Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies
Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies
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附近明亮的红外星系中的温暖氢分子
DOI：
10.3847/1538-3881/aaca35
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发表时间：
2018-05
期刊：
影响因子：
--
通讯作者：
et al.
中科院分区：
文献类型：
--
作者：
Petric Andreea O.;Armus Lee;Flagey Nicolas;Guillard Pierre;Howell Justin;Inami H;Charm;aris Vassillis;Evans Aaron;Stierwalt Sabrina;Diaz-Santos Tanio;Lu Nanyao;et al.
中红外氢分子（H2）辐射是星系合并和射电星系中的一种强有力的冷却剂;它是与合并、星星形成和超大质量黑洞吸积相关的气体演化和能量耗散的潜在关键示踪剂。作为大天文台全天LIRG巡天的一部分，我们在斯皮策观测的214个发光红外星系（LIRG）中的91%中至少检测到一个旋转跃迁中的中红外H2线发射。我们使用H2激发图来估计这些星系中温暖分子气体的质量和温度范围。我们发现，LIRGs中的红外辐射主要来自活动星系核（AGN）有大约100 K高的H2的质量平均激发温度比LIRGs中的红外辐射主要来自星星形成。10%到15%的LIRG具有足够宽的H2发射线，可以被斯皮策红外光谱仪（IRS）的高分辨率模块解析或部分解析。这些来源往往是合并和包含活动星系核。这表明H2谱线发射的很大一部分是由活动星系核活动通过X射线、宇宙射线和湍流提供动力的。我们发现在H2气体的动能和H2的红外光度比之间的统计显着的相关性。具有最大暖气体动能的源是合并。我们推测，合并增加了大量流入的生产，导致可观察到的广泛的H2配置文件和可能更密集的气体。
Mid-infrared molecular hydrogen (H2) 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 H2 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 H2 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 H2 mass-averaged excitation temperatures than LIRGs in which the IR emission originates mostly from star formation. Between 10% and 15% of LIRGs have H2 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 H2 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 H2 gas and the H2 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 H2 profiles and possibly denser gas.
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低红移时帕洛马绿 QSO 的赫歇尔调查
DOI：
10.1088/0067-0049/219/2/22
发表时间：
2015-05
期刊：
Astrophysical Journal, The - Supplement Series
影响因子：
--
作者：
Petric Andreea O.;Ho L. C.;Flagey Nicolas J. M.;Scoville N. Z.
通讯作者：
Scoville N. Z.
DOI：
10.3847/0004-637x/825/2/128
发表时间：
2016-05
期刊：
The Astrophysical Journal
影响因子：
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作者：
K. Larson;D. Sanders;J. Barnes;C. M. Ishida;A. Evans;U. Vivian;J. Mazzarella;Don-Chan Kim;G. Privon;I. Mirabel;H. Flewelling
通讯作者：
K. Larson;D. Sanders;J. Barnes;C. M. Ishida;A. Evans;U. Vivian;J. Mazzarella;Don-Chan Kim;G. Privon;I. Mirabel;H. Flewelling
DOI：
10.1088/0004-637x/814/1/39
发表时间：
2015-09
期刊：
The Astrophysical Journal
影响因子：
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作者：
G. Privon;G. Privon;G. Privon;R. Herrero-Illana;A. S. Evans;A. S. Evans;K. Iwasawa;M. Pérez-Torres;L. Armus;T. Díaz-Santos;T. Díaz-Santos;Eric J. Murphy;S. Stierwalt;S. Aalto;J. Mazzarella;L. Barcos-Muñoz;H. J. Borish;H. Inami;D. Kim;E. Treister;J. Surace;S. Lord;John E. Conway;D. Frayer;A. Alberdi
通讯作者：
G. Privon;G. Privon;G. Privon;R. Herrero-Illana;A. S. Evans;A. S. Evans;K. Iwasawa;M. Pérez-Torres;L. Armus;T. Díaz-Santos;T. Díaz-Santos;Eric J. Murphy;S. Stierwalt;S. Aalto;J. Mazzarella;L. Barcos-Muñoz;H. J. Borish;H. Inami;D. Kim;E. Treister;J. Surace;S. Lord;John E. Conway;D. Frayer;A. Alberdi
DOI：
10.1088/0067-0049/182/2/628
发表时间：
2009-05
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
S. Veilleux;D. Rupke;D. Rupke;D.-C. Kim;D.-C. Kim;R. Genzel;E. Sturm;D. Lutz;A. Contursi
通讯作者：
S. Veilleux;D. Rupke;D. Rupke;D.-C. Kim;D.-C. Kim;R. Genzel;E. Sturm;D. Lutz;A. Contursi
DOI：
10.1088/0004-637x/723/2/993
发表时间：
2010-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
T. Díaz-Santos;V. Charmandaris;L. Armus;A. Petric;J. Howell;E. Murphy;J. Mazzarella;S. Veilleux;G. Bothun;H. Inami;P. Appleton;A. Evans;S. Haan;J. Marshall;D. Sanders;S. Stierwalt;J. Crete;Forth Observatoire de Paris;Spitzer Science Center;Ipac;U. York;U. Oregon;Nasa Herschel Science Center;U. Virginia;University of Honolulu
通讯作者：
T. Díaz-Santos;V. Charmandaris;L. Armus;A. Petric;J. Howell;E. Murphy;J. Mazzarella;S. Veilleux;G. Bothun;H. Inami;P. Appleton;A. Evans;S. Haan;J. Marshall;D. Sanders;S. Stierwalt;J. Crete;Forth Observatoire de Paris;Spitzer Science Center;Ipac;U. York;U. Oregon;Nasa Herschel Science Center;U. Virginia;University of Honolulu