J/ApJ/761/114 Multi-wavelength study of clusters of galaxies. II. (Atlee+, 2012)
A multi-wavelength study of low-redshift clusters of galaxies.
II. Environmental impact on galaxy growth.
Atlee D.W., Martini P.
<Astrophys. J., 761, 114 (2012)>
=2012ApJ...761..114A 2012ApJ...761..114A
ADC_Keywords: Clusters, galaxy ; Photometry, infrared ; Galaxies, IR ; Redshifts
Keywords: galaxies: clusters: general; galaxies: evolution
galaxies: star formation; infrared: galaxies
Abstract:
Galaxy clusters provide powerful laboratories for the study of galaxy
evolution, particularly the origin of correlations of morphology and
star formation rate (SFR) with density. We construct visible to MIR
spectral energy distributions of galaxies in eight low-redshift
(z<0.3) clusters and use them to measure stellar masses and SFRs as a
function of environment. A partial correlation analysis indicates that
the SFRs of star-forming galaxies (SFGs) depend strongly on M* (>99%
confidence) with no dependence on R/R200 or projected local density
at fixed mass. A merged sample of galaxies from the five best measured
clusters shows ∝(R/R200)1.1±0.3 for galaxies with
R/R200≤0.4. A decline in the fraction of SFGs toward the cluster
center contributes most of this effect, but it is accompanied by a
reduction in for SFGs with R≤0.1R200. The increase in the
fraction of SFGs toward larger R/R200 and the isolation of SFGs with
reduced SFRs near the cluster center are consistent with the
truncation of star formation by ram-pressure stripping, as is the
tendency for more massive SFGs to have higher SFRs. We conclude that
stripping is more likely than slower processes to drive the properties
of SFGs with R<0.4R200 in clusters. We also find that galaxies near
the cluster center are more massive than galaxies farther out in the
cluster at ∼3.5σ, which suggests that dynamical relaxation
significantly impacts the distribution of cluster galaxies as the
clusters evolve.
Description:
In Paper I (Atlee et al., 2011, Cat. J/ApJ/729/22), we constructed
SEDs from multi-wavelength observations (visible-wavelength images
from the 2.5m du Pont telescope at Las Campanas observatory, MIR
images from the IRAC and MIPS instruments on the Spitzer Space
Telescope (between 2008 November and 2009 April), and X-ray images
extracted from the Chandra archive).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 28 6 Cluster sample (table added by CDS)
table1.dat 36 216 Spectroscopic completeness
table2.dat 85 942 Mid-IR completeness
table3.dat 94 488 Cluster member summary
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
J/ApJS/199/22 : UV-FIR photometry of galaxies (Hernandez-Fernandez+, 2012)
J/MNRAS/425/1215 : Multiwavelength survey of AGNs (Klesman+, 2012)
J/ApJ/729/22 : Paper I: SEDs of galaxy cluster members (Atlee+, 2011)
J/ApJ/713/970 : Low-resolution SED templates for galaxies (Assef+, 2010)
J/A+A/486/9 : Redshifts in z∼0.25 clusters (Verdugo+, 2008)
J/A+A/477/55 : ACO 1825 and AC 114 EROs photometry (Hempel+, 2008)
J/ApJ/664/761 : BVRI photometry of AGNs in clusters (Martini+, 2007)
J/MNRAS/379/867 : BCG C4 cluster catalog (Von Der Linden+, 2007)
J/ApJS/122/51 : 10 rich galaxy clusters spectroscopic cat. (Dressler+ 1999)
J/ApJ/496/39 : Properties of poor groups of galaxies. I. (Zabludoff+ 1998)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Cluster identifier (as in table 1)
8- 13 F6.4 --- z Cluster redshift from Paper I (J/ApJ/729/22)
15- 28 A14 --- SName Cluster identifier understandable by SIMBAD
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Unique cluster identifier (a1689, a2104,
a3125, a3128, ac114 or ms1008)
8- 12 F5.2 mag Imag [14.3/23.2] Median I band Vega magnitude for
galaxies in this magnitude bin
14- 18 F5.3 --- Rad [0.03/0.4] Median radius of galaxies in this
bin scaled to virial radius
20- 27 E8.2 --- Compl [0/41] Fraction of galaxies in bin with
spectroscopic redshifts
29- 36 E8.2 --- e_Compl [0/3170] Uncertainty in Compl
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Unique cluster identifier (as in table 1)
8- 11 F4.2 --- Rad [0/0.4] Median radius of galaxies in this bin
scaled to virial radius
13- 20 E8.2 Jy F8 [0/2]?=0 Mean IRAC 8um flux density (1)
22- 30 E9.2 --- C8 [0/1]?=-1 Fraction of cluster members where F8
can be detected (2)
32- 39 E8.2 --- E_C8 [0/1] Upper uncertainty in C8
41- 48 E8.2 --- e_C8 [0/1] Lower uncertainty in C8
50- 57 E8.2 Jy F24 [0/1]?=0 Mean MIPS 24um flux density (1)
59- 67 E9.2 --- C24 [0/1]?=-1 Fraction of cluster members where F24
can be detected (2)
69- 76 E8.2 --- E_C24 [0/1.5] Upper uncertainty in C24
78- 85 E8.2 --- e_C24 [0/1.5] Lower uncertainty in C24
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Note (1): Of model SEDs that contribute to this bin.
Note (2): Fluxes are calculated by integrating model SEDs with random
combinations of the Assef et al. 2010 (J/ApJ/713/970) star forming
templates across the published instrument response functions. If the
SFR inferred from the rest frame luminosities in the model SEDs are
outside the range 10-2<SFR/(1M☉/yr)<102, the associated
fluxes are not included in the sample. Because Assef et al. 2010
templates are not constructed to have identical SFRs in the 8um and
24um channels, this sometimes means that an SED with a valid SFR in
one channel will not appear in another. When a flux bin is occupied in
one channel and not in another, the empty channel has fν=0 and
Cλ=-1. This is the case for the first flux bin in AC114.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Cluster name
7 A1 --- --- [-]
8- 10 I03 --- Gal Galaxy name (1)
12- 13 I2 h RAh Hour of Right Ascension (J2000) (2)
15- 16 I2 min RAm Minute of Right Ascension (J2000) (2)
18- 22 F5.2 s RAs Second of Right Ascension (J2000) (2)
24 A1 --- DE- [-] Sign of the Declination (J2000) (2)
25- 26 I2 deg DEd Degree of Declination (J2000) (2)
28- 29 I2 arcmin DEm Arcminute of Declination (J2000) (2)
31- 34 F4.1 arcsec DEs Arcsecond of Declination (J2000) (2)
36- 40 F5.3 --- z [0.05/0.4] Redshift (3)
42 A1 --- l_M* Limit flag on M*
43- 50 E8.2 10+10Msun M* [0.006/365] Stellar mass (4)
52- 59 E8.2 10+10Msun e_M* ? Statistical error in M*
61- 68 E8.2 10+10Msun s_M* [0.08/29.4]? Systematic error in M*
70 A1 --- l_SFR Limit flag on SFR (5)
71- 78 E8.2 Msun/yr SFR [0.01/777000]? Star formation rate (6)
80- 87 E8.2 Msun/yr e_SFR [0.03/3.5]? Statistical error in SFR
89- 94 F6.2 --- delta [0.2/999] Substructure parameter δ (7)
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Note (1): Object name is identical to the name given in Table 2 of Atlee et
al. 2011 (Paper I, J/ApJ/729/22; <[AMA2011] {Name} NNN> in Simbad).
Note (2): As determined from the R band images of identified cluster members.
Note (3): As determined by Martini et al. (2006ApJ...644..116M 2006ApJ...644..116M; 2007, Cat.
J/ApJ/664/761) where available, or from the literature otherwise.
Note (4): Derived using mass-to-light ratios appropriate for each galaxy's
color and assuming a scaled Salpeter IMF with Bruzual & Charlot
population synthesis model (Bell & de Jong 2001ApJ...550..212B 2001ApJ...550..212B, T4).
Note (5): Upper limits are quoted at 3σ in the more sensitive of the
8um and 24um bands.
Note (6): Either from the 8um luminosity, the 24um luminosity or by taking
the geometric mean of the two, depending on the measurements available.
Note (7): Of (Dressler & Schectman 1988AJ.....95..985D 1988AJ.....95..985D), where
δ=(11/σ2)*[(vlocal-v)2+(σlocal-σ)2],
where the local average velocities (v) and velocity dispersions
(σ) are calculated over the 10 nearest neighbors of each galaxy.
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History:
From electronic version of the journal
References:
Atlee et al. Paper I. 2011ApJ...729...22A 2011ApJ...729...22A Cat. J/ApJ/729/22
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 08-Aug-2014