New FUV diagnostics of the atmosphere of the hot-Jupiter HD 209458b with HST/COS

0 Assigned ID: 501 ----- Attempting Submission 1 (Fri Apr 10 15:04:08 GMT 2015) ----- HST Phase I Proposal 501 (hd209UVv1.apt) successfully submitted. Receipt: # 501-1 ----- Attempting Submission 2 (Fri Apr 10 22:52:25 GMT 2015) ----- 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. ORBITAL VISIBILITY OVERRUN Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. 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. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. 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. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Dear Bill For Visit 3, I set SCHED to 50, and shortened the exposure and buffer times to reduce a total of 90-100 secs per orbit. FYI: I am getting a warning of a visibility overrun in Visit 01 exposure 4 that I cannot edit. See below. Gilda Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN Occurrence: 01 Explanation: Applies to: #<Container for exposure 004> An exposure or exposures which required visibility was forced to overlap with the occultation. The exposure(s) can be removed from occultation by specifying different exposure times for the exposures in the orbit, or by specifying a different orbit number for the offending subexposure(s). Clicking on the offending subexposure in the Orbit Planner display will select the corresponding subexposure in the spreadsheet. -1929248395 ----- Attempting Submission 2 (Mon Nov 02 20:01:30 GMT 2015) ----- HST Phase II Proposal 14090 (GO-14090-phase2v2.apt) successfully submitted. Receipt: # 14090-2 ----- Attempting Submission 3 (Mon Nov 02 21:09:26 GMT 2015) ----- HST Phase II Proposal 14090 (GO-14090-phase2v3.apt) successfully submitted. Receipt: # 14090-3 ----- Attempting Submission 4 (Mon Nov 23 19:58:34 GMT 2015) ----- HST Phase II Proposal 14090 (GO-14090-phase2v4.apt) successfully submitted. Receipt: # 14090-4 ----- Attempting Submission 5 (Wed Nov 25 19:57:37 GMT 2015) ----- We now specify a different FP-POS per visit in order to satisfy the multiple FP-POS usage for the whole program. The single grating setting and FP-POS per visit will maintain the stability in the instrumental setup that is needed to reliably measure the planetary transit absorption and its spectral signature in a given visit. This has been demonstrated in our previous analyses of COS FUV archival data of HD 189733b (Ben-Jaffel & Ballester 2013) and of our target HD 209458 (Ballester & Ben-Jaffel 2015). New FUV diagnostics of the atmosphere of the hot-Jupiter HD 209458b with HST/COS As the first known transiting exoplanet, HD 209458b has set various precedents in the study of the lower and upper atmospheres of worlds beyond our solar system. The discovery with HST STIS/G140L FUV transit observations of this hot Jupiter of an extended upper atmosphere of H I and heavy O I and C II species has driven much theoretical work to explain the heating and inflation at high altitudes caused by the large XUV input from the nearby star. Our recent work shows however that the stellar activity and XUV input have been significantly overestimated in all previous studies. With up-to-date upper-atmosphere models combined with magnetospheric simulations, we find that for the STIS results of line-integrated absorptions of about 10%, the extended distributions of O I and C II should be accompanied by broad line-absorption profiles from non-thermal processes together with supersolar abundances in O and C, and the planet may also possess an extended magnetosphere. The picture is degenerate, but can be significantly improved if detections better than the 2-3 sigma measurements from STIS are obtained. The unique FUV capabilities of HST COS/G130M will be exploited for this key target. Line-integrated absorptions in both O I and C II will be measured at ~ 5-10 sigma. For the first time, absorption line profiles will be adequately resolved, with information on Doppler shifts and equivalent widths to help distinguish between atmospheric scenarios and potential magnetospheric phenomena. Will observe HD 209458 during three transits of its hot Jupiter, spanning 4 HST orbits per transit. Each visit will start with the planet around orbital phase 0.957-0.970 to observe before transit (orbit 1), during transit (orbits 2 and 3) and after transit (orbit 4) and properly sample the baseline stellar fluxes. We will use COS G130M in time-tagged mode with the 1291 grating setting and a single FP-POS per visit, in order to sample all O I 1304, C II 1335, and Si III 1206 Ang simultaneously, and to keep a consistent zero wavelength and dispersion. This is key for the program's goal of measuring the planetary absorption line profiles. The repeatability provided by a single setup together with the time-tagging of the data will also allow for selection of part of the exposures with respect to the sampling of the transit light curve as needed per visit. Ideally there should be the lowest possible geocoronal (O I 1304 Ang) background as is possible when observing near opposition (near SHADOW conditions). However, the timing of the transits is a stronger time scheduling constraint, and we need to observe 3 transits to build up the S/N, hopefully all in this cycle. EXTRA-SOLAR PLANETS 12 false true false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM NO G0V star. This object was generated by the targetselector and retrieved from the SIMBAD database. V376PEG HD209458 J2000 J2000 B=8.21 J=6.591 COS/FUV Spectroscopic No No G130M 1291 1449229948037 /private/var/folders/zc/ljhf1lgn10b1yd9ytmwlp4jr00070l/T/OPVisit8726799586517372547.xml The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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