0 Assigned ID: 434 ----- Attempting Submission 1 (Fri Apr 07 08:12:18 GMT 2017) ----- HST Phase I Proposal 434 (Kapteyn_star_HST_Cycle25_Phase1.pdf.apt) successfully submitted. Receipt: # 434-1 ----- Attempting Submission 2 (Fri Apr 07 20:40:10 GMT 2017) ----- HST Phase I Proposal 434 (Kapteyn_star_HST_Cycle25_Phase1.pdf.apt) successfully submitted. Receipt: # 434-2 ----- Attempting Submission 3 (Fri Apr 07 22:41:01 GMT 2017) ----- Increased slit width from 0.06" to 0.2" and deleted PEAK/ACQ exposure. 1212830627 ----- Attempting Submission 1 (Thu Jul 20 22:00:46 GMT 2017) ----- ----- Attempting Submission 2 (Wed Jul 26 23:06:40 GMT 2017) ----- ----- Attempting Submission 3 (Mon Aug 07 21:48:44 GMT 2017) ----- ----- Attempting Submission 4 (Mon Sep 18 20:21:32 GMT 2017) ----- ----- Attempting Submission 5 (Mon Feb 05 22:05:02 GMT 2018) ----- ----- Attempting Submission 6 (Thu Dec 06 22:00:57 GMT 2018) ----- ----- Attempting Submission 7 (Thu May 23 21:13:46 GMT 2019) ----- ----- Attempting Submission 8 (Fri Oct 18 19:21:20 GMT 2019) ----- Visit Planner was run for the proposed redo visit, and the orbital overrun is for visits that have already been executed. H I Lyman alpha (LyA; 1216 A) is the brightest emission line in the UV spectrum of F-K dwarfs and is as bright as the rest of the entire 1150-3000 A emission from M dwarfs. Stellar LyA emission plays a critical role in the chemistry of exoplanet atmospheres, energy transport in the stellar chromosphere, and in probing the density structure of the ISM. Thus, accurately characterizing LyA is critically important. However, interstellar H I removes more than 50% of the stellar LyA flux even for the nearest stars, necessitating reconstruction from the observed line profile wings and an assumption concerning the shape of the line core. The Sun (a G2 dwarf) is the only star for which we have high-resolution direct observations of the line core shape, which is self-reversed. Self-reversal in the LyA line core likely depends on spectral type, so incorrect assumptions of the line core shape for stars cooler or more active than the Sun will result in erroneous intrinsic LyA fluxes. We propose to directly measure with high spectral resolution (STIS E140M) the LyA line cores of five high radial velocity stars (G8 V to M4 V). These will be the first measurements of the LyA line with large Doppler shifts and sufficient resolution to probe the LyA line core shape. We will quantify the self-reversal depth, width, and symmetry, and compare amongst the spectral types. STIS E230H spectra will measure the Mg II line core shapes to test whether they are a good proxy for the LyA core shape. This program will create the first publicly available LyA intrinsic profile templates for late-type stars and update widely-used stellar LyA databases like the MUSCLES Treasury Survey. The target list is composed of nearby (< 6 pc), high radial velocity (> +/-80 km/s) G, K, and M dwarfs. These targets will allow us to measure the shapes of the H I LyA (1216 A) and Mg II (2798, 2802 A) line cores as the line cores are Doppler shifted away from the interstellar H I and Mg II absorption and the geocoronal H I emission. To observe H I LyA (1216 A), we will use the STIS E140M grating with the narrow 52" x 0.05" slit to minimize geocoronal LyA contamination and separate the line core from the ISM absorption trough. We will also use the STIS E230H grating with the 0.2" x 0.2" slit to measure the Mg II (2798, 2802 A) line cores. All of these exposures will be obtained in time-tag mode to identify any flares. Our sample includes two late G/early K type dwarfs, and three early-to-mid M dwarfs, including Barnard's Star (GJ 699), the 4th closest star to the Earth, and GJ 411 (HD 95735), the 6th closest star to Earth. This five-member sample spans G, K, and M spectral types to elucidate any dependence in the line core shapes on spectral type (this is expected to depend on the stellar surface magnetic fields). Each of our five targets has its own visit. No visit has more than 4 orbits, and we have elected to obtain all of our LyA and Mg II observations contemporaneously as we are seeking correlations between these line core shapes and the shapes may vary on longer time scales with stellar activity/variability. Exposure time calculations for the LyA observations (STIS E140M) were carried out using known or estimated fluxes, and in the case of Kapteyn's star (HD 33793), a fit to the COS G130M archival observation. Kapteyn's star (M1 V) and GJ 783A (HD 191408; K2.5 V) have archival Mg II (STIS E230H) observations, and this data was used in the ETC. For the remaining three stars (a G8 V, M2 V, and M4 V) without archival Mg II observations, we scaled the Mg II fluxes to match the appropriate distance and to correspond to approximately the appropriate spectral type. Stellar Physics 6 false false true false false false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM M V-IV NO KAPTEYN-STAR GJ-191 J2000 J2000 STAR EXTRA-SOLAR PLANETARY SYSTEM G V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. GJ-139 HD-20794 J2000 J2000 STAR K V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. GJ-783-A HR-7703 J2000 J2000 STAR M V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. GJ-699 V2500-OPH J2000 J2000 STAR EXTRA-SOLAR PLANETARY SYSTEM M V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. GJ-411 LHS-37 J2000 J2000 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230H 2713 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230H 2713 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230H 2812 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230H 2812 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230H 2812 1558645959405 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. 1554320993000 111.53832680487068 (Tic-Visit :proposal-id 15190 :visit-id "01" :proposal-version -1 :trans-version "20181130" :date "23-May-2019 17:12:38.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 626672 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2952 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "01" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2983 :al-overhead-at-end 0 :internal-dur-at-end 2110 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "01" :orbit-number 3 :pcs-time 302 :si-vis-utilization 2983 :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 3285 :pcs-gap 0 ) true 3 0 Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1932 s to 1945 s. The updated ETC run (0.2x0.06 at 1932 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 3093 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~13 at the peak of the emission line profile to ~14. The ETC Run has been updated to include a Kurucz spectral model of an early M dwarf, but it did not significantly change the output. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1461 s to 1474 s. The updated ETC run (0.2x0.06 at 1461 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~9 at the peak of the emission line profile to ~10. 1558645963295 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. To ensure that the Lyman alpha airglow emission coincides spectrally with the ISM absorption trough, Hubble must not observe this target between February 12 - June 21 (any year). 1536057055000 61.7625444256885 (Tic-Visit :proposal-id 15190 :visit-id "02" :proposal-version -1 :trans-version "20181130" :date "23-May-2019 17:12:42.0" :trans-errors '(:WARNINGS 2 :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 470144 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2927 :al-overhead-at-end 0 :internal-dur-at-end 2135 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "02" :orbit-number 2 :pcs-time 302 :si-vis-utilization 3038 :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 3200 :pcs-gap 0 ) true 2 2 Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure decreased from 1852 s to 1865 s. The updated ETC run (0.2x0.06 at 1852 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~36 at the peak of the emission line profile to ~38. Re-running the orbit planner after changing all E140M apertures to 0.2x0.06 with auto-adjust to pack the orbits, this exposure time increased from 300 s to 306 s. The original ETC run is still included (for 300 s). The updated ETC Run includes a stellar model with more complete spectral coverage than before, so the buffer time has been reduced to account for the increased global count rate. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 2192 s to 2199 s. The updated ETC run (0.2x0.06 at 2192 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~39 at the peak of the emission line profile to ~42. 1517867986986 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. 1544834165000 29.20454334387611 (Tic-Visit :proposal-id 15190 :visit-id "03" :proposal-version -1 :trans-version "20171009" :date "05-Feb-2018 16:59:46.0" :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 400576 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2964 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3298 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3076 :al-overhead-at-end 0 :internal-dur-at-end 412 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3298 :pcs-gap 0 ) true 2 0 Exp time reduced from 0.2s to 0.1s to reduce the likelihood of saturation. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1890 s to 1903 s. The updated ETC run (0.2x0.06 at 1890 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~19 at the peak of the emission line profile to ~21. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1965 s to 1978 s. The updated ETC run (0.2x0.06 at 1965 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~20 at the peak of the emission line profile to ~21. ETC Run was updated to include a Kurucz stellar model and the higher global count rates resulted in recommended buffer times that were below the minimum 99 s. Thus, the mode has been changed from TIME-TAG to ACCUM. This change resulted in some unused orbit visibility time, so the adjusted total exposure time is now 503 seconds, which does not appear to significantly change the detectory safety (STIS.sp.1024426). 1505765622107 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. To ensure that the Lyman alpha airglow emission coincides spectrally with the ISM absorption trough, Hubble must not observe this target between January 4 - June 5 (any year). 1534083072000 110.0 (Tic-Visit :proposal-id 15190 :visit-id "04" :proposal-version -1 :trans-version "20170613" :date "18-Sep-2017 16:13:41.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 835344 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2869 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2980 :al-overhead-at-end 0 :internal-dur-at-end 316 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2980 :al-overhead-at-end 0 :internal-dur-at-end 316 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "04" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2980 :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 3202 :pcs-gap 0 ) true 4 0 Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time was increased from 1864 s to 1877 s. The updated ETC run (0.2x0.06 at 1864 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~23 at the peak of the emission line profile to ~24. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 2950 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~27 at the peak of the emission line profile to ~29. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 2937 s to 2950 s. The updated ETC run (0.2x0.06 at 2937 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~27 at the peak of the emission line profile to ~29. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. The exposure time was maintained at 1418 s. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~19 at the peak of the emission line profile to ~21. Re-running the orbit planner after changing all of the E140M apertures to 0.2x0.06 and using auto-adjust to pack the orbits, this exposure time was increased from 1018 s to 1029 s. The original ETC run is still included (for 1018 s). The ETC run has been updated to include a Kurucz model of an early M dwarf in addition to the Mg H & K lines. This did not significantly change the output. 1544133558323 The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. 1557942497000 105.0 (Tic-Visit :proposal-id 15190 :visit-id "05" :proposal-version -1 :trans-version "20181130" :date "06-Dec-2018 16:59:18.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 765808 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2867 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "05" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2898 :al-overhead-at-end 0 :internal-dur-at-end 316 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "05" :orbit-number 3 :pcs-time 302 :si-vis-utilization 2898 :al-overhead-at-end 0 :internal-dur-at-end 316 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "05" :orbit-number 4 :pcs-time 302 :si-vis-utilization 2898 :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 3200 :pcs-gap 0 ) true 4 0 Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1854 s to 1867 s. The updated ETC run (0.2x0.06 at 1854 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~30 at the peak of the emission line profile to ~33. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 3008 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~39 at the peak of the emission line profile to ~41. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 2995 s to 3008 s. The updated ETC run (0.2x0.06 at 2995 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~38 at the peak of the emission line profile to ~41. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 1997 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~32 at the peak of the emission line profile to ~34. Re-running the orbit planner after changing all the E140M apertures to 0.2x0.06 and using auto-adjust to pack the orbits, this exposure time increased from 497 s to 508 s. The original ETC run is still listed (for 497 s). The ETC was updated to include a Kurucz spectral model of an early M dwarf, but this did not significantly change the output. 1571426401817 The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. /private/var/folders/2p/z31d5hvs6tg091dmxl7h0l_4006w5l/T/OPVisit13735666165038681217.xml (Tic-Visit :proposal-id 15190 :visit-id "06" :proposal-version -1 :trans-version "20190514" :date "18-Oct-2019 13:20:01.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 609168 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15190 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15190 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2807 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "06" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2898 :al-overhead-at-end 0 :internal-dur-at-end 316 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15190 :visit-id "06" :orbit-number 3 :pcs-time 302 :si-vis-utilization 2898 :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 3200 :pcs-gap 0 ) true 3 0 Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Re-running the orbit planner and using auto-adjust to pack the orbits, the exposure time for this exposure increased from 1854 s to 1867 s. The updated ETC run (0.2x0.06 at 1854 s) shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~30 at the peak of the emission line profile to ~33. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 3008 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~39 at the peak of the emission line profile to ~41. Changed to the 0.2"x0.06" slit to avoid order overlap in echelle mode. Exposure time maintained at 1997 seconds. The updated ETC run shows a marginal increase in the SNR per resel of the Lyman alpha profile, from ~32 at the peak of the emission line profile to ~34. Re-running the orbit planner after changing all the E140M apertures to 0.2x0.06 and using auto-adjust to pack the orbits, this exposure time increased from 497 s to 508 s. The original ETC run is still listed (for 497 s). The ETC was updated to include a Kurucz spectral model of an early M dwarf, but this did not significantly change the output.