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. 0 Assigned ID: 4945 ----- Attempting Submission 1 (Mon Dec 18 18:37:48 GMT 2023) ----- Joint XMM For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. 0 ----- Attempting Submission 1 (Fri Jan 19 05:42:36 GMT 2024) ----- The choice of FP-POS is justified in the Proposal Description. The link between obscuration and outflows in AGN was first discovered in NGC 5548. This archetypal Sy-1 galaxy underwent major changes due to obscuring winds from the accretion disk. These remarkable winds, captured by joint X-ray/UV spectroscopy, have significant impact on their environment. Swift monitoring shows that over the last 10 years the obscuration in NGC 5548 has gradually declined. This presents a valuable opportunity for analyses that have not been feasible before due to too much obscuration. The lowered obscuration facilitates high-resolution RGS spectroscopy of the outflow to ascertain its evolution. We need to constrain the intrinsic continuum with NuSTAR and EPIC+OM, and the UV outflow with HST/COS. We request joint XMM (180 ks), NuSTAR (70 ks), and HST (2 orbits) spectra. This HST observation (2 orbits) was approved as part of a joint XMM program to obtain the HST/COS spectrum of NGC 5548 to study the obscuring wind in this AGN. The HST observation needs to be taken simultaneously as justified in the XMM proposal (the source and the obscuring wind are variable). Therefore, please coordinate with the XMM planners. The most likely XMM visibility window is: 2024-12-21 to 2025-02-03 The HST exposure time is based on our 2021/2022 observations of NGC 5548 (Mehdipour, M. et al. 2022, ApJL, 934, L24), which required 2 orbits per visit to observe Ly-alpha, N V, and C IV with gratings G130M and G160M. We have confirmed this with the ETC tool. Two orbits yields a S/N of at least 10 per resolution element in the continuum using the G130M grating with central wavelength 1222 and 1291 (for modeling Ly-alpha and N V) and using the G160M grating with central wavelengths 1600 and 1623 (for modeling Si IV and C IV). This is adequate to measure the parameters of the broad UV absorption lines associated with the obscurer, as well as the narrow absorption lines (including low ionization lines) associated with the warm absorber outflows. For the BUFFER-TIME, we obtained the recommended buffer (2/3 of the buffer fill time) from the ETC for each exposure. In order to obtain the requisite S/N in the minimum number of orbits, we request the use of Lifetime Position 4 for both the G130M and G160M observations. This was requested as required in the Phase 1 proposal with XMM. This will also replicate our observations from 2021/2022 and enable a one-to-one comparison. Because we are using two different CENWAVES with each grating and two FP-POS positions in each, we already accomplish the actual objectives of switching between different FP-POS settings: (1) Better science return: the spectrum is placed at four different locations on the detector, enabling us to detect and reject detector anomalies like dead spots, hot spots, grid-wire shadows, etc. (2) Spread the flux across the detector in multiple locations, especially in bright emission lines, to decrease charge depletion and extend the lifetime of the detectors. We do not want to sacrifice S/N with unnecessary extra exposures and increased overhead during each visit by using all 4 FP-POS settings with each CENWAVE. When only one CENWAVE is used, then 4 FP-POS settings makes sense, but that's not the case for our observations. Our chosen FPPOS settings reflect our S/N requirements while still meeting the objectives of using different FP-POS settings in our program. Reduced gyro does not impact the feasibility of our program. Also, orientation limitation would not impact our program. na Supermassive Black Holes and Active Galaxies 6 false false false false false false SUPPORTED GALAXY ACCRETION DISK BLR SEYFERT WIND NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1533 COS/FUV Spectroscopic No No G160M 1623 1705641152076 The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. 1738427348000 277.57410250285915 (Tic-Visit :proposal-id 17591 :visit-id "01" :proposal-version -1 :trans-version "20230626" :date "19-Jan-2024 00:12:31.0" :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 261504 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17591 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17591 :visit-id "01" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2467 :al-overhead-at-end 0 :internal-dur-at-end 2485 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17591 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2518 :al-overhead-at-end 0 :internal-dur-at-end 489 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2910 :pcs-gap 0 ) true 2 0 Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019), we took the lowest observed flux (1.8e-14 erg/cm^2/s/A), to calculate the required exposure time to obtain S/N ratio of 30 for ACQ/IMAGE with BOA. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated.