Resubmission with last page of the attachment (Past HST Use) removed to comply with the GO/MC template requirements. (APT crashed upon submission, so I'm not sure the third submission was received. The submission comment still applies.) 1798159738 Assigned ID: 1188 ----- Attempting Submission 1 (Wed Sep 30 21:23:19 GMT 2015) ----- HST Phase I Proposal 1188 (Phase1.apt) successfully submitted. Receipt: # 1188-1 ----- Attempting Submission 2 (Thu Oct 01 21:35:13 GMT 2015) ----- HST Phase I Proposal 1188 (Phase1.apt) successfully submitted. Receipt: # 1188-2 ----- Attempting Submission 3 (Fri Oct 02 07:38:41 GMT 2015) ----- 0 A second transit has been observed with Spitzer, which changes the transit ephemeris. I have now updated to period and T0 accordingly. The program can re-enter scheduling. 812077358 ----- Attempting Submission 1 (Fri Dec 11 21:13:45 GMT 2015) ----- ----- Attempting Submission 2 (Tue Dec 15 15:41:39 GMT 2015) ----- ----- Attempting Submission 3 (Thu Mar 03 10:06:36 GMT 2016) ----- ----- Attempting Submission 4 (Mon Apr 11 12:07:05 GMT 2016) ----- In July 2015, we announced the discovery of the super-Earth HD 219134b, orbiting a V = 5.57 star 6.5-pc away from us (Motalebi et al. 2015). This is the brightest and closest transiting system known so far. With Spitzer and HARPS-N, we measured the density of HD 219134b, which is compatible with a rocky planet, possibly containing a large amount of volatile species. The planet receives high stellar irradiation, which could significantly erode its atmosphere. Preliminary estimates indicate that this 4.5 Earth-mass object should nonetheless retain a substantial atmosphere. HD 219134b lies sufficiently far from its star to allow the formation of a hydrogen cloud with a detectable coma. HST is the only telescope able to detect, for the first time, atmospheric escape from a super-Earth, by observing a Lyman-alpha transit. The detection of escaping hydrogen will represent a smoking gun for the presence of water vapor in the lower atmosphere. Constraining the mass-loss rate will allow us to probe the evolution of super-Earths and assess whether hotter super-Earths can be evaporation remnants. Resolving the Lyman-alpha absorption signal will also bring new insights on the dynamics in the exospheric clouds, revealing interaction between the host star and its super-Earth through radiation pressure and stellar wind. A non-detection could hint at a CO/CO2-rich 'super-Venus' and will prepare for adapted follow-up observations. Both outcomes will thus motivate new proposals in Cycle 24. We are going to observe the UV transit of the brightest (V=5.6) and closest (6 pc) known transiting planet, which is a super-Earth. The star is a K2 dwarf and we estimated its Lyman-alpha emission line by scaling up the one of HD 189733 (K dwarf at 19 pc), taking into account the flux dilution due to the distance and the interstellar hydrogen column. Our target should bear the brightest Lyman-alpha flux ever observed for an exoplanet host-star. It should be at similar flux levels, though, as previously observed targets such as active M dwarfs AD Leo or HD 32008, and less intense than other observed targets such as 70 Oph or Xi Boo (see Wood et al. 2005, ApJS 159, 118). We seize this opportunity to observe during one HST orbit, before the planetary transit, with the E140H echelle grating, to access 100,000 spectral resolution and explore the FUV range to measure other possible chromospheric emission lines. The rest of the observations (4 HST orbits: 1 before, 1 during, and 2 after the optical transit) will be carried out with the more sensitive G140M grism. The peak flux is ~2.5x10-12 erg s-1 cm-2 A-1 at 1215.3 A: it is lower than the local limit point source flux for the MAMA with G140M (which is 9.4x10-11 erg s-1 cm-2 A-1 according to the Approximate MAMA Spectroscopic Bright-Object Limits, Table 13.45 of the STIS instrument handbook). The star is also well fainter than the bright object magnitude limit (V=1.3 for a K2V star) given for the MAMA/G140M. EXTRA-SOLAR PLANETS 3 false true false false false false AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM K V-IV NO HD219134 J2000 J2000 U=7.460, B=6.560 STIS/FUV-MAMA Spectroscopic No No E140H 1234 STIS/FUV-MAMA Spectroscopic No No G140M 1222 1460376399532 /private/var/folders/js/1c80b2_s5dl3q50f53ds0cgh0000gn/T/OPVisit1007070738635983901.xml The scheduling data was generated by CASM 24.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14461 :visit-id "01" :proposal-version -1 :trans-version "20160129" :date "11-Apr-2016 14:06:38.0" :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 1064288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14461 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14461 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2684 :al-overhead-at-end 0 :internal-dur-at-end 339 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3017 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14461 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2795 :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 3017 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14461 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2795 :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 3017 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14461 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2795 :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 3017 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14461 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2795 :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 3017 :pcs-gap 0 ) true 5 0 Using our scaled Lyman-alpha line model, the count rate for the entire detector in 2127s is 182 counts/s. The maximum buffer time should thus be 2x10^6 / 182 ~ 11,000s. Because of other chromospheric emission in the range of the echelle grism, we consider a factor of 10x as a margin, so we keep on using our "classic" 900-s buffer time setting. The count rate on the entire detector is 200 counts/s. The count rate on the entire detector is 200 counts/s. The count rate on the entire detector is 200 counts/s. The count rate on the entire detector is 200 counts/s.