J/MNRAS/485/586 Star formation in galaxy cluster cores (Rodriguez-Munoz+, 2019)
Quantifying the suppression of the (un)-obscured star formation in galaxy
cluster cores at 0.2≤z≤0.9.
Rodriguez-Munoz L., Rodighiero G., Mancini C., Perez-Gonzalez P.G.,
Rawle T.D., Egami E., Mercurio A., Rosati P., Puglisi A., Franceschini A.,
Balestra I., Baronchelli I., Biviano A., Ebeling H., Edge A.C.,
Enia A.F.M., Grillo C., Haines C.P., Iani E., Jones T., Nonino M.,
Valtchanov I., Vulcani B., Zemcov M.
<Mon. Not. R. Astron. Soc., 485, 586-619 (2019)>
=2019MNRAS.485..586R 2019MNRAS.485..586R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Clusters, galaxy ; Galaxy catalogs ;
Photometry, ultraviolet ; Photometry, infrared
Keywords: galaxies: clusters: general - galaxies: evolution -
galaxies: star formation - catalogues
Abstract:
We quantify the star formation (SF) in the inner cores (R/R200~<0.3)
of 24 massive galaxy clusters at 0.2~<z~<0.9 observed by the Herschel
Lensing Survey and the Cluster Lensing and Supernova survey with
Hubble. These programmes, covering the rest-frame ultraviolet to
far-infrared regimes, allow us to accurately characterize stellar
mass-limited (M*>1010M☉) samples of star-forming cluster
members (not)-detected in the mid- and/or far-infrared. We release the
catalogues with the photometry, photometric redshifts, and physical
properties of these samples. We also quantify the SF displayed by
comparable field samples from the Cosmic Assembly Near-infrared Deep
Extragalactic Legacy Survey. We find that in intermediate-z cluster
cores, the SF activity is suppressed with respect the field in terms
of both the fraction (F) of star-forming galaxies (SFGs) and the rate
at which they form stars (SFR and sSFR=SFR/M*). On average, the F of
SFGs is a factor ∼2 smaller in cluster cores than in the field.
Furthermore, SFGs present average SFR and sSFR typically ∼0.3dex
smaller in the clusters than in the field along the whole redshift
range probed. Our results favour long time-scale quenching physical
processes as the main driver of SF suppression in the inner cores of
clusters since z∼0.9, with shorter time-scale processes being very
likely responsible for a fraction of the missing SFG population.
Description:
We have presented a detailed analysis of the SF activity within 24
massive clusters cores at 0.2~<z~<0.9 targeted by the HLS (Egami et
al. 2010A&A...518L..12E 2010A&A...518L..12E) and CLASH (Postman et al.
2012ApJS..199...25P 2012ApJS..199...25P, Cat. J/ApJS/199/25) surveys. The deep
multiwavelength photometric data set on these fields cover the whole
rest-frame UV-to-FIR regimes. In particular, we have made use of the
CLASH catalogues, which contain photometry measured on HST ACS/WFC
(F435W, F475W, F606W, F625W, F775W, F814W, and F850LP), WFC3/UVIS
(F225W, F275W, F336W, and F390W), and WFC3/IR (F105W, F110W, F125W,
F140W, and F160W) imaging. Then, we have combined these catalogues
with others built on Spitzer/IRAC (Fazio et al. 2004ApJS..154...10F 2004ApJS..154...10F)
(3.6, 4.5, 5.8, and 8.0µm) and MIPS (Rieke et al.
2004ApJS..154...25R 2004ApJS..154...25R) (24µm) bands, and Herschel/PACS (100 and
160µm) and SPIRE (Griffin et al. 2010A&A...518L...3G 2010A&A...518L...3G) (250, 350,
and 500µm), deblending the former in the position of the CLASH
catalogues and selecting the most probable UV/optical counterpart for
the sources in the MIR and FIR bands. Finally, we have also gathered
the spectroscopic informations available on these fields, mainly
released by CLASH-VLT (Rosati et al. 2014Msngr.158...48R 2014Msngr.158...48R) and GLASS
(Schmidt et al. 2014ApJ...782L..36S 2014ApJ...782L..36S; Treu et al. 2015ApJ...812..114T 2015ApJ...812..114T,
Cat. J/ApJ/812/114) surveys.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 110 24 Description of the galaxy cluster sample
table2.dat 33 26 Overview of the photometric bands used in this
work
table3.dat 54 24 Limiting fluxes (5σ) of the Spitzer and
Herschel photometric catalogues used in this
work
table4.dat 30 10 Summary of some of the quantities used for the
identification of cluster members and an
evaluation of the technique
table5.dat 108 24 Number of galaxies selected with the different
criteria used to build the final samples of
star-forming cluster members (R/R200<0.1),
and average SF activity indicators
table6.dat 145 24 Number of galaxies selected with the different
criteria used to build the final samples of
star-forming cluster members (0.1<R/R200<0.2),
and average SF activity indicators
table7.dat 145 24 Number of galaxies selected with the different
criteria used to build the final samples of
star-forming cluster members (0.2<R/R200<0.3),
and average SF activity indicators
table8.dat 145 24 Number counts and average properties of field
galaxy samples
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Cluster ID
10- 11 I2 h RAh Right ascension (J2000) (1)
13- 14 I2 min RAm Right ascension (J2000) (1)
16- 20 F5.2 s RAs Right ascension (J2000) (1)
22 A1 --- DE- Declination sign (J2000) (1)
23- 24 I2 deg DEd Declination (J2000) (1)
26- 27 I2 arcmin DEm Declination (J2000) (1)
29- 32 F4.1 arcsec DEs Declination (J2000) (1)
34- 38 F5.3 --- z Redshift from Postman et al.
(2012ApJS..199...25P 2012ApJS..199...25P, Cat. J/ApJS/199/25)
40 A1 --- f_z [*] Flag on redshift (2)
42- 45 I4 km/s sigcl Velocity dispersion σcl (3)
47- 49 I3 km/s E_sigcl ? Upper error on sigcl
51- 53 I3 km/s e_sigcl ? Lower error on sigcl
55 A1 --- r_sigcl References for sigcl (5)
57- 60 I4 kpc R200 Radius within which the mean density is 200
times the critical density at the redshift
where the cluster is located (4)
62- 64 I3 kpc E_R200 ? Upper error on R200
66- 68 I3 kpc e_R200 ? Lower error on R200
70 A1 --- r_R200 References for R200 (5)
72 A1 --- l_SFRUV Limit flag on SFRUV
74- 79 F6.2 Msun/yr SFRUV ? SF activity of the BCG as quantified through
the emission of the UV, corrected for
extinction (Fogarty et al.
2015ApJ...813..117F 2015ApJ...813..117F)
81- 85 F5.2 Msun/yr e_SFRUV ? Error on SFRUV
87- 90 F4.1 Msun/yr SFRFIR ? SF activity of the BCG as quantified through
the emission of the FIR (Rawle et al.
2012ApJ...747...29R 2012ApJ...747...29R)
92- 94 F3.1 Msun/yr e_SFRFIR ? Error on SFRFIR
96-100 F5.3 --- C CC tracer C parameter as published by
Donahue et al. 2016ApJ...819...36D 2016ApJ...819...36D
102-104 I3 --- Nzpec ? Number of spectroscopic redshifts within the
area covered by the CLASH catalogue
(∼0.0015deg2)
106-110 A5 --- r_Nzpec References for Nzpec (5)
--------------------------------------------------------------------------------
Note (1): Coordinates of the cluster centre as in Postman et al.
(2012ApJS..199...25P 2012ApJS..199...25P, Cat. J/ApJS/199/25)
Note (2): Flag as follows:
* = 0.209 according to Mercurio et al. (2003A&A...397..431M 2003A&A...397..431M,
Cat. J/A+A/397/431)
Note (3): We use the value 1600km/s when no observational estimation was found
in the literature
Note (4): R200∼Rvirial according to the simulations of Evrard, Metzler & Navarro
1996ApJ...469..494E 1996ApJ...469..494E; we use R200=2000kpc, see for instance
Umetsu et al. (2014ApJ...795..163U 2014ApJ...795..163U), for those cases for which no
precise value was found in the literature
Note (5): References as follows:
a = Geller et al. (2014ApJ...783...52G 2014ApJ...783...52G, Cat. J/ApJ/783/52)
b = Mercurio et al. (2003A&A...397..431M 2003A&A...397..431M, Cat. J/A+A/397/431)
c = Gomez et al. (2012AJ....144...79G 2012AJ....144...79G)
d = Balestra et al. (2016ApJS..224...33B 2016ApJS..224...33B, Cat. J/ApJS/224/33)
e = Biviano et al. (2013A&A...558A...1B 2013A&A...558A...1B)
f = Ebeling et al. (2007ApJ...661L..33E 2007ApJ...661L..33E)
g = Annunziatella et al. (2016A&A...585A.160A 2016A&A...585A.160A)
h = Newman et al. (2013ApJ...765...24N 2013ApJ...765...24N)
i = Rosati et al. (2014Msngr.158...48R 2014Msngr.158...48R)
j = Coe et al. (2012ApJ...757...22C 2012ApJ...757...22C, Cat. J/ApJ/757/22)
k = Karman et al. (2015A&A...574A..11K 2015A&A...574A..11K)
l = Huchra et al. (2012ApJS..199...26H 2012ApJS..199...26H, Cat. J/ApJS/199/26)
m = Ebeling, Ma & Barrett (2014ApJS..211...21E 2014ApJS..211...21E, Cat. J/ApJS/211/21)
n = Treu et al. (2015ApJ...812..114T 2015ApJ...812..114T, Cat. J/ApJ/812/114) and
Schmidt et al. (2014ApJ...782L..36S 2014ApJ...782L..36S)
o = Ravindranath & Ho (2002ApJ...577..133R 2002ApJ...577..133R)
p = Cohen & Kneib (2002ApJ...573..524C 2002ApJ...573..524C)
q = Shectman et al. (1996ApJ...470..172S 1996ApJ...470..172S, Cat. VII/203)
r = Abazajian et al. (2009ApJS..182..543A 2009ApJS..182..543A, Cat. II/294)
s = sigma and R200 derived using the value of the mass within R200 (M200)
from Umetsu et al. (2014ApJ...795..163U 2014ApJ...795..163U)
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Band Name of the instrument and observing band
13- 21 F9.5 um wleff Effective wavelength of the filter
23- 27 F5.2 arcsec FWHM Median FWHM of the PSF
29- 33 A5 --- Project Name of the project to which the data
belongs (1)
--------------------------------------------------------------------------------
Note (1): Project as follows:
a = Spitzer Programs numbers 17 (PI: Fazio), 83 (PI: Rieke), 545 (PI: Egami),
40652 (PI: Kocevski), 50393 (PI: Kocevski), 60034 (PI: Egami), and
80168 (PI: Bouwens)
b = Spitzer Programs numbers 83 (PI: Rieke), 40652 (PI: Kocevski),
40872 (PI: Smith), and 50393 (PI: Kocevski)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Cluster ID
10- 12 F3.1 uJy FIRAC3.6 Spitzer/IRAC 3.6um limiting flux (5σ)
14- 16 F3.1 uJy FIRAC4.5 Spitzer/IRAC 4.5um limiting flux (5σ)
18- 20 F3.1 uJy FIRAC5.8 ? Spitzer/IRAC 5.8um limiting flux (5σ)
22- 24 F3.1 uJy FIRAC8.0 ? Spitzer/IRAC 8.0um limiting flux (5σ)
26- 30 F5.1 uJy FMIPS24 ? Spitzer/MIPS 24um limiting flux (5σ)
32- 34 F3.1 mJy FPACS100 Herschel/PACS 100um limiting flux (5σ)
36- 39 F4.1 mJy FPACS160 Herschel/PACS 160um limiting flux (5σ)
41- 44 F4.1 mJy FSPIRE250 Herschel/SPIRE 250um limiting flux (5σ)
46- 49 F4.1 mJy FSPIRE350 Herschel/SPIRE 350um limiting flux (5σ)
51- 54 F4.1 mJy FSPIRE500 Herschel/SPIRE 500um limiting flux (5σ)
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Cluster ID
10- 12 I3 --- Nz Number of spectroscopic members (1)
14- 17 F4.2 --- sigNMAD Normalized median absolute deviation of the
difference between the zphot and the zspec (2)
19 I1 --- n Number of sigNMAD to be used in the integration
of the P(z) (3)
21- 24 F4.2 --- Pthr Membership probability threshold
26- 27 I2 --- K Completeness level (per cent)
29- 30 I2 --- I Fraction of interlopers (per cent)
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Note (1): The spectroscopic cluster members are identified as those galaxies
with zspec within the redshift range defined by the redshift of the
cluster, zcl, and its velocity dispersion, σcl.
In practice, we use the following criteria (see Cava et al.
2009A&A...495..707C 2009A&A...495..707C, Cat. J/A+A/495/707):
|zcl-zspec|<3σcl(1+zcl)
Note (2): sigNMAD is defined as
sigNMAD=1.48median(|Δz-median(Δz)/|1+zspec|), where
Δz=zphot-zspec
Note (3): Redshift probability distribution, P(z), given by the EAZY code
(Brammer, van Dokkum & Coppi 2008ApJ...686.1503B 2008ApJ...686.1503B)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Cluster ID
10- 11 I2 --- Membcut Number of cluster members with a detection
at a level >3σ in IRAC 4.5um and
M*>1010M☉
13- 15 I3 --- Memb Number of cluster members without the
M* cut
17- 18 I2 --- UVJSF Number of galaxies selected as
star-forming using the UVJ diagram
and/or detected in the MIR and/or FIR
(M>1010M☉), what we call the
UVJ-SF sample
20 I1 --- MFIRcut Cluster members with M*>1010M☉
detected in the MIR and/or FIR with
SFRTIR>10M☉/yr what we call MFIR
sample
22 I1 --- MFIR Total number of cluster members without
SFRTIR cut
24- 27 F4.2 --- FUVJSF Fraction of UVJ-SF galaxies, obtained
using as reference the number of cluster
members with M*>1010M☉
29- 32 F4.2 --- e_FUVJSF Error on FUVJSF
34- 37 F4.2 --- FMFIR ? Fraction of M-FIR galaxies, obtained
using as reference the number of cluster
members with M*>1010M☉
39- 42 F4.2 --- e_FMFIR ? Error on FMFIR
44- 48 F5.2 [Msun] MUVJSF Stellar mass of the UVJ-SF sample
50- 53 F4.2 [Msun] E_MUVJSF Upper error on MUVJSF (84th quantile)
55- 58 F4.2 [Msun] e_MUVJSF Lower error on MUVJSF (16th quantile)
60- 64 F5.2 [Msun] MMFIR ? Stellar mass of the M-FIR sample
66- 70 F5.2 [Msun/yr] SFRUVJSF Total SFR for the UVJ-SF sample obtained
as the addition of the SFRTIR and the
SFRUV when the former is available, and
the SFRUVcorr in the rest of the
cases (1)
72- 75 F4.2 [Msun/yr] E_SFRUVJSF Upper error on SFRUVJSF (84th quantile)
77- 80 F4.2 [Msun/yr] e_SFRUVJSF Lower error on SFRUVJSF (16th quantile)
82- 85 F4.2 [Msun/yr] SFRMFIR ? Total SFR for the M-FIR sample obtained
as the addition of the SFRTIR and the
SFRUV (1)
87- 92 F6.2 [yr-1] sSFRUVJSF Specific star formation rate for the
UVJ-SF sample (2)
94- 97 F4.2 [yr-1] E_sSFRUVJSF Upper error on sSFRUVJSF (84th quantile)
99-102 F4.2 [yr-1] e_sSFRUVJSF Lower error on sSFRUVJSF (16th quantile)
104-108 F5.2 [yr-1] sSFRMFIR ? Specific star formation rate for the
M-FIR sample (2)
--------------------------------------------------------------------------------
Note (1): SFRTIR is defined as SFRTIR=1.8x10-10LTIR/L☉ in M☉/yr,
where LTIR is the integrated total IR luminosity. And SFRUV is defined
as SFRUV=5.9x10-10L2800/L☉ in M☉/yr, where L2800 is the
rest-frame monochromatic luminosity at 2800Å (uncorrected for
extinction).
For those galaxies not detected by MIPS or Herschel, we compute SFRTOT
by correcting the UV luminosities for dust attenuation (AUV) following
the expression: SFRTOT=SFRUVcorr=SFRUVx100.4AUV
Note (2): The specific star formation rate is defined as the ratio between the
SFR and the stellar mass of a galaxy
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat table7.dat table8.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- ID Cluster ID
10- 12 I3 --- Membcut Number of cluster members with a detection
at a level >3σ in IRAC 4.5um and
M*>1010M☉
14- 17 I4 --- Memb Number of cluster members without the
M* cut
19- 21 I3 --- UVJSF Number of galaxies selected as
star-forming using the UVJ diagram and/or
detected in the MIR and/or FIR
(M>1010M☉), what we call the
UVJ-SF sample
23- 25 I3 --- MFIRcut Cluster members with M*>1010M☉
detected in the MIR and/or FIR with
SFRTIR>10M☉/yr what we call MFIR
sample
27- 29 I3 --- MFIR Total number of cluster members without
SFRTIR cut
31- 34 F4.2 --- FUVJSF ? Fraction of UVJ-SF galaxies, obtained
using as reference the number of cluster
members with M*>1010M☉
36- 39 F4.2 --- e_FUVJSF ? Error on FUVJSF
41- 44 F4.2 --- FMFIR ? Fraction of M-FIR galaxies, obtained
using as reference the number of cluster
members with M*>1010M☉
46- 49 F4.2 --- e_FMFIR ? Error on FMFIR
51- 55 F5.2 [Msun] MUVJSF ? Stellar mass of the UVJ-SF sample
57- 60 F4.2 [Msun] E_MUVJSF ? Upper error on MUVJSF (84th quantile)
62- 65 F4.2 [Msun] e_MUVJSF ? Lower error on MUVJSF (16th quantile)
67- 71 F5.2 [Msun] MMFIR ? Stellar mass of the M-FIR sample
73- 76 F4.2 [Msun] E_MMFIR ? Upper error on MMFIR (84th quantile)
78- 81 F4.2 [Msun] e_MMFIR ? Lower error on MMFIR (16th quantile)
83- 87 F5.2 [Msun/yr] SFRUVJSF ? Total SFR for the UVJ-SF sample obtained
as the addition of the SFRTIR and the
SFRUV when the former is available, and
the SFRUVcorr in the rest of the
cases (1)
89- 92 F4.2 [Msun/yr] E_SFRUVJSF ? Upper error on SFRUVJSF (84th quantile)
94- 97 F4.2 [Msun/yr] e_SFRUVJSF ? Lower error on SFRUVJSF (16th quantile)
99-102 F4.2 [Msun/yr] SFRMFIR ? Total SFR for the M-FIR sample obtained
as the addition of the SFRTIR and the
SFRUV (1)
104-107 F4.2 [Msun/yr] E_SFRMFIR ? Upper error on SFRMFIR (84th quantile)
109-112 F4.2 [Msun/yr] e_SFRMFIR ? Lower error on SFRMFIR (16th quantile)
114-119 F6.2 [yr-1] sSFRUVJSF ? Specific star formation rate for the
UVJ-SF sample (2)
121-124 F4.2 [yr-1] E_sSFRUVJSF ? Upper error on sSFRUVJSF (84th quantile)
126-129 F4.2 [yr-1] e_sSFRUVJSF ? Lower error on sSFRUVJSF (16th quantile)
131-135 F5.2 [yr-1] sSFRMFIR ? Specific star formation rate for the
M-FIR sample (2)
137-140 F4.2 [yr-1] E_sSFRMFIR ? Upper error on sSFRMFIR (84th quantile)
142-145 F4.2 [yr-1] e_sSFRMFIR ? Lower error on sSFRMFIR (16th quantile)
--------------------------------------------------------------------------------
Note (1): SFRTIR is defined as SFRTIR=1.8x10-10LTIR/L☉ in M☉/yr,
where LTIR is the integrated total IR luminosity. And SFRUV is defined
as SFRUV=5.9x10-10L2800/L☉ in M☉/yr, where L2800 is the
rest-frame monochromatic luminosity at 2800Å (uncorrected for
extinction).
For those galaxies not detected by MIPS or Herschel, we compute SFRTOT
by correcting the UV luminosities for dust attenuation (AUV) following
the expression: SFRTOT=SFRUVcorr=SFRUVx100.4AUV
Note (2): The specific star formation rate is defined as the ratio between the
SFR and the stellar mass of a galaxy
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 12-Sep-2022