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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.
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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.0Assigned ID: 1181
----- Attempting Submission 1 (Wed Nov 20 17:47:33 GMT 2019) -----Joint HST/NRAOCOS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.Hi all. This is a first complete Phase II submission for program 16054.
We would greatly appreciate help from STScI in checking and optimizing this phase II.
There is some unused orbital visibility still, which we would like to fix before observations are taken,
but we also would like an expert to look over the Phase II submission for other issues that we may not know about.
Second submission - fixed comments under "team expertise" section.
Third submission [JP] - addressed the comments from Crystal Mannfolk and Will Fischer to
fix coordinates and central wavelengths, add ETC calculations, use TIME-TAG, and fill observation time.
Fourth submission [JER] - reduced visit 3 from two orbits to one orbit, per TTRB instructions on
disposition of the orbit formerly allocated to target 2 and visit 2.
Fifth submission [JP] - minor adjustment to fill orbit time for Visit 03.-998050007----- Attempting Submission 1 (Wed Jan 08 08:58:26 GMT 2020) -----
HST Phase II Proposal 16054 (vla_hst_ph2_v200107a.apt) successfully submitted.
Receipt: # 16054-1
----- Attempting Submission 2 (Wed Jan 08 11:28:52 GMT 2020) -----
----- Attempting Submission 4 (Wed Jan 15 20:16:22 GMT 2020) -----
----- Attempting Submission 5 (Sat Jan 18 14:35:33 GMT 2020) -----
----- Attempting Submission 6 (Thu Jan 30 19:20:39 GMT 2020) -----Remaining warnings, to our knowledge, are all informational.
We know that we added an investigator, and we understand that calibration of COS data
for extended sources poses some challenges (but we've used such data before on similar objects).Mapping HI 21cm emission in Green Pea galaxiesGreen Pea Galaxies are compact, low-mass, extreme starburst systems in the nearby Universe, with strong emission lines that rival the stellar continuum in their total luminosity. Such strong line emission demands vigorous star formation, with characteristic ages of just a few million years for the stellar populations that dominate the optical and UV light. Green Peas are the best analogs of high redshift Lyman-alpha emitting galaxies, with many showing high leakage of ionizing photons. Until recently, little information was available about the neutral gas, the fuel for star formation, in Green Peas. We have now used the Arecibo and Green Bank Telescopes to measure the HI content of a sample of Green Peas. We propose here to use the JVLA to map the HI 21cm emission from six galaxies of our sample, and to also obtain HST-COS FUV spectroscopy covering the Lyman-alpha line and the far-ultraviolet metal lines of five of the six galaxies, to infer the spatial distribution of the HI, and derive the HI column density, filling factor, and kinematics, to understand the conditions that promote Ly-alpha escape. We request 48 JVLA L- band hours in C-array, and seven HST-COS orbits, for this project, including all overheads and calibration.We wish to obtain COS FUV spectra of 6 low-redshift green peas that have detected 21-cm HI radio emission and have no UV spectra covering restframe \lya\ line in the archives. We will use these spectra to characterize \lya\ line emission (where present), \lya\ line absorption, and metal line absorption. These measurements will enable us to measure the \lya\ escape fraction, and to measure the neutral gas column density and covering fraction using multiple tracers. This will enable the \lya\ escape to be compared to the neutral gas supply in a statistically useful sample of Green Peas for the first time. Existing archival data + currently approved observing programs supply another 2 (soon to be 3 objects), which we will include in our analysis for an overall sample of 9 objects. Among the two currently in the archive, all show measurable damped \lya\ absorption, and one shows a strong, narrow \lya\ emission line also. One object has a spectrum taken with G140L which is low enough resolution to preclude robust radiative transfer modelling.Kanekar, Ghosh, and Chengalur are all radio experts and are managing the VLA portion of this program.
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