0 Assigned ID: 341 ----- Attempting Submission 1 (Thu Apr 06 23:55:28 GMT 2017) ----- POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures. The dither patterns we use should be the standard 4-point dithers for maximizing PSF sampling. If there is anything incorrect about our choices, please let us known as soon as possible. Thanks! -903336498 ----- Attempting Submission 1 (Mon Jul 17 17:55:30 GMT 2017) ----- HST Phase II Proposal 15319 (15319_Phase2_version1_bak.apt) successfully submitted. Receipt: # 15319-1 ----- Attempting Submission 2 (Tue Jul 18 17:38:51 GMT 2017) ----- We only have one visit because our program is less than 5 orbits. The warnings generated by the APT pertain to concerns about dithering the ramp filter observations, which have a small FOV. However, the dithers are very small with respect to the FOV, and so should present no issue, unless I have misunderstood something. The HST View of Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy? Galaxy interactions are ubiquitous and play a fundamental role in the evolution of galaxies and their supermassive black holes (SMBHs). While major galaxy mergers (M1/M2~1) often trigger accretion onto both SMBHs and enhance AGN activity, the influence of minor mergers (M1/M2<1/3) on AGN fueling is poorly understood, although there is evidence that minor mergers predominantly trigger AGN activity in the primary galaxy. The dual AGN system Was 49, by contrast, is a unique system composed of a dwarf galaxy in a minor (M1/M2~1/10) merger with a disk galaxy in which the dwarf galaxy hosts a heavily obscured AGN with a luminosity of over 10^45 erg/s, while the AGN in the primary galaxy is over one thousand times less luminous. Furthermore, the black hole powering the AGN in the dwarf galaxy is much larger than black hole/galaxy scaling relations predict, with a mass of over 2% that of the stellar mass of its host. While the stellar host of this powerful AGN has been identified, the low spatial resolution of ground-based observations has limited our ability to determine the nature of this strange object. High-resolution continuum and narrow-band imaging of Was 49 is critical to understanding how such a powerful AGN could exist in a such a low mass host galaxy, as well as how this AGN is affecting its environment. Only Hubble has the resolving power and the filtering capability to determine the structure of this dwarf galaxy and the effect that the powerful AGN it hosts is having on it. This study will yield key insights into how large black holes grow in low mass galaxies, the role of minor mergers on SMBH fueling, and the effect of AGN 'feedback' before merger coalescence. The final TAC allocation was the same as our original proposal. Therefore, the observations will be split into three orbits. In one orbit, WFC3 will be used for observations with the F225W and F160W filters, 3 frames per filter, with a total of 30 minutes and 6 minutes, respectively. For another orbit, ACS will be used, with the FR551N filter x 3 frames, total = 25 minutes, and the FR647M filter x 3 frames, total = 6 minutes. For the third orbit, ACS will be used, with the FR716N filter x 3 frames, total = 25 minutes, and the FR914M filter x 3 frames, total = 6 minutes. The ACS ramp filters will be centered as follows. FR551N: 532.6 nm ([OIII]5007 at z = 0.06353) FR647M: 585.0 nm FR716N: 698.1 nm FR914M: 860.0 nm (H-alpha at z = 0.06353) Massive Black Holes And Their Host Galaxies 6 false false false false false false false SUPPORTED GALAXY INTERACTING GALAXY NLR SEYFERT J2000 J2000 WFC3/UVIS Imaging No No F225W WFC3/IR Imaging No No F160W ACS/WFC RampFilter No No FR551N ACS/WFC RampFilter No No FR647M ACS/WFC RampFilter No No FR716N ACS/WFC RampFilter No No FR914M POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 2 false POS-TARG DITHER 0.262 LINE 0.192 false false 68.14 4 18.39 ACS-WFC-DITHER-BOX 3 false The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1528246498000 112.30000000000001 (Tic-Visit :proposal-id 15319 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "18-Jul-2017 13:37:08.0" :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 1336768 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15319 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15319 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2891 :al-overhead-at-end 0 :internal-dur-at-end 596 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3225 :pcs-gap 0 ) true 1 0 AGN F160W magnitude = 17.9 (Vega; SED fit prediction) 1522330373000 168.67071139659862 (Tic-Visit :proposal-id 15319 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "18-Jul-2017 13:36:47.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 1137264 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15319 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15319 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2892 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3225 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15319 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3001 :al-overhead-at-end 0 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3225 :pcs-gap 0 ) true 2 0 The dither pattern is the standard 4 point box dither to optimize PSF sampling. The dither should not be an issue for the limtied FOV of the ramp filters. The dither pattern is the standard 4 point box dither to optimize PSF sampling. The dither should not be an issue for the limtied FOV of the ramp filters. The dither pattern is the standard 4 point box dither to optimize PSF sampling. The dither should not be an issue for the limtied FOV of the ramp filters. The dither pattern is the standard 4 point box dither to optimize PSF sampling. The dither should not be an issue for the limtied FOV of the ramp filters. Repeat of failed visit 01. 1530174138000 109.09724121213372 (Tic-Visit :proposal-id 15319 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "18-Jul-2017 13:37:08.0" :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 1336768 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15319 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15319 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2891 :al-overhead-at-end 0 :internal-dur-at-end 596 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3225 :pcs-gap 0 ) false 1 0 AGN F160W magnitude = 17.9 (Vega; SED fit prediction)