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Titolo:
A photometric and spectroscopic study of dwarf and giant galaxies in the Coma Cluster. II. Spectroscopic observations

Autore:

Mobasher, B; Bridges, TJ; Carter, D; Poggianti, BM; Komiyama, Y; Kashikawa, N; Doi, M; Iye, M; Okamura, S; Sekiguchi, M; Shimasaku, K; Yagi, M; Yasuda, N;

Indirizzi:: Space Telescope Sci Inst, Baltimore, MD 21218 USA Space Telescope Sci Inst Baltimore MD USA 21218 , Baltimore, MD 21218 USA European Space Agcy, Dept Space Sci, F-75738 Paris 15, France European Space Agcy Paris France 15 Space Sci, F-75738 Paris 15, France Anglo Australian Observ, Epping, NSW 2121, Australia Anglo Australian Observ Epping NSW Australia 2121 ng, NSW 2121, Australia John Moores Univ, Wirral CH41 1LD, Merseyside, England John Moores Univ Wirral Merseyside England CH41 1LD , Merseyside, England Osserv Astron Padova, I-35122 Padua, Italy Osserv Astron Padova Padua Italy I-35122 on Padova, I-35122 Padua, Italy Subaru Telescope, Hilo, HI 96720 USA Subaru Telescope Hilo HI USA 96720Subaru Telescope, Hilo, HI 96720 USA Natl Astron Observ, Tokyo 1818588, Japan Natl Astron Observ Tokyo Japan 1818588 tron Observ, Tokyo 1818588, Japan Univ Tokyo, Inst Astron, Sch Sci, Mitaka, Tokyo 1810015, Japan Univ TokyoMitaka Tokyo Japan 1810015 h Sci, Mitaka, Tokyo 1810015, Japan Univ Tokyo, Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan Univ Tokyo Tokyo Japan 1130033 Ctr Early Universe, Tokyo 1130033, Japan Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan Univ Tokyo Tokyo Japan 1130033 t Astron, Bunkyo Ku, Tokyo 1130033, Japan Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan Univ Tokyo Chiba Japan 2778582 , Inst Cosm Ray Res, Chiba 2778582, Japan
Titolo Testata:: ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
fascicolo: 2, volume: 137, anno: 2001,
pagine: 279 - 296
SICI:: 0067-0049(200112)137:2<279:APASSO>2.0.ZU;2-2
Fonte:: ISI
Lingua:: ENG
Soggetto:: STAR-FORMATION; DYNAMICS;
Keywords:: galaxies : clusters : general; galaxies : clusters : individual (Coma); galaxies : distances and redshifts; galaxies : kinematics and dynamics;
Tipo documento:: Article
Natura:: Periodico
Settore Disciplinare:: Physical, Chemical & Earth Sciences
Citazioni:: 15
Recensione:
Indirizzi per estratti:: Indirizzo: Mobasher, B Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA Space Telescope Sci Inst 3700 San Martin Dr Baltimore MD USA 21218



Citazione:: B. Mobasher et al., "A photometric and spectroscopic study of dwarf and giant galaxies in the Coma Cluster. II. Spectroscopic observations", ASTROPH J S, 137(2), 2001, pp. 279-296

Abstract

This is the second paper in a series studying the photometric and spectroscopic properties of galaxies of different luminosities in the Coma Cluster. We present the sample selection, spectroscopic observations, and completeness functions. To study the spectral properties of galaxies as a function of their local environment, two fields were selected for spectroscopic observations to cover both the core (Coma 1) and outskirts (i.e., southwest of the core and centered on NGC 4839; Coma 3) of the cluster. To maximize the efficiency of spectroscopic observations, two subsamples were defined, consisting of "bright" and "faint" galaxies, both drawn from magnitude-limited parent samples. Medium-resolution spectroscopy (6-9 Angstrom) was then carried out for a total of 490 galaxies in both fields (302 in Coma 1 and 188 inComa 3), using the WYFFOS multifiber spectrograph on the William Herschel Telescope. The galaxies cover a range of 12<R<20, corresponding to -23<M-R<-15 (H-0=65 km s(-1) Mpc(-1)). The redshifts for these galaxies are measured with an accuracy of 75 km s(-1). The spectral line strengths and equivalent widths are also measured for the same galaxies and analyzed in the next paper of this series. A total of 189 (Coma 1) and 90 (Coma 3) galaxies are identified as members of the Coma Cluster. An analysis of the colors show that only two members of the Coma Cluster in our sample have B-R>2. The completeness functions for our sample are calculated. These show that the bright sample is 65% complete at R<17 mag, becoming increasingly incomplete toward fainter magnitudes, while the faint sample follows a monotonically decreasing completeness function at R>19 mag.

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Documento generato il 26/05/13 alle ore 09:38:04