Computer Science
Scientific paper
Nov 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35279109p&link_type=abstract
VizieR On-line Data Catalog: J/A+A/527/A109. Originally published in: 2011A&A...527A.109P
Computer Science
Models, Galaxies: Photometry, Energy Distributions
Scientific paper
Simulated dust/PAH emission SEDs for the diffuse component of our model, for the parameter space sampled by the calculations:
-------------------------------------------------- | tau^f._B | SFR' | Old | B/D | | Msolar/yr | | -------------------------------------------------- 1 | 0.1 | 0.0 | 0.0 | 0.00 2 | 0.3 | 0.1 | 0.1 | 0.25 3 | 0.5 | 0.2 | 0.2 | 0.50 4 | 1.0 | 0.5 | 0.5 | 1.00 5 | 2.0 | 1.0 | 1.0 | 2.00 6 | 4.0 | 2.0 | 2.0 | 7 | 8.0 | 5.0 | 5.0 | 8 | | 10.0 | 10.0 | 9 | | 20.0 | 20.0 | -------------------------------------------------- where SFR' = SFR x (1-F) In total there are 2835 combinations, however those with SFR=0 and old=0 (no stellar luminosity at all) cannot exist, therefore the library contain only 2800 simulated SEDs. (the cases SFR'=0.0, Old=0.0 not simulated).
The second set of simulated data needed to fit the panchromatic SEDs is the library of attenuations in the UV/optical/NIR as a function of {tau}fB and inclination i. The description of the general characteristics of the attenuation curves can be found in Tuffs et al. (2004A&A...419..821T, Paper III), while the updated version of the calculations (due to the change in the dust model) is described in Appendix B and C of this present paper (Paper V).
To facilitate access to the information and to allow the attenuation to be calculated for any inclination, the attenuation curves are presented in form of polynomial function fits to the simulated data. The fitted function is given by Eq. 6 in Paper III. The values of the fitted coefficients are tabulated below for the old stellar disk (disk), young stellar disk (sdisk) and bulge. These are updates of Tables 4-6 from Paper III. The format is kept the same but calculations at two new UV wavelength (1500 and 3650Å) are added to the tables, to increase the sampling in the UV spectral region.
(5 data files).
Dopita Mike A.
Fischera Joerg
Kylafis Nick D.
Madore Barry F.
Popescu Costin
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