DDT/ToO proposal 1968798425 Assigned ID: 1114 ----- Attempting Submission 1 (Fri Jul 03 13:46:07 GMT 2020) ----- 0 ----- Attempting Submission 1 (Fri Jul 17 20:03:02 GMT 2020) ----- 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 0 Mrk 590 is a changing-look AGN that is currently in an unusual low flux state, after several years of flaring. This offers a very rare opportunity to constrain the unknown threshold ionizing luminosity required for production of broad emission lines in AGN, something that is very difficult to do unless the target and conditions are just right. Given the stochastic nature of black hole accretion and the past history of strong flares this program cannot wait for the next Cycle. We propose to obtain a 1-orbit COS spectrum of Mrk 590 now (non-disruptive, within the normal ~3 week turn around time scale) to test for the presence of broad UV emission lines. We will measure UV broad-line fluxes (or upper limits) and constrain the UV-EUV continuum emission from the accretion disk. By combining these measurements and previous observations of this target we will constrain the threshold ionizing luminosity required for broad-line production. This allows us to test existing theoretical models of broad line production. This HST program is part of a larger ongoing campaign with Swift, NuSTAR, XMM and VLT to provide a comprehensive account of the 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 propose to obtain COS low resolution FUV observations of the Seyfert 1 galaxy Mrk 590 to determine if the AGN thermal emission and broad emission lines are present at the current X-ray level as detected by Swift. Using the G140L grating @1105 Ang we will be able to cover the Lya1215, NV1240, Si IV + O IV1400, C IV1549, HeII1640 and CIII]1909 broad emission lines in a single exposure. The grating resolution is adequate to resolve the typical AGN narrow emission components; the width of the [O III]5007 narrow line is FWHM~400 km s-1. As explained in the Phase I, the target has been closely monitored with SWIFT. The latest UVW2 flux (centroid wavelength 1928), obtained on July 15th 2020, is equal to ~2.4e-15 erg s-1 cm-2 Ang-1. Note: the target has already been successfully observed in the same configurations during faint state (PID 13518) 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 70 s. For our ETC calculations we assume a flat continuum in f_l normalized to the min observed UVW2 flux since 2014 f_l ~6.5e-16 erg s-1 cm-2 Ang-1 @1928 Ang (http://etc.stsci.edu/etc/results/COS.ta.1456009/). 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 2 times more luminous than the max detected in the past 10 years f_l ~8.4e-15 erg s-1 cm-2 Ang-1 @1928 Ang (http://etc.stsci.edu/etc/results/COS.ta.1456018/). SCIENCE: We use the G140L grating at 1105Ang with FP_POS=ALL. For ETC calculations we assume a QSO FOS template, redshifted to z=0.02609 and normalized to the observed UVW2 flux in July 2020 (http://etc.stsci.edu/etc/results/COS.sp.1456015/). 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 2 times more luminous than the max detected in the past 10 years f_l ~8.4e-15 erg s-1 cm-2 Ang-1 @1928 Ang (http://etc.stsci.edu/etc/results/COS.sp.1456016/). Since 2014 this team has been monitoring Mrk 590 with Swift, NuSTAR, VLA/VLBA and groundbased telescopes including VLT/Xshooter, Nordic Optical Telescope, Gemini, LBT and MDM telescopes and have 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. 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 * 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. * PhD student D.P. Lawther is the team expert on Swift and NuSTAR data analysis (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. Lawther is responsible for processing and analysing the Swift, NuSTAR and XMM data in support of this HST program. Lawther also has expertise with photoionization modeling (Lawther et al. 2018, MNRAS, 481, 533) and will apply this expertise to this project. * Dr. B. M. Peterson is a long term expert on AGN variability and reverberation mapping (i.e., time series analysis) and observational studies of AGN physics. Dr. Peterson is a co-investigator of previous studies of Mrk 590, including reverberation mapping studies and the paper identifying Mrk 590 as a changing-look AGN: Denney et al. 2014. Dr. Peterson will assist the time series analysis (X-ray - UV/optical study of emission lines and continuum). * 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 and is PI on a recently published optical IFU study with VLT/MUSE presenting spatially resolved imaging and kinematics of the central regions of Mrk 590 (Raimundo et al. 2019) and is currently leading a study of the fuelling mechanisms in this AGN (Raimundo et al. 2020, in prep.). 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 0 false SUPPORTED GALAXY ACCRETION DISK BLR NUCLEUS SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 AGN V-band magnitude is currently 14.8mag COS/FUV Spectroscopic No No G140L 1105 /private/var/folders/mq/5zr2tpc15m35ymqm8nqqgf0r0001_y/T/OPVisit11049744859919514236.xml 1595016175057 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. COS FUV spectrum (Tic-Visit :proposal-id 16417 :visit-id "01" :proposal-version -1 :trans-version "20200518" :date "17-Jul-2020 16:02:55.0" :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 87168 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16417 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16417 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2748 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0