0 Assigned ID: 5184 ----- Attempting Submission 1 (Mon Mar 25 15:24:02 GMT 2024) ----- HST Phase I Proposal 5184 successfully submitted. Receipt: # 5184-1 ----- Attempting Submission 2 (Tue Mar 26 13:27:20 GMT 2024) ----- HST Phase I Proposal 5184 successfully submitted. Receipt: # 5184-2 ----- Attempting Submission 3 (Tue Mar 26 13:32:30 GMT 2024) ----- HST Phase I Proposal 5184 successfully submitted. Receipt: # 5184-3 ----- Attempting Submission 4 (Tue Mar 26 14:29:13 GMT 2024) ----- HST Phase I Proposal 5184 successfully submitted. Receipt: # 5184-4 ----- Attempting Submission 5 (Tue Mar 26 21:07:34 GMT 2024) ----- HST Phase I Proposal 5184 successfully submitted. Receipt: # 5184-5 ----- Attempting Submission 6 (Tue Mar 26 23:22:41 GMT 2024) ----- COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE 0 ----- Attempting Submission 1 (Fri Aug 09 18:01:46 GMT 2024) ----- coordinates are accurate to 0.1" - target has successfully been observed with COS in the past A new laboratory for fundamental AGN physics A bona-fide AGN in the 1990s, Mrk 590 now flares repeatedly in a low flux 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 up to five COS spectra of Mrk 590 at different X-ray/UV 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 flow, and 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 (new and archival) observations obtained with Swift, NuSTAR, LCO and VLT we will provide a comprehensive account of the black hole accretion state changes during the early onset of AGN activity. 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, including the extreme variability seen in some objects. 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 5 ToOs (1 orbit each), that will be triggered based on SWIFT and LCO monitoring. Mrk590 is being monitored with Swift every 10 days and with LCO every 4 days. Once the source Xray flux drops below the `2013 low', we will obtain VLT reference spectra to confirm the lack of broad lines. If broad Halpha emission is still present below `2013 low', the HST program will not be triggered until Mrk 590 fades further to a point where the optical broad lines and continuum vanish both in VLT & LCO data. This ensures that we capture the initial response of the broad-line region to a subsequent continuum increase. We reserve (up to) 3 COS ToOs to identify the threshold for no broad UV lines to be present (Limit 1) to exclude hysteresis effects (i.e. a line `afterglow'). Then, we activate VLT, LCO and HST observations when the XRT flux rises above one of two well-defined XRT flux levels, selected to be evenly spaced between Limit 1 and Limit 2, e.g. at (0.3, 0.9) x 10e11 erg/s/cm2. We have requested 4 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 cy32. The current observing strategy (see below) is based on past successful COS observations of the same sources. 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 (aka NGC 863) with Swift, NuSTAR, VLA/VLBA and observed with groundbased telescopes including VLT/Xshooter, VLT/MUSE, Las Cumbres Observatory, 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 AGN physics, including the optical changing-look AGN phenomenon, the nature of the radio source in Mrk590 and to study AGN fuelling. Currently, the team has an ongoing joint Swift-VLBA program that runs through February 2025, a joint Swift-NuSTAR program through June 2024 and an ongoing VLT/X-shooter ToO program through Sept 2024. The VLT program supports this proposed program. A proposal to extend this VLT ToO program through Sept 2027 is in review. LCO monitoring (photometry and spectroscopy) is guaranteed through August 2025, paid via St. Andrews University, UK, with a planned paid extention to Sept 2027. We will submit telescope proposals in 2024 and 2025 to extend the Swift monitoring (through Swift, VLBA and NuSTAR) for another 2 years beyond February 2025. 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 Lawther et al. (2023, MNRAS, 519, 3903) 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 former 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 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 (Lawther et al. 2023, MNRAS, 519, 3903 and Lawther et al. 2024, in prep). 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 assist in applying 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 Mrk590 that have been executed since 2014. Dr. Vestergaard will analyse the HST and VLT data to constrain the UV and EUV ionizing continuum emission. Supermassive Black Holes and Active Galaxies 6 false false true false false false false false SUPPORTED GALAXY ACCRETION DISK BLR NLR SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 aka Mrk590 The scheduling data was generated by CASM 31.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 31.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 31.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 31.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 31.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1105 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit8037088078674972147.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. (Tic-Visit :proposal-id 17742 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "09-Aug-2024 13:51:00.0" :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 17742 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17742 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :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 3005 :pcs-gap 0 ) true 1 0 Non disruptive ToO. The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit13138722289742771602.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. (Tic-Visit :proposal-id 17742 :visit-id "02" :proposal-version -1 :trans-version "20240604" :date "09-Aug-2024 13:51:00.0" :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 17742 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17742 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :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 3005 :pcs-gap 0 ) true 1 0 Non disruptive ToO. The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit12336379034835119373.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. (Tic-Visit :proposal-id 17742 :visit-id "03" :proposal-version -1 :trans-version "20240604" :date "09-Aug-2024 13:51:01.0" :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 17742 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17742 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :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 3005 :pcs-gap 0 ) true 1 0 Non disruptive ToO. The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit3622014298813764254.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. (Tic-Visit :proposal-id 17742 :visit-id "05" :proposal-version -1 :trans-version "20240604" :date "09-Aug-2024 13:51:01.0" :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 17742 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17742 :visit-id "05" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :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 3005 :pcs-gap 0 ) true 1 0 Non disruptive ToO. The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit6414638839437278735.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. (Tic-Visit :proposal-id 17742 :visit-id "04" :proposal-version -1 :trans-version "20240604" :date "09-Aug-2024 13:53:11.0" :trans-errors '(:WARNINGS 5 :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 17742 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17742 :visit-id "04" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :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 3005 :pcs-gap 0 ) true 1 0 Disruptive ToO.