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. This target is not used in this proposal. Target is a required field. Instrument is a required field. Instrument Setup(s) is a required field. Please specify your scheduling constraints or 'No Constraints' on all Observation forms. 0 Assigned ID: 37 ----- Attempting Submission 1 (Thu Aug 02 13:15:19 GMT 2018) ----- Joint Chandra/HST POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. This version has been updated to deal with the new HST gyro situation, with typical reduction of <1 minute per exposure. 786382312 ----- Attempting Submission 1 (Tue Aug 21 22:20:11 GMT 2018) ----- ----- Attempting Submission 2 (Tue Dec 11 17:24:41 GMT 2018) ----- This is a small dither (sub-arcsecond) to sample the PSF and deal with cosmic rays and instrumental artefacts. We have confirmed in Aladin via APT that the r<5 arcsec region of interest is centered in the appropriate quadrant of WFC3. The dither step should be too small to make a significant difference to the science, assuming the aimpoint is correct. We propose a 250ks ACIS-S observation of IC 5063, a nearby type II Seyfert galaxy with strong 5 arcsec- long double-lobed radio emission interacting with a dense molecular disk to create a fast molecular outflow. The mechanism coupling the AGN to the molecular ISM is complex, and includes (1) photoionization, and (2) collisional ionization (shocks) from the interaction with small radio jets. (3) This process may also generate large-scale winds. There is no clear well-understood feedback picture. Hydro-dynamical simulations have shown that multiphase hot/cold interactions are important to understanding feedback. IC5063 is the optimal galaxy where we can image the details of that coupling directly with Chandra at a scale compatible with the ALMA and HST data. We aim to measure H-alpha, H-beta, the [S II] 6717,6731 and red continuum of IC 5062 (z~0.011) to complement existing [O III] and blue continuum observations previously made using WFPC2. Ratios between continuum-subtracted line maps will be used to make "BPT maps" to diagnose the local ionization state. The blue "continuum" observations should include lines in the [O III] H-beta complex, but with our new Balmer observations we will be able to determine any such contamination to better precision than was previously possible. The overall goals are similar to Program #15350 (PI: Maksym), as are the basic strategies. This program requires some changes with respect to specific filters, and it is a WFC3-only program (e.g. #15350 was a larger program that required ACS and the ramp filters for some targets). We begin with the archival FR553N [O III] images from HST WFPC2 to locate the faintest useful [O III] regions. We then assume the nuclear spectrum from the 6dF survey for line/line/continuum ratios. There is no ETC option for WFPC2-based normalization, so based on inspection of the ACS F606W filter throughput curve, we assume that it is a reasonable approximation for WFPC2 F606W for the purposes of spectral normalization. For the regions of interest, we infer S/N~3 within [1300,500,800]s for [FQ492N,F665N,F673N]. The 6dF spectrum does not cover the full F763M red continuum filter, so we assume the NGC 1068 Sy2 spectrum (200s). We will therefore obtain the optimal S/N with FQ492N and F763M packed in one orbit, and F665N, F673N packed in the other. For actual exposures, we expect S/N closer to ~5 per pixel in the fainter [O III] regions. Saturation does not appear to be an issue. We use an "optimal" pre-set dither to sample the PSF in all cases. This pattern shift is small enough that it should not affect quad filter vignetting, particularly given the region of interest is r<5 arcsec in extent. The exposure for FQ492N (H-beta) is most demanding, and based on its long exposure we use 3 pointings to eliminate cosmic rays. For all other filters, 2 exposures should be sufficient. We have packed exposures to ensure that buffer dumps can be read out in parallel to subsequent exposures. The bright object tool shows two bright objects which may be mildly saturated. These are not of interest to the program, and are far enough from the aimpoint that they may not fall within the FOV. From the ETC, saturation is not a danger. The BOT warns of 2 saturating stars that are not near the regions of interest. We use a 12e- pre-flash for all exposures. Massive Black Holes And Their Host Galaxies 6 false false false false false false false SUPPORTED GALAXY NLR NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No FQ492N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F763M POS-TARG DITHER 0.145 This pattern is meant to sample the PSF, and to offset from hot pixels. LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 2 false POS-TARG DITHER 0.135 This pattern is meant to sample the PSF, and to offset from hot pixels. LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 3 false 1544548317100 /private/var/folders/s1/wrm78pt95d170cr669g4yxc40000gn/T/OPVisit17380564221397013683.xml The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. Two short F763M exposures will sample the red continuum for lines observed in Visit 02, with a 2-point dither for cosmic rays and PSF sampling. Three FQ492N exposures will sample H-beta, with a 3-point dither for cosmic rays and PSF sampling. (Tic-Visit :proposal-id 15609 :visit-id "01" :proposal-version -1 :trans-version "20181130" :date "11-Dec-2018 12:11:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1443728 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15609 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15609 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3053 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3389 :pcs-gap 0 ) true 1 0 Two short F763M exposures will sample the red continuum for lines observed in Visit 02, with a 2-point dither for cosmic rays and PSF sampling. Three FQ492N exposures will sample H-beta, with a 3-point dither for cosmic rays and PSF sampling. 1544548329710 /private/var/folders/s1/wrm78pt95d170cr669g4yxc40000gn/T/OPVisit528675402745870759.xml The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. Two F665N exposures will sample the H-alpha, with a 2-point dither for cosmic rays and PSF sampling. Two F673N exposures will sample [S II], with a 2-point dither for cosmic rays and PSF sampling. (Tic-Visit :proposal-id 15609 :visit-id "02" :proposal-version -1 :trans-version "20181130" :date "11-Dec-2018 12:12:09.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15609 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15609 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3054 :al-overhead-at-end 123 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3389 :pcs-gap 0 ) true 1 0 Two F665N exposures will sample the H-alpha, with a 2-point dither for cosmic rays and PSF sampling. Two F673N exposures will sample [S II], with a 2-point dither for cosmic rays and PSF sampling.