Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details. 0 Assigned ID: 2884 ----- Attempting Submission 1 (Wed Mar 23 16:13:35 GMT 2022) ----- Our observations are feasible with the Cycle 30 LP specifications for COS. 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 LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY INEFFICIENT ORDERING OF FP-POS POSITIONS REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE 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 LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY COS LP6 EXPOSURE WITH MORE THAN 2400 SECONDS VISIBILITY Adjusted all remaining COS visits to use a single FP-POS. This is necessary for wavelength and flux stability for the proposal's science case. -448143544 ----- Attempting Submission 1 (Fri Jul 08 19:15:40 GMT 2022) ----- HST Phase II Proposal 17156 successfully submitted. Receipt: # 17156-1 ----- Attempting Submission 2 (Wed Aug 31 20:13:57 GMT 2022) ----- ----- Attempting Submission 3 (Thu Oct 06 17:22:57 GMT 2022) ----- HST Phase II Proposal 17156 successfully submitted. Receipt: # 17156-3 ----- Attempting Submission 4 (Sun Dec 04 22:43:12 GMT 2022) ----- HST Phase II Proposal 17156 successfully submitted. Receipt: # 17156-4 ----- Attempting Submission 5 (Wed Dec 07 14:33:50 GMT 2022) ----- I believe all of the warnings are OK and none are critical errors. Transit surveys employing small telescopes have revealed a population of ultra-hot gas giant planets (T_eff > 2000 K, R_p > R_Jup) orbiting early-type stars, worlds unlike anything in our solar system. Many of these planets orbit hot host stars (A-type) with very short periods (P_orb < 5 days), experiencing large radiative heating rates. These ultra-hot planets are the most far-ultraviolet (FUV)-irradiated systems known. However, their extreme-ultraviolet (EUV) irradiation, which drives mass loss from traditional hot Jupiters, is likely quite low. We propose an FUV transit spectroscopy experiment to study four planets straddling the ``EUV divide'' to quantify the transition from EUV-driven to FUV-driven escape. We will use these data to measure the dependence of atmospheric ionization and mass loss rate on the relative strengths of the stellar FUV and EUV radiation fields. A-stars emit strong photospheric flux at FUV wavelengths, providing a backlight against which a myriad of outflowing species can be observed. Our FUV spectroscopic program will measure transit depths in never-before-detected low-ionization, neutral, and molecular species believed to be rapidly escaping from the atmosphere of these planets (e.g., S I, Si II, C I, N I, Al II, and possibly CO and He II). These observations will provide mass loss and atmospheric ionization measurements of planets orbiting A-type stars to test the importance of the FUV/EUV radiation environment and characterize atmospheric escape in its most extreme forms. We propose to observe one transit each of KELT-9b, KELT-20b, WASP-33b, and MASCARA-1b using HST's far-UV spectroscopic instruments in a pilot program to 1) detect low-ionization/neutral metal species and possibly molecules in the escaping exoplanetary atmosphere (predicted spectral detections are given below) and 2) model the light curve to infer the mass loss rates (and thus the ultimate fates of these planets). We have based our observing methodology after the 5-orbit transit sequence used for many short-period exoplanet transit observations with HST (e.g., Lecavelier et al. 2012; Vidal-Madjar et al. 2013; Ehrenreich et al. 2015). These observations place the first spectroscopic measurements ahead of the ingress of primary transit, followed by a combination of pre-transit, in-transit, and post-transit phase coverage (see Figure 4). Because these observations of FUV transits around A stars are the first of their kind, we elected to conduct this Small GO pilot program: 5 orbits x 4 targets = 20 total orbits. We will use these results to motivate future spectroscopic investigations of specific targets of interest. Depending on the target brightness, we will employ either the STIS E140M mode or the COS G160M mode. For KELT-9b, which is the brightest target, we will use the STIS instrument with the standard 0.2 arcsecond x 0.2 arcsecond slit and the E140M grating mode. We chose E140M instead of the more-standard G140M mode for several science-focused reasons: First, the G140M mode has an instantaneous bandpass of roughly 50 angstroms, whereas E140M covers approximately 1150-1700 angstrom in a single observation. Second, A stars have strong H I photospheric absorption, so while most transit studies target Lyman-alpha with G140M, we instead focus on the entire rest of the FUV spectrum except Lyman-alpha, necessitating a broader wavelength coverage. Third, KELT-9 is a factor of 10-100 times brighter in the FUV than the typical planet-hosting cool star, making the higher-resolution/broader bandpass E140M mode feasible. We note that jitter-driven spectral resolution degradation (see recent STIS ISR) does not compromise the science return from this program. We have estimated exposure times, signal-to-noise ratios, and verified instrumental safety using the on-line STScI ETCs. KELT-9b is too bright to carry out these observations using the FUV MAMA detector's time-tag mode, so we will operate in the ACCUM mode using observations of a fixed exposure time. We estimate approximately 2800s per observation prior to Earth occultation, and break this into four 700 second exposures per orbit - resulting in a S/N = 18.3 per exposure per spectral resolution element at R~40,000 (STIS.sp.1045254) at 1420 angstroms. This will result in 20 high S/N, high spectral resolution light curve points per visit. KELT-20b, WASP-33b, and MASCARA-1b are fainter and better suited to the higher-sensitivity of the COS instrument. Comparison of UV transit features between COS and STIS has been previously demonstrated (e.g., Linsky et al. 2010; Garcia-Munoz et al. 2021). For KELT-20b, WASP-33b, and MASCARA-1b, we will use the COS G160M mode in time-tagged mode. We chose G160M over the G130M grating used in some previous transit observations (e.g., Linsky et al. 2010; Ben-Jaffel & Ballester 2013) for two primary reasons: 1) the stars are all cooler than 10,000K, meaning that their continuum flux begins to fall precipitously below 1400 angstroms and as noted below, low-ionization species (H I, O I, C II) have strong photospheric and interstellar absorption that will make the transit detection difficult, and 2) several key neutral, low-ionization metals, and (possibly) molecules have strong features in the G160M bandpass (including C I, Si II, Fe II, and CO). The APT observation planning tool indicates approximately 3000s of observing time per orbit for these stars, which we break into three 1000s exposures (note the data will be taken in time-tagged mode, enabling post facto rebinning to arbitrary cadence). The S/Ns per resolution elements (R~16,000) at 1420 angstroms generated by the on-line ETC are ~50, 8, and 8 for KELT-20b, WASP-33b, and MASCARA-1b, respectively. We note that many of the predicted species (e.g., CO, C I) are multiplet features, so we will integrate the lightcurves over many spectral resolution elements, enhancing the detection threshold for these species. Title: Transiting Ultra-hot Gas Giants: Astrophysical Laboratories for Atmospheric Escape Studies PIs: P. W. Cauley and K. France - University of Colorado The Co-PI (Kevin France) and analysis team (Luca Fossati, Christian Schneider, Vincent Bourrier, Wilson Cauley) of this proposal have extensive experience with the analysis and publication of optical and ultraviolet transit spectra and coordinated X-ray observations (France et al. 2016; Loyd et al. 2016; Schneider et al. 2015; Fossati et al. 2010, 2015, 2018; Bourrier et al. 2014, 2016, 2019; Cauley et al. 2017, 2019). We will develop new data analysis tools to study the wavelength-dependent optical depths of the expected large number of spectral features seen for the first time due to the large mass loss rate and the contrast with the FUV photospheric continuum. These tools will include spectral coaddition routines for in-transit and out-of-transit spectra, light curve creation and analysis tools, and spectral fitting routines to characterize line-widths, transit depths, and equivalent widths of prominent features that appear in the outflow of our four target planets. Co-Is Cauley also brings experience with H-alpha transit observations of short-period planets around A-stars. In addition to the observational expertise, our team has conducted modeling analysis of the KELT-9 and KELT-20 systems (Tommi Koskinen, Luca Fossati, Chenliang Huang) to inform the choice of observing modes used in this proposed study. Starting with the detection of Lyman-alpha transit absorption in the HD 209458b system by Vidal-Madjar et al. (2003), considerable HST resources have been devoted to the study of atomic gas outflow from short-period planets. That initial study was followed by the detection of O I, C II, Si III and Fe III on the same planet (Vidal-Madjar et al. 2004, 2013; Linsky et al. 2010, Cubillos et al. 2020). These observations inspired several independent groups to develop 1D, 2D, and 3D models to study both the physical characteristics of the upper atmospheres of close-in planets and the escaping gas and plasma surrounding them (e.g., Koskinen et al. 2007; 2013a,b; Bourrier et al. 2013, 2016, Huang et al. in prep). These data will likely generate new modeling and analysis efforts beyond the proposal team. In contrast with Lyman-alpha, which is not accessible for exoplanets around A stars, C, N, O, Si, Fe, and other metals are heavy minor species. Our team has access to a model that can simulate the escape of these species (Koskinen et al. 2013 a,b; Fossati et al. 2020, 2021, Huang et al. in prep.). This model has been used to show that heavy atoms and ions escape the atmosphere with detectable abundances because they are ``dragged'' along by a sufficient mass flow of lighter H and protons (see Figure 3 for initial model atmospheric temperature profiles for KELT-9b and Figure 1 for a model of WASP-121 b). These models allow us to translate observed planetary transit light curves into global mass loss rates: combining the depth and shape of the lightcurves with the spectral profiles translates directly into the astrophysical observables. In general, we expect elements with ionization potential lower than about 11~--~12 eV to be dominantly ionized while the neutral fraction of elements such as H, O and C that have higher ionization potentials can be significant due to the low EUV flux of the star (see Figure 2). We will complement these tools with the EVE transit spectroscopy modeling code (Bourrier et al. 2013, 2016) to fit the full spectral information contained in the time-series absorption spectra of species we will detect in the exospheres. EVE enables us to take the observational data to derive information about their dynamics, density, and mass loss rates (see references noted above). Exoplanets and Exoplanet Formation 6 false false true false false false false SUPPORTED STAR A0-A3 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR A0-A3 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR F3-F9 NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR A4-A9 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1589 1670423416298 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17156 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "07-Dec-2022 08:30:15.0" :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 1548720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17156 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17156 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "01" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "01" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 450 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) false 5 0 1670423078500 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17156 :visit-id "02" :proposal-version -1 :trans-version "20220630" :date "07-Dec-2022 08:24:37.0" :trans-errors '(:WARNINGS 4 :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 7914560 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17156 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17156 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "02" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "02" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 603 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) false 5 0 1665076014845 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1669454986000 120.35091295679717 (Tic-Visit :proposal-id 17156 :visit-id "03" :proposal-version -1 :trans-version "20220630" :date "06-Oct-2022 12:06:54.0" :trans-errors '(:WARNINGS 11 :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 1783456 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17156 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17156 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "03" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "03" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "03" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 499 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) false 5 0 1670609140261 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /private/var/folders/8t/mg1bkfyj20xf2vfc_9vyhfs80006z1/T/OPVisit14143932642991951030.xml This visit is a duplicate of failed visit 03. (Tic-Visit :proposal-id 17156 :visit-id "53" :proposal-version -1 :trans-version "20220630" :date "09-Dec-2022 13:05:39.0" :trans-errors '(:WARNINGS 11 :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 1783456 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17156 :visit-id "53" :obset-id "53" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17156 :visit-id "53" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "53" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "53" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "53" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "53" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 499 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) true 5 0 1670423143354 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17156 :visit-id "04" :proposal-version -1 :trans-version "20220630" :date "07-Dec-2022 08:25:42.0" :trans-errors '(:WARNINGS 4 :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 1696384 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17156 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17156 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "04" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 2483 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17156 :visit-id "04" :orbit-number 5 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 565 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) false 5 0