0 Assigned ID: 1 ----- Attempting Submission 1 (Thu Mar 07 00:54:38 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. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. We have communicated with our contact scientist and the COS team has approved our use of LP3 with CENWAVE=1327. We have also been approved to use a single FP-POS setting. We are aware that 5 consecutive orbits with COS is abnormal but establishing an out-of-transit baseline for our star is absolutely essential to our science case. Scheduling one of our orbits apart from the other four increases the chances of instrument or stellar variability causing spurious in-transit absorption. 806049500 ----- Attempting Submission 1 (Wed May 08 23:20:39 GMT 2019) ----- HST Phase II Proposal 15710 (hd189_phII.apt) successfully submitted. Receipt: # 15710-1 ----- Attempting Submission 2 (Fri May 10 12:42:01 GMT 2019) ----- HST Phase II Proposal 15710 (hd189_phII.apt) successfully submitted. Receipt: # 15710-2 ----- Attempting Submission 3 (Thu May 30 13:59:32 GMT 2019) ----- We do not provide ETC runs for the acquisition exposures since these are standard exposure times and settings for HD 189733. They are identical to HST program ID 14767. Planets with very short orbital periods, or hot planets, are subject to large amounts of stellar radiation which in turn can cause them to evaporate. For Neptune and super-Earth mass planets this mass loss process is important on evolutionary timescales, potentially stripping significant fractions of the atmosphere. To date, however, observations of hot planet evaporation are severely limited and models of the observed signatures are highly uncertain. The evaporated material in the exosphere is typically observed in the wings of the hydrogen Lyman-alpha line, which can only be captured with UV-capable instruments aboard HST, restricting the number of potential targets. Recently, the excited helium line at 10830 angstroms has been shown to be a reliable tracer of extended hot planet atmospheres and has been used to estimate mass loss from the observed targets. He I 10830 angstroms can be observed from the ground, greatly expanding the accessible target pool for studies of hot planet mass loss. In the 2019A observing semester, we were awarded a night to observe the transit of HD 189733 b at He I 10830 angstroms. We propose the first ever simultaneous observations of Lyman-alpha and He I 10830 angstroms around this prototypical hot Jupiter in order to place stronger constraints on its mass loss rate by forcing thermosphere and exosphere models of the simultaneous data to agree. This unique approach will illuminate shortcomings in both the He I and Lyman-alpha models, leading to better mass loss models for targets with only He I 10830 angstrom observations. This is critical due to the large number of He I 10830 transits that will be observed in the near future. We will use COS with the G130M grating (R~16,000-21,000) with a central wavelength setting of 1291 angstroms (Segment B = 1132-1274 angstroms, Segment A=1291-1433 angstroms) to observe the hydrogen Lyman-alpha line at 1216 angstroms with the goal of detecting absorption in the atmosphere of the hot Jupiter HD 189733 b. We request 5 orbits bracketing the transit of HD 189733 b which begins at UT 10:15 on 07-25-2019. This is the only possible time for the observations as this is the same transit we will be observing from the ground using the spectrograph NIRSPEC on Keck II. Five orbits are necessary in order to adequately sample the out-of-transit stellar Lyman-alphaflux both pre- and post-transit: two orbits sample the transit while the other three occur pre- and post-transit. This mitigates the possibility of the baseline out-of-transit fluxes being contaminated by material that is leading or trailing the planet or stochastic changes in the line flux due to stellar activity. Although STIS has been the primary instrument for exoplanet Lyman-alpha observations, new work by Bourrier et al. (2018b) has shown that subtracting the COS airglow emission at Lyman-alpha can reliably produce spectra with higher signal-to-noise (SN) than STIS obser- vations. We have performed our own airglow analysis of recent HD 189733 COS observations (Program ID 14767) and found that the resulting Lyman-alpha line profiles are consistent with those obtained by STIS (see Figure 4). In fact, due to the greater efficiency of COS, we find that airglow-subtracted exposures from single orbits, or t=2700 seconds, with COS G130M have comparable SN to STIS spectra averaged across t=8600 seconds (4 orbits). Thus COS offers a significant SN advantage even accounting for the airglow subtraction. Our instrument setup will also allow us to analyze a suite of metal lines for absorption in HD 189733 b's atmosphere. This includes, for example, Si III at 1206 angstroms, N V at 1243 angstroms, O I near 1300 angstroms, and C I and O I near 1355 angstroms, some of which have previous marginal detections of in-transit variations (e.g., Bourrier et al. 2013, Ben-Jael & Ballester 2013). Follow-up variability analysis of these lines will be performed with our data set. The visibility of HD 189733 is ~50 minutes during a single HST orbit. We will observe HD 189733 for the entirety of each orbit with exposure times of 2700 seconds. The COS spectra shown in Figure 4 were observed with similar exposure times, resulting in a SN ~10-20 per dispersion element across the important regions of the Lyman-alpha wings (gray shaded regions in the right panel of Figure 4). HD 189733 has been successfully observed with our setup and is within the brightness limits for the proposed exposure times. Our team is highly experienced in working with HST COS and STIS data. PI P. Wilson Cauley has experience working with and publishing HST COS data (see Cauley & Johns-Krull 2016, ApJ, 825, 147) and is an expert in ground-based exoplanet transmission spectra. Co-I Kevin France has led numerous successful HST observing proposals, including the MUSCLES treasury survey (France et al. 2016, ApJ, 820, 89). Co-I Allison Youngblood has extenxive experience leading HST proposals and working with STIS and COS data. Co-I Seth Redfield has also led numerous successful HST proposals, mainly in field of mapping ISM absorption. Co-I Evgenya Shkolnik is an expert in the UV emission from late-type stars and leads the HST HAZMAT program (ID 14784). Co-I Laura Kreidberg is an expert in the reduction and analysis of space-based exoplanet transmission spectra. Co-I Vincent Bourrier has published numerous studies of Lyman-alpha absorption in exoplanet atmospheres using HST STIS and COS data. He is also an expert in modeling the extended atmosphere absorption seen in Lyman-alpha using the EVE code. Co-Is Ruth Murray-Clay, John McCann, and Antonija Oklopcic are theorists who specialize in detailed models of escaping exoplanet atmospheres. John McCann has recently produced hydrodynamic simulations of hot planet mass loss and Antonija Oklopcic produced the first isothermal wind model of He I 10830 angstrom absorption in hot planet atmospheres. Planets and Planet Formation 0 false AVAILABLE STAR K V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1222 1559224752107 The scheduling data was generated by CASM 27.0. 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