TY - JOUR
T1 - Multiphase ISM in the z = 5.7 Hyperluminous Starburst SPT 0346-52
AU - Litke, Katrina C.
AU - Marrone, Daniel P.
AU - Aravena, Manuel
AU - Béthermin, Matthieu
AU - Chapman, Scott C.
AU - Dong, Chenxing
AU - Hayward, Christopher C.
AU - Hill, Ryley
AU - Jarugula, Sreevani
AU - Malkan, Matthew A.
AU - Narayanan, Desika
AU - Reuter, Cassie A.
AU - Spilker, Justin S.
AU - Sulzenauer, Nikolaus
AU - Vieira, Joaquin D.
AU - Weiß, Axel
N1 - Funding Information:
We thank the anonymous referee for the insightful and thorough comments. We also thank Chris Marslender for his computational support. The SPT is supported by the US National Science Foundation (NSF) through grant OPP-1852617. K.C.L., D.P.M., J.D.V., K.P., and S.J. acknowledge support from the US NSF under grants AST-1715213 and AST-1716127. K.C.L. and S.J. acknowledge support from the US NSF NRAO under grants SOSPA4-007 and SOSPA5-001, respectively. J.D.V. acknowledges support from an A. P. Sloan Foundation Fellowship. M.A. acknowledges partial support from FONDECYT grant 1211951, ANID+PCI+INSTITUTO MAX PLANCK DE ASTRONOMIA MPG 190030, ANID+PCI+REDES 190194, and ANID BASAL project FB210003. N.S. is a member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This material has made use of the Ocelote high-performance computer, which is part of the high-performance computing (HPC) resources supported by the University of Arizona TRIF, UITS, and RDI and maintained by the UA Research Technologies department. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2013.1.01231.S, #2015.1.01580.S, and #2016.1.01565.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of NASA’s Astrophysics Data System. This research also uses the Cosmology Calculator by Wright (). Cloudy has been supported by NSF (1816537), NASA (ATP 17-ATP17-0141), and STScI (HST-AR-15018).
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/4/1
Y1 - 2022/4/1
N2 - With ςSFR ∼4200 M ⊙ yr-1 kpc-2, SPT 0346-52 (z = 5.7) is the most intensely star-forming galaxy discovered by the South Pole Telescope. In this paper, we expand on previous spatially resolved studies, using ALMA observations of dust continuum, [N ii] 205 μm, [C ii] 158 μm, [O i] 146 μm, and undetected [N ii] 122 μm and [O i] 63 μm emission to study the multiphase interstellar medium (ISM) in SPT 0346-52. We use pixelated, visibility-based lens modeling to reconstruct the source-plane emission. We also model the source-plane emission using the photoionization code cloudy and find a supersolar metallicity system. We calculate T dust = 48.3 K and λ peak = 80 μm and see line deficits in all five lines. The ionized gas is less dense than comparable galaxies, with n e < 32 cm-3, while ∼20% of the [C ii] 158 μm emission originates from the ionized phase of the ISM. We also calculate the masses of several phases of the ISM. We find that molecular gas dominates the mass of the ISM in SPT 0346-52, with the molecular gas mass ∼4× higher than the neutral atomic gas mass and ∼100× higher than the ionized gas mass.
AB - With ςSFR ∼4200 M ⊙ yr-1 kpc-2, SPT 0346-52 (z = 5.7) is the most intensely star-forming galaxy discovered by the South Pole Telescope. In this paper, we expand on previous spatially resolved studies, using ALMA observations of dust continuum, [N ii] 205 μm, [C ii] 158 μm, [O i] 146 μm, and undetected [N ii] 122 μm and [O i] 63 μm emission to study the multiphase interstellar medium (ISM) in SPT 0346-52. We use pixelated, visibility-based lens modeling to reconstruct the source-plane emission. We also model the source-plane emission using the photoionization code cloudy and find a supersolar metallicity system. We calculate T dust = 48.3 K and λ peak = 80 μm and see line deficits in all five lines. The ionized gas is less dense than comparable galaxies, with n e < 32 cm-3, while ∼20% of the [C ii] 158 μm emission originates from the ionized phase of the ISM. We also calculate the masses of several phases of the ISM. We find that molecular gas dominates the mass of the ISM in SPT 0346-52, with the molecular gas mass ∼4× higher than the neutral atomic gas mass and ∼100× higher than the ionized gas mass.
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U2 - 10.3847/1538-4357/ac58f9
DO - 10.3847/1538-4357/ac58f9
M3 - Article
AN - SCOPUS:85128714816
SN - 0004-637X
VL - 928
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 179
ER -