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

Abstract

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...

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

“…This conclusion that [CII] is mostly optically thin has been assumed several times since (e.g. Stacey et al 1991a;HaileyDunsheath et al 2010;Stacey et al 2010;De Breuck et al 2011;Rawle et al 2014).…”

“…Spatially resolved [CII] and CO observations are required to differentiate between the PDR and diffuse components. Observations of another lensed DSFGs, HLSJ091828.6+514223 at z = 5.243 (Rawle et al 2014), do show that the [CII] and CO(1-0) have a consistent structure and velocity profile, though the resolution may not go down to the scales of the GMCs (a few hundred pc). Observations of [CII] and CO at spatial resolutions of ∼50 mas are required to constrain this diffuse component in our DFSGs.…”

“…Rawle et al 2014). This is the first sample of sources with spectrally resolved data with S/N 3 in both [CII] and CO making it possible to compare the shapes of velocity profiles.…”

“…Benford et al in prep., Carilli et al 2002a SDP.141 4.24 60 ± 9 38.7 ± 4.6 66.2 ± 17.7 46.1 ± 3.2 10 − 30 Cox et al 2011 BRI1335-0417 † 4.41 15.7 ± 2.5 4.4 ± 0.8 17.7 ± 4.9 51.3 ± 4.4 - Wagg et al 2010;Carilli et al 2002b ALESS65.1 4.45 3.2 ± 0.4 < 1.11 3.12 ± 1.40 44.3 ± 5.1 - Swinbank et al 2012;Huynh et al 2014 BR1202-0725 † 4.69 15.8 ± 1.8 5.4 ± 0.7 34.1 ± 8.4 55.1 ± 4.3 - Wagg et al 2012;Carilli et al 2002b HDF850.1 5.19 7.5 ± 0.8 2.2 ± 0.5 1.7 ± 1.6 29.9 ± 7.7 1.5 − 1.7 Neri et al 2014;Walter et al 2012 HLSJ091828.6+514223 5.24 82.4 ± 2.3 43.0 ± 3.3 97.5 ± 24.4 48.7 ± 3.0 8.9 ± 1.9 Rawle et al 2014 SDSSJ1044-0125 † 5.78 1.6 ± 0.4 1.6 ± 0.3 5.6 ± 5.1 59.8 ± 25.8 - Wang et al 2013 SDSSJ2310+1855 † 6.00 8.7 ± 1.4 12.1 ± 1.0 20.0 ± 14.5 61.8 ± 20.7 - Wang et al 2013 HerMESFLS3 6.34 14.9 ± 3.1 4.6 ± 1.5 29.9 ± 9.6 52.8 ± 6.2 2.2 ± 0.3 Riechers et al 2013 SDSSJ1148+5251 † 6.42 4.6 ± 0.5 6.4 ± 0.7 9.8 ± 6.7 60.9 ± 15.7 - Table A1. Source names are based on positions measured with the SPT (Mocanu et al 2013).…”

“…Seventeen have been added to the number of z > 4 [CII] detections in the past decade (Maiolino et al 2005(Maiolino et al , 2009Iono et al 2006;Wagg et al 2010;Ivison et al 2010;De Breuck et al 2011;Cox et al 2011;Swinbank et al 2012;Venemans et al 2012;Walter et al 2012;Riechers et al 2013;Wang et al 2013;Rawle et al 2014;De Breuck et al 2014;Neri et al 2014). Many of these objects have been selected based on the presence of a luminous active galactic nuclei (AGN; e.g.…”