J/A+A/631/A156 Stellar populations of quiescent galaxies (Diaz-Garcia+, 2019)
Stellar populations of galaxies in the ALHAMBRA survey up to z∼1.
II. Stellar content of quiescent galaxies within the dust-corrected
stellar mass-colour and the UVJ colour-colour diagrams.
Diaz-Garcia L.A., Cenarro A.J., Lopez-Sanjuan C., Ferreras I.,
Cervino M., Fernandez-Soto A., Gonzalez Delgado R.M., Marquez I.,
Povic M., San Roman I., Viironen K., Moles M., Cristobal-Hornillos D.,
Lopez-Comazzi A., Alfaro E., Aparicio-Villegas T., Benitez N.,
Broadhurst T., Cabrera-Cano J., Castander F.J., Cepa J., Husillos C.,
Infante L., Aguerri J.A.L., Martinez V.J., Masegosa J., Molino A.,
del Olmo A., Perea J., Prada F., Quintana J.M.
<Astron. Astrophys. 631, A156 (2019)>
=2019A&A...631A.156D 2019A&A...631A.156D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Photometry, HST ; Stars, masses ; Stars, ages ;
Abundances, [Fe/H]
Keywords: galaxies: stellar content - galaxies: photometry -
galaxies: evolution - galaxies: formation -
Abstract:
Our aim is to determine the distribution of stellar population
parameters (extinction, age, metallicity, and star formation rates) of
quiescent galaxies within the rest-frame stellar mass-colour diagrams
and UVJ colour-colour diagrams corrected for extinction up to z∼1.
These novel diagrams reduce the contamination in samples of quiescent
galaxies owing to dust-reddened galaxies, and they provide useful
constraints on stellar population parameters only using rest-frame
colours and stellar mass.
We set constraints on the stellar population parameters of quiescent
galaxies combining the ALHAMBRA multi-filter photo-spectra with our
fitting code for spectral energy distribution, MUlti-Filter FITting
(MUFFIT), making use of composite stellar population models based on
two independent sets of simple stellar population (SSP) models. The
extinction obtained by MUFFIT allowed us to remove dusty star-forming
(DSF) galaxies from the sample of red UVJ galaxies. The distributions
of stellar population parameters across these rest-frame diagrams are
revealed after the dust correction and are fitted by LOESS, a
bi-dimensional and locally weighted regression method, to reduce
uncertainty effects.
Quiescent galaxy samples defined via classical UVJ diagrams are
typically contaminated by a 20% fraction of DSF galaxies. A
significant part of the galaxies in the green valley are actually
obscured star-forming galaxies (30-65%). Consequently, the transition
of galaxies from the blue cloud to the red sequence, and hence the
related mechanisms for quenching, seems to be much more efficient and
faster than previously reported. The rest-frame stellar mass-colour
and UVJ colour-colour diagrams are useful for constraining the age,
metallicity, extinction, and star formation rate of quiescent galaxies
by only their redshift, rest-frame colours, and/or stellar mass. Dust
correction plays an important role in understanding how quiescent
galaxies are distributed in these diagrams and is key to performing a
pure selection of quiescent galaxies via intrinsic colours.
Description:
Based on images from the ALHAMBRA-survey:
Moles et al., 2008AJ....136.1325M 2008AJ....136.1325M
Cristobal-Hornillos et al., 2009ApJ...696.1554C 2009ApJ...696.1554C
Aparicio-Villegas et al., 2010AJ....139.1242V 2010AJ....139.1242V ALHAMBRA
Area: 2.8deg2
Telescope: 3.5m on Calar Alto (www.caha.es)
Epoch Observation Dates: 2005-2012
Reference catalogue (photometry and photometric redshifts):
Molino et al., 2014MNRAS.441.2891M 2014MNRAS.441.2891M
File table1 contains the full set of stellar population parameters of
the sample of quiescent galaxies obtained using the SED-fitting code
MUFFIT (Diaz-Garcia et al., 2015A&A...582A..14D 2015A&A...582A..14D), the ALHAMBRA
photometric data (Moles et al., 2008AJ....136.1325M 2008AJ....136.1325M), and the BC03 SSP
models and the BC03 SSP models (Bruzual et al., 2003MNRAS.344.1000B 2003MNRAS.344.1000B).
Files qabasti and qapadova contain the same data than table1, but the
results were obtained using the SSP model of EMILES (Vazdekis et al.,
2016MNRAS.463.3409V 2016MNRAS.463.3409V BaSTI and Padova00 isochrones, respectively) to
build the sample of composite stellar population models.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 268 15894 ID, coordinates, stellar population properties,
uncertainties, and some fitting parameters,
using MUFFIT
qabasti.dat 268 16108 ID, coordinates, stellar population properties,
uncertainties, and some fitting parameters,
using EMILES (BaSTI isochrones)
qapadova.dat 268 14328 ID, coordinates, stellar population properties,
uncertainties, and some fitting parameters,
but using EMILES (Padova00 isochrones)
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See also:
https://archive.cefca.es/catalogues : ALHAMBRA quiescent galaxies Home Page
http://cosmo.iaa.es/content/alhambra-gold-catalog :
ALHAMBRA Gold Catalogue Home Page
Byte-by-byte Description of file: qabasti.dat qapadova.dat table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 I11 --- Name Object ID Number of the source
(814+Field+Pointing+CCD+ColorProindex)
13- 20 F8.4 deg RAdeg Right ascension (J2000)
22- 28 F7.4 deg DEdeg Declination (J2000)
30- 35 F6.3 mag F814W ALHAMBRA synthetic band (detection)
37- 41 F5.3 mag e_F814W ALHAMBRA synthetic band uncertainty
43- 47 F5.2 --- S/N Average signal-to-noise ratio
(galaxy photometry)
49- 50 I2 --- Nband Number of bands used in the analysis
52- 60 F9.4 --- Chi2 Reduced chi-squared value
62- 66 F5.3 --- z Photo redshift
68- 72 F5.3 --- e_z Photo redshift uncertainty
74- 88 F15.1 Msun Mstar Stellar mass
90-103 F14.1 Msun e_Mstar Stellar mass uncertainty
105-109 F5.3 mag Av Extinction (Rv=3.1)
111-115 F5.3 mag e_Av Extinction uncertainty
117-122 F6.3 Gyr AgeL Luminosity-weighted age
124-128 F5.3 Gyr e_AgeL Luminosity-weighted age uncertainty
130-135 F6.3 Gyr AgeM Mass-weighted age
137-141 F5.3 Gyr e_AgeM Mass-weighted age uncertainty
143-148 F6.3 [yr] logAgeL Luminosity-weighted age (log-scale)
150-154 F5.3 [yr] e_logAgeL Luminosity-weighted age uncertainty (log)
156-161 F6.3 [yr] logAgeM Mass-weighted age (log-scale)
163-167 F5.3 [yr] e_logAgeM Mass-weighted age uncertainty (log-scale)
169-174 F6.3 [-] [M/H]L Luminosity-weighted metallicity
176-180 F5.3 [-] e_[M/H]L Luminosity-weighted metallicity uncertainty
182-187 F6.3 [-] [M/H]M Mass-weighted metallicity
189-193 F5.3 [-] e_[M/H]M Mass-weighted metallicity uncertainty
195-200 F6.3 [Msun/yr] logSFR Star formation rate
202-206 F5.3 [Msun/yr] e_logSFR Star formation rate uncertainty
208-214 F7.3 [yr-1] logsSFR Specific star formation rate
216-220 F5.3 [yr-1] e_logsSFR Specific star formation rate uncertainty
222-226 F5.3 mag U-V Rest-frame colour F365W-F551W
228-232 F5.3 mag e_U-V Rest-frame colour F365W-F551W uncertainty
234-238 F5.3 mag V-J Rest-frame colour F551W-J
240-244 F5.3 mag e_V-J Rest-frame colour F551W-J uncertainty
246-250 F5.3 mag (U-V)int Intrinsic rest-frame colour F365W-F551W
(corrected for extinction)
252-256 F5.3 mag e_(U-V)int Intrinsic rest-frame colour uncertainty
(corrected for extinction)
258-262 F5.3 mag (V-J)int Intrinsic rest-frame colour F551W-J
(corrected for extinction)
264-268 F5.3 mag e_(V-J)int Intrinsic rest-frame colour uncertainty
(corrected for extinction)
--------------------------------------------------------------------------------
Acknowledgements:
Luis A. Diaz-Garcia, ladg84(at)gmail.com, cenarro(at)cefca.es
References:
Bruzual & Charlot, 2003MNRAS.344.1000B 2003MNRAS.344.1000B
Moles et al., 2008AJ....136.1325M 2008AJ....136.1325M
Cristobal-hornillos et al., 2009ApJ...696.1554C 2009ApJ...696.1554C
Aparicio-Villegas et al., 2010, Cat. J/AJ/139/1242
Molino et al., 2014, J/MNRAS/441/2891
Diaz-Garcia et al., 2015A&A...582A..14D 2015A&A...582A..14D
Vazdekis et al., 2016MNRAS.463.3409V 2016MNRAS.463.3409V
(End) Patricia Vannier [CDS] 25-Sep-2019