0Assigned ID: 5582
----- Attempting Submission 1 (Tue Mar 26 19:33:03 GMT 2024) -----
HST Phase I Proposal 5582 successfully submitted.
Receipt: # 5582-1
----- Attempting Submission 2 (Tue Mar 26 23:00:08 GMT 2024) -----POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.0----- Attempting Submission 1 (Fri Aug 16 10:35:04 GMT 2024) -----We apply a 2-point dither pattern (ACS-WFC-DITHER-LINE) with parameters recommended in the section 7.2 of the
ACS handbook allowing simultaneous elimination of hot pixels and cosmic ray hits in post-observation processing.Mg II maps to reveal how ionizing photons escape local LyC emitting galaxiesUpcoming observations aim to constrain the soures of cosmic reionization, but the high-redshift intergalactic medium precludes direct observations of ionizing photons (or LyC photons). Alternative methods must indirectly estimate the escape of ionizing photons from high redshift galaxies. The extragalactic community has invested vast resources to amass a collective sample of 90 nearby galaxies with ionizing continuum observations. However, these reveal an unsettling fact: while the observed LyC escape fraction correlates with indirect indicators, there is substantial scatter. Indicators cannot infer the escape fraction of individual galaxies. Here, we propose 31 orbits of HST/ACS ramp-filter imaging to determine if geometry drives this scatter. We will map the Mg II, [O II], and [O III] at <250 pc resolution in 5 galaxies with LyC observations and pre-existing seeing-limited ground based IFU. Our targets show compact/unresolved configurations of both neutral and ionized gas, span similar ranges in [OIII]/[OII] line flux ratio and Lyman alpha peak separation, but have a factor of 30 difference in the observed LyC escape fractions (fesc(LyC)~3-90%). The spatial resolution of the IFU data does not probe the location where the LyC is detected and therefore cannot explain such a high factor difference. Higher resolution HST observations must reveal the impact of the HI geometry on LyC leakage. These maps will (1) stringently explore the role of geometry in the escape of LyC, (2) uncover the origin of the scatter in indirect LyC indicators, and (3) guide how JWST can use indirect tracers to infer the LyC escape fraction at high redshift.We propose 31 orbits of HST ACS/WFC imaging with the ramp filters. Our science goals are to spatially map the highly ionized gas (using the [O III] 5007 A emission line), the ionized gas (using the [O II] 3727 A emission line), and the low column density neutral gas (using the Mg II 2800 A resonant emission line) on the r<1" spatial scales. While ground-based observations have provided clues to the geometry of LyC escape, they also demonstrate that much of the important astrophysics happens on spatial scales that are not resolvable from the ground. The exquisite 0.05" (250 pc at the redshift of our sources) resolution of the HST/ACS imaging are crucial to resolving the geometry of LyC escape.
To isolate emission and continuum regions, we will use the tunable narrow and medium ACS ramp filters. These filters are ideal for this science because they isolate narrow wavelength bands (between 70-100 A for the narrow-band filters) with only the desired emission lines. We aim to observe Mg II, [O III] 5007 A, and [O II] 3727 A plus a continuum filter for each line. We will tune the filter to the emission line wavelength and tune the continuum filters to more than 150 A (twice the filter width) from the nebular emission lines and ensure that there are no other strong nebular emission lines within the bandpass. Our three strong leakers already have observations of [O III] 5007, and [O II] 3727 A plus their continuum from the PID 16245 HST program, so only Mg II observations are requested from these sources to probe their small-scales H I neutral gas distributions.
We wish to compare the small-scale gaseous geometry of compact galaxies with different fesc . We selected confirmed LyC leakers from the LzLCS (Flury et al. 2022) and Izotov et al. (2022) observed with the ground-based IFU Keck/KCWI instrument, whose spatial analysis is presented in Leclercq et al. (2024). Our targets are chosen to be compact in Mg II and [O II] (i.e., unresolved, or close to be unresolved in KCWI data), and to have a 30 factor difference in fesc(LyC). We aim at understanding if and how unresolved differences can explain such different escape fractions. Our 5 selected targets are at z > 0.34 and therefore their Mg II is observable with the bluest ACS ramp filter (FR388N). Note that we excluded one target with compact Mg II (r < 1 kpc) because the exposure time requested to map Mg II was too high (>20 orbits).
Our ground-based IFU observations of Mg II and [O II] have seeing of ~1" and cannot inform on the spatial distribution of the gas that allows ionizing photons to escape the galaxy, but they can inform on the estimated flux levels of the two emission lines. We used the available SDSS spectra to determine the [O III] flux levels. Our targets are pure Mg II emitters with total Mg II fluxes ranging from 1.1 to 3.5x10^{-16} erg/s/cm^2. Using the ACS ramp filter ETC, the FR388N filter tuned to a center wavelength of the Mg II line center, and assuming that the total Mg II emission is uniformly distributed over the NUV size, it takes between 2,121 and 20,159 s to reach a signal-to-noise of 10 in the default extraction region of a 5x5 box. We will use Voronoi tessellation to reach lower surface brightnesses. This setup will test the gaseous geometry on sizes relevant to impact the observed LyC escape fractions.
We take a similar procedure to determine the [O III] and [O II] emission. Our three strong leakers already have [O III] and [O II] and their continuum observations from the program PID 16245. We find that the required total exposure times for the two weaker leakers are less than 100 s for the incredibly bright [O III] emission using the FR656N filter for J1137 and the FR716N filter for J0141. The exposures for the [O II] emission line using the FR505N filter are between 200-300 s. We estimate continuum fluxes using the SDSS magnitudes in the g-band. To increase the speeds of the continuum detections, we use the medium band tunable filters with bandpasses 9% of the central wavelength. We will use F647M centered at lbda_c=7100 A to obtain [O III] continuum and two different tunings of the F459M filter to obtain Mg II (lbda_c=4200A) and [O II] (lbda_c=4800A) continuum. We aim to detect the continuum at a signal-to-noise ratio of 100 in the continuum to accurately subtract the continuum from the emission lines. These SNR can be obtained in between 800-5000 s, depending on the galaxy and the filters chosen. To properly sample the PSF we will dither between the observations using the line 2-point dither pattern (ACS-WFC-DITHER-LINE with parameters recommended in the section 7.2 of the ACS handbook allowing simultaneous elimination of hot pixels and cosmic ray hits in post-observation processing), breaking the total exposure times into at least two observations. We assume that each orbit has 2,400 s of usable time. This means that the [O II], [O III], and continuum observations can be obtained in 2 to 3 orbits depending on the objects. Meanwhile, the Mg II observations require between 1-8 orbits per galaxy. In total, we will require 31 orbits to obtain the total integration. We choose to use the WFC1-MRAMP aperture.
We will use the three different stellar continuum observations to model the stellar plus nebular continuum shape to properly account for the underlying continua. We will then study the spatial distribution of the Mg II and compare it to the [O II] and [O III] emission. By testing the physical picture of LyC escape, we will reveal whether the gas morphologies of LyC emitting galaxies are different than non-LyC emitting galaxies and see if geometry contributes to the scatter observed in the indirect indicator plots.The team is comprised of a large fraction of the Local-Redshift Lyman Continuum Survey (LzLCS). We have substantial experience with the HST/COS data that make up the escape fraction trends presented by the LzLCS. We have extensive experience dealing with detailed narrow and broad band imaging programs (Finkelstein, Hayes, Ji, Schaerer), as well as observations of ionizing photons and high-ionziation emission line galaxies (Borthukur, Chisholm, Finkelstein, Hayes, Heckman, Henry, Jaskot, Schaerer, Ravindranath, Thuan, Izotov). The team has extensive experience in using observed, spatially resolved imaging programs to determine the underlying stellar continuum and modeling the crucial parameters to isolate the nebular emission properties (e.g. Hayes et al. 2014).Galaxies6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=21.66, NUV=21.85GALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=21.31, NUV=21.61GALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=22.10, NUV=21.57GALAXYDWARF COMPACTSTARBURSTJ2000J2000NUV=22.46GALAXYDWARF COMPACTSTARBURSTJ2000J2000FUV=21.35, NUV=22.04ACS/WFCRampFilterNoNoFR388NACS/WFCRampFilterNoNoFR459MACS/WFCRampFilterNoNoFR388NACS/WFCRampFilterNoNoFR459MACS/WFCRampFilterNoNoFR388NACS/WFCRampFilterNoNoFR459MACS/WFCRampFilterNoNoFR388NACS/WFCRampFilterNoNoFR459MACS/WFCRampFilterNoNoFR505NACS/WFCRampFilterNoNoFR656NACS/WFCRampFilterNoNoFR647MACS/WFCRampFilterNoNoFR388NACS/WFCRampFilterNoNoFR459MACS/WFCRampFilterNoNoFR505NACS/WFCRampFilterNoNoFR716NACS/WFCRampFilterNoNoFR647MPOS-TARGDITHER0.146LINEfalsefalse247.17ACS-WFC-DITHER-LINE1falseThe scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.1767184613000289.0506074384575(Tic-Visit
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