0Assigned ID: 136
----- Attempting Submission 1 (Wed Apr 05 12:31:11 GMT 2017) -----
HST Phase I Proposal 136 (Lya2submitted.apt) successfully submitted.
Receipt: # 136-1
----- Attempting Submission 2 (Wed Apr 05 13:15:08 GMT 2017) -----1223 replaced by 12221046272664----- Attempting Submission 1 (Mon Jul 10 13:16:53 GMT 2017) -----
----- Attempting Submission 2 (Wed Oct 11 20:24:38 GMT 2017) -----Lyman alpha emission in nearby star-forming galaxies with the lowest metallicities and the highest [OIII]/[OII] ratiosThe Lyman alpha line of hydrogen is the strongest emission line in galaxies and the tool of predilection for identifying and studying star-forming galaxies over a wide range of redshifts, especially in the early universe. However, it has become clear over the years that not all of the Lyman alpha radiation escapes, due to its resonant scattering on the interstellar and intergalactic medium, and absorption by dust. Although our knowledge of the high-z universe depends crucially on that line, we still do not have a complete understanding of the mechanisms behind the production, radiative transfer and escape of Lyman alpha in galaxies. We wish here to investigate these mechanisms by studying the properties of the ISM in a unique sample of 8 extreme star-forming galaxies (SFGs) that have the highest excitation in the SDSS spectral data base. These dwarf SFGs have considerably lower stellar masses and metallicities, and higher equivalent widths and [OIII]5007/[OII]3727 ratios compared to all nearby SFGs with Lyman alpha emission studied so far with COS. They are, however, very similar to the dwarf Lyman alpha emitters at redshifts ~3-6, which are thought to be the main sources of reionization in the early Universe. By combining the HST/COS UV data with data in the optical range, and using photoionization and radiative transfer codes, we will be able to study the properties of the Lyman alpha in these unique objects, derive column densities of the neutral hydrogen N(HI) and compare them with N(HI) obtained from the HeI emission-line ratios in the optical spectra. We will derive Lyman alpha escape fractions and indirectly Lyman continuum escape fractions.We adopt an observing strategy allowing to compare two independent indirect methods for the determination of the LyC escape fraction, one is from the Ly-alpha profile derived using these observations and another using HeI emission-line ratios from independent optical observations with ground-based telescopes. In this proposal we selected the range of [OIII]/[OII] = 23 - 39 to observe eight compact galaxies at redshifts z~0.03 - 0.07. These galaxies are bright enough to ensure that we obtain within a reasonable observing time a spectrum with a S/N high enough in the FUV region to measure well the Ly-alpha profile. They have a compact or unresolved morphology in the SDSS image so that the 2.5 arcsec diameter COS aperture measures the totality of the galaxy's light and global quantities can be derived. NUV acquisition images of the targets will be obtained with the standard MirrorA and the ACQ/IMAGE mode to reach a S/N~40 inside a 9x9 pixel box centered on the brightest part of the galaxy. The total time needed for acquisition depends on the NUV magnitude of the object and its compactness. The NUV magnitudes are obtained from the GALEX database, and the NUV angular radii are assumed to be R05~0.15 arcsec, similar to angular radii of GPs observed in the proposal GO. Therefore, the surface brightness per square arcsec of our galaxies is flux(NUV)/(pi R05^2). The acquisition exposure times were calculated selecting the "EXTENDED" option and adopting a S/N of 40. As a bonus, we will be able to study the morphology of the selected objects with these acquisition images. The TAs are up to one orbit long. We plan to use COS in combination with the medium-resolution G130M grating with central wavelength 1223A to observe the Ly-alpha line at wavelengths greater than 1250A in selected galaxies. The geocoronal Ly-alpha with this grating falls into the gap between segments A and B ensuring that the COS safety condition is satisfied. Adopting the same extrapolation of the SED derived from the SDSS spectrum we have calculated for each object the required exposure time to obtain a S/N > 5 for a 10-pixel binned spectrum, enough to measure any residual intensity in the LIS lines. The ETC "EXTENDED" mode was adopted. Buffer times for science exposures were adopted to be 2/3 of the values returned by ETC for G130M grating. The 4 FP-POS split was used in all cases.Galaxies and the IGMCosmology6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=21.39, NUV=21.51, acq=1450s, http://etc.stsci.edu/etc/results/COS.ta.930822/, exp=8600s, http://etc.stsci.edu/etc/results/COS.sp.930845/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=20.64, NUV=20.43, acq=505s, http://etc.stsci.edu/etc/results/COS.ta.930823/, exp=2900s, http://etc.stsci.edu/etc/results/COS.sp.930847/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=21.67, NUV=21.58, acq=1500s, http://etc.stsci.edu/etc/results/COS.ta.930825/, exp=13380s, http://etc.stsci.edu/etc/results/COS.sp.930850/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=22.12, NUV=21.74, acq=1500s, http://etc.stsci.edu/etc/results/COS.ta.930825/, exp=6200s, http://etc.stsci.edu/etc/results/COS.sp.930857/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=20.26, NUV=20.25, acq=440s, http://etc.stsci.edu/etc/results/COS.ta.930829/, exp=1970s, http://etc.stsci.edu/etc/results/COS.sp.930862/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=21.04, NUV=20.58, acq=610s, http://etc.stsci.edu/etc/results/COS.ta.930831/, exp=4900s, http://etc.stsci.edu/etc/results/COS.sp.930865/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=21.50, NUV=21.31, acq=1200s, http://etc.stsci.edu/etc/results/COS.ta.930833/, exp=9900s, http://etc.stsci.edu/etc/results/COS.sp.930867/GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV=20.54, NUV=20.66, acq=670s, http://etc.stsci.edu/etc/results/COS.ta.930835/, exp=2500s, http://etc.stsci.edu/etc/results/COS.sp.930869/COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1300The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.154089237500068.7008380564018(Tic-Visit
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)true30Galex NUV mag for this target is 21.39. The ETC run listed here uses the "Extended source that fills the aperture (1.25 arcsec radius)" option. We estimate that our target has R < 0.2", so that the actual required time to S/N = 40 is 4-5 times shorter (8000s in the ETC run converts to ~1600s for this target). The exposure time used here is the maximum time possible for an ACQ/IMAGE and is our best TA strategy. This target has one of the faintest Galex NUV mag of the targets in this program. The other ACQ/IMAGE ETC runs in this program will use the placeholder ETC run for their Galex NUV mags. The COS.ta.930822 ETC run demonstrates that all TAs in this program are with extremely low brightest pixel counts rates ( ~< 0.1 cps).This ETC run assumes that the target is more compact than our ACQ/IMAGE estimate (R=0.2") and is 6x brighter than our expected flux at 1300.0. This ETC shows that our count rates are safe to the instrument. As all of our targets are fainter than this ETC run, we use this ETC run for all G130M exposures in this program. The Buffer time for the G130M for this ETC run is 2/3 * 30,000 = 20,000. We will use this buffer time for all G130M exposures in this program.The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.151694434900070.17683475753569(Tic-Visit
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