0Assigned ID: 1216
----- Attempting Submission 1 (Thu Feb 28 14:50:47 GMT 2013) -----
HST Phase I Proposal 1216 (C21-Lyman-Limit.apt) successfully submitted.The number of orbits used does not match the number allocated
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.
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.
INEFFICIENT ORDERING OF FP-POS POSITIONSI grabbed the exisiting visit 51 (which is the repeat for 10) and added 1 orbit, which I was given by the TTRB for the partial failure of visit11.
Visit 51 now has 5 orbits. I did not touch visit 12, whose 5 orbits also need a repeat.1622748401----- Attempting Submission 1 (Mon Jun 24 16:35:43 GMT 2013) -----
----- Attempting Submission 2 (Tue Mar 18 19:39:31 GMT 2014) -----The coordinates are known to 0.4" or better.
I used FP-POS=ALL. I have no influence on the ordering.Pushing COS to the (Lyman-)LimitThe newly attained UV sensitivity of COS below 1150 A opens a wavelength domain not available since the end of the FUSE mission in 2007 and enables fundamentally new UV science with HST. We take advantage of this capability and propose COS+G140L spectroscopy of three carefully selected starburst galaxies at cz =13,000 km/s to measure or place stringent limits on the intrinsic Lyman continuum, and constrain the fraction of hydrogen-ionizing photons that escape the galaxies. Our galaxies were selected to have reliable, observed fluxes at 1000 A (based on FUSE archival spectra), and physical properties that provide the most favorable conditions for measuring the escape of Lyman continuum photons. The opacity to ionizing photons within star-forming galaxies, even in our own Galaxy, remains highly uncertain. Using Starburst99 with our newly developed set of model atmospheres, we will compute significantly improved constraints on the expected Lyman continuum. By measuring the redshifted Lyman break we can derive or set an upper limit to the escape fraction of ionizing radiation. In contrast, prior FUSE observations below 912 A are dominated by systematics due to variable background noise. The proposed observations will also enable studies of outflows, the interstellar reddening law, and stellar population properties, including star-formation rates and the stellar initial mass function. We will compare our results to existing data at higher redshift in an effort to understand the evolution of the escape fraction with redshift, and to shed light on the conditions that must have prevailed if primeval galaxies were responsible for reionizing the intergalactic medium at z >6.We will use COS and the G140L (1280) grating to collect R = 2000 spectra in the wavelength range ~875 Angstroms to 2100 Angstroms of the central starburst regions of the three nuclear starburst galaxies listed in Table 1. We carefully considered the trades between the G130M and G140L gratings. Both gratings (coincidentally) provide similar S/N in the Lyman continuum when rebinned to the same spectral resolution. Therefore our choice is driven by the performance longward of 912 Angstroms. G130M has R = 10,000, as compared to R =2000 for G140L. However, the G130M setting exactly duplicates the existing FUSE spectra, both in terms of resolving power and specific wavelength coverage. The FUSE data are of good quality longward of the Lyman break. The G140L data will open new parameter space by extending to ~2300 Angstroms, which allows us to study the stellar populations and the reddening law simultaneously with the Lyman continuum measurement. This is a clear case in favor of G140L.
The galaxies are at a redshift of ~0.04 (column 2 of Table 1), providing a window of ~40 Angstroms between the Milky Way and the intrinsic Lyman edge. The total luminosities (column 3) and oxygen abundances (column 4) are taken from the literature. The galaxies were observed before with FUSE; therefore accurate flux information for estimating exposure times and evaluating target acquisition strategies are available. Most of the UV flux is concentrated in the central ~2 kpc sized nuclear starburst so that the smaller COS aperture size (circular 2.5 arcsec diameter versus 30 by 30 square arcsec) is not an issue. The observed FUSE fluxes (column 5 of Table 1) were measured in the archival spectra and refer to a wavelength of 1000 Angstroms, hereafter F(1000). The observed FUSE fluxes at shorter wavelengths are dominated by systematics and cannot used here. This is illustrated in Figures 2 and 3, which show the case of Haro 11, a controversial FUSE Lyman continuum detection with claimed values of fesc between 10% Bergvall et al. (2006) and an upper limit of 2% (Grimes et al. 2007).
The SEDs of the three galaxies are more or less flat at these wavelengths. The exposure times are driven by the primary science goal of the program, constraining the Lyman continuum. We account for the intrinsic Lyman break by assuming an average Lyman continuum flux of 0.5 times F(1000) for each galaxy. The most stringent upper limits on the escape fraction of Lyman radiation in individual galaxies at low to intermediate redshifts are 2% (Bridge et al. 2010). We therefore aim to reach S/N = 50 integrated over the accessible 40 Angstroms of the Lyman continuum. The G140L grating with its ~0.5 Angstroms resolution (over six pixels) covers 40/0.5 = 80 resolution elements. Since geocoronal emission lines are not an issue for the COS background (as opposed to FUSE!), we gain a factor of sqrt(80) = 9 in S/N by binning. The current version of the COS ETC uses an overly conservative value of ~4.5 x 10e-6 c/s/pix for the dark current, whereas the currently observed values are ~1.5 x 10e-6 c/s/pix. We therefore corrected the ETC predictions by using the current values. Since all observations are time-tagged, we can test the actual dark rate during the observations, and if necessary, we will a posteriori remove observations affected by temporary bursts of high background. The required exposure times to reach S/N = 50 in the Lyman continuum are 39 ks, 24 ks, and 19 ks for Tol 0440-381, Tol 1247-232, and Mrk 54, respectively (column 6 of Table 1). At all wavelengths longward of the Lyman edge we will reach an S/N > 50 at the original R = 2000 resolving power of the G140L grating (except for slight degradations due to the targets not being point sources).
The expected orbit duration for the three galaxies is 3200 s. This translates into 12, 7, and 6 orbits for Tol 0440-381, Tol 1247-232, and Mrk 54, respectively, if only exposure times are accounted for. The maximum visit duration per galaxy is 5 orbits. Therefore we need to split the observations into groups of three or two visits. We will perform a standard imaging target acquisition. This will provide deep, scientifically valuable UV images at a resolution of ~0.05 arcsec. Accounting for guide star acquisitions, a 3 by 3 target search, re-acquisitions, visit splits, and all the overheads, we require one more orbit for each galaxy. Therefore the final orbit request is (12+1), (7+1), and (6+1) orbits (column 7). This gives a grand total of 28 orbits.ISM IN EXTERNAL GALAXIESDefaultfalsetruefalsefalsefalseSUPPORTEDGALAXYSTARBURSTThis object was generated by the target selector and retrieved from the SIMBAD database.J2000J2000F(1000)=1.0e-14GALAXYSTARBURSTThis object was generated by the target selector and retrieved from the SIMBAD database.J2000J2000F(1000)=1.5e-14GALAXYSTARBURSTThis object was generated by the target selector and retrieved from the SIMBAD database.J2000J2000F(1000)=2.0e-14COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG140L1280COS/FUVSpectroscopicNoNoG140L1280The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.139399488300089.0(Tic-Visit
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