0Assigned ID: 1589
----- Attempting Submission 1 (Fri Mar 01 18:00:01 GMT 2013) -----
----- Attempting Submission 3 (Sat Mar 02 01:43:30 GMT 2013) -----Reduced exposure times from 2256 to 1976 sec to widen scheduling windows-14292316----- Attempting Submission 1 (Thu Jun 13 16:20:38 GMT 2013) -----
----- Attempting Submission 2 (Tue Jun 18 17:21:14 GMT 2013) -----The Eccentric Debris Ring Around HD 202628: Signs of Planetary PerturbationsDebris disks are the signposts of planetary systems: collisions among asteroidal and cometary parent bodies maintain the observed dust population against losses to radiation pressure, stellar wind, and P-R drag. Disk images establish the size scale of an exoplanetary system. They can reveal central holes, rings, gaps, warps, and asymmetries in the dust distribution that indicate the presence of planetary perturbers. In 2011 we discovered a large debris disk in HST coronagraphic images. HD 202628's disk is an eccentric ring with a sharp inner edge and cleared central zone - only the third such system ever imaged, and with the faintest surface brightness ever for a disk seen in scattered light. Key differences for this object are its larger ring diameter and eccentricity, and the solar-type of the host star. The discovery image represents only two orbits of integration and suffers from low overall signal to noise. We propose a series of deeper imaging observations with the STIS coronagraph over multiple roll angles. Important parameters of the ring to be clarified by the new data are the sharpness of the ring inner edge, its outermost radial extent, and the strength of radial/azimuthal brightness density gradients. From these we can derive constraints on the mass and orbit of the perturbing planet. The outcome of our program will be the best evidence to date for a distant planetary companion to a sun-like star.We will observe the debris disk around the star HD 202628 with the STIS coronagraph. We will observe the target at 9 different roll orientations of the telescope to improve the diversity needed to perform the iterative PSF subtraction needed to reveal the faint disk. There will be three epochs of observations, each composed of three contiguous orbits. Within each epoch, the three orbits are separated by spacecraft rolls of 15 degrees from each other. The first orbit of each epoch is separated by 45 degrees from that of the previous epoch.
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