The Next Generation Virgo Cluster Survey (NGVS). XVIII. Measurement and Calibration of Surface Brightness Fluctuation Distances for Bright Galaxies in Virgo (and Beyond) [PDF]
We describe a program to measure surface brightness fluctuation (SBF) distances to galaxies observed in the Next Generation Virgo Cluster Survey (NGVS), a photometric imaging survey covering 104 deg2 of the Virgo cluster in the u*, g, i, and z bandpasses
M. Cantiello+9 more
semanticscholar +1 more source
Infrared Surface Brightness Fluctuations of Magellanic Star Clusters [PDF]
We present surface brightness fluctuations (SBFs) in the near--IR for 191 Magellanic star clusters available in the Second Incremental and All Sky Data releases of the Two Micron All Sky Survey (2MASS), and compare them with SBFs of Fornax Cluster galaxies and with predictions from stellar population models. Our goals are twofold.
Michael C. Liu+2 more
openaire +3 more sources
A novel method for tracking structural changes in gels using widely accessible microcomputed tomography is presented and validated for various hydro‐, alco‐, and aerogels. The core idea of the method is to track positions of micrometer‐sized tracer particles entrapped in the gel and relate them to the density of the gel network.
Anja Hajnal+3 more
wiley +1 more source
MEASURING INFRARED SURFACE BRIGHTNESS FLUCTUATION DISTANCES WITH HST WFC3: CALIBRATION AND ADVICE [PDF]
We present new calibrations of the near-infrared (near-IR) surface brightness fluctuation (SBF) distance method for the F110W ( J 110 ?> ) and F160W ( H 160 ?> ) bandpasses of the Wide Field Camera 3 Infrared Channel (WFC3/IR) on the Hubble Space ...
J. Jensen+7 more
semanticscholar +1 more source
Towards gradient detection of surface brightness fluctuations
Abstract: Surface Brightness Fluctuations (SBF) magnitudes have been proved as a potential tool for the study of composite stellar populations in galaxies. In particular, we focus on the detection of metal-poor secondary components in metal-rich dominated early type galaxies. Our current work consists in studying radial profiles of SBFs, hence we study
Pablo Rodríguez Beltrán+3 more
openaire +2 more sources
Observations of surface-brightness fluctuations in Virgo
VRI photometric observations of surface-brightness fluctuation in 13 Virgo Cluster galaxies, M32, and NGC 3379, obtained using an 800 x 800 CCD array on the 4-m telescope at KPNO during March 1989, are reported. The data-reduction techniques are described in detail, and the results are presented in tables and graphs.
Gerard A. Luppino+2 more
openaire +2 more sources
Measuring Distances Using Infrared Surface Brightness Fluctuations [PDF]
Surface brightness fluctuations (SBFs) are much brighter in the IR than they are at optical wavelengths, making it possible to measure greater distances using IR SBFs. We report new K' (2.1 micron) SBF measurements of 9 galaxies in the Fornax and Eridanus clusters using a 1024^2-pixel HgCdTe array.
Joseph B. Jensen+3 more
openaire +3 more sources
Measuring Distances to Low-luminosity Galaxies Using Surface Brightness Fluctuations [PDF]
Abstract We present an in-depth study of surface brightness fluctuations (SBFs) in low-luminosity stellar systems. Using the MIST models, we compute theoretical predictions for absolute SBF magnitudes in the LSST, HST ACS/WFC, and proposed Roman Space Telescope filter systems.
Johnny P. Greco+4 more
openaire +3 more sources
Surface brightness fluctuations as primary and secondary distance indicators [PDF]
The surface brightness fluctuations (SBF) method measures the variance in a galaxy's light distribution arising from fluctuations in the numbers and luminosities of individual stars per resolution element. Once calibrated for stellar population effects, SBF measurements with HST provide distances to early-type galaxies with unrivaled precision. Optical
openaire +5 more sources
Detection of CFIRB with AKARI/FIS Deep Observations [PDF]
The Cosmic Far-Infrared Background (CFIRB) contains information about the number and distribution of contributing sources and thus gives us an important key to understand the evolution of galaxies.
Chris P. Pearson+33 more
core +1 more source