The ACS Virgo Cluster Survey. IV. Data Reduction Procedures for Surface Brightness Fluctuation Measurements with the Advanced Camera for Surveys

AbstractWe present the size-luminosity relation (SLR) for disk galaxies observed in eight clusters from the ESO Distant Cluster Survey (EDisCS). These clusters, at redshifts 0.4 < z < 0.8, were observed with the Hubble Space Telescope's Advanced Camera for Surveys. While we observe a change in the SLR with redshift, namely that there is an absence of low surface brightness galaxies at high redshift, we demonstrate that this could be a product of selection effects and thus is not a confirmation of evolution. We also compare the SLR for cluster and field galaxies in each redshift bin and see no significant effects of environment on the SLR.

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Near-infrared surface brightness fluctuation measurements with the Hubble Space Telescope's WFC3/IR channel

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312021734 ◽

2012 ◽

Vol 8 (S289) ◽

pp. 371-374

Author(s):

Hyejeon Cho ◽

Joseph B. Jensen ◽

John P. Blakeslee ◽

Brigham S. French ◽

Hyun-chul Lee ◽

...

Keyword(s):

Surface Brightness ◽

Near Infrared ◽

Hubble Space Telescope ◽

Wide Field ◽

Population Synthesis ◽

Early Type ◽

Distance Method ◽

Brightness Fluctuation ◽

Advanced Camera For Surveys ◽

Fornax Cluster

AbstractThe surface brightness fluctuation (SBF) method at near-infrared (NIR) wavelengths is a powerful tool for estimating distances to unresolved stellar systems with high precision. The IR channel of the Wide Field Camera 3 (WFC3), installed on board the Hubble Space Telescope (HST) in 2009, has a greater sensitivity and a wider field of view than the previous generation of HST IR instruments, making it much more efficient for measuring distances to early-type galaxies in the Local Volume. To take full advantage of its capabilities, we need to empirically calibrate the SBF distance method for WFC3's NIR passbands. We present the SBF measurements for the WFC3/IR F160W bandpass filter using observations of 16 early-type galaxies in the Fornax and Virgo Clusters. These have been combined with existing (g475–z850) color measurements from the Advanced Camera for Surveys Virgo and Fornax Cluster Surveys to derive a space-based H160-band SBF relation as a function of color. We have also compared the absolute SBF magnitudes to those predicted by evolutionary population synthesis models in order to study stellar population properties in the target galaxies.

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The ACS Virgo Cluster Survey. II. Data Reduction Procedures

The Astrophysical Journal Supplement Series ◽

10.1086/422977 ◽

2004 ◽

Vol 154 (2) ◽

pp. 509-517 ◽

Cited By ~ 67

Author(s):

Andres Jordan ◽

John P. Blakeslee ◽

Eric W. Peng ◽

Simona Mei ◽

Patrick Cote ◽

...

Keyword(s):

Data Reduction ◽

Virgo Cluster ◽

Cluster Survey

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The properties of bright globular clusters, ultra-compact dwarfs and dwarf nuclei in the Virgo core: hints on origin of ultra-compact dwarf galaxies (UCDs)

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318006701 ◽

2018 ◽

Vol 14 (S344) ◽

pp. 384-388

Author(s):

Chengze Liu ◽

Eric W. Peng ◽

Patrick Côté ◽

Hong-Xin Zhang ◽

Laura Ferrarese ◽

...

Keyword(s):

Globular Clusters ◽

Surface Brightness ◽

Dwarf Galaxies ◽

Virgo Cluster ◽

Spatial Distributions ◽

Next Generation ◽

Cluster Survey ◽

Low Surface Brightness ◽

Color Gradient

AbstractBased on the data from the Next Generation Virgo cluster Survey (NGVS), we statistically study the photometric properties of globular clusters (GCs), ultra-compact dwarfs (UCDs) and dwarf nuclei in the Virgo core (M87) region. We found an obvious negative color (g - z) gradient in GC system associate with M87, i.e. GCs in the outer regions are bluer. However, such color gradient does not exist in UCD system, neither in dwarf nuclei system around M87. In addition, we found that many UCDs are surrounded by extended, low surface brightness envelopes. The dwarf nuclei and UCDs show different spatial distributions from GCs, with dwarf nuclei and UCDs (especially for the UCDs with visible envelopes) lying at larger distances to the Virgo center. These results support the view that UCDs (at least for a fraction of UCDs) are more tied to dwarf nuclei than to GCs.

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