0Assigned ID: 4712
----- Attempting Submission 1 (Wed May 24 22:09:10 GMT 2023) -----
HST Phase I Proposal 4712 successfully submitted.
Receipt: # 4712-1Loosened phase constraints for Visits 02 and 04.-83995900----- Attempting Submission 1 (Wed Sep 06 16:56:15 GMT 2023) -----
HST Phase II Proposal 17534 successfully submitted.
Receipt: # 17534-1
----- Attempting Submission 2 (Tue Sep 12 17:46:19 GMT 2023) -----
HST Phase II Proposal 17534 successfully submitted.
Receipt: # 17534-2
----- Attempting Submission 3 (Tue Sep 12 18:55:57 GMT 2023) -----
----- Attempting Submission 4 (Thu Oct 12 14:10:17 GMT 2023) -----
----- Attempting Submission 5 (Fri Oct 27 15:01:17 GMT 2023) -----
----- Attempting Submission 6 (Thu Apr 17 00:19:31 GMT 2025) -----A young burping planet: characterizing the variable atmospheric escape of the exciting AU Mic bAtmospheric escape is the prevailing evolutionary theory that explains current exoplanet demographics - pertaining to the most common exoplanet types, short-period sub-Neptunes and super-Earths, in particular. Two 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 b is the 4.2 Earth radius inner planet orbiting with a period of 8 days. The planet's youth, high levels of X-ray and UV radiation, and proximity to its bright host indicate this planet is likely experiencing atmospheric mass loss. Previous STIS UV observations of this planet show a highly variable Lyman-alpha transit, going from no detected planetary outflow to detected. Even more strange, the detection occurs before the white-light transit of the planet, meaning the neutral hydrogen outflow is moving ahead of the planet. This could be explained by 1) variable photoionization of the outflow, or 2) turbulent interactions with the stellar wind environment that cause a "burping" of the outflow. We propose for two additional transits of this planet to test this hypothesis. Observing the extreme behavior of this young planet will provide critical constraints on atmospheric escape models.We will observe 2 AU Mic b transits with STIS FUV-MAMA E140M. Each transit will comprise 2 HST visits of 3 and 5 orbits each (8 orbits per transit). An example transit is shown in Figure 3. Five back-to-back orbits in a single visit can be scheduled to avoid crossings of the South Atlantic Anomaly, and a single visit provides improved stability when compared to re-acquiring the target over multiple visits. The first visit of each transit will comprise 3 orbits 8-12 hours before the white-light mid-transit, capturing the extent of a leading arm of planetary material. The second visit will comprise 5 orbits capturing six hours centered on the white-light mid-transit. We will also observe 2 orbits loosely scheduled over 24 hours before each of the 2 transits. This will provide a baseline observation of the unocculted host star to assess whether there have been long-term changes in the stellar activity. Our entire observing plan consists of 20 orbits.Keighley Rockcliffe has analyzed several Lyman-alpha transits of young exoplanets (GO-14615 and -15836) and is the PI of GO-17219 which will provide AU Mic c Lyman-alpha transits. She is an expert in observationally characterizing atmospheric escape in young exoplanet systems.
Dr. Elisabeth Newton is an expert on M dwarf systems, with a particular focus on young systems with exoplanets.
Allison Youngblood is the PI of multiple HST programs to study the UV emission from late-type stars, including a large survey of the UV emission from JWST Cycle 1 transiting exoplanet host stars (GO-16701) and a Lyman alpha transit of TOI-1231b (GO-16700). She is experienced in analyzing Lyman alpha emission from M dwarfs.
Peter Plavchan is an expert on the AU Mic planets and observationally constraining their properties.
Dr. Mann is an expert on the fundamental properties of late-type and young stars. He also has done extensive work on the discovery and characterization of young transiting planets. He is co-PI of the THYME survey and the PI of a JWST Cycle 1 program on the 17 Myr transiting planet HIP67522 b.
Pa Chia Thao is a graduate student who has had extensive experience using ground- and space-based telescopes (HST, Spitzer) to study the transmission spectrum of young planets.
Adina Feinstein is an expert in transit observations of young planets, stellar activity, and is the lead software developer for several time-series photometry extraction and analyses, and HST data reduction pipelines.
Patrick Lowrance is a senior scientist at Caltech/IPAC and is currently the lead of the Roman Space Telescope effort at IPAC. He has studied exoplanet transits and direct imaging and has been a Co-I on several HST and Spitzer programs to study exoplanet transits including AU Mic (HST 15835, 14241, 13178, 13176 and Spitzer 14241, 14214).
Hans Mueller has an extensive background in modeling plasma/neutral interaction regions like astrospheres carved out of the interstellar medium by stellar winds. He models the interaction of stellar winds with the neutral evaporating atmosphere of close-in exoplanets.
Ethan Schreyer and James Owen are experts in modeling atmospheric escape on various types of exoplanets.
PI Rockcliffe and Newton have institutional access to the 1.3 and 2.4m telescopes at MDM, Dartmouth has a 25% share of both telescopes. Newton has access to LCO as an "LCO extended family" member from TAC service. Team members Mann and Newton have had multiple successful LCO programs to support space-based observations with TESS and HST. Mann has institutional access to SOAR.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalseSUPPORTEDSTARM V-IVPRE-MAIN SEQUENCE STARJ2000J2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode./private/var/folders/jj/gh_vs4h933g07vk6bs52gxnwf2ybxw/T/OPVisit16619598099009631829.xmlTwo exposures 24 hours before transit to observe the unocculted star.1716411850000260.75816570344386(Tic-Visit
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