J/ApJ/777/18 Stellar mass functions of galaxies to z=4 (Muzzin+, 2013)
The evolution of the stellar mass functions of star-forming and quiescent
galaxies to z = 4 from the COSMOS/UltraVISTA survey.
Muzzin A., Marchesini D., Stefanon M., Franx M., McCracken H.J.,
Milvang-Jensen B., Dunlop J.S., Fynbo J.P.U., Brammer G., Labbe I.,
van Dokkum P.G.
<Astrophys. J., 777, 18 (2013)>
=2013ApJ...777...18M 2013ApJ...777...18M
ADC_Keywords: Redshifts ; Galaxies, IR ; Surveys
Keywords: galaxies: evolution; galaxies: fundamental parameters;
galaxies: high-redshift; galaxies: luminosity function, mass function
Abstract:
We present measurements of the stellar mass functions (SMFs) of
star-forming and quiescent galaxies to z=4 using a sample of 95675
Ks-selected galaxies in the COSMOS/UltraVISTA field (Muzzin et al.
2013ApJS..206....8M 2013ApJS..206....8M). The SMFs of the combined population are in good
agreement with previous measurements and show that the stellar mass
density of the universe was only 50%, 10%, and 1% of its current value
at z∼0.75, 2.0, and 3.5, respectively. The quiescent population drives
most of the overall growth, with the stellar mass density of these
galaxies increasing as ρstar∝(1+z)-4.7±0.4 since
z=3.5, whereas the mass density of star-forming galaxies increases as
ρstar∝(1+z)^-2.3 ±0.2^. At z>2.5, star-forming
galaxies dominate the total SMF at all stellar masses, although a
non-zero population of quiescent galaxies persists to z=4. Comparisons
of the Ks-selected star-forming galaxy SMFs with UV-selected SMFs at
2.5<z<4 show reasonable agreement and suggest that UV-selected samples
are representative of the majority of the stellar mass density at
z>3.5. We estimate the average mass growth of individual galaxies by
selecting galaxies at fixed cumulative number density. The average
galaxy with log(Mstar/M☉)=11.5 at z=0.3 has grown in mass by
only 0.2dex (0.3dex) since z=2.0 (3.5), whereas those with
log(Mstar/M☉)=10.5 have grown by >1.0dex since z=2. At z<2,
the time derivatives of the mass growth are always larger for
lower-mass galaxies, which demonstrates that the mass growth in
galaxies since that redshift is mass-dependent and primarily
bottom-up. Lastly, we examine potential sources of systematic
uncertainties in the SMFs and find that those from photo-z templates,
stellar population synthesis modeling, and the definition of quiescent
galaxies dominate the total error budget in the SMFs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 106 180 Best-fit SMF parameters from SED modeling
table4.dat 106 60 Best-fit SMF parameters from UVJ color-color
diagram (rest-frame U-V versus V-J)
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See also:
II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007)
J/A+A/556/A55 : Multi-color photometry of star-forming galaxies (Ilbert+, 2013)
J/ApJ/771/85 : Dynamical masses of z∼2 quiescent gal. (van de Sande+, 2013)
J/MNRAS/428/1128 : UDS/COSMOS HiZELS galaxies (Sobral+, 2013)
J/A+A/544/A156 : UltraVISTA Catalogue Release DR1 (McCracken+, 2012)
J/ApJ/735/86 : NEWFIRM MBS: photometric catalogs (Whitaker+, 2011)
J/ApJ/682/985 : FIREWORKS photometry of GOODS CDF-S (Wuyts+, 2008)
J/ApJ/675/234 : Stellar mass functions for gal. 0<z<4 (Perez-Gonzalez+, 2008)
J/ApJS/172/70 : zCOSMOS-bright catalog (Lilly+, 2007)
J/ApJ/655/51 : HDFS IRAC observations of 2<z<3.5 galaxies (Wuyts+, 2007)
J/AJ/131/1891 : Photom. survey of MS 1054-03 field (Foerster-Schreiber+, 2006)
J/AJ/125/1107 : Ultra-deep near-IR observation in HDF-S (Labbe+, 2003)
Byte-by-byte Description of file: table[34].dat
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Bytes Format Units Label Explanations
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1- 3 F3.1 --- zmin [0.2/3] Lower limit redshift boundary
5- 7 F3.1 --- zmax [0.5/4] Upper limit redshift boundary
9- 17 A9 --- Sample Sample used (1)
19- 23 I5 --- Nu [13/43118] Number of galaxies used
25- 29 F5.2 [Msun] M* [10/12.2] Characteristic stellar mass M* (2)
31- 34 F4.2 [Msun] E_M* Upper uncertainty in M*
36- 39 F4.2 [Msun] e_M* Lower uncertainty in M*
41- 45 F5.2 10-4/Mpc3 Phi* [0.01/48.1] Number density of galaxies
normalization Φ* (2)
47- 50 F4.2 10-4/Mpc3 E_Phi* Upper uncertainty in Phi
52- 55 F4.2 10-4/Mpc3 e_Phi* Lower uncertainty in Phi
57- 61 F5.2 --- alpha [-2.4/3.4] Low-mass-end slope α
63- 66 F4.2 --- E_alpha Upper uncertainty in alpha
68- 71 F4.2 --- e_alpha Lower uncertainty in alpha
73- 78 F6.3 10-4/Mpc3 Phi*2 [0.002/13]? Log of 2nd characteristic
stellar mass (3)
80- 84 F5.3 10-4/Mpc3 E_Phi*2 ? Upper uncertainty in Phi2
86- 90 F5.3 10-4/Mpc3 e_Phi*2 ? Lower uncertainty in Phi2
92- 96 F5.2 --- alpha2 [-2.6/-1.2]? The 2nd low-mass-end slope (3)
98-101 F4.2 --- E_alpha2 ? Upper uncertainty in alpha2
103-106 F4.2 --- e_alpha2 ? Lower uncertainty in alpha2
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Note (1): Sample as follows:
A = all galaxy samples;
Q = quiescent galaxy samples;
SF = star-forming galaxy samples;
MET = leaving metallicity as a free parameter in SED modeling;
SFH = allowing a delayed-tau model star formation history in SED modeling;
DUSTY = including an additional old-and-dusty template in SED modeling;
MA05 = using the Maraston (2005MNRAS.362..799M 2005MNRAS.362..799M) models instead of the
Bruzual & Charlot (2003MNRAS.344.1000B 2003MNRAS.344.1000B) models in SED modeling.
UVpVJm = movement of the UV or VJ cut in measurement by plus 0.1mag;
UVmVJp = movement of the UV or VJ cut in measurement by minus 0.1mag.
Note (2): The stellar mass functions (SMF) Φ(M), the density of galaxies,
is assumed to follow a Schechter (1976ApJ...203..297S 1976ApJ...203..297S) function given in
Eq.(4): Φ(M)=(ln10)Φ*[10(M-M*)(1+α)].exp[-10(M-M*)].
Here M=log(Mstar/M☉) is the stellar logarithmic mass, α is the
low-mass-end slope, M*=log(M*star/M☉) is the characteristic mass,
and Φ* is the normalization (see section 3). The parameters are
determined using the maximum-likelihood method outlined by Sandage et al.
(1979ApJ...232..352S 1979ApJ...232..352S).
Note (3): Fit to two Schechter functions simultaneously.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 26-Mar-2015