Insights on star formation histories and physical properties of \$1.2 {\textbackslash}leq z {\textbackslash}lesssim 4 \$ Herschel-detected galaxies

Insights on star formation histories and physical properties of \$1.2 {\textbackslash}leq z {\textbackslash}lesssim 4 \$ Herschel-detected galaxies. Sklias, P., Schaerer, D., Elbaz, D., Pannella, M., Schreiber, C., & Cava, A. ArXiv e-prints, 1705:arXiv:1705.01174, May, 2017.
$Insights on star formation histories and physical properties of \$1.2 {\textbackslash}leq z {\textbackslash}lesssim 4 \$ Herschel-detected galaxies [link]$ Paper abstract bibtex

We test the impact of using variable star forming histories (SFHs) and the use of the IR luminosity (LIR) as a constrain on the physical parameters of high redshift dusty star-forming galaxies. We explore in particular the stellar properties of galaxies in relation with their location on the SFR-M* diagram. We perform SED fitting of the UV-NIR and FIR emissions of a large sample of GOODS-Herschel galaxies, for which rich multi-wavelength observations are available. We test different SFHs and imposing energy conservation in the SED fitting process, to face issues like the age-extinction degeneracy and produce SEDs consistent with observations. Our models work well for the majority of the sample, with the notable exception of the high LIR end, for which we have indications that our simple energy conservation approach cannot hold true. We find trends in the SFHs fitting our sources depending on stellar mass M* and z. Trends also emerge in the characteristic timescales of the SED models depending on the location on the SFR-M* diagram. We show that whilst using the same available observational data, we can produce galaxies less star-forming than usually inferred, if we allow declining SFHs, while properly reproducing their observables. These sources can be post-starbursts undergoing quenching, and their SFRs are potentially overestimated if inferred from their LIR. Fitting without the IR constrain leads to a strong preference for declining SFHs, while its inclusion increases the preference of rising SFHs, more so at high z, in tentative agreement with the cosmic star formation history. Keeping in mind that the sample is biased towards high LIR, the evolution shaped by our model appears as both bursty (initially) and steady-lasting (later on). The global SFH of the sample follows the cosmic SFH with a small scatter, and is compatible with the "downsizing" scenario of galaxy evolution.

@article{sklias_insights_2017,
	title = {Insights on star formation histories and physical properties of \$1.2 {\textbackslash}leq z {\textbackslash}lesssim 4 \$ {Herschel}-detected galaxies},
	volume = {1705},
	url = {http://adsabs.harvard.edu/abs/2017arXiv170501174S},
	abstract = {We test the impact of using variable star forming histories (SFHs) and 
the use of the IR luminosity (LIR) as a constrain on the physical
parameters of high redshift dusty star-forming galaxies. We explore in
particular the stellar properties of galaxies in relation with their
location on the SFR-M* diagram. We perform SED fitting of the UV-NIR and
FIR emissions of a large sample of GOODS-Herschel galaxies, for which
rich multi-wavelength observations are available. We test different SFHs
and imposing energy conservation in the SED fitting process, to face
issues like the age-extinction degeneracy and produce SEDs consistent
with observations. Our models work well for the majority of the sample,
with the notable exception of the high LIR end, for which we have
indications that our simple energy conservation approach cannot hold
true. We find trends in the SFHs fitting our sources depending on
stellar mass M* and z. Trends also emerge in the characteristic
timescales of the SED models depending on the location on the SFR-M*
diagram. We show that whilst using the same available observational
data, we can produce galaxies less star-forming than usually inferred,
if we allow declining SFHs, while properly reproducing their
observables. These sources can be post-starbursts undergoing quenching,
and their SFRs are potentially overestimated if inferred from their LIR.
Fitting without the IR constrain leads to a strong preference for
declining SFHs, while its inclusion increases the preference of rising
SFHs, more so at high z, in tentative agreement with the cosmic star
formation history. Keeping in mind that the sample is biased towards
high LIR, the evolution shaped by our model appears as both bursty
(initially) and steady-lasting (later on). The global SFH of the sample
follows the cosmic SFH with a small scatter, and is compatible with the
"downsizing" scenario of galaxy evolution.},
	urldate = {2017-05-12},
	journal = {ArXiv e-prints},
	author = {Sklias, P. and Schaerer, D. and Elbaz, D. and Pannella, M. and Schreiber, C. and Cava, A.},
	month = may,
	year = {2017},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:1705.01174},
}

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We perform SED fitting of the UV-NIR and FIR emissions of a large sample of GOODS-Herschel galaxies, for which rich multi-wavelength observations are available. We test different SFHs and imposing energy conservation in the SED fitting process, to face issues like the age-extinction degeneracy and produce SEDs consistent with observations. Our models work well for the majority of the sample, with the notable exception of the high LIR end, for which we have indications that our simple energy conservation approach cannot hold true. We find trends in the SFHs fitting our sources depending on stellar mass M* and z. Trends also emerge in the characteristic timescales of the SED models depending on the location on the SFR-M* diagram. We show that whilst using the same available observational data, we can produce galaxies less star-forming than usually inferred, if we allow declining SFHs, while properly reproducing their observables. 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