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

By P. V. van Dokkum, M. Franx, D. Fabricant, G. Illingworth, D. Kelson. 2000

231 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Spectroscopic Identification of a Protocluster at z = 2.300: Environmental Dependence of Galaxy Properties at High Redshift (2005, background): “Most of the galaxies studied have been selected to have the morphological appearance of early type galaxies, possibly leading to different subsets of galaxies being selected at different epochs (called “progenitor bias” by van Dokkum et al. 2000).”
Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers (2012, background): “One of the most significant is “progenitor-bias”, which refers to the issue that samples of ETGs at high redshift might be biased towards the oldest progenitors of present-day early-type galaxies [66, 67], therefore not sampling the same population studied at intermediate redshifts.”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “…emission line strength, also show a trend with redshift (Allington-Smith et al. 1993; Oemler et al. 1997; Balogh et al. 1997; Couch et al. 1998; van Dokkum et al. 2000; Fasano et al. 2000; Lubin et al. 2002; Goto et al. 2003; Treu et al. 2003; Wilman et al. 2005; Poggianti et al. 2006; Desai et…”
The spatial and kinematic distributions of cluster galaxies in a ΩCDM universe: comparison with observations (2000, background): “Van Dokkum et al (2000) dispense with the distiction between elliptical and S0, and study the evolution of the fraction of early-type galaxies in rich clusters.”
UV-Optical Colors as Probes of Early-Type Galaxy Evolution (2006, background): “The lack of redshift evolution of the slope and scatter in optical CMRs (e.g. Bower et al. 1992, 1998; Ellis et al. 1997; Stanford et al. 1998; Gladders et al. 1998; van Dokkum et al. 2000) is consistent with a high formation redshift (z > 2), as is the evolution in their zero-point.”
Evolution since z = 1 of the Morphology-Density Relation for Galaxies (2004, background): “Nevertheless, several authors have measured the total early–type fraction fE+S0 in individual clusters atz≃1 (e.g. van Dokkum et al. 2000, 2001; Lubin et al. 2002).”
THE 3D-HST SURVEY: HUBBLE SPACE TELESCOPE WFC3/G141 GRISM SPECTRA, REDSHIFTS, AND EMISSION LINE MEASUREMENTS FOR ∼100,000 GALAXIES (2015, methodology): “As the input images have exactly half-pixel offsets by design, this results in a one-to-one correspondence between input and output pixels (e.g., van Dokkum et al. 2000) and offers the key benefit of preserving the individual pixel errors.”
The Morphology-Density Relation in z ~ 1 Clusters (2005, methodology): “However, for the present work, we do not classify galaxies as merger/peculiar systems (as done by van Dokkum et al. 2000, hereafter vD00) if one of the above standard morphological categories can indeed be applied to the individual objects involved in the merger.”
K-Band Properties of Galaxy Clusters and Groups: Luminosity Function, Radial Distribution, and Halo Occupation Number (2004, background): “Observations have suggested a higher frequency of merger events in high-redshift clusters (e.g., van Dokkum et al. 2000).”
The Assembly of Diversity in the Morphologies and Stellar Populations of High-Redshift Galaxies (2005, background): “101 Brinchmann et al. 1998; Lilly et al. 1998; Simard et al. 1999; van Dokkum et al. 2000; Stanford et al. 2004; Ravindranath et al. 2004), the morphological mix of galaxies at these redshifts shows an increase in the abundance of irregular and peculiar galaxies, particularly at fainter magnitudes…”
The Evolving Luminosity Function of Red Galaxies (2006, background): “A red galaxy locus is also observed within the z 1 cluster and field galaxy populations (van Dokkum et al. 2000; Blakeslee et al. 2003; Bell et al. 2004; Willmer et al. 2006).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, background): “As discussed by Willmer et al. (2006), this division between the red sequence and blue cloud is derived from the work of van Dokkum et al. (2000), in which the color–magnitude relation for early–type (i.e., solely morphologically–selected) galaxies is measured.”
The 2df SDSS LRG and QSO survey: evolution of the luminosity function of luminous red galaxies to z= 0.6 (2006, background): “One potential problem for studies of massive elliptical/early-type galaxies, particularly those tracking the evolution with redshift, is that of progenitor bias (van Dokkum & Franx 1996; van Dokkum et al. 2000).”
The Effect of Environment on the Ultraviolet Color-Magnitude Relation of Early-Type Galaxies (2006, background): “Later studies confirmed that this trend was not a selection effect (Dressler et al. 1997; van Dokkum et al. 2000).”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, methodology): “The fundamental plane zeropoint brightens by 1-2 mag (van Dokkum et al. 2000, Gebhardt et al. 2003, van Dokkum & Ellis 2003, Treu et al. 2005a,b, van der Wel et al. 2005), the magnitude-radius zeropoint brightens by 1-1.6 mag (Trujillo & Aguerri 2004; McIntosh et al. 2005), and M∗B for red galaxies…”
Bimodal gas accretion in the Horizon–MareNostrum galaxy formation simulation (2008, methodology): “As a consequence, the colour index (U-B) is also used as a proxy for the SFR as measured from [OII], and an absolute magnitude-dependent colour cut is made as an alternative to the SFR cut (van Dokkum et al. 2000).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “1 (e.g. Stanford et al. 1998; van Dokkum et al. 2000; Smith et al. 2005; Postman et al. 2005; Cooper et al. 2006; Capak et al. 2007; Poggianti et al. 2008).”