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Assigned ID: 319
----- Attempting Submission 1 (Fri Apr 10 00:43:21 GMT 2015) -----
HST Phase I Proposal 319 (apt_accretingprotoplanets_8apr2015.apt) successfully submitted.
Receipt: # 319-1
----- Attempting Submission 2 (Fri Apr 10 00:51:54 GMT 2015) -----
0
----- Attempting Submission 1 (Mon Jul 20 14:51:29 GMT 2015) -----
Imaging Accreting Protoplanets in the Young Cluster IC 348
Giant planets generate accretion luminosity as they form, much of which is radiated in the form of Halpha line emission at 6563 Ang. We propose a novel survey to identify accreting protoplanets in the young (~2 Myr) cluster IC 348. Our efficient program will target 225 cluster members, offering the first opportunity to study sub-Jovian-mass planets with direct imaging and characterize a population of planets generally inaccessible with ground-based adaptive optics imaging. This survey will clarify the origin of planetary-mass companions on ultra-wide orbits of hundreds of AU by probing masses of ~0.5-5 MJup, which is below the fragmentation limit set by disk instability and cloud fragmentation but should be heavily populated in the case of planet/core scattering. Based on the frequency of massive giant planets at wide separations, we also stand to increase the number of accreting 5-15 Mjup companions by ~50%. Finally, these data will have lasting value as a rich resource to study accretion, multiplicity, and the internal kinematics of IC 348.
The primary goal of this survey is to obtain deep imaging of as many IC 348 cluster members as possible with WFC3 with the narrow band Halpha filter. The most efficient way to do this is to target the densent part of the cluster in a mosaic pattern. Based on the WFC3 exposure time calculator, we achieve a S/N of 7 for an accreting 0.5 MJup planet in 1100 seconds with the F656N filter. We therefore require ~20 min per field. To avoid reacquisition overheads we will offset by 120" mid-orbit to obtain a second pointing. For each orbit this produces a 160"x240" rectangular coverage with an overlapping 160"x40" strip.
Each orbit will consist of a 6 min acquisition sequence, UVIS exposure overheads (2.6 min + 3x2.1 min), four 9.5 min exposures (a dithered pair at the initial pointing and another dithered pair after the 120" offset), and spacecraft maneuvers (2x0.5 min + 1.1 min for the offset), totaling 55 min.
We will use ACS/WFC to obtain F625-W-band observations of this region with as much overlap as our WFC3 observations as possible. Each field uses a WFC3-UVIS-MOSAIC-LINE pattern to dither over the inter-chip gap on both detectors.
EXTRA-SOLAR PLANETS
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