0Assigned ID: 73
----- Attempting Submission 1 (Tue Apr 08 19:54:07 GMT 2014) -----
HST Phase I Proposal 73 (Lalpha.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 12:25:54 GMT 2014) -----
HST Phase I Proposal 73 (Lalpha.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 14:29:23 GMT 2014) -----If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.0----- Attempting Submission 1 (Wed Jul 23 15:09:10 GMT 2014) -----Our coordinates are accurate within 0.4" or better.Green Peas and diagnostics for Lyman continuum leaking in star-forming dwarf galaxiesOne of the key questions in observational cosmology is the identification of the sources responsible for cosmic reionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the bulk of the ionizing photons. However, attempts at identifying individual galaxies showing Lyman continuum (LyC) leakage have so far not been successful, both at high and low redshifts. We propose here to observe directly the LyC of five so-called "Green Pea" (GP) galaxies. GPs share many of the properties of the Lyman Break galaxies at high z (compactness, low mass, low metallicity, high specific star formation rate, gas-rich and clumpy morphology) and may constitute local examples of the long sought-after LyC leaking galaxies. The five GPs have been identified by searching the Sloan Data Release 10 spectral data base of 2 million spectra for non-AGN emission-line objects that meet the following criteria: high [OIII]5007/[OII]3727 ratios, large GALEX FUV fluxes, and redshifted enough (z~0.3) so that the LyC is shifted into the sensitive spectral range of COS. Our unique GP sample will allow us to combine for the first time four fundamental tests for LyC leaking in galaxies and validate their usefulness as LyC leaking indicators : 1) direct measurements of the LyC; 2) high [OIII]/[OII] ratios; 3) characteristics of the Lyman alpha line profile; and 4) residual intensities in the low-ionization ISM absorption UV lines.To select our LyC leaking candidates, we have applied the following selection criteria to the spectral data base of 2 million spectra of Data Release 10 of the Sloan Digital Sky Survey (SDSS; Abazajian et al. 2009) 1) a non-AGN emission-line spectrum with [O iii]/[O ii]>5; 2) a GALEX FUV flux >2.3x10-16 erg s-1 cm-2 A-1; this constraint ensures that we obtain within a reasonable observing time a spectrum with a S/N high enough in the FUV region to measure well the LyC, the Ly profile and the ISM low-ionization metal absorption lines (LIS); 3) a redshift z ~0.3 so that the LyC of the object is shifted into the wavelength range where COS is most sensitive; and 4) a compact or unresolved morphology in the SDSS image so that the 2.5" diameter COS aperture measures the totality of the galaxy's light and global quantities can be derived. These criteria gave us a total sample of 5 objects.
NUV acquisition images of the targets will be obtained with the standard Mirror A and the AQN/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 flux of the objects and its compactness. The NUV fluxes are obtained from the GALEX database, and the optical angular radii R05 at half of maximum intensity are estimated from the ACS/WFPC2/COS observations of similar objects at similar redshifts. According to Cardamone et al. (2009, MNRAS, 399, 1191) and A. Henry (private communication), the angular radius of our objects at the redshift of ~0.3 is R05 ~ 0.3". Therefore, the surface brightness per square arcsec of our galaxies is flux(NUV)/(pi R05^2). We also assume that our galaxies can consist of not only a single, but two knots of star formation with equal fluxes. Then a lower limit to the surface brightness used as input parameter in the ETC for image acquisition can be estimated as flux(NUV)/(pi R05^2)/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.
We plan to use COS in combination with 2 gratings: 1) the low-resolution G140L grating (<900 - 2385 A) to measure the LyC. Adopting a flat spectral energy distribution in Fnu, the GALEX FUV magnitude, an intrinsic Lyman break of 2 (Schaerer 2003), we have calculated for each object the required number of orbits to probe the LyC escape fraction down to 5% (the 2 z~0 Ly leakers with measured LyC give escape fractions of this order, Leitet et al. 2013), with SNR > 5 for a 100-pixel binned spectrum. 2) the medium-resolution G160M grating (1410 - 1796 A) to observe the Ly-alpha and LIS lines. Adopting a flat spectral energy distribution in Fnu and the GALEX FUV flux, 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. In all cases the ETC "EXTENDED" mode was adopted. Buffer times for science exposures were adopted to be 2/3 of the values returned by ETC for both G140L and G160M gratings.COSMOLOGY12RegularfalsetruefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTJ2000J2000FUV=20.71+/-0.05, NUV=20.75+/-0.04GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTJ2000J2000FUV=20.66+/-0.30, NUV=20.38+/-0.17GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTJ2000J2000FUV=20.72+/-0.17, NUV=20.97+/-0.15GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTJ2000J2000FUV=20.16+/-0.17, NUV=20.31+/-0.05GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTJ2000J2000FUV=21.02+/-0.31, NUV=20.76+/-0.18COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 23.0.CASM was run in Phase II mode.none142752313900095.7971066195878(Tic-Visit
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