Connecting the lower and upper atmospheres of a warm-Neptune. Implications for planetary evolution.

0 Assigned ID: 692 ----- Attempting Submission 1 (Fri Apr 08 18:54:07 GMT 2016) ----- HST Phase I Proposal 692 (hatp11b.apt) successfully submitted. Receipt: # 692-1 ----- Attempting Submission 2 (Fri Apr 08 20:24:53 GMT 2016) ----- HST Phase I Proposal 692 (hatp11b.apt) successfully submitted. Receipt: # 692-2 ----- Attempting Submission 3 (Fri Apr 08 22:36:56 GMT 2016) ----- HST Phase I Proposal 692 (hatp11b.apt) successfully submitted. Receipt: # 692-3 not clear why visit planner is needed, and not working. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. Current - ACQ/PEAK and SCI aperture changed tp 52x0.05D1 for STISFUV visit, visit 02. Previous - target acquisiton changed to spectroscopic acquisition. -1409636567 ----- Attempting Submission 1 (Wed Jul 20 23:19:52 GMT 2016) ----- ----- Attempting Submission 2 (Fri Oct 14 15:47:50 GMT 2016) ----- HST Phase II Proposal 14625 (GO-14625.apt) successfully submitted. Receipt: # 14625-2 ----- Attempting Submission 3 (Fri Oct 14 19:42:02 GMT 2016) ----- HST Phase II Proposal 14625 (GO-14625.apt) successfully submitted. Receipt: # 14625-3 ----- Attempting Submission 4 (Wed Oct 26 18:39:21 GMT 2016) ----- We must use COS/G130M (1291) with a single FP-POS (and single CENWAVE) over the full visit to keep a consistent zero wavelength (and dispersion). The S/N of the stellar lines is not large enough to adequately correlate and co-add spectra of different FP-POSs (as found for archival HD 209458 COS spectra with multiple FP-POSs; Ballester & Ben-Jaffel, ApJ 2015). This requirement was stated in the Phase 1 proposal, to obtain reliable wavelengths and shapes of the planetary line absorption profiles that will constrain the results and modeling. A single FP-POS per visit was used in our Cycle 23 GO 14090 program on HD 209458b, of FP-POS=2, 3, and 4. Here we chose FP-POS=1 to compensate for the health of the detector, but it can be changed. A balance of single FP-POSs is recomended in the Cycle 24 COS IHB, Sec. 5.8. Connecting the lower and upper atmospheres of a warm-Neptune. Implications for planetary evolution. The FUV transit technique specific to HST is unique at characterizing the upper atmospheres of exoplanets. Indeed, the uppermost layers of a planet orbiting close to an EUV-bright star undergo great heating, inflation and mass escape. FUV transit observations of the warm-Neptune GJ 436b have revealed an immense H I cloud with an escaping cometary tail, evidencing substantial mass loss that can significantly affect the atmospheric composition and evolution of the planet. As known to take place on hot Jupiters, the outflow of the light hydrogen-dominated escaping material can drag along heavier species. All three key atoms of H I, O I, and C II that reside in the uppermost layers have strong resonant FUV lines. Here we propose FUV transit observations of the warm-Neptune HAT-P-11b, which is the only low-mass exoplanet to have positively revealed water absorption in a relatively clear lower atmosphere, thus showing that oxygen is available in measurable amounts in its bulk atmosphere. One transit will be made with STIS/G140M and another with COS/G130M, which will measure the spatial extent as well as global velocity/energy properties in all three H I, O I, and C II atoms. With such data we can study the processes involved in the escape and space physics environment. Together with comprehensive, iterative modeling of the lower and upper atmospheres, and of the magnetosphere expected for these planets, we can gain insight into the composition and escape in the uppermost planetary regions, and into how they relate to the lower atmosphere and thus the planetary properties. We will observe two transits of HAT-P-11b, 5 HST orbits each: one with COS/G130M (1291) to sample O I and C II lines, and the other with STIS/G140M (1222) for H I Ly-alpha. For both instruments, a single time-tagged exposure will be taken during each orbit. Both visits should start with the planet around orbital phase 0.961-0.964 to observe before, during and after nominal transit. If possible, the COS visit should be the one scheduled the closest possible to opposition (near SHADOW) for minimum geocoronal O I 1304 A. COS: COS/G130M (1291) must be used with a single FP-POS (and single CENWAVE) over the full visit. The need was stated in the Phase 1 proposal to obtain consistent zero wavelengths and line shapes of the planetary line absorption profiles. The stellar lines will not be bright enough to adequately correlate and co-add spectra of different FP-POSs (as found for archival HD 209458 COS spectra with multiple FP-POSs; Ballester & Ben-Jaffel, ApJ 2015). Single FP-POSs per visit of 2, 3, and 4 were used in our Cycle 23 GO 14090 program on HD 209458b. Here we chose FP-POS=1 to compensate for the detector health between programs (Cycle 24 COS IHB, Sec. 5.8), but the value can be changed. STIS: WAVECAL=NO was approved and we will execute a WAVE calibration exposure after each orbit's visibility. Extrasolar Planets and Planet Formation 12 false true false false false false AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM K III-I NO This object was generated by the targetselector and retrieved from the SIMBAD database. 4780 K2V-K4V star. J2000 J2000 STIS/FUV-MAMA Spectroscopic No No G140M 1222 COS/FUV Spectroscopic No No G130M 1291 1476473952518 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 1477648487000 77.2924147315507 (Tic-Visit :proposal-id 14625 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "14-Oct-2016 12:39:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 939392 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14625 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14625 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3019 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3352 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3130 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3352 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3130 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3352 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3130 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3352 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3130 :al-overhead-at-end 0 :internal-dur-at-end 417 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3352 :pcs-gap 0 ) false 5 0 The ETC was run with a COS/G130M spectrum of HD 189733, which of similar type and activity level, and closer in at 19 vs 37 pc. /private/var/folders/n5/3r9vhghn4_902ty53m9y2sm8000xls/T/OPVisit7555787256334421912.xml 1477506675694 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14625 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "26-Oct-2016 11:31:15.0" :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 1061728 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14625 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14625 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2657 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2777 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2777 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2777 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14625 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2777 :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 2999 :pcs-gap 0 ) true 5 0 Saturation is calculated at 0.19 seconds. Minimum exposure time (0.1 seconds) used here, target has Vmag=9.47, which is within limiting magintude of 8.4 with F28X50LP (Table 8.3 STIS handbook). ETC for STIS/G140M spectrum of FUV-brighter star HD-189733.