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Warm Molecular Hydrogen in Nearby, Luminous Infrared Galaxies
Abstract : 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 (GOALS). 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 100K 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 in-flows leading to observable broad H2 profiles and possibly denser environments.
Keywords :
Astrophysics of Galaxies
Cited literature [45 references]
https://hal.sorbonne-universite.fr/hal-01960939
Contributor : Gestionnaire Hal-Upmc Connect in order to contact the contributor
Submitted on : Wednesday, December 19, 2018 - 4:11:48 PM
Last modification on : Tuesday, May 17, 2022 - 9:38:01 AM
Long-term archiving on: : Thursday, March 21, 2019 - 2:41:35 AM
Contributor : Gestionnaire Hal-Upmc Connect in order to contact the contributor
Submitted on : Wednesday, December 19, 2018 - 4:11:48 PM
Last modification on : Tuesday, May 17, 2022 - 9:38:01 AM
Long-term archiving on: : Thursday, March 21, 2019 - 2:41:35 AM
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1805.09926.pdf
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