Safety submission Resubmission 1: full proposal Resubmission 2: disturbing typos corrected Resubmission 3: clarified 1-2 points. Resubmission 4: Duplication box updated Resubmission 5: Co-I change -1272296644 Assigned ID: 1624 ----- Attempting Submission 1 (Thu Apr 08 14:28:22 GMT 2021) ----- HST Phase I Proposal 1624 successfully submitted. Receipt: # 1624-1 ----- Attempting Submission 2 (Fri Apr 09 13:23:39 GMT 2021) ----- HST Phase I Proposal 1624 successfully submitted. Receipt: # 1624-2 ----- Attempting Submission 3 (Fri Apr 09 19:11:42 GMT 2021) ----- HST Phase I Proposal 1624 successfully submitted. Receipt: # 1624-3 ----- Attempting Submission 4 (Fri Apr 09 21:26:27 GMT 2021) ----- HST Phase I Proposal 1624 successfully submitted. Receipt: # 1624-4 ----- Attempting Submission 5 (Fri Apr 09 22:02:10 GMT 2021) ----- HST Phase I Proposal 1624 successfully submitted. Receipt: # 1624-5 ----- Attempting Submission 6 (Fri Apr 09 22:42:10 GMT 2021) ----- Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Used SWIFT fluxes to review observing strategy. 1525827256 ----- Attempting Submission 1 (Thu Jul 29 14:25:33 GMT 2021) ----- ----- Attempting Submission 2 (Thu Jul 29 19:30:50 GMT 2021) ----- ----- Attempting Submission 3 (Mon Jan 10 21:06:18 GMT 2022) ----- Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. The program consists of 4 ToOs (1 orbit per visit). Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. 715231712 After a 10-year hiatus, Mrk 590 has rekindled its nuclear activity and is now strongly flaring in a low X-ray state. This offers a very rare opportunity to follow in real time the onset of AGN activity that can lead to better insights on the AGN central engine physics. While directly impacting galaxy evolution through energetic feedback, the AGN structure and physics are still poorly understood. We wish to catch the early onset of AGN activity to test details of AGN accretion physics that cannot be constrained in any other way. We propose a ToO program to obtain four COS spectra of Mrk 590 at different X-ray flux levels as its AGN builds up. We will measure UV broad-line fluxes, constrain the UV and EUV ionizing continuum emission from the accretion disk, and establish the critical ionizing luminosity required for broad-line production, something that is still unknown. This allows us to test theoretical model predictions for the broad-line region physics. The efficient strategy we employ ensures that instructive constraints are obtained with a very modest HST program - yet, the full time request may not be needed. HST is the only telescope that can obtain spectra of the far-UV emission below 1900A that are crucial to reach our science goals. By combining this HST program with observations obtained with Swift, NuSTAR, XMM and VLT we will provide a comprehensive account of the black hole accretion state changes during the early onset of AGN activity as the AGN builds up. These HST/COS data will contribute with unique information to the legacy database on this intriguing object that will undoubtedly spawn new insight on AGN physics and the changing-look AGN phenomenon. We request COS low-resolution FUV observations of Seyfert 1 galaxy Mrk 590 to determine the strength of the AGN thermal disk continuum emission and the broad emission lines. Using the G140L grating with the 1105 cenwave setting (=1120-2100A) we will cover the Ly 1215, Nv 1240, Si iv+Oiv 1400, Civ 1549, and He ii 1640 broad emission lines in a single exposure. The resolution (R 1500-4000) is adequate to resolve the typical AGN narrow emission components; the [O III] 5007 narrow line width is FWHM~400 km s-1. The program consists of 4 ToOs (1 orbit each), that will be triggered based on SWIFT XRT and UV monitoring. Initially, Mrk590 will be monitored with Swift every 12 days. The first visit will be triggered when the XRT flux gets less than L1=0.3e-11 erg s-1 cm-2. The remaining 3 visits will be triggered once the XRT flux rises above the following limits: (0.5, 0.9, 1.3) x 10e-11 erg s-1 cm-2. Once the second orbit is triggered, SWIFT monitoring will intensify to ~daily cadence. We have requested 3 non disruptive ToOs (requested response time ~21 days) and 1 disruptive ToO (requested response time ~7 days). The disruptive ToO will be triggered only in case of rapid rise of the X-Ray and UV fluxes. We request long term status for these observations since we cannot guarantee trigger during cy29. The current observing strategy (see below) is based on previous COS observations of the same sources (e.g. PID 15448). We will update strategy, exposure time and ETC calculations as needed once visits are triggered and SWIFT UV fluxes are available. ==================================================== ACQUISITION: The target has precise 2MASS coordinates (ICRS reproduced with an error < 0.1"). We plan to use ACQ/IMG NUV MIRRORB and an exp time of 140s. For our ETC calculations we assume a flat continuum in fl normalized to half of the min observed UVW2 flux f_l ~1.1e-15 erg s-1 cm-2 Ang-1 @1928 Ang (http://etc.stsci.edu/etc/results/COS.ta.1030198/). This will ensure acquisition in case of "faint" state. The source will not pose a threat to the detector even if it ends up being 5 times more luminous than the max detected in the past 80 days (http://etc.stsci.edu/etc/results/COS.ta.1030199/). SCIENCE: We use the G140L grating at 1105Ang with FP_POS=ALL. For ETC calculations we assume a flat continuum normalized to the mean observed UVW2 flux in the past 80 days (http://etc.stsci.edu/etc/results/COS.sp.1030204/). Buffer time is set to 2/3 of the ETC buffer time. The source will not pose a threat to the detector even if it ends up being 5 times more luminous than the past 80 days (http://etc.stsci.edu/etc/results/COS.sp.1030205/). Since 2014 this team has been monitoring Mrk 590 with Swift, NuSTAR, VLA/VLBA and observed with groundbased telescopes including VLT/Xshooter, VLT/MUSE, Nordic Optical Telescope, Gemini, LBT, and MDM telescopes. Thereby the team has followed the flares that have occurred since 2017. With these multi-wavelength campaigns, the team studies the central engine physics in attempts to understand the optical changing-look AGN phenomenon, the nature of the radio source in Mrk 590 and to study AGN fuelling. Currently, the team has an ongoing 2-year joint Swift-VLBA program that runs through July 2022, a joint Swift-NuSTAR program through June 2022 and an ongoing VLT/X-shooter ToO program through HST Cycle 29. The VLT program supports this proposed program. A proposal to extend this VLT ToO program through Sept 2024 is in review. If needed, we can also obtain optical-IR spectroscopy with Nordic Optical Telescope or Gemini to support this HST program. We will submit telescope proposals in 2021 to extend the Swift monitoring (through Swift, VLBA XMM and NuSTAR) for another 2 years beyond July 2022. Team members have been involved with several studies of Mrk 590 as a Changing-Look AGN with more in preparation: Denney et al. 2014, ApJ, 796, 134 Koay et al. 2016a, MNRAS,455, 2745 Koay et al. 2016b, MNRAS, 460, 304 Mathur et al. 2018, ApJ, 866, 123 Raimundo et al. 2019, MNRAS, 486, 123 Of particular relevance: Lawther et al. (2021, in prep.) will present time-series analysis of the X-ray, UV, optical light curves since early 2017. * Dr. G. De Rosa is an expert on UV-optical-IR spectroscopy and COS instrument specialist. Dr. De Rosa will process and flux calibrate the COS data. * Dr. J.Y. Koay is a radio/sub-mm expert on AGN. With Koay as a lead, this team has two published papers on ALMA observations of Mrk 590 (Koay et al. 2016a,b; MNRAS,455, 2745; MNRAS, 460, 304) addressing the cold molecular gas reservoir and the radio source in Mrk 590, with a third ALMA paper in preparation. * Dr. D.P. Lawther is an expert on Swift and NuSTAR data analysis (e.g., Lawther et al. 2017, MNRAS, 467, 4674) and responsible for analysing the Mrk 590 X-ray spectra and performing time-series analysis of the X-ray and UV-optical light curves of Mrk 590 based on new and existing data obtained with Swift, NuSTAR, XMM and groundbased telescopes in order to constrain the nature of the inner accretion disk. A paper on time series analysis of existing X-ray and UV-optical light curves from Swift, NuSTAR and XMM telescopes is in preparation (Lawther et al. 2021; based on Dr. Lawther's recent PhD thesis). Dr. Lawther is responsible for processing and analysing the Swift, XMM and NuSTAR data in support of this HST program. Dr. Lawther also has expertise with photoionization modeling (Lawther et al. 2018, MNRAS, 481, 533) and will apply this expertise to this project. * Dr. S. Raimundo is expert on X-ray-UV properties of AGN accretion disk emission and in modelling the disk emission. Dr. Raimundo also has extensive spectroscopic experience with many telescopes, including VLT (Xshooter, MUSE) and Gemini. With Dr Raimundo as lead the team has published an optical IFU study with VLT/MUSE presenting spatially resolved imaging and kinematics of the central regions of Mrk 590 (Raimundo et al. 2019, MNRAS,486, 123); a follow up study of the fuelling mechanisms in this AGN is underway. Dr. Raimundo will perform accretion disk modeling of the SED based on the VLT, HST and X-ray data. * Dr. M. Vestergaard has long term expertise in spectroscopic studies of AGN and the AGN central engine, including analysis of VLT/X-shooter and HST/COS data. Dr. Vestergaard is the PI of many of the observational programs of Mrk 590 that have been executed since 2014. Dr. Vestergaard will analyse the HST and VLT data to constrain the UV and EUV continuum emission. Supermassive Black Holes and Active Galaxies 6 false false true false false false false false SUPPORTED GALAXY ACCRETION DISK BLR SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 1627586843312 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. 01/12/2022 GDR SWIFT flux: flambda@1928=1.12e-15 erg s-1 cm-2 Ang-1; Observing strategy is OK, no changes to observation plan (added ETC calculations). Acquisition will stil be succesful if the source gets significantly fainter, while it will not pose a risk if it gets 5x brighter (https://etc.stsci.edu/etc/results/COS.ta.1683253/) 1642988106000 70.6993671561954 (Tic-Visit :proposal-id 16699 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "29-Jul-2021 15:27:23.0" :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 52416 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16699 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16699 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2746 :al-overhead-at-end 0 :internal-dur-at-end 334 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 Non disruptive ToO. 1700122532192 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. /private/var/folders/zc/ljhf1lgn10b1yd9ytmwlp4jr00070l/T/OPVisit5777862038363674378.xml Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. 1700576348000 45.942968747574014 (Tic-Visit :proposal-id 16699 :visit-id "02" :proposal-version -1 :trans-version "20230626" :date "16-Nov-2023 03:15:29.0" :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 52416 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16699 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16699 :visit-id "02" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2690 :al-overhead-at-end 0 :internal-dur-at-end 350 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) true 1 0 Non disruptive ToO. 1627586844821 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. (Tic-Visit :proposal-id 16699 :visit-id "03" :proposal-version -1 :trans-version "20210514" :date "29-Jul-2021 15:27:24.0" :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 52416 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16699 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16699 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2746 :al-overhead-at-end 0 :internal-dur-at-end 334 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 Non disruptive ToO. 1627586845541 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. Observing strategy and exposure times are currently based on previous COS observations (PID 15448). We will update acq settings, exp times and ETC calculations as soon as the observations are triggered and SWIFT UV fluxes are available. (Tic-Visit :proposal-id 16699 :visit-id "04" :proposal-version -1 :trans-version "20210514" :date "29-Jul-2021 15:27:25.0" :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 52416 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16699 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16699 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2746 :al-overhead-at-end 0 :internal-dur-at-end 334 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 Disruptive ToO.