0Assigned ID: 3363
----- Attempting Submission 1 (Fri Mar 25 17:40:43 GMT 2022) -----STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUMEUpdated schedulability to 100. Updated target coordinate epoch to 2000 (previously listed as 2016). "New target" now listed as V-AU-MIC2.179367837----- Attempting Submission 1 (Mon Jul 11 16:15:53 GMT 2022) -----
HST Phase II Proposal 17219 successfully submitted.
Receipt: # 17219-1
----- Attempting Submission 2 (Fri Oct 14 17:46:37 GMT 2022) -----
HST Phase II Proposal 17219 successfully submitted.
Receipt: # 17219-2
----- Attempting Submission 3 (Wed Nov 16 20:28:09 GMT 2022) -----The 4 errors correspond to potentially high data volumes during the two HST visits. I have been assured that HST can handle this since it does not receive many high data volume requests.The evaporating atmosphere of a planet in the young bright multiplanet system AU MicTwo planets have been detected around the 23 Myr pre-main sequence M dwarf AU Mic; their known age makes them good probes for early stages of exoplanet evolution. AU Mic c is the 2.56 Earth radius outer planet orbiting with a period of 18.9 days. It has a mass of about 20 Earth masses. The planet's relatively low density, high levels of X-ray and UV radiation, proximity to its bright host, and its youth indicate this planet is likely experiencing atmospheric mass loss. This makes it an excellent target for STIS UV observations to look for escaping neutral hydrogen during transit at Lyman-alpha. AU Mic b, even closer to its host, already has similar observations, so observations of AU Mic c will provide the opportunity to explore atmospheric escape process for multiple planets in the same system. With STIS observations of AU mic c, we can constrain the planet's mass loss rate and potentially the dynamics of the upper atmosphere. Observations of AU Mic c will provide much needed additional data to test atmospheric escape models.This program aims to detect the transit of AU Mic c in the Lyman-alpha emission line of its host using HST/STIS. We will observe 2 transits, each comprised of a single visit of 5 orbits (10 orbits total) using STIS FUV-MAMA E140M. The 5 back-to-back orbits in a single visit can be scheduled to avoid crossings of the South Atlantic Anomaly. Both 5-orbit visits will probe the same regions of the planet transit: 2 orbits capturing before and after the white-light transit, with 1 orbit at the transit midpoint. With this observing strategy, we will have a full view of the exosphere transit. Two orbits per transit are loosely scheduled between 5 to 24 hours before each transit (4 orbits total). This will provide a baseline observation of the unocculted host star.Keighley Rockcliffe works extensively with Lyman-alpha transits of young exoplanets. Dr. Elisabeth Newton is an expert on M dwarf systems, with a particular focus on young systems. Emily Gilbert, Dr. Peter Plavchan, and Dr. Thomas Barclay have all worked with the AU Mic system. Dr. Allison Youngblood is an expert in M dwarfs, and their UV radiation in particular. Girish Duvvuri also works on stellar radiation from a modeling perspective. Dr. Hans Mueller works on hydrodynamical modeling of plasmas, including stellar and planetary winds. Dr. Peter Gao and Dr. Eric Lopez are both exoplanet experts, with a particular emphasis on exoplanet atmospheres.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMPRE-MAIN SEQUENCE STARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMPRE-MAIN SEQUENCE STARJ2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425Timing link suitability includes constraints ([02 After 01 by 0.2 to 1.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.2 orbits (5 -24 hours) before AU Mic c transit to obtain baseline from unocculted AU Mic. 1 of 2 visits to capture the first transit of AU Mic c.166754585200073.0(Tic-Visit
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