0 Assigned ID: 1309 ----- Attempting Submission 1 (Wed Dec 07 20:19:57 GMT 2016) ----- Completed coordinate info 275424865 ----- Attempting Submission 3 (Mon Dec 12 21:33:42 GMT 2016) ----- ----- Attempting Submission 4 (Tue Dec 13 15:26:02 GMT 2016) ----- We have recently completed reconnaissance studies of the TRAPPIST-1 system with the Spitzer and Hubble Space Telescopes. Owing to a 20-d long follow-up with Spitzer, we have now constrained the system architecture up to the ice line. Thanks to 4 non-consecutive HST/STIS orbits, we have determined the potential for further studies of the system in the UV--notably to search for hydrogen exospheres--and characterized the UV environment of TRAPPIST-1's planets, which is an essential contributing factor to their potential habitability. These reconnaissance studies with the synergetic Great Observatories emphasize the system uniqueness for Earth-sized comparative planetology and for the search for extrasolar habitats. We request here 5 consecutive HST/STIS orbits to build upon our UV exploratory program and confirm the presence of an extended exosphere exosphere around TRAPPIST-1~c. These observations will inform us on its volatile reservoir while complementing the insights gained with HST/WFC3 (GOs 14500 and 14873). Our request for immediate HST/STIS followup will fulfill the urgent need to inform the community about TRAPPIST-1 planets in order to guide their follow-up, notably in the context of the upcoming JWST Cycle 1 proposal. We propose to observe the transits of TRAPPIST-1's planets with WFC3 on Dec.4, Dec. 29, and Jan. 10 to obtain their tansmission spectra and assess the presence of extended atmospheres. Extrasolar Planets and Planet Formation 0 AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM We 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. 2014 TRAPPIST-1 J2000 J2000 V=18.80+-0.08, R=16.47+-0.07, I=14.0+-0.1, J=11.35+-0.02, K=10.30+-0.02 STIS/FUV-MAMA Spectroscopic No No G140M 1222 1481642724621 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. C:\Users\Julien\AppData\Local\Temp\OPVisit8533103771231945119.xml (Tic-Visit :proposal-id 14900 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "13-Dec-2016 10:25:23.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1132976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14900 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14900 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2880 :al-overhead-at-end 0 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14900 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14900 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14900 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14900 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 639 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) true 5 0 We 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. Following the same observational strategy as GO14493 for this target. We 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. Following the same observational strategy as GO14493 for this target. We 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. Following the same observational strategy as GO14493 for this target. We 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. Following the same observational strategy as GO14493 for this target. We 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. Following the same observational strategy as GO14493 for this target.