WARM MOLECULAR HYDROGEN EMISSION IN NORMAL EDGE-ON GALAXIES NGC 4565 AND NGC 5907

Journal Article · Wed Sep 15 00:00:00 EDT 2010 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/140/3/753· OSTI ID:21443248

Laine, Seppo ^[1]; Appleton, Philip N ^[2]; Gottesman, Stephen T ^[3]; Ashby, Matthew L. N. ^[4]

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1. Spitzer Science Center, Caltech, MS 220-6, Pasadena, CA 91125 (United States)
2. NASA Herschel Science Center, California Institute of Technology, Pasadena, CA 91125 (United States)
3. Department of Astronomy, University of Florida, Gainesville, FL 32611-2055 (United States)
4. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

We have observed warm molecular hydrogen in two nearby edge-on disk galaxies, NGC 4565 and NGC 5907, using the Spitzer high-resolution infrared spectrograph. The 0-0 S(0) 28.2 {mu}m and 0-0 S(1) 17.0 {mu}m pure rotational lines were detected out to 10 kpc from the center of each galaxy on both sides of the major axis, and in NGC 4565 the S(0) line was detected at r = 15 kpc on one side. This location is beyond the transition zone where diffuse neutral atomic hydrogen starts to dominate over cold molecular gas and marks a transition from a disk dominated by high surface-brightness far-infrared (far-IR) emission to that of a more quiescent disk. It also lies beyond a steep drop in the radio continuum emission from cosmic rays (CRs) in the disk. Despite indications that star formation activity decreases with radius, the H{sub 2} excitation temperature and the ratio of the H{sub 2} line and the far-IR luminosity surface densities, {Sigma}(L{sub H{sub 2}})/{Sigma}(L{sub TIR}), change very little as a function of radius, even into the diffuse outer region of the disk of NGC 4565. This suggests that the source of excitation of the H{sub 2} operates over a large range of radii and is broadly independent of the strength and relative location of UV emission from young stars. Although excitation in photodissociation regions is the most common explanation for the widespread H{sub 2} emission, CR heating or shocks cannot be ruled out. At r = 15 kpc in NGC 4565, outside the main UV- and radio-continuum-dominated disk, we derived a higher than normal H{sub 2} to 7.7 {mu}m polycyclic aromatic hydrocarbon (PAH) emission ratio, but this is likely due to a transition from mainly ionized PAH molecules in the inner disk to mainly neutral PAH molecules in the outer disk. The inferred mass surface densities of warm molecular hydrogen in both edge-on galaxies differ substantially, being 4(-60) M{sub sun} pc{sup -2} and 3(-50) M{sub sun} pc{sup -2} at r = 10 kpc for NGC 4565 and NGC 5907, respectively. The higher values represent very unlikely point-source upper limits. The point-source case is not supported by the observed emission distribution in the spectral slits. These mass surface densities cannot support the observed rotation velocities in excess of 200 km s{sup -1}. Therefore, warm molecular hydrogen cannot account for dark matter in these disk galaxies, contrary to what was implied by a previous Infrared Space Observatory study of the nearby edge-on galaxy NGC 891.

• OSTI ID: 21443248
• Journal Information: Astronomical Journal (New York, N.Y. Online), Vol. 140, Issue 3; Other Information: DOI: 10.1088/0004-6256/140/3/753; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COSMIC RADIATION
GALAXIES
HYDROGEN
LUMINOSITY
MASS
NONLUMINOUS MATTER
PHOTOLYSIS
POINT SOURCES
POLYCYCLIC AROMATIC HYDROCARBONS
STAR EVOLUTION
STARS
AROMATICS
CHEMICAL REACTIONS
DECOMPOSITION
ELEMENTS
EVOLUTION
HYDROCARBONS
IONIZING RADIATIONS
MATTER
NONMETALS
OPTICAL PROPERTIES
ORGANIC COMPOUNDS
PHOTOCHEMICAL REACTIONS
PHYSICAL PROPERTIES
RADIATION SOURCES
RADIATIONS