Papers › The Panchromatic Hubble Andromeda Treasury
The Panchromatic Hubble Andromeda Treasury
J. J. Dalcanton, B. F. Williams, D. Lang, T. R. Lauer, J. S. Kalirai, A. C. Seth, A. Dolphin, P. Rosenfield, D. R. Weisz, E. F. Bell, L. C. Bianchi, M. L. Boyer, N. Caldwell, H. Dong, C. E. Dorman, K. M. Gilbert, L. Girardi, S. M. Gogarten, K. D. Gordon, P. Guhathakurta, P. W. Hodge, J. A. Holtzman, L. Johnson, S. S. Larsen, A. Lewis, J. L. Melbourne, K. A. G. Olsen, H. -W. Rix, K. Rosema, A. Saha, A. Sarajedini, E. D. Skillman, K. Z. Stanek
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The Panchromatic Hubble Andromeda Treasury (PHAT) is an on-going HST Multicycle Treasury program to image ~1/3 of M31's star forming disk in 6 filters, from the UV to the NIR. The full survey will resolve the galaxy into more than 100 million stars with projected radii from 0-20 kpc over a contiguous 0.5 square degree area in 828 orbits, producing imaging in the F275W and F336W filters with WFC3/UVIS, F475W and F814W with ACS/WFC, and F110W and F160W with WFC3/IR. The resulting wavelength coverage gives excellent constraints on stellar temperature, bolometric luminosity, and extinction for most spectral types. The photometry reaches SNR=4 at F275W=25.1, F336W=24.9, F475W=27.9, F814W=27.1, F110W=25.5, and F160W=24.6 for single pointings in the uncrowded outer disk; however, the optical and NIR data are crowding limited, and the deepest reliable magnitudes are up to 5 magnitudes brighter in the inner bulge. All pointings are dithered and produce Nyquist-sampled images in F475W, F814W, and F160W. We describe the observing strategy, photometry, astrometry, and data products, along with extensive tests of photometric stability, crowding errors, spatially-dependent photometric biases, and telescope pointing control. We report on initial fits to the structure of M31's disk, derived from the density of RGB stars, in a way that is independent of the assumed M/L 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. (Abridged)
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