Comparison of star formation rates from Ha and infrared luminosity as seen by Herschel

被引：24

作者：

Dominguez Sanchez, H. ^{[1
,2
]}

Mignoli, M. ^{[1
]}

Pozzi, F. ^{[3
]}

Calura, F. ^{[1
]}

Cimatti, A. ^{[3
]}

Gruppioni, C. ^{[1
]}

Cepa, J. ^{[2
]}

Sanchez Portal, M. ^{[4
]}

Zamorani, G. ^{[1
]}

Berta, S. ^{[5
]}

Elbaz, D. ^{[6
]}

Le Floc'h, E. ^{[7
]}

Granato, G. L. ^{[8
]}

Lutz, D. ^{[5
]}

Maiolino, R. ^{[9
]}

Matteucci, F. ^{[10
]}

Nair, P. ^{[1
,11
]}

Nordon, R. ^{[5
]}

Pozzetti, L. ^{[1
]}

Silva, L. ^{[8
]}

Silverman, J. ^{[12
]}

Wuyts, S. ^{[5
]}

Carollo, C. M. ^{[13
]}

Contini, T. ^{[14
]}

Kneib, J. -P. ^{[15
]}

Le Fevre, O. ^{[15
]}

Lilly, S. J. ^{[13
]}

Mainieri, V. ^{[16
]}

Renzini, A. ^{[17
]}

Scodeggio, M. ^{[18
]}

Bardelli, S. ^{[1
]}

Bolzonella, M. ^{[1
]}

Bongiorno, A. ^{[5
]}

Caputi, K. ^{[19
]}

Coppa, G. ^{[1
,3
]}

Cucciati, O. ^{[8
]}

de la Torre, S. ^{[18
,20
]}

de Ravel, L. ^{[15
,19
]}

Franzetti, P. ^{[18
]}

Garilli, B. ^{[18
]}

Iovino, A. ^{[20
]}

Kampczyk, P. ^{[13
]}

Knobel, C. ^{[13
]}

Kovac, K. ^{[13
]}

Lamareille, F. ^{[14
]}

Le Borgne, J. -F. ^{[14
]}

Le Brun, V. ^{[15
]}

Maier, C. ^{[13
]}

Magnelli, B. ^{[5
]}

Pello, R. ^{[14
]}

机构：

[1] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy

[2] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain

[3] Alma Mater Studiorum Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[4] ESA, European Space Astron Ctr ESAC, Madrid 28692, Spain

[5] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[6] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France

[7] Univ Paris Diderot, CEA Saclay, Lab AIM, CEA,DSM,CNRS,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France

[8] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[9] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[10] Univ Trieste, Dipartimento Fis, Sez Astron, I-34127 Trieste, Italy

[11] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[12] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan

[13] ETH, Inst Astron, CH-8093 Zurich, Switzerland

[14] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France

[15] Univ Aix Marseille, Lab Astrophys Marseille, F-13388 Marseille 13, France

[16] European So Observ, D-85748 Garching, Germany

[17] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[18] IASF Milano, INAF, I-20133 Milan, Italy

[19] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands

[20] Osserv Astron Brera, INAF, I-20121 Milan, Italy

[21] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 426卷 / 01期

关键词：

dust; extinction; galaxies: formation; infrared: galaxies; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE INDICATORS; HIGH-REDSHIFT GALAXIES; DIGITAL SKY SURVEY; DEEP-FIELD-SOUTH; SIMILAR-TO; FORMING GALAXIES; FORMATION HISTORIES; STARBURST GALAXIES; DISK GALAXIES;

D O I：

10.1111/j.1365-2966.2012.21710.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We empirically MD 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 = 0.060.46 with both Ha detection [from 20k redshift Cosmological Evolution (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 us to estimate extinction values for each galaxy even if the H beta emission line measurement is not reliable. We calculate the LIR by integrating from 8 up to 1000 mu m the spectral energy distribution (SED) that is best fitting our data. We compare the SFR(Ha) with the SFR(LIR). We find a very good agreement between the two star formation rate (SFR) estimates, with a slope of m = 1.01 +/- 0.03 in the log SFR(LIR) versus log SFR(Ha) diagram, a normalization constant of a = -0.08 +/- 0.03 and a dispersion of s = 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 specific star formation rate (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 similar to 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 in normalization. For the Sd, irregular sample (Sd/Irr), the formal best-fitting slope becomes much steeper (m = 1.62 +/- 0.43), but it is still consistent with 1 at the 1.5s level, because of the reduced statistics of this sub-sample.

引用

页码：330 / 341

页数：12

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