First resubmission2122448207Assigned ID: 4027
----- Attempting Submission 1 (Mon May 22 13:57:44 GMT 2023) -----
HST Phase I Proposal 4027 successfully submitted.
Receipt: # 4027-1
----- Attempting Submission 2 (Mon May 22 14:09:14 GMT 2023) -----
HST Phase I Proposal 4027 successfully submitted.
Receipt: # 4027-2Revised per suggestions by Debopam Som.1600017456----- Attempting Submission 1 (Mon Aug 28 19:07:42 GMT 2023) -----
HST Phase II Proposal 17542 successfully submitted.
Receipt: # 17542-1
----- Attempting Submission 2 (Mon Aug 28 19:17:43 GMT 2023) -----
HST Phase II Proposal 17542 successfully submitted.
Receipt: # 17542-2
----- Attempting Submission 3 (Tue Aug 29 14:36:38 GMT 2023) -----
----- Attempting Submission 4 (Thu Jul 11 16:17:04 GMT 2024) -----Emission-Line Imaging of the M 82 Wind: Moving from Phenomenology to PhysicsGalactic winds play an essential role in the evolution of galaxies and the IGM. Despite an abundance of data and improving simulations, deep mysteries remain. The most widely-used probes of winds are UV and optical data that measure outflows of warm ionizied gas. However, we still do not understand how this gas is created, heated, and accelerated. Such understanding is required to use these probes to elucidate the underlying physics of galactic winds. More specifically, the emission from this gas may dominate the radiative cooling of the wind, draining away kinetic energy, and hence determining the wind's dynamical evolution and large-scale impact.
This is a proposal to obtain a set of narrow-band images tracing four different emission-lines in the warm-ionized gas in the proto-typical wind driven by M 82. With these data, we can map out key diagnostic line ratios on scales as small as a pc, where complex structures dominate the exisiting HST image of the emission. This will make it possible to fully disentangle the relative contibutions of collisional ionization (which drains energy from the wind) vs. photoionization by the light leaking out from the starburst. The data will also allow us to test competing models for the origin and acceleration of warm ionized gas in M82 and galactic winds in general.
We will compare these data to new JWST images of the M 82 wind, to state-off-the art high-resolution numerical simulations, and to exisiting IFU optical spectra. By addressing the key questions on the origin, heating, and acceleration of the warm ionized gas, we will move our understanding of galactic winds along the path from phenomenology to physics.Our science goal is to use narrow-band images of the southern portion of the M 82 outflow to daignose the physical processes responsible for creating and acceleraing the emission-line clouds. We will take narrow-band images of [OIII]5007, H-alpha, and [SII]6717,6731. The new H-alpha image will be used on its own, and will also be used in conjunction with the existing ACS H-alpha+[NII]6548,6584 image to create a pure [NII] image. We will also take a broad-band F606W image to subtract stellar continuum emission from the narrow-band images.
Based on ETC, we will need to post-flash by different amounts for each narrow band image to achieve a minimum of 20 counts per pixel (to insure good CTE). We choose not to dither so that the individual exposure times for the narrow-band images fill the orbit. This is to minimize the effects of the post-flash on the S/N ratio. Based on the relative fluxes of the emission-lines, we plan to spend 5 orbits imaging H-alpha, 10 on [SII], 10 on [OIII], and one (CR-SPLIT) with F606W. There will then be enough images for each filer to do cosmic ray rejection.PI - Tim Heckman has spent over three decades developing and utilizing observational diagnostics of galactic winds. He is an experienced HST user.
Co-I: Lee Armus has made seminal observations of galactic winds and has deep expertise in both optical and IR observations of dusty starburst galaxies at low- and high-z. He will lead the comparison of the HST and JWST images of the M 82 wind.
Co-I's Lisa Kewley and Ralph Sutherland have developed and employed a powerful tool-kit for using emission-lines to study starbursts and active galactic nuclei. These models will be used in our analysis.
Co-I's Jeff Rich and Patrick Shopbell have obtained and are analyzing the Palomar CWI IFU spectra that will be compared to the HST images.
Co-I's Brant Robertson and Evan Schneider have developed state-of-the-art high resolution numerical simulations of galactic winds and will augment the existing simulations specifically to compare to our requested data.Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYEMISSION LINE NEBULASTARBURSTYESJ2000J2000WFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF673NWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF775WHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.(Tic-Visit
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