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Modelling the spectral energy distribution of galaxies - II. Disk opacity and star formation in 5 edge-on spirals

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Popescu,  C. C.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

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Tuffs,  R.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

Misiriotis, A., Popescu, C. C., Tuffs, R., & Kylafis, N. D. (2001). Modelling the spectral energy distribution of galaxies - II. Disk opacity and star formation in 5 edge-on spirals. Astronomy & Astrophysics, 372(3), 775-783. Retrieved from http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2001A%26A..372.775M&db_key=AST&high=3fd59969ac20031.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0011-8580-5
Abstract
Using tools previously described and applied to the prototype galaxy NGC 891, we model the optical to far-infrared spectral energy distributions (SED) of four additional edge-on spiral galaxies, namely NGC 5907, NGC 4013, UGC 1082 and UGC 2048. Comparing the model predictions with IRAS and, where available, submillimeter and millimeter observations, we determine the respective roles of the old and young stellar populations in grain heating. In all cases, the young population dominates, with the contribution of the old stellar population being at most 40%, as previously found for NGC 891. After normalization to the disk area, the massive star-formation rate (SFR) derived using our SED modeling technique, which is primarily sensitive to the non-ionizing ultraviolet output from the young stellar population, lies in the range 7 x 10(-4) 2 x 10(2) M-circle dot yr(-1) kpc(-2). This is consistent with normalized SFRs derived for face-on galaxies of comparable surface gas densities from H-alpha observations. Though the most active star-forming galaxy of the five in absolute terms, NGC 891 is not an exceptional system in terms of its surface density in SFR.