0Assigned ID: 462
----- Attempting Submission 1 (Fri Feb 24 16:21:57 GMT 2012) -----
HST Phase I Proposal 462 (hstcycle20.apt) successfully submitted.
----- Attempting Submission 2 (Sat Feb 25 00:00:52 GMT 2012) -----The remaining APT warnings are addressed in the Observing Description:
The target coordinates are precise enough for ACQ/IMAGE (the warning is superfluous given the APT entry for the position accuracy).
In Phase I we requested to maximize COS wavelength coverage by using FP-POS=3 and 4 only.
shortened exp. 2, visit 7 by 6 seconds. There was an overrun.
auto adjusted all orbits, shortened exposures 2-4 in visit 3 by 5 seconds each to keep it to 3 orbits.-325595859----- Attempting Submission 1 (Thu Jun 21 21:25:56 GMT 2012) -----
----- Attempting Submission 2 (Wed Oct 31 14:45:19 GMT 2012) -----
HST Phase II Proposal 13013 (13013.apt) successfully submitted.
----- Attempting Submission 3 (Wed Oct 31 15:13:12 GMT 2012) -----The target coordinates from SDSS are precise enough for ACQ/IMAGE. In accordance with our Phase I proposal we request COS G140L observations with FP-POS=3 and 4 to maximize wavelength coverage and to provide sufficient correction for fixed-pattern noise, grid wires and gain sag at our low S/N.How Extended was Helium II Reionization? A Statistical Census Probing Deep into the Reionization EraThe advent of GALEX and HST/COS have revolutionized studies of HeII reionization. In Cycle 17 we pioneered an effective strategy that combines highly efficient GALEX/FUV selection with HST/COS spectroscopy. Our proven approach now accounts for more than half of the science-grade HeII Ly-alpha transmission spectra in the HST archive. The clear picture emerging from these data is that z~2.7-3 marks the end of HeII reionization. However, comparison to our state-of-the-art radiative transfer simulations indicates that the duration of HeII reionization and its stochasticity remain virtually unconstrained because of the sparseness of current data at z>3. It is thus unequivocal that the path forward is COS spectra of higher redshift (z>3) QSOs deep into the reionization era. Further, a statistical census is crucial given the large sightline-to-sightline variance implied by limited existing data and verified by our numerical models. We request 21 orbits to obtain science-grade COS far-UV spectra of 7 UV-bright QSOs (newly discovered by our dedicated survey), which will double the HeII pathlength at z>3. Comparison of the distribution of HeII optical depths to our simulations will constrain the duration and stochasticity of reionization. Additional leverage will be obtained by observing the anticipated spectral hardening of the UV radiation field as reionization progresses, achieved by combining HeII transmission with ancillary coeval HI Ly-alpha forest spectra. Our survey also enables statistical investigations of the sources of HeII reionization from the HeIII QSO proximity zones, and by identifying foreground QSOs via a dedicated ground-based imaging and spectroscopic survey.We will obtain COS FUV G140L spectra of 7 z>3.1 quasars to search for intergalactic HeII absorption. The targets are spectroscopically confirmed FUV-bright quasars discovered by our team in a dedicated survey. Given the ~80% success rate of previous HeII surveys using GALEX-selected high-redshift quasars, we will directly obtain science-grade HeII absorption spectra.
Our targets have accurate GALEX FUV magnitudes covering the quasar continuum redward of the HeII break at z<3.5 and accurate GALEX NUV magnitudes for reliable acquisition via ACQ/IMAGE. All targets are safe to observe with COS and have precise SDSS coordinates. With the COS ETC we estimated NUV imaging acquisition exposure times of 40-300s to reach the recommended S/N=40 for our sometimes NUV-faint targets. The G140L grating provides the wavelength coverage to define the quasar continuum and the necessary resolution to measure the patchy HeII absorption at the end of HeII reionization (z~2.7). For each target we plan a single 3-orbit visit, yielding a S/N~3 per resolution element at 1400A, in agreement with our previous experience (note that the ETC overestimates the S/N in the low-count regime). For one target we request CVZ observations.
Continuous wavelength coverage at good sensitivity (lambda>1100A) is required to give maximum coverage of the HeII absorption, only provided by the G140L 1105A setup in the bluest grating setting (FP-POS=4, lambda>1110A corresponding to z>2.66). To correct for the COS grid wires (any further fixed-pattern noise is unimportant at our S/N) we request G140L 1105A observations at FP-POS=3 and 4, in accordance with our Phase I proposal. One-orbit exposures per setup will ensure proper background assessment of COS and the contaminating geocoronal emission. All spectra will be recorded in TIME-TAG mode with concurrent wavelength calibration (TAGFLASH). Time intervals spent in the Earth's shadow will be used to correct for geocoronal OI and NI emission. Given our faint sources, airglow will dominate the COS count rates. However, even at the high airglow conditions conservatively assumed in our ETC calculations, buffer times are longer than the exposure times, except for the CVZ target. All exposure times have been adjusted to use the full visibility period in each orbit. For the CVZ target we will issue a buffer dump slightly before the end of each exposure to minimize readout overhead. To correct z>3.25 HeII Gunn-Peterson troughs for geocoronal OI emission, we will take only one exposure in FP-POS=4 in which geocoronal OI falls on a COS grid wire. For z<3.25 targets in which OI falls on the quasar continuum, two exposures in FP-POS=4 maximize depth at the shortest wavelengths.In accordance with our Phase I proposal we request CVZ observations for QSO-170621+590406.QUASAR ABSORPTION LINES AND IGM12false0.00.0falsefalsefalsefalseSUPPORTEDGALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=1.36+/-0.23 E-16, F(2316)=1.40+/-0.09 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=2.72+/-0.10 E-16, F(2316)=2.22+/-0.04 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=0.92+/-0.12 E-16, F(2316)=0.42+/-0.04 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=1.34+/-0.47 E-16, F(2316)=0.26+/-0.09 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=1.56+/-0.29 E-16, F(2316)=0.81+/-0.13 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=1.27+/-0.22 E-16, F(2316)=0.67+/-0.06 E-16GALAXYLYMAN ALPHA CLOUDQSOJ2000J2000F(1539)=1.55+/-0.21 E-16, F(2316)=0.72+/-0.14 E-16COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105/private/var/folders/Pi/PiItoBTTEo4iuUPDCliQok++5+6/-Tmp-/OPVisit719389841856228596.xmlThe scheduling data was generated by CASM 20.2.CASM was run in Phase II mode.(Tic-Visit
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