The dispersion in the near-infrared surface brightness fluctuations in the Virgo cluster

1994 ◽  
Vol 433 ◽  
pp. 567 ◽  
Author(s):  
Michael A. Pahre ◽  
Jeremy R. Mould
Keyword(s):  
Surface Brightness ◽  
Near Infrared ◽  
Virgo Cluster ◽  
Surface Brightness Fluctuations

scholarly journals Near-infrared surface brightness fluctuations and optical colours of Magellanic star clusters

2005 ◽  
Vol 363 (4) ◽  
pp. 1279-1289 ◽  
Author(s):  
R. A. González-Lópezlira ◽  
M. Y. Albarrán ◽  
M. Mouhcine ◽  
M. C. Liu ◽  
G. Bruzual-A. ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Near Infrared ◽  
Star Clusters ◽  
Surface Brightness Fluctuations

Surface brightness fluctuations and the distance to the Virgo Cluster

1989 ◽  
Vol 346 ◽  
pp. L57 ◽  
Author(s):  
John L. Tonry ◽  
Edward A. Ajhar ◽  
Gerard A. Luppino
Keyword(s):  
Surface Brightness ◽  
Virgo Cluster ◽  
Surface Brightness Fluctuations

scholarly journals Near-IR Imaging of Elliptical Galaxies

1995 ◽  
Vol 164 ◽  
pp. 443-443 ◽  
Author(s):  
M.A. Pahre ◽  
S. Djorgovski ◽  
K. Matthews ◽  
D. Shupe ◽  
R. De Carvalho ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Stellar Population ◽  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Fundamental Plane ◽  
Near Ir ◽  
Surface Brightness Fluctuations ◽  
Distance Indicator ◽  
Color Gradients ◽  
Optical Color

We have imaged more than thirty early-type galaxies in the K-band to investigate their stellar populations. Our surface brightness fluctuations (SBF) measurements for the nearest 14 galaxies produce a mean fluctuations magnitude in the K-band of The scatter in the Virgo cluster is small at 0.18 mag, which implies that infrared SBF is potentially a good distance indicator (Pahre & Mould 1994). Inspection of the simple stellar population tracks of Worthey (1994) suggests that a plot of the fluctuation color against broadband color (V – I) might be useful in discriminating between age and metallicity effects in elliptical galaxies. We have measured (r – K) color gradients for the entire sample utilizing three methods, two of them independent of sky-subtraction errors, as found in Sparks & Jørgensen (1993). Our color gradients are consistent with a mean metallicity gradient of 0.14 mag dex−1, which is somewhat smaller than that implied by optical color and line gradients alone, suggesting that age gradients may also be important. Finally, we have constructed an infrared Fundamental Plane (FP) which is consistent with its optical counterpart; continued work will determine if there is a significant change in the tilt of the FP between the optical and infrared.

Infrared Surface Brightness Fluctuations in Virgo Cluster Elliptical Galaxies

1996 ◽  
Vol 468 ◽  
pp. 519 ◽  
Author(s):  
Joseph B. Jensen ◽  
Gerard A. Luppino ◽  
John L. Tonry
Keyword(s):  
Surface Brightness ◽  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Surface Brightness Fluctuations

scholarly journals Cosmic distances from surface brightness fluctuations

2012 ◽  
Vol 8 (S289) ◽  
pp. 304-311 ◽  
Author(s):  
John P. Blakeslee
Keyword(s):  
Surface Brightness ◽  
Near Infrared ◽  
Hubble Space Telescope ◽  
Stellar System ◽  
Distance Scale ◽  
Wide Field ◽  
Coma Cluster ◽  
Infrared Wavelength ◽  
Surface Brightness Fluctuations ◽  
Advanced Camera For Surveys

AbstractHigh spatial-resolution measurements of surface brightness fluctuations (SBFs) with the Hubble Space Telescope (HST) provide the most precise distances available to early-type galaxies beyond the Local Group. The observable SBF magnitude in a given bandpass is a basic property of any stellar system, corresponding to a ratio of the first and second moments of the stellar luminosity function. Calibration of the method has presented challenges, but we now have an excellent empirical determination of how the SBF observable varies with galaxy color in broad bandpasses at the red end of the optical spectrum, and we are working towards a similar calibration for HST's Wide-Field Camera 3 in the near-infrared wavelength range, where the SBF magnitudes are considerably brighter. From HST Advanced Camera for Surveys data, we have determined the relative distances of the Virgo and Fornax clusters to within a precision of 2%, and resolved their internal structures. More recent measurements allow us to tie the Coma cluster, the standard of comparison for distant cluster studies, to the same precise distance scale. The SBF method can be calibrated in an absolute sense either empirically using Cepheids or theoretically based on stellar population models. The agreement between model and empirical zero points provides an independent confirmation of the Cepheid distance scale.

scholarly journals USING Hα MORPHOLOGY AND SURFACE BRIGHTNESS FLUCTUATIONS TO AGE-DATE STAR CLUSTERS IN M83

2011 ◽  
Vol 729 (2) ◽  
pp. 78 ◽  
Author(s):  
Bradley C. Whitmore ◽  
Rupali Chandar ◽  
Hwihyun Kim ◽  
Catherine Kaleida ◽  
Max Mutchler ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Star Clusters ◽  
Surface Brightness Fluctuations

scholarly journals The Surface Brightness Fluctuations and Globular Cluster Population of NGC 4478

1997 ◽  
Vol 483 (2) ◽  
pp. 745-753 ◽  
Author(s):  
Eric H. Neilsen, Jr. ◽  
Zlatan I. Tsvetanov ◽  
Holland C. Ford
Keyword(s):  
Globular Cluster ◽  
Surface Brightness ◽  
Surface Brightness Fluctuations
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