0Assigned ID: 940
----- Attempting Submission 1 (Fri Apr 07 21:42:46 GMT 2017) -----
HST Phase I Proposal 940 (GO25.pdf.apt) successfully submitted.
Receipt: # 940-1
----- Attempting Submission 2 (Fri Apr 07 23:33:10 GMT 2017) -----
----- Attempting Submission 3 (Sun Apr 09 04:35:46 GMT 2017) -----LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.
The proposal is part of a cycle 25 large program (75 orbits or more in one cycle) and so should use Schedulability 100.RESUBMISSION: visits C3, F3, and H2 added following acceptance of 2 HOPRs.1741575862----- Attempting Submission 1 (Fri Jul 14 20:44:50 GMT 2017) -----
----- Attempting Submission 2 (Tue Jul 18 20:07:26 GMT 2017) -----
----- Attempting Submission 4 (Tue Sep 05 21:55:03 GMT 2017) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 5 (Sat Sep 09 19:03:53 GMT 2017) -----
----- Attempting Submission 6 (Mon Sep 11 20:49:12 GMT 2017) -----
----- Attempting Submission 7 (Wed Oct 04 18:27:44 GMT 2017) -----
----- Attempting Submission 8 (Thu Oct 12 21:31:57 GMT 2017) -----
----- Attempting Submission 9 (Wed Oct 18 21:32:02 GMT 2017) -----
----- Attempting Submission 10 (Mon Oct 23 15:50:11 GMT 2017) -----Topics previously discussed with our program coordinator.Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ahead of JWSTUsing the Spitzer Space Telescope, our team has discovered 7 Earth-sized planets around the nearby Ultra-cool dwarf star TRAPPIST-1. These planets are the first to be simultaneously Earth-sized, temperate, and amenable for in-depth atmospheric studies with space-based observatories (notably, JWST). TRAPPIST-1's system thus provides us with the first opportunity to probe the atmospheres of Earth-sized exoplanets and search for signs of habitability beyond our solar system, which will require spectral information from the UV to the IR to complete their atmospheric puzzles.
We request 114 HST orbits to complete the UV+NIR survey of the 7 planets in preparation for their in-depth followup with JWST. The suggested low-density of the planets combined with their complex orbital resonance chain indicate that they migrated inward to their current positions and may harbor large water rich reservoir or leftover primordial H2 atmospheres. We have already ruled out the presence of clear H2 atmospheres for the 5 innermost planets using WFC3 and are requesting 16 WFC3 orbits to complete the TRAPPIST-1 NIR reconnaissance survey. Our primary request consists in 98 STIS orbits to complete the survey for extended H-exospheres around each of the planets. H-exospheres are the most accessible observables for volatile reservoirs, which have not been ruled out by our WFC3 observations. Exosphere detection is only amenable using HST unique capabilities in the UV and are pivotal to guide JWST's in-depth followup. The combined information from HST's UV and NIR observations will allow us put the first critical pieces of the atmospheric puzzle in place for these temperate earth-sized worlds.This program will observe two transits of each TRAPPIST-1 planets with STIS (in LY-a) to search for signs of exospheres while acquiring extra baseline measurements to monitor the star's activity.
In addition, 16 WFC3 orbits to complete the TRAPPIST-1 NIR reconnaissance survey that has already ruled out the presence of clear H2 atmospheres for the 5 innermost planets.Planets and Planet Formation0falsefalsetruefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETARY SYSTEMWe measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we use the mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.
We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinates and proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).
Radial velocity comes from Barnes et al. 2014TRAPPIST-1J2000J2000V=18.80+-0.08, R=16.47+-0.07, I=14.0+-0.1, J=11.35+-0.02, K=10.30+-0.02WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.151287564600067.20911426819069(Tic-Visit
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)false40The scheduling data was generated by CASM 26.0.5.CASM was run in Phase II mode.50156932302600069.5635012762175(Tic-Visit
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)false40The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.1532024567000248.27999999999997(Tic-Visit
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)true42The scheduling data was generated by CASM 26.0.5.CASM was run in Phase II mode.1595268742000246.6518529681428(Tic-Visit
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)true60We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.150607269000070.09468052770649(Tic-Visit
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)true70We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.150658196700069.202278851383(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.150564926500071.6941682368392(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.153661863200084.98328096190431(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.52.81525617151000247.5646332145027(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.160261884300068.2258275319675(Tic-Visit
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.Original requirements
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.Original requirements
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.154364979400067.3185064049758(Tic-Visit
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1559558396000247.26832844353612(Tic-Visit
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.BETWEEN is being used to force into the correct orbits to capture the transit.
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)true40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1557705048000247.48964762026992(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.160466631200067.6576996941333(Tic-Visit
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We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.160499798000067.59621105304751(Tic-Visit
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.163418164700068.22334174517161(Tic-Visit
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)false40We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.
We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.