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J/ApJ/723/251    Keck/LRIS confirmation of Coma membership    (Chiboucas+, 2010)

Keck/LRIS spectroscopic confirmation of Coma cluster dwarf galaxy membership assignments. Chiboucas K., Tully R.B., Marzke R.O., Trentham N., Ferguson H.C., Hammer D., Carter D., Khosroshahi H. <Astrophys. J., 723, 251-266 (2010)> =2010ApJ...723..251C
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, HST ; Redshifts ; Spectroscopy ; Morphology Keywords: galaxies: clusters: individual (Coma) - galaxies: dwarf Abstract: Keck/LRIS multi-object spectroscopy has been carried out on 140 of some of the lowest and highest surface brightness faint (19<R<22) dwarf galaxy candidates in the core region of the Coma Cluster. These spectra are used to measure redshifts and establish membership for these faint dwarf populations. The primary goal of the low surface brightness sample is to test our ability to use morphological and surface brightness criteria to distinguish between Coma Cluster members and background galaxies using high resolution Hubble Space Telescope/Advanced Camera for Surveys images. Candidates were rated as expected members, uncertain, or expected background. From 93 spectra, 51 dwarf galaxy members and 20 background galaxies are identified. Our morphological membership estimation success rate is ∼100% for objects expected to be members and better than ∼90% for galaxies expected to be in the background. We confirm that low surface brightness is a very good indicator of cluster membership. High surface brightness galaxies are almost always background with confusion arising only from the cases of the rare compact elliptical (cE) galaxies. The more problematic cases occur at intermediate surface brightness. Many of these galaxies are given uncertain membership ratings, and these were found to be members about half of the time. In a sample of 47 high surface brightness, ultracompact dwarf candidates, 19 objects have redshifts which place them in the Coma Cluster, while another 6 have questionable redshift measurements but may also prove to be members. Description: We use the Keck LRIS low resolution imaging spectrometer in multi-object spectroscopy mode. A dichroic was used to split light at 5600Å between red and blue detectors. We observed four masks over two nights 2008 April 2 and 3 (resolution of ∼200km/s). This work is part of the Hubble Space Telescope/Advanced Camera for Surveys (HST/ACS) Coma Cluster Treasury Survey (Carter et al. 2008ApJS..176..424C), a two-passband imaging survey originally designed to cover 740arcmin2 in the Coma Cluster to a depth of IC∼26.6 for point sources and µe,I<26.0mag/arcsec2 for extended sources. Over 200arcmin2 have been completed. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 120 101 LRIS (membership test sample) redshift results
See also: VII/42 : GMP catalogue: galaxies in the Coma cluster (Godwin+ 1983) J/MNRAS/411/2439 : Coma Treasury Survey. Structural parameters (Hoyos+, 2011) J/MNRAS/404/1745 : Dwarf galaxies in Coma supercluster (Mahajan+, 2010) J/MNRAS/392/1265 : Faint galaxies in Coma cluster spectroscopy (Smith+, 2009) J/ApJS/175/462 : Spectroscopy of Coma early-type galaxies (Corsini+, 2008) J/ApJS/169/225 : Photometry in the Coma cluster (Eisenhardt+, 2007) J/A+A/451/1159 : BVRI imaging of the Coma cluster (Adami+, 2006) J/A+A/459/679 : RB photometry of LSBG in Coma (Adami+, 2006) J/ApJ/602/664 : Morphology of galaxies in Coma cluster (Gutierrez+, 2004) J/A+A/395/753 : Spectroscopy of Coma galaxies. II. (Wegner+, 2002) J/AJ/121/2331 : SDSS redshifts in the Coma cluster (Castander+, 2001) J/ApJS/137/279 : Spectroscopic Survey in Coma (Mobasher+, 2001) J/A+A/296/643 : LSB galaxies in Coma (Karachentsev+ 1995) J/A+AS/111/265 : Velocities in Coma cluster (Biviano+ 1995) J/ApJS/97/77 : Catalog of Coma Cluster Galaxies (Doi+ 1995) J/MNRAS/243/390 : Galaxy redshift survey in a Coma (Karachentsev+ 1990) : Coma Cluster Treasury Survey homepage Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- S Status (Mm, Bg, Un, PM, or PB) (1) 4- 10 I7 --- ID [10162/4042826] Identification number 11 A1 --- f_ID [he] Note on the observation (2) 13 I1 --- PT ?=x [1/5] Membership probability defined by N.T. on HST/ACS image (3) 15 I1 --- PF ?=x [1/4] Membership probability defined by H.F. on HST/ACS image (3) 17- 21 F5.2 mag Rmag [18.68/23.41]? R-band magnitude (4) 22 A1 --- f_Rmag [f] Blended photometry (2) 24- 28 F5.2 mag F814Wc ? HST/ACS F814W magnitude; corrected (5) 30- 34 F5.2 mag F814W ? HST/ACS F814W magnitude (5) 36- 39 F4.2 mag B-V ? (B-V) color index (3" aperture) (4) 40 A1 --- f_B-V [f] Blended photometry (2) 42- 46 F5.2 mag g-I ? (F475W-F814W) color index (2.25" aperture) 48- 52 F5.2 mag/arcsec2 mu0 ? Central surface brightness (µ0(R)) 54- 58 F5.2 mag/arcsec2 mue ? Mean effective surface brightness (<µe,F814W>) 60- 61 I2 h RAh [12/13] Hour of right ascension (J2000) 63- 64 I2 min RAm Minute of right ascension (J2000) 66- 70 F5.2 s RAs Second of right ascension (J2000) 72 A1 --- DE- [+] Sign of declination (J2000) 73- 74 I2 deg DEd [27/28] Degree of declination (J2000) 76- 77 I2 arcmin DEm Arcminute of declination (J2000) 79- 83 F5.2 arcsec DEs Arcsecond of declination (J2000) 85- 90 I6 km/s czA ? Absorption redshift 92- 94 I3 km/s e_czA ? czA uncertainty (6) 96- 99 F4.1 aW/m2/nm Rfx ? Relative flux (in 10-16erg/s/cm2/Å) 101-106 I6 km/s czE ? Emission redshift 107 A1 --- f_czE [g] redshift from red-side (2) 109-111 I3 km/s e_czE ? czE uncertainty 113-116 F4.1 --- S/N [3.7/61.1]? Signal to noise ratio per Angstrom around 5000Å 118-120 A3 --- MType Morphological type
Note (1): Membership status as follows: Mm = Member Bg = Background Un = Uncertain PM = Possible member (failed) PB = Possible background (failed) Note (2): Flag as follows: e = Object was observed in a separate run in 2009. f = Photometry is for two blended components including the UCD target and another source centered 0.9 arcsec west of it. g = Redshift measurement from red-side data. h = Object was observed in two masks. Note (3): Membership probability classes of the authors (N.Trenton and H.Ferguson) as follows: 1 = expected member 2 = probable member 3 = possible member 4 = expected background 5 = the galaxy was an extra object that landed in the slit x = no membership probability assigned See section 2.1.1 for further explanations. Note (4): BVR photometry from catalog of Adami et al. (2006, Cat. J/A+A/451/1159). Note (5): F814W photometry comes from SExtractor measurements from our ACS data (Hammer et al. 2010ApJS..191..143H). Note (6): Errors include contributions from the cross-correlation measurement uncertainty and from the uncertainties in the sky line wavelength calibration shift.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 13-Jul-2012
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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