2014A&A...568A..90R


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET15:04:43

2014A&A...568A..90R - Astronomy and Astrophysics, volume 568A, 90-90 (2014/8-1)

Molecular gas heating in Arp 299.

ROSENBERG M.J.F., MEIJERINK R., ISRAEL F.P., VAN DER WERF P.P., XILOURIS E.M. and WEISS A.

Abstract (from CDS):

(Ultra) luminous infrared galaxies ((U)LIRGs) are nearby laboratories that allow us to study similar processes to those occurring in high redshift submillimeter galaxies. Understanding the heating and cooling mechanisms in these galaxies can give us insight into the driving mechanisms in their more distant counterparts. Molecular emission lines play a crucial role in cooling excited gas, and recently, with Herschel Space Observatory we have been able to observe the rich molecular spectrum. Carbon monoxide (CO) is the most abundant and one of the brightest molecules in the Herschel wavelength range. CO transitions from J=4-3 to 13-12 are observed with Herschel, and together, these lines trace the excitation of CO. We study Arp 299, a colliding galaxy group, with one component (A) harboring an active galatic nucleus and two more (B and C) undergoing intense star formation. For Arp 299 A, we present PACS spectrometer observations of high-J CO lines up to J=20-19 and JCMT observations of 13CO and HCN to discern between UV heating and alternative heating mechanisms. There is an immediately noticeable difference in the spectra of Arp 299 A and Arp 299 B+C, with source A having brighter high-J CO transitions. This is reflected in their respective spectral energy line distributions. We find that photon-dominated regions (PDRs, UV heating) are unlikely to heat all the gas since a very extreme PDR is necessary to fit the high-J CO lines. In addition, this extreme PDR does not fit the HCN observations, and the dust spectral energy distribution shows that there is not enough hot dust to match the amount expected from such an extreme PDR. Therefore, we determine that the high-J CO and HCN transitions are heated by an additional mechanism, namely cosmic ray heating, mechanical heating, or X-ray heating. We find that mechanical heating, in combination with UV heating, is the only mechanism that fits all molecular transitions. We also constrain the molecular gas mass of Arp 299 A to 3x109M and find that we need 4% of the total heating to be mechanical heating, with the rest UV heating. Finally, we caution against the use of 12CO alone as a probe of physical properties in the interstellar medium.

Abstract Copyright:

Journal keyword(s): ISM: molecules - photon-dominated region (PDR) - galaxies: ISM - galaxies: starburst - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/A+A/568/A90): list.dat fits/*>

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2864 2
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 3992 2
3 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 691 0
4 IC 694 G 11 28 27.312 +58 34 42.29   18.2       ~ 232 2
5 APG 299C G 11 28 30.63 +58 33 49.0           ~ 24 0
6 NAME NGC 3690 West GiP 11 28 30.69 +58 33 33.4   11.8       ~ 604 4
7 NGC 3690 IG 11 28 31.326 +58 33 41.80   13.19 12.86     ~ 867 4
8 NAME NGC 3690 East AGN 11 28 33.07 +58 33 54.2   11.8       ~ 609 4
9 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1739 3
10 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2625 4
11 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1447 2

    Equat.    Gal    SGal    Ecl

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2019.11.17-15:04:43

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