0 Assigned ID: 675 ----- Attempting Submission 1 (Wed Jan 30 22:44:50 GMT 2019) ----- HST Phase I Proposal 675 (LHS3844_HSTCycle26Mid.apt) successfully submitted. Receipt: # 675-1 ----- Attempting Submission 2 (Thu Jan 31 00:01:53 GMT 2019) ----- HST Phase I Proposal 675 (LHS3844_HSTCycle26Mid.apt) successfully submitted. Receipt: # 675-2 ----- Attempting Submission 3 (Thu Jan 31 00:57:34 GMT 2019) ----- HST Phase I Proposal 675 (LHS3844_HSTCycle26Mid.apt) successfully submitted. Receipt: # 675-3 ----- Attempting Submission 4 (Thu Jan 31 01:00:45 GMT 2019) ----- For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. 0 ----- Attempting Submission 1 (Tue Apr 16 19:35:59 GMT 2019) ----- For the COS G130M, CENWAVE 1291A, only FP-POS 3 & 4 are allowed. We require this CENWAVE to achieve our science goals of covering the full UV spectrum of LHS 3844 with HST/COS. For COS G160M and COS G230L we vary FP-POS after each exposure. The recently discovered strongly irradiated terrestrial exoplanet LHS3844b presents a first opportunity to understand the impact of the UV environment produced by an M dwarf star on planetary atmospheric escape processes. Astronomers were recently awarded 100 hours with Spitzer to measure the infrared phase curve of LHS 3844b and determine if this planet has retained an atmosphere. Whether we learn that the planet has retained or lost its atmosphere, we argue that it essential to constrain the UV spectrum of its host star, LHS 3844, which in turn will allow us to test models of UV-driven hydrodynamic escape. Due to the faintness of LHS 3844, it would be prohibitive to directly observe the UV spectrum to high precision over the full wavelength range. Instead, we propose to leverage the results of the MUSCLES treasury program and use line-to-line emission correlations in order to obtain a robust estimate of the UV spectrum of LHS 3844 from only 10 spacecraft orbits. We will use HST/COS to observe the full UV spectrum, from 1150-3200A, of LHS 3844, an M4.5 star at a distance of 14.9 pc (M = 0.151 Solar masses, R = 0.189 Solar radii). All data will be obtained in TIME-TAG mode so that we monitor the star's activity during the exposures, which we can compare to previous flare frequency distributions for M dwarfs derived from other HST/COS spectra (Loyd et al., 2018). We will use the FLASH=YES setting to maximize exposure time on target. We vary FP-POS as much as possible for the gratings we use. We base our COS observing strategy on the successful MUSCLES (GO Program 13650) and Mega-MUSCLES (GO Program 15071) surveys. We scaled the MUSCLES HST/COS data of the mid-M dwarf GJ 1214 to the distance and stellar radius of LHS 3844, and used this scaled data as an input to the Space Telescope Science Institute exposure time calculator (ETC) for COS. Given that LHS 3844 has H-alpha emission consistent with 0A EW, a 128-day rotation period, and showed no flares during 28 days of 2-minute cadence TESS observations (Vanderspek et al., 2018), we do not expect this star (V = 15.3, estimated U = 18.53; Pecaut & Mamajek, 2013) to pose a threat to the COS detectors. The Bright Object Tool finds all stars in the aperture field to be safe for target acquisition with the NUV imager as well as for our science observations of FUV and NUV spectra. To measure the prominent emission lines in the FUV we will use COS G130M (Si III, N V, C II, Si IV) and COS G160M (C IV, He II). We will expose for a combined total of 17802s with COS G130M. These observations will provide S/N > 4 for prominent lines in this range. We break up these obesrvations into 2 visits of 3 orbits each for ease of scheduling. This set-up will still allow us to monitor LHS 3844 for flares, which occur on the timescales of minutes to hours, but will be less constraining than if we could observe for 6 contiguous orbits. We get this flare monitoring "for free" since we need these exposures to build up S/N in UV lines of interest. We will expose for a combined total of 8854s with COS G160M which will provide S/N > 4 for C IV and S/N > 2 for He II. The Si IV, C IV, and He II lines are particularly important for estimating the EUV flux. For the NUV we will expose for a total of 2864s with COS G230L and detect the Mg II doublet at S/N > 5. There is a transiting planet in the system, but the expected signal from the planet is small compared to our photon-noise limited uncertainties. Given the size and temperature of this planet (R = 1.36 Earth radii, Teq = 805 K) we do not expect it to have an evaporating exosphere that would contribute UV line emission. In the interest of efficient scheduling, it is not necessary to put a phase constraint on these observations due to the planet transits. In the APT we provide COS ETCs corresponding to the exposure time in each orbit. Here are the ETCs for the combined exposure times for each set up: COS G130M: COS.sp.1349239; COS G160M COS.sp.1349243; COS G230L: COS.sp.1349244. 1) Professor David Charbonneau discovers and characterizes exoplanets, with a focus on those transiting nearby M-dwarfs that are amenable to spectroscopic study of their atmospheres. He has been PI on 2 HST/STIS programs and Co-I on an additional 27 HST programs. He serves as PhD advisor to Hannah Diamond-Lowe. 2) Hannah Diamond-Lowe is a graduate student working with Dr. David Charbonneau on detecting and characterizing small exoplanet atmospheres. As PI of this proposal she will lead a resulting paper with active support from the Co-Is. 3) Dr. Laura Kreidberg is a seasoned user of HST, including a successful proposal to study K2-3 with only HST/COS (GO program 15110). Dr. Kreidberg has led five papers based on HST data and is the PI of the 100-hour Spitzer program to observe a complete phase curve of LHS 3844b (Spitzer DDT program 14204). 4) Dr. Jennifer Winters studies the fundamental properties of the nearby M dwarfs, with a specific focus on their stellar multiplicity. She is the PI of a Guest Investigator proposal to determine the flare rates and energies of the mid-to-late M dwarfs within 15 pc (including LHS 3844) with TESS. 5) Dr. Allison Youngblood is an expert in UV spectroscopy of cool dwarf stars, specifically Ly-alpha reconstructions and stellar flare analysis with STIS and COS data. She has PI'ed two recent STIS proposals (GO 15190 and 15463), and participated in the HST MUSCLES and Mega-MUSCLES Treasury Surveys (GO 13650 and 15071) which utilized all of the proposed COS modes. Planets and Planet Formation 0 false false true false false false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM M V-IV NO LHS3844 J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1600 COS/NUV Spectroscopic No No G230L 2950 /home/hannah/Harvard-SmithsonianCfA/PlanetarySystems/LHS3844/HSTCycle26Mid/PhaseII/OP-cache/LHS3844_phaseII-v01.xml 1555442995629 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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