fourth submission-330320622Assigned ID: 2923
----- Attempting Submission 1 (Thu Mar 24 00:49:30 GMT 2022) -----
HST Phase I Proposal 2923 successfully submitted.
Receipt: # 2923-1
----- Attempting Submission 2 (Thu Mar 24 14:32:54 GMT 2022) -----
HST Phase I Proposal 2923 successfully submitted.
Receipt: # 2923-2
----- Attempting Submission 3 (Fri Mar 25 16:08:39 GMT 2022) -----
HST Phase I Proposal 2923 successfully submitted.
Receipt: # 2923-3
----- Attempting Submission 4 (Fri Mar 25 18:59:38 GMT 2022) -----
----- Attempting Submission 5 (Sun Mar 27 15:28:41 GMT 2022) -----For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.Resubmission with two HOPRs added for vists 2 and 5.1868864683----- Attempting Submission 1 (Fri Jul 08 15:04:36 GMT 2022) -----
HST Phase II Proposal 17220 successfully submitted.
Receipt: # 17220-1
----- Attempting Submission 2 (Wed Sep 07 13:09:34 GMT 2022) -----
----- Attempting Submission 3 (Mon Jun 26 18:18:20 GMT 2023) -----I decided against using all four FP positions for the targets with only two orbits. The data will be in a low S/N regime.
I ran the ETC recently to calculate the total required exposure times and then worked out the number of necessary orbits (as explained in the Proposal Information section of this Phase II.Are There Two Classes of Lyman-Leaky Galaxies?The largest uncertainty in understanding the Epoch of Reionization (EOR) concerns the physical processes that enable Lyman Continuum (LyC) photons to escape the ISM in EOR galaxies. In recent years there has been significant progress in finding leaky galaxies at both low (z < 0.4) and moderate (z ~ 3) redshifts. At low-z most of the known leaky galaxies are relatively low-mass galaxies hosting intense starbursts.
However, there are now three examples at low-z that are dramatically different: they have relatively large stellar masses and SFRs and very compact sizes (leading extremely large values of SFR/Area). They are so disjoint in their properties from other low-z leaky galaxies that the physical processes that enable the LyC leakage are almost certainly different. Intruigingly, they are actually quite similar to known leaky galaxies at z ~ 3 in terms of mass and SFR.
In this proposal we request time to observe five new potential members of this class of massive compact leaky starbursts, selected to have the same properties as the three currently-known examples. Our goals are to directly detect escaping LyC radiation, quantify its escape fraction, ascertain whether these galaxies show the other UV properties associated with leakiness, and improve our knowledge of their demographics.
These galaxies can significantly broaden our horizons in understanding the full range of processes that enable the escape of LyC radiation. They may also represent the best local analogs to the most massive/luminous EOR galaxies, which may have been major contributors to reionization, and which will be the brightest EOR galaxies (allowing the most detailed studies with JWST).Observing Description
1. Sample Selection
We have used the SDSS DR12, GALEX-GR6, and WISE catalogs to identify galaxies meeting the following criteria: z > 0.25, stellar mass > 10^10 solar masses, strong [SII] deficiency, far-UV flux > 10^-16 erg cm^-2 s^-1 Ang^-1, and u-band half-light radius < 0.5 arcsec, no sign of an AGN. This results in a sample of 5 targets.
2. Observational Set-up
We will aquire two types of data:
We will perform COS target acquistion images using the standard near-UV imaging mode. This methofd produces the most reliable results for target centering in the COS primary science aperture (PSA), We will use the PSA MIRROR A mode. The images will be of sufficient quality for us to measure the size and structure of the starburst and assess the relationship between the escape of LyC radiation and starburst compactness and/or SFR/area.
We will use the COS G140L 800 grating to collect data below the Lyman limit.
3. Required Exposure Times
The exposure times were calculated uisng the on-line STScI COS Exposure Time Calculator. We first used the GALEX FUV and NUV fluxes to estimate a flux at 1000 (1+z) Ang. We corrected this for aperture effects by assuming that the relative flux inside the COS aperture to the total is the same as the same ratio derived from SDSS u--band images. This method has proved reliable in the past.
G140L: The intrinsic amplitude of the Lyman break in the stellar population (no ISM) is typically a factor of 2 to 3. Our goal is to reach a relative escape fraction of 10% at a 3-sigma confidence level. This implies measuing the LyC at a flux level of 3 to 5% of the flux at 1000(1+z) Ang. These measurements will be made by smoothing the data and measuring the flux in a window extending from the Lyman break to roughlly 20 to 80 Ang blueward (depending on the redshift of the galaxy). Based on ETC simulations, the required exposure times require 2 to 4 orbits per galaxy.
NUV ACQ Images: We have used the GALEX NUV fluxes and the SDSS u-band half-light radius. We aim for a total S/N of 40 to be able to accurately measure the NUV size. This implies exposure times of roughly 300 sec per target.PI:
Timothy Heckman is an experienced user of COS to study starburst galaxies, including their outflows and the development of diagnostics of escaping Lyman continuum radiation.
Co-I's
Sanch Borthakur has used COS to study the escape of Lyman continuum radiation and the properties of the circum-galactic medium.
John Chisholm has used COS to study galactic outflows, the escape of Lyman continuum radiation, and the stellar population of starbursts.
Sophia Flury led the analysis of the LzLCS data and is the lead author on the two papers describing the survey and presenting the initial results.
Mauro Giavalisco is an expert of the properties of star-forming galaxies at intermediate and high redshift.
Matt Hayes has worked extensively on the escape of Lyman Alpha emission from galaxies.
Alaina Henry has used COS extensively and has pioneered the use of Mg II emission as an indicator of escaping Lyman continuum radiation.
Anne Jaskot has used COS extensively and is the PI of the Low-z Lyman Continuum Survey.
Zhiyang Ji has used models of the spectral energy distribution of the LzLyCS galaxies to measure their SFR and stellar masses.
Claus Leitherer is an expert on stellar populations in starburst galaxies and on the use of COS to detect escaping LyC radiation.
Goeran Oestlin has studied the escape of LyC radiation and the properties of the Ly alpha emission using COS data.
Roderik Overzier has conducted detailed multiwaveband obseravtions of Lyman Break Analogs.
Daniel Schaerer is an expert on both the stellar populations of starburst galaxies and in the interpretation of the signposts of leaky galaxies.
Bingjie Wang has pioneered the use of [SII]-deficiency as an indicator of LyC leakage.
Xinfeng Xu is an expert on the analysis of COS data on both AGN- and starburst-driven outflows.Intergalactic Medium and the Circumgalactic MediumGalaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYSTARBURSTNOJ2000J2000GALAXYSTARBURSTNOJ2000J2000GALAXYSTARBURSTNOJ2000J2000GALAXYSTARBURSTNOJ2000J2000GALAXYSTARBURSTNOJ2000J2000COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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