0 Assigned ID: 1212 ----- Attempting Submission 1 (Tue Sep 29 22:08:03 GMT 2020) ----- HST Phase I Proposal 1212 successfully submitted. Receipt: # 1212-3 ----- Attempting Submission 4 (Wed Sep 30 18:33:03 GMT 2020) ----- HST Phase I Proposal 1212 successfully submitted. Receipt: # 1212-4 I hope I have made the phase requirements/options as clear as possible, please let me know if further clarification is needed. 1341691422 ----- Attempting Submission 1 (Mon Nov 16 23:38:16 GMT 2020) ----- The HI Lyman alpha line dominates the ultraviolet emission of late type-stars. Observing Lyman alpha is vital for projects that wish to understand the chromospheric structure and behaviour of stars, as well as modeling the chemistry and characteristics of exoplanetary atmospheres. However, observing the Lyman alpha line is extremely difficult due to obscuration from the Interstellar Medium and telluric airglow. The numerous HST programs observing Lyman alpha lines rely on reconstruction models, which take what parts of the line can be observed and, via various recipes, infer the integrated flux and profile of the rest of the line. Testing the accuracy of such reconstruction techniques is difficult, requiring a system where the line can be observed in an obscured state and compared with the unobscured line. We have identified a system where this is possible: A close white dwarf-M dwarf binary where the high radial velocity change over the binary orbit moves the M dwarf Lyman alpha line in and out of obscuration. We propose to obtain phase-resolved STIS spectroscopy of the system to observe the Lyman alpha line at different levels of obscuration, which will then be tested against the maximum velocity, unobscured line. We describe our detailed planning of the experimental set up to calculate the small investment of HST time required and account for complexities such as flaring and coronal heating. This experiment will provide an unprecedented test of the Lyman alpha reconstructions that are at the heart of multiple past, present and (most likely) future HST programs. The target is EG Uma, a post common envelope binary consisting of a white dwaf and an M dwarf. The four observations will obtain phase-resolved spectroscopy of the M dwarf Lyman alpha line emission line. The period is given by https://ui.adsabs.harvard.edu/abs/2000MNRAS.312...70B/abstract as HJD = 2449800:79131(58)+66765930(57), where the ephermeris is the blue-to-red crossing time of the radial velocity curve of the M dwarf. The four observations will observe the Lyman alpha line at four phases, measureing the line at different velocities. The ~16hr orbital period means that the velocity does not change by much during an HST orbit, increasing the scheduling flexability: Visit 01 should be obtained between phase 0.95 and 0.05. We expect to detect the wings of the Lyman alpha ine with S/N 10-20. Visit 02 should be obtained between phase 0.2 and 0.3. We expect to detect most of the Lyman alpha ine with S/N ~30. Visit 03 should be obtailed between phase 0.45 and 0.55. We expect to detect the wings of the Lyman alpha ine with S/N 10-20. Vist 04 should be obtained between 0.7 and 0.8, at maxmium radial veloctiy, This is the key observation of the proposal, when the Lyman alpha line will be clear of airglow and ISM absorption. We expect to detect the peak of the Lyman alpha ine with S/N 30-40. Note that Figure 2 of the proposal is out by phase = 0.5, the numbers here are correct. The order in which the observations are taken is unimportant. To increase flexability, Visits 01 and 03 may be obtained at the same phase (either 0.95-0.05 or 0.45-0.55) if scheduling them at different phases is impossible. Visit 02 can also be moved to phase 0.7-0.8 for a minor loss in scientific return. 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. Allison Youngblood is an expert on the reconstruction of Lyman alpha lines at M dwarfs. She has written multiple papers on the subject and has been PI or CoI on several HST programs observing Lyman alpha lines, and has developed one of the most widely used reconstruction codes. 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 habitability. 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 the lead or co-author on over 20 papers using HST UV spectroscopic observations. 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. Brian Wood is an expert in Lyman alpha line observation and reconstruction. He has lead various HST programs covering the Lyman alpha line of various spectral types, particularly in relation to stellar winds. Seth Redfield has led efforts to characterise the local ISM and has developed the most widely used ISM map, leading a variety of HST programs obtaining spectra of ISM lines in multiple spectral types. Jeremy Drake is a member of the Chandra science division and has published multiple studies on the high energy environment of stars. Odette Toloza is an expert in ultraviolet spectroscopy of white dwarfs, with a particular focus on the model atmosphere fitting and time-resolved observations. Stellar Physics and Stellar Types Exoplanets and Exoplanet Formation 6 false false true false false false false SUPPORTED EXT-STAR DA M V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/FUV-MAMA Spectroscopic No No G140M 1222 STIS/FUV-MAMA Spectroscopic No No G140M 1222 STIS/FUV-MAMA Spectroscopic No No G140M 1222 STIS/FUV-MAMA Spectroscopic No No G140M 1222 1605569410724 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.950/0.050. The scheduling data was generated by CASM 28.2. 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The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1617372434000 173.0 (Tic-Visit :proposal-id 16449 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "16-Nov-2020 17:30:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 157024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16449 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16449 :visit-id "02" :obset-id "A2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16449 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2549 :al-overhead-at-end 0 :internal-dur-at-end 440 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) false 1 0 1605569411966 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.450/0.550. The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1617097967000 174.1589514916452 (Tic-Visit :proposal-id 16449 :visit-id "03" :proposal-version -1 :trans-version "20200619" :date "16-Nov-2020 17:30:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 157024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16449 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16449 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16449 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2549 :al-overhead-at-end 0 :internal-dur-at-end 440 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) false 1 0 1617826316548 /private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit18250972110210059803.xml Repeat of Visit 03 (Tic-Visit :proposal-id 16449 :visit-id "53" :proposal-version -1 :trans-version "20200619" :date "07-Apr-2021 16:11:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 157024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16449 :visit-id "53" :obset-id "53" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16449 :visit-id "53" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16449 :visit-id "53" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2549 :al-overhead-at-end 0 :internal-dur-at-end 440 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) true 1 0 1605569412569 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.700/0.800. The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1617343853000 172.5 (Tic-Visit :proposal-id 16449 :visit-id "04" :proposal-version -1 :trans-version "20200619" :date "16-Nov-2020 17:30:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 157024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16449 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16449 :visit-id "04" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16449 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2549 :al-overhead-at-end 0 :internal-dur-at-end 440 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) false 1 0