0 Assigned ID: 2190 ----- Attempting Submission 1 (Fri Apr 09 20:12:12 GMT 2021) ----- HST Phase I Proposal 2190 successfully submitted. Receipt: # 2190-1 COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Resubmission to reduce ORIENT range allowed for more optimal placement. This results in loss of 1 day in schedulability -680648924 ----- Attempting Submission 1 (Wed Jul 21 22:15:10 GMT 2021) ----- ----- Attempting Submission 2 (Fri Aug 06 21:58:42 GMT 2021) ----- ----- Attempting Submission 3 (Wed Aug 18 20:24:57 GMT 2021) ----- ----- Attempting Submission 4 (Tue Jan 11 15:07:09 GMT 2022) ----- HST Phase II Proposal 16728 successfully submitted. Receipt: # 16728-4 ----- Attempting Submission 5 (Tue Jan 11 15:11:29 GMT 2022) ----- The COS target is spatially resolved and will require non-standard data reductions. Our team has experience using COS for extended sources and will follow techniques outlined in Somalwar et al., 2020. Galaxy evolution models require feedback from AGN to suppress star-formation in massive galaxies. However, the mechanisms that enable AGN feedback to reach galactic scales are hotly debated. Two key models are: (1) direct radiation pressure on dust and (2) ISM entrainment in hot winds. Measurements of the presence and properties of any hot wind component of AGN outflows thus represent a critical means of identifying dominant AGN feedback mechanisms. Sensitive and spatially resolved UV diagnostics from highly ionized emission go beyond differentiating AGN photoionized gas and shocks to serve as barometers that enable estimates of any hot wind pressure. These highly ionized UV line diagnostics (O VI/N V) were recently used to demonstrate that the dynamics of the UV emitting, outflowing clouds from a prototypical superwind driven by a radio-quiet AGN are dominated by radiation pressure with negligible compression by a hot wind. These observations indicate that this AGN outflow is driven by radiation pressure or was driven by a hot wind that has since dissipated despite ongoing AGN activity. On the other hand, AGN outflows driven along the jets of radio-loud systems are thought to be ISM entrained in a hot wind associated with the jets. To test this prediction, we propose the first spatially resolved UV spectroscopy and complementary high-resolution VLA data of a known 5-30 kpc outflow of a recently rejuvenated radio-loud AGN. This will enable unique insights into the wind driving mechanisms, the physical conditions/properties of the outflow, and a detailed study of the jet and cool outflow morphology compared to a radio-quiet case. Our program goal is to obtain UV spectroscopy of the outflows driven by a radio-loud obscured quasar, J0113+0106 at z=0.2809. The spectra will enable UV diagnostics of the physical conditions of the outflowing gas based on the Ly-alpha, NV, and OVI emission lines. These lines occur at observed wavelengths of 1323, 1557, and 1587 Angstroms at z=0.2809. Based on optical spectra of the source, the line widths will be hundreds of km/s, so the low-resolution UV dispersers on COS and STIS are ideal. COS is a more sensitive UV spectrograph, and its large aperture is well-matched to the size of the Ly-alpha blob. We will therefore use COS G140L to observe the Ly-alpha blob, which covers the desired wavelength range. The spectral resolution of COS G140L will be degraded due to the extended nature of the target but is still more than sufficient for our purposes. The desired S/N can be obtained in 1 orbit. We will split the COS observations into four exposures, each at a different FP-POS setting to minimize flat fielding errors in the final spectrum. The COS aperture is too large to separate emission knots along the jet, so observing this region requires using STIS in longslit mode. We will orient the slit with the line connecting the knots along a position angle between 238.3 and 239.3 degrees, requiring an ORIENT of 283.3-284.3 degrees or 103.3-104.3 degrees. The knots observed in Ly-alpha emission are well matched to the 52x2" long slit, which will deliver the desired spectral coverage and resolution when paired with the G140L disperser. The desired exposure time can be achieved in three orbits which we will package into a single STIS visit to minimize overheads. To schedule the STIS observations, we will use the 2" slit width, which enabled a larger range of ORIENT options and enabled scheduling of the observations. The morphologies of both the nucleus and the blob are complicated and not well suited to direct target acquisition. Therefore, we will perform acquisition using a star, J011340.94+010730.71-ACQ-STAR, which has NUV- and i-band magnitudes of 22.3 and 16.3, respectively. The offset from the acquisition star to the two science targets is 1.3 arcmin. Coordinates for all three objects are from the Hyper Suprime-Cam survey. HSC astrometry is tied to GAIA and has a precision of 0.03 arcsec or better. We verified the acquisition star coordinates against GAIA directly and found excellent agreement. For COS, we will use ACQ/IMAGE acquisition with MIRRORA and a total exposure of 130 seconds, delivering an S/N of 35 (COS.ta.1525952). For the STIS CCD acquisition, we will use the F28X50LP filter with an exposure time of 3 seconds, delivering S/N more than sufficient for target acquisition (STIS.ta.1526127). The COS aperture and STIS slit are large enough that we do not anticipate issues if operating in 2-gyro mode apart from somewhat increased overheads when slewing from the acquisition star to the science targets. Our team consists of leading observers and theorists who are experts in multi-wavelength constraints and models for AGN feedback that incorporate HST data. Collectively, we have published over 100 articles on observations and theory of AGN outflows and have a strong record of combining HST data with models for new insights into galaxy and black hole evolution. PI S. Johnson has extensive experience with HST+COS and STIS both in archival analysis and as PI of the pilot for the current proposal which was led by co-I J. Somalwar and published in Somalwar et al., 2020. co-PI J. Stern is a theorist with extensive background on AGN outflows and a strong history of close collaboration with observers to discriminate between proposed AGN feedback mechanisms. J. Stern's modelling demonstrated that UV line ratios provide unique constraints on the physics of galactic scale AGN outflows (see Stern et al., 2016, Somalwar et al., 2020). K. Nyland is a leading expert on VLA observations and AGN feedback and will help guide the VLA observations planning, data reduction, analysis, and interpretation. A. Goulding is an expert in multi-wavelength observations of AGN whose analysis will help combine the proposed UV and radio data with insights from archival X-ray images. co-I's H.-W. Chen, J. Greene, J. Mulchaey, G. Rudie, G. Walth, and N. Zakamska are leading observers with collective experience studying AGN and galaxy evolution from the X-ray to radio. Their expertise will enable us to maximize the use of the proposed HST observations by combining constraints with those from existing multi-wavelength datasets. Moreover, with specialization ranging from black holes to the diffuse circum-galactic gas their perspective will provide broad context for interpreting the proposed observations in light of other observations of galaxy evolution generally. co-I M. Gaspari, is an expert simulations of galactic scale outflows whose input will enable us to make invaluable comparisons predictions from hydrodynamic simulations. Supermassive Black Holes and Active Galaxies Galaxies 6 false false true false false false false 1 true SUPPORTED GALAXY QUASAR RADIO GALAXY WIND YES J2000 J2000 NUV=21.7 EXT-MEDIUM WIND YES J2000 J2000 STAR G III-I G V-IV NO Coordinates are from GAIA+HSC J2000 NUV=22.3 i=16.3 STIS/FUV-MAMA Spectroscopic No No G140L 1425 COS/FUV Spectroscopic No No G140L 1105 1628286935346 The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. Spectroscopic observations of an [O III] emitting blob with COS+G140L. The acquisition sequence is performed on a nearby star followed by an offset to the science target position (Tic-Visit :proposal-id 16728 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "06-Aug-2021 17:55:35.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 52416 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16728 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16728 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2746 :al-overhead-at-end 0 :internal-dur-at-end 334 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 1641913843785 /private/var/folders/yt/tcmlxl155t37xjmj8043f09w0000gn/T/OPVisit9657449757173074831.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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