F. Zhang, L. Li, Y. Zhang, X. Kang, Z. Han
Using the evolutionary population synthesis (EPS) models with and without
binary interactions (BIs), we present LHa, L[OII], Li;UV and LFIR for Burst,
S0, Sa-Sd and Irr galaxies, and present the calibrations of star formation rate
(SFR) in terms of these diagnostics.
By comparison, we find that BIs lower the SFR.vs.LHa and SFR.vs.L[OII]
conversion factors by ~0.2 dex. Moreover, BIs do not significantly vary the
calibrations of SFR in terms of Li;UV. In addition, BIs have little effect on
the flux at 2800{\deg}A. At last, the calibration of SFR from LFIR is almost
unaffected by BIs. This is caused by the fact that BIs almost do not affect the
bolometric magnitudes of SPs.
We also discuss the effects of initial mass function (IMF), gas-recycle
assumption and EPS models (including models) on these SFR calibrations.
Comparing the results by using Salpeter (S55) IMF with those by using Miller &
Scalo (MS79) IMF, we find that the SFR.vs.LHa and SFR.vs.L[OII] conversion
factors by using S55 IMF are greater by 0.4 and 0.2 dex than those by using
MS79 IMF for the models with and without BIs, respectively. The SFR.vs.Li;UV
and SFR.vs.LFIR conversion factors by using S55 IMF are larger by an amount of
0.2 dex than the corresponding ones by using MS79 IMF. The inclusion of
gas-recycle assumption only lowers these SFR calibrations at faint SFR.
Moreover, comparing the results when using different EPS models, we find that
the differences in the SFR.vs.LHa and SFR.vs.L[OII] conversion factors reach ~
0.7 and 0.9 dex, the difference in the SFR.vs.LFIR conversion factor reaches
0.4 and 0.8 dex, and the differences in the SFR.vs.Li;UV conversion factors
reach 0.3 and 0.2 dex when using S55 and NON-S55 IMF (including Cha03, K01,
K93' and MS79 IMFs, partly caused by the difference in the IMF), respectively.
At last, we give the conversion coefficients between SFR and these diagnostics
for all models.
View original:
http://arxiv.org/abs/1112.1165
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