Astronomical Data Center
ADC/CDS Standard Document for Catalog:
/journal_tables/AJ/122/1125/
The following is the "ReadMe" document that describes this ADC catalog. You can access the files described here in three ways:
J/AJ/122/1125 BVRI photometry in 3 high-z clusters (Postman+, 2001)
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A study of nine high-redshift clusters of galaxies.
IV. Photometry and spectra of clusters 1324+3011 and 1604+4321.
Postman M., Lubin L.M., Oke J.B.
<Astron. J. 122, 1125 (2001)>
=2001AJ....122.1125P
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ADC_Keywords: Clusters, galaxy ; Photometry, UBVRI ; Redshifts
Keywords: cosmology: observations - galaxies: clusters: general
Abstract:
New photometric and spectroscopic observations of galaxies in the
directions of three distant clusters are presented as part of our
ongoing high-redshift cluster survey. The clusters are Cl 1324+3011 at
z=0.76, Cl 1604+4304 at z=0.90, and Cl 1604+4321 at z=0.92. We
have spectroscopically confirmed cluster membership for 2040 galaxies
in each system and have also obtained spectra for over 280 field
galaxies spanning the range 0<z<2.5.
Objects:
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RA (2000) DE Designation(s)
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13 24 20.6 +30 13 02 GHO 132201+302842 = Cl J1324+3011 (z=0.76)
16 04 25.2 +43 04 52 GHO 160244+431254 = Cl J1604+4303 (z=0.90)
16 04 32 +43 21 18 GHO 160253+432924 = Cl J1604+4321 (z=0.92)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 109 161 Field Cl J1324+3011 photometric and spectroscopic data
table3.dat 109 116 Field Cl J1604+4304 photometric and spectroscopic data
table4.dat 109 163 Field Cl J1604+4321 photometric and spectroscopic data
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See also:
J/AJ/116/560 : Cl J0023+0423 and Cl J1604+4304 spectroscopy (Postman+ 1998)
J/AJ/116/584 : Cl J0023+0423 and Cl J1604+4304 morphology (Lubin+ 1998)
Byte-by-byte Description of file: table2.dat table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- [PLO2001] Keck object identification number (1)
6- 7 A2 --- f_[PLO2001] Flag on ID (2)
9- 13 F5.2 mag Bmag ? The apparent AB_B_ passband magnitude
15- 19 F5.2 mag Vmag ? The apparent AB_V_ passband magnitude
21- 25 F5.2 mag Rmag ? The apparent AB_R_ passband magnitude
27- 31 F5.2 mag Imag ? The apparent AB_I_ passband magnitude
33- 38 F6.4 --- z ?=9.000 The geocentric redshift
40 I1 --- q_z [0/4] Measure of the quality in z (3)
42- 46 F5.2 --- b ? Logarithmic slope of the broadband energy
distribution (in mag/[Hz], units of
ABmag per unit interval of log(nu))
48- 51 F4.1 Gyr tau ? Best fit e-folding timescale for a
constant-age (4.8Gyr at z=0.9) model
53 A1 --- f_tau [l] l: indicates acceptable fit is not
possible for tau<20Gyr
55- 57 A3 --- SpClass [ak+ ] Spectral classification (4)
59- 62 F4.1 Gyr Age ? Age of the best fit tau=0.6 model
64- 69 F6.1 0.1nm EW[OII] ? [OII] (3727{AA}) rest equivalent width
in Angstroms (5)
71- 76 F6.1 0.1nm EWHbeta ? H{beta} rest equivalent width
in Angstroms (5)
78- 83 F6.1 0.1nm EW[OIII] ? [OIII] (5007{AA}) rest equivalent width
in Angstroms (5)
85- 89 F5.2 --- Jl ? Modified lower jump parameter (6)
91- 95 F5.2 --- Ju ? Modified upper jump parameter (7)
97-101 F5.2 solMass/yr SFR ? The estimated star formation rate
103-108 F6.2 mag BMAG ? Absolute rest AB B-band magnitude
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Note (1): Identifications:
In table2.dat: [PLO2001] J1324+3011 NNNN, in Simbad
In table3.dat: [PLO2001] J1604+4304 NNNN, in Simbad
In table4.dat: [PLO2001] J1604+4321 NNNN, in Simbad
For table3.dat, two spectroscopically confirmed members of Cl 1604+4304
lie near the edge of our LRIS imager and, hence, only have photometric
information for the R-band. These two galaxies are not included in
Table 3 but their redshifts are 0.9040 and 0.9073.
Note (2): Note on galaxy:
* = Considered to be a member of the cluster;
** = the brightest cluster galaxy.
Note (3): Quality redshift:
0: no redshift
1: redshift possible
2: redshift probably correct
3: redshift almost certainly correct
4: redshift is certain
Note (4): Spectral classification:
a = Objects have spectra that are dominated by Balmer lines, lack any
G-band absorption, and have a Ca II K line strength that is no
more than 25% of the strength of the H + H{epsilon} line.
a+k = Objects have strong Balmer lines, a CaII K line that is
approximately 50% of the strength of the H + H{epsilon} line,
and a detectable G-band line.
k+a = Objects have a CaII K line that is equal in strength to
H + H{epsilon}, and have a G-band feature that is as strong as
H{gamma}, if H{gamma} is not filled with emission.
k = Objects have a CaII K line is stronger than H + H{epsilon},
have very strong 3835{AA} and G-band features, and exhibit
little or no H{gamma} absorption.
Note (5): Emission line equivalent widths are given as negative values and
positive values are used for absorption features.
Note (6): Defined as the difference of the average flux (expressed in AB
magnitudes) measured from 3400 to 3700{AA} and the defined continuum
at the central wavelength of this band (i.e. 3550{AA}).
Note (7): Defined as the difference of the average flux (expressed in AB
magnitudes) measured from 3750 to 3980{AA} and the defined continuum
at the central wavelength of this band (i.e. 3865{AA}).
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History:
From electronic version of the journal
References:
Oke et al., Paper I 1998AJ....116..549O
Postman et al., Paper II 1998AJ....116..560P, Cat. <J/AJ/116/560>
Lubin et al., Paper III 1998AJ....116..584L, Cat. <J/AJ/116/584>
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(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 14-Jan-2002
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