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. 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. 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. 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. 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: 3519 ----- Attempting Submission 1 (Fri Mar 25 20:41:25 GMT 2022) ----- According to COS instructions for Cycle 30 for G160M, at S/N<20 STScI recommends using LP6. However, since we wish to obtain all exposures in one orbit, mimicking the successful observations in program 16196, staying at LP4 after the G130M exposure and avoiding the overheads associated with using LP6 for G160M is necessary to meet our goals for S/N. Note that the LP6 wavecals would consume more than the total time planned for the G160M exposures at LP4, hence they are completely impractical. 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. 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. 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. 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. 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 (Fri Jul 15 12:16:20 GMT 2022) ----- Restricted mode is necessary to use LP4 for our COS exposures. This was approved in our Phase I. For our G160M exposures, we use two different WAVECENs, and two FPPOS apiece, for a total of 4 FPPOS positions in G160M. This worked very well in our previous program, 16196. Characterizing the structure and kinematics of the gas surrounding supermassive black holes at the centers of galaxies is crucial for understanding accretion and black-hole growth, as well as outflows and associated feedback for host-galaxy evolution. Intensive, successful reverberation mapping campaigns with HST on the active galactic nuclei (AGN) of NGC 5548 (Cycle 20) and Mrk 817 (Cycle 28) have revealed a wealth of information on the structure of their broad-emission-line regions (BLR), their accretion disks, and the new, unexpected obscuring outflows visible in their X-ray and far-UV spectra. The BLR of these AGN are dominated by virial motions, and the obscuring outflows play a significant role in regulating the ionizing flux reaching the BLR gas. Although HST observations of Mrk 817 are complete, continued monitoring in X-ray, UV, and optical with Swift (2 years, every other day), NICER (1 year, every other day), and ground-based observatories have been approved and are ongoing (private communication). To take advantage of these multi-wavelength programs, we propose to continue observing Mrk 817 with COS, with a cadence of one orbit per month throughout Cycle 30. Our primary science goal is to monitor the continued evolution of the obscuring outflow, perhaps even watching as it dissipates; measure its continued impact on the characteristics of the BLR; and, via a triggered observation, do a comprehensive broad-band evaluation of the state of Mrk 817's accretion disk and broad emission-line properties once the obscuration has melted away. Observing Description for Cycle 30 Proposal, 17105 The primary science goal of this proposal is to monitor the broad line region (BLR) of the Seyfert 1 galaxy Mrk 817 and the outflowing obscuring wind in conjunction with ongoing Swift and NICER X-ray, NUV, and optical monitoring. Swift and NICER will observe Mrk 817 on a 2-day cadence. We will observe Mrk 817 on a monthly basis for all active months of Cycle 30, a total of 14 in all, from October 2022 to November 2023. This program uses the same instrumental setups as GO-16196, a Cycle 28 (2020-2022) monitoring program on Mrk 817, and known as the Space Telescope and Optical Reverberation Mapping 2 (STORM 2) program (Kara et al. 2021). The STORM 2 program obtained COS spectra on a 2-day cadence for 155 months with 165 observations. Our current program will not do reverberation mapping, but will place the broad line emission and strength of the obscuring outflow in the context provided by the more extensive Swift and NICER monitoring programs. Data Quality Requirements: Spectral Coverage, Resolution, and Signal-to-Noise Ratios: For HST/COS, obtaining suitable data (in terms of S/N and spectral resolution) in a single orbit on a bright target is not a challenge. We will use the same instrumental setup as in GO-16196, which used the G130M/1222 setting plus G160M/1533 and G160M/1577 to observe the 1100-1750 A wavelength range in a single orbit covering all the emission and absorption features of interest at once (Ly alpha, NV, Si IV, CIV, and He II in emission; P V, C III*, Ly alpha, N V, Si IV, and C IV in absorption). As described in our proposal, minimzing overheads to fit all required exposures into a single orbit and for compatibility with the observations in GO-16196, we request that all COS observations be done at Lifetime Position 4. To obtain adequate S/N in absorption-line troughs and the emission-line profiles, we require S/N~10 in the continuum per resolution element. For program 16196, the S/N in the continuum at 1180 A ranged from 9 to 15 over the full range of brightness in Mrk 817, which was from 4.4e-14 to 10.5e-14 erg/sec/cm2/A, with variations on timescales of days to weeks. For this proposal, we base our ETC simulations (v30.2) on the HST spectra from STORM 2, for which the median flux at 1390 A in the FUV is F(1390A) = 7.3e-14 erg/s/cm2/A. Mrk 817 is a bright AGN, so imaging target acquisitions with either MIRRORA or MIRRORB can result in unacceptably high count rates. However, spectroscopic target acquisitions take too long, leaving little time for science. We find that the best safe compromise is an imaging target acquisition using the Bright Object Aperture (BOA) on COS and MIRRORA. To allow for successful acquisition even if the target becomes fainter than usual, we plan our exposure time for the historical minimum flux of 1e-14 erg/s/cm2/A. Mrk 817 was observed safely with COS on during the whole of STORM 2, well below any bright object flux limits. There are no bright objects in the field, and it was safely acquired during all months of the year over the full range of scheduled position angles. Program Duration: Because it is near the ecliptic pole, Mrk 817 is continuously visible to HST throughout the year. This allows for monthly visits during all twelve months. Schedulability: There are no ORIENT restrictions for our target and it is continuously accessible throughout the year for 365 days on account of its high ecliptic latitude, aside from possible intervals due to OBAD-shortened orbits. (Once these are known, we should schedule our single-orbit visits to avoid them.) Ideally, our observations should be made approximately 1 month apart, similar to the COS flux calibration programs, with windows of +-1 week around each observation. Successive observations should be at least two weeks apart. We emphasize that evenly spaced intervals are not required, and there can be some leeway in the "at least two weeks apart" requirement. The continuous visibility allows great freedom in scheduling the campaign. However, we wish to maximise our overlap with the Swift and NICER campaigns, so observations should start immediately at the beginning of Cycle 30 and contnue for its entirety. Guide-star availability may show that only single guide stars are available during some time intervals. This is acceptable, and it had no impact on data quality during GO-16196. Our observations are short enough that roll is not critical, and COS transmission is not strongly dependent on precise centering, so the slight drift associated with single-guide-star guiding does not have a deleterious impact on our data quality. We can't specify the single-guide-star acquisition mode ourselves, so any visits likely to be affected by this issue should be handled by the PC at the appropriate time. One-gyro Impacts. In the event of a necessary change to 1-gyro mode for HST, Mrk 817 is still visible year round. Scheduling may be more limited, b ut it is possible in all months. We believe that we can still conduct a successful program in such circumstances since there are still long intervals of regular schedulability. Requirements for Target of Opportunity triggering and observation: Another goal of our proposal is to see Mrk 817 emerge from its current state dominated by a strong obscuring outflow. When soft X-ray absorption as measured by NICER and Swift has diminished to levels consistent with only foreground Milky Way absorption (hardness ratio < -0.3 for s full month), or if HST/COS spectra show that the UV absorption lines have disappeared, we will trigger a non-disruptive TOO observation that will use four additional orbits to obtain a view of the full UV portion of the spectrum from the Lyman limit in Mrk 817 (940 A observed) to 3200 A. When combined with ground-based spectra, we will cover the full wavelength range in Mrk 817 from the Lyman limit (912 A) to 10,000 A (past the Paschen edge at 8206 A), allowing us to fit the continuum shape to accretion disk models, and search for contribution from diffuse continuum emission associated with Balmer and Paschen recombination spectra. The four HST orbits will consist of four 500 s exposures using all four FP-POS positions with G130M/1096; four 250 s exposures using all four FP-POS positions with G130M/1222; four 200 s exposures using all four FP-POS with G160M/1533; four 200 s exposures using all four FP-POS with G160M/1577; and a 1700 s exposure with STIS NUV-MAMA/G230L. To obtain an accurate measure of the spectral energy distribution of Mrk 817 when the COS, STIS, and ground-based spectra are combined, we request the use of the MSMOFF option for the NUV-MAMA observation in order to obtain the best absolute flux calibration. This is a long-term ToO that should persist into Cycle 31 if not triggered during Cycle 30. Most of the team members were members of both the AGN STORM team that carried out program HST-GO-13330 on NGC 5548, and STORM2, performing reverberation mapping of Mrk 817, the subject of this proposal. PI: Dr. Gerard Kriss will coordinate the work of the team and participate in analysis and interpretation of the data. He modeled the UV spectra for AGN STORM and STORM2, and will do the same for this program. Co-PI: Dr. Gisella De Rosa is a COS expert and was responsible for reducing the AGN STORM COS spectra and calibrating the STORM 2 data. She will supervise the data reduction and analysis for this program. Dr. Yasaman Homayuni is an expert on AGN structure as revaeled by reverberation mapping. She led the data analysis for STORM 2. Dr. Edward Cackett is PI of an approved NICER program to monitor Mrk 817. He will supervise coordination with X-ray observations. Mr. Ethan Partington has led the analysis of the NICER data from STORM2, and will continue to lead this effort. Dr. Jonathan Gelbord is PI of an already approved Swift 2-year prograam to monitor Mrk 817. He will supervise coordination with the Swift program in order to determine the trigger for the proposed ToO visit. Dr. Erin Kara is an expert X-ray observer. Dr. Aaron Barth is experienced observer of AGN broad-line and accretion disk spectra. He will oversee the ground-based program. Dr. Keith Horne is a reverberation mapping expert. He will be responsible for interpreting the ongoing monitoring in light of velocity-delay maps from STORM2. Dr. Hermine Landt is an expert in NIR BLR and outflow observations and will coordinate the ground-based NIR observaations. Dr. Gary J. Ferland and Dr. Maryam Dehghanian are photoionization modeling experts. They will aid in interpreting models for the BLR region and the absorbing outflows. Dr. Kirk Korista and Dr. Michael Goadwill develop theoretical models, as they did for AGN STORM. All investigators will participate in analysis and interpretation of the data. Supermassive Black Holes and Active Galaxies 6 false false true false false false false false AVAILABLE GALAXY ACCRETION DISK BLR NUCLEUS SEYFERT WIND NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F(1180) = 7e-14 erg/cm2/s/A COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1096 STIS/NUV-MAMA Spectroscopic No No G230L 2376 1657887073494 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1664905243000 30.039812407137788 (Tic-Visit :proposal-id 17105 :visit-id "01" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:13.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887075661 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1667814891000 353.264 (Tic-Visit :proposal-id 17105 :visit-id "02" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:15.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887076894 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1670126597000 331.3628437642383 (Tic-Visit :proposal-id 17105 :visit-id "03" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:16.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887078070 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1673137493000 298.7030481498408 (Tic-Visit :proposal-id 17105 :visit-id "04" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:17.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887079254 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1675700493000 265.0 (Tic-Visit :proposal-id 17105 :visit-id "05" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:18.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "05" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887080410 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1678139929000 241.19266453168257 (Tic-Visit :proposal-id 17105 :visit-id "06" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:20.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887082249 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1681459863000 195.89999999999998 (Tic-Visit :proposal-id 17105 :visit-id "07" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:21.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887083419 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1683818213000 169.2 (Tic-Visit :proposal-id 17105 :visit-id "08" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:23.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "08" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887083419 HOPR repeat of visit 8 1685854024000 144.66055084983242 (Tic-Visit :proposal-id 17105 :visit-id "08" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:23.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "08" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887085039 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1686372778000 144.66128775686047 (Tic-Visit :proposal-id 17105 :visit-id "09" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:24.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "09" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887086158 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1688901550000 119.11979945991561 (Tic-Visit :proposal-id 17105 :visit-id "10" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:25.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "10" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887087266 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1690685688000 100.19927495657589 (Tic-Visit :proposal-id 17105 :visit-id "11" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:27.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "11" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887088352 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1694313756000 57.94192336596461 (Tic-Visit :proposal-id 17105 :visit-id "12" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:28.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "12" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887089618 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 1696743857000 29.385216530339704 (Tic-Visit :proposal-id 17105 :visit-id "13" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:29.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "13" :obset-id "13" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "13" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1657887090759 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17105 :visit-id "14" :proposal-version -1 :trans-version "20220516" :date "15-Jul-2022 08:11:30.0" :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 122112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "14" :obset-id "14" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "14" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2556 :al-overhead-at-end 0 :internal-dur-at-end 344 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) false 1 0 Target Acq assumes an FOS-based QSO spectrum at z=0.031455, E(B-V)=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe. 1687196465824 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. This visit is for a target of opportunity observation to be triggered when the obscuring outflow in Mrk 817 has dissapated as indicated by Swift and NICER hardness ratios indicative of only Milky Way foreground absorption (HR < -0.3 for 1 month), or absence of broad UV absorption in the HST/COS spectrum. The minmum time after triggering is 21 days so as to be non-disruptive. This is a long-term ToO that should persist into Cycle 31 if not triggered during Cycle 30. 1688445401000 123.79262250958368 (Tic-Visit :proposal-id 17105 :visit-id "15" :proposal-version -1 :trans-version "20220630" :date "19-Jun-2023 13:41:05.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 557552 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17105 :visit-id "15" :obset-id "15" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 17105 :visit-id "15" :obset-id "A5" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17105 :visit-id "15" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2557 :al-overhead-at-end 20 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17105 :visit-id "15" :orbit-number 2 :pcs-time 393 :si-vis-utilization 2542 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17105 :visit-id "15" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2551 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17105 :visit-id "15" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2548 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2950 :pcs-gap 0 ) true 4 0 Target Acq assumes an FOS-based QSO spectrum at z=0.0314555, E(B-V=0.02, and F(1390)=1.0e-14, less than half the lowest flux observed in the 2020-2022 reverberation-mapping campaign, PID 16196. ETC run COS.ta.1809303 uses F(1390)=2.e-13, twice the brightet level in 2021, and shows that the observation is safe.