0 Assigned ID: 1138 ----- Attempting Submission 1 (Fri Sep 27 16:21:29 GMT 2019) ----- HST Phase I Proposal 1138 (LTT1445A.apt) successfully submitted. Receipt: # 1138-1 ----- Attempting Submission 2 (Fri Sep 27 18:56:19 GMT 2019) ----- 1) The BOP justification for the M star target was submitted via email. 2) The additional coI, Dr. Youngblood, was supposed to be in the original APT coI list but was left off in error. Her additon has been approved. 3) 11/25/19 changes: a) the proper motion values had been reversed. This was corrected. b) FP-POS for the COS G130M and G160M were changed to "ALL." 4) 12/5/19 changes: Changed the FP-POS from ALL to specific positions to get time request correct. 5) 12/9/19: added a FP-POS=4 to the G160M observations. 1998739849 ----- Attempting Submission 1 (Fri Nov 15 18:57:29 GMT 2019) ----- ----- Attempting Submission 2 (Mon Nov 25 20:59:13 GMT 2019) ----- ----- Attempting Submission 3 (Thu Dec 05 17:27:41 GMT 2019) ----- ----- Attempting Submission 4 (Mon Dec 09 15:47:23 GMT 2019) ----- The additional coI, Dr. Youngblood, was supposed to be in the original APT coI list but was left off in error. Her additon has been approved. 11/25/19: After updating the FP-POS values I re-ran the orbit planner for Visits 1 and 2. Even though the orbit layout are clearly correct (5 and 3 orbits, respectively), APT has assigned then different values (e.g., orbit 20 instead of orbit 5) and thinks the program is 33 orbits instead of 10. I am not sure how to fix this. I also get a warning about ineffecient layout of FP-POS settings after selecting "ALL." 12/5/19: Fixed issue above. 12/9/19: Added FP-POS=4 to G160M. UV Spectroscopy of LTT1445A: Evaluating the Energetic Irradiance on a Nearby Terrestrial Exoplanet JWST will be able to observe the atmospheres of rocky planets transiting nearby M dwarfs. A few such planets are already known and TESS has begun to find more. To interpret observations of the exoplanets' atmospheres, we must understand the high-energy SED of their host stars: EUV irradiation can erode a planet's gaseous envelope, FUV/NUV-driven photochemistry shapes an atmosphere's molecular abundances, and flares can affect long term stability. A number of recent surveys have used HST's UV capabilities to characterize the energetic irradiance spectra of M stars across a range of stellar masses, ages, and activity levels. While the surveys have proven invaluable for predicting the evolution of an exoplanet's atmosphere and its potential to support life, they have also shown scatter in behavior and irradiance properties for stars of similar type. As a result, direct UV observations remain the gold standard for understanding the effects of the stellar irradiance on its exoplanet compansions in the most promising targets for JWST observations. We propose here to obtain UV (1150-3200 A) spectroscopy and time-series monitoring of the new terrestrial planet host system, LTT1445Ab. Recently discovered by TESS, this system is the closest transiting system with an exoplanet around a low mass (0.25 Msun) star and has immediately risen to prominence as a potential target for characterization of its atmosphere. Our proposed observations will provide the UV context necessary to determine the likelihood of atmospheric formation and retention, the identification of potential (false positive) biomarkers, and the impacts of stellar activity on the exoplanet atmospheric stability. Observing Modes: For a full census of the UV emission incident on the habitable zone (HZ) around LTT1445A, we require spectral coverage from 1150-3100 A: the G130M, G160M, and G230L modes of COS and the G140M and G230L modes of STIS. In the FUV (excepting Lya) we will use COS G130M and COS G160M. Emission from Lya, Si IV, C IV, and He II is particularly interesting because these lines provide constraints on the Lyman continuum/EUV (100 - 900 A) irradiance in these systems. COS is essential for a moderate spectral resolution line census as the lower effective area and higher detector background of STIS make observations of all but the very brightest lines prohibitively time consuming. We will use the medium resolution COS modes to resolve chromospheric lines and maximize contrast from narrow features. At NUV wavelengths, we will use STIS G230L to observe the ( > 2200 A) NUV continuum, Fe II 2400 and 2600, and Mg II 2800, but we will take advantage of the superior sensitivity of the COS G230L mode to observe the 1750-2100 A region that is important to the photodissociation of O2 and the production of O3. In order to calibrate the UV data to visible/IR photospheric models, we will also acquire short optical observations with the STIS G430L. We will use the G140M mode of STIS with the 52"x0.1" slit to measure the Lya profile for our target. STIS is needed over COS for Lya to minimize geocoronal contamination with a narrow slit. Lya experiences absorption from the intervening local ISM and the line must be reconstructed to provide a reliable measure of the local Lya field in these systems. Short duration (minutes to hours) flares are most common on M dwarfs and we will use the most sensitive UV photon-counting mode on HST (COS G130M) to perform 8-hour variability studies (5 contiguous spacecraft orbits) of characteristic chromospheric and transition region lines (C II, Si III, C IV, Si IV, He II, and N V) for our target. This observation strategy naturally splits the target campaign into 3 HST visits: 1) COS G130M (5 orbits), 2) COS G160M+G230L (3 orbits), and 3) STIS G140M+G230L+G430L (2 orbits). Employing this strategy in APT, we find that LTT1445A has three months of visibility during midcycle observing window (11/1/2019-3/31/2020). A key science goal for the program is to estimate the EUV emission from the star and its effects on heating the planet's atmosphere. Using the FUV data alone, we will estimate the EUV flux using empirical scaling relations from Linsky et al. 2014. A more detailed calculation using DEM calculations is desirable but requires X-ray observations in combination with the FUV. We will apply for these under a separate proposal; this approach has proven successful for previous programs of this nature. Exposure Time Calculations: We estimated the expected flux from LTT1445A using the observed quiescent spectrum of GJ 436 (from MAST), scaled to the distance of LTT1445A. The 5 orbit COS G130M variability observations will produce deep spectral observations in the 1150-1420 A range. For the remaining UV wavelengths, we estimated exposure times based on the amount of time required to achieve S/N>=10 per resolution element in the characteristic emission lines: Ly (STIS G140M), C IV (COS G160M), and Mg II (STIS G230L). We estimate SNR>=5 in the NUV continuum (1900 A, COS G230L and 2850 A, STIS G230L) and S/N>20 in the optical (STIS G430L). Using the STScI on-line ETCs, we have estimated the total exposure time per target resulting in a total observing time allocation request of 10 orbits. Safety: We reviewed LTT1445A against the bright object screening limits for M stars and it meets the specications for the COS and STIS FUV detectors. The COS BOP would fail if Lya was observed. To avoid this (and because we are using STIS to get the Lya emission), we are using the G130M/1222 grating settting. We veried that we will not have to request a specic range of roll angles to keep LTT1445BC out of the COS Bright Object Aperture: the PSA and BOA are separated by 13 arcsec vs. 7 arcsec between LTT1445A and LTT1445BC. Dr. Froning is the PI of the HST Mega-MUSCLES Treasury Survey, a large program using HST, Chandra, XMM, Swift, and several ground-based telescopes to obtain pan-chromatic spectroscopy of a broad survey of M stars to evaluate their high energy irradiance environment, exoplanet atmospheric parameters and biomarker production, and the potential for habitabilty. Dr. Froning is an experienced observer and instrument developer with expertise in stellar astrophysics and the design and development of UV/OIR imagers and spectrographs for ground and space facilities. She was the Project Scientist for the Cosmic Origins Spectrograph and is an the lead or co-author on over 20 papers using HST UV spectroscopic observations. David Wilson is a PI of two previous HST programs (13719, 15189) obtaining ultraviolet spectroscopy of stars using both COS and STIS, and has published multiple first-author papers based on HST data. He has extensive experience with the HST calibration tools to perform the non-standard reductions necessary for studying late-type stars, and has completed bright-object protection checks for multiple programs. Kevin France was the PI of the MUSCLES Treasury Survey as well as a host of other HST programs focused on the UV properties of exoplanetary systems and T Tauri stars. Allison Youngblood was a member of the MUSCLES team and has published a number of papers focused on the quiescent and flare properties of M stars. Girish Duvvuri has developed a new method of estimating the EUV properties of M stars by applying Differential Emission Measure calculations based on X-ray and FUV observations. Yamila Miguel and Sarah Rugheimer are members of the MUSCLES and Mega-MUSCLES teams and are experts in using the M star spectral and flare information provided by UV observations to model the atmospheres and photochemistry/biomarker tracers of exoplanets around low mass stars. Planets and Planet Formation Stellar Physics 0 false false true false true false false SUPPORTED STAR M III-I M V-IV NO Coordinates from Henry et al. 2018, AJ, 155, 265. Proper motions from GAIA. LTT1445A J2000 J2000 Star is part of a triple system. Target is the brightest component, LTT1445A. COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1600 COS/NUV Spectroscopic No No G230L 2950 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140M 1222 The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. /private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit4682119980436707288.xml G430L/G230L/G140M exposures. 1582577334000 91.39999999999998 (Tic-Visit :proposal-id 16033 :visit-id "03" :proposal-version -1 :trans-version "20191203" :date "16-Mar-2020 16:15:38.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 734096 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16033 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16033 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2763.0 :al-overhead-at-end 0 :internal-dur-at-end 178.0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16033 :visit-id "03" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2854 :al-overhead-at-end 0 :internal-dur-at-end 622 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 2 0 /private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit4682119980436707288.xml G430L/G230L/G140M exposures. 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