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.) Small GO Proposals are not allowed in Cycle 26 unless they are Joint Programs. Wavelength is a required field. Wavelength is a required field. 0 Assigned ID: 613 ----- Attempting Submission 1 (Tue Nov 27 14:51:57 GMT 2018) ----- Joint HST/XMM For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. TIMETAG EXPOSURE SHORTENED TO AVOID DATA LOSS Updated BUFFER TIMES again. Please ignore the immediate prior resubmission, v2. -1483252148 ----- Attempting Submission 1 (Tue Jan 08 15:45:50 GMT 2019) ----- ----- Attempting Submission 2 (Thu May 30 17:16:36 GMT 2019) ----- HST Phase II Proposal 15669 (mrk110_15669v2.apt) successfully submitted. Receipt: # 15669-2 ----- Attempting Submission 3 (Thu May 30 17:24:57 GMT 2019) ----- For G160M, for such a short exposure time and S/N, 4 FPPOS positions for each of our two central wavelength settings is overkill. We plan for 2 FPPOS positions for each setting, giving four different locations on the detector for each wavelength. Thanks to high resolution spectroscopy, the X-ray emitting broad line region has been recently discovered and studied in few bright type 1 Seyferts. We propose to observe for 120 ks the bright AGN Mrk110, simultaneously with HST-COS. The goal is to model for the first time the panchromatic broad line region emission in a Narrow Line Seyfert~1 galaxy. We will use the broad lines from the optical, UV and X-rays in a global modeling that will characterize the stratification, extend and ionization of the broad line emitting region, whose Xray extension still awaits a full characterization. We will observe Mrk 110 with HST-COS simultaneously with one of our three XMM-Newton/RGS pointings. With this HST observation we will study as many as 6 broad emission lines (Ly alpha, N V, C II, Si IV, C IV, and He II), which will be the backbone for our modeling of the X-ray broad-line region (XBLR). From our past work, in cases like this where no absorption lines are present, a S/N of 10 in the continuum is adequate to deblend Ly alpha and C IV from the neighboring N V and He II lines. The historical mean UV flux of Mrk 110 is F(1403 A)=1.3e-14 erg cm-2 s-1 A-1 (Dunn et al. 2006), a faintest observed flux of 1.2e-14, and a brightest observed flux of 1.8e-14. The target poses no bright object risk for any grating spectrum, and its flux is faint enough, even allowing for a factor of two potential brightening beyond its brightest observed flux, to use an imaging target acquisition. To guard against potential acquisition failure in the event the target is fainter than expected, we use an exposure time for Mirror B assuming Mrk 110 is only half as bright as it has ever been observed. We will use central wavelength setting 1222 for G130M to black geocoronal Ly alpha allowing us to use both detector segments and all four FP-POS positions to cover 1100-1360 A. COS ETC v26.2 gives an exposure time of 1502 s to reach S/N=10 at 1360, near the overlap with grating G160M. We will use grating G160M at central wavelength settings of 1533 and 1589 to cover Si IV, C IV, and He II. Achieving S/N=10 at 1560 in the continuum near C IV requires 2167 s. Massive Black Holes And Their Host Galaxies 6 false false false false false false false SUPPORTED GALAXY BLR NUCLEUS SEYFERT NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 1.3e-14 at 1403 A COS/FUV Spectroscopic No No G130M COS/FUV Spectroscopic No No G160M 1559236957934 /Users/gak/proposals/XMM_2018/mrk110/phase2/OP-cache/mrk110_15669v3-v01.xml The scheduling data was generated by CASM 27.0. CASM was run in Phase II mode. Coordinate with 1 of 3 planned XMM-Newton observations. (Tic-Visit :proposal-id 15669 :visit-id "01" :proposal-version -1 :trans-version "20181130" :date "30-May-2019 13:22:37.0" :trans-errors '(:WARNINGS 1 :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 548176 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15669 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15669 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2608 :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 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15669 :visit-id "01" :orbit-number 2 :pcs-time 302 :si-vis-utilization 2640 :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 2942 :pcs-gap 0 ) true 2 0 We use a conservatively long acquisition time (based on a flux lvel of 0.6e-14, half the previously observed minimum) to guard against an acquisition failure in case the target is in an unexpectedly low-flux state.