First submission of Phase 1 proposal: Wind Structure of 31 Cygni from UV Eclipse Mapping.-1737567069Assigned ID: 4671
----- Attempting Submission 1 (Wed May 24 21:35:29 GMT 2023) -----This is a Phase II resubmission for program 17416 implementing (slightly) revised STIS grating & aperture configurations for the 31 Cyg total eclipse Visits 4 & 5
(Mar 2024) when the bright UV continum of the target (31 Cyg) will be absent, and rescheduling Visit 8 (egress) to mid-May 2024.
For the eclipse visits (Visits 4 & 5), we propose to observe 31 Cyg with the medium-resolution STS echelle gratings (E140M & E230M) using the
bare 0.2X0.06 aperture, instead of the neutral density 31X0.05NDB slit used for out-of-eclipse observations. Otherwise, the
sequence of planned science exposures for the eclipse visits (Visits 4 & 5) is the same as for (all other) out-of-eclipse visits.
We have also included updated ETCs for the eclipse observations, based on observed UV eclipse spectra of 31 Cyg obtained with FUSE and IUE, to confirm
that these observations do not exceed the MAMA bright limits.
About 150s of unused orbit time has also been left at the end of the (1st and only) orbit for Visits 4, 5 & 8, in order to make these visits schedulable in the Visit Planner.
When this unused time is present, the range of schedulable dates shown in the Visibility Planner is greatly expanded, and allows the total eclipse period to be
properly sampled. With this change, we have now rescheduled the planned Visit 8 for mid-May 2024 to better sample the egress from eclipse. Without the
additional 150s of unused time left in the orbit, this visit is not schedulable (in fact, no schedulable time would be available in May 2024).
The only other change involves renumbering the later visits. The inclusion of this additional May 2024 visit (now Visit 8) means that the former Visit 8 (in June 2024)
now becomes Visit 9, and the former Visit 9 (in Sept 2024) now becomes Visit 10. The previously planned Jan-Feb 2025 visit (the former Visit 10) has been deleted.469639394----- Attempting Submission 2 (Fri Sep 29 18:31:52 GMT 2023) -----
HST Phase II Proposal 17416 successfully submitted.
Receipt: # 17416-2
----- Attempting Submission 3 (Tue Oct 17 01:59:50 GMT 2023) -----Wind Structure of 31 Cygni from UV Eclipse MappingObserving the stellar wind of a mass-losing red supergiant in an eclipsing binary system in absorption against the ultraviolet continuum of a hot companion provides an elegant way of mapping the structure of the supergiant's wind with high spatial resolution. Repeated observations near eclipse allow the wind to be mapped as the line of sight to the hot companion sweeps through the wind. The bright eclipsing binary 31 Cygni (K4 Ib + B3 V) is ideal for this work. It is bright enough for high-resolution UV spectroscopy with well-separated components and an orbital period of 10.34 years. In the ultraviolet, the hot early-type companion dominates the flux, thereby avoiding the complexities of analyzing a composite spectrum. We propose to map the wind structure of the 31 Cyg red supergiant by observing the FUV spectrum near and during the March 2024 eclipse at 10 visits with HST/STIS. These UV observations can only be done with HST.We propose to observe the FUV spectrum of the red supergiant eclipsing binary 31 Cygni (K5 Ib + B3 V) from 1150 - 3050 A using theE140M echelle grating, 2 prime tilts of the E230M echelle grating (at central wavelengths of 1978 and 2707 A), and 1 tilt of the E230H echelle grating (at a central wavelength of 2912 A) at 10 epochs (HST visits) during the ingress, totality, and egress phases of the Feb-Apr 2024 eclipse of 31 Cygni. In this event, the red supergiant primary will eclipse the hot B-type companion. The duration of total eclipse is 57 days (2024 Feb 21 through Apr 18), with mid-eclipse on 2024 Mar 22. The proposed UV echelle observations at each observation epoch (HST visit) will fit into a single HST orbit, so the entire program can be carried out in just 10 orbits. Three visits (1,8,9) will provide observations of the RSG wind away from eclipse. Two visits (2,7) will sample atmospheric eclipse when the line of sight to the hot companion passes deep into the extended outer atmosphere of the red supergiant. Two visits (3,6) will sample deep atmospheric eclipse at times just prior to the onset (ingress) of total eclipse, and just after emergence (egress) from totality. Two visits (4,5) will observe the FUV spectrum during total eclipse, when the B-type continuum is occulted and an emission line spectrum seen due to the scattering of hot star photons by the wind of the RSG star. One final visit (10) will observe the intrinsic FUV spectrum of the hot companion even further from eclipse, when circumstellar absorption from the red supergiant's wind should be minimal. This final visit is to provide a baseline stellar spectrum of the hot companion for analyses of the additional circumstellar absorption seen at phases closer to eclipse, as well as yielding an additional radial velocity point to refine the secondary orbit. The dates of the proposed 10 visits are shown in Table 1 below.
Table 1. Summary of Proposed Visits Near & During the Eclipse of 31 Cygni
Visit Start Date Window End Date Window Eclipse Stage
1 2023 Dec 21 2024 Jan 16 Wind absorption - ingress
2 2024 Feb 13 2024 Feb 15 Atmospheric eclipse - ingress
3 2024 Feb 16 2024 Feb 19 Partial eclipse - ingress
4 2024 Mar 10 2024 Mar 21 Total eclipse - 1st visit - wind scattered emission line spectrum
5 2024 Mar 23 2024 Apr 04 Total eclipse - 2nd visit - wind scattered emission line spectrum
6 2024 Apr 20 2024 Apr 23 Partial eclipse - egress
7 2024 Apr 24 2024 Apr 26 Atmospheric eclipse - egress
8 2024 May 10 2024 May 22 Wind absorption - egress
9 2024 Jun 10 2024 Jun 19 Far wind absorption - egress
10 2024 Sep 09 2024 Sep 26 Out of eclipse - intrinsic B star spectrum
These observation dates have been constrained by use of BETWEEN dates for each visit, and AFTER constraints to ensure that each visit is executed after the preceding visit. For Visits 4, 5 & 8, about 150 s of "unused" orbit visibility (according to the Orbit Planner) has been left at the end of the science program to allow schedulability at the requested dates of those visits. The orbit duration shown in the Orbit planner is apparently an average value of the actual orbit visibility. If unused time is left at the end of the orbit, then the available range of schedulable dates shown in the Visit Planner expands. Therefore, we have added a block of unused time at the ends of those 3 visits, as needed to permit those visits to be scheduled during the windows set by the BETWEEN constraints for those visits. Removing any of this "unused" orbit time impacts the schedulability of these 3 visits, according to the APT Visit Planner.
The following two ephemerii were used to predict times of the March 2024 eclipse:
1. Gyldenkerne & Johansen 1970 A&AS,1,129 based on the 1962 eclipse [GJ70], and
2. Stencel et al. 1984 ApJ, 281, 751, based on the 1982 eclipse [S84].
The GJ70 ephemeris predicts a 2024 mid-eclipse on JD 2460391.69, while S84 yields a 2024 mid-eclipse time of JD 2460391.75. These values only differ by 0.06 days or 86 minutes, and so the average mid-eclipse time of JD 2460391.72 = 2024 Mar 22 at 05:17 UT has been used for this work. The predicted length of totality is 57.66 days. Totality begins on JD 2460361.70 (2024 Feb 21) and ends on JD 2460419.36 (2024 Apr 18), with partial eclipse phases lasting about 4-5 days before and after these dates, respectively. The two mid-eclipse visits (Visit 4 & 5) are planned to bracket the 12 day periods prior to and immediately following mid-eclipse respectively. Both Visit 4 & 5 will occur within the central half of the total eclipse period, to avoid possible exposure of the MAMA detectors to the hot star's UV-bright continuum.
Observations for each visit will begin with acquiring the target in the visible in the F25D5 aperture, and then performing a peakup using the neutral density 0.3X0.05ND aperture (to avoid saturating the CCD due to the brightness of the target in the visible). These acquisitions and peakups will be carried out in the visible spectral region (where the flux is dominated by the red supergiant primary) for each visit because the hot companion will be faint & variable in the UV during eclipse, and peakups in the UV might be problematic at those times. Four science exposures will be carried for each visit using E140M (at the fixed central wavelength, or cenwave, of 1425 A), E230M at the 2 cenwaves of 1978 and 2707 A, and E230H at the cenwave of 2912 A (see Table 2 below for details). The B-type secondary star in 31 Cygni is UV-bright (out of eclipse), with FUV fluxes near 2.0e-10 ergs/cm^2/s/A from 1240-1300A, decreasing to 5.0e-11 erg/cm^2/s/A at 2350 A and to 3.0e-11 ergs/cm^2/s/A at 3000 A. The maximum global count rate of ~150,000 counts/s occurs for the E230H/2912 exposure with the 0.2X0.09 aperture. The other medium-resolution STIS echelle exposures use the 31X0.05NDB neutral density aperture to reduce the bright continuum flux, except for Visit 4 & 5 during total eclipse (when the B star's UV-bright continuum is absent), which use the bare 0.2X0.06 aperture. The hot star in 31 Cygni is a B-type main-sequence star, and its continuum flux is not expected to vary, and has never been observed to vary (except for occultation of the flux during eclipse). None of these STIS/MAMA echelle observations exceed the bright limits for a non-variable source (except during elcipse, when that source is occulted). The investigators have observed 31 Cyg with a similar observational setup before without problems or violation of the UV/MAMA bright limits.
Each of the 10 planned visits will be 1 orbit in length, and will contain a similar sequence of planned STIS UV spectroscopic exposures. The exposure lengths and setup for all but 3 of the 10 visits are identical. The only differences are for the total eclipse visits (visits 4 & 5), which will observe the spectrum with the E140M & E230M gratings with longer exposures using the bare 0.2X0.06 aperture (instead of the neutral density 31X0.05NDB slit) because the hot star's UV-bright continuum will be absent during eclipse, and only a (much) weaker emission line spectrum will be present. Visit 8 will observe circumstellar absorption from the red supergiant's wind, along a sightline about 1 month after egress, using slightly shorter exposure times than the other visits (Table 2 below) in order to allow scheduling this observation during the preferred mid-May period. Otherwise, the only difference between the out-of-eclipse visits is the planned observation date, which will be constrained by BETWEEN timing requirements to lie between specified dates chosen to sample key events near and during the eclipse.
Table 2. Summary of STIS Spectroscopic Grating Configurations, Exposure Times, ETC IDs and S/N Estimates
Detector/Grating Observation Type Aperture Cenwave ETC ID Exp Time (s) S/N
CCD/ACQ All F25ND5 1892621 2 135
CCD/ACQ/PEAK All 0.3X0.05ND 1892619 0.1 140
GO-WAVECAL/E140M Calibration Lamp 0.2X0.06 1425 20
STIS/E140M Out-of-eclipse 31X0.05NDB 1425 1891728 240 20-40
STIS/E140M Total eclipse 0.2X0.06 1425 1893440 180 20-30 (em lines)
GO-WAVECAL/E230M Calibration Lamp 0.2X0.06 1978 20
STIS/E230M Out-of-eclipse 31X0.05NDB 1978 1891736 195 25-40
STIS/E230M Total eclipse 0.2X0.06 1978 1893441 155 30-50 (em lines)
STIS/E230M Out-of-eclipse 31X0.05NDB 2707 1891738 101 25-30
STIS/E230M Total eclipse 0.2X0.06 2707 1893442 80 30-50 (em lines)
GO-WAVECAL/E230M Calibration Lamp 0.2X0.06 2707 20
STIS/E230H Out-of-eclipse 0.2X0.09 2912 1891754 68 20-30
STIS/E230H Total eclipse 0.2X0.09 2912 1893443 240 30-40 (Mg II h&k lines)
GO-WAVECAL/E230H Calibration Lamp 0.2X0.09 2912 20
The ETC calculations shown here used a user-supplied input file based on a composite of FUSE, HST & IUE/LSA UV and visible fluxes of 31 Cyg. Acquisition and peakup using the CCD visible flux used a Pickles K4I (3990K) model normalized to a flux F_lambda = 1.184e-10 egs/cm2/s/A at 5500 A, consistent with the above user-supplied input file in this region. (That user input spectrum only extends longward to 5685 A, so Pickles model fluxes are used to model the extension of the observed spectrum into the red and IR regions, as observed by the CCD detector during acquisition and peakup). Total eclipse ETC calculations used a combination of UV total eclipse observations from FUSE Program D123 Visits 3 & 4 (June-July 2003), and IUE SWP18108 & LWR 14262 LSA images (Sept 1982).
To optimize packing of the science observations into each a single orbit's visibility period, we have turned off default wavecals (WAVECAL=NO) , and specified user GO wavecals with each science exposure. This allows the final GO wavelcal to be done during Earth occultation, which optimizes the available time for science exposures. The GO exposure times are the default 20 seconds for all 4 calibration lamp exposures.Team Expertise
The team has extensive experience in the reduction and analysis of ultraviolet spectra from HST, especially with the STIS spectrograph. The team also has many years of experience in the field of fundamental stellar parameters, radial velocity and spectroscopic orbit analyses.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDSTARB3-B5 V-IVCIRCUMSTELLAR MATTERINTERACTING BINARYWINDThis object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000F_lam(1270 A)= 1.9e-10 ergs/cm^2/s/A. FUV flux is from main-sequence B star and is NOT variable (except during eclipse)STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598Timing link suitability includes constraints ([02 After 01])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 1 will observe the UV continuum of the hot companion of 31 Cyg, with circumstellar absorption from the stellar wind of the red supergiant primary superimposed, about 2.5 months prior to ingress into eclipse.170346933400028.76524353177831(Tic-Visit
:proposal-id 17416
:visit-id "01"
:proposal-version -1
:trans-version "20230626"
:date "29-Sep-2023 15:19:46.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "01"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2820
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.Timing link suitability includes constraints ([02 After 01] [03 After 02])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 2 will observe the UV continuum of the hot companion of 31 Cyg, seen through the extended outer atmosphere of the supergiant approaching ingress into eclipse.1707877712000334.0(Tic-Visit
:proposal-id 17416
:visit-id "02"
:proposal-version -1
:trans-version "20230626"
:date "29-Sep-2023 15:19:47.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "02"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2820
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.Timing link suitability includes constraints ([03 After 02] [04 After 03])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 3 will observe the UV continuum of the hot companion of 31 Cyg during the partial eclipse ingress phase.1708054151000332.08381089691227(Tic-Visit
:proposal-id 17416
:visit-id "03"
:proposal-version -1
:trans-version "20230626"
:date "29-Sep-2023 15:19:47.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "03"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2820
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.Timing link suitability includes constraints ([04 After 03] [05 After 04])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 4 will observe the UV emission line spectrum seen in total eclipse. This spectrum is formed by B-star continuum photons scattered by the wind of the red supergiant. This is the 1st visit in total eclipse, with a window from mid-eclipse - 12 days to mid-eclipse (Mar 22).1710520748000300.6285803001514(Tic-Visit
:proposal-id 17416
:visit-id "04"
:proposal-version -1
:trans-version "20230626"
:date "11-Oct-2023 21:21:07.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "04"
:obset-id "04"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "04"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2667
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Timing link suitability includes constraints ([05 After 04] [06 After 05])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 5 will observe the UV emission line spectrum seen in total eclipse. This spectrum is formed by B-star continuum photons scattered by the wind of the red supergiant. This is the 2nd visit in total eclipse, with a window from mid-eclipse (Mar 22) to mid-eclipse + 12 days.1711437079000289.6557625308174(Tic-Visit
:proposal-id 17416
:visit-id "05"
:proposal-version -1
:trans-version "20230626"
:date "11-Oct-2023 21:39:16.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "05"
:obset-id "05"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "05"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2667
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Use bare 0.2X0.06 aperture when B star is in total eclipse, and UV continuum absent.Timing link suitability includes constraints ([06 After 05])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 6 will observe the UV continuum of the hot companion of 31 Cyg during the partial eclipse egress phase.1713708543000264.4872885441231(Tic-Visit
:proposal-id 17416
:visit-id "06"
:proposal-version -1
:trans-version "20230626"
:date "29-Sep-2023 15:19:50.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "06"
:obset-id "06"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "06"
:orbit-number 1
:pcs-time 443
:si-vis-utilization 2820
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3263
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 7 will observe the UV continuum of the hot companion of 31 Cyg, seen through the extended outer atmosphere of the supergiant following egress from eclipse.1724470339000155.0(Tic-Visit
:proposal-id 17416
:visit-id "07"
:proposal-version -1
:trans-version "20240627"
:date "05-Aug-2024 12:17:41.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "07"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2682
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3062
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 8 will observe the UV continuum of the hot companion of 31 Cyg, with circumstellar absorption from the supergiant's stellar wind following egress from eclipse. This is a special setup with reduced exposure times for Visit 8 to allow schedulability in May 2024.(Tic-Visit
:proposal-id 17416
:visit-id "08"
:proposal-version -1
:trans-version "20240627"
:date "08-Aug-2024 17:03:38.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "08"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2666
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3062
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.Timing link suitability includes constraints ([10 After 09])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 9 will observe the UV continuum of the hot companion of 31 Cyg, with circumstellar absorption from the supergiant's stellar wind about 3 months post-eclipse.(Tic-Visit
:proposal-id 17416
:visit-id "09"
:proposal-version -1
:trans-version "20240627"
:date "08-Aug-2024 17:03:44.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "09"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2680
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3062
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.Timing link suitability includes constraints ([10 After 09])The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.Visit 10 will observe the intrinsic spectrum of the B-star companion, out-of-eclipse and (relatively) uncontaminated by circumstellar absorption from the supergiant's wind about 6 months post-eclipse.(Tic-Visit
:proposal-id 17416
:visit-id "10"
:proposal-version -1
:trans-version "20240627"
:date "08-Aug-2024 17:03:47.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 348512
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17416
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17416
:visit-id "10"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2680
:al-overhead-at-end 81
:internal-dur-at-end 394
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3062
:pcs-gap 0
)true10Exposure saturates in 38.54 sec.Exposure saturates in 1.15 sec.Total count rate 89138 counts/sec.Total count rate 66,830 count/sec.Total count rate 98791 counts/sec.Total count rate 149654 counts/sec.