J/ApJS/247/43 WWFI g'-band obs. of bright cluster galaxies (Kluge+, 2020)
Structure of brightest cluster galaxies and intracluster light.
Kluge M., Neureiter B., Riffeser A., Bender R., Goessl C., Hopp U.,
Schmidt M., Ries C., Brosch N.
<Astrophys. J. Suppl. Ser., 247, 43 (2020)>
=2020ApJS..247...43K 2020ApJS..247...43K
ADC_Keywords: Clusters, galaxy; Galaxies, photometry; Optical; Morphology;
Redshifts
Keywords: cD galaxies; Galaxy formation; Galaxy stellar halos;
Surface photometry; Scaling relations; Brightest cluster galaxies
Abstract:
Observations of 170 local (z≲0.08) galaxy clusters in the northern
hemisphere have been obtained with the Wendelstein Telescope Wide
Field Imager (WWFI). We correct for systematic effects such as
point-spread function broadening, foreground star contamination,
relative bias offsets, and charge persistence. Background
inhomogeneities induced by scattered light are reduced down to
ΔSB>31 g' mag/arcsec2 by large dithering and subtraction of
night-sky flats. Residual background inhomogeneities brighter than
SBσ<27.6 g' mag/arcsec2 caused by galactic cirrus are
detected in front of 23% of the clusters. However, the large field of
view allows discrimination between accretion signatures and galactic
cirrus. We detect accretion signatures in the form of tidal streams in
22%, shells in 9.4%, and multiple nuclei in 47% of the brightest
cluster galaxies (BCGs) and find two BCGs in 7% of the clusters. We
measure semimajor-axis surface brightness profiles of the BCGs and
their surrounding intracluster light (ICL) down to a limiting surface
brightness of SB=30 g' mag/arcsec2. The spatial resolution in the
inner regions is increased by combining the WWFI light profiles with
those that we measured from archival Hubble Space Telescope images or
deconvolved WWFI images. We find that 71% of the BCG+ICL systems have
surface brightness (SB) profiles that are well described by a single
Sersic function, whereas 29% require a double Sersic function to
obtain a good fit. We find that BCGs have scaling relations that
differ markedly from those of normal ellipticals, likely due to their
indistinguishable embedding in the ICL.
Description:
The observations have been carried out with the 2m Fraunhofer
telescope at the Wendelstein Observatory. It is located in the
Bavarian Alps, 70km southeast from Munich, Germany. We have utilized
the Wendelstein Wide Field Imager (WWFI) for our survey as its first
light instrument. We have chosen the g' band for all observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 78 170 Brightest cluster galaxy (BCG) sample
table4.dat 170 170 *Structural parameters of the BCG
and their surrounding intracluster light (ICL)
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Note on table4.dat: All parameters are corrected for PSF broadening, dust
extinction, cosmic dimming and are K-corrected.
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See also:
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
J/ApJ/440/28 : Brightest Cluster Galaxies velocities (Postman+ 1995)
J/AJ/130/873 : BQS objects in the SDSS DR3 area (Jester+, 2005)
J/ApJ/664/226 : Nuker law parameters of early-type galaxies (Lauer+, 2007)
J/MNRAS/379/867 : BCG C4 cluster catalog (von der Linden+, 2007)
J/ApJS/182/216 : Surface photometry of Virgo ellipticals (Kormendy+, 2009)
J/ApJS/195/15 : Luminosity profiles of BCGs (Donzelli+, 2011)
J/ApJ/765/28 : CFHTLS galaxies with faint tidal features (Atkinson+, 2013)
J/MNRAS/442/3544 : Kinematic tracers in Umbrella galaxy (Foster+, 2014)
J/ApJ/797/82 : Brightest cluster galaxies in Abell clusters (Lauer+, 2014)
J/A+A/581/A10 : VEGAS: A VST Early-type GAlaxy Survey (Capaccioli+, 2015)
J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)
J/A+A/588/A77 : NGC 3923 MegaCam image (Bilek+, 2016)
J/A+A/601/A86 : PSF models fits maps (Karabal+, 2017)
J/A+A/620/A111 : Confirmed PN in M87 outer regions (Longobardi+, 2018)
J/A+A/623/A1 : Fornax Deep Survey with VST. V. Isophote fit (Iodice+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Cluster Cluster name (1)
7- 30 A24 --- BCG Brightest galaxy name in cluster
32- 33 I2 h RAh Hour of right ascension (J2000)
35- 36 I2 min RAm Minute of right ascension (J2000)
38- 41 F4.1 s RAs Second of right ascension (J2000)
43 A1 --- DE- Sign of declination (J2000)
44- 45 I2 deg DEd Degree of declination (J2000)
47- 48 I2 arcmin DEm Arcminute of declination (J2000)
50- 51 I2 arcsec DEs Arcsecond of declination (J2000)
53- 60 F8.6 --- z [0.016/0.16] Redshift
62- 66 F5.3 kpc/arcsec Scale [0.3/2.7] Angular scale
68- 72 A5 --- Sel L14 selection (2)
74- 78 A5 --- HST Whether HST images were used to increase
the spatial resolution of the inner light
profiles
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Note (1): Cluster names beginning with "AWM," "L," and "MKW" are taken from
the Albert+ (1977ApJ...211..309A 1977ApJ...211..309A), Von Der Linden+ (2007, J/MNRAS/379/867 ;
<SDSS-C4-DR3 NNNN> in Simbad), and Morgan & Lesh (1965ApJ...142.1364M 1965ApJ...142.1364M)
catalogs, respectively.
Note (2): Comparison to the brightest cluster galaxy (BCG) selection by
L14 (Lauer+ 2014, J/ApJ/797/82): the items stand for agreement ("check"),
our BCG choice is the second-ranked galaxy L14 (M2), or the cluster is
not present in L14 ("-") and our choice is neither the first- nor the
second-ranked galaxy in L14.
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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- 5 A5 --- Cluster Cluster name
7- 11 F5.2 --- n1 [1.2/77.2] Sersic index of inner
component (3)
13- 18 F6.2 --- e_n1 [0.09/112] Error in n1
20- 28 E9.3 kpc re1 [2.3/158300] Effective radius of
inner component (3)
30- 38 E9.3 kpc E_re1 [0.2/777800] Upper error in re1
40- 48 E9.3 kpc e_re1 [0.2/152400] Lower error in re1
50- 54 F5.2 mag/arcsec2 SBe1 [19.5/38.8] Effective g' band surface
brightness of inner component (3)
56- 60 F5.2 mag/arcsec2 e_SBe1 [0.04/14.3] Error in SBe1
62- 65 F4.2 --- n2 [0.1/8]? Sersic index of outer
component (3)
67- 71 F5.2 --- e_n2 [0.01/34.3]? Error in n2
73- 79 F7.2 kpc re2 [51/3980]? Effective radius of
outer component (3)
81- 89 E9.3 kpc E_re2 [0.9/170000000000]? Upper error in re2
91- 99 E9.3 kpc e_re2 [0.9/160000000000]? Lower error in re2
101-105 F5.2 mag/arcsec2 SBe2 [25/32.7]? Effective g' band surface
brightness of outer component (3)
107-111 F5.2 mag/arcsec2 e_SBe2 [0.04/19.7]? Error in SBe2
113-116 F4.2 --- f2 [0.2/2]? Light fraction in
outer component (4)
118-121 F4.2 --- e_f2 [0.01/0.3]? Error in f2
123-131 E9.3 kpc re [7/64590] Effective radius from
direct integration (5)
133-141 E9.3 kpc e_re [0.1/64340] Error in re
143-147 F5.2 mag/arcsec2 SBe [22/32.4] Effective surface brightness
from direct integration (5)
149-152 F4.2 mag/arcsec2 e_SBe [0.01/6] Error in SBe
154-159 F6.2 mag Mtot [-26.2/-21.6] Integrated brightness (5)
161-164 F4.2 mag e_Mtot [0/1.1] Error in Mtot
166-170 A5 --- Type Type(s) of accretion signature (6)
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Note (3): The parameters of the single Sersic fits (cf. Eq. 11:
SB(a)=SBe+c(n).[(a/ae)1/n-1] where ae is the effective radius)
or double Sersic fits (cf. Eq. 12:
SB(a)=-2.5log10(10-0.4SB1(a)+10-0.4SB2(a)). These errors
are calculated solely from the covariance matrices of the fits.
Note (4): The fraction of the integrated outer Sersic component compared to the
total galaxy light S2/(S1+S2) is calculated by integrating both
semi-major axis Sersic functions out to infinite radius. Both
components are assumed to have the same ellipticity profiles.
Note (5): The parameters from 2-D profile integration are corrected for
undetected ICL (see Sec. 5.4) and the errors are estimated from
that correction.
Note (6): Feature code as follows:
a = 2BCGs;
b = Shells;
c = Tidal Streams;
d = Multiple Nuclei.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Jun-2020