0 Assigned ID: 1269 ----- Attempting Submission 1 (Fri Sep 30 18:27:38 GMT 2016) ----- 1/9 Royle - Updated visit 01 to utilize SAA-impacted PHASE window on Jan 27 9/13 Royle - Opened PHASE window on visit 05, extending it later by 0.0002 -19204861 ----- Attempting Submission 1 (Thu Jul 21 21:58:03 GMT 2016) ----- HST Phase II Proposal 14758 (HST-GO-14758-WFC3.apt) successfully submitted. Receipt: # 14758-1 ----- Attempting Submission 2 (Thu Dec 15 20:13:21 GMT 2016) ----- ----- Attempting Submission 3 (Fri Dec 16 19:22:13 GMT 2016) ----- ----- Attempting Submission 4 (Fri Dec 16 23:13:23 GMT 2016) ----- ----- Attempting Submission 5 (Mon Jan 09 14:01:11 GMT 2017) ----- ----- Attempting Submission 6 (Wed Sep 13 20:11:53 GMT 2017) ----- In-house processing Initial Reconaissance of a Transiting Rocky Planet in a Nearby M-Dwarf's Habitable Zone The composition of a terrestrial planet's atmosphere is the end result of accretion, coupled with ongoing processes such as atmospheric escape, outgassing from the interior, and planetary surface processes. We have just discovered a transiting terrestrial planet in a small nearby star's habitable zone. Due to the proximity of the host star and the size of the transit depth, possible constituents for this planet's atmosphere can be detected with the Hubble Space Telescope. Here we propose to use STIS to obtain observations of the host star at Lyman-alpha. A detection of the host star at Lyman-alpha wavelengths will pave the way for observations of Lyman-alpha transits in Cycle 25. The stellar activity UV is an important constraint for future atmospheric modeling, atmospheric escape, and interpreting possible future detections of Oxygen and ozone with JWST or future ELTs. We also propose to obtain two transit observations with WFC3/IR to search for absorption features from a cloud-free, hydrogen rich atmosphere. Detection of a low mean molecular weight atmosphere means future observations should span a broad wavelength range, while a high mean molecular weight atmosphere means future observations should go deeper over a more narrow wavelength range. The results of this Hubble/STIS and Hubble/WFC3 investigation would inform the optimal strategy to observe this object in Cycle 25 and for JWST's GTO program (to be proposed in April 2017 and finalized September 2017). We will observe two transits of the terrestrial planet LHS 1140b with WFC3/IR grism spectroscopy. LHS 1140b resides in the habitable zone of its host star and has a 24.73712 +/- 0.00025 day period. This, combined with the visibility window of HST, means that there are only 2 transits visible with HST before the Cycle 25 proposal deadline, and only one additional transit visible with HST before the Cycle 25 mid-cycle proposal deadline. We will observe two transits of the rocky exoplanet LHS 1140b with WFC3/IR grism spectroscopy. The core science observations consist of continuous high-cadence spectra, taken during the transit with the G141 grism. We will use these data to measure the wavelength-dependent transit depth from 1.1 to 1.7 microns in order to determine if LHS 1140's atmosphere is dominated by hydrogen. We will use a spatial scan for the transit observations, to maximize duty cycle and to mitigate flat-fielding uncertainties by averaging over many pixels. We have chosen a scan rate of 0.14"/second to maintain a similar S/N ratio as observations of GJ 1214b performed by Kreidberg et al. (2014). The scan speed is slow enough, and the observing field sparse enough, that LHS 1140's spectrum will not overlap with other stars in the field, given our mild ORIENT constraints. During the first orbit of each visit (which is usually discarded from transit science observations), we will gather direct images as well as deep imaging spectra in stare-mode (without a spatial scan). Visits 3 and 4 are deep UV exposures designed to determine if LHS 1140 (the host star) emits at Ly-alpha. These observations are not connected to Visits 1 or 2 in any way and can be scheduled any time out of transit. **The Following Items Need Particular PC/CS Attention** PHASE constraints are included that amount to an available range of 60 minutes per 24.73712 day orbital period for the planet. This constraint ensures that the 3rd orbit in each transit observation is during mid-transit. The orbital ephemeris is up-to-date and will not change before these observations are performed, as no more transits are visible from ground-based facilities. Extrasolar Planets and Planet Formation 0 false false false true false false AVAILABLE STAR EXTRA-SOLAR PLANET EXTRA-SOLAR PLANETARY SYSTEM M V-IV NO This object was generated by the target selector and retrieved from the SIMBAD database. The position, proper motion, and the parallax was obtained from Winters et al. (2016). The error on the position was taken from 2MASS, which is tied to the ICRS. J2000 H = 9.092 +/- 0.026, K = 8.821 +/- 0.024 WFC3/IR Spectroscopic No No G141 STIS/FUV-MAMA Spectroscopic No No G140M 1222 POS-TARG DITHER 0.636 LINE false false 2 41.788 WFC3-IR-DITHER-LINE 1 false The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. The phase constraint on the first direct image in this visit is designed such that the 3rd orbit overlaps the transit of LHS 1140b. If need be to enable scheduling, the phase or orient constraints could be relaxed slightly. 1485547848000 77.65895939102631 (Tic-Visit :proposal-id 14888 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "09-Jan-2017 08:54:06.0" :trans-errors '(:WARNINGS 6 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1323040 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14888 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14888 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14888 :visit-id "01" :obset-id "B1" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14888 :visit-id "01" :obset-id "C1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14888 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2842 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3221 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "01" :orbit-number 2 :pcs-time 333 :si-vis-utilization 2877 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3221 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "01" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2889 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3221 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "01" :orbit-number 4 :pcs-time 333 :si-vis-utilization 2895 :al-overhead-at-end 0 :internal-dur-at-end 457 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3221 :pcs-gap 0 ) false 4 2 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. /private/var/folders/h2/_3b1kkv56nn2rfp1zrxtm0sc0006z1/T/OPVisit4721442853990785739.xml The phase constraint on the first direct image in this visit is designed such that the 3rd orbit overlaps the transit of LHS 1140b. If need be to enable scheduling, the phase or orient constraints could be relaxed slightly. (Tic-Visit :proposal-id 14888 :visit-id "05" :proposal-version -1 :trans-version "20170613" :date "13-Sep-2017 16:06:46.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1611120 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14888 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14888 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2837 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "05" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2982 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "05" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2982 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14888 :visit-id "05" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2982 :al-overhead-at-end 0 :internal-dur-at-end 457 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) true 4 0 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. In this UV observation, we will measure the Lyman-alpha flux from the host star. Very loose timing requirements are needed for the STIS/UV visits -- we simply want to observe far from times of the known planet's transit. 1502960048000 266.6510726791225 (Tic-Visit :proposal-id 14888 :visit-id "03" :proposal-version -1 :trans-version "20160601" :date "16-Dec-2016 18:12:53.0" :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 244016 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14888 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14888 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2888 :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 3221 :pcs-gap 0 ) false 1 0 The ETC quotes a time to saturation of 5.04s for the F28X50LP filter, and a time of 0.0270s to reach S/N=40. Our 1.0s exposure time for the ACQ should reach 20% of saturation. The ETC lists a time to saturation through the 52X0.05 slit of 11.08s and a total count rate of 57433e/s. With our 2.0s exposures, we should reach 114,000 source electrons, sufficient for peak-up but still well below saturation. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. In this UV observation, we will measure the Lyman-alpha flux from the host star. Very loose timing requirements are needed for the STIS/UV visits -- we simply want to observe far from times of the known planet's transit. 1502965770000 266.69438317082654 (Tic-Visit :proposal-id 14888 :visit-id "06" :proposal-version -1 :trans-version "20160601" :date "16-Dec-2016 18:12:55.0" :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 244016 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14888 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14888 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2888 :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 3221 :pcs-gap 0 ) false 1 0 The ETC quotes a time to saturation of 5.04s for the F28X50LP filter, and a time of 0.0270s to reach S/N=40. Our 1.0s exposure time for the ACQ should reach 20% of saturation. The ETC lists a time to saturation through the 52X0.05 slit of 11.08s and a total count rate of 57433e/s. With our 2.0s exposures, we should reach 114,000 source electrons, sufficient for peak-up but still well below saturation.