Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. The total number of Primary Orbits used in all Cycles must equal the total number of Primary Orbits specified on all the Observations. (Compare totals reported on the first and second pages of the PDF Preview.) US Admin CoI is a required field. Wavelength is a required field. Please specify your scheduling constraints or 'No Constraints' on all Observation forms. 0 Assigned ID: 1240 ----- Attempting Submission 1 (Wed Sep 07 14:12:40 GMT 2016) ----- Joint Chandra/HST Initial submission of Phase II for Mrk 1018 ToO observations. The catalog UV magnitude of the AGN is too bright in the catalog as it is a transient source and shown to dim since 2013. Recent HST-COS observations were taken in Feb 2016 that should serve as the reference to check the health of the detector. Ongoing ground-based u-band monioring is being performed to check whether the AGN is further dimming or re-brighten. This information will be passed with the trigger so that saftey assumption can be re-evlauted compared to our initial plan. -1259008941 ----- Attempting Submission 1 (Mon Oct 03 21:41:42 GMT 2016) ----- We propose a joint TOO observation of Chandra (50 ks) and HST (2 orbits) of Mrk 1018. In February this year, we discovered the unambiguous case of a "changing look" quasar completing a full cycle: Mrk 1018 transformed from a Seyfert 1.9 to a Seyfert 1 in 1984, and it has just now transitioned back into a Seyfert 1.9. This state change is accompanied by extreme dimming in both X-ray and optical which might be still ongoing. Joint HST and Chandra observations are needed to constrain the current physical state of the accretion disk and embedded hot corona, respectively. This program will only be triggered if our optical monitoring programs detects a change of more than a factor of 5 in optical flux of Mrk 1018. Note that this proposal is accompanied by a GO proposal of the same object. Standard two-orbit COS/FUV G140L observation of Markarian 1018, using the Primary Science Aperture. 40 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 12 false false false false false false SUPPORTED GALAXY BLR QSO SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. UGC01597 HE0203-0031 J2000 J2000 7.5 counts/s in the 250s long COS NUV (PSA and MIRRORB) acquisition images from Feb 2016 COS/FUV Spectroscopic No No G140L 1484935346229 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /private/var/folders/tc/ydsxjyy102b9cplf304tbl300005f2/T/OPVisit1384613160682925887.xml UV spectroscopy of Lya and FUV continuum with COS of Mrk 1018 at the nucleus. (Tic-Visit :proposal-id 14853 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "20-Jan-2017 13:02:25.0" :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 365504 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14853 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14853 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2877 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3210 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14853 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2988 :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 3210 :pcs-gap 0 ) true 2 0 The nucleus of Mrk 1018 has significantly dimmed compared to the GALEX observations. Observations with COS in Feb 2016 show a total contrate in the NUV acquisition images of 920 counts/s and the FUV QSO spectrum had a continuum flux of 1e-15 erg/s/cm2/A at 1310A. We currently perform u-band monitoring with ground-based telescope which confirm that the nucleus has further dimmed by 0.4mag. We therefore assume that it is safe to use the PSA/MIRRORA configuration and base the ETC computation a continuum flux of 0.5e-15 erg/s/cm2/A to be little more conservative. We may need to update this slightly if something dramatic happens when triggering these observations. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the HST-COS observation taken in Feb 2016. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the HST-COS observation taken in Feb 2016. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the HST-COS observation taken in Feb 2016. ETC run is attached to verify the maximum count/rates expected if the source would be as bright as in the HST-COS observation taken in Feb 2016.