0Assigned ID: 398
----- Attempting Submission 1 (Fri Apr 05 11:15:39 GMT 2019) -----
HST Phase I Proposal 398 (cos-dwarf-190404.apt) successfully submitted.
Receipt: # 398-1
----- Attempting Submission 2 (Fri Apr 05 15:09:36 GMT 2019) -----
HST Phase I Proposal 398 (cos-dwarf-190404.apt) successfully submitted.
Receipt: # 398-2
----- Attempting Submission 3 (Fri Apr 05 19:47:00 GMT 2019) -----
HST Phase I Proposal 398 (cos-dwarf-190404.apt) successfully submitted.
Receipt: # 398-3
----- Attempting Submission 4 (Fri Apr 05 20:33:41 GMT 2019) -----The target acquisition time (exposure 1) of visits 1,2,5,6 are changed from 60s to 120s, and all other exposures are adjusted accordingly.-1738404315----- Attempting Submission 1 (Tue Jul 23 00:28:46 GMT 2019) -----
HST Phase II Proposal 15915 (hst-dwarf-v2.apt) successfully submitted.
Receipt: # 15915-1
----- Attempting Submission 2 (Tue Jul 23 07:14:34 GMT 2019) -----
----- Attempting Submission 4 (Fri Jan 24 17:29:31 GMT 2020) -----AGN Feedback in Dwarf GalaxiesFeedback processes play a vital role in the evolution of dwarf galaxies. While the stellar processes are believed to be the dominant source of feedback in dwarf galaxies, it is still under debate whether stellar feedback can reproduce all the properties of the dwarf galaxies we see today. There is growing evidence, both observational and theoretical, that feedback from active galactic nuclei (AGN) may also contribute to the evolution of dwarf galaxies. Indeed, recent Keck optical observations have revealed large-scale (reaching beyond the half-light radii) and fast (broad [OIII] linewidths up to 2000 km/s) outflows in a sample of dwarf galaxies with AGN. Remarkably, only one dwarf galaxy with an AGN (NGC 4395) has been examined so far in the rest-frame far-ultraviolet (FUV). So here we propose to conduct COS/FUV spectroscopy on the three dwarf galaxies with the fastest AGN outflows based on the optical data. The FUV band is rich in spectroscopic diagnostics of the neutral, low-ionization, and high-ionization gas phases. COS will thus allow us to quantify the kinematics, column densities, and energetics of all three gas phases at once. These results will be compared with the optical properties of these outflows, as well as with the vast literature on galactic winds in pure star-forming dwarf galaxies, to help us evaluate the impact of AGN feedback on dwarf galaxies and their environments.We were allocated 17 orbits to observe 3 targets with COS G160M with cenwave =1533 A. For each of the two brighter targets, the allocated 5 orbits are split into two visits of 2 orbits and 3 orbits respectively. This follows the recommendation by the Cycle 27 Phase II Proposal Instructions that visits of 2 or 3 orbits are easier for scheduling. For the faintest target, the 7 orbits allocated are split into two visits of 3 orbits and 4 orbits respectively. Splitting the 7 orbits into three visits will significantly increase the overheads and is thus not optimal given the faintness of the target.
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. All of the targets are safe to observe and there is no BOT warning. The exposure times are generous to make sure that S/N > 20.
The spectroscopic exposures are set with different FP-POS values in each orbit to reduce the fixed pattern noise. We get all four FP-POS settings for all targets. 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. High-ionization lines from C IV, Si IV, and weaker low-ionization lines from Si II and C II fit within the wavelength coverage of the data. All of the observation set-ups follow the COS 2025 policy (Table 2.1 of COS Handbook). 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.
To our knowledge, there is no impact from the possible reduced-gyro operations except the scheduling of the observations.University of Maryland graduate student Mr. Weizhe Liu has been working on galactic outflow-related science for three years, and has just first-authored a paper focused on the metal-enriched (most likely through galactic outflows), gaseous halo of Mrk 273. He has re-analyzed the archival HST/COS data of the ``dwarf Seyfert'' NGC 4395 from the HST Spectroscopic Legacy Archive and developed tools for the detection and characterization of galactic outflows from UV spectroscopy. Prof. Sylvain Veilleux is the Ph.D advisor of Mr. Weizhe Liu, and is one of the foremost authorities in the field of AGN feedback and galactic outflows. He has been the P.I. of four recent COS programs (PID #12569, 13460, 15662, 15322 - untriggered ToO). These programs are focused on the strong outflows and gaseous environments of low-redshift PG quasars and ULIRGs, which have already led to 22 refereed papers, including two first-authored by Veilleux. Prof. Todd Tripp is one of the leading experts on the reduction and analysis of COS data. He has led three large HST programs (PID #9184,11741,13846), which have produced 67 refereed papers, including works from other groups that have analyzed the acquired data with assorted (and usually novel) approaches. Prof. Frederick Hamann has made significant contributions to the field of quasar outflows, especially through optical and UV spectroscopy. He has led a paper on the discovery of an exceptional outflow in PG 1411+442 with COS data (PID #12569). Prof. David Rupke is an experienced expert in the studies of galactic outflows with multi-wavelength data, and has carried out an HST/STIS NUV spectroscopy observation of the galactic wind in a local ULIRG (PID #14184). Prof. Gabrila Canalizo and Ms. Christina Manzano-King have carried out the optical Keck long-slit spectroscopy that has led to the discovery of the AGN winds in these dwarf galaxies. They will help with the analysis and interpretation of the HST data.Massive Black Holes And Their Host Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTWINDNOJ2000J2000m(FUV) = 20.01 (AB)GALAXYDWARF COMPACTWINDNOJ2000J2000m(FUV) = 20.47 (AB)GALAXYDWARF COMPACTWINDNOJ2000J2000m(FUV) = 19.94 (AB)COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1533/Users/weizheliu/Box Sync/cos-dwarf/dwarfAGN/cycle27/OP-cache/phaseII_200124-v01.xmlThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.(Tic-Visit
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