0 Assigned ID: 3059 ----- Attempting Submission 1 (Wed Aug 29 13:58:33 GMT 2012) ----- chandra Steve Penton is my contact person for this proposal, and I have been in communication with him on several relevant issues. This is a second submission after some changes suggested by Steve. 1397586419 ----- Attempting Submission 1 (Wed Sep 12 21:36:52 GMT 2012) ----- ----- Attempting Submission 2 (Fri Sep 14 20:55:19 GMT 2012) ----- I have discussed these remaining problems with Steve Penton, and I believe they are not applicable in my case. We propose a 170 ks HETGS observation of the bright Seyfert 1 galaxy NGC 3783 to explore the new parameter space of high-resolution warm absorber (WA) variation in ionization, structure, and kinematics over 11 yr. NGC 3783 is the ideal candidate for such a long-term variation study, due to its extraordinary baseline of HETGS (from 2000-2001) and UV spectroscopy, its extremely rich absorption spectrum, and its X-ray/UV brightness. In addition to mapping long-term WA evolution in unprecedented detail, we will assess joint X-ray/UV absorption variations over long time scales with a supporting HST COS spectrum; substantial UV variations over the past 11 yr indicate that corresponding X-ray variations should be detected and be physically informative. Note this is an accepted joint proposal between HST COS and Chandra HETGS. As per our original Chandra proposal, we prefer that the HST and Chandra observations be conducted reasonably close together in time (within about 10 days), although we do not have a formal time constraint. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Our new observations will complement about 30 yr of existing low-resolution and high-resolution UV spectroscopy. One orbit with each of the medium-resolution (G160M and G130M) FUV gratings should provide a S/N of about 30 in 3 ks (based on the HST exposure-time calculator) at excellent resolution (about 16 km/s). The continuum of NGC 3783 has been consistently bright, with F_lambda of about 4e-14 erg/s/cm^2/A at 1470 A (e.g., see Figure 1a of Gabel et al. 2003a), so we do not expect a low S/N for our observations. The advantages of high S/N for this observation justify the use of a second HST orbit. Note this is an accepted joint proposal between HST COS and Chandra HETGS. As per our original Chandra proposal, we prefer that the HST and Chandra observations be conducted reasonably close together in time (within about 10 days), although we do not have a formal time constraint. I would be happy to provide a copy of the original Chandra + HST proposal if desired. Also, Steven Penton there at STScI has a copy already, I believe. Note this is an accepted joint proposal between HST COS and Chandra HETGS. As per our original Chandra proposal, we prefer that the HST and Chandra observations be conducted reasonably close together in time (within about 10 days), although we do not have a formal time constraint. 12 false 0.0 0.0 false false false false SUPPORTED GALAXY ACCRETION DISK SEYFERT WIND This object was generated by the targetselector and retrieved from the NED database. J2000 J2000 COS/FUV Spectroscopic No No G130M COS/FUV Spectroscopic No No G160M The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 1347656027842 /private/var/folders/zz/zzzivhrRnAmviuee+++cm+++8AU/-Tmp-/OPVisit8563389925761831566.xml (Tic-Visit :proposal-id 13115 :visit-id "01" :proposal-version -1 :trans-version "20120802" :date "14-Sep-2012 16:53:47.0" :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 835168 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13115 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13115 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2671 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3004 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13115 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2782 :al-overhead-at-end 0 :internal-dur-at-end 395 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3004 :pcs-gap 0 ) true 2 0 Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Previous COS observations place the target flux at F(1280)=4.5E-14; we used this flux to simulate the target with a composite QSO spectrum redshifted to z=0.00973. Total count rate on Segment A is 745 counts/s. To get S/N=40 on Seg A would take about 3.4s, we use 10s to ensure a good centering and allow for target variability. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Previous COS observations place the target flux at F(1280)=4.5E-14; we used this flux to simulate the target with a composite QSO spectrum redshifted to z=0.00973. Total count rate on Segment A is 745 counts/s. To get S/N=40 on Seg A would take about 3.4s, we use 10s to ensure a good centering and allow for target variability. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system. Here we are essentially repeating the HST COS observations of NGC 3783 done as part of program 12212 in order to investigate variation of its intrinsic multi-component UV absorption-line system.