CaltechAUTHORS
  A Caltech Library Service

A Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns

Lu, Nanyao and Zhao, Yinghe and Díaz-Santos, Tanio and Xu, C. Kevin and Gao, Yu and Armus, Lee and Isaak, Kate G. and Mazzarella, Joseph M. and van der Werf, Paul P. and Appleton, Philip N. and Charmandaris, Vassilis and Evans, Aaron S. and Howell, Justin and Iwasawa, Kazushi and Leech, Jamie and Lord, Steven and Petric, Andreea O. and Privon, George C. and Sanders, David B. and Schulz, Bernhard and Surace, Jason A. (2017) A Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns. Astrophysical Journal Supplement Series, 230 (1). Art. No. 1. ISSN 1538-4365. https://resolver.caltech.edu/CaltechAUTHORS:20170505-095027368

[img] PDF - Published Version
See Usage Policy.

2552Kb
[img] PDF - Submitted Version
See Usage Policy.

15Mb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20170505-095027368

Abstract

We describe a Herschel Space Observatory 194–671 μm spectroscopic survey of a sample of 121 local luminous infrared galaxies and report the fluxes of the CO J to J–1 rotational transitions for 4 ⩽ J ⩽ 13, the [N ii] 205 μm line, the [C i] lines at 609 and 370 μm, as well as additional and usually fainter lines. The CO spectral line energy distributions (SLEDs) presented here are consistent with our earlier work, which was based on a smaller sample, that calls for two distinct molecular gas components in general: (i) a cold component, which emits CO lines primarily at J ≾ 4 and likely represents the same gas phase traced by CO (1−0), and (ii) a warm component, which dominates over the mid-J regime (4 < J ≾ 10) and is intimately related to current star formation. We present evidence that the CO line emission associated with an active galactic nucleus is significant only at J > 10. The flux ratios of the two [C i] lines imply modest excitation temperatures of 15–30 K; the [C i] 370 μm line scales more linearly in flux with CO (4−3) than with CO (7−6). These findings suggest that the [C i] emission is predominantly associated with the gas component defined in (i) above. Our analysis of the stacked spectra in different far-infrared (FIR) color bins reveals an evolution of the SLED of the rotational transitions of H_2 O vapor as a function of the FIR color in a direction consistent with infrared photon pumping.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4365/aa6476DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4365/aa6476/metaPublisherArticle
https://arxiv.org/abs/1703.00005arXivDiscussion Paper
ORCID:
AuthorORCID
Lu, Nanyao0000-0002-8948-1044
Zhao, Yinghe0000-0002-9128-818X
Díaz-Santos, Tanio0000-0003-0699-6083
Xu, C. Kevin0000-0002-1588-6700
Gao, Yu0000-0003-0007-2197
Armus, Lee0000-0003-3498-2973
Mazzarella, Joseph M.0000-0002-8204-8619
van der Werf, Paul P.0000-0001-5434-5942
Appleton, Philip N.0000-0002-7607-8766
Charmandaris, Vassilis0000-0002-2688-1956
Evans, Aaron S.0000-0003-2638-1334
Iwasawa, Kazushi0000-0002-4923-3281
Petric, Andreea O.0000-0003-4030-3455
Privon, George C.0000-0003-3474-1125
Sanders, David B.0000-0002-1233-9998
Surace, Jason A.0000-0001-7291-0087
Additional Information:© 2017 American Astronomical Society. Received 2016 September 9. Accepted 2017 February 22. Published 2017 May 3. This paper benefited from a number of thoughtful comments made by the anonymous referee. The work presented here is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided in part by NASA through an award issued by JPL/Caltech. N.L. acknowledges partial support from the Natural Science Foundation of China (NSFC) under grant No. 11673028. Y.Z. is partially supported by NSFC grant No. 11673057. Y.G. and Y.Z. are partially supported by NSFC grants No. 11173059, 11390373, and 11420101002, and the CAS pilot-b project No. XDB09000000. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT 1151239. V.C. acknowledges partial support from the EU FP7 Grant PIRSES-GA-2012-316788. K.I. acknowledges support by the Spanish MINECO under grantAYA2013-47447-C3-2-P and MDM-2014-0369 of ICCUB (Unidad deExcelencia "María de Maeztu"). G.C.P. was supported by a FONDECYT postdoctoral fellowship (No. 3150361). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Natural Science Foundation of China11673028
Natural Science Foundation of China11673057
Natural Science Foundation of China11173059
Natural Science Foundation of China11390373
Natural Science Foundation of China11420101002
Chinese Academy of SciencesXDB09000000
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)31130005
Fondo Nacional de Desarrollo Científico y Tecnolόgico (FONDECYT)1151239
Marie Curie FellowshipPIRSES-GA-2012-316788
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2013-47447-C3-2-P
Unidad de Excelencia "María de Maeztu"MDM-2014-0369
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3150361
Subject Keywords:galaxies: active; galaxies: ISM; galaxies: star formation; infrared: galaxies; ISM: molecules; submillimeter: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20170505-095027368
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170505-095027368
Official Citation:Nanyao Lu et al 2017 ApJS 230 1
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77216
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:05 May 2017 18:04
Last Modified:05 Nov 2019 05:45

Repository Staff Only: item control page