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J/ApJS/134/355 Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)
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The radio galaxy populations of nearby Northern Abell clusters
Miller N.A., Owen F.N.
<Astrophys. J. Suppl. Ser. 134, 355 (2001)>
=2001ApJS..134..355M
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ADC_Keywords: Clusters, galaxy ; Galaxies, radio ; Redshifts
Keywords: catalogs - galaxies: clusters: general -
galaxies: distances and redshifts - radio continuum: galaxies
Abstract:
We report on the use of the NRAO VLA Sky Survey (NVSS) to identify
radio galaxies in 18 nearby Abell clusters. The listings extend from
the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc),
which corresponds to 1.5 Abell radii and approximately 4 orders of
magnitude in galaxy density. To create a truly useful catalog, we have
collected optical spectra for nearly all of the galaxies lacking
public velocity measurements. Consequently, we are able to
discriminate between those radio galaxies seen in projection on the
cluster and those that are in actuality cluster members. The resulting
catalog consists of 329 cluster radio galaxies plus 138 galaxies
deemed foreground or background objects, and new velocity measurements
are reported for 273 of these radio galaxies. The motivation for the
catalog is the study of galaxy evolution in the cluster environment.
The radio luminosity function is a powerful tool in the identification
of active galaxies, as it is dominated by star-forming galaxies at
intermediate luminosities and active galactic nuclei (AGNs) at higher
luminosities. The flux limit of the NVSS allows us to identify AGNs
and star-forming galaxies down to star formation rates less than
1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the
NVSS, allows us to produce a catalog of considerable depth and
breadth. In addition to these data, we report detected infrared fluxes
and upper limits obtained from IRAS data. It is hoped that this
database will prove useful in a number of potential studies of the
effect of environment on galaxy evolution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 120 329 Cluster radio galaxy data, with absolute
quantities (tables 5 and 7 of the paper)
table6.dat 93 138 Non-cluster radio galaxy data
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See also:
http://www.cv.nrao.edu/NVSS/NVSS.html : the NVSS Home Page
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
Byte-by-byte Description of file: table5.dat table6.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ACO The Abell cluster designation
12- 13 I2 h RAh Right Ascension (J2000) (1)
15- 16 I2 min RAm Right Ascension (J2000) (1)
18- 21 F4.1 s RAs Right Ascension (J2000) (1)
22 A1 --- DE- Declination sign
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- 39 F6.4 --- z ? Heliocentric redshift
41 A1 --- f_z [afj] Flag on z (2)
43- 46 F4.1 mag Rmag The Gunn-Oke R-band magnitude from the POSS II
48 A1 --- f_Rmag [g] Indicates magnitude contaminated by star
50 A1 --- l_S1.4GHz Limit flag on S1.4GHz. Source contained within
larger extended radio emission
51- 57 F7.1 mJy S1.4GHz The NVSS radio flux density at 1.4GHz
59 A1 --- f_S1.4GHz [adehk] Flag on S1.4GHz (3)
61- 66 F6.3 Jy S60um ? The IRAS IR flux density at 60{mu}m
68 A1 --- f_S60um [bc] Flag on S60um (4)
70 A1 --- l_S100um Limit flag on S100um
71- 76 F6.3 Jy S100um ? The IR flux density at 100{mu}m
78 A1 --- f_S100um [bc] Flag on S100um (4)
80- 84 F5.2 --- QVal ? The FIR-radio correlation value (5)
86- 94 A9 --- Name The common name
95 A1 --- f_Name [i] Indicates part of galaxy pair or system (6)
98-102 F5.1 mag RMag ? Absolute computed Gunn-Oke aperture
R-band magnitude (table5 only)
104 A1 --- f_RMag [c] Indicates photometry corrupted by
presence of a star inside the aperture
106 A1 --- l_P1.4GHz Limit flag on P1.4GHzzz
107-110 F4.1 [W/Hz] P1.4GHz ? Log of the radio power at 1.4GHz (table5 only)
112 A1 --- f_P1.4GHz [d] Indicates a pair of galaxies (7)
114 A1 --- l_LFIR ? Limit flag on LFIR (table5 only)
115-118 F4.1 [solLum] LFIR ? Log of the far-IR luminosity (table5 only)
120 A1 --- f_LFIR [ab] Flag on LFIR (8)
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Note (1): Based on the optical position of the radio galaxy.
Note (2):
a = Redshift found in NED.
f = This is actually a pair of elliptical galaxies. The redshift presented
is the average of the NED values for the two individual galaxies,
0.0238 and 0.0222. Note also that the position and magnitude listed
in this table are for the galaxy pair taken together.
i = No redshift was obtained for these objects.
Note (3):
a = Overlay shows radio emission originates from background galaxy and not
the cluster member.
d = Extended radio source (see Table 2).
e = Resolved radio source. The flux was determined directly from the NVSS
image.
h = Source accepted from Sijbring list. Flux is the 21 cm Sijbring value
modified to 20 cm assuming a spectral index of 0.8.
k = This is a pair of galaxies. The NVSS peak and integral flux likely
represents contributions from each individual galaxy. The pair is
depicted in Fig. 1.
Note (4):
b = IRAS detection, with data from XSCANPI (see section 3.1).
c = Non-detection. The value quoted is a 3{sigma} upper limit based on
the local rms reported by XSCANPI.
Note (5): FIR-radio correlation value defined by Helou et al.,
1985ApJ...298L...7H, as
q = log{[FIR/(3.75x20^12^Hz)]/Sp(1.4GHz)},
where 3.75x20^12^Hz is the frequency at 80{mu}m.
Note (6): This galaxy is most likely to be the radio source on account of
either its optical spectrum or magnitude.
Note (7): The NVSS flux likely represents the combination of the two galaxies,
and the corresponding power is consequently an upper limit. The
galaxy pair may be seen in Figure 1.
Note (8):
a = Object IR flux densities derived using XSCANPI. The source was
detected at 60 or 100 {mu}m, but not both. The FIR luminosity is
estimated using a flux density in the nondetected band equal to
3 times the rms noise.
b = Object not detected at either 60 or 100{mu}m. Upper limit based
on 3 times the rms noise at 60{mu}m or 100{mu}m, as determined
from XSCANPI.
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History:
From electronic version of the journal; tables 5 and 7 merged in
a single table.
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(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 04-Sep-2001