0 Assigned ID: 2431 ----- Attempting Submission 1 (Fri Apr 09 23:14:50 GMT 2021) ----- HST Phase I Proposal 2431 successfully submitted. Receipt: # 2431-1 ----- Attempting Submission 2 (Tue Apr 13 22:57:30 GMT 2021) ----- HST Phase I Proposal 2431 successfully submitted. Receipt: # 2431-2 ----- Attempting Submission 3 (Tue Apr 13 23:32:18 GMT 2021) ----- For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. COS EXPOSURE TIME ADJUSTED TO WAVECAL LAMP FLASH DURATION COS EXPOSURE TIME ADJUSTED TO WAVECAL LAMP FLASH DURATION For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. 0 ----- Attempting Submission 1 (Thu Jul 29 00:53:35 GMT 2021) ----- HST Phase II Proposal 16685 successfully submitted. Receipt: # 16685-1 ----- Attempting Submission 2 (Thu Jul 29 21:41:03 GMT 2021) ----- ----- Attempting Submission 3 (Fri Mar 03 22:01:55 GMT 2023) ----- For the first warning could we just ignore the fact that we are not using all 4 positions. For the second warning we are not concerned with the exposure time of the wavecal lamp as we are not getting usable science images on this visit. Low Mass Evaporating Planets: A Search for the Star-Planet Interaction in Kepler-535 Exoplanet-host stars with planets at short separations can influence each other (commonly termed the star-planet interaction or SPI), via a variety of mechanisms. Understanding SPI in exoplanet host stars is thus crucial for understanding the evolution of both the planet and its host star, but observational evidence for SPI is generally scarce. An important signature of SPI is UV emission, and time-resolved FUV spectroscopy with HST/COS has provided compelling evidence for, and details of, the SPI phenomenon in HD189733, which has a Jupiter-mass planet. We now propose to search for SPI in the exoplanet host star Kepler-535, which hosts a 0.21 Jupiter-radius (Rjup) planet. Our search is motivated by an intriguing new result that we have found using GALEX data: stars in which the innermost planet has a radius less than about 0.4 Rjup are statistically much more likely to have high FUV/NUV flux ratios, compared to those where the radius is significantly larger. We hypothesize that this is because it may be easier to get mass-loss from the atmosphere of Neptune and sub-Neptune mass planets as a result of irradiation by the star. When material from this evaporated mass falls onto the star, it gets heated to high temperatures (~50,000K) as has been been observed in HD189733. The high temperature plasma results in a high FUV/NUV ratio. We propose to use COS spectroscopy of diagnostic FUV lines that can effectively probe the amount of mass evaporating from the planet, and help in determining the dynamics of the gas around the planet. The results from this study will enable testing state-of-art MHD models of such systems. Our goal is to obtain time-resolved spectroscopy of the planet bearing star Kepler-535 with COS, at planetary orbital phases in the range ~ 0.5-0.63. We will use the G130M grating with central wavelength set to 1281 A in order to cover the range ~1150-1450 A, as in the study of FUV-line variability in the exoplanet host-star HD 189733 by Pillitteri et al. (2015), in order to cover the major FUV lines that probe hot gas (~20, 000 to 100,000 K). The main lines in this range are the H Lya, Si II, Si III, Si IV, C II, C III lines, and N V lines. We will need 5 orbits to observe the egress of the planet from secondary transit sampling the same orbital phase range in Petal15 (0.499-0.625). By taking the observations in TIME-TAG mode, we will be able to look for any changes in the line profiles in the 1150-1450 A range on short time-scales (1-40 min). We have used the GALEX FUV-band flux density for Kepler-535 (32 uJy) to estimate the expected line fluxes for it as follows. Taking the average flux of each lines observed with COS in HD189733 (table 4 of Petal15) that lies in the FUV GALEX bandpass (1344-1786A A), from epoch 1, we estimate the contribution of each line to a GALEX band-averaged FUV flux density - the strongest of these lines (e.g., Si IV 1403) have typical fluxes of few X 10|^-15 erg cm^-2 s^-1. In contrast, the brightest lines observed by Petal15 lie shortwards of the blue edge of the GALEX FUV bandpass, e.g., the CII 1335 doublet, which has a typical flux of few X 10^-14 erg cm^-2 s^-1. In order to estimate the contribution of lines that lie within the GALEX FUV band but were not covered in the COS spectra taken by Petal15, we used the following procedure. We (i) constructed three high temperature collisionally excited plasma models using the CLOUDY code, at the temperatures of the three components derived for the plasma flow by Petal15 (25,000, 50,000 and 80,000 K) and averaged them, (ii) scaled the resulting average spectrum to an observed flux of the Si IV1403 line of 3 X 10^-15 erg cm^-2 s^-1, and (iii) integrated the resulting spectrum over the GALEX FUV bandpass (using the FUV filter transmission curve) to derive an expected GALEX FUV-band flux of ~10 uJy for HD189733. Since the observed FUV flux of Kepler-535 is 32 uJy, we expect, conservatively assuming that it is experiencing mass-loss at a rate that is one-third that of HD189733b, that its lines will be roughly as bright as those observed towards HD189733. We note that the signal-to-noise ratio of the bright lines observed with COS towards HD189733 is quite high (S/N~20), so even if the lines we observe are a further factor 2 lower than estimated, we will still be able to detect these lines with adequate sensitivity in order to be able to robustly detect flux variations of 25% or more (note that Petal15 find variations of a factor ~2 towards HD189733). We will 2 sub-exposures per visit (with FP-POS=3 and FP-POS=4since FP-POS=ALL is not available for the grating we need to cover our desired wavelength range) , with typical integration times of 930 sec each, per epoch. Each set of 2 exposures requires one orbit. Sahai, Principal Research Scientist at the Jet Propulsion Laboratory, brings over 3 decades of observational experience in studying mass loss in evolved stars, using all major space-based and ground-based observatories (e.g., HST, Chandra, XMM-Newton, Spitzer, ISO, GALEX, SOFIA, Keck, VLA, ALMA) to the proposed study. He has extensive experience with modeling of multiwavelength data to investigate the complex processes of mass loss. During the last decade, much of his work has focussed on using UV (and X-ray) observations to study a new sub-class of AGB stars that show highly variable UV and X-ray emission, likely associated with accretion activity around main-sequence companions. He is well-versed in the analysis of HST UV TIME-TAG data - one of his recent papers used this analysis to discover and characterize flickering activity in an AGB star due to an accretion flow. During the last two years, he has worked extensively on the UV properties of exoplanet host stars using the GALEX archive, and a paper is nearing completion. In support of this work, he authored a proposal to the NASA-RFI NNH17ZDA010L: Possible NASA Astrophysics SmallSats (Topic 1: Science Mission Concepts) entitled "SPLINE - The Star PLanet INteraction Explorer", that would use a 40-cm telescope to study SPI by monitoring the FUV spectrum in the 1300-1600 A range. Gardner is a PhD student and National Science Foundation Graduate Research Fellow whose interest and research lies within the characterization and detection of extra-solar planets. She is using diffuser-assisted, multi-broadband transit photometry at the University of Wyoming's 2.3m telescope to probe the atmospheres around close-in, "hot" Jupiter exoplanets. She is also involved in the mechanical design and commissioning of a new high resolution radial velocity spectrograph at UW that was designed for TESS exoplanet candidate reconnaissance. The data obtained in this proposal will be used as part of her Ph.D. thesis. Sahai will lead the scientific effort, being responsible for the overall management of the study, major scientific analyses and final publication of the results. Exoplanets and Exoplanet Formation Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED STAR EXTRA-SOLAR PLANET G III-I NO This object was generated by the targetselector and retrieved from the SIMBAD database. 2MASS-J19461599+4941465 J2000 J2000 B=13.66, J=12.14, H=11.91, K=11.85 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1309 Timing link suitability includes constraints ([Sequence (01 02) within 0.2 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16685 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "03-Mar-2023 14:53:55.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 52304 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16685 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16685 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2045 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) false 1 0 Timing link suitability includes constraints ([Sequence (01 02) within 0.2 days] [Sequence (02 03) within 0.2 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. 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(Tic-Visit :proposal-id 16685 :visit-id "03" :proposal-version -1 :trans-version "20220630" :date "03-Mar-2023 14:53:58.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 52304 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16685 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16685 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2345 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) false 1 0 Timing link suitability includes constraints ([Sequence (03 04) within 0.1 days] [Sequence (04 05) within 0.1 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. 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