0Assigned ID: 4662
----- Attempting Submission 1 (Wed May 24 21:19:39 GMT 2023) -----
HST Phase I Proposal 4662 successfully submitted.
Receipt: # 4662-1
----- Attempting Submission 2 (Wed May 24 23:53:15 GMT 2023) -----
HST Phase I Proposal 4662 successfully submitted.
Receipt: # 4662-2
----- Attempting Submission 3 (Wed May 24 23:55:39 GMT 2023) -----
HST Phase I Proposal 4662 successfully submitted.
Receipt: # 4662-30----- Attempting Submission 1 (Thu Sep 14 20:38:46 GMT 2023) -----Establishing the Geometry of Lyman Continuum EscapeThe past decade has seen remarkable success in the direct detection of the fraction of ionizing radiation escaping from compact star-forming galaxies (r_50 < 500 pc) with high star formation rates (10 - 100 Msol yr^-1) in the rest frame Lyman continuum using the G140L, CENWAV800 mode of COS. We can now use confirmed LyC leakers to test how geometry and kinematics influence ionizing radiation escape in starbursting galaxies. We propose a pilot program to probe the nature of the outflows in a carefully chosen set of bright leakers and non-leakers, spanning a narrow range of metallicity to control on abundance uncertainties. We will use high resolution spectroscopy from COS G130M and archival G160M, to analyze absorption line profiles of HI and the host of low and high ionization species. We will employ the Semi-Analytical Line Transfer (SALT) code to determine the geometry, terminal velocities, and mass outflow rates as a function of ionization for each atomic species. We will address the long standing problem of whether ionizing radiation, at these select metallicities, escapes through holes in a patchy ISM/CGM or through a relatively smooth and tenuous density bounded optically thin medium. These analyses will inform the potential yield of a future program to examine objects at lower metallictities where the range in observed escape fraction is more extreme but the objects are fainter.For this pilot project our 6 targets were picked from the set of LzLCS objects within a narrow range of metallicity (8.2 < 12+log(O/H) < 8.5) and light weighted age (Saldana-Lopez et al. 2022) (3.1 < age(Myr) < 5.9), having the highest rest frame F1100. We selected three of these with the highest fLyC, and three with no fLyC. These 6 bright objects offer an exposure efficient program for meaningful tests of the SALT parameter determination, while controlling for metallicity and age to minimize potential variations in those parameters. This proof of concept for the SALT determination of geometry can then be proposed for a broader sample of stellar ages, metallicities, and escape fraction where the variation in escape fraction is more extreme.
We will acquire data with a velocity resolution of 80 km s^-1 at a continuum signal-to-noise of 10 using G130M. We will use these new data along with archival G160M of our objects to assess the kinematics of absorption and emission line structures.
These observations of high and low escape fraction objects will allow high fidelity determination, using the diagnostic power of SALT, of the line core optical depth, column density as a function of velocity, covering fraction, terminal velocity, and geometry. These data, when used in conjunction with Cloudy models to determine the nebular ionization parameter and degree of ionization stratification between the high- and non-leakers, will allow us to address whether there is a trend in outflow strength as a function of fLyC that warrants further investigation with an expanded data set.
We will also take advantage of recently acquired imaging data from ACS/SBC (F150LP, F165LP) and WFC3/UVIS (F438W, F547M, F850LP) from the LACOS program (Hayes - HST 17069), along with the NUV acquisition images obtained here, to assess the broadband spectral energy distributions, account for dust attenuation, and assess the geometry of extended emission beyond the aberrated COS aperture.
The six target Visits (J1053, J1158, J1540, J1440, J1033, J0917) are ordered by orbit allocations (2, 3, 4, 4, 5, 5) determined from ETC analysis of previously acquired G140 CENWAV=800 observations. All targets are point like with FWHM ranging from 0.18 to 0.44 arcsec.
Initial acquisitions will use the Mirror A NUV ACQ/Image mode with exposure times conservatively calculated from the ETC by adding 1 magnitude to the GALEX NUV magnitude and then doubling the given exposure time. This is similar to the algorithm used in the Low z LyC ACQ/Images to set up the G140L observations from which these targets were derived (Jaskot - HST 15626).
Five of target will be observed at CENWAV 1222 in FP-POS 1-4 in both A and B Segments. One of them (J103344+635317, Visit 05) will be observed in CENWAV 1291, using only in FP-POS 3-4 to allow spectral acquisition in both A and B Segments.
It is expected that each visit will fully use the orbital allocation for each target.Our team is deeply involved with the study of Lyman Continuum escape processes in low redshift galaxies using the techniques of far-UV spectroscopy and photometry. We have --
Experts in UV observations and analysis: Jaskot, McCandliss;
Experts in the reduction in far-UV spectra from COS and FUSE: Flury, McCandliss;
Experts in the fitting of spectral synthesis models to the SEDs of star-forming galaxies: Co-Is Saldana-Lopez, Flury;
Experts in the modelling of Lyman alpha, low and high ionization far-UV line profiles in static and outflowing media and the analysis of optical emission lines for the determination of gas-phase metallicity : Carr, Jaskot, Scarlata;
In addition:
Co-I Jaskot is the PI of Cycle 26 Low-z Lyman Continuum Survey
PI Carr has extensive experience with the semi-analytic line transfer (SALT) model analysis of medium resolution COS data of Green Pea galaxies and will lead this effort.
Co - PI McCandliss has been conducting astronomical research using space-base UV (HUT, FUSE, COS and Sounding Rockets) for the past 30+ years. He showed that COS was had sensitivity ~ that of FUSE down to 900 Angstroms and led the calibration proposal that enabled the development of the G140L CENWAV800 mode, upon which the Low-z Lyman Continuum Survey was based.GalaxiesIntergalactic Medium and the Circumgalactic Medium0falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1378=122e-17 (rest 1100), FUV=19.32, NUV=18.98GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1367=85e-17 (rest 1100), FUV=19.31, NUV=19.58GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1424=72e-17 (rest 1100), FUV=19.75, NUV=19.41GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1430=71e-17 (rest 1100), FUV=19.63, NUV=19.56GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1481=50e-17 (rest 1100), FUV=19.89, NUV=19.88GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000f1430=43e-17 (rest 1100), FUV=20.13, NUV=19.78COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222/private/var/folders/b9/jx3rgsbx0tgf9j1xp52tw6km0005ml/T/OPVisit15102125106261806849.xmlThe scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.(Tic-Visit
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