Assigned ID: 762
----- Attempting Submission 1 (Fri Feb 24 21:51:20 GMT 2012) -----
----- Attempting Submission 1 (Mon Jul 02 19:50:29 GMT 2012) -----
STIS Coronagraphy of Bright New Debris Disks from the WISE All-Sky Survey
Debris disks trace the collisional breakdown of asteroid and comet parent bodies orbiting nearby main sequence stars. While present in ~15% of FGK stars - as diagnosed by infrared excess measurement by IRAS, ISO, and Spitzer - only 6 debris disks have been detected in scattered light around late-type stars. The detectability of debris disks in scattered light trends strongly with the magnitude of their infrared excess, so progress in this field depends on identifying new stars with strong excess. The Wide-Field Infrared Survey Explorer (WISE) has recently completed new, sensitive all-sky mapping in the 3.3, 4.6, 12, and 22 micron bands. Association of the WISE sources to Hipparcos stars has led to the identification of 348 nearby main sequence stars with robustly detected warm 22 micron excesses not previously known. We propose STIS coronagraphic imaging for seven of the brightest debris disks that WISE has found in association with solar-type and intermediate mass stars within 120 pc. All seven have excesses stronger than the successfully imaged disk of HD 107146, and two have disks as bright at Beta Pic. Our goal is to obtain the first resolved images of these disks at ~5 -15 AU resolution, define the disk sizes and orientations, and uncover disk substructures indicative of planetary perturbations. The results should double the number of debris disks imaged around late-type stars, opening a wider window into the structure of planetary systems.
We are using the STIS coronagraph to image circumstellar debris disks around 7 stars with WISE-detected excesses. Each target is observed in two back-to-back orbits, with the two orbits separated by ~30 deg in telescope roll. The two rolls allow separation of the disk and instrumental components of the image using an interative algorithm. At the beginning of each orbit the usual STIS coronagraph acquisition is done. Then, a ~2000 sec exposure (split into multiple shorter CR-splits) is taken with the star located behind the coronagraphic wedge at WEDGEA1.0. Each orbit uses the same image sequence. Exposure times and CR-splits are chosen to minimize, but not completely prevent, saturation.
ISM AND CIRCUMSTELLAR MATTER
12
false
0.0
0.0
false
false
false
false
SUPPORTED
STAR
F3-F9
HIP-62657
J2000
J2000
STAR
F3-F9
HIP-117481
J2000
J2000
STAR
F3-F9
HIP-77441
J2000
J2000
STAR
F0-F2
HIP-52947
J2000
J2000
STAR
F0-F2
HIP-67497
J2000
J2000
STAR
A0-A3 V-IV
HIP-84881
J2000
J2000
STAR
B6-B9.5 V-IV
HIP-26062
J2000
J2000
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
STIS/CCD
Imaging
Yes
No
WEDGEA1.0
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