J/ApJ/817/118 SFR-M* relation from ZFOURGE (Tomczak+, 2016)
The SFR-M* relation and empirical star-formation histories from ZFOURGE at
0.5<z<4.
Tomczak A.R., Quadri R.F., Tran K.-V.H., Labbe I., Straatman C.M.S.,
Papovich C., Glazebrook K., Allen R., Brammer G.B., Cowley M.,
Dickinson M., Elbaz D., Inami H., Kacprzak G.G., Morrison G.E.,
Nanayakkara T., Persson S.E., Rees G.A., Salmon B., Schreiber C.,
Spitler L.R., Whitaker K.E.
<Astrophys. J., 817, 118 (2016)>
=2016ApJ...817..118T 2016ApJ...817..118T (SIMBAD/NED BibCode)
ADC_Keywords: Redshifts ; Galaxies, IR ; Ultraviolet
Keywords: galaxies: evolution; galaxies: luminosity function, mass function;
galaxies: star formation
Abstract:
We explore star formation histories (SFHs) of galaxies based on the
evolution of the star formation rate stellar mass relation (SFR-M*).
Using data from the FourStar Galaxy Evolution Survey (ZFOURGE) in
combination with far-IR imaging from the Spitzer and Herschel
observatories we measure the SFR-M* relation at 0.5<z<4. Similar to
recent works we find that the average infrared spectral energy
distributions of galaxies are roughly consistent with a single
infrared template across a broad range of redshifts and stellar
masses, with evidence for only weak deviations. We find that the
SFR-M* relation is not consistent with a single power law of the
form SFR∝M*α at any redshift; it has a power law
slope of α∼1 at low masses, and becomes shallower above a
turnover mass (M0) that ranges from 109.5 to 1010.8M☉,
with evidence that M0 increases with redshift. We compare our
measurements to results from state-of-the-art cosmological
simulations, and find general agreement in the slope of the SFR-M*
relation albeit with systematic offsets. We use the evolving SFR-M*
sequence to generate SFHs, finding that typical SFRs of individual
galaxies rise at early times and decline after reaching a peak. This
peak occurs earlier for more massive galaxies. We integrate these SFHs
to generate mass growth histories and compare to the implied mass
growth from the evolution of the stellar mass function (SMF). We find
that these two estimates are in broad qualitative agreement, but that
there is room for improvement at a more detailed level. At early times
the SFHs suggest mass growth rates that are as much as 10x higher than
inferred from the SMF. However, at later times the SFHs under-predict
the inferred evolution, as is expected in the case of additional
growth due to mergers.
Description:
The FourStar Galaxy Evolution Survey (ZFOURGE : Straatman C. M. S.,
Spitler L. R., Quadri R. F. et al 2015 ApJ submitted) is a deep
near-IR survey conducted with the FourStar imager covering one 11'x11'
pointing in each of the three legacy fields CDF-S (Giacconi et al.
2002, J/ApJS/139/369), COSMOS (Capak et al. 2007, II/284) and UDS
(Lawrence et al. 2007, see II/319) reaching depths of ∼26mag in J1,
J2, J3, and ∼25mag in Hs, Hl, and Ks.
We make use of Spizer/MIPS (GOODS-S: PI Dickinson, COSMOS: PI
Scoville, UDS: PI Dunlop) and Herschel/PACS data (GOODS-S: Elbaz et
al. 2011, J/A+A/533/A119, COSMOS & UDS: PI Dickinson) for measuring
total infrared luminosities (LIR) to derive SFRs. Imaging from these
observatories used in this study include 24, 100 and 160um.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 120 80 SFR-M* relations data
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See also:
II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)
II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007)
III/250 : The VIMOS VLT deep survey (VVDS-DEEP) (Le Fevre+ 2005)
J/MNRAS/421/3060 : Subaru/XMM Deep Field radio imaging. III. (Simpson+, 2012)
J/A+A/533/A119 : GOODS-Herschel North and South catalogs (Elbaz+, 2011)
J/A+A/532/A90 : PACS Evolutionary Probe (PEP-DR1) catalogs (Lutz+, 2011)
J/A+A/512/A12 : VLT/VIMOS spectroscopy in GOODS-South field (Balestra+, 2010)
J/ApJS/184/218 : The zCOSMOS 10k-bright spectroscopic sample (Lilly+, 2009)
J/ApJ/696/1195 : COSMOS AGN spectroscopic survey. I. (Trump+, 2009)
J/ApJ/682/985 : FIREWORKS photometry of GOODS CDF-S (Wuyts+, 2008)
J/A+A/478/83 : GOODS-South Field VLT/FORS2 redshifts. III. (Vanzella+, 2008)
J/ApJ/655/51 : HDFS IRAC observations of 2<z<3.5 galaxies (Wuyts+, 2007)
J/MNRAS/361/525 : Las Campanas Infrared Survey. V. (Doherty+, 2005)
J/ApJ/621/673 : Line indices for 124 early-type galaxies (Thomas+, 2005)
J/ApJS/155/271 : CDF-S: Optical spectroscopy (Szokoly+, 2004)
J/ApJ/586/794 : Multiwavelength luminosities of galaxies (Bell, 2003)
J/ApJS/139/369 : Chandra Deep Field South. 1 Ms catalog (Giacconi+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 --- zlow [0.5/3] Lower redshift bin range
6- 9 F4.2 --- zup [0.7/4] Upper redshift bin range
11- 16 F6.3 [Msun] logM [8.6/11.4] Log stellar mass (1)
18- 22 F5.2 [Lsun] logLUVf [9/10.6] Log restframe UV luminosity (2)
24- 27 F4.2 [Lsun] e_logLUVf Lower error in logLUVf
29- 32 F4.2 [Lsun] E_logLUVf [0/0.3] Upper error in logLUVf
34- 38 F5.2 [Lsun] logLIRf [8.1/12.5] Log bolometric IR luminosity (2)
40- 43 F4.2 [Lsun] e_logLIRf Lower error in logLIRf
45- 48 F4.2 [Lsun] E_logLIRf [0.02/1] Upper error in logLIRf
50- 54 F5.2 [Msun/yr] logSFRf [-0.4/2.5] Log UV+IR star-formation
rate (2)
56- 59 F4.2 [Msun/yr] e_logSFRf [0.02/0.2] Lower error in logSFRf
61- 64 F4.2 [Msun/yr] E_logSFRf Upper error in logSFRf
66- 70 F5.2 [Lsun] logLUVsf [9/10.6] Log restframe UV luminosity (3)
72- 75 F4.2 [Lsun] e_logLUVsf Lower error in logLUVsf
77- 80 F4.2 [Lsun] E_logLUVsf [0/0.4] Upper error in logLUVsf
82- 86 F5.2 [Lsun] logLIRsf [8.2/12.5] Log bolometric IR luminosity (3)
88- 91 F4.2 [Lsun] e_logLIRsf [0.02/0.8] Lower error in logLIRsf
93- 96 F4.2 [Lsun] E_logLIRsf Upper error in logLIRsf
98-102 F5.2 [Msun/yr] logSFRsf [-0.4/2.6] Log UV+IR star-formation
rate (3)
104-107 F4.2 [Msun/yr] e_logSFRsf [0.02/0.2] Lower error in logSFRsf
109-112 F4.2 [Msun/yr] E_logSFRsf Upper error in logSFRsf
114-116 I3 --- Nall [7/752] Number of galaxies from full sample
118-120 I3 --- Nsf [7/747] Number of galaxies from SF sample
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Note (1): Center of 0.25dex bins.
Note (2): For full sample (star-forming plus quiescent).
Note (3): For star-forming (SF) sample.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 18-Apr-2016