0 Assigned ID: 1556 ----- Attempting Submission 1 (Sat Sep 30 12:53:56 GMT 2017) ----- ----- Attempting Submission 2 (Sat Sep 30 18:14:12 GMT 2017) ----- 0 ----- Attempting Submission 1 (Tue Dec 05 16:05:49 GMT 2017) ----- Atmopsheric Escape from the Closest Super-Earth at High Spectral Resolution The super-Earth HD 219134b has the brightest (V=5.6) and closest (6.5 pc) known host star of any transiting exoplanet. The planet density is compatible with a rocky composition containing a large amount of volatile species (i.e., H2O). Under high stellar irradiation, the planet is likely losing a fraction of its atmosphere and water photodissociation could give rise to an extended cloud of hydrogen. For larger planets, this cloud can be detected as a blueshifted absorption in the stellar H I Lyman-alpha line. So far, no spectral signature of an atmosphere (escaping or not) has been convincingly detected on a super-Earth. Our recent STIS/FUV observation revealed a *redshifted* H I Lya transit signature of 8.2+/-1.9%. While scenarios with a redshifted atmospheric signature exist, the mandatory first step is to rule out stellar variability that could have mimicked a transit signature. This is straightfoward to do with new transit observations. Confirming this H detection is primordial, as it will be a smoking gun for the presence of water vapor in the lower atmosphere. Furthermore, we have established HD 219134 as the brightest Lyman-alpha source among all measured transiting exoplanet host stars, making it possible to use the high-resolution (R=114,000) echelle grating E140H for transit observation. We obtained a first E140H spectrum of the star, revealing strong emission lines of O I and C II in addition to H I Lyman-alpha. This enables the simultaneous search for hydrogen, oxygen, and carbon in the upper extended atmosphere of the planet. Finding these elements escaping from a super-Earth will bring exciting constraints on the nature of the elusive lower atmosphere. 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. We are observing with the E140H echelle grating two transits of the planet HD219134b with two HST visits of 4 HST orbits each. Observations of this target were already done with the same settings (E140H echelle grating) during cycle 23 (Proposal id 14461). Planets and Planet Formation Stellar Physics 3 false true false false false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM K V-IV NO HR-8832 J2000 J2000 U=7.460, B=6.560 STIS/FUV-MAMA Spectroscopic No No E140H 1234 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. /Users/baptistelavie/Documents/Observations/Proposals/HD219134/HST/Mid_cycle_25/phaseII/OP-cache/HD219134_PhaseII-v01.xml (Tic-Visit :proposal-id 15430 :visit-id "01" :proposal-version -1 :trans-version "20171009" :date "05-Dec-2017 16:50:28.0" :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 837600 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15430 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15430 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2677 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 582 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) true 4 0 Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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 scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. /Users/baptistelavie/Documents/Observations/Proposals/HD219134/HST/Mid_cycle_25/phaseII/OP-cache/HD219134_PhaseII-v02.xml (Tic-Visit :proposal-id 15430 :visit-id "02" :proposal-version -1 :trans-version "20171009" :date "05-Dec-2017 16:50:32.0" :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 837600 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15430 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15430 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2677 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 263 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15430 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 582 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) true 4 0 Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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. Using previous spectrum obtained with proposal 14461, the count rate for the entire detector in 2127s is ~180 counts/s. The maximum buffer time should thus be 2x10^6 / 180 ~ 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.