THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY

By J. J. Dalcanton, Benjamin F. Williams, Dustin Lang, Tod R. Lauer, J. Kalirai, Anil Seth, A. Dolphin, P. Rosenfield, D. Weisz, Eric F. Bell and 25 more. 2012

325 citations recorded by the source corpus.

The Panchromatic Hubble Andromeda Treasury is an ongoing Hubble Space Telescope Multi-Cycle Treasury program to image ∼1/3 of M31's star-forming disk in six filters, spanning from the ultraviolet (UV) to the near-infrared (NIR). We use the Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) to resolve the galaxy into millions of individual stars with projected radii from 0 to 20 kpc. The full survey will cover a contiguous 0.5 deg2area in 828 orbits. Imaging is being obtained in the F275W and F336W filters on the WFC3/UVIS camera, F475W and F814W on ACS/WFC, and F110W and F160W on WFC3/IR. The resulting wavelength coverage gives excellent constraints on stellar temperature, bolometric luminosity, and extinction for most spectral types. The data produce photometry with a signal-to-noise ratio of 4 at mF275W = 25.1, mF336W = 24.9, mF475W = 27.9, mF814W = 27.1, mF110W = 25.5, and mF160W = 24.6 for single pointings in the uncrowded outer disk; in the inner disk, however, the optical and NIR data are crowding limited, and the deepest reliable magnitudes are up to 5 mag brighter. Observations are carried out in two orbits per pointing, split between WFC3/UVIS and WFC3/IR cameras in primary mode, with ACS/WFC run in parallel. All pointings are dithered to produce Nyquist-sampled images in F475W, F814W, and F160W. We describe the observing strategy, photometry, astrometry, and data products available for the survey, along with extensive testing of photometric stability, crowding errors, spatially dependent photometric biases, and telescope pointing control. We also report on initial fits to the structure of M31's disk, derived from the density of red giant branch stars, in a way that is independent of assumed mass-to-light ratios and is robust to variations in dust extinction. These fits also show that the 10 kpc ring is not just a region of enhanced recent star formation, but is instead a dynamical structure containing a significant overdensity of stars with ages >1 Gyr.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/19e9ebbe0792ac0ad442e071367b4f0cb7dcfc86

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Citations in the corpus

The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library (2018, background): “The M31 ancillary program targets regions in M31 where the underlying physical properties are wellconstrained from resolved stellar population analyses, provided by the Panchromatic Hubble Andromeda Treasury (PHAT; Dalcanton et al. 2012).”
Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates (2018, methodology): “…survey of the entire ∼2 deg2 WFIRST microlensing survey fields, in a similar manner to the Panchromatic Hubble Andromeda Treasury (PHAT) survey (Dalcanton et al. 2012), would require ∼1500 HST pointings, or ∼750 JWST NIRCAM pointings, and would provide immense legacy value for what will…”
On the fraction of star formation occurring in bound stellar clusters (2012, background): “These include M31, which is currently undergoing an extensive survey by the PHAT team (Dalcanton et al. 2012; Johnson et al. 2012) under the Hubble Space Telescope treasury programme.”
A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team (2021, methodology): “A much larger sample of M31 Cepheids is available from the HST PHAT Treasury program (Dalcanton et al. 2012), but the filters used to observe it do not correspond to the three used here, limiting its utility.”
THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. X. ULTRAVIOLET TO INFRARED PHOTOMETRY OF 117 MILLION EQUIDISTANT STARS (2014, methodology): “These single-CCD DOLPHOT catalogs were culled for artifacts using the same criteria as those used for the single-camera photometry in Dalcanton et al. (2012a).”
The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s (2019, methodology): “PHAT (Dalcanton et al. 2012) imaged 0.5 deg2 of the Andromeda galaxy in six bands; 414 orbits (2360 ksec) were used for F110W and F160W observations reaching depths of about 25.5 and 24.6, respectively, in the uncrowded outer disk.”
CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITH HST/COS AND HST/STIS ABSORPTION-LINE SPECTROSCOPY (2012, background): “Since the star formation histories of local dwarfs (Mateo 1998; Skillman 2005) as well as the histories of our Galaxy and M31 (Dalcanton et al. 2012) are now being constructed, it may be possible in the near future to construct a chemical evolution model for the entire Local Group assuming overall m”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “On the observational front, large quantities of precise data from recent and ongoing space- and ground-based programs have initiated an explosive growth in fields such as asteroseismology (e.g., CoRoT; Baglin et al. 2006, Kepler; Gilliland et al. 2010), time-domain astronomy (e.g., Palomar Transient”
ANDROMEDA'S DUST (2013, background): “The 11.2 kpc ring coincides with a peak in the H i 21 cm emission, a ring of star formation (seen in Hα; Devereux et al. 1994), and a ∼40% overdensity of stars with ages >1 Gyr (Dalcanton et al. 2012).”
THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, background): “…USA 8 Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA tions into individual stars (e.g., Dalcanton et al. 2012) or using integral-field spectroscopy, trying to directly reconstruct their individual formation history.”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “Analyses of the HST PHAT Treasury data (Dalcanton et al. 2012) by Riess et al. (2012), Kodric et al. (2015), and Wagner-Kaiser et al. (2015) used samples of Cepheids discovered from the ground with NIR and optical magnitudes from HST to derive low-dispersion P–”