Version #3 + tweaks to the abstract1754604602Assigned ID: 1516
----- Attempting Submission 1 (Tue Apr 06 20:22:08 GMT 2021) -----
HST Phase I Proposal 1516 successfully submitted.
Receipt: # 1516-1
----- Attempting Submission 2 (Thu Apr 08 19:26:09 GMT 2021) -----
HST Phase I Proposal 1516 successfully submitted.
Receipt: # 1516-2
----- Attempting Submission 3 (Fri Apr 09 19:15:00 GMT 2021) -----
HST Phase I Proposal 1516 successfully submitted.
Receipt: # 1516-3
----- Attempting Submission 4 (Fri Apr 09 23:24:50 GMT 2021) -----INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONSVersion 1596863689----- Attempting Submission 1 (Thu Jul 22 15:19:13 GMT 2021) -----All of these warnings were discussed with Primary Support Contact Elizabeth Nance. They fall under two categories:
APT is warning us about our inefficient ordering of FP-POS positions (3 or 4). But our choice of wavelength setting (cenwave = 1291 A) is dictated by our science. Once that is fixed and given that we need the full wavelength coverage (segments A and B simultaneously), it sets our request to use only FP-POS = 3 and 4 following COS2025 policies.
The other warning has to do with the fact that target #2 appears to be slightly extended so there will be "calibration limitations". We have taken note of this warning. Nothing else can be done about it.The Impact of Radio-Mode Feedback on the Circumgalactic Medium of Centaurus AThe iconic radio galaxy Centaurus A is the nearest example of radio-mode AGN feedback in action. Gas accretion onto the central supermassive black hole has powered multiple cycles of jet- and wind-driven outflows that span 10 orders of magnitude in physics scale from the milli-parsec radio jets and ultra-fast X-ray wind to the mega-parsec scale radio structure. Yet we still do not know if this giant radio structure is affecting the thermodynamic state of the circumgalactic medium (CGM) enough to prevent future star formation in this galaxy, as predicted by cosmological hydrodynamical simulations of massive galaxies. Here we propose high-S/N COS FUV spectroscopy of four newly catalogued FUV-bright background QSOs with projected distances of 130-150 kpc from Cen A to directly probe the radio structure of Centaurus A for the first time. These data will be combined with archival data of similar quality on QSOs with projected distances of 270-510 kpc (which will be used as control sight lines outside of the radio structure) to probe the covering fraction, kinematics, ionization, relative metallicity, and multi-phase nature of the CGM using a diverse set of diagnostics (Si II, Si III, Si IV, O I, and C II). These data will provide new insights into the process of radio-mode feedback and new tests for current and future models.We requested and were allocated 25 orbits to observe 4 targets with COS G130M. The requested number of orbits per target ranges from 5 to 9 orbits. We follow the Cycle 29 recommendations to limit the durations of each visit to 1-3 orbits: the 5-orbit allocations for targets #1 and #4 are each split into two visits of 3+2 orbits, the 6-orbit allocation for target #3 is split into two visits of 3+3 orbits, and the 9-orbit allocation for target #2 is split into three visits of 3+3+3 orbits. This strategy will reduce time loss to overheads (target acquisition) associated with shorter 1-orbit visits, increase time spent on target, and thus S/N.
For each visit, we first use ACQ/IMAGE to obtain a NUV image of the field and center the aperture on the intensity peak. For this procedure, we make use of MIRRORA for all of the targets since all of them have integrated GALEX NUV magnitudes > 18 (listed under "V magnitude" in the target description) so they are not particularly bright. The exposure time of 60 seconds for ACQ/IMAGE is generous and results in S/N that range over 50-100.
For the spectroscopic observations, we request the cenwave = 1291 A setting with both segments A and B for all of our targets to capture redshifted Si II 1190/1193, Si III 1206, Si II 1260, O I 1302, Si II 1304, C II 1334, and Si IV 1393/1402 from the CGM of Centaurus A (z = 0.00183). These metal transitions are among the strongest in massive quiescent, star-forming, and active galaxies, and cover a range of ionization level which can be used to constrain the conditions of the absorbing gas. Following the COS2025 policies, we only use FP-POS = 3 and 4 to get equal exposures for segments A and B. The exposures are split into 1 or 2 equal-duration observations per orbit with different FP-POS values to reduce the fixed pattern noise. The number of spectroscopic observations per orbit is chosen to minimize the overhead and maximize the on-target exposure time. All of the observations are done in TIME-TAG mode. This temporal sampling will allow us to exclude poor quality data and get improved thermal correction and background removal. For simplicity and to guard against the (unlikely) possibility that our targets are more than ~50% brighter than expected, we set buffer-time = exposure-time.
According to the Bright Object Tool (BOT), there are no bright sources near our targets that could cause a problem for COS.
The RA and DEC coordinates of these objects are extracted from the GSC 2.3 database and have been verified using the finding charts generated by the Target Confirmation tool of APT. The nearest target in the sample, target #2 (z = 0.1), appears to be slightly extended.Prof. Sylvain Veilleux from the University of Maryland is the PI of this program. He is an authority in the field of AGN feedback and galactic outflows. He has been the PI of five recent COS programs (PID #12569, 13460, 15662, and 15322 - untriggered ToO). These programs are focused on the strong outflows and gaseous environments of low-redshift PG quasars and ULIRGs, and have already led to 22 refereed papers, including two first-authored by Veilleux. Two other papers from these programs are nearing submission to refereed journals.
Mr. Weizhe Liu is an astronomy graduate student at the University of Maryland who is doing his PhD thesis under the supervision of PI Veilleux. His PhD thesis is on galactic outflow-related science: he has so far first-authored two papers on (1) the metal-enriched X-ray emitting gaseous halo of Mrk 273, a nearby ultraluminous infrared galaxy, and (2) the properties of AGN-driven outflows in 8 dwarf galaxies based on Gemini and Keck integral field spectroscopic data. He is leading the analysis of the COS data from program #15662. He is also the PI of a recent COS program (PID #15915) to study a subset of 3 of the 8 above dwarf galaxies with the fastest AGN outflows. He has analyzed all of the data from #15662 and all of the existing data from #15915 so far, and developed tools for the detection and characterization of galactic outflows from UV spectroscopy in the process.
Dr. Ben McKinley is a Research Fellow at the Curtin Institute of Radio Astronomy in Australia. He is the first author of a paper, recently submitted to Nature Astronomy, that describes the results from the analysis of the new MWA 185 MHz data of Cen A shown in Figures 2 and 3 of this proposal. His expertise is on the radio-mode feedback of Cen A. He first-authored a comprehensive paper on the jet/wind outflow in Cen A in 2018.Supermassive Black Holes and Active GalaxiesIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQUASARNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000GALEX FUV 18.75 mag (integrated)GALAXYQUASARSEYFERTYESThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000GALEX FUV 19.81 mag. (integrated)GALAXYQUASARSEYFERTNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000GALEX FUV 19.11 mag. (integrated)GALAXYBL LACQUASARNOThis object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000GALEX FUV 18.97 mag. (integrated)COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.165595513400096.99243865111839(Tic-Visit
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