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J/AJ/129/31       A deep radio survey of Abell 2125. II            (Owen+, 2005)

A deep radio survey of Abell 2125. II. Accelerated galaxy evolution during a cluster-cluster merger. Owen F.N., Ledlow M.J., Keel W.C., Wang Q.D., Morrison G.E. <Astron. J., 129, 31-52 (2005)> =2005AJ....129...31O
ADC_Keywords: Clusters, galaxy ; Photometry ; Radio sources Keywords: cosmology: observations - galaxies: clusters: individual (Abell 2125) - galaxies: elliptical and lenticular, cD - galaxies: evolution - galaxies: starburst - infrared: galaxies Abstract: Using our extensive radio, optical, near-IR, and X-ray imaging and spectroscopy, we consider the reason for the unusually large number of radio-detected galaxies, mostly found outside the cluster core, in Abell 2125 (z=0.2465, richness class 4). With 20cm VLA data, we detect continuum emission from 90 cluster members. The multiwavelength properties of these galaxies suggest that most of the radio emission is due to an enhanced star formation rate. The recent dynamical study of Miller et al. (2004, Cat. J/ApJ/613/841) suggests that A2125 is undergoing a major cluster-cluster merger, with our view within 30° of the merger axis and within 0.2Gyr of core passage. The combination of projection effects and the physical processes at work during this special time in the cluster's evolution seem likely to be responsible for the unusual level of activity we see in the cluster. We argue that tidal effects on individual cluster members, often far from the cluster core, are responsible for the increased star formation. Our results are consistent with the idea that disk galaxies during this phase of a cluster's evolution undergo rapid evolution through a burst of star formation on their way to becoming S0 galaxies. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 87 90 A2125 member radio sources table2.dat 66 90 A2125 Gunn-Oke magnitudes table4.dat 49 90 A2125 member physical parameters table8.dat 34 90 A2125 star-formation index
See also: J/AJ/129/26 : A deep radio survey of Abell 2125. I (Owen+, 2005) J/ApJ/613/841 : Redshifts in A2125 (Miller+, 2004) J/AJ/118/625 : Radio sources in Abell 2125 and 2645 (Dwarakanath+, 1999) J/ApJ/611/821 : X-raying A2125 (Wang+, 2004) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Name Source name (G1) (1) 7- 8 I2 h RAh Hour of Right Ascension (J2000) 10- 11 I2 min RAm Minute of Right Ascension (J2000) 13- 17 F5.2 s RAs Second of Right Ascension (J2000) 19- 22 F4.2 s e_RAs Estimated error in RAs 24- 25 I2 deg DEd Degree of Declination (J2000) 27- 28 I2 arcmin DEm Arcminute of Declination (J2000) 30- 33 F4.1 arcsec DEs Arcsecond of Declination (J2000) 35- 37 F3.1 arcsec e_DEs Estimated error in DEs 39- 42 F4.1 Mpc Dist Distance from the nominal cluster center (2) 44- 50 F7.1 uJy Sp20cm Uncorrected peak flux density in units of µJy/beam size 52- 58 F7.1 uJy S20cm Corrected total flux density 60- 64 F5.0 uJy e_S20cm Estimated error in S20cm 66 A1 --- l_Size [<] Limit flag on Size 67- 70 F4.1 arcsec Size Best fit size, major axis (3) 71 A1 --- --- [x] 72- 74 F3.1 arcsec Size1 ? Best fit size, minor axis (3) 76- 78 I3 arcsec PA ? Best fit size, position angle (3) 80- 85 F6.4 --- z Redshift 86 A1 --- n_z [e] Indicates emission lines were present in the spectrum (Miller et al. 2004, Cat. J/ApJ/613/841)
Note (1): For members identified with radio emission detected at >5σ above the noise. Note (2): Where the center is RA=15:41:15.00 and DE=66:16:00.0. Note (3): If the source is resolved and fitted with a two dimensional Gaussian, we give the deconvolved major axis size (FWHM), the minor axis size and the position angle. If only a size is given, this value has been estimated from the image by hand.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Name Source name (G1) 7- 11 F5.2 mag Umag Gunn-Oke aperture U band AB magnitude 13- 17 F5.2 mag Bmag Gunn-Oke aperture B band AB magnitude 19- 23 F5.2 mag Vmag Gunn-Oke aperture V band AB magnitude 25- 29 F5.2 mag Rmag Gunn-Oke aperture R band AB magnitude 31- 35 F5.2 mag Imag Gunn-Oke aperture I band AB magnitude 37- 41 F5.2 mag 8010mag Gunn-Oke aperture 8010Å band AB magnitude 43- 47 F5.2 mag 9170mag Gunn-Oke aperture 9170Å band AB magnitude 49- 53 F5.2 mag Jmag ?=-9.00 Gunn-Oke aperture J band AB magnitude 55- 59 F5.2 mag Hmag ?=-9.00 Gunn-Oke aperture H band AB magnitude 61- 65 F5.2 mag Kmag ?=-9.00 Gunn-Oke aperture K band AB magnitude
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Name Source name (G1) 7 A1 --- l_size Limit flag on size 8- 12 F5.1 kpc size Largest linear size 14- 18 F5.2 [W/Hz] logL20 Log of the absolute 20cm luminosity 20- 23 F4.2 Mpc pDist Projected distance from cluster center 25- 29 F5.1 mag RMAG Absolute rest frame R band magnitude 31 I1 --- sp The hyperz spectral type (1) 33- 36 F4.1 Gyr Age The hyperz age (1) 38- 40 F3.1 mag AV The hyperz V band extinction (1) 42- 47 F6.4 --- z Redshift 48 A1 --- n_z [e] Indicates emission lines were present in the spectrum (Miller et al. 2004, Cat. J/ApJ/613/841)
Note (1): Hyperz is a public photometric redshift code (Bolzonella, Miralles & Pello, 2000A&A...363..476B).
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Name Source name (G1) 7- 9 F3.1 --- L20cm 20cm luminosity property "star-formation index" score 11- 13 F3.1 --- sAlign Align property "star-formation index" score 15- 17 F3.1 --- sMag Magnitude property "star-formation index" score 19- 21 F3.1 --- sEmis Emission property "star-formation index" score 23- 25 F3.1 --- sAge Age property "star-formation index" score 27- 29 F3.1 --- sDust Dust property "star-formation index" score 31- 33 F3.1 --- sTotal Total "star-formation index" score
Global Notes: Note (G1): The first two digits are the facet number and the last three a sequence number.
History: * 06-Jul-2005: From electronic version of the journal * 10-Jul-2007: inconsistencies between tables 2 and 4: -- table2, record#18: name changed from 18071 to 18701 -- table4, record#19: z changed to 0.2558 (Miller 2004ApJ...613..841M) -- table4, record#37: z changed to 0.2430 (Miller 2004ApJ...613..841M) -- table4, record#53: z changed to 0.2560 (Miller 2004ApJ...613..841M) References: Owen et al., Paper I 2005AJ....129...26O, Cat. J/AJ/129/26
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 06-Jul-2005
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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