Cannot find file /Users/gak/proposals/cycle31/mrk817/mrk817_c31.pdf
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.BETWEENs are not optimal. Will adjust during Phase II.1306589811Assigned ID: 4676
----- Attempting Submission 1 (Wed May 24 21:39:51 GMT 2023) -----Our Description of the Observations justifies the use of LP4 for the G160M exposures. These are all 1-orbit exposures in the same orbit as a G130M/1222 at LP4, and their S/N is <20. Using LP4 is necessary to minimize overheads and fit all exposures into 1 orbit.For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.Restricted mode is necessary to use LP4 for our COS exposures using G160M. 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. The maximum SNR is only ~10, so additional FP-POS settings make little improvement in data quality.-1033093607----- Attempting Submission 1 (Thu Sep 07 18:58:09 GMT 2023) -----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. The maximum
SNR is only ~10, so additional FP-POS settings make little improvement in data quality.Evolution of the Obscuring Outflow in the Active Galaxy Mrk 817The intensive multi-wavelength campaign to monitor the active galaxy Mrk 817 with HST, Swift, and NICER is now the longest, most intensive probe of an AGN's broad emission line region, the continuum emitted by its accretion disk, and its evolving, powerful X-ray and UV-absorbing outflow. Understanding the structure and kinematics of the gas surrounding supermassive black holes is crucial for understanding accretion, black-hole growth and associated feedback governing host-galaxy evolution. The BLR of Mrk 817 is dominated by virial motions, and its obscuring outflow plays a significant role in regulating the ionizing flux reaching the BLR gas. Continued monitoring of Mrk 817 in X-ray, UV, and optical with Swift (2 years, every other day), NICER (2 years, every other day), and ground-based observatories is still 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 in Cycle 31 through April 2024, the end of the current Swift monitoring program. Our primary science goal is to monitor the continuing evolution of the obscuring outflow, which has been dissipating over the past several months as shown by Swift, NICER, and HST spectra. Observing the moment that the obscurer has dissipated completely and how the BLR reacts to this clearing would be a unique moment in the life of an AGN never seen before. We also propose a triggered observation to obtain a comprehensive broad-band spectrum of Mrk 817's accretion disk and broad emission-lines from the Lyman limit to 1 micrometer once Swift, NICER, and HST have confirmed that the obscuration has dissipated.We will observe the Seyfert 1 galaxy Mrk 817 monthly to monitor changes in its various ionized outflows and emission-lines. Our individual observations will be the same as those used in the HST reverberation mapping campaign in 2020-2022 (PID 16196) as described in Homayouni et al. (2023) and the ongoing Cycle 30 program 17105. Since it is near the ecliptic pole, Mrk 817 is continuously visible to HST throughout the year. It has a minimum visibility of 48 m for science exposures, allowing
for the exposure times below after accounting for instrument overheads. Our monthly cadence will sample the far-UV spectrum over the 1070-1750 A wavelength
range with COS at Lifetime Position 4 (LP4). We will use G130M/1222 with four 60 s exposures at all four focal-plane (FP-POS) positions, G160M/1533 with exposures of 175 s and 180 s at FP-POS 1 and 2, and G160M/1577 with two 195 s exposures at FP-POS 3 and 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 programs 16196 and 17105, 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 14e-14 erg/sec/cm2/A. Based on the COS Instrument Science Report 2021-02 (Sankrit & Rowlands 2021), COS sensitivity in both gratings is declining by only ~1% per year, so we expect to obtain similar S/N in similar exposure times in Cycle 31. Our planned monthly observations will monitor changes in absorption and emission line strengths over the full cycle of the coordinated Swift, NICER, and ground-based observations which continue through April 2024. 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 programs 16196 and 17105, 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 14e-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 and program 17105, 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 31 and contnue through April 2024. 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 where a strong obscuring outflow is still present. 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 32 if not triggered during Cycle 31.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 revealed 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 program 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 and he PI of two past XMM-Newton programs for observations of Mrk 817 coordinated with HST.
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 Goad will 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 Galaxies6falsefalsetruefalsefalsefalsefalsefalseAVAILABLEGALAXYACCRETION DISKBLRNUCLEUSSEYFERTWINDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000F(1180)=7e-14COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1096STIS/NUV-MAMASpectroscopicNoNoG230L2376The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.(Tic-Visit
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