0 Assigned ID: 6 ----- Attempting Submission 1 (Fri Feb 19 19:48:08 GMT 2016) ----- Phase II plan for the DD observations of Mrk1018. Critical issue will be to converge on health/safety aspects as the source is catalouged to be a bright type 1 AGN, but current photometry has indicated that it has significantly faded. ACQ/IMAGE template changed from MIRRORA to MIRRORB and increase exposure times to 250sec to allow for a larger in potential NUV fluxes to be detected without safety issues. 2084854643 ----- Attempting Submission 1 (Tue Feb 23 10:56:07 GMT 2016) ----- ----- Attempting Submission 2 (Tue Feb 23 19:51:58 GMT 2016) ----- We propose an urgent, exciting, and short observation of Mrk 1018, the first changing look quasar ever discovered to unambiguously undergo a full cyclical transformation, flickering from Type 2 (narrow lined), to Type 1 (broad lined), and back to Type 2 once more. The source first transitioned from a Seyfert 1.9 to a Seyfert 1 nucleus in 1984, and remained broad-lined for 29 years. Last week, in analyzing our new VLT/MUSE IFU data, we were astonished to discover that the source has transitioned *back* to a Seyfert 1.9, sometime between 2013 and now. This is the first time a quasar has unambiguously gone "there and back again", and its second retreat to the shadows is not yet complete: the AGN has dimmed by a factor of 50-100 in *both* X-ray and optical since 2013, showing no signs of slowing. This extreme variability is due either to dramatic intermittency in the accretion rate, or because eclipsing clouds, which vacated our line of sight to reveal the broad line region in 1984, are occulting the broad line region once more. *Both* Chandra and HST are urgently needed to discriminate between these two hypotheses. A DDT is necessary because this event may be a very short-lived "flicker" (lasting mere months, rather than another year). With our Chandra DDT approved yesterday, we now require UV-through-NIR photometry with HST to (1) construct a clean pan-chromatic SED of the nucleus during this flicker event, (2) use Ly-a and UV continuum to constrain accretion models, and (3) map the circumnuclear environment on 80 pc scales, while the AGN is very dim. This is a short-lived chance to place simultaneous *temporal* and *physical* constraints on the Type 1 lifetime in a QSO. Standard two-orbit COS/FUV G140L observation of Markarian 1018, using the Primary Science Aperture. 150 sec ACQ/IMAGE observation to center on the UV photocentroid (the point source associated with the AGN). Four science exposures, spread over two orbits, are used to cycle through all four FP-POS positions. Massive Black Holes and their Hosts Galaxies 0 SUPPORTED GALAXY BLR QUASAR SEYFERT NO This object was generated by the targetselector and retrieved from the NED database. UGC01597 HE0203-0031 J2000 J2000 maximum continuum flux of 1.2e-14erg/s/cm2/A at 1350A from IUE and HST/FOS spectroscopy during bright phase. ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F625W WFC3/UVIS Imaging No No F336W WFC3/IR Imaging No No F140W COS/FUV Spectroscopic No No G140L 1105 1456256880610 /tmp/OPVisit8164189909180695672.xml The scheduling data was generated by CASM 24.0. CASM was run in Phase II mode. UV spectroscopy of Lya and FUV continuum with COS of Mrk 1018 at the nucleus. (Tic-Visit :proposal-id 14486 :visit-id "01" :proposal-version -1 :trans-version "20160129" :date "23-Feb-2016 20:48:00.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 330560 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14486 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14486 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2877 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3210 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14486 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2985 :al-overhead-at-end 0 :internal-dur-at-end 407 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3210 :pcs-gap 0 ) true 2 0 The exposure time for the acquisition is based on the assumption that the flux of the AGN nucleus has dropped by up to a factor 100 compared to the bright type 1 phase. We therefore set the exposure times so that the nucleus should be detected. If the source would be as bright as a few years ago the detector count limit would be exceeded by a factor of 3. However, recent ground-based u-band imaging obtained a week ago confirms that the u-band flux has dropped by several magnitudes compared to the original brightness between 1984 and 2012. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the archival IUE and HST/FOS spectra. However, we suspect that the source has dropped by a factor of ~50-100 in the FUV. Buffer times and count rates should be perfectly fine in any case. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the archival IUE and HST/FOS spectra. However, we suspect that the source has dropped by a factor of ~50-100 in the FUV. Buffer times and count rates should be perfectly fine in any case. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the archival IUE and HST/FOS spectra. However, we suspect that the source has dropped by a factor of ~50-100 in the FUV. Buffer times and count rates should be perfectly fine in any case. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the archival IUE and HST/FOS spectra. However, we suspect that the source has dropped by a factor of ~50-100 in the FUV. Buffer times and count rates should be perfectly fine in any case.