Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 3320
----- Attempting Submission 1 (Fri Mar 25 16:35:52 GMT 2022) -----
----- Attempting Submission 2 (Sun Mar 27 15:36:10 GMT 2022) -----Due to the updated guidelines, we will only use 2 FP-POS observations to decrease the on-orbit overheads (our spectra require S/N < 20).The number of orbits used exceeds the number allocatedThis is the phase II resubmission following the TTRB decision to repeat visit 7 (HOPR 92780)-1831408005----- Attempting Submission 1 (Thu Jul 14 22:36:20 GMT 2022) -----
HST Phase II Proposal 17153 successfully submitted.
Receipt: # 17153-1
----- Attempting Submission 2 (Sat Oct 08 15:11:26 GMT 2022) -----
HST Phase II Proposal 17153 successfully submitted.
Receipt: # 17153-2
----- Attempting Submission 3 (Tue Nov 22 01:52:09 GMT 2022) -----
----- Attempting Submission 4 (Wed Jul 26 17:31:50 GMT 2023) -----
----- Attempting Submission 5 (Mon Oct 16 14:12:03 GMT 2023) -----
----- Attempting Submission 6 (Wed Nov 22 21:22:36 GMT 2023) -----
Your proposal could not be saved.
Submission aborted.
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 7 (Tue Mar 19 16:45:46 GMT 2024) -----This is the phase II resubmission following the TTRB decision to repeat visit 7.
We ran the orbit and visit planner for this new visit only (22).Resolving Lyman Alpha emission in a complete sample of Lyman Continuum leakers and non-leakersDetermining the contribution of galaxies to cosmic reionization is one of the most pressing challenges of modern observational cosmology. Because the IGM is optically thick to ionizing radiation (LyC) during the epoch of reionization, indirect LyC escape probes are needed. Recent reionization studies have used indirect LyC tracers calibrated on samples that do not fully represent the diversity of the LyC emitters population. Here we propose 49 orbits of HST-COS observations to obtain high resolution spectra of the most promising LyC tracer, the Lyman Alpha (Lya) emission, for 15 galaxies with rigorous LyC constrains selected from the new Low-Redshift Lyman Continuum Survey (LzLCS). Our targets will complete an existing archival sample of 31 galaxies, sampling the full range of possible high redshift LyC escape fractions. By assessing whether the Lya profiles of non/weak LyC leakers are observationally distinguishable from those of moderate leakers, our observations will test if Lya can distinguish between galaxies that could and could not have reionized the universe. The large LyC escape fraction dynamical range of our complete sample of LyC leakers and nonleakers will investigate if the large scatter observed between the Lya profile and escape fractions in the archival sample can be explained by a spread in other physical parameters. This proposal will also validate other indirect tracers by comparing the Lya and Mg II profiles with radiative transfer models. Our observations will establish a definitive sample of indirect LyC probes that the James Webb Space Telescope urgently needs to unveil the sources of cosmic reionization.The Lyman alpha (Lya) spectra from the actual LzLCS survey obtained with the HST-COS G140L grism are at too low spectral resolution to resolve the Lya profiles into expected double peak. To complement the existing high resolution Lya archival sample, we propose to obtain FUV spectroscopy of 15 galaxies spanning a large range of LyC escape fraction, hereafter, fesc(LyC). We will use COS and the G160M grism to measure the Lya line profiles (all objects show Lya emission in the low-resolution G140L spectra). The central wavelengths are chosen to optimize the signal-to-noise (S/N) and ensure that the Lya does not fall in the detector gaps. COS+G160M is the only combination that provides the sensitive, high-resolution FUV spectroscopy needed for this project.
The 15 new targets are taken from the LzLCS survey. They were selected to complement the existing archival sample of objects with high resolution Lya spectra in the low (<1%), moderate (1-10%) and high (>10%) fesc(LyC) range. We selected the 5 strongest LzLCS LyC emitters for their uniqueness, since there are only few objects known so far with higher escape fraction. We selected 6 LzLCS non-leakers with stringent fesc(LyC) upper limits and 3 weak LyC leakers (<1%), doubling the size of the zero/low fesc(LyC) sample with high resolution Lya data. In the moderate fesc(LyC) range, we selected 4 LzLCS galaxies. Our sample was chosen to (i) include LyC leakers and non-leakers, (ii) have Lya observable in less than 6 HST orbits, and (iii) preserve the diversity observed in the parent LzLCS sample in terms of Lya EW, O32 and Ha EW.
The exposure times are estimated using COS ETC (v30.2) in the FUV spectroscopic mode for the G160M grating. The effective resolution will be lower for more extended galaxies. From available COS NUV imaging, however, we find that the majority of our targets are compact, with half light radii <0.2". The effective spectral resolution achieved for a source of 0.3" will typically be R~10000 (corresponding to ~ 30 km/s), sufficient for the analysis of the Lya profile (Henry et al. 2015). The Lya flux ranges from 7x10^{-15} up to 49x 10^{-15} erg/s/cm^2 and have been measured from the publicly available LzLCS G140L observations (Flury et al. 2022). The galaxies are between 0.219 < z < 0.364, corresponding to Lya at observed wavelengths between 1587 and 1659 A. In the ETC we assumed a FWHM of the Lya line of 3 A (e.g., Henry et al. 2015; Yang et al. 2017). With an exposure time between 1158 and 13476s, we reach a S/N = 10 per resolution element at the line peak position. This S/N is sufficient to measure the peak separations in Lya profiles from archival samples. All targets have already been observed with COS and pass the COS bright object check.
The target acquisition will follow the successful strategy used in the LzLCS program (15626). We will obtain acquisition images in the ACQ/IMAGE mode with Mirror A. The calculation of the acquisition exposure times is based on the LzLCS program calculations (ETC for a S/N of 40, assuming a point-like source). We divide the LzLCS values by a factor 1/2^2 to obtain a S/N=20 (between 12 and 215s).
We follow the COS handbook guidelines to determine the buffer times. We first calculate the buffer time from the spectroscopic ETC and GALEX FUV magnitude and multiply by 2/3. For all our targets, this re-scaled buffer time is longer than an individual FP-POS exposure and longer than 110 seconds. As recommended by the COS handbook, we therefore adopt the ETC buffer time multiplied by 2/3.
We attempt to schedule all of the objects in 2-3 orbit visits. Galaxies that require more than 3 orbits and can also have their science carried out in multiple visits, have been broken up into multiple visits. There are two galaxies (J083440+480541 and J130559+422638) which cannot achieve the required sensitivity in multiple orbits, thus we schedule them as single 4 and 5 orbit visits, respectively. Our spectra requiring S/N < 20, we use at least 3 FP-POS per configuration and per visit.
Reduced-gyro operations will impact the Lyman alpha fluxes of our targets leading to larger flux uncertainties that will moderately impact the science goals of our program. Moreover, the fact that not all orientations will be possible is not an issue because we do not have position angle restriction.A large fraction of the team are CoI and PI of the Local-Redshift Lyman Continuum Survey (LzLCS) from which the targets are selected (Flury et al. 2022). Part of the team has also contributed to the recent discovery of the low-z strong LyC leakers/emitters with HST/COS observations (Izotov et al. 2016ab, 2018b, 2021). We have extensive experience with COS spectroscopy and spectroscopy in general. The team has also assembled and analysed a lot of ancillary data (imaging and spectroscopy) of the LzLCS including the present targets. This includes also high-resolution optical spectra obtained with Keck, VLT, and others. The team has also extensive
experience in radiation transfer modeling (Verhamme+) and has developed state-of-the-art tools which can be used to model the Lya line observations and compare to existing MgII models.Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.33, NUV=20.35GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.11, NUV=20.19GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=22.21, NUV=22.52GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=22.21, NUV=21.25GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.83, NUV=20.84GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.31, NUV=21.83GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=21.34, NUV=22.24GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.63, NUV=20.68GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.89, NUV=19.88GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.83, NUV=21.23GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.31, NUV=19.58GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=20.81, NUV=22.28GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.45, NUV=19.30GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=22.18, NUV=22.85GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000FUV=19.75, NUV=19.41COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1694174008000272.20451518666323(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Obset
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)
(Tic-Orbit
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)true10The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1681294816000153.6154947834135(Tic-Visit
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(Tic-Obset
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)
(Tic-Orbit
:proposal-id 17153
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(Tic-Orbit
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)true20The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.1698794580000320.4120743504298(Tic-Visit
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(Tic-Orbit
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(Tic-Obset
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)true10The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.169051506700094.61690471970587(Tic-Visit
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)
(Tic-Obset
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)
(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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:pcs-gap 0
)true50The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1689922193000121.75789540707927(Tic-Visit
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)
(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 17153
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)
(Tic-Orbit
:proposal-id 17153
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(Tic-Orbit
:proposal-id 17153
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:low-sky "N"
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:pcs-gap 0
)true40The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.16997798980004.551759114927307(Tic-Visit
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:date "13-Oct-2023 16:20:10.0"
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:number-of-orbits 1
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:data-volume 52368
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:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
:proposal-id 17153
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3389
:pcs-gap 0
)true10The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.1709932582000261.0(Tic-Visit
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)
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)
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)true10