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dc.contributor.author
Domínguez, H.
dc.contributor.author
Mignoli, M.
dc.contributor.author
Pozzi, F.
dc.contributor.author
Calura, F.
dc.contributor.author
Cimatti, A.
dc.contributor.author
Gruppioni, C.
dc.contributor.author
Cepa, J.
dc.contributor.author
Sánchez-Portal, M.
dc.contributor.author
Zamorani, Gianni
dc.contributor.author
Berta, S.
dc.contributor.author
Elbaz, D.
dc.contributor.author
LeFloc'h, E.
dc.contributor.author
Granato, G. L.
dc.contributor.author
Lutz, D.
dc.contributor.author
Maiolino, R.
dc.contributor.author
Mateucci, F.
dc.contributor.author
Nair, P.
dc.contributor.author
Nordon, R.
dc.contributor.author
Pozzetti, L.
dc.contributor.author
Silva, L.
dc.contributor.author
Silverman, J.
dc.contributor.author
Wuyts, S.
dc.contributor.author
Carollo, C. Marcella
dc.contributor.author
Contini, T.
dc.contributor.author
Kneib, J.-P.
dc.contributor.author
LeFevrè, O.
dc.contributor.author
Lilly, S. J.
dc.contributor.author
Mainieri, V.
dc.contributor.author
Renzini, A.
dc.contributor.author
Scodeggio, M.
dc.contributor.author
Bardelli, S.
dc.contributor.author
Bolzonella, M.
dc.contributor.author
Bongiorno, A.
dc.contributor.author
Caputi, K.
dc.contributor.author
Coppa, G.
dc.contributor.author
Cucciati, O.
dc.contributor.author
de la Torre, S.
dc.contributor.author
de Ravel, L.
dc.contributor.author
Franzetti, P.
dc.contributor.author
Garilli, B.
dc.contributor.author
Iovino, A.
dc.contributor.author
Kampczyk, P.
dc.contributor.author
Knobel, C.
dc.contributor.author
Kovac, K.
dc.contributor.author
Lamareille, F.
dc.contributor.author
Le Borgne, J.-F.
dc.contributor.author
Maier, V. le Brun. C.
dc.contributor.author
Magnelli, B.
dc.contributor.author
Pellò, R.
dc.contributor.author
Peng, Y.
dc.contributor.author
Pérez-Montero, E.
dc.contributor.author
Riccardelli, E.
dc.contributor.author
Riguccini, L.
dc.contributor.author
Tanaka, M.
dc.contributor.author
Tasca, L. A. M.
dc.contributor.author
Tresse, L.
dc.contributor.author
Vergani, D.
dc.contributor.author
Zucca, E.
dc.date.accessioned
2017-06-10T13:35:18Z
dc.date.available
2017-06-10T13:35:18Z
dc.date.issued
2012
dc.identifier.uri
http://hdl.handle.net/20.500.11850/63034
dc.description.abstract
We empirically test the relation between the SFR(LIR) derived from the infrared luminosity, LIR, and the SFR(Ha) derived from the Ha emission line luminosity using simple conversion relations. We use a sample of 474 galaxies at z = 0.06 - 0.46 with both Ha detection (from 20k zCOSMOS survey) and new far-IR Herschel data (100 and 160 {\mu}m). We derive SFR(Ha) from the Ha extinction corrected emission line luminosity. We find a very clear trend between E(B - V) and LIR that allows to estimate extinction values for each galaxy even if the Ha emission line measurement is not reliable. We calculate the LIR by integrating from 8 up to 1000 {\mu}m the SED that is best fitting our data. We compare SFR(Ha) with the SFR(LIR). We find a very good agreement between the two SFR estimates, with a slope of m = 1.01 \pm 0.03 in the SFR(LIR) vs SFR(Ha) diagram, a normalization constant of a = -0.08 \pm 0.03 and a dispersion of sigma = 0.28 dex.We study the effect of some intrinsic properties of the galaxies in the SFR(LIR)-SFR(Ha) relation, such as the redshift, the mass, the SSFR or the metallicity. The metallicity is the parameter that affects most the SFR comparison. The mean ratio of the two SFR estimators log[SFR(LIR)/SFR(Ha)] varies by approx. 0.6 dex from metal-poor to metal-rich galaxies (8.1 < log(O/H) + 12 < 9.2). This effect is consistent with the prediction of a theoretical model for the dust evolution in spiral galaxies. Considering different morphological types, we find a very good agreement between the two SFR indicators for the Sa, Sb and Sc morphologically classified galaxies, both in slope and normalization. For the Sd, irregular sample (Sd/Irr), the formal best-fit slope becomes much steeper (m = 1.62 \pm 0.43), but it is still consistent with 1 at the 1.5 sigma level, because of the reduced statistics of this sub-sample.
dc.language.iso
en
dc.publisher
Cornell University
dc.title
Comparison of star formation rates from Halpha and infrared luminosities as seen by Herschel
dc.type
Working Paper
ethz.pages.start
arXiv:1205.4573
ethz.size
13 p.
ethz.notes
Submitted on 21 May 2012.
ethz.publication.place
Ithaca, NY
ethz.publication.status
published
ethz.leitzahl
ETH Zürich::00002 - ETH Zürich::00012 - Lehre und Forschung::00007 - Departemente::02010 - Dep. Physik / Dep. of Physics::03612 - Carollo, Marcella / Carollo, Marcella
ethz.leitzahl.certified
ETH Zürich::00002 - ETH Zürich::00012 - Lehre und Forschung::00007 - Departemente::02010 - Dep. Physik / Dep. of Physics::03612 - Carollo, Marcella / Carollo, Marcella
ethz.date.deposited
2017-06-10T13:36:58Z
ethz.source
ECIT
ethz.identifier.importid
imp5936504f1c78f28752
ethz.ecitpid
pub:99968
ethz.eth
yes
ethz.availability
Metadata only
ethz.rosetta.installDate
2017-07-12T23:36:18Z
ethz.rosetta.lastUpdated
2018-12-02T05:51:18Z
ethz.rosetta.versionExported
true
ethz.COinS
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