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Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies
Petric, Andreea O.1,2; Armus, Lee3; Flagey, Nicolas2; Guillard, Pierre4; Howell, Justin3; Inami, Hanae5; Charmandaris, Vassillis6,7; Evanss, Aaron8,9; Stierwalt, Sabrina8,9; Diaz-Santos, Tanio3,10; Lu, Nanyao11,12; Spoon, Henrik13; Mazzarella, Joe3; Appleton, Phil3; Chan, Ben3; Chu, Jason1; Hand, Derek14; Privon, George15; Sanders, David1; Surace, Jason3; Xu, Kevin3; Zhao YH(赵应和)3,16,17,18
Source PublicationASTRONOMICAL JOURNAL
2018-12-01
Volume156Issue:6Pages:24
DOI10.3847/1538-3881/aaca35
Contribution Rank第16完成单位
Indexed BySCI
Keywordgalaxies: active galaxies: interactions galaxies: ISM galaxies: starburst
Abstract

Mid-infrared molecular hydrogen (H-2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies; it is a potential key tracer of gas evolution and energy dissipation associated with mergers, star formation, and accretion onto supermassive black holes. We detect mid-IR H-2 line emission in at least one rotational transition in 91% of the 214 Luminous Infrared Galaxies (LIRGs) observed with Spitzer as part of the Great Observatories All-sky LIRG Survey. We use H-2 excitation diagrams to estimate the range of masses and temperatures of warm molecular gas in these galaxies. We find that LIRGs in which the IR emission originates mostly from the Active Galactic Nuclei (AGN) have about 100 K higher H-2 mass-averaged excitation temperatures than LIRGs in which the IR emission originates mostly from star formation. Between 10% and 15% of LIRGs have H-2 emission lines that are sufficiently broad to be resolved or partially resolved by the high-resolution modules of Spitzer's Infrared Spectrograph (IRS). Those sources tend to be mergers and contain AGN. This suggests that a significant fraction of the H-2 line emission is powered by AGN activity through X-rays, cosmic rays, and turbulence. We find a statistically significant correlation between the kinetic energy in the H-2 gas and the H-2 to IR luminosity ratio. The sources with the largest warm gas kinetic energies are mergers. We speculate that mergers increase the production of bulk inflows leading to observable broad H-2 profiles and possibly denser gas.

Funding ProjectNASA[1407] ; EU[PIRSES-GA-2012-316788] ; NSFC[11673028] ; National Key R&D Program of China[2017YFA0402704]
Funding OrganizationNASA[1407] ; EU[PIRSES-GA-2012-316788] ; NSFC[11673028] ; National Key R&D Program of China[2017YFA0402704]
Language英语
Subject Area天文学 ; 星系与宇宙学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-6256
URL查看原文
WOS IDWOS:000452546300001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordSPITZER-SPACE-TELESCOPE ; STAR-FORMATION ; STATISTICAL-METHODS ; ASTRONOMICAL DATA ; H-2 EMISSION ; UPPER LIMITS ; GAS ; CLASSIFICATION ; SPECTROGRAPH ; SIMULATIONS
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/18609
Collection丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
Corresponding AuthorPetric, Andreea O.
Affiliation1.Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
2.Canada–France–Hawaii Telescope, 65-1238 Mamalahoa Highway, Kamuela, HI 96743, USA
3.Infrared Processing & Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125, USA
4.Institut d'Astrophysique de Paris, 96 bis boulevard Arago, F-75014 Paris, France
5.Universite de Lyon, 92 Rue Pasteur, F-69007, Lyon, France
6.Department of Physics, University of Crete, GR-71003 Heraklion, Greece
7.IAASARS, National Observatory of Athens, GR-15236, Penteli, Greece
8.Department of Astronomy, University of Virginia, Charlottesville, VA 22903, USA
9.National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
10.Nucleo de Astronomia de la Facultad de Ingenieria, Universitad Diego Portales, Av. Ejercito Libertador 441, Santiago, Chile
11.National Astronomical Observatories, Chinese Academy of Sciences (CAS), Beijing 100012, People's Republic of China
12.China-Chile Joint Center for Astronomy, Camino El Observatorio 1515, Las Condes, Santiago, Chile
13.Department of Astronomy, Cornell University, 616A Space Science Building, Ithaca, NY 14853, USA
14.Department of Physics and Astronomy, University of Hawaii, 200 W. Kawili St., Hilo, HI 96720, USA
15.Instituto de Astrofisica, Facultad de Fisica, Pontificia Universitad Catolica de Chile, Casilla 306, Santiago 22, Chile
16.Yunnan Observatories, CAS, Kumming 65011, People's Republic of China
17.Key laboratory for the Structure and Evolution of Celestial Objects, CAS, Kumming 65011, People's Republic of China
18.Purple Mountain Observatory, CAS, Nanjing, 210008, People's Republic of China
Recommended Citation
GB/T 7714
Petric, Andreea O.,Armus, Lee,Flagey, Nicolas,et al. Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies[J]. ASTRONOMICAL JOURNAL,2018,156(6):24.
APA Petric, Andreea O..,Armus, Lee.,Flagey, Nicolas.,Guillard, Pierre.,Howell, Justin.,...&Zhao YH.(2018).Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies.ASTRONOMICAL JOURNAL,156(6),24.
MLA Petric, Andreea O.,et al."Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies".ASTRONOMICAL JOURNAL 156.6(2018):24.
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