0Assigned ID: 5595
----- Attempting Submission 1 (Tue Mar 26 19:56:02 GMT 2024) -----
HST Phase I Proposal 5595 successfully submitted.
Receipt: # 5595-1
----- Attempting Submission 2 (Tue Mar 26 22:51:13 GMT 2024) -----I am resubmitting this Phase II proposal to include Visit 06, which is a partial repeat of Visit 02 following a guide star reacquisition failure.-796984623----- Attempting Submission 1 (Fri Aug 16 16:53:32 GMT 2024) -----
----- Attempting Submission 2 (Fri Oct 18 20:46:24 GMT 2024) -----
----- Attempting Submission 3 (Mon Jan 13 22:18:23 GMT 2025) -----Resolving the Origins of Extraplanar Dust using UV Reflection NebulaeDusty outflows from star-forming regions trace the circulation of mass and metals between galaxy disks and their gaseous environments. As much as half of the dust in the local universe may be found outside of galaxy disks, but we do not know what physical mechanisms dominate the dust transport. The morphology of the extraplanar dust is a key indicator of dust transport by ejective feedback through galactic chimneys (clumpy/filamentary) or by radiation pressure (smooth). However, the dust morphology is unknown at distances of more than a kiloparsec from the disks of normal, star-forming galaxies. At these distances, UV light scattered by dust grains provides a powerful tool for detecting the dust, but these reflection nebulae are unresolved by GALEX and Swift observations. We propose to resolve these nebulae using HST/WFC3 F225W imaging of six nearby, normal ~L* galaxies (five new observations, one archival). These observations will determine whether ejective feedback or radiation pressure dominates the dust transport out of galaxy disks with and without active chimney-mode feedback, as seen in H-alpha images. This pilot program will also enable efficient and precise measurements of the metal mass found in the expelled dust in a future program. These objectives are essential for understanding the physical processes that regulate star formation by coupling the mass and metal reservoirs of the interstellar and circumgalactic media.Scientific goals: This program will study ejective and radiative stellar feedback in star-forming disk galaxies by measuring the morphology of extraplanar dust detected via scattered UV light. If ejective feedback dominates the dust transport out of galaxy disks, then the extraplanar dust morphology is expected to be clumpy. In contrast, if radiative feedback is important, then the morphology will be smoother. Our observing strategy is therefore designed to detect scattered light from dust on scales as small as l = 100 pc at the disk-halo interfaces of five nearby (D = 10 - 20 Mpc), edge-on disk galaxies. These obseravtions will also inform the best strategy for obtaining accurate measurements of the total extraplanar dust mass in future observing programs.
Observing strategy: We use WFC3-UVIS and the F225W filter to image extraplanar dust via scattered near-UV light in high SNR images. Our exposure times are chosen to detect extraplanar dust in regions of size l = 100 pc (1" - 2", or 25 - 50 pixels) at z = 3 kpc with SNR = 3, if the dust is smooth. The choice of z = 3 kpc is based on the typical extent of extraplanar reflection nebulae, and we use GALEX/NUV images to determine the typical NUV surface brightnesses of the sample galaxies at these distances from the disk. If the dust is clumpy instead of smooth, we will achieve a higher SNR in the clumps, and we will enlarge the aperture as needed to achieve significant detections of any residual, diffuse emission. The exposure time requirements result in two orbits allocated to each of the five galaxies for a total of ten orbits.
We center the WFC3-UVIS pointings on the galaxy centers, where the NUV halos tend to be brightest, to optimize the SNR. The WFC3-UVIS FOV spans 8 - 18 kpc at the distances of the sample galaxies, allowing the extraplanar NUV surface brightness profile to be measured within at least twice the characteristic scale height of the NUV nebulae (typically a few kiloparsecs). We use the two-point WFC3-UVIS-GAP-LINE pattern to fill in the chip gap and remove cosmic rays and detector artifacts. As the scales that we aim to resolve (~ 1") are larger than the PSF, we do not dither further to resample the PSF. We employ a post-flash of 9 or 10 e- to mitigate CTE effects in the faint regions of the images. We thus obtain two full-orbit exposures for each galaxy, which optimizes the SNR of faint extraplanar structures.The proposed program will obtain HST/WFC3 F225W imaging to perform a morphological study of ultraviolet reflection nebulae from extraplanar dust in six nearby, edge-on disk galaxies. The WFC3 F225W images will be analyzed in conjunction with archival H-alpha images to determine the relationship between the dust and the warm ionized gas in galactic fountain flows. Investigators Boettcher and Hodges-Kluck are experts in the study of extraplanar dust via UV reflection nebulae in nearby galaxies and in multi-wavelength observations of star-formation feedback.
PI Boettcher has extensive experience in the analysis of UV imaging data of extraplanar reflection nebulae from GALEX. She is also an expert in the study of extraplanar gas in nearby galaxies, including the analysis of H-alpha observations to study ejective feedback and galactic fountains in star-forming disks.
Co-I Hodges-Kluck is a leading expert in the study of UV reflection nebulae and cirumgalactic dust with GALEX and Swift observations. He also has expertise in multi-wavelength observations of the interstellar and circumgalactic medium for the study of star-formation driven outflows.
The team will combine their multi-wavelength expertise to maximize the scientific output of the proposed UV and archival optical imaging.Intergalactic Medium and the Circumgalactic MediumGalaxies6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYSPIRALThis object was generated by the targetselector and retrieved from the NED database.J2000J2000SURF-NUV-AB = 25.3 mag/sqarcGALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000SURF-NUV-AB = 25.5 mag/sqarcGALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mu_NUV_AB = 24.5 mag/sqarcGALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mu_NUV_AB = 25.6 mag/sqarcGALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000mu_NUV_AB = 25.3 mag/sqarcWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF225WPOS-TARGMOSAICDITHER42.414WFC3-UVIS-DITHER-BOXfalse81.785true0.1120.173285.759POS-TARGWFC3-UVIS-GAP-LINE23.8841falseThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.A bright star within the FOV (RA = 188.20335d, dec = 0.12584d; V ~ 10.9 mag) may produce figure-8 ghosts in quadrant A if it falls on quadrant D. We restrict the ORIENT to ensure that the star does not fall on quadrant D.(Tic-Visit
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