0 Assigned ID: 2330 ----- Attempting Submission 1 (Fri Apr 09 22:01:03 GMT 2021) ----- LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. ORBITAL VISIBILITY OVERRUN LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. LIFETIME-POS is required with G140L when not in Supported mode. Duplicated visit 4 into visit 54 for repetition after failure. 2042102540 ----- Attempting Submission 1 (Fri Jul 30 00:47:35 GMT 2021) ----- HST Phase II Proposal 16659 successfully submitted. Receipt: # 16659-1 ----- Attempting Submission 2 (Wed Sep 01 14:54:03 GMT 2021) ----- HST Phase II Proposal 16659 successfully submitted. Receipt: # 16659-2 ----- Attempting Submission 3 (Mon Sep 13 22:06:17 GMT 2021) ----- ----- Attempting Submission 4 (Tue Nov 02 21:38:39 GMT 2021) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 5 (Wed Dec 01 23:29:07 GMT 2021) ----- ----- Attempting Submission 6 (Sun Jan 16 22:13:59 GMT 2022) ----- ----- Attempting Submission 7 (Tue Jan 25 13:58:19 GMT 2022) ----- ----- Attempting Submission 8 (Fri Apr 29 15:20:39 GMT 2022) ----- ----- Attempting Submission 9 (Thu Jul 07 14:29:08 GMT 2022) ----- ----- Attempting Submission 11 (Wed Feb 15 23:27:56 GMT 2023) ----- ----- Attempting Submission 12 (Tue Oct 24 18:47:27 GMT 2023) ----- ----- Attempting Submission 13 (Sat Nov 25 16:42:11 GMT 2023) ----- Some of the tools cannot be executed because related to BOP visits Accreting white dwarfs as probes of compact binary evolution In the last 20 years, the study of compact interacting binaries has led to two major breakthroughs in astrophysics: the discovery of dark energy and the first detection of gravitational waves. Although binaries are critically important to probe the properties of the Universe and to test fundamental physical theories, our understanding of their evolution and final fate is still far from being complete. Accreting white dwarfs are ideal laboratories in which to test the models of compact binary evolution. We here propose a COS Treasury program specifically designed to explore those regions of the parameter space that have been previously poorly studied and where major discrepancies between the theory and observations are found. Combining the high-quality ultraviolet data with the parallaxes from Gaia, we will accurately measure effective temperatures, masses and accretion rates for 43 accreting white dwarfs (the minimum number required to homogeneously sample the entire physical parameter space spanned by this diverse population) thereby testing the mechanisms of angular momentum loss which drive the evolution of all kinds of binaries. The white dwarf masses are a key ingredient in the pathway toward Supernova Type Ia explosions and by obtaining their accurate values, we will constrain both the single and the double-detonation scenarios. Finally, only the ultraviolet allows the detection of the nitrogen and carbon resonance lines. From their abundances, we will establish the formation channel for the most compact systems, which will later be used to verify the performance of the space-mission LISA and calibrate the detector for future gravitational wave source discoveries. The aim of this program is to obtain far-ultraviolet COS/G140L and STIS/E140M spectroscopy of 43 accreting white dwarfs (WDs). While past HST observations have studied in detail systems in the range 70 min < Porb < 150 min, very few observations have been obtained of long- (Porb > 150 min) and short- (Porb < 60 min) period accreting WDs, which are therefore the targets of this proposal. We have screened the literature for systems that are bright enough to be observed in 3-5 HST orbits each. The set of targets was chosen to ensure a homogeneous sampling across the Porb range and to maximise the chances of detecting the white dwarf in the UV, and avoiding frequently outbursting systems. The actual observations are relatively straight-forward: target acquisition, depending on the target brightness, will be done with NUV imaging, or in dispersed light using the G140L grating. The coordinates and proper motions are drawn from Gaia EDR3, hence we do not precede the observations with a search pattern. Depending on the target brightness, the COS G140L spectroscopy will extend over 2, 3, 4, 5 or 6 orbits. We will make use of all 4 FP-POS positions. Our targets can be divided in two sub-classes according to their observational properties: 1) Dwarf novae: systems characterised by quiescent states of low-mass transfer rates onto the WD, interrupted by bright disc outbursts, during which the binary typically brightens by 2-5 magnitudes. In order to ensure that HST spectroscopy is obtained during quiescence, when the WD is the dominant emission source and safe to be observed, we will obtain intensive continuous ground-based monitoring up until 24 h prior to the HST observations. 2) Nova-likes: systems in the period range 180 min < Porb < 240 min are typically characterised by high average accretion rates which keep the disc in a stable hot state, equivalent to a permanent outburst. Occasionally the accretion rate drastically drops ("low state"), unveiling the WD. Our sample contains nine systems falling in this category. We will photometrically monitor them from the ground and the HST observations will be triggered via a non-disruptive ToO only once a low state is detected. We expect to detect ~3 systems in low state per year and the observations of these targets will be carried out over the over the next three cycles, in order to observe nine of these systems by the end of the program. Several of the targets are eclipsing (GS Pav, V1239 Her, 2MASS J15445360+2553488, YZ LMi, ZTFJ040749.30-000716.67, ASASSN-14cn, ZTF-J2252-0519). We have included their ephemeris in order for the target acquisition to be scheduled such that it avoids the eclipse (in a similar strategy as that of HST program 12870). Impact of reduced-gyro operations: For the dwarf nova targets, we do not expect major impacts on our program in case of reduced-gyro operations. Prolonged acquisition procedures will not significantly affect the SNR we can achieve, while a possible extension of our program into the next cycle will not preclude our science goals, nor affect in any way the feasibility of our observations. Instead, with time critical observations becoming much more difficult to schedule, reduced-gyro operations could potentially affect the observations of the nova-like targets, for which long-term non-disruptive ToOs are necessary. The additional nova-likes targets we have include can possibility mitigate the limitations related to reduced-gyro operations by offering (i) alternative pointings that can compensate for the limited sky accessibility, (ii) alternative observing windows that could be more easily included in the schedule. Anna Pala is an expert in the analysis of HST/COS ultraviolet spectra of accreting white dwarfs, focusing in particular on their interpretation in the context of compact binary evolution (e.g. Pala et al. 2017MNRAS.466.2855P). Thomas Kupfer, Paul Groot and Matthew Green are experts on the detailed analysis of photometric and spectroscopic data of accreting white dwarfs with a focus on systems with Porb < 60 min to (i) put constraints on the evolutionary history of individual systems (e.g. Green et al. 2018MNRAS...476..1663G, Kupfer et al. 2016MNRAS.457.1828K, Groot et al. 2001ApJ...558L.123G) and (ii) obtain a more coherent picture of the population of known systems (Kupfer et al. 2013MNRAS.432.2048K). Boris Gaensicke has been using HST for ultraviolet spectroscopy of accreting white dwarfs since Cycle 6, focusing on the study of their fundamental parameters and evolution of (e.g. Gaensicke et al. 2003ApJ...594..443G). Matthias Schreiber, Dean Townsley, Gijs Nelemans and Christian Knigge are experts in modelling the evolution of accreting white dwarfs. They will provide the theoretical background against which the data will be analysed (e.g. Schreiber et al. 2016MNRAS.455L..16S, Townsley & Gaensicke 2009ApJ...693.1007T, Nelemans et al. 2016ApJ...817...69N, Knigge et al. 2011ApJS..194...28K). Tom Marsh, Paula Szkody and Odette Toloza are experts in the analysis of time-resolved observations, focusing on the study of pulsating accreting white dwarfs from time-tagged HST/COS spectroscopy (e.g. Marsh et al. 2016Natur.537..374M, Szkody et al. 2017AJ....153..123S, Toloza et al. 2016MNRAS.459.3929T) and on the modelling of eclipse light curves (e.g Marsh et al. 2014MNRAS.445..309M). Elme Breedt is an expert on studying the population of accreting white dwarfs based on large scale surveys like CRTS (e.g. Breedt et a. 2014MNRAS.443.3174B). Knox Long, Edward Sion, Patrick Godon, Pablo Rodrigues-Gil, Domitilla de Martino and Gagik Tovmassian have a detailed experience in the analysis and interpretation of ultraviolet data of accreting white dwarfs, particularly (i) in the study of low states of systems in the period range 180 min < Porb < 240 min and in the determination of their fundamental parameters (e.g. Pablo Rodrigues-Gil et al. 2004A&A...424..647R, de Martino et al. 2008A&A...481..149D, Tovmassian et al. 2017A&A...608A..36T) and (ii) in modelling the ultraviolet emission of the accretion flows, winds and boundary layers in accreting white dwarfs (e.g. Long & Knigge 2002ASPC..261..327L, Sion et al. 2011ApJ...741...63S, Godon et al. 2016ApJ...833..146G). Stella Kafka is the director of the American Association of Variable Star Observers (AAVSO) and will co-ordinate the ground-based photometry accompanying the HST/COS campaign. Stellar Physics and Stellar Types 0 false false true true false false false false AVAILABLE STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 NUV = 17.49, Gaia EDR3 1925596502097065344, G=16.2, parallax = 1.17(4) mas. STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 FUV = 13.4, Gaia EDR3 4951395327129718528, G=13.5, parallax = 2.04(1) mas. STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 FUV=14.0, NUV=13.8, Gaia EDR3 2329317895999827840, G=13.6, parallax = 1.64(2) mas. UNIDENTIFIED BLANK FIELD NO This target is a blank piece of sky whihc is the bright object safe pointing and is 9.723" away at PA 47.2 degrees from GD-1662 J2000 STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 FUV=16.5, NUV=16.5, Gaia EDR3 552158697769217664, G=15.04, parallax = 1.09(2) mas. STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 Gaia EDR3 3436435910858051200, G=18.6, parallax = 2.2(2) mas. UNIDENTIFIED BLANK FIELD NO This target is a blank piece of sky which is the Safe target offset position for science visit 07. It is 9.706" away at PA 233.0 degrees from V-KR-AUR J2000 STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 FUV = 16.2, Gaia EDR3 4222299752184927616, G=14.8, parallax = 1.53(3) mas. STAR INTERACTING BINARY IRREGULAR VARIABLE NOVA-LIKE NO J2000 J2000 FUV=16.7, NUV=16.5, G=13.9, Gaia EDR3 4124654392314770048, G=parallax=2.07(1) mas. COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16659 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "21-Oct-2021 15:51:22.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 313136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16659 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16659 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2536 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2929 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2537 :al-overhead-at-end 0 :internal-dur-at-end 410 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2929 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 2 more magnitudes. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 2 more magnitudes. Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16659 :visit-id "02" :proposal-version -1 :trans-version "20210514" :date "21-Oct-2021 15:51:23.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 313136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16659 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16659 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2534 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 410 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2927 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 2 more magnitudes. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 2 more magnitudes. Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). The scheduling data was generated by CASM 31.1. CASM was run in Phase II mode. This should be scheduled in evening local-time on a thursday or friday. Flags need to be cleared during the work day. Weekends & holidays are to be avoided since the CS must clear the target within 24 hours of HST execution 1700187856000 79.0 (Tic-Visit :proposal-id 16986 :visit-id "04" :proposal-version -1 :trans-version "20230626" :date "24-Oct-2023 15:00:59.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 713296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "04" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2467 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16986 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2518 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. The scheduling data was generated by CASM 31.1. CASM was run in Phase II mode. /private/var/folders/z3/xy_g1v_s5fz9yrhzb8thz4cr0001qc/T/OPVisit414298711653930755.xml This should be scheduled in evening local-time on a thursday or friday. Flags need to be cleared during the work day. Weekends & holidays are to be avoided since the CS must clear the target within 24 hours of HST execution (Tic-Visit :proposal-id 16986 :visit-id "54" :proposal-version -1 :trans-version "20230626" :date "27-Nov-2023 11:16:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 713296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "54" :obset-id "54" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "54" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2467 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16986 :visit-id "54" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2518 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) true 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. This visit allocates and sets up the safe position offset slot for visit 04 which will use that slot. this S/C visit should go 3-5 days before visit 04. This visit will only contain one exposure 1699871238000 79.0 false -1 -1 This visit is for BOP checking the safe target only and should not execute onboard HST. (Tic-Visit :proposal-id 16986 :visit-id "04" :proposal-version -1 :trans-version "20230626" :date "24-Oct-2023 15:00:59.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 713296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "04" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2467 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16986 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2518 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.6 (as measured from IUE data obtained in low state), through the ETC. The exposure time allows for the system fading another magnitude. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. Buffer-time set conservatively short in case the system is observed in a brighter state than the low state minimum. The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16659 :visit-id "06" :proposal-version -1 :trans-version "20210514" :date "21-Oct-2021 15:51:26.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 426224 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16659 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16659 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2615 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3008 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "06" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3008 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "06" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2616 :al-overhead-at-end 0 :internal-dur-at-end 410 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3008 :pcs-gap 0 ) false 3 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. Exposure time based on a 50000K WD model, scaled to the distance to the system, but conservatively allowing for the target fading two more magnitudes. Exposure time based on a 50000K WD model, scaled to the distance to the system, but conservatively allowing for the target fading two more magnitudes. Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Timing link suitability includes constraints ([07 After 0O by at least 3.0 days]) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. This should be scheduled on a Thursday/Friday evening local time. 1678513839000 90.0 (Tic-Visit :proposal-id 16986 :visit-id "07" :proposal-version -1 :trans-version "20220630" :date "16-Feb-2023 10:35:55.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 330560 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16986 :visit-id "07" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2536 :al-overhead-at-end 0 :internal-dur-at-end 426 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) false 2 1 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. Computed assuming a WD model with Teff=30000K, scaled to NUV=18 (allowing the target to be fainter by one magnitude compared to previous low state observations obtained with Swift). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Timing link suitability includes constraints ([07 After 0O by at least 3.0 days]) The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. This visit allocates and sets up the safe position offset slot for visit 07 which will use that slot. This S/C visit should go earlier in the week while Visit 07 will be 3-5 days later. The S/C visit will only contain 1 exposure 1678082287000 90.0 (Tic-Visit :proposal-id 16986 :visit-id "0O" :proposal-version -1 :trans-version "20220630" :date "16-Feb-2023 10:35:55.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "11" :si-bright-earth-limb-angle 20.0 :data-volume 0 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "0O" :obset-id "0O" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "0O" :orbit-number 1 :pcs-time 383 :si-vis-utilization 5 :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 3165 :pcs-gap 0 ) false 1 0 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. This visit is for BOP checking the safe target only and should not execute on board HST (Tic-Visit :proposal-id 16986 :visit-id "0P" :proposal-version -1 :trans-version "20220630" :date "16-Feb-2023 10:35:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 330560 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16986 :visit-id "0P" :obset-id "0P" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16986 :visit-id "0P" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16986 :visit-id "0P" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2536 :al-overhead-at-end 0 :internal-dur-at-end 426 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. Computed assuming a WD model with Teff=30000K, scaled to NUV=18 (allowing the target to be fainter by one magnitude compared to previous low state observations obtained with Swift). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16659 :visit-id "08" :proposal-version -1 :trans-version "20210514" :date "21-Oct-2021 15:51:27.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 374064 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16659 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16659 :visit-id "08" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2525 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2918 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "08" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2526 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2918 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "08" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2526 :al-overhead-at-end 0 :internal-dur-at-end 382 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2918 :pcs-gap 0 ) false 3 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 1 more magnitudes. I ran a WD spectrum with Teff=50000K, scaled to the distance to the system, through the ETC. The exposure time allows for the system fading 1 more magnitudes. Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16659 :visit-id "09" :proposal-version -1 :trans-version "20210514" :date "21-Oct-2021 15:51:28.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 313136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16659 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16659 :visit-id "09" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2536 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2929 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16659 :visit-id "09" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2537 :al-overhead-at-end 0 :internal-dur-at-end 410 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2929 :pcs-gap 0 ) false 2 0 LONG-TERM TOO This is one of the targets in which the white dwarf is visible only during a low state. We will trigger the ToO when the occurrence of a low state is detected by our ground-based monitoring. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.8 (as measured from Galex photometry in low state), through the ETC. The exposure time allows for the system fading another magnitude. I ran a WD spectrum with Teff=50000K, scaled to FUV=16.8 (as measured from Galex photometry in low state), through the ETC. The exposure time allows for the system fading another magnitude. Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state). Buffer-time set conservatively short in case the system is brighter (which will still be safe, but the buffer would overflow if set to the appropriate value for the low state).