THE ACS NEARBY GALAXY SURVEY TREASURY

By J. J. Dalcanton, B. Williams, Anil Seth, A. Dolphin, J. Holtzman, K. Rosema, E. Skillman, A. Cole, L. Girardi, Stephanie M. Gogarten and 17 more. 2007

406 citations recorded by the source corpus.

The ACS Nearby Galaxy Survey Treasury (ANGST) is a systematic survey to establish a legacy of uniform multi-color photometry of resolved stars for a volume-limited sample of nearby galaxies (D < 4 Mpc). The survey volume encompasses 69 galaxies in diverse environments, including close pairs, small and large groups, filaments, and truly isolated regions. The galaxies include a nearly complete range of morphological types spanning a factor of ∼104 in luminosity and star formation rate. The survey data consist of images taken with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST), supplemented with archival data and new Wide Field Planetary Camera 2 (WFPC2) imaging taken after the failure of ACS. Survey images include wide field tilings covering the full radial extent of each galaxy, and single deep pointings in uncrowded regions of the most massive galaxies in the volume. The new wide field imaging in ANGST reaches median 50% completenesses of mF475W = 28.0 mag, mF606W = 27.3 mag, and mF814W = 27.3 mag, several magnitudes below the tip of the red giant branch (TRGB). The deep fields reach magnitudes sufficient to fully resolve the structure in the red clump. The resulting photometric catalogs are publicly accessible and contain over 34 million photometric measurements of >14 million stars. In this paper we present the details of the sample selection, imaging, data reduction, and the resulting photometric catalogs, along with an analysis of the photometric uncertainties (systematic and random), for both ACS and WFPC2 imaging. We also present uniformly derived relative distances measured from the apparent magnitude of the TRGB.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1f71cf71aa3b36600dfb236a398afb096d36281d

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Citations in the corpus

CONVERTING FROM 3.6 AND 4.5 μm FLUXES TO STELLAR MASS (2012, methodology): “…histories (SFHs) recovered from synthesizing the stellar optical color-magnitude diagrams (CMDs) that are available for nearby galaxies (e.g. Harris & Zaritsky 2004, 2009; Dalcanton et al. 2009) to calculate the stellar mass on a region-by-region basis and use those measurements to calibrate F3.”
A GALEX ULTRAVIOLET IMAGING SURVEY OF GALAXIES IN THE LOCAL VOLUME (2010, methodology): “To extend the coverage of the galaxy population to dwarf spheroidals, dwarf ellipticals and the faintest irregular galaxies, such systems from the ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009) were also targeted for both GALEX and Spitzer observations.”
Fitting the integrated spectral energy distributions of galaxies (2010, methodology): “…surveys which have acquired groundbased narrowband Hα (Kennicutt et al. 2008), GALEX ultraviolet (Lee et al., in prep.) and HST resolved stellar population imaging (Dalcanton et al. 2009), by collecting Spitzer IRAC and MIPS infrared imaging for a sample of 258 galaxies derived from these programs.”
THE LARGE-SCALE STRUCTURE OF THE HALO OF THE ANDROMEDA GALAXY. I. GLOBAL STELLAR DENSITY, MORPHOLOGY AND METALLICITY PROPERTIES (2013, methodology): “In this endeavor the Hubble Space Telescope has been a powerful tool in recent years (see, e.g., Dalcanton et al. 2009, and references therein).”
THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. X. ULTRAVIOLET TO INFRARED PHOTOMETRY OF 117 MILLION EQUIDISTANT STARS (2014, background): “As our deepest bands are the same bands and are of comparable depth to Dalcanton et al. (2009), we expect our background galaxy contamination density to be similar.”
THE ACS NEARBY GALAXY SURVEY TREASURY. IX. CONSTRAINING ASYMPTOTIC GIANT BRANCH EVOLUTION WITH OLD METAL-POOR GALAXIES (2010, methodology): “Selecting AGB and RGB stars To identify the location of RGB stars, we adopted the magnitude of the TRGB (mTRGB) from Dalcanton et al. (2009), who identified the TRGB in uncrowded low extinction regions of each galaxy using the edge-detection method of Méndez et al. (2002).”
CONFIRMATION OF FAINT DWARF GALAXIES IN THE M81 GROUP (2013, methodology): “For M81 galaxies not part of our HST follow-up, we use ACS data from the ANGST survey (Dalcanton et al. 2009) taken in similar passbands and reaching about 1 mag deeper.”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, background): “/M 〉) = 7.6), the star-forming dwarfs from the ACS Nearby Galaxy Survey Treasury program (ANGST; Dalcanton et al. 2009; Weisz et al. 2011a,b) have SFHs that most closely resembled the highest mass galaxies in the SDSS sample (log(〈M?”
THE GHOSTS SURVEY. I. HUBBLE SPACE TELESCOPE ADVANCED CAMERA FOR SURVEYS DATA (2011, methodology): “We configured dolphot with parameters similar to those used in the ACS Nearby Galaxy Survey Treasury program (Dalcanton et al. 2009, hereafter ANGST). dolphot initially aligns the dithered exposures using bright stars in common between the frames; generally, the alignment is good to ∼0.”
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, methodology): “For Sextant A the errors are determined in the same way, but using the data from Dalcanton et al. (2009). c© 2014 RAS, MNRAS 000, 1–19”
THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME (2011, methodology): “The ACS Nearby Galaxy Survey Treasury (ANGST; Dalcanton et al. 2009) was designed to help remedy this situation.”