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Using [C I] to probe the interstellar medium in z ∼ 2.5 sub-millimeter galaxies.

Alaghband-Zadeh, S. and Chapman, S.C. and Swinbank, A.M. and Smail, I. and Danielson, A.L.R. and Decarli, R. and Ivison, R.J. and Meijerink, R. and Weiss, A. and van der Werf, P.P. (2013) 'Using [C I] to probe the interstellar medium in z ∼ 2.5 sub-millimeter galaxies.', Monthly notices of the Royal Astronomical Society., 435 (2). pp. 1493-1510.

Abstract

We present new [C I](1–0) and 12CO(4–3) Plateau de Bure Interferometer observations of five sub-millimeter galaxies (SMGs) and combine these with all available [C I](1–0) literature detections in SMGs to probe the gas distribution within a sample of 14 systems. We explore the [C I](1–0) properties of the SMG population, particularly investigating the ratio of the [C I](1–0) luminosity to various 12CO transition and far-infrared luminosities. We find that the SMGs with new observations extend the spread of L[CI](1-0)/LFIR to much higher values than found before, with our complete sample providing a good representation of the diverse z > 2 SMG population. We compare the line ratios to the outputs of photodissociation region (PDR) models to constrain the physical conditions in the interstellar medium (ISM) of the SMGs, finding an average density of 〈log (n/cm−3)〉 = 4.3 ± 0.2 and an average radiation field (in terms of the local field value, G0) of 〈log (G0)〉 = 3.9 ± 0.4. Overall, we find the SMGs are most comparable to local ultraluminous infrared galaxies (ULIRGs) in G0 and n; however, a significant tail of 5 of the 14 SMGs are likely best compared to less compact, local starburst galaxies, providing new evidence that many SMGs have extended star formation distributions and are therefore not simply scaled up versions of local ULIRGs. We derive the ISM properties of a sample of quasars also finding that they have higher densities and radiation fields on average than the SMGs, consistent with the more extreme local ULIRGs, and reinforcing their interpretation as transition objects. We explore the limitations of using simple PDR models to understand [C I], which may be concomitant with the bulk H2 mass rather than PDR distributed. We therefore also assess [C I] as a tracer of H2, finding that for our sample SMGs, the H2 masses derived from [C I] are often consistent with those determined from low excitation 12CO. We conclude that [C I] observations provide a useful tool to probe the bulk gas and gas processes occurring within merging SMGs, however more detailed, resolved observations are required to fully exploit [C I] as a diagnostic.

Item Type:Article
Keywords:Galaxies: evolution, Galaxies: high redshift, Galaxies: ISM, Galaxies: starburst.
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Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1093/mnras/stt1390
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2013 The Authors Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.
Date accepted:No date available
Date deposited:30 June 2014
Date of first online publication:October 2013
Date first made open access:No date available

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