The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk, using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved into more than 100 million stars, enabling a wide range of scientific endeavors.
The PHAT observations are grouped into 23 "bricks", each listed under a different proposal ID. Each brick consists of a 3x6 array of pointings, producing complete coverage in the UV, optical, and NIR. Each brick is observed as two 3x3 "half bricks", with observations taken ~6 months apart. In the first observing season, a 3x3 half brick of WFC3 pointings is completed in primary, while parallel observations produce a highly overlapping 3x3 tile of ACS observations in the adjacent half brick. After 6 months, the telescope can be rotated by 180 degrees from the original orientation, such that the primary WFC3 pointings cover the area that was tiled by ACS in the first season, and vice versa. Each pointing is observed for 2 orbits, using the 2 WFC3 cameras for one orbit each.
Filters: F275W+F336W (WFC3/UVIS), F475W+F814W (ACS/WFC), F110W+F160W (WFC3/IR)
Depth: UVIS data reach a magnitude limit of ~25 in F275W and F336W. ACS data reach maximum depths of ~28 magnitudes in F475W and ~27 magnitudes in F814W in the uncrowded outer disk. In these same regions, WFC3/IR data reach maximum depths of ~26.5 and ~25.5 in F110W and F160W, respectively. However, the depth is crowding limited in the optical and NIR, and thus is a strong function of radius. As a result, photometry in the inner bulge fields is far shallower.
All available catalogs are listed at http://archive.stsci.edu/vo/mast_services.html.
The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk,
using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved
into more than 100 million stars, enabling a wide range of scientific endeavors.
Space Telescope A901/902 Galaxy Evolution Survey (STAGES)
Short Name:
HST.STAGES
Date:
23 Jul 2020 19:41:16
Publisher:
Space Telescope Science Institute Archive
Description:
STAGES is a large area (0.5x0.5 degree) survey of the complex Abell 901(a,b)/902 multiple-cluster system at z=0.165. An 80-tile imaging mosaic in F606W was conducted in HST cycle 13 with the HST/ACS instrument.
The Space Telescope Imaging Spectrograph (STIS) was installed in HST on Feb. 14, 1997, replacing the GHRS spectrograph. STIS provides spectra and images at ultraviolet and visible wavelengths, probing the Universe from our solar system out to cosmological distances.
The WFPC2 is used to obtain high resolution images of astronomical objects over a relatively wide field of view and a broad range of wavelengths (1150 to 11,000 Å).
The WF/PC-1 was used from April 1990 to November 1993, to obtain high resolution images of astronomical objects over a relatively wide field of view and a broad range of wavelengths (1150 to 11,000 Angstroms).
