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Powerful H_2 Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H_2 and a Comparison with [C II] 157.7 μm Emission and Kinematics

Appleton, P. N. and Guillard, P. and Togi, A. and Alatalo, K. and Boulanger, F. and Cluver, M. and Pineau des Forêts, G. and Lisenfeld, U. and Ogle, P. and Xu, C. K. (2017) Powerful H_2 Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H_2 and a Comparison with [C II] 157.7 μm Emission and Kinematics. Astrophysical Journal, 836 (1). Art. No. 76. ISSN 1538-4357.

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We map for the first time the two-dimensional H_2 excitation of warm intergalactic gas in Stephan's Quintet on group-wide (50 × 35 kpc^2) scales to quantify the temperature, mass, and warm H_2 mass fraction as a function of position using Spitzer. Molecular gas temperatures are seen to rise (to T > 700 K) and the slope of the power-law density–temperature relation flattens along the main ridge of the filament, defining the region of maximum heating. We also performed MHD modeling of the excitation properties of the warm gas, to map the velocity structure and energy deposition rate of slow and fast molecular shocks. Slow magnetic shocks were required to explain the power radiated from the lowest-lying rotational states of H_2, and strongly support the idea that energy cascades down to small scales and low velocities from the fast collision of NGC 7318b with group-wide gas. The highest levels of heating of the warm H_2 are strongly correlated with the large-scale stirring of the medium as measured by [C ii] spectroscopy with Herschel. H_2 is also seen associated with a separate bridge that extends toward the Seyfert nucleus in NGC 7319, from both Spitzer and CARMA CO observations. This opens up the possibility that both galaxy collisions and outflows from active galactic nuclei can turbulently heat gas on large scales in compact groups. The observations provide a laboratory for studying the effects of turbulent energy dissipation on group-wide scales, which may provide clues about the heating and cooling of gas at high z in early galaxy and protogalaxy formation.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Appleton, P. N.0000-0002-7607-8766
Guillard, P.0000-0002-2421-1350
Togi, A.0000-0001-5042-3421
Alatalo, K.0000-0002-4261-2326
Cluver, M.0000-0002-9871-6490
Lisenfeld, U.0000-0002-9471-5423
Ogle, P.0000-0002-3471-981X
Xu, C. K.0000-0002-1588-6700
Additional Information:© 2017. The American Astronomical Society. Received 2016 September 8; revised 2016 December 21; accepted 2017 January 10; published 2017 February 9. This paper is dedicated to the work of James Houck of Cornell University (1940–2015), who was the PI of the Spitzer IRS instrument. Without his vision and dedication to building a superb instrument, the work described in this paper would never been possible. This work is based, in part, on observations (and archival observations) made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The work is also based, in part, on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Partial support for the Herschel work was provided by NASA through an award issued by JPL/Caltech. U.L. acknowledges support by the research projects AYA2011-24728 and AYA2014-53506-P financed by the Spanish Ministerio de Economía y Competividad and by FEDER (Fondo Europeo de Desarrollo Regional) and the Junta de Andalucía (Spain) grants FQM108.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Ministerio de Economía y Competividad (MEC)AYA2011-24728
Ministerio de Economía y Competividad (MEC)AYA2014-53506-P
Fondo Europeo de Desarrollo Regional (FEDER)UNSPECIFIED
Junta de AndalucíaFQM108
Subject Keywords:galaxies: individual (Stephanʼs Quintet – NGC 7318a, NGC 7318b, NGC 7319)
Issue or Number:1
Record Number:CaltechAUTHORS:20170210-135050275
Persistent URL:
Official Citation:P. N. Appleton et al 2017 ApJ 836 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74213
Deposited By: George Porter
Deposited On:13 Feb 2017 15:49
Last Modified:09 Mar 2020 13:19

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