J/ApJS/199/23 IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)
Infrared and ultraviolet star formation in brightest cluster galaxies in the
ACCEPT sample.
Hoffer A.S., Donahue M., Hicks A., Barthelemy R.S.
<Astrophys. J. Suppl. Ser., 199, 23 (2012)>
=2012ApJS..199...23H 2012ApJS..199...23H
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, infrared ;
Photometry, ultraviolet ; X-ray sources ; Cross identifications
Keywords: galaxies: elliptical and lenticular, cD
Abstract:
We present infrared (IR) and ultraviolet (UV) photometry for a sample
of brightest cluster galaxies (BCGs). The BCGs are from a
heterogeneous but uniformly characterized sample, the Archive of
Chandra Cluster Entropy Profile Tables (ACCEPT), of X-ray galaxy
clusters from the Chandra X-ray telescope archive with published gas
temperature, density, and entropy profiles. We use archival Galaxy
Evolution Explorer (GALEX), Spitzer Space Telescope, and Two Micron
All Sky Survey (2MASS) observations to assemble spectral energy
distributions (SEDs) and colors for BCGs. We establish a mean near-UV
(NUV) to 2MASS K color of 6.59±0.34 for quiescent BCGs. We use this
mean color to quantify the UV excess associated with star formation in
the active BCGs. We use both fits to a template of an evolved stellar
population and library of starburst models and mid-IR star formation
relations to estimate the obscured star formation rates (SFRs). We
present IR and UV photometry and estimated equivalent continuous SFRs
for a sample of BCGs.
Description:
The original galaxy cluster sample is from the Archive of Chandra
Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al.
2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used
the 2MASS archive and previous literature to determine the locations
of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the
GALEX object identifiers for each BCG detected and the Astronomical
Observing Request (AOR) numbers from the Spitzer archive observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 164 258 Brightest Cluster Galaxy identifications
table3.dat 72 243 Physical properties
table4.dat 86 243 Fluxes matched to UV aperture
table5.dat 132 243 Spitzer aperture flux
table6.dat 76 243 2MASS aperture flux
table7.dat 68 243 Star Formation Rates
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/ApJS/199/22 : UV to far-IR catalog of galaxies (Hernandez-Fernandez+, 2012)
J/MNRAS/403/683 : GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)
J/ApJS/182/12 : ICM entropy profiles (ACCEPT) (Cavagnolo+, 2009)
J/ApJ/704/1586 : BCGs with radio AGN (Sun, 2009)
J/ApJS/176/39 : IR survey of brightest cluster galaxies I. (Quillen+, 2008)
J/ApJ/686/966 : Spitzer-FLS catalog of clusters of galaxies (Muzzin+, 2008)
J/MNRAS/306/857 : ROSAT Brightest Cluster Sample. III. (Crawford+, 1999)
http://www.pa.msu.edu/astro/MC2/accept/ : ACCEPT home page
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster name
19 A1 --- f_Name [g] Flag on name (1)
21- 39 A19 --- GALEX First GALEX IAU name(s) (mostly HHMMSS.s+DDMMSS)
40 A1 --- f_GALEX Flag on GALEX (1)
42- 57 A16 --- GALEX2 Second GALEX IAU name(s) (HHMMSS.s+DDMMSS)
58 A1 --- f_GALEX2 Flag on GALEX2 (1)
60- 77 A18 --- 2MASX 2MASX identifier (mostly HHMMSSss+DDMMSSs)
79-115 A37 --- IRAC Spitzer/IRAC AOR number(s) (1)
117-164 A48 --- MIPS Spitzer/MIPS AOR number(s) (1)
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Note (1): Comments for the notes following an identifier are:
a = MIPS observation includes a 24 micron observation.
b = MIPS observation includes a 70 micron observation.
c = GALEX observation only includes FUV measurement.
d = GALEX observation only includes NUV measurement.
e = GALEX observation includes both NUV and FUV measurement.
f = MIPS observation includes a 160 micron observation.
g = Spitzer observations were made by Donahue as part of the
DDT program 488.
h = Due to an anomalous point source in the pbcd reduction, the images
needed to be reduced from the bcd frames.
i = GALEX observation was taken as a Guest Investigator for
Hicks et al. (2010ApJ...719.1844H 2010ApJ...719.1844H).
j = IRAC observation only has bands 1 and 3 on target.
k = IRAC observation only has bands 2 and 4 on target.
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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- 18 A18 --- Name Cluster name
19 A1 --- n_Name [l] Note on Abell 644 (1)
21- 26 F6.4 --- z [0.0031/0.89] ACCEPT database redshift
28- 33 F6.2 keV.cm2 Entr ACCEPT database central entropy (2)
35- 42 F8.2 keV.cm2 K100 ACCEPT database entropy profile (2)
44- 47 F4.2 --- alpha ACCEPT database best-fit power law index (2)
49- 52 F4.2 kpc/arcsec Scale Size scale (3)
54- 59 F6.2 arcsec IRrad Spitzer radius (4)
61- 64 F4.1 arcsec UVrad ? GALEX radius (5)
66- 72 F7.2 kpc Offset ? Centroid offset
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Note (1): The UV data for Abell 644 is taken from Hicks et al.
(2010ApJ...719.1844H 2010ApJ...719.1844H).
Note (2): Quantities defined in Cavagnolo et al. (2009, Cat. J/ApJS/182/12)
are from radially fit entropy profiles with a functional form
K(r)=K0+Kx(r/rx)α, where K0 is the central
entropy in excess above the power law fit, K100 is the entropy
profile normalization at 100h70-1kpc from the X-ray centroid,
and alpha is the best-fit power law index.
Note (3): The size scale is calculated as the angular distance size assuming
the standard cosmology in the paper.
Note (4): The IR radii are set at 14.3h70-1kpc in size and are used for
2MASS and IRAC aperture measurements except in the case where the
aperture is below 5". In this case the aperture is set to be 5"
to minimize large aperture corrections.
Note (5): The UV radius is set by the aperture photometry in the GALEX database
which most closely matches the GALEXView total flux measurement.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster name
20- 21 A2 --- R [ab ] in Hicks et al. sample (6)
23- 27 F5.2 mag NUV ? GALEX/NUV band magnitude
29- 34 F6.4 mag e_NUV ? Error in NUV (7)
36- 40 F5.2 mag FUV ? GALEX/FUV band magnitude
42- 47 F6.4 mag e_FUV ? Error in FUV (7)
49- 53 F5.2 mag Jmag ? 2MASS J band magnitude
55- 60 F6.4 mag e_Jmag ? Error in Jmag (7)
62- 66 F5.2 mag Hmag ? 2MASS H band magnitude
68- 73 F6.4 mag e_Hmag ? Error in Hmag (7)
75- 79 F5.2 mag Ksmag ? 2MASS Ks band magnitude
81- 86 F6.4 mag e_Ksmag ? Error in Ksmag (7)
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Note (6): Flag as follows:
a = BCGs are also in the Hicks et al. (2010ApJ...719.1844H 2010ApJ...719.1844H) sample.
b = BCG GALEX fluxes are taken from Hicks et al. (2010ApJ...719.1844H 2010ApJ...719.1844H).
Note (7): Fluxes reported with errors equal to 0 are 3σ upper limits.
For NUV upper limits, the 2MASS flux is matched with a 7" aperture
such that it is similar in size to the GALEX PSF.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster name
20 A1 --- S [e] IRAC flux remosaicked (8)
22- 28 F7.2 mJy S3.6 ? Spizter/IRAC 3.6 micron band flux density
30- 38 F9.5 mJy e_S3.6 ? Error in S3.6
40- 46 F7.2 mJy S4.5 ? Spizter/IRAC 4.5 micron band flux density
48- 52 F5.2 mJy e_S4.5 ? Error in S4.5
54- 59 F6.2 mJy S5.8 ? Spizter/IRAC 5.8 micron band flux density
61- 65 F5.2 mJy e_S5.8 ? Error in S5.8
67- 72 F6.2 mJy S8.0 ? Spizter/IRAC 8.0 micron band flux density
74- 78 F5.2 mJy e_S8.0 ? Error in S8.0
80 A1 --- f_S8.0 [f] Flag on S8.0 (9)
82- 88 F7.2 mJy S24 ? Spitzer/MIPS 24 micron band flux density
90 A1 --- f_S24 [bcf] Flag on S24 (9)
92- 97 F6.2 mJy e_S24 ? Error in S24
99-105 F7.2 mJy S70 ? Spitzer/MIPS 70 micron band flux density
107 A1 --- f_S70 [ad] Flag on S70 (9)
109-115 F7.2 mJy e_S70 ? Error in S70
117-123 F7.2 mJy S160 ? Spitzer/MIPS 160 micron band flux density
125 A1 --- f_S160 [ad] Flag on S160 (9)
127-132 F6.2 mJy e_S160 ? Error in S160
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Note (8):
e = IRAC flux measurements derived from a Basic Calibrated Data (BCD) image
that was remosaicked.
Note (9): Flag as follows:
a = Originally, aperture flux measurement indicated a detection. However,
24 micron flux measurement and visual inspection indicated
contamination in the aperture where flux is likely from an unrelated
source. The reported measurement is now an upper limit computed using
the point source estimate at 16".
b = Source not extended but has significant contamination. Point source
measurement at 35" radius is greater than 10% error margin.
c = Source not extended but has mild source contamination. Point source
measurement at 35" radius is within 10% error.
d = Flux measurement is a filtered detection.
f = Source is extended in the MIPS 24 micron image. 24 micron flux measured
within the aperture (see Table 3). Note an aperture radius of 35" was
used for NGC4636 because of significant point source contamination
outside of 35".
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster Name
20- 26 F7.2 mJy SJ ? 2MASS J band flux density
28- 33 F6.2 mJy e_SJ ? Error in SJ
35- 41 F7.2 mJy SH ? 2MASS H band flux density
43- 48 F6.2 mJy e_SH ? Error in SH
50- 56 F7.2 mJy SKs ? 2MASS Ks band flux density
58- 63 F6.2 mJy e_SKs ? Error in SKs
65- 70 F6.2 mJy SK24 ? The K24 band flux density (24um aperture
for K band)
72- 76 F5.2 mJy e_SK24 ? Error in SK24
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Cluster name
20- 24 F5.2 Msun/yr SFRUV ? Star formation rate from UV data (10)
26- 29 F4.2 Msun/yr e_SFRUV ? Error in SFRUV (11)
31- 36 F6.2 Msun/yr SFRIR ? Star formation rate from IR data (12)
38- 43 F6.2 Msun/yr SFR70 ? Star formation rate from 70 micron data (13)
45- 49 F5.2 Msun/yr e_SFR70 ? Error in SFR70 (11)
51- 56 F6.2 Msun/yr SFR24 ? Star formation rate from 24 micron data (13)
58- 62 F5.2 Msun/yr e_SFR24 ? Error in SFR24 (11)
64- 68 F5.2 10+10Msun Mass ? Stellar mass
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Note (10): UV SFR are calculated for all objects, including those in high
K0 systems. Upper limits are then calculated using the uncertainties
on the NUV, K, and inert BCG color. If a star formation rate is
consistent with a SFR of zero within 3σ, a 3σ upper limit
is reported.
Note (11): A star formation rate uncertainty of 0 identifies the quoted
rate as a 3σ upper limit.
Note (12): The IR SFR is estimated by a fit to the Groves et al.
(2008ApJS..176..438G 2008ApJS..176..438G) models.
Note (13): The 24 and 70 micron SFRs are estimated from empirical
relationships reported in Calzetti et al. (2010ApJ...714.1256C 2010ApJ...714.1256C) and
the uncertainties are calculated using the 24 and 70 micron flux
uncertainties, respectively.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 23-Mar-2012