Emission-line galaxies in the Slice of the Universe

Salzer, John J.; Aldering, G.; Bothun, G. D.; Mazzarella, J. M.; Lonsdale, C. J.

doi:10.1086/114902

Cited by 7 publications

(6 citation statements)

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“…This decrease in the fraction of ELGs in a dense medium, has been previously observed e.g. by Gisler (1978), Dressier et al (1985) and Salzer et al (1988), and it is related to the morphologydensity relation (Dressier 1980): in a denser environment, a lower quantity of gas available corresponds to a higher predominance of early-type (E-SO) galaxies and, therefore, to a reduced presence of star-forming systems, dominated by late-type galaxies.…”

Section: Frequency and Hubble Types Of Ucm Elgs In The Coma Clustersupporting

confidence: 65%

Photometric and morphological analysis of UCM galaxies. II. Statistical results and interpretation

Vitores

Zamorano

Rego

et al. 1996

Astron. Astrophys. Suppl. Ser.

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A b s tra c t. -We present the results of Thuan & Gunn r CCD imaging observations of the Universidad Complutense de Madrid (UCM) sample of emission-line galaxies (ELGs) selected by the presence of Ha emission in low resolution objective-prism spectra. In this work, a total of 212 objects from the UCM survey have been photometrically and morphologically characterized. In a previous paper, the observations, basic reductions and morphological classification for the UCM objects were presented. Here, we analyse the statistical properties of the sample and their interpretations. (2) The sample presents a very heterogeneous morphological population of galaxies. There is a clear predominance of late-type galaxies, with 66% being Sb or later. (3) We have found a set of galaxies specially interesting. In particular, we propose 9 candidates to BCD (blue compact dwarf galaxy), five of them previously unknown. (4) About 10% of the ELGs of the sample show typical parameters of SO types, and in the subsample of 16 UCM interacting galaxies, 25% are SO type galaxies. (5) In the set of UCM galaxies inside the Coma cluster, 71% exhibit Hubble types Sb or later.

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Section: Frequency and Hubble Types Of Ucm Elgs In The Coma Clustersupporting

confidence: 65%

Photometric and morphological analysis of UCM galaxies. II. Statistical results and interpretation

Vitores

Zamorano

Rego

et al. 1996

Astron. Astrophys. Suppl. Ser.

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“…3B shows the same structure we observe in the optical, although more sparsely sampled. Galaxies with emission lines (25) and galaxies of low surface brightness (26) also trace the same largescale structure.…”

Section: Recent Results Of the Cfa Surveymentioning

confidence: 85%

Mapping the Universe

Geller

Huchra

1989

Science

781

606

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Maps of the galaxy distribution in the nearby universe reveal large coherent structures. The extent of the largest features is limited only by the size of the survey. Voids with a density typically 20 percent of the mean and with diameters of 5000 km s(-1) are present in every survey large enough to contain them. Many galaxies lie in thin sheet-like structures. The largest sheet detected so far is the "Great Wall" with a minimum extent of 60 h(-1) Mpc x 170 h(-1) Mpc, where h is the Hubble constant in units of 100 km s(-1) Mpc(-1). The frequent occurrence of these structures is one of several serious challenges to our current understanding of the origin and evolution of the large-scale distribution of matter in the universe.

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“…Indications that morphological segregation also exists among field galaxies have been given by several works (Davis & Geller 1976, Giovanelli, Haynes & Chincarini 1986, Eder et al 1989, Lahav, Nemiroff & Piran 1990, Mo & Börner 1990, Santiago & Strauss 1992. While morphological segregation is fairly well established, at least on scales up to ∼ 10h −1 Mpc (H0 = 100h km s −1 Mpc −1 ), it has been more difficult to establish if the clustering properties of galaxies depend on luminosity (Phillipps & Shanks 1987, Alimi, Valls-Gabaud & Blanchard 1988, Hamilton 1988, Salzer, Hanson & Gavazzi 1990, Iovino et al 1993, surface brightness (Davis & Djorgovski 1985, Santiago & da Costa 1990, Thuan et al 1991, spectral properties (Salzer et al 1988) or circular velocity (White, Tully & Davis 1988, Mo & Lahav 1993. On the theoretical side, the existence of segregation among galaxies and the indirect evidence for segregation between light and matter on galactic and extra-galactic scales has led to the formulation of scenarios of biased galaxy formation (Kaiser 1984, Babul & White 1991.…”

Section: Introductionmentioning

confidence: 98%

The two-point correlation function and morphological segregation in the Optical Redshift Survey

Hermit

Santiago

Lahav

et al. 1996

Monthly Notices of the Royal Astronomical Society

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We study the clustering of galaxies in real and redshift space using the Optical Redshift Survey (ORS). We estimate the two point correlation function in redshift space, ξ(s), for several subsamples of ORS, spanning nearly a factor of 30 in volume. We detect significant variations in ξ(s) among the subsamples covering small volumes. For volumes > ∼ (75h −1 Mpc) 3 , however, the ORS subsamples present very similar clustering patterns. Fits of the formξ(s) = ( s s0 ) −γs give best-fit values in the range 1.5 ≤ γ s ≤ 1.7 and 6.5 ≤ s 0 ≤ 8.8h −1 Mpc for several samples extending to redshifts of 8000 km s −1 . However, in several cases ξ(s) is not well described by a single power-law, rendering the best-fit values quite sensitive to the interval in s adopted. We find significant differences in clustering between the diameter-limited and magnitude-limited ORS samples within a radius of 4000 km s −1 centered on the Local Group; ξ(s) is larger for the magnitude-limited sample than for diameter-limited one. We interpret this as an indirect result of the morphological segregation coupled with differences in morphological mix. We split ORS into different morphological subsamples and confirm the existence of morphological segregation of galaxies out to scales of s ∼ 10h −1 Mpc. Our results indicate that the relative bias factor between early type galaxies and late-types may be weakly dependent on scale. If real, this would suggest non-linear biasing.We also compute correlations as a function of radial and projected separations, ξ(r p , π), from which we derive the real space correlation function, ξ(r). We obtain values 4.9 ≤ r 0 ≤ 7.3h −1 Mpc and 1.5 ≤ γ r ≤ 1.7 for various ORS samples. As before, these values depend strongly on the range in r adopted for the fit. The results obtained in real space confirm those found using ξ(s), i.e. in small volumes, magnitude limited samples show larger clustering than do diameter limited ones. There is no difference when large volumes are considered. Our results prove to be robust to adoption of different estimators of ξ(s) and to alternative methods to compensate for sampling selection effects.

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Emission-line galaxies in the Slice of the Universe

Cited by 7 publications

References 0 publications

Photometric and morphological analysis of UCM galaxies. II. Statistical results and interpretation

Photometric and morphological analysis of UCM galaxies. II. Statistical results and interpretation

Mapping the Universe

The two-point correlation function and morphological segregation in the Optical Redshift Survey

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