided, or at least minimized by observing rest-frame far-IR FSL. While some galaxies such as Arp 220 are optically thick out to λ rest =240 µm (Rangwala et al 2011), the extinction corrections to far-IR FSL are at most ∼50% for the shortest wavelength lines (Uzgil et al 2016). Moreover, these far-IR FSL are often brighter than their optical counterparts (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…After a slow start, the [OIII] 88 µm line is quickly becoming a popular line to confirm redshifts of galaxies in the epoch of reionization (z 6), where it shifts into the submillimetre atmospheric windows below 500 GHz Inoue et al 2016;Carniani et al 2017;Marrone et al 2018;Vishwas, et al 2018;Hashimoto, et al 2018;Walter et al 2018;Tamura et al 2019;Tadaki et al 2019;Hashimoto et al 2019;Novak et al 2019). Deep Herschel/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects (Valtchanov et al 2011;Coppin et al 2012;George et al 2013;Uzgil et al 2016;Rigopoulou et al 2018;Zhang et al 2018), or in stacked spectra (Wardlow et al 2017;Wilson et al 2017;Zhang et al 2018). These include the only detections of the [OI] 63 µm line at high redshift reported thus far.…”

Section: Introductionmentioning

confidence: 99%

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A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Breuck

Weiß

Béthermin

et al. 2019

A&A

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We present a study of six far-infrared fine structure lines in the z=4.225 lensed dusty star-forming galaxy SPT 0418-47 to probe the physical conditions of its inter stellar medium (ISM). In particular, we report Atacama Pathfinder EXperiment (APEX) detections of the [OI] 145µm and [OIII] 88µm lines and Atacama Compact Array (ACA) detections of the [NII] 122 and 205µm lines. The [OI] 145µm / [CII] 158µm line ratio is ∼5× higher compared to the average of local galaxies. We interpret this as evidence that the ISM is dominated by photo-dissociation regions with high gas densities. The line ratios, and in particular those of [OIII] 88µm and [NII] 122µm imply that the ISM in SPT 0418-47 is already chemically enriched close to solar metallicity. While the strong gravitational amplification was required to detect these lines with APEX, larger samples can be observed with the Atacama Large Millimeter/submillimeter Array (ALMA), and should allow observers to determine if the dense, solar metallicity ISM is common among these highly star-forming galaxies.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Breuck

Weiß

Béthermin

et al. 2019

A&A

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“…Federrath & Klessen 2012;Federrath et al 2017;Zhou et al 2017), and at higher E-mail: ayan.acharyya@anu.edu.au redshifts (z ∼ 2) where the star-formation rate (SFR) is at its peak (e.g. Uzgil et al 2016;Kewley et al 2016;Kulas et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Rest-frame UV and optical emission line diagnostics of ionized gas properties: a test case in a star-forming knot of a lensed galaxy at z ∼ 1.7

Acharyya

Kewley

Rigby

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We examine the diagnostic power of rest-frame ultraviolet (UV) nebular emission lines, and compare them to more commonly used rest-frame optical emission lines, using the test case of a single star-forming knot of the bright lensed galaxy RCSGA 032727-132609 at redshift z ∼ 1.7. This galaxy has complete coverage of all the major rest-frame UV and optical emission lines from Magellan/MagE and Keck/NIRSPEC. Using the full suite of diagnostic lines, we infer the physical properties: nebular electron temperature (T e ), electron density (n e ), oxygen abundance (log (O/H)), ionisation parameter (log (q)) and interstellar medium (ISM) pressure (log (P/k)). We examine the effectiveness of the different UV, optical and joint UV-optical spectra in constraining the physical conditions. Using UV lines alone we can reliably estimate log (q), but the same is difficult for log (O/H). UV lines yield a higher (∼1.5 dex) log (P/k) than the optical lines, as the former probes a further inner nebular region than the latter. For this comparison, we extend the existing Bayesian inference code IZI, adding to it the capability to infer ISM pressure simultaneously with metallicity and ionisation parameter. This work anticipates future rest-frame UV spectral datasets from the James Webb Space Telescope (JWST ) at high redshift and from the Extremely Large Telescope (ELT) at moderate redshift.

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“…and E n is the kinetic energy of the molecule. In the high redshift quasars, X-rays from AGNs are frequently proposed to explain the CO excitation at high J transitions (Bradford et al 2009;Gallerani et al 2014;Uzgil et al 2016).…”

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confidence: 99%

“…Right column: J2310+1855 (black squares) in comparison with high redshift quasars. The plotted quasars are APM 08279+5255(Bradford et al 2011;Weiß et al 2007;Riechers et al 2009) (grey), Cloverleaf(Bradford et al 2009;Uzgil et al 2016) (red), J1148+5251Walter et al 2003;Beelen et al 2006;Riechers et al 2009;Gallerani et al 2014) (blue), J0439+1634) (green) and J0100+2802) (magenta).…”

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confidence: 99%

Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

Wang

Riechers

et al. 2020

ApJ

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We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO (8 − 7), (9 − 8), H 2 O(2 0,2 − 1 1,1 ) and OH + (1 1 − 0 1 ) and NOrthern Extended Millimeter Array (NOEMA) observations of CO (5 − 4), (6 − 5), (12 − 11) and (13 − 12) towards the z = 6.003 quasar SDSS J231038.88+185519.7, aiming to probe the physical conditions of the molecular gas content of this source. We present the best sampled CO spectral line energy distribution (SLED) at z = 6.003, and analyzed it with the radiative transfer code MOLPOP-CEP. Fitting the CO SLED to a one-component model indicates a kinetic temperature T kin = 228 K, molecular gas density log(n(H 2 )/cm −3 )=4.75, and CO column density log(N (CO)/cm −2 ) = 17.5, although a two-component model better fits the data. In either case, the CO SLED is dominated by a "warm" and "dense" component. Compared to samples of local (Ultra) Luminous Infrared Galaxies ((U)LIRGs), starburst galaxies and high redshift Submillimeter Galaxies (SMGs), J2310+1855 exhibits higher CO excitation at (J ≥ 8), like other high redshift quasars. The high CO excitation, together with the enhanced L H2O /L IR , L H2O /L CO and L OH + /L H2O ratios, suggests that besides the UV radiation from young massive stars, other mechanisms such as shocks, cosmic rays and X-rays might also be responsible for the heating and ionization of the molecular gas. In the nuclear region probed by the molecular emissions lines, any of these mechanisms might be present due to the powerful quasar and the starburst activity.

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Constraining the Ism Properties of the Cloverleaf Quasar Host Galaxy With Herschel Spectroscopy

Cited by 33 publications

References 74 publications

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Rest-frame UV and optical emission line diagnostics of ionized gas properties: a test case in a star-forming knot of a lensed galaxy at z ∼ 1.7

Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

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