J/ApJ/783/52 Redshifts in the field of A383 (Geller+, 2014)
A redshift survey of the strong-lensing cluster Abell 383.
Geller M.J., Hwang H.S., Diaferio A., Kurtz M.J., Coe D., Rines K.J.
<Astrophys. J., 783, 52 (2014)>
=2014ApJ...783...52G 2014ApJ...783...52G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, spectra ; Redshifts
Keywords: dark matter - galaxies: clusters: individual: Abell 3833 -
galaxies: distances and redshifts -
galaxies: kinematics and dynamics - gravitational lensing: weak
Abstract:
Abell 383 is a famous rich cluster (z=0.1887) imaged extensively as a
basis for intensive strong- and weak-lensing studies. Nonetheless,
there are few spectroscopic observations. We enable dynamical analyses
by measuring 2360 new redshifts for galaxies with rPetro≤20.5 and
within 50' of the Brightest Cluster Galaxy (BCG;
R.A.2000=42.014125°,decl.2000=-03.529228°). We apply the
caustic technique to identify 275 cluster members within 7h-1Mpc of
the hierarchical cluster center. The BCG lies within -11±110km/s and
21±56 h-1kpc of the hierarchical cluster center; the velocity
dispersion profile of the BCG appears to be an extension of the
velocity dispersion profile based on cluster members. The distribution
of cluster members on the sky corresponds impressively with the
weak-lensing contours of Okabe et al. especially when the impact of
foreground and background structure is included. The values of
R200=1.22±0.01h-1Mpc and
M200=(5.07±0.09)x1014h-1M☉ obtained by application of
the caustic technique agree well with recent completely independent
lensing measures. The caustic estimate extends direct measurement of
the cluster mass profile to a radius of ∼5h-1Mpc.
Description:
We used SDSS photometry from DR8 (Aihara et al., 2011ApJS..193...29A 2011ApJS..193...29A;
see DR9 in cat. V/139) to select objects for spectroscopic
observations.
We used Hectospec instrument mounted on the MMT 6.5m telescope at Fred
Lawrence Whipple Observatory for studying A383. Hectospec is a
multiobject fiber-fed spectrograph with 300 fibers deployable over a
circular field-of-view with a diameter of 1°. The spectra cover
the wavelength range 3500-9150Å at a resolution of 6.2Å FWHM.
Table1 lists the 2360 Hectospec redshifts for galaxies in the region
around A383.
Objects:
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RA (ICRS) DE Designation(s)
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02 48 06.9 -03 29 32 Abell 383 = 1RXS J024802.6-033206
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 76 2510 Redshifts in the field of A383
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See also:
V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012)
VII/259 : 6dF galaxy survey final redshift release (Jones+, 2009)
J/ApJ/776/91 : Galaxy spectroscopic redshifts in 2 clusters (Lemze+, 2013)
J/ApJ/767/15 : Hectospec Cluster Survey (HeCS) (Rines+, 2013)
J/ApJ/757/22 : Strong and weak lensing analysis of A2261 (Coe+, 2012)
J/ApJS/199/34 : Clusters of galaxies in SDSS-III (Wen+, 2012)
J/AJ/124/1266 : Redshift survey around Abell 2199 (Rines+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq [1/2510] Running sequence number of object
6- 24 A19 --- SDSS SDSS object identification (DR10; see DR9 in
cat. V/139)
26- 27 I2 h RAh Hour of Right Ascension (J2000)
29- 30 I2 min RAm Minute of Right Ascension (J2000)
32- 36 F5.2 s RAs Second of Right Ascension (J2000)
38 A1 --- DE- Sign of the Declination (J2000)
39- 40 I2 deg DEd Degree of Declination (J2000)
42- 43 I2 arcmin DEm Arcminute of Declination (J2000)
45- 49 F5.2 arcsec DEs Arcsecond of Declination (J2000)
51- 56 F6.3 mag rmag [12.2/21.7] The SDSS-DR10 r-band Petrosian
magnitude
58- 64 F7.5 --- z [3e-05/6.2] Redshift
66- 72 F7.5 --- e_z [1e-05/2.1] Uncertainty in z
74 I1 --- r_z [1/5] Source reference of z (1)
76 I1 --- Mm [0/1] Membership flag (0=A383 non-member,
1=A383 member)
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Note (1): Reference codes are defined as below:
1 = This study;
2 = SDSS DR10 (see DR9 in cat. V/139);
3 = Newman et al. (2013ApJ...765...25N 2013ApJ...765...25N);
4 = NASA/IPAC Extragalactic Database (NED; http://ned.ipac.caltech.edu/);
5 = Fred Lawrence Whipple Observatory (FLWO) 1.5-meter.
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 13-Apr-2016