For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 5447
----- Attempting Submission 1 (Tue Mar 26 15:26:24 GMT 2024) -----
HST Phase I Proposal 5447 successfully submitted.
Receipt: # 5447-1"Proposals can be submitted with the warning present."0----- Attempting Submission 1 (Fri Jul 26 14:54:10 GMT 2024) -----Target has been confirmed using the images saved from the confirmation tool.The largest BAL acceleration: testing disk wind modelsQuasar outflows are invoked as the major agent of AGN feedback and are crucial for the mass inflow/outflow balance in the vicinity of super massive black holes. Significant effort was invested over the past 3 decades in creating theoretical models for the formation and acceleration of these outflows. However, there is no decisive empirical test that confirms or refutes such models. These models have specific predictions for an outflow found in its acceleration phase. Recently, an outflow with the largest acceleration ever detected was found, and it is the ideal candidate to test acceleration models. Previous HST observations in 2011 and 2017 showed that the outflow's velocity shifted by -1550 km/s (the largest shift observed to date). Any one episode of acceleration can be accommodated by a disk-wind model solution. However, that solution predicts specific acceleration and distance values for future times and thus can be tested.
We propose a 3rd epoch of observations, which will yield both the velocity and distance from the central source for the outflow. Thus, we will obtain a full empirical test for the acceleration models, and more generally, an unprecedented observational study of a broad absorption line outflow acceleration.To accurately determine the outflow distance to the central source (R), a minimal spectral resolution of 5000 is needed as well as high throughput. Therefore, the use of COS G130M and G160M is necessary.
The photoionization solution (PIS) derived from the 2017 epoch and the corresponding electron number denity (n_e) (and therefore R) are loosely constrained. The PIS can be better constrained if we can measure the ionic column densities (N_ion) for both O IV and Na IX, as compared with the current upper limits. Our simulations for a range of S/N show that to obtain a meaningful constraint on the M95 acceleration model, a S/N of 30 per a R = 5000 resolution element is required. Using the COS ETC, we determine that the desired S/N can be obtained in 7 ks and 13 ks for the G130M and G160M gratings, respectively. Taking into account the overheads, this translates to a total of 11 orbits.
In selecting our grating settings, we have chosen central wavelengths to avoid placing the gap between the COS detectors on any of the crucial spectral features we will use in our analysis. For ETC calculations we use the FOS-based QSO composite spectrum at the redshift of the object with a foreground E(B-V) as given by NED. Since the object has been observed safely with COS before, there are no bright object concerns for our observations. To plan our observations, we use ETC calculations that are conservative (both fainter and brighter) to ensure success. W e plan target acquisition exposure times for minimum flux that is 3x lower than the observed flux, and set BUFFER-TIME for flux 3x brighter, and use the factor of 2/3 recommended by the ETC. In practice, all BUFFER times from the ETC are >4000 secs, so, to optimize buffer useage and minimize overheads, we generally choose BUFFER-TIME such that BUFFER-TIME=ExposureTime - 110 s.PI Dr. Arav published several refereed papers on analyzing COS data of quasar outflows, including on a similar quasar outflow: Arav et al. 2020, APJS 247:37 HST/COS Observations of Quasar Outflows in the 500A-1050A Rest Frame. I. The Most Energetic Outflows in the Universe and Other Discoveries
The Co-I team has substantial expertise in both the data and science of this proposal:
Dr Jerry Kriss: An expert on COS data and in the analysis of AGN outflows based on COS data.
Dr. Korista is an AGN expert, with several publications on quasar and Seyfert outflows involving HST UV spectral observations.
Dr. Xinfeng Xu, has published, three papers from HST GO-14777, which targeted similar quasar outflows with COS observations, including Xu et al., 2020a,b.
Dr Dehghanian is an expert on Cloudy photoionization simulations, which are vital for this project.Supermassive Black Holes and Active Galaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYNUCLEUSQSOWINDNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J20001.3e-15 at 1516 ACOS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.(Tic-Visit
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