0Assigned ID: 6021
----- Attempting Submission 1 (Mon Nov 25 14:08:27 GMT 2024) -----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.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.0----- Attempting Submission 1 (Wed Dec 18 20:46:50 GMT 2024) -----We aknowlegde that extended targets have calibration limitationsThe HI properties of low-z Green Pea galaxiesGreen Pea galaxies (GPs) are low-mass, extreme starburst systems in the nearby Universe, with powerful emission
lines, including forbidden [OIII] lines, that rival the stellar continuum in luminosity. GPs with high values of O32,
the ratio of the [OIII]5007 line luminosity to the [OII]3727 line luminosity, are expected to be the best analogs of
the high-redshift galaxies that reionized the Universe, with a number of such GPs showing high leakage of ionizing
photons. Recent Arecibo and GBT studies have detected 21cm emission from ~60% of the GPs with O32<10, they
only obtained 21cm non-detections from GPs with O32>10. We propose to use the VLA to carry out deep 21cm
spectroscopy of 8 GPs with z<0.05 and O32>10, to measure their HI masses, HI-to-stellar mass ratios, and HI
depletion timescales. We also propose to obtain HST-COS far-UV spectroscopy covering the Lyman-alpha line and
the metal lines of four of the 8 GPs, which do not currently have HST-COS spectroscopy, to infer the Ly-alpha
escape fraction, the HI column density and the HI filling factor, and compare these to the HI properties inferred from
the VLA 21cm images. We request 78 L-band hours in C-array, and four HST-COS orbits for this proposal.One orbit of COS spectroscopy on each of four Green Peas for which VLA time was allocated, and for which no prior COS spectroscopy exists.Nissim Kaneka is a Radio astronomer working on 21cm and CO observations of Green Peas. Uses 21cm, CO, and CII-158 micron lines to study high-z
galaxies, and also works on the ISM of the Milky Way and nearby galaxies.
Archishman Khasnovi is a Ph.D. student working on the 21cm and CO observations of Green Peas.
James Rhoads is an expert on the population properties of Lyman alpha galaxies, on Lyman alpha based tests of cosmological reionization, and on wide-field narrowband surveys.
Sangeeta Malhotra is the PI of the US side of the LAGER survey. She pioneered reionization tests using Lyman alpha galaxies, starting with Malhotra & Rhoads 2004. She also has a long standing interest in the physical properties of Lyman alpha galaxies, and recently has been investigating the physical properties of their low redshift analogs.
John Pharo is an expert on emission line galaxies including green pea galaxies.
Isak Wold is an expert on emission line galaxies with an emphasis on Lyman alpha emitters across all redshifts, and with long experience of UV observations.Galaxies6falsefalsefalsefalsefalsefalsefalsetrueSECONDARYNRAOVLA/25A-407falseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESJ2000J2000GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESJ2000J2000GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESJ2000J2000GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESJ2000J2000The scheduling data was generated by CASM 32.1.3.CASM was run in Phase I mode.COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 32.1.3.CASM was run in Phase I mode.COS/FUVSpectroscopicNoNoG130M1222The scheduling data was generated by CASM 32.1.3.CASM was run in Phase I mode.COS/FUVSpectroscopicNoNoG130M1222The scheduling data was generated by CASM 32.1.3.CASM was run in Phase I mode.COS/FUVSpectroscopicNoNoG130M1291/private/var/folders/1l/lh25bjxs2s776hsgwkn81pvc0000gz/T/OPVisit12887245540042066305.xmlThe scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.(Tic-Visit
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