0 Assigned ID: 1603 ----- Attempting Submission 1 (Tue Oct 10 17:25:29 GMT 2017) ----- For a visit On Hold For another, a minimum separation of less than 17.0 Days is disruptive and requires permission from your program coordinator. (The minimum should allow time to receive/analyze the data, and rewrite/resubmit/reschedule the visit.) Visit 01 --> schedulability 100% Updated phase 2 for visits 02 and 03 and their timing requirements; note the warning on visit 03. 568806939 ----- Attempting Submission 1 (Wed Oct 18 20:53:51 GMT 2017) ----- HST Phase II Proposal 15404 (15404.apt) successfully submitted. Receipt: # 15404-1 ----- Attempting Submission 2 (Thu Oct 19 01:02:04 GMT 2017) ----- HST Phase II Proposal 15404 (15404.apt) successfully submitted. Receipt: # 15404-2 ----- Attempting Submission 3 (Thu Oct 19 21:56:44 GMT 2017) ----- ----- Attempting Submission 4 (Thu Nov 09 19:16:44 GMT 2017) ----- As per agreement with PC, I checked the boxes 'on hold' and entered the timing requirements. The suitable timing requirements voilate the limit for non-disruptive ToO, but this program is already categorized as disruptive ToO by PC. Thanks! 0 After a 10-year hiatus, Mrk 590 appears to be rekindling its nuclear activity! This offers a very rare opportunity to document the onset of AGN activity as it occurs that can lead to a better understanding of the long-standing issue of how AGNs are fuelled. We request a single observation as soon as possible and a five-visit ToO program triggered by the 0.3-10keV Swift X-ray flux to establish with HST/COS the amount of UV nuclear continuum and line emission at each of the 6 observing epochs, ~3 weeks apart, and thereby probe the AGN accretion state changes with time as the AGN turns on. We currently monitor Mrk 590, in response to two sudden and strong X-ray flares in Sept 2017, following previous minor flares, which indicate that the AGN may soon turn on again. We continue to monitor Mrk 590 with Swift (optical-UV-X-ray continuum), the VLBA (radio continuum) and optical ground-based telescopes. We are missing a ~1000 A< lambda< ~2000A spectrum to characterize the state of the far-UV emission. We aim to establish when a thin accretion disk and the broad emission line region are re-established. Given the nature of this transitory state we cannot wait for the next GO program in Cycle 27. These data will be combined with continuing monitoring with Swift and ground-based telescopes in order to determine the time scales and order in which the emission components appear as the central engine is being re-established. 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 have re-appeared in response to the significant increase in X-ray and far-UV emission as detected by Swift when this program is triggered. 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, and in the past 80 days UVW2 fluxes (centroid wavelength 1928) have varied from a minimum of ~2.2e-15 erg s-1 cm-2 Ang-1 to a max of ~4.0 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 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/). Massive Black Holes And Their Host Galaxies 0 SUPPORTED GALAXY ACCRETION DISK BLR SEYFERT NO The source has been monitored with SWIFT, information sent to cs. J2000 J2000 UM2=3.5 erg s-1 cm-2 Ang-1 (pivot wavelength 2246 ang) 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 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 1508450079990 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1509563646000 11.568650260568603 (Tic-Visit :proposal-id 15404 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "19-Oct-2017 17:54:39.0" :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 15404 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15404 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2642 :al-overhead-at-end 0 :internal-dur-at-end 331 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) true 1 0 1508374833838 Timing link suitability includes constraints ([03 After 02 by 5.0 to 28.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 15404 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "18-Oct-2017 21:00:33.0" :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 15404 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15404 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2866 :al-overhead-at-end 0 :internal-dur-at-end 331 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) true 1 0 Waiting for the trigger from Swift X-ray monitoring that is currently undertaken. PI will trigger the observation on the program website when relevant. We kindly ask for this visit to be scheduled as soon as is possible after the trigger. 1510235703329 /private/var/folders/4n/8bmj59qd6g79221m1j80lg2w0000gr/T/OPVisit2042777739607719005.xml Timing link suitability includes constraints ([03 After 02 by 5.0 to 28.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 15404 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "09-Nov-2017 14:55:02.0" :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 15404 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15404 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2866 :al-overhead-at-end 0 :internal-dur-at-end 331 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3202 :pcs-gap 0 ) true 1 0 This visit should occur as soon as possible after 5 days from visit 02 (visit 02 is triggered). However, a time frame up to 28 days is acceptable. Any later and the science goals cannot be achieved.