J/ApJ/661/750 Photometry and spectroscopy of MS 1054-03 members (Tran+, 2007)
A Keck spectroscopic survey of MS 1054-03 (z = 0.83): forming the red sequence.
Tran K.-V.H., Franx M., Illingworth G.D., Van Dokkum P., Kelson D.D.,
Blakeslee J.P., Postman M.
<Astrophys. J., 661, 750-767 (2007)>
=2007ApJ...661..750T 2007ApJ...661..750T
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Redshifts ;
Equivalent widths
Keywords: galaxies: clusters: individual (MS 1054-03) -
galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: fundamental parameters
Abstract:
Using a magnitude-limited, spectroscopic survey of the X-ray-luminous
galaxy cluster MS 1054-03, we isolate 153 cluster galaxies and measure
MS 1054's redshift and velocity dispersion to be z=0.8307±0.0004
and σz=1156±82km/s. The absorption-line, post-starburst
("E+A"), and emission-line galaxies, respectively, make up 63%±7%,
15%±4%, and 23%±4% of the cluster population. With photometry from
HST ACS, we find that the absorption-line members define an
exceptionally tight red sequence over a span of ∼3.5mag in i775: their
intrinsic scatter in (V606-i775) color is only 0.048±0.008,
corresponding to a (U-B)z scatter of 0.041.
Description:
In 1998 May, a 5'x6' mosaic of the MS 1054-03 field was taken with
WFPC2 on HST. Six slightly overlapping pointings were taken in both
the F606W and F814W filters.
For most of our analysis, we use the photometry and morphological
information derived from imaging taken with HST ACS. A 2x2 overlapping
mosaic (5.8'x5.8') was taken in F775W and F850LP in 2002 December, and
the same pattern executed in F606W in 2004 January/February. A
detailed description of the ACS image reduction is presented in
Blakeslee et al. (2006, Cat. J/ApJ/644/30).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 114 145 MS 1054-03 Members
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See also:
J/ApJS/157/228 : Catalog of galaxy morphology in 4 clusters (Saintonge+ 2005)
J/ApJ/644/30 : HST Observations of 2 high-z clusters (Blakeslee+ 2006)
J/AJ/131/1891 : Photometric survey of MS 1054-03 (Foerster-Schreiber+ 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Type Member type: Absorption, Emission, Probable
Members, Post-starburst, No Measured [OII]
19 A1 --- --- [H]
20- 23 I4 --- HST [159/8001] Blakeslee et al. (2006, Cat.
J/ApJ/644/30) identification number (1)
24 A1 --- --- [/]
25- 28 I4 --- HST2 ? Second HST identification number
30- 35 F6.4 --- z Redshift
37 I1 --- q_z [1,3] Redshift quality, 3=best (2)
39 A1 --- --- [B]
40- 43 I4 --- Ident ? Identification number from unknown origin (1)
45- 49 F5.2 mag imag ? The i775 band AB magnitude (3)
51- 55 F5.3 mag V-i ? The (V-i775) AB color index (3)
57- 58 I2 --- MType ? Morphological type (4)
60- 61 A2 --- n_MType [99] in a merging system (5)
63- 68 F6.1 arcsec oRA Offset in Right Ascension (6)
70- 75 F6.1 arcsec oDE Offset in Declination (6)
77- 81 F5.1 0.1nm EW(OII) ? The O II Equivalent width (7)
83- 86 F4.1 0.1nm e_EW(OII) ? Error in OII (7)
88- 92 F5.1 0.1nm EW(Hd) ? Hδ equivalent width (7)
94- 97 F4.1 0.1nm e_EW(Hd) ? Error in Hd (7)
99-103 F5.1 0.1nm EW(Hg) ? Hγ equivalent width (7)
105-108 F4.1 0.1nm e_EW(Hg) ? Error in Hg (7)
110-112 I3 km/s sigma ? Internal velocity dispersion
114 A1 --- n_sigma [de] Note about sigma measurement (8)
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Note (1): Contrary to that indicating in the paper, HST numbers correspond
to Blakeslee et al. (2006, Cat. J/ApJ/644/30, [BHF2006]), and Ident
numbers are NOT from Blakeslee et al. (2006).
Note (2): In our analysis, we consider only members with a redshift quality
flag of 3. The typical redshift errors from the cross-correlation are
∼30km/s, and we find that the median error estimated from galaxies
observed in multiple masks is 50km/s. Candidate members with 2 or 1
are listed at the end of the table.
Note (3): ACS magnitudes and colors are measured within an effective radius
determined from fitting 2-D Sersic profiles. At z=0.83, imag and
(V-imag) closely correspond to rest-frame B and (U-B).
Note (4): As assigned by Postman et al. (2005ApJ...623..721P 2005ApJ...623..721P) using the ACS
imaging.
Note (5): 99 = a member that is also visually classified to be part of a
merging system (van Dokkum et al., 2000ApJ...541...95V 2000ApJ...541...95V).
Note (6): With respect to the brightest cluster galaxy (H4520).
Its J2000 coordinates are 10:57:00.0-03:37:36.2. Positive Δ(RA)
is west and positive Δ(Dec) is north.
Note (7): In units of Angstroms; the indices are determined using the same
bandpasses as Fisher et al. (1998, Cat. J/ApJ/498/195).
Note (8): Note as follows:
d = The internal velocity dispersion is measured directly
(Wuyts et al., 2004ApJ...605..677W 2004ApJ...605..677W) and has errors of ∼ 10-15%.
e = The internal velocity dispersion is measured using the method
and measurements described in Tran et al. (2003ApJ...590..238T 2003ApJ...590..238T)
and the errors, especially at L<L*, can easily be >20%.
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History:
*05-Oct-2007: From electronic version of the journal
*25-Oct-2012: Identification labels corrected
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 04-Oct-2007