0Assigned ID: 4066
----- Attempting Submission 1 (Tue May 23 02:29:02 GMT 2023) -----
HST Phase I Proposal 4066 successfully submitted.
Receipt: # 4066-1
----- Attempting Submission 2 (Tue May 23 05:01:34 GMT 2023) -----
HST Phase I Proposal 4066 successfully submitted.
Receipt: # 4066-2
----- Attempting Submission 3 (Wed May 24 16:00:05 GMT 2023) -----POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.Repeat of Exposure ID IF7Y02010 corresponding to visit 02. The visit no corresponding to repeat observation is 52. Observations of three sub-exposures taken with Filter F673N are to be repeated.-1301837968----- Attempting Submission 1 (Sat Sep 09 22:58:17 GMT 2023) -----
----- Attempting Submission 2 (Fri May 31 01:12:55 GMT 2024) -----This is a repeat obseravation (visit to be repeated is 52). These warning messages were shown in the past APT submission as well and my program coordinator gave me a go ahead.Dissecting Red geyser winds: low luminosity AGNs with large scale outflows in the ionized phaseSpatially resolved optical spectroscopy from ground-based SDSS-MaNGA survey has recently discovered a new class of early-type galaxies - known as red geysers, that show signatures of large-scale active galactic nuclei (AGN) driven winds in the ionized gas phase. These are exciting candidates for black hole feedback driven by radiatively inefficient AGNs in quiescent galaxies. However, MaNGA's spatial resolution is relatively low (1-2 kpc), and is thus insufficient to probe the ionized winds close to the vicinity of the AGN. We propose a small program of 5 orbits to observe the ionized gas in a prototypical red geyser that is interacting with a companion galaxy using a combination of narrowband filters of the HST WFC3/UVIS instrument. This HST observation will be complemented by a large set of existing datasets from SDSS-MaNGA, Gemini GMOS, LOFAR (radio), and Keck ESI. Using HST, we will obtain an order-of-magnitude increase in the spatial resolution of ionized gas, traced by H-alpha, [OIII], [NII], and H-beta emission lines, using four narrowband filters. Our study will open a new window for studying low luminosity AGN-driven winds in early-type galaxies. We will be able to exploit the extremely high angular resolution of HST to probe length scales down to a few tens of pc zooming in close to the black hole, which is impossible to resolve using ground-based observations. The simultaneously large field of view will help us capture the complete picture of this fascinating interacting galaxy with winds. This study will serve as a pilot study on the red geyser sample, which will be supplemented in the future with additional objects with diverse characteristics.## Our target ###
Tha main science goal of our proposal is to study outflowing ionized winds in a nearby (z = 0.0245) quiescent (Early type) galaxy called "red geyser". This galaxy hosts a Low luminosity AGN and shows large scale biconical outflows with ground-based IFU data from MaNGA survey. Using HST narrowband filters, we will be able to spatially resolve the outflow near the center with a resolution of 0.1'' or equivalent.
### choice of filters ######
We are proposing to observe a red geyser at z=0.0245 using WFC3-UVIS narrow-band and
broadband imaging. We will use 4 NB filters FQ672N, F673N, FQ508N, and FQ492N which are uniquely suited to capture Ha, [NII], [OIII]5007, and Hb nebular emission lines at the redshift of our source. While FQ672N, FQ508N, and FQ492N quad filters suitably cover the wavelength range around the Ha, [OIII]5007 and Hbeta emission lines for our red geyser target, the F673N filter cover both Ha and [NII]6584. We will subtract the Ha (obtained from FQ672N) from the Ha+[NII]
(obtained from F673N) to get the pure [NII] image.
The emission lines will trace the ionized gas properties. The filters are chosen such that the NB filters have bandpasses that span the range of velocities we expect to observe in the lines. Among those 4 filters, the three quad Filters FQ672N, FQ508N, and FQ492N will be placed centered on the red geyser. But filter F673N has a larger field of view and will be placed enclosing both the red geyser and its companion galaxy. So, it will be placed at the optimal position between the red geyser and the companion galaxy. We will use broadband filters F775W and F475W to detect the stellar continuum that will enable continuum subtraction from emission line measurements.
## exposure time #######
We want to observe the ionized gas in the nuclear region of our target with a sufficient angular resolution of 0.1'' while simultaneously catching the low surface brightness emission in the outskirts at a radial distance > 5 kpc. Hence, to compute the exposure time, we aim for an emission line detection per resolution element with a minimum signal to noise of 3 at a ~5 kpc radial distance from the center. We estimate exposure times based on existing integral
field spectroscopy from MaNGA data. Based on MaNGA data, the average Ha (integrated line) flux from our target
within an aperture of diameter 3'' at a radial distance of 4 kpc from the center is 8*10^-16
ergs/s/cm2/arcsec2.
Using the ETC, we find that the exposure time needed
to detect a single Ha line within an extraction aperture of 0.1'' at a radial distance of 5 kpc using WFC3 at an S/N
~3 is 43 minutes. This will give us S/N > 12 per pixel within the central 2 kpc * 2kpc region. To increase the S/N ratio for regions with inadequate flux,
particularly towards the outskirts, we will adopt optimal Voronoi binning.
We request 3 exposures / dithers for each narrowband filter for robust cosmic-ray removal. Including overheads, this amount to 1 orbit being requested per narrowband filter. Additionally, We will split 1 orbit between the two broadband filters. For the 2 broadband filters, we will use a 2-point dither pattern.Thus, This gives a total of 5 orbits for the complete set of narrow- and wide-band images for our red geyser.
Reduction of gyros will have no effect on our program.The proposal team has substantial technical experience
in imaging and emission line analyses. The team consists of leading scientific
experts in outflows and AGNs. Prof. Kevin Bundy and Dr. Namrata Roy carried out the primary analysis of MaNGA IFU data in the discovery and characterization of the red geysers. They carried out the LOFAR radio analyses, initial emission line kinematic analyses from existing MaNGA and Keck ESI data and constructed a toy wind model to compare to the data. Prof. Timothy Heckman is a foremost expert in winds and outflow, kinematics and emission line modeling and has been a collaborator in the red geyser projects. Dr. Alaina Henry is an expert in space based observations and galaxy formation. Dr. Xinfeng Xu has extensive experience in studying galactic outflows and their feedback effects, and has tremedous expertise in using HST data. He has worked broadly on quasar outflows specifically from HST/COS datasets.Supermassive Black Holes and Active GalaxiesGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYELLIPTICALINTERACTING GALAXYLINERWINDYESJ2000J2000u = 17.04, g = 15.12, r = 14.17, i = 13.67, z = 13.37GALAXYELLIPTICALINTERACTING GALAXYLINERTIDAL TAILWINDYESJ2000u = 17.04, g = 15.12, r = 14.17, i = 13.67, z = 13.37WFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoFQ672NWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoFQ492NWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF475WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falsePOS-TARGDITHER0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE2falseThe scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.1709037437000140.96818564354987(Tic-Visit
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