Unobstructed Observations of the Intrinsic Lyman-alpha Emission of Low-mass Stars

0 Assigned ID: 391 ----- Attempting Submission 1 (Fri Apr 07 04:21:56 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) successfully submitted. Receipt: # 391-1 ----- Attempting Submission 2 (Fri Apr 07 17:44:20 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) successfully submitted. Receipt: # 391-2 ----- Attempting Submission 3 (Fri Apr 07 23:08:50 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 4 (Fri Apr 07 23:10:04 GMT 2017) ----- ----- Attempting Submission 5 (Fri Apr 07 23:12:00 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 6 (Fri Apr 07 23:12:14 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 7 (Fri Apr 07 23:12:49 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 8 (Fri Apr 07 23:15:07 GMT 2017) ----- ----- Attempting Submission 9 (Fri Apr 07 23:16:43 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 10 (Fri Apr 07 23:20:27 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) failed submission. ----- Attempting Submission 11 (Fri Apr 07 23:23:47 GMT 2017) ----- ----- Attempting Submission 12 (Fri Apr 07 23:28:24 GMT 2017) ----- HST Phase I Proposal 391 (ATP1.apt) successfully submitted. Receipt: # 391-12 These proposed observations were fairly straightforward, as there is only one spectroscopic observing mode being used. Please let me know if there are any issues with this submitted phase II. Thanks! -866175571 ----- Attempting Submission 1 (Fri Jul 07 21:04:17 GMT 2017) ----- Unobstructed Observations of the Intrinsic Lyman-alpha Emission of Low-mass Stars Recent discoveries of potentially habitable planets around low-mass stars have highlighted the need for a comprehensive understanding of the radiation environments in which such planets reside. Of particular importance is knowledge of the FUV radiation, as low-mass stars are typically much more active than solar-type stars and the proximity of their habitable zones (HZs) can be one tenth the distance. Such radiation has the potential to strip away a planet's atmosphere and alter its photochemistry. The vast majority of the flux emitted by low-mass stars at FUV wavelengths occurs in the Lyman-alpha line at 1216 Angstroms. However, measuring a low-mass star's direct Lyman-alpha emission is almost always impossible because of the contaminating effects of interstellar hydrogen and geocoronal airglow. By focusing on two stars with very large radial velocities (>150 km/s), emission due to Lyman-alpha will be Doppler shifted away from the contaminating sources allowing for rare opportunities to measure the intrinsic Lyman-alpha emission for K and M stars. Such observations will be vital for empirically guiding UV upper-atmosphere models of low-mass stars and for informing us how accurate reconstructed Lyman-alpha emission and correlations from other UV diagnostic lines are for known planet hosts. We have identified the only K and M dwarfs for which a complete and accurate measurement of Lyman-alpha line profile is possible. We will use HST/STIS to observe unobstructed Lyman-alpha emission from two low-mass stars, Ross 825 (K3) and Ross 1044 (M2), with exceptionally large radial velocities (>150 km/s). For each target, we will first perform a STIS target acquisition sequence (ACQ/SEARCH and ACQ/IMAGE), which take # seconds. We will then use the STIS/G140M grating to observe the Lyman-alpha wavelength region with the 52" x 0.1" slit centered at 1222 Angstroms, settings used successfully in the past for K and M dwarfs. Stellar Physics Planets and Planet Formation 6 false true false false false false SUPPORTED STAR K V-IV NO J2000 J2000 NUV = 18.85 STAR M V-IV NO J2000 J2000 NUV = 21.59 STIS/FUV-MAMA Spectroscopic No No G140M 1222 STIS/FUV-MAMA Spectroscopic No No G140M 1222 1499461038156 /Users/aschneid10/Desktop/Proposals/HST/Cycle_25/High_RVs/ATP/OP-cache/ATP1-v01.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 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