prop_v5.pdf381658463Assigned ID: 4126
----- Attempting Submission 1 (Tue May 23 17:03:21 GMT 2023) -----
HST Phase I Proposal 4126 successfully submitted.
Receipt: # 4126-1
----- Attempting Submission 2 (Wed May 24 20:13:33 GMT 2023) -----The number of orbits used exceeds the number allocatedv1: The current observing strategy is to have two exposures per orbit to allow us to fill the WFC3/UVIS detector gap and remove crays, hot pixels, etc, using Pattern Type = WFC3-UVIS-GAP-LINE. I am not certain that this is the best strategy since the 4-orbit visits result in 8 separate exposures. A possibly better strategy for these 4-orbit visits is to instead have a single exposure per orbit to get higher S/N while changing the coordinates of the "target" by ~3-4" between each orbit to fill the detector gap, dither, remove crays, hot pixels, etc. One potential problem with this latter strategy is that the direction of the shifts may not be optimized to fill the detector gap. Your advice would be most welcome here!
v2: The one-orbit visits are now split into three exposures instead of two to better remove artifacts, using pattern type = WFC3-UVIS-DITHER-LINE-3PT, center pattern clicked, PA = 84.759 deg, and shift of 2.414" to cover the detector gap. The proposal description was changed accordingly.
v1: I also would like to make sure that my constraints on ORIENT are correct: does "min=324 deg and max = 24 deg" indeed mean that ORIENT can only be between 324-360 deg or 0-24 deg. Please confirm.
v2: Confirmed. No change.
v3: The position of target #9, NGC 4666, was shifted by ~19" to the E and ~19" to the S to find guide stars.
v4: Following the advice of Dr. Joel Green @ STScI, we have excluded Orients ~ 240's deg for visit #5, target #5, NGC 1569, "to avoid a bright star that could cause figure-8 anomalies if it lands in Quadrant D."
v6: Visit #4 partially failed. Created new visit #11 to redo observations #1 and #5 (which had star trails). Observations #2, 3, 4 were judged ok by STScI so were not redone.
v7: Visit #55 partially failed. Created new visit #60 to redo three of the four F225W observations (#1, 2, and 3), and the F336W observations (the old obs #5 now obs #4), using a total of four orbits instead of the original five.
This is a second attempt at submitted v7.
v8: Visit #60 partially failed. Created new visit #62 to redo three of the four F225W observations. The PA constraints were also relaxed by 5-10 degrees.203194157----- Attempting Submission 1 (Thu Sep 07 20:05:32 GMT 2023) -----
HST Phase II Proposal 17535 successfully submitted.
Receipt: # 17535-1
----- Attempting Submission 2 (Mon Sep 11 14:52:02 GMT 2023) -----
HST Phase II Proposal 17535 successfully submitted.
Receipt: # 17535-2
----- Attempting Submission 3 (Mon Sep 11 20:17:43 GMT 2023) -----
----- Attempting Submission 4 (Fri Oct 20 13:30:08 GMT 2023) -----
----- Attempting Submission 5 (Wed Oct 02 14:02:39 GMT 2024) -----
----- Attempting Submission 6 (Mon Apr 28 18:17:43 GMT 2025) -----
----- Attempting Submission 7 (Thu Jan 08 20:46:06 GMT 2026) -----I was advised by Dr. Alison Vick to submit this revised phase II file despite these warnings/problems.Dust in Galactic Winds and Fountains: A Near-UV Survey of Nearby Highly Inclined Starburst and Active Disk GalaxiesThe amount of dust outside of galaxies, inferred from reddening measurements of background quasars and galaxies by foreground galaxy halos, is comparable to that within galaxies. The recent discoveries of dusty winds driven by stellar or SMBH processes that extend on 100-kpc scales suggest that winds are one source, and possibly the main source, of the enriched circumgalactic medium (CGM), although the processes by which the dust is launched, entrained, and possibly altered in these winds remain uncertain. This is due to the fact that the angular resolution (5") of present-day observations is insufficient to extract the dust signal at the base of the wind against the bright galaxy, and allow to pinpoint where the dust lies relative to the cool, warm, and hot gas phases of the winds. We propose to map, for the first time on sub-arcsecond scale (<10-100 pc), the ultraviolet light reflected off of extraplanar dust in 10 nearby highly inclined disk galaxies with well-known galactic winds or fountains, spanning a range in stellar masses, energy sources (stellar or AGN), and dust erosion processes (shocks, stellar or AGN photoionization). The dust maps, derived from deep WFC3 F225W and F336W images, will be compared with existing sub-arcsecond maps and velocity fields of the ionized gas to determine the mechanisms by which the dust is launched and carried into the halos of these galaxies, and whether the dust experiences any evolution on its journey to the halos. The <10-100 pc resolution is critical since the processes that can alter or even destroy the dust and the clouds in which it resides operate on such scales. The results will inform future modeling and IR observations.A total of 44 orbits is used, split between the WFC3/F225W observations (34 orbits) and WFC3/F336W observations (10 orbits). The observations are relatively straightforward. All of the objects, except M82, are centered within the WFC3 FOV. To take full advantage of the WFC3 FOV, each object is observed at a specific position angle (PA) such that the major or minor axis of the host galaxy aligns with the sides of the WFC3 format. The exposures are divided into two or three shorter sub-exposures per orbit to allow to remove cosmic rays, hot pixels, and other detector blemishes, improve sampling for the astrometric solution, improve photometric accuracy by averaging flat-field errors, and bridge the gap between the two chips. A post flash is used for both the F225W and F336W observations to avoid charge traps.
The observational goal of this program is to reach a limiting (S/N = 3) surface brightness (SB) in the F225W band within the region where the GALEX NUV SB is at least 27 mag AB arcsec. The SB limit of the F225W observation is chosen to allow us to trace the full extent of the dusty wind in each object, beyond the galactic disks, based on the GALEX NUV images. There are two exceptions: M82 and NGC 253. In M82, the one-orbit F225W observation reaches a limiting (S/N ~ 3) SB of ~ 25.7 mag AB arcsec-2. Moreover, it is centered on the UV-brighter southern cone rather than the nucleus to allow us to study the dust out to ~ 3 kpc from the nucleus. The F225W observation of NGC 253 is centered on the nucleus but is otherwise the same as that of M82: three exposures within one orbit (~2800 sec in total) with WFC3/F225W, reaching a GALEX NUV band SB limit of 25.7 mag AB arcsec-2. A post flash of 17 e- is needed for both M82 and NGC 253 according to the WFC3 ETC (WFC3UVIS.im.1852753). For the other 8 objects in the sample, a limiting SB in the GALEX NUV band of 27 mag AB arcsec-2 is reached in ~12,000 seconds split in 8 exposures over four orbits, when observing with the F225W filter, according to the WFC3 ETC (WFC3UVIS.im.1889384). A post flash of 14 e- is needed to avoid charge traps. For all these calculations, we use a circular aperture with radius of 0.5-0.6" and assume that the UV scattered light has a flat flambda spectral energy distribution (the results are insensitive to this assumption). 34 orbits are needed to observe 10 objects.
The SB limit of the F336W observations is chosen to make sure that these images reliably remove the direct stellar light in the F225W image. It is therefore important to choose a SB limit that captures the faint stellar light from the disk. A quantitative inspection of the GALEX NUV data indicates that we must have good S/N in the region corresponding to a GALEX NUV SB of ~ 25.3 mag AB arcsec-2. According to the WFC3 ETC, a GALEX NUV SB limit of 25.3 mag AB arcsec-2 is reached within one orbit if the F336W observation is split into three exposures to deal with the cosmic rays and allow for dithering (WFC3UVIS.im.1852745). A post flash of 16 e- is needed to avoid charge traps.Prof. Sylvain Veilleux (U. of Maryland) studies active and starburst galaxies, near and far, and their impact on the environment. He has recently published a comprehensive review on cool dusty outflows and their implications, which is directly relevant to the present proposal. He has extensive experience with the analysis and interpretation of UV, visible, and infrared images and 1D/2D spectra obtained with HST, Spitzer, Herschel, JWST, and ground-based telescopes of the galaxies in the present sample. He is a co-I on cycle 1 JWST program ID #1701 (PI Bolatto) to image M82 and NGC 253 with NIRCam and MIRI. These data will be compared with the HST data on these objects.
Dr. Edmund Hodges-Kluck (NASA Goddard Space Flight Center) studies nearby galaxies, including the Milky Way, their circumgalactic medium, and galaxy ecosystems in general. He is highly experienced with the analysis of X-ray and UV imaging and spectroscopic data. He has first-authored a number of papers on extraplanar dust in nearby galaxies based on GALEX and Swift UVOT data. The present proposal builds on the success of these papers to study the extraplanar dust at higher resolution. He produced Monte Carlo Radiative Transfer (MCRT) scattering models to analyze the GALEX data; his code will be adapted to analyze the HST data.GalaxiesSupermassive Black Holes and Active Galaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database. Slight shifts of ~18" to the E and S to find guide starsJ2000J2000GALAXYSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WPOS-TARGMOSAICDITHER42.414WFC3-UVIS-DITHER-BOXfalse81.785true0.1120.173285.759POS-TARGWFC3-UVIS-GAP-LINE23.8841falsePOS-TARGDITHER2.414LINEfalsetrue385.759WFC3-UVIS-DITHER-LINE-3PT2falseThe scheduling data was generated by CASM 31.1.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/sherwin/17535/OP-cache/17535-v01.xml1729826155000298.0(Tic-Visit
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