Butcher-Oemler Effect

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Title:
The galaxy population of Cl1601+42 at
Authors:
Dahlén, Tomas; Fransson, Claes; Näslund, Magnus
Affiliation:
Stockholm Observatory, Department of Astronomy, SCFAB, SE-106 91 Stockholm, Sweden
Journal:
Monthly Notices of the Royal Astronomical Society, Volume 330, Issue 1, pp. 167-183. (MNRAS Homepage)
Publication Date:
02/2002
Origin:
MNRAS
MNRAS Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL: CL1601+42, GALAXIES: DISTANCES AND REDSHIFTS, GALAXIES: LUMINOSITY FUNCTION, MASS FUNCTION, COSMOLOGY: OBSERVATIONS
Abstract Copyright:
(c) 2002 The Royal Astronomical Society
Bibliographic Code:
2002MNRAS.330..167D

Abstract

Photometric redshifts are used to determine the rest-frame luminosity function (LF) of both early- and late-type galaxies to for the cluster Cl1601+42 at . The total LF shows a steep faint-end slope , indicating the existence of a population of numerous dwarf galaxies. Luminous galaxies, with are mostly red, early-type galaxies, with a LF best described by a Gaussian. Faint galaxies are predominantly blue, late-type galaxies, well fitted by a Schechter function with . Compared with clusters at lower redshift, the steepening of the faint end starts at brighter magnitudes for Cl1601+42, which may indicate a brightening of the present-day dwarf population relative to the giant population with increasing redshift. Early-type galaxies are centrally concentrated, and dominate the core region, implying that the radial gradient of early-type galaxies seen in local clusters is already established at . Bright, late-type galaxies are rare, consistent with a decrease in star formation in field galaxies as they are accreted on to the cluster, while faint, blue galaxies are evenly distributed across the cluster, except for a depletion in the core region. The blue fraction is , which is somewhat lower than the Butcher-Oemler average at . The value of f B is found to increase with limiting magnitude and with radius from the centre.

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Title:
Hidden star-formation in the cluster of galaxies Abell 1689
Authors:
Duc, P.-A.; Poggianti, B. M.; Fadda, D.; Elbaz, D.; Flores, H.; Chanial, P.; Franceschini, A.; Moorwood, A.; Cesarsky, C.
Affiliation:
AA( CNRS URA 2052; CEA, DSM, DAPNIA, Service d'astrophysique, 91191 Gif-sur-Yvette Cedex, France), AB(Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AC(Instituto de Astrofisica de Canarias, Via Lactea s/n, 38200 La Laguna - Tenerife, Spain; CEA, DSM, DAPNIA, Service d'astrophysique, 91191 Gif-sur-Yvette Cedex, France), AD(CEA, DSM, DAPNIA, Service d'astrophysique, 91191 Gif-sur-Yvette Cedex, France; Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA 95064,USA), AE(DAEC/LUL, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon, France; CEA, DSM, DAPNIA, Service d'astrophysique, 91191 Gif-sur-Yvette Cedex, France), AF(CEA, DSM, DAPNIA, Service d'astrophysique, 91191 Gif-sur-Yvette Cedex, France), AG(Dipartimento di Astronomia, Universitàdi Padova, Vicolo dell'Osservatorio, 5, 35122 Padova, Italy), AH(European Southern Observatory, Karl-Schwarzchild-Strasse, 2 85748 Garching bei München, Germany), AI(European Southern Observatory, Karl-Schwarzchild-Strasse, 2 85748 Garching bei München, Germany)
Journal:
Astronomy and Astrophysics, v.382, p.60-83 (2002) (A&A Homepage)
Publication Date:
01/2002
Origin:
A&A
A&A Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1689, GALAXIES: EVOLUTION, INFRARED: GALAXIES
Abstract Copyright:
(c) 2002: Astronomy & Astrophysics
Bibliographic Code:
2002A&A...382...60D

Abstract

At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75 micron (LW2 filter) and 16 cluster members at 15 micron (LW3 filter) within a clustercentric radius of 0.5 Mpc \citep[][ Paper I]{Fadda00b}. We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by \citet{Butcher84}, that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular. Sources with a low [15 micron]/[6.75 micron] flux ratio typically consist of luminous passive early-type galaxies while those with a high MIR color index are mainly luminous, blue, emission-line, morphologically disturbed spirals, i.e. the star-forming galaxies usually associated with the ``Butcher-Oemler'' effect. On the other hand, at least 30% of the 15 micron sources have optical counterparts showing no evidence for current star-formation activity, while their 15 micron emission is most likely due to obscured star formation. We argue that the LW3 luminosity measured in the cluster members is a reliable tracer of the total infrared luminosity which in A1689 galaxies peaks at Lir = 6.2 x 1010 Lo . We derive from \Lir a star-formation rate free of dust extinction, SFR(IR), which we compare with that determined in the optical from the flux of the \OIIt emission line, SFR(opt). The highest total star formation rates (11 sfr) and dust extinction are measured in those galaxies exhibiting in their optical spectrum a signature of a dusty starburst. In contrast, none of the galaxies with post-starburst optical spectra has been detected by ISOCAM down to a 15 micron flux limit corresponding to 1.4 sfr. We find a median SFR(IR) of the LW3-detected galaxies of 2 sfr that is ten times higher than the median SFR(opt) of the \OIIt- detected galaxies. The ratio SFR(IR)/SFR(opt) is in fact very high, ranging between 10 and 100 for LW3-detected galaxies with \OIIt emission. We conclude that a major part, at least 90%, of the star formation activity taking place in Abell 1689 is hidden. Whether the high extinction measured in the star-forming cluster members results from the cluster environment itself or reflects a comparable extinction in the coeval field is still unclear. Based on observations collected at the European Southern Observatory, La Silla, Chile (ESO No. 61.A-0619).

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Title:
Anomalous Star Formation Activity of Less-Luminous Galaxies in a Cluster Environment
Authors:
Tajiri, Yuka Y.; Kamaya, Hideyuki
Affiliation:
AA(Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; tajiri@kusastro.kyoto-u.ac.jp, kamaya@kusastro.kyoto-u.ac.jp)
Journal:
The Astrophysical Journal, Volume 562, Issue 2, pp. L125-L128. (ApJ Homepage)
Publication Date:
12/2001
Origin:
UCP
ApJ Keywords:
Galaxies: Clusters: General, Stars: Formation
Abstract Copyright:
(c) 2001: The American Astronomical Society
Bibliographic Code:
2001ApJ...562L.125T

Abstract

We discuss a correlation between the star formation activity (SFA) and the luminosity of star-forming galaxies at intermediate redshifts of 0.2<=z<=0.6 in both cluster and field environments. The equivalent width (EW) of [O II] is used for the measurement of SFA, and the R-band absolute magnitude, MR, is used for the measurement of luminosity. In less-luminous (MR>~-20.7) galaxies, we find (1) the mean EW ([O II]) of cluster galaxies is smaller than that of field galaxies but that (2) some cluster galaxies have as large EWs ([O II]) as that of actively star-forming field galaxies. Based on both of these results, we discuss a new possible mechanism for the Butcher-Oemler (BO) effect, assuming that the luminosity of a galaxy is proportional to its dynamical mass. Our proposal is that BO galaxies are less-massive cluster galaxies with smaller peculiar velocities. They are then stable against Kelvin-Helmholtz instability (KHI) and are not affected by the tidal interaction between clusters and themselves. Their interstellar medium (ISM) would hardly be stripped, and their SFA would be little suppressed. Hence, as long as such galaxies keep up their SFA, the fraction of blue galaxies in a cluster does not decrease. As a cluster becomes virialized, however, such galaxies become more accelerated, the ISM available for SFA is stripped by KHI, and their color evolves redward, which produces the BO effect.

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Title:
Galaxy Population in a Cluster of Galaxies around the Radio Galaxy 3C 324 at z=1.2
Authors:
Nakata, Fumiaki; Kajisawa, Masaru; Yamada, Toru; Kodama, Tadayuki; Shimasaku, Kazuhiro; Tanaka, Ichi; Doi, Mamoru; Furusawa, Hisanori; Hamabe, Masaru; Iye, Masanori; Kimura, Masahiko; Komiyama, Yutaka; Miyazaki, Satoshi; Okamura, Sadanori; Ouchi, Masami; Sasaki, Toshiyuki; Sekiguchi, Maki; Yagi, Masafumi; Yasuda, Naoki
Affiliation:
AA(Dep. of Astronomy, School of Science, The University of Tokyo nakata@astron.s.u-tokyo.ac.jp) AB(Astronomical Institute, Tohoku University) AC(National Astronomical Observatory of Japan) AD(Dep. of Astronomy, School of Science, The University of Tokyo) AE(Dep. of Astronomy, School of Science, The University of Tokyo) AF(National Astronomical Observatory of Japan) AG(Institute of Astronomy, The University of Tokyo) AH(Dep. of Astronomy, School of Science, The University of Tokyo) AI(Dept. of Mathematical and Physical Sciences, Japan Women's University) AJ(National Astronomical Observatory of Japan) AK(Institute for Cosmic Ray Research, The University of Tokyo) AL(Subaru Telescope, NAOJ) AM(National Astronomical Observatory of Japan) AN(Dep. of Astronomy, School of Science, The University of Tokyo) AO(Dep. of Astronomy, School of Science, The University of Tokyo) AP(Subaru Telescope, NAOJ) AQ(Institute for Cosmic Ray Research, The University of Tokyo) AR(National Astronomical Observatory of Japan) AS(National Astronomical Observatory of Japan)
Journal:
Publications of the Astronomical Society of Japan, Vol.53, No. 6, pp. 1139-1152
Publication Date:
12/2001
Origin:
PASJ
Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL (3C 324), GALAXIES: ELLIPTICAL AND LENTICULAR, CD, GALAXIES: EVOLUTION, GALAXIES: FORMATION, GALAXIES: LUMINOSITY FUNCTION, MASS FUNCTION
Abstract Copyright:
(c) 2001: Astronomical Society of Japan
Bibliographic Code:
2001PASJ...53.1139N

Abstract

We discuss the properties of galaxies around the radio galaxy 3C 324 at z=1.2 based on BVRIK' multi-band imaging data. We have applied a photometric-redshift technique to objects in the 3C 324 field, and identified 35 objects as plausible cluster members. We have found that red and luminous members are concentrated in a small region enclosed by a circle of 40'' radius (0.33 Mpc at z=1.2 for Ω0 = 0.3, λ0 = 0.7, H0 = 70 km s-1 Mpc-1 cosmology) from the 3C 324 galaxy. The 3C 324 cluster is probably much more compact in size compared with the local clusters. We constructed a K'-band luminosity function of the cluster members and fitted a Schechter function, and found the characteristic magnitude to be K'*AB = 20.2 +/- 0.6. This value is consistent with the extrapolation of the pure passive evolution seen for z < 1 clusters. We have identified eight bright galaxies which form a red color--magnitude sequence. The slope of the sequence is consistent with the passive evolution model down to K'AB < 22 K'AB; we also found that there is no clear age variation in these bright red galaxies. However, seven out of these eight galaxies exhibit a significant excess in the rest UV light with respect to the passive evolution model. This may suggest that the massive early-type galaxies in this high-redshift cluster are still forming stars to some extent. We have confirmed a truncation of the color--magnitude sequence at K'AB~22 faint passively-evolving galaxies may not yet be present in this cluster at z ~ 1.2. The overall color distribution of the cluster members, selected by the photometric redshift technique, is found to be very broad. We derived the fraction of blue galaxies in this cluster following a definition of Butcher and Oemler (1984, AAA 038.160.068), and obtained fB = 0.39 +/- 0.28, which is higher than that for z < 1 clusters. This indicates that the star-formation activity of this cluster is, on the average, higher than that of lower redshift counterparts.

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Title:
Reconstructing the history of star formation in rich cluster cores
Authors:
Kodama, Tadayuki; Bower, Richard G.
Affiliation:
AA(Department of Physics, University of Durham, South Road, Durham DH1 3LE ; Department of Astronomy, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan), AB(Department of Astronomy, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan)
Journal:
Monthly Notices of the Royal Astronomical Society, Volume 321, Issue 1, pp. 18-36. (MNRAS Homepage)
Publication Date:
02/2001
Origin:
MNRAS
MNRAS Keywords:
GALAXIES: CLUSTERS: GENERAL, GALAXIES: EVOLUTION, GALAXIES: FORMATION, GALAXIES: STELLAR CONTENT
Abstract Copyright:
(c) 2001 The Royal Astronomical Society
Bibliographic Code:
2001MNRAS.321...18K

Abstract

Our study begins by revisiting the photometric Butcher-Oemler effect using data from seven CNOC clusters at 0.23<~z<0.43. We construct the foreground/background-corrected colour-magnitude diagrams for these clusters. Our analysis shows that the CNOC clusters reproduce the trend of increasing blue galaxy fraction with redshift as seen by Butcher & Oemler. We use these data to investigate the history of star formation in clusters by connecting these clusters as snapshots at different redshifts. We address two key issues. First, we ask whether the simple fading and passive evolution of the blue galaxies is consistent with the properties of galaxies in nearby clusters, such as the Coma cluster. We find that the evolution of star-forming field galaxies towards redder colour (once the star formation ceases on entry into the cluster environment) can successfully reconstruct colours and magnitudes of galaxies in the local cluster. There is no requirement for widespread disruption of these galaxies. Since the blue galaxies fade as they age, the fainter galaxies on the present-day colour-magnitude relation tend to have more extended star formation histories than their bright counterparts. However, this effect is not sufficient to cause a sizeable age variation for the galaxies along the colour-magnitude relation, implying that the slope is dominated by variations in metal abundance. Secondly, we address the nature of the Butcher-Oemler effect itself. We compare the distribution of galaxies in the colour-magnitude diagrams and hence infer the evolution of the rate at which galaxies have arrived in the cluster. Models in which star formation is abruptly truncated as galaxies are accreted by the cluster have difficulty in reproducing the observed colour distribution. In contrast, if star formation declines on a 1-Gyr time-scale after accretion, the galaxy accretion history we infer is consistent from cluster to cluster and matches well the distribution expected in simple theoretical models. The Butcher-Oemler effect is thus driven both by the declining star formation rates of field galaxies and by a decline in the rate at which fresh galaxies are accreted by the cluster. Our study naturally leads to a comparison of the global star formation histories of galaxies in clusters and the field. We show that the star formation rate per galaxy mass for galaxies in cluster cores is significantly smaller than that of the field environment below z<1 due to the truncation of star formation. However, the factor by which star formation is suppressed is dependent on the cluster accretion history. High-quality observations of clusters at higher redshifts are needed to define this relation better.

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Title:
The Butcher-Oemler Effect in 295 Clusters: Strong Redshift Evolution and Cluster Richness Dependence
Authors:
Margoniner, V. E.; de Carvalho, R. R.; Gal, R. R.; Djorgovski, S. G.
Affiliation:
AA(; Bell Laboratories, Lucent Technologies, 600 Mountain Avenue, Murray Hill, NJ 07974; vem@physics.bell-labs.com.; Observatório Nacional, Rua General José Cristino, São Cristovão, CEP 20921-400, Rio de Janeiro, Brazil.), AB(; Observatório Nacional, Rua General José Cristino, São Cristovão, CEP 20921-400, Rio de Janeiro, Brazil.), AC(; Palomar Observatory, California Institute of Technology, MC 105-24, Pasadena, CA 91125.), AD(; Palomar Observatory, California Institute of Technology, MC 105-24, Pasadena, CA 91125.)
Journal:
The Astrophysical Journal, Volume 548, Issue 2, pp. L143-L146. (ApJ Homepage)
Publication Date:
02/2001
Origin:
UCP
ApJ Keywords:
Galaxies: Clusters: General, Galaxies: Evolution
Abstract Copyright:
(c) 2001: The American Astronomical Society
Bibliographic Code:
2001ApJ...548L.143M

Abstract

We examine the Butcher-Oemler effect and its cluster richness dependence in the largest sample studied to date: 295 Abell clusters. We find a strong correlation between cluster richness and the fraction of blue galaxies, fB, at every redshift. The slope of the fB(z) relation is similar for all richnesses, but at a given redshift, fB is systematically higher for poor clusters. This is the chief cause of scatter in the fB versus z diagram; the spread caused by the richness dependence is comparable to the trend in fB over a typical redshift baseline so that conclusions drawn from smaller samples have varied widely. The two parameters, z and a consistently defined projected galaxy number density N, together account for all of the observed variation in fB within the measurement errors. The redshift evolution of fB is real and occurs at approximately the same rate for clusters of all richness classes.

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Title:
The Evolution of Population Gradients in Galaxy Clusters: The Butcher-Oemler Effect and Cluster Infall
Authors:
Ellingson, E.; Lin, H.; Yee, H. K. C.; Carlberg, R. G.
Affiliation:
AA(Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309; e.elling@casa.colorado.edu), AB(Steward Observatory, University of Arizona, Tucson, AZ 85721; hlin@as.arizona.edu), AC(Department of Astronomy, University of Toronto, Toronto, ON, M5S 3H8, Canada; hyee@makalu.astro.utoronto.ca, carlberg@moonray.astro.utoronto.ca; Guest observer, Canada-France-Hawaii Telescope, operated jointly by NRC of Canada, CNRS of France, and University of Hawaii.), AD(Department of Astronomy, University of Toronto, Toronto, ON, M5S 3H8, Canada; hyee@makalu.astro.utoronto.ca, carlberg@moonray.astro.utoronto.ca)
Journal:
The Astrophysical Journal, Volume 547, Issue 2, pp. 609-622. (ApJ Homepage)
Publication Date:
02/2001
Origin:
UCP
ApJ Keywords:
Galaxies: Clusters: General, Galaxies: Evolution, Galaxies: Statistics
Abstract Copyright:
(c) 2001: The American Astronomical Society
Bibliographic Code:
2001ApJ...547..609E

Abstract

We present photometric and spectroscopic measurements of the galaxy populations in clusters from the CNOC1 sample of rich, X-ray-luminous clusters at 0.18<z<0.55. A classical measure of the galaxy blue fraction for spectroscopically confirmed cluster members shows a significant Butcher-Oemler effect for the sample, but only when radii larger than 0.5r200 are considered. We perform a principal component analysis of galaxy spectra to divide the total cluster light into contributions from stellar populations of different ages. Composite radial distributions of different stellar populations show strong gradients as a function of clustercentric radius. The composite population is dominated by evolved populations in the core, and gradually changes at radii greater than the virial radius to one which is similar to coeval field galaxies. We do not see evidence at any radius within the clusters for an excess of star formation over that seen in the coeval field. Within this redshift range, significant evolution in the fractional population gradient is seen. Both low- and high-redshift clusters have similar populations in the cluster cores, but higher redshift clusters have steeper gradients and more star-forming galaxies at radii outside of the core region-in effect, a restatement of the Butcher-Oemler effect. Luminosity density profiles are consistent with a scenario where this phenomenon is due to a decline over time in the infall rate of field galaxies into clusters. Depending on how long galaxies reside in clusters before their star formation rates are diminished, this suggests a decrease in the infall into clusters of a factor of ~3 between z>0.8 and z~0.5. We also discuss alternative scenarios for the evolution of cluster populations.

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Title:
The evolutionary history of early-type galaxies as derived from the fundamental plane
Authors:
Pahre, M. A.; Djorgovski, S. G.; De Carvalho, R. R.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Mail Stop 20, 60 Garden Street, Cambridge, MA 02138, U.S.A.; mpahre@cfa.harvard.edu), AB(Palomar Observatory, California Institute of Technology, Mail Stop 105-24, Pasadena, CA 91125, U.S.A.; george@oracle.caltech.edu), AC(Departamento de Astrofisica, Observatorio Nacional, MCT, Rua General José Cristino 77, 20921-030 São Cristóvão, Rio de Janeiro, Brazil; reinaldo@obsn.on.br)
Journal:
Astrophysics and Space Science, v. 276, Issue 2/4, p. 983-990 (2001). (Ap&SS Homepage)
Publication Date:
00/2001
Origin:
KLUWER
Abstract Copyright:
(c) 2001 Kluwer Academic Publishers
Bibliographic Code:
2001Ap&SS.276..983P

Abstract

The fundamental plane (FP) scaling relations and their evolution are a powerful tool for studying the global properties of early-type galaxies and their evolutionary history. The form of the FP, as derived by surveys in the local Universe at wavelengths ranging from the U to the K band, cannot be explained by metallicity variations alone among early-type galaxies; systematic variations in age, dark matter content, or homology breaking are required. A large-scale study of early-type galaxies at 0.1 < z < 0.6 demonstrates that the SB intercept of the FP, the rest frame (U-V) colour, and the absorption line strengths all evolve passively, thereby implying a high mean formation redshift for the stellar content. The slope of the FP evolves with redshift, which is broadly consistent with systematic age effects occurring along the early-type galaxy sequence. The implication that the least luminous early-type galaxies formed later than the luminous galaxies is discussed in the context of the evolution of the colour-magnitude relation, the Butcher-Oemler effect and hierarchical galaxy formation models.

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Title:
Dynamical and content evolution of a sample of clusters from z ~ 0 to z ~ 0.5
Authors:
Adami, C.; Holden, B. P.; Castander, F. J.; Mazure, A.; Nichol, R. C.; Ulmer, M. P.
Affiliation:
AA( LAM, Traverse du Siphon, 13012 Marseille, France; Department of Physics and Astronomy, NU, Dearborn Observatory, 2131 Sheridan, 60208-2900 Evanston, USA), AB(Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, USA), AC(Observatoire Midi-Pyrenees 14, Avenue Edouard Belin, 31400 Toulouse, France; Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, USA), AD( LAM, Traverse du Siphon, 13012 Marseille, France), AE(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA), AF(Department of Physics and Astronomy, NU, Dearborn Observatory, 2131 Sheridan, 60208-2900 Evanston, USA)
Journal:
Astronomy and Astrophysics, v.362, p.825-834 (2000) (A&A Homepage)
Publication Date:
10/2000
Origin:
A&A
A&A Keywords:
GALAXIES: CLUSTERS: GENERAL, COSMOLOGY: OBSERVATIONS, COSMOLOGY: LARGE-SCALE STRUCTURE OF UNIVERSE
Abstract Copyright:
(c) 2000: Astronomy & Astrophysics
Bibliographic Code:
2000A&A...362..825A

Abstract

In this paper, we present an analysis of the dynamics and segregation of galaxies in rich clusters from z ~ 0.32 to z ~ 0.48 taken from the CFHT Optical PDCS (COP) survey and from the CNOC survey (Carlberg et al. 1997). Our results from the COP survey are based upon the recent observational work of Adami et al. (2000a) and Holden et al. (2000) and use new spectroscopic and photometric data on six clusters selected from the Palomar Distant Cluster Survey (PDCS; Postman et al. 1996). We have compared the COP and CNOC samples to the ESO Nearby Abell Cluster Survey (ENACS: z ~ 0.07). Our sample shows that the z <= 0.4 clusters have the same velocity dispersion versus magnitude, morphological type and radius relationships as nearby ( ~ 0.07) Abell clusters. The z ~ 0.48 clusters exhibit, however, departures from these relations. Furthermore, there appears to be a higher fraction of late-type (or bluer, e.g. Butcher & Oemler, 1984) galaxies in the distant clusters compared to the nearby ones. The classical scenario in which massive galaxies virialize before they evolve from late into early type explain our observations. In such a scenario, the clusters of our sample began to form before a redshift of approximately 0.8 and the late-type galaxy population had a continuous infall into the clusters.

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Title:
Hubble Space Telescope Photometry and Keck Spectroscopy of the Rich Cluster MS 1054-03: Morphologies, Butcher-Oemler Effect, and the Color-Magnitude Relation at Z = 0.83
Authors:
van Dokkum, Pieter G.; Franx, Marijn; Fabricant, Daniel; Illingworth, Garth D.; Kelson, Daniel D.
Affiliation:
AA(Present address: California Institute of Technology, MS 105-24, Pasadena, CA 91125), AB(Leiden Observatory, P.O. Box 9513, NL-2300 RA, Leiden, The Netherlands), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02318), AD(University of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064), AE(D. T. M., Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington DC, 20015)
Journal:
The Astrophysical Journal, Volume 541, Issue 1, pp. 95-111. (ApJ Homepage)
Publication Date:
09/2000
Origin:
UCP
ApJ Keywords:
galaxies: clusters: individual (MS 1054-03), Galaxies: Elliptical and Lenticular, cD, Galaxies: Evolution, Galaxies: Structure
Abstract Copyright:
(c) 2000: The American Astronomical Society
Bibliographic Code:
2000ApJ...541...95V

Abstract

We present a study of 81 I-band selected, spectroscopically confirmed members of the X-ray cluster MS 1054-03 at z=0.83. Redshifts and spectral types were determined from Keck spectroscopy. Morphologies and accurate colors were determined from a large mosaic of HST WFPC2 images in RF606W and IF814W, corresponding to U and B in the rest frame. Early-type galaxies constitute only 44% of this galaxy population. This fraction is much lower than in comparable rich clusters at low redshift. Thirty-nine percent are spiral galaxies, and 17% are mergers. The early-type galaxies follow a tight and well-defined color-magnitude relation, with the exception of a few outliers. The observed scatter is 0.029+/-0.005 mag in rest frame U-B. Most of the mergers lie close to the CM relation defined by the early-type galaxies. They are bluer by only 0.07+/-0.02 mag, and the scatter in their colors is 0.07+/-0.04 mag. Spiral galaxies in MS 1054-03 exhibit a large range in their colors. The bluest spiral galaxies are ~0.7 mag bluer than the early-type galaxies, but the majority is within +/-0.2 mag of the early-type galaxy sequence. The red colors of the mergers and the majority of the spiral galaxies are reflected in the fairly low Butcher-Oemler blue fraction of MS 1054-03: fB=0.22+/-0.05, similar to intermediate redshift clusters and much lower than previously reported values for clusters at z~0.8. The slope and scatter of the CM relation of early-type galaxies are roughly constant with redshift, confirming previous studies that were based on ground-based color measurements and very limited membership information. However, the scatter in the combined sample of early-type galaxies and mergers (i.e., the sample of future early-type galaxies) is twice as high as the scatter of the early-type galaxies alone. This is a direct demonstration of the ``progenitor bias'': high-redshift early-type galaxies seem to form a homogeneous, old population because the progenitors of the youngest present-day early-type galaxies are not included in the sample. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.

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Title:
Cluster Populations in A115 and A2283
Authors:
Rakos, Karl D.; Schombert, James M.; Odell, Andrew P.; Steindling, Susanna
Affiliation:
AA(Institute for Astronomy, University of Vienna, A-1180, Wien, Austria; rakosch@astro1.ast.univie.ac.at), AB(Department of Physics, University of Oregon, Eugene, OR 97403; js@abyss.uoregon.edu), AC(Department of Physics and Astronomy, Northern Arizona University, Box 6010, Flagstaff, AZ 86011; andy.odell@nau.edu), AD(Wise Observatory and the School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel; susan@wise1.tau.ac.il)
Journal:
The Astrophysical Journal, Volume 540, Issue 2, pp. 715-725. (ApJ Homepage)
Publication Date:
09/2000
Origin:
UCP
ApJ Keywords:
Galaxies: Clusters: General, galaxies: clusters: individual (A115, A2283), Galaxies: Evolution
Abstract Copyright:
(c) 2000: The American Astronomical Society
Bibliographic Code:
2000ApJ...540..715R

Abstract

This paper presents four-color narrowband photometry of clusters A115 (z=0.191) and A2283 (z=0.182) in order to follow the star formation history of various galaxy types. Although located at similar redshifts, the two clusters display very different fractions of blue galaxies (i.e., the Butcher-Oemler effect; fB=0.13 for A115, fB=0.30 for A2283). A system of photometric classification is applied to the cluster members that divides the cluster population into four classes based on their recent levels of star formation. It is shown that the blue population of each cluster is primarily composed of normal star-forming (star formation rate<1 Msolar yr-1) galaxies at the high-luminosity end but with an increasing contribution from a dwarf starburst population below M5500=-20. This dwarf starburst population appears to be the same population of low-mass galaxies identified in recent Hubble Space Telescope imaging, possible progenitors to present-day cluster dwarf ellipticals, irregulars, and blue compact dwarfs. Deviations in the color-magnitude relationship for the red galaxies in each cluster suggest that a population of blue S0s is evolving into present-day S0 colors at this epoch. The radial distribution of the blue population supports the prediction of galaxy harassment mechanisms for tidally induced star formation operating on an infalling set of gas-rich galaxies.

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Title:
An excess of mid-IR luminous galaxies in Abell 1689?
Authors:
Fadda, D.; Elbaz, D.; Duc, P.-A.; Flores, H.; Franceschini, A.; Cesarsky, C. J.; Moorwood, A. F. M.
Affiliation:
AA( CEA Saclay - Service d'Astrophysique, Orme des Merisiers, 91191 Gif-sur-Yvette Cédex, France), AB( CEA Saclay - Service d'Astrophysique, Orme des Merisiers, 91191 Gif-sur-Yvette Cédex, France), AC(CNRS URA 2052 and CEA Saclay - Service d'Astrophysique, Orme des Merisiers, 91191 Gif-sur-Yvette Cédex, France; University of Cambridge, Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK), AD( CEA Saclay - Service d'Astrophysique, Orme des Merisiers, 91191 Gif-sur-Yvette Cédex, France), AE(Dipartimento di Astronomia, Universitàdi Padova, Vicolo dell'Osservatorio, 5, 35122 Padova, Italy), AF(European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany), AG(European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany)
Journal:
Astronomy and Astrophysics, v.361, p.827-840 (2000) (A&A Homepage)
Publication Date:
09/2000
Origin:
A&A
A&A Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL: A 1689, GALAXIES: EVOLUTION, COSMOLOGY: OBSERVATIONS, INFRARED: GALAXIES
Abstract Copyright:
(c) 2000: Astronomy & Astrophysics
Bibliographic Code:
2000A&A...361..827F

Abstract

We present the results of infrared observations of Abell 1689, an exceptionally rich cluster of galaxies at intermediate redshift (z^simeq 0.181). It was observed with ISOCAM, at 6.7 mum and 15 mum , and ISOPHOT at 200 mum from the Infrared Space Observatory (ISO). The cluster galaxies detected above a sensitivity limit of 0.15 mJy in the 6.7 mum band, whose emission is mostly dominated by their stellar component, show optical colors similar to the overall cluster population and are gathered in the center of the cluster, following the distribution of the cluster early-types. In the 15 mum band, above a sensitivity limit of 0.3 mJy, the galaxies spectroscopically confirmed to be cluster members are blue outliers of the cluster color-magnitude relation and become brighter going from the center to the outer parts of the cluster. We compare the 6.7 mum and 15 mum fluxes and the cumulative distributions of the B-[6.75] and B-[15] colors of the A1689 galaxies, above our 90% completeness limits of 0.2 and 0.4 mJy for 6.7 mum and 15 mum respectively, to the galaxies of two nearby clusters, Virgo and Coma, and to the field galaxies at the same redshift of the cluster. Although the B-[6.7] color distributions of the three clusters are compatible, we find a systematic excess of B-[15] color distribution for the galaxies located in Abell 1689 with respect to Coma or Virgo galaxies. This result proves the existence of a mid-infrared equivalent of the Butcher-Oemler effect measured in the optical. The comparison of 15 mum flux and B-[15] color distributions of A1689 and field galaxies does not show strong differences between the population of starburst galaxies in the cluster and in the field. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) with the participation of ISAS and NASA

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Title:
The Palomar Abell Cluster Optical Survey. I. Photometric Redshifts for 431 Abell Clusters
Authors:
Gal, R. R.; de Carvalho, R. R.; Brunner, R.; Odewahn, S. C.; Djorgovski, S. G.
Affiliation:
AA(Observatório Nacional, Rua General José Cristino 77, 20921-400 São Cristóvão, Rio de Janeiro, RJ, Brazil rrg@astro.caltech.edu), AB(Observatório Nacional, Rua General José Cristino 77, 20921-400 São Cristóvão, Rio de Janeiro, RJ, Brazil), AC(Department of Physics and Astronomy, Arizona State University, Box 871504, Tempe, AZ 85287-1504), AD(Department of Physics and Astronomy, Arizona State University, Box 871504, Tempe, AZ 85287-1504), AE(Palomar Observatory, California Institute of Technology, Mail Stop 105-24, Pasadena, CA 91125)
Journal:
The Astronomical Journal, Volume 120, Issue 2, pp. 540-551. (AJ Homepage)
Publication Date:
08/2000
Origin:
UCP
AJ Keywords:
Catalogs, Galaxies: Clusters: General, Surveys
Abstract Copyright:
(c) 2000: The American Astronomical Society
Bibliographic Code:
2000AJ....120..540G

Abstract

This paper presents photometric redshifts for 431 Abell clusters imaged as part of the Palomar Abell Cluster Optical Survey, of which 236 are new redshifts. We have obtained moderately deep, three-band (Gunn gri) imaging for this sample at the Palomar Observatory 60 inch (1.5 m) telescope, as part of the photometric calibration of the Digitized Second Palomar Sky Survey. Our data acquisition, reduction, and photometric calibration techniques are described, and photometric accuracy and consistency are demonstrated. An empirical redshift estimator is presented, utilizing background-corrected median g-r colors and mean g magnitudes for the ensemble of galaxies in each field. We present photometric redshift estimates for the clusters in our sample with an accuracy of σz=0.038. These redshift estimates provide checks on single-galaxy cluster redshifts, as well as distance information for studies of the Butcher-Oemler effect, luminosity functions, mass-to-light ratios, and many other projects.

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Title:
Photometric Properties of 48 Clusters of Galaxies. I. The Butcher-Oemler Effect
Authors:
Margoniner, V. E.; de Carvalho, R. R.
Affiliation:
AA(Bell Laboratories, Lucent Technologies, 700 Mountain Avenue, Murray Hill, NJ 07974; vem@physics.bell-labs.com.; Observatório Nacional, Rua General José Cristino 77, 20921-400 São Cristóvão, Rio de Janeiro, RJ, Brazil; reinaldo@on.br), AB(Observatório Nacional, Rua General José Cristino 77, 20921-400 São Cristóvão, Rio de Janeiro, RJ, Brazil; reinaldo@on.br)
Journal:
The Astronomical Journal, Volume 119, Issue 4, pp. 1562-1578. (AJ Homepage)
Publication Date:
04/2000
Origin:
UCP
AJ Keywords:
GALAXIES: CLUSTERS: GENERAL, GALAXIES: EVOLUTION, GALAXIES: FUNDAMENTAL PARAMETERS, GALAXIES: PHOTOMETRY
Abstract Copyright:
(c) 2000: The American Astronomical Society
Bibliographic Code:
2000AJ....119.1562M

Abstract

We present gri CCD photometry of 44 Abell clusters and four cluster candidates. Twenty-one clusters in our sample have spectroscopic redshifts. Fitting a relation between mean g, r, and i magnitudes and redshift for this subsample, we have calculated photometric redshifts for the remainder with an estimated accuracy of approximately 0.03. The resulting redshift range for the sample is 0.03<z<0.38. Color-magnitude diagrams are presented for the complete sample and used to study evolution of the galaxy population in the cluster environment. Our observations show a strong Butcher-Oemler effect, with an increase in the fraction of blue galaxies (fB) with redshift that seems more consistent with the steeper relation estimated in 1995 by Rakos and Schombert than with the original one by Butcher and Oemler in 1984. However, in the redshift range between about 0.08 and 0.2, where most of our clusters lie, there is a wide range of fB-values, consistent with no redshift evolution of the cluster galaxy population. A large range of fB-values is also seen between about 0.2 and 0.3, when we add X-ray clusters from Smail et al. to our sample. The discrepancies between samples underscore the need for an unbiased sample to understand how much of the Butcher-Oemler effect is due to evolution and how much to selection effects. We also tested the idea proposed by Garilli et al. in 1996 that there is a population of unusually red galaxies that could be associated either with the field or clusters, but we find that these objects are all near the limiting magnitude of the images (20.5<r<22) and have colors that are consistent with those expected for stars or field galaxies at z~0.7.

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Title:
The Butcher-Oemler Effect at Moderate Redshift
Authors:
Metevier, Anne J.; Romer, A. Kathy; Ulmer, M. P.
Affiliation:
AA(Department of Physics and Astronomy, Dearborn Observatory, Northwestern University, 2131 Sheridan Road, Evanston, IL 60208-2900 metevier@lilith.astro.nwu.edu), AB(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213-3890 romer@astro.phys.cmu.edu), AC(Department of Physics and Astronomy, Dearborn Observatory, Northwestern University, 2131 Sheridan Road, Evanston, IL 60208-2900 m-ulmer2@nwu.edu)
Journal:
The Astronomical Journal, Volume 119, Issue 3, pp. 1090-1099. (AJ Homepage)
Publication Date:
03/2000
Origin:
UCP
AJ Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL (ABELL 98, ABELL 115, ABELL 2356), GALAXIES: EVOLUTION, GALAXIES: PHOTOMETRY
Abstract Copyright:
(c) 2000: The American Astronomical Society
Bibliographic Code:
2000AJ....119.1090M

Abstract

We present the results of Butcher-Oemler-style analysis of three moderate-redshift (0.1<z<0.2) clusters that have bimodal X-ray surface brightness profiles. We find that at least two of these clusters exhibit unusually high fractions of blue galaxies (fb's) as compared with clusters at comparable redshifts studied by Butcher & Oemler. This implies that star formation is occurring in a high fraction of the galaxies in the two clusters. Our results are consistent with hierarchical clustering models in which subcluster-subcluster mergers create shocks in the intracluster medium. The shocks, in turn, induce simultaneous starbursts in a large fraction of cluster galaxies. Our study therefore lends weight to the hypothesis that the Butcher-Oemler effect is an environmental, as well as evolutionary, phenomenon.

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