Science Keywords: Select from 2 to 5 items. Wavelength is a required field. Wavelength is a required field. 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. Please specify your scheduling constraints or 'No Constraints' on all Observation forms. 0 Assigned ID: 3877 ----- Attempting Submission 1 (Fri Nov 25 15:13:25 GMT 2022) ----- Joint XMM/HST Unschedulable Visit Unschedulable Visit To make compatible with COS policy (as requested by John Debes), the 1222 exposures are changed to to 1291 FP-POS=3 and FP-POS=4. Changed from one visit to two visits. Set the sched to 100 and re-adjusted the exposure times ---- Missagh Mehdipour is added as a CoI, and the Phase II contact, after getting approved from Claus Leitherer. Please see our justification for our choices of FP-POS settings in the Proposal Description. 1417636926 ----- Attempting Submission 1 (Sun Dec 11 18:26:28 GMT 2022) ----- ----- Attempting Submission 2 (Thu Nov 09 15:31:04 GMT 2023) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 3 (Mon Jun 10 15:42:45 GMT 2024) ----- ----- Attempting Submission 4 (Fri Jun 21 19:21:36 GMT 2024) ----- To make compatible with COS policy (as requested by John Debes), the 1222 exposures are changed to to 1291 FP-POS=3 and FP-POS=4. Changed from one visit to two visits. Set the sched to 100 and re-adjusted the exposure times ---- Missagh Mehdipour is added as a CoI, and the Phase II contact, after getting approved from Claus Leitherer. Please see our justification for our choices of FP-POS settings in the Proposal Description. Various types of photoionised outflows are observed from AGN. A 200 ks XRISM PV observation is scheduled to study the nature of the outflows in NGC 3783, the best case for this purpose. We propose joint observations of XMM-Newton, NuSTAR, HST, and Swift. XMM/RGS characterises lower ionised absorbers in soft X-rays. In combination with the higher ionised ones revealed by XRISM, we can study all absorbers comprehensively. XMM/EPIC and NuSTAR determine the spectral energy distribution and constrain the continuum. HST accurately measures outflow velocity from UV absorption lines. Swift observations preceding XRISM brings the flux history for photoionisation modelling of the variable absorbers. This HST observation (approved as part of a joint XMM-Newton proposal) plans to obtain the COS spectrum of NGC 3783 during observation with the upcoming XRISM mission. The contemporaneous HST UV spectrum of NGC 3783 is crucial for AGN wind studies with the groundbreaking XRISM mission. NGC 3783 is a Performance Verification (PV) target of XRISM and will certainly be observed. However, currently, prior to the launch of XRISM, the exact observation time is not known. In the scheduling requirement section, we have specified the two visibility windows of XMM-Newton. The XRISM observation will likely be taken in the second visibility window, which is 12-Dec-2023 to 24-Jan-2024. As justified in the XMM-Newton proposal, the HST observation is needed to be taken during the XRISM observation. Our HST/COS time and setup is based on the prior observations of NGC 3783 (Mehdipour et al. 2017, A&A, 607, A28; Kriss et al. 2019, A&A, 621, A12), which required 2 orbits to constrain broad absorption lines of Ly-alpha, N V, and C IV with gratings G130M and G160M. This also allows measurement of weak, low-ionization lines associated with the new ionization state of the warm absorber. Following the Phase II Proposal instructions and the allowed COS settings for Cycle 30, the central wavelengths and FPPOS positions that we have selected provide the optimum full spectral coverage of the interested regions with the G130M and G160M gratings, minimize spectral gaps, and maximize the potential of the detection of the relevant broad and narrow absorption lines. This enables us to fully explore the UV spectral signatures of the obscuring outflow in NGC 3783. Thus, for our observation we utilize G130M/1222, G130M/1291, G160M/1600, and G160M/1623. We obtained the required time for each exposure using the COS Exposure Time Calculator (ETC) tool and the NGC 3783 UV fluxes at 1368 A published by Dunn et al. (2006), PASP, 118, 572. As the HST/COS spectrum of NGC 3783 (Kriss et al. 2019) is approximately flat in the NUV and FUV, we used a flat spectrum in ETC. The redshift z=0.00973 and foreground extinction of E(B-V)=0.107 are taken into account. For the target acquisition we used the minimum UV flux of 1.2e-14 erg/cm^2/s/A and calculated the required exposure time to get a S/N of 30 using ACQ/IMAGE with BOA. Using the median flux of 4.7e-14 erg/cm^2/s/A, the exposure times were calculated to give a S/N of at least 10 for each exposure with G130M/1222, G130M/1291, G160M/1600, and G160M/1623. The maximum UV flux ever observed (10.8e-14) does not pose a bright object risk for COS. NGC 3738 has been acquired and observed with HST COS before, and there are no bright field objects that would prove an overlight risk to COS. For the BUFFER-TIME, we obtained the recommended buffer (2/3 of the buffer fill time) from the ETC for each exposure. Please note 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 FP-POS settings reflect our S/N requirements while still meeting the objectives of using different FP-POS settings in our program. Although reduced gyro operations for HST would be unfortunate, our program would still remain fully feasible. Reduced gyro operations would approximately halve the opportunities for coordination with XMM-Newton and XRISM. Also, any orientation limitation would not impact our program. n/a 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 G130M 1291 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G160M 1623 1718997249829 Timing link suitability includes constraints ([02 After 01 by 0.1 to 0.1 days]) The scheduling data was generated by CASM 32.1. CASM was run in Phase II mode. 51 1721534025000 132.0 (Tic-Visit :proposal-id 17273 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "21-Jun-2024 15:14:09.0" :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 130752 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17273 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17273 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2680 :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 3060.0 :pcs-gap 0 ) true 1 0 Using NGC 3783 minimum flux of 1.2e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve target acquisition with S/N of 30. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of at least 10 with G130M/1222. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of at least 10 with G160M/1600. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1377 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of 11 with G160M/1623. 1718997304794 Timing link suitability includes constraints ([02 After 01 by 0.1 to 0.1 days]) The scheduling data was generated by CASM 32.1. CASM was run in Phase II mode. 51 1721539729000 132.0 (Tic-Visit :proposal-id 17273 :visit-id "02" :proposal-version -1 :trans-version "20240604" :date "21-Jun-2024 15:15:04.0" :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 130752 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17273 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17273 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2680 :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 3060.0 :pcs-gap 0 ) true 1 0 Using NGC 3783 minimum flux of 1.2e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve target acquisition with S/N of 30. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of at least 10 with G130M/1291. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of at least 10 with G160M/1600. Using NGC 3783 median flux of 4.7e-14 erg/cm2/s/A at 1377 A (Dunn et al. 2006), we calculated the exposure time to achieve S/N of 11 with G160M/1623.