BR1202–0725: an extreme multiple merger at<i>z</i>= 4.7

Salomé, P.; Guèlin, M.; Downes, D.; Cox, P.; Guilloteau, S.; Omont, A.; Gavazzi, R.; Neri, R.

doi:10.1051/0004-6361/201219955

Cited by 52 publications

(81 citation statements)

References 55 publications

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“…The corrections and uncertainties ensure that a direct estimate of n and G 0 is not meaningful, but we can compare the general location of the HLS0918 components with other observed galaxy populations. The integrated emission from HLS0918 is similar to local ULIRGs and less than 0.5 dex from three well-studied, high-redshift sources: the SMG HFLS3 (z = 6.34; Riechers et al 2013), the quasar host galaxy BRI1335-0417 (z = 4.41; Riechers et al 2008), and BRI1202-0725N, the SMG component of a quasar/SMG merger at z = 4.7, which cannot be deblended from its companion at some wavelengths (Momjian et al 2005;Salomé et al 2012). In contrast, two other well-studied high-z SMGs, SMMJ2135 (z = 2.3; Swinbank et al 2010;Ivison et al 2010b) and LESSJ0332 (z = 4.76;De Breuck et al 2011), are more than half a magnitude larger in L [C ii] /L FIR , which is interpreted as an atomic gas density more than a magnitude lower than that of HLS0918.…”

Section: Physical Properties Of the Pdrmentioning

confidence: 78%

[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

Rawle

Egami

Bussmann

et al. 2014

ApJ

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101

125

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Citation for published item:wleD FhF nd igmiD iF nd fussmnnD FF nd qurwellD wF nd svisonD FtF nd fooneD pF nd gomesD pF nd hnielsonD eFvFF nd exD wF nd ihrdD tF nd milD sF nd winnkD eFwF nd eltieriD fF nd flinD eFF nd glementD fF nd hessugesEvdskyD wF nd idgeD eFgF nd pzioD qFqF nd tonesD F nd uneiD tFEF nd ymontD eF nd ¡ erezEqonz¡ lezD FqF nd hererD hF nd lthnovD sF nd vn der erfD FF nd lthD qF nd mojskiD wF nd emovD wF @PHIRA 9g ss nd IPgy@IEHA emission mps in rvtHWIVPVFTCSIRPPQ X strongly lensed interting system t z a SFPRF9D estrophysil journlFD UVQ @IAF pF SWF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACT We present Submillimeter Array [C ii] 158 μm and Karl G. Jansky Very Large Array 12 CO(1-0) line emission maps for the bright, lensed, submillimeter source at z = 5.2430 behind A 773: HLSJ091828.6+514223 (HLS0918). We combine these measurements with previously reported line profiles, including multiple 12 CO rotational transitions, [C i], water, and [N ii], providing some of the best constraints on the properties of the interstellar medium in a galaxy at z > 5. HLS0918 has a total far-infrared (FIR) luminosity L FIR(8-1000 μm) = (1.6 ± 0.1) × 10 14 L μ −1 , where the total magnification μ total = 8.9 ± 1.9, via a new lens model from the [C ii] and continuum maps. Despite a HyLIRG luminosity, the FIR continuum shape resembles that of a local LIRG. We simultaneously fit all of the observed spectral line profiles, finding four components that correspond cleanly to discrete spatial structures identified in the maps. The two most redshifted spectral components occupy the nucleus of a massive galaxy, with a source-plane separation <1 kpc. The reddest dominates the continuum map (demagnified L FIR,component = (1.1 ± 0.2) × 10 13 L ) and excites strong water emission in both nuclear components via a powerful FIR radiation field from the intense star formation. A third star-forming component is most likely a region of a merging companion (ΔV ∼ 500 km s −1 ) exhibiting generally similar gas properties. The bluest component originates from a spatially distinct region and photodissociation region analysis suggests that it is lower density, cooler, and forming stars less vigorously than the other components. Strikingly, it has very strong [N ii] emission, which may suggest an ionized, molecular outflow. This comprehensive view of gas properties and morphology in HLS0918 previews the science possible for a large sample of high-redshift galaxies once ALM...

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Section: Physical Properties Of the Pdrmentioning

confidence: 78%

[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

Rawle

Egami

Bussmann

et al. 2014

ApJ

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101

125

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“…Xia et al 2012). In addition, one can look at the submm output of dust-obscured QSOs to search for evidence of recent mergers (e.g., Carilli et al 2002;Krips et al 2005;Riechers et al 2008;Salomé et al 2012;Carniani et al 2013), and outflows can be observed in bright CO lines (e.g., Veilleux et al 2013;Sun et al 2014;Feruglio et al 2015;Spilker et al 2018).…”

mentioning

confidence: 99%

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Hill

Chapman

Scott

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A primary goal of the SCUBA-2 Web survey is to perform tomography of the early inter-galactic medium by studying systems containing some of the brightest quasistellar objects (QSOs; 2.5 < z < 3.0) and nearby submillimetre galaxies. As a first step, this paper aims to characterize the galaxies that host the QSOs. To achieve this, a sample of 13 hyper-luminous (L AGN > 10 14 L ) QSOs with previous submillimetre continuum detections were followed up with CO(3-2) observations using the NOEMA interferometer. All but two of the QSOs are detected in CO(3-2); for one non-detection, our observations show a tentative 2σ line at the expected position and redshift, and for the other non-detection we find only continuum flux density an order of magnitude brighter than the other sources. In three of the fields, a companion potentially suitable for tomography is detected in CO line emission within 25 arcsec of the QSO. We derive gas masses, dynamical masses and far-infrared luminosities, and show that the QSOs in our sample have similar properties as compared to less luminous QSOs and SMGs in the literature, despite the fact that their black-hole masses (which are proportional to L AGN ) are 1-2 orders of magnitude larger. We discuss two interpretations of these observations: this is due to selection effects, such as preferential face-on viewing angles and picking out objects in the tail ends of the scatter in host-galaxy mass and blackhole mass relationships; or the black hole masses have been overestimated because the accretion rates are super-Eddington.

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“…By including other published SMGs at different redshifts (Magdis et al 2011;Combes et al 2012;Salomé et al 2012;Walter et al 2012;Riechers et al 2013), we have plotted the L CO(1-0) /M dust versus redshift for all of them in the right panel of Fig. 12 similarly to Tan et al (2014).…”

Section: Star Formation and The Molecular Gas Content In High-redshifmentioning

confidence: 99%

Molecular gas in theHerschel-selected strongly lensed submillimeter galaxies atz ~ 2–4 as probed by multi-JCO lines

Yang

Omont

Beelen

et al. 2017

A&A

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We present the IRAM-30 m observations of multiple-J CO (J up mostly from 3 up to 8) and [C I]( 3 P 2 → 3 P 1 ) ([C I](2-1) hereafter) line emission in a sample of redshift ∼ 2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [C I](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around J up ∼ 5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density n H 2 ∼ 10 2.5 -10 4.1 cm −3 and the kinetic temperature T k ∼ 20-750 K. The gas thermal pressure P th ranging from ∼ 10 5 K cm −3 to 10 6 K cm −3 is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with n H 2 ∼ 10 2.8 -10 4.6 cm −3 and T k ∼ 20-30 K, which is less correlated with star formation, and a high-excitation one (n H 2 ∼ 10 2.7 -10 4.2 cm −3 , T k ∼ 60-400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the J up ≥ 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2-1) lines follow the tight linear correlation between the luminosities of the [C I](2-1) and the CO(1-0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30) × 10 10 M , derived based on the CO(3-2) fluxes and α CO(1-0) = 0.8M ( K km s −1 pc 2 ) −1 , suggests a typical molecular gas depletion time t dep ∼ 20-100 Myr and a gas to dust mass ratio δ GDR ∼ 30-100 with ∼ 20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L CO /M dust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H 2 O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H 2 O lines are co-spatially located.

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BR1202–0725: an extreme multiple merger atz= 4.7

Cited by 52 publications

References 55 publications

[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Molecular gas in theHerschel-selected strongly lensed submillimeter galaxies atz ~ 2–4 as probed by multi-JCO lines

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BR1202–0725: an extreme multiple merger atz= 4.7

Cited by 52 publications

References 55 publications

[C II] AND12CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

[C II] AND12CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Molecular gas in theHerschel-selected strongly lensed submillimeter galaxies atz ~ 2–4 as probed by multi-JCO lines

Contact Info

Product

Resources

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[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

[C II] AND¹²CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24