0Assigned ID: 5327
----- Attempting Submission 1 (Tue Mar 26 04:19:28 GMT 2024) -----
HST Phase I Proposal 5327 successfully submitted.
Receipt: # 5327-1
----- Attempting Submission 2 (Tue Mar 26 20:31:49 GMT 2024) -----
HST Phase I Proposal 5327 successfully submitted.
Receipt: # 5327-2
----- Attempting Submission 3 (Tue Mar 26 23:22:35 GMT 2024) -----POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.Use POS TARG to move the slit along the long-slit for each orbit.2017347909----- Attempting Submission 1 (Fri Aug 16 04:25:23 GMT 2024) -----
HST Phase II Proposal 17758 successfully submitted.
Receipt: # 17758-1
----- Attempting Submission 2 (Tue Aug 27 19:10:44 GMT 2024) -----
----- Attempting Submission 3 (Wed Apr 16 23:48:57 GMT 2025) -----
HST Phase II Proposal 17758 successfully submitted.
Receipt: # 17758-3
----- Attempting Submission 4 (Tue Apr 22 18:46:56 GMT 2025) -----Could you help me check the POS TARG set ups for the F505N_1 and F505N_2 exposures? My aim is to make some dithers both good and small enough for the ramp filter observations. I didn't find enough information from the instrument handbook.Radio Jet-driven AGN Feedback in Dwarf Galaxies: A Pilot StudyIt is still under debate whether stellar feedback can effectively shape the evolution of dwarf galaxies as expected. 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, energetic outflows have been discovered in some dwarf galaxies with AGN, which can provide feedback to their dwarf hosts. In addition to such outflow-driven feedback, radio jet-driven feedback is the other one of the two fundamental forms of AGN feedback. Radio jet is also deemed an important mechanism for the launch of some powerful outflows. A close examination of the radio jet-related feedback is essential for a more comprehensive understanding of AGN feedback in dwarf galaxies. So here we propose to map the [O III]-emitting gas and examine radio jet-driven feedback and its relation to the rapid outflow in a dwarf galaxy with the most extended radio jet known in such systems, using high spatial resolution (~50 pc) ACS imaging and STIS long-slit spectroscopy. Our main objectives are: (1) characterize the role of the radio jet in driving the outflow; (2) examine the interaction between the radio jet and the interstellar medium; (3) obtain the dynamics of the outflow; (4) evaluate the overall impact from the radio jet and the outflow on the evolution of dwarf galaxies.Imaging: We will obtain a high-S/N ACS/WFC FR505N narrow band image for [O iii] 4959,5007 and an ACS/WFC F550M medium band image for the continuum on the red side of the [O iii] line. The FR505N filter is centered on 5150 A to put the redshifted [O iii] doublet in the high throughput window of the filter. The exposure time of the FR505N observation is calculated based on the best-fit [O iii] 4959,5007 doublet model to the Keck/KCWI spectrum extracted from a spaxel 0.5 away from the galaxy center (where the observed radio jet ends). The exposure time of the F550M observation is calculated based on the SDSS spectrum scaled to the flux level of the Keck/KCWI spectrum used above instead, since the Keck/KCWI spectrum does not cover the correct wavelength range. A target S/N of 30 for both observations will be adequate for a good quality [O iii] emission line-only map. The final exposure time requested are 2435 s and 635 s, respectively, and the two observations will be obtained in the same orbit.
Spectroscopy: We will also carry out STIS/G430M (4950-5236 A) and STIS/G750M (6482-7054 A) long-slit spectroscopy along the radio jet (see Fig. 3 of proposal for a sketch). The gratings are chosen to ensure a good spectral resolution (FWHM ~50 km/s) to fully resolve the emission line profiles (with overall FWHM of 100-200 km/s). The slit size is chosen to be 52'' X 0.2'', with the slit width comparable to the radio jet. The slit will be centered on the flux peak of the VLA continuum image.
The exposure time is calculated based on the same Keck/KCWI spectrum 0.5'' away from the galaxy center and the SDSS spectrum scaled to the flux level of the Keck/KCWI spectrum for the G430M and G750M gratings, respectively. Based on our experience, the target S/N are ~4 per spatial pixel per spectral resolution element at the observed wavelength of Hbeta and [O i] 6300 emission line for the two gratings, respectively. The Hbeta and [O i] 6300 are the faintest lines we aim to observe in each grating, and the requested ex- posure time will thus allow for robust detections and decomposition of all optical emission lines required to fulfill our science goals. A spatial binning of 1 is chosen to keep the finest spatial resolution. The final exposure time requested is ~9620s (or 3 orbits adopting anorbital visibility of 55 min) for each grating.
Target Acquisition: for the spectroscopy, we will use the standard STIS ACQ method
for an extended source with aperture F28X50LP, Gain=4, frame=1 and a spectrum template of Seyfert 2 NGC 1068 scaled to the r-band surface brightness of our target, 17.1 mag. arcsec^-2.University of Arizona postdoc Dr. Weizhe Liu has been working on AGN feedback-related science since his
PhD thesis and has first-authored a paper in 2020 focused on the AGN-driven outflows in a sample of dwarf
galaxies where the target of this proposal is chosen. He is the P.I. of the cycle 27 program "AGN Feedback in
Dwarf Galaxies" with HST/COS (PID #15915) and Co.I. of two other recent HST programs (PID
#15662,16698). The FUV spectroscopy data have revealed the absorption line-traced fast outflows in the three
dwarf AGN (including the target in this proposal). This result adds new evidence of AGN feedback in dwarf galaxies and the paper will be submitted before this July.
Prof. Sylvain Veilleux is one of the foremost authorities in the field of AGN feedback and galactic outflows. He
has been the P.I. of six recent HST programs adopting ACS, STIS and COS (PID #13460, 12569, 12570,
15662, 16698, 15322 - untriggered ToO). These programs are focused on the strong outflows and gaseous
environments of low-redshift PG quasars and ULIRGs, as well as the radio mode AGN feedback, which have
already led to 22 refereed papers, including three first-authored by Veilleux.
Prof. David Rupke is an experienced expert in the studies of galactic outflows with multi-wavelength data, and
he is the P.I. of two recent HST programs: the HST/STIS NUV spectroscopy observation of the galactic wind in
a local ULIRG (PID #14184) and the STIS observation of emission from the circumgalactic medium of the
galaxy with a 100-kpc scale galactic wind (PID #16231).
Prof. Gabriela Canalizo has led the optical Keck long-slit and integral field spectroscopy that has led to the
discovery of the AGN winds in these dwarf galaxies.
Prof. Richard Mushotzky is a well-known expert on AGN physics and has extensive experience with multi-
wavelength data of nearby AGN. He will help with the interpretaion of the proposed HST data, together with the archival multi-wavelength data of the target.
Dr. Thomas Bohn and Ms. Archana Aravindan have both been working on the long-slit spectroscopy and IFS
data of these dwarf galaxies, and have published papers on the AGN-driven outflows in these sources based on
those data. Dr. Huan Li also has extensive expereince with AGN spectroscopy.GalaxiesSupermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ACS/WFCImagingNoNoF550MACS/WFCRampFilterNoNoFR505NSTIS/CCDSpectroscopicNoNoG430M5093STIS/CCDSpectroscopicNoNoG750M6768POS-TARGDITHER0.145LINEfalsefalse285.29ACS-WFC-DITHER-LINE5falseThe scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode./Users/weizheliu/HST_dwarf_ACS_STIS/cycle32/phase2/OP-cache/J0954_cycle32_phase2_250422-v01.xml(Tic-Visit
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