Science Keywords is a required field. Science Keywords: Select from 3 to 5 items. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. 0 Assigned ID: 2506 ----- Attempting Submission 1 (Fri Jun 20 15:27:02 GMT 2014) ----- HST Phase I Proposal 2506 (Ebrero-Merged-APT.apt) successfully submitted. ----- Attempting Submission 2 (Mon Jun 23 11:31:53 GMT 2014) ----- PI changed affiliations For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. 0 ----- Attempting Submission 1 (Fri Jul 11 14:49:13 GMT 2014) ----- Regarding both warnings, I think the first one is already addressed in the observing strategy, where we use for each grating three central wavelengths and different FP-POS settings for each of them in order to avoid gaps in critical parts of the spectrum. For the second one I think the target coordinates are accurate enough to ensure good quality data. AGN mass outflows inject enormous amounts of matter and energy into the interstellar medium of the host galaxy. Their location, structure, and importance as contributors to cosmic feedback processes are not yet fully understood. We propose to observe the Seyfert 1 galaxy NGC 985 with XMM-Newton for 240 ks using RGS as the prime instrument in order to accurately characterize the different ionized phases and kinematic components of the warm absorber. Together with HST/COS we will study the connection between the X-ray and UV absorbers and put stringent limits on the location of these winds in the context of the unification model of AGN. Our program consists of two 5-orbit visits simultaneous with two XMM-Newton observations. The second visit is nominally 12 days after the first XMM observation. For a median historical continuum flux of 2e-14 erg cm^{-2} s^{-1} A^{-1} (Dunn et al. 2006, PASP, 118, 572) the on-line COS Exposure Time Calculator requires 2700 s in G130M/1309 to cover Ly-alpha and N V, 3200 s with G160M/1600 for Si IV and C IV, and 5700 s with G140L/1280 to cover Ly-beta and O VI. In a single 5-orbit visit we can achieve the requisite exposure times with all three gratings. Each visit in our program will consist of multiple spectra for each grating. Since NGC 985 is faint enough, and all historical flux levels are more than a factor of two below safe limits, we will use an imaging target acquisition for each visit. For G130M, we will use three central wavelength settings that avoid placing the gap between segments A and B near the intrinsic absorption complex in NGC 985. At the same time, each central wavelength setting will obtain coverage of the segment gap in the other spectra. For each central wavelength setting, we will use different FP-POS settings, giving us a total of 4 independent grating settings with G130M that will allow us to eliminate all detector features and maximize our S/N in the merged spectrum. For G160M, we will again have 5 independent grating settings, but spread among four central wavelength settings in order to place the gap between the segments in the red wing of C IV as far from line center as possible, so that detector edge effects do not affect the intrinsic absorption lines in the blue wing of C IV. To allow for a broad range of variability in NGC 985, we have chosen BUFFER TIMES significantly shorter than the 2/3 factor recommended in the ETC. We have also chosen the BUFFER TIMES to be integer multiples of (exposure time - 110 s) to minimze the overheads due to buffer readouts between successive exspoures. These observations pose no bright object concerns. All historical flux levels for NGC 985 lie well below the bright object limits for COS. Since Mrk 335 has been observed successfully before with STIS, there are also no surrounding field objects that are too bright. This is confirmed by the BOT tool for GALEX in APT. The violation indicated in the GSC-II BOT check is for the extended host galaxy. AGN/QUASARS Default false false false false false SUPPORTED GALAXY SEYFERT This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 1.47e-14 at 1413 A COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G140L 1280 /tmp/OPVisit2615357890514310296.xml 1405084169664 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. Simultaneous with first XMM-Newton visit. (Tic-Visit :proposal-id 13812 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "11-Jul-2014 15:09:29.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 2122448 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13812 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13812 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2629 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2774 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2765 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2770 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) true 5 0 Exposure time is 5x ETC result to allow for target variability. We want to ensure successful target acquisition even if the target is much fainter than expected. 1291 with FP-POS=4 gives wavelength coverage down to 1130 A. Gap is still placed in red wing of Ly alpha, but far enough to the blue of N V to avoid the intrinsic absorption. 1309 with FP-POS=4 places gap on red side of N V, and avoids overlap with gap in subsequent 1327 exposures. 1327 with FP-POS=1 and 2 places gap in far red wing of N V, and non-overlapping with gaps in 1291 and 1309. 1327 with FP-POS=1 and 2 places gap in far red wing of N V, and non-overlapping with gaps in 1291 and 1309. 1577 FP-POS=3,4 places gap in far blue wing of C IV. 1577 FP-POS=3,4 places gap in far blue wing of C IV. 1611 with FP-POS=1 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. 1600 with FP-POS=2 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. 1589 with FP-POS=3 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. /tmp/OPVisit363118926850711250.xml 1405084173027 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. Simultaneous with second XMM-Newton visit. This is nominally 12 days after the first observation. (Tic-Visit :proposal-id 13812 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "11-Jul-2014 15:09:32.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 2122448 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13812 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13812 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2629 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2774 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2765 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2770 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13812 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2998 :pcs-gap 0 ) true 5 0 Exposure time is 5x ETC result to allow for target variability. We want to ensure successful target acquisition even if the target is much fainter than expected. 1291 with FP-POS=4 gives wavelength coverage down to 1130 A. Gap is still placed in red wing of Ly alpha, but far enough to the blue of N V to avoid the intrinsic absorption. 1309 with FP-POS=4 places gap on red side of N V, and avoids overlap with gap in subsequent 1327 exposures. 1327 with FP-POS=1 and 2 places gap in far red wing of N V, and non-overlapping with gaps in 1291 and 1309. 1327 with FP-POS=1 and 2 places gap in far red wing of N V, and non-overlapping with gaps in 1291 and 1309. 1577 FP-POS=3,4 places gap in far blue wing of C IV. 1577 FP-POS=3,4 places gap in far blue wing of C IV. 1611 with FP-POS=1 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. 1600 with FP-POS=2 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. 1589 with FP-POS=3 places gap in far wing of C IV with no overlap with gaps in other central wavelngth settings. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.