0Assigned ID: 3078
----- Attempting Submission 1 (Thu Mar 24 22:47:50 GMT 2022) -----
HST Phase I Proposal 3078 successfully submitted.
Receipt: # 3078-1
----- Attempting Submission 2 (Fri Mar 25 23:36:45 GMT 2022) -----LONG STIS MAMA SU LIKELY TO INTERSECT THE SAACorrected phase constraints for the remaining visits, namely 2 and 4390207335----- Attempting Submission 1 (Wed Jun 22 22:57:08 GMT 2022) -----
----- Attempting Submission 2 (Wed Jan 04 19:43:01 GMT 2023) -----
----- Attempting Submission 3 (Wed Jan 25 18:47:46 GMT 2023) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 4 (Fri Mar 24 23:34:01 GMT 2023) -----
----- Attempting Submission 5 (Mon May 15 22:58:29 GMT 2023) -----APT won't let me run the target confirmation tool, but the target hasn't changedLyman alpha measurements from two mini Neptunes around one starMulti-planet systems are ideal for studying mass loss because the two planets share the same high-energy irradiation history and similar formation histories. TOI 560c is the outer companion of TOI 560b, the first young mini Neptune with measured helium absorption from its escaping atmosphere. We propose to observe this planet with STIS/G140M to measure Lyman alpha absorption from its outflow. Atmospheric escape is especially interesting to probe in the young mini Neptune regime because it predominantly occurs in the active youth of a star's life, creating the radius gap which divides super-Earths (1--1.8 REarth) from mini-Neptunes (2--3 REarth). These observations will allow us to test recently published theoretical models of Lyman alpha absorption, in particular differentiating between different regimes of mass loss and constraining the wind launching mechanism. The TOI 560c observations, combined with existing Ly alpha and helium observations of TOI 560b, will enable a comparative study of mass loss from planets in the same system.Our program will observe 3 transits of HD 73583c. Each transit observation will consist of 5 consecutive orbits, of which 2 are in-transit. We set the phase requirements to +- 0.5 hours for all visits. We may adjust the phase requirements as visits are completed to try to maximize the phase coverage. The ephemeris uncertainty is around 6 minutes at the end of the year.
We planned our observations so that the first orbit of each visit has an ACQ and ACQ-PEAKUP exposure, followed by a science exposure and wavelength calibration. Subsequent orbits only have a science exposure and a wavelength calibration exposure, with no ACQ or ACQ-PEAKUP. Because the few minutes' difference in orbital visibility due to precession has minimal impact on our science, we change the schedulability parameter from 30 to 90 to make scheduling easier. If possible, we kindly ask the Program Coordinator to expand our science observations to fill up the entire orbital visibility for the orbits that are actually scheduled.
Reduced gyro mode impacts our program by limiting the number of scheduling opportunities. Otherwise, we do not forsee major impacts from RGM.Michael Zhang studies exoplanet atmospheres and was the PI of program 16319, which measured Ly alpha outflow from another mini Neptune, and program 16779, which looks for Ly alpha outflow from TOI 560b. He has additionally studied helium mass loss using Keck/NIRSPEC.
Heather Knutson has extensive expertise in many areas of exoplanet atmosphere observations, especially with HST and Spitzer.
James Owen is an expert in the theoretical understanding of mass loss, and has recently written a paper on the fundamentals of Ly alpha transit observations (Owen et al 2022). He has also written seminal papers in the field (e.g. Owen & Wu 2013), in addition to multiple review papers (e.g. Owen 2019).
Fei Dai is an expert on numerical modelling of exoplanet mass loss, especially from small planets such as mini Neptunes.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARK V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.TOI-560J2000J2000STIS/FUV-MAMASpectroscopicNoNoG140M1222The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.1682658411000102.63749237185579(Tic-Visit
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