0 Assigned ID: 913 ----- Attempting Submission 1 (Fri Apr 07 21:26:32 GMT 2017) ----- HST Phase I Proposal 913 (bubble_COS.apt) successfully submitted. Receipt: # 913-1 ORBITAL VISIBILITY OVERRUN COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Switched visit 1 of the nuclear pointing to 1105 central wavelength. -748044351 ----- Attempting Submission 1 (Fri Jul 14 16:12:13 GMT 2017) ----- HST Phase II Proposal 15280 (bubble_COS.apt) successfully submitted. Receipt: # 15280-1 ----- Attempting Submission 2 (Mon Jul 17 17:05:13 GMT 2017) ----- HST Phase II Proposal 15280 (bubble_COS.apt) successfully submitted. Receipt: # 15280-2 ----- Attempting Submission 3 (Tue Jul 18 14:16:02 GMT 2017) ----- HST Phase II Proposal 15280 (bubble_COS.apt) successfully submitted. Receipt: # 15280-3 ----- Attempting Submission 4 (Wed Jul 19 17:36:05 GMT 2017) ----- HST Phase II Proposal 15280 (bubble_COS.apt) successfully submitted. Receipt: # 15280-4 ----- Attempting Submission 5 (Mon Mar 12 20:57:36 GMT 2018) ----- We are aware of the calibration issues with extended sources for COS and are prepared to put forward the extra effort required in the data reduction. Spatially resolved rest-UV spectroscopy of a prototypical quasar driven superwind at low-z Powerful galaxy-wide winds launched by quasars are thought to be a common evolutionary phase of massive galaxies, but observations of this phenomena are scarce. We have conducted a multi-wavelength observational campaign for J1356+1026, a poster-child obscured quasar driving a superwind at z=0.123. J1356+1026 is driving a nuclear molecular outflow and an extended ionized outflow observed as an [OIII] emitting bubble at ~10 kpc that is spatially coincident with soft X-ray emission. Quasar-driven winds carry material at a wide range of densities and temperatures making it difficult to measure their energetics and the dominant phases are unknown. Here we propose spatially resolved rest-UV spectroscopy by acquiring circum-nuclear absorption spectra of J1356+1026 and emission spectra of its off-nucleus bubble using COS+G140L. The circum-nuclear spectrum will provide measurements of the outflow velocity through blueshifted absorption while the off-nuclear spectrum of the bubble will measure the ionization state and mechanisms of the outflow through powerful UV diagnostic lines. Together, these spectra will enable a more complete mass, energy and momentum accounting of a spatially resolved quasar driven superwind for the first time. Furthermore, detection of shocked gas through OVI emission will enable us to infer properties of the enigmatic volume-filling, low density component of the wind. To our knowledge, this will be the first spatially resolved rest UV spectroscopy of a quasar wind and the proposed observations will serve as a pilot to guide future HST proposals. Our program goal is to obtain UV spectroscopy of the outflows being driven by J1356+1026 at z=0.123 to enable powerful UV diagnostics of the physical conditions of the outflowing gas. The wide wavelength coverage and moderate resolution of COS+G140L is ideally matched to our goal of obtaining UV spectra of J1356+1026. At z=0.123, the G140L spectrum will include intermediate and high ionization lines such as SiIV, CIV, NV, and OVI in addition lower ionization features such as CII, SiII, and SiIII. In addition, the COS primary science aperture is 2.5" in diameter which corresponds to 5.5 kpc at z=0.123. This is sufficient to include the majority of the light from both the nucleus which hosts the luminous AGN and the bubble with one pointing each. The COS aperture at these pointings is shown in Figure 1 panels C and D of the Phase I proposal. Based on the estimates from our phase 1 proposal, the nuclear pointing will require 4 orbits and the off-nuclear bubble pointing will require 1 orbit. The five orbit program will be split between two 2 orbit visits for the nucleus and a single 1 orbit visit for the bubble. One 2 orbit visit will observe the nucleus in G140L/1280 in all four FP-POS positions and the second will similarly observe G140L/1105 in all four FP-POS positions. The 1 orbit visit will observe the nucleus in G140L/1105 in all four FP-POS positions which provides coverage of all features of interest at z=0.123. J1356+1026 exhibits two nuclei, and though the targetted North nucleus is dominant in the blue, the irregular shape makes target acquisition with an offset star preferred. In order to place the nucleus in the COS aperture, we will acquire a nearby offset star with nuv magnitude 19.5 for 35 seconds, ensuring a total S/N of 50 based on the COS NUV acquisition ETC. We will then perform a 54" offset to place the nucleus in the aperture and acquire the proposed G140L nuclear spectra. We will acquire the bubble similarly. The bubble exhibits a clear ridge and spatial orientation and we will set the orient so that the COS spatial axis runs along the ridge (North-South) to within +/- 5 deg as described in Phase I. We therefore place an orient requirement of 130-140 deg on visit 2. 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CASM was run in Phase II mode. 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