0Assigned ID: 765
----- Attempting Submission 1 (Fri Apr 10 20:20:29 GMT 2015) -----
HST Phase I Proposal 765 (gotoqs_cos.apt) successfully submitted.
Receipt: # 765-1
----- Attempting Submission 2 (Fri Apr 10 23:07:57 GMT 2015) -----
HST Phase I Proposal 765 (gotoqs_cos.apt) successfully submitted.
Receipt: # 765-2
----- Attempting Submission 3 (Fri Apr 10 23:08:51 GMT 2015) -----In preparing this proposal, I referenced several archival QSO COS programs and their respective phase II proposals to ensure our
technical specifications were within reasonable parameters. Our program setup is similar. One difference may be that we choose to use Mirror A,
where many archival proposals use Mirror B.
Edit: resubmitted after removing orbital visibility overrun.
Edit 2: changed Q1005, Q1328, Q1452, and Q1659 to use G140L_1280 instead of G140L_1105 for purposes of additional wavelength coverage. updated relevant buffer times and ETC runs.
Edit 3: added NUV fluxes from GALEX for all targets.186099603----- Attempting Submission 1 (Mon Jul 20 08:53:42 GMT 2015) -----
HST Phase II Proposal 14137 (gotoqs_c23_pII.apt) successfully submitted.
Receipt: # 14137-1
----- Attempting Submission 2 (Mon Jul 20 15:03:12 GMT 2015) -----
HST Phase II Proposal 14137 (gotoqs_c23_pII.apt) successfully submitted.
Receipt: # 14137-2
----- Attempting Submission 3 (Tue Jul 21 20:07:05 GMT 2015) -----
HST Phase II Proposal 14137 (gotoqs_c23_pII.apt) successfully submitted.
Receipt: # 14137-3
----- Attempting Submission 4 (Tue Dec 08 22:21:13 GMT 2015) -----Damped Lyman-alpha Systems in the Disks of Low-z SDSS Galaxies on Top of QSOsDamped Lyman-alpha (DLA) and sub-DLA absorbers dominate the mass density of neutral gas in the Universe (log N(HI) > 20.3 and 19.0< log N(HI) < 20.3 respectively) and are easily detected in the spectra of background QSOs. Though they have been studied for decades, the relationship between DLAs, sub-DLAS, and the properties of their host galaxies remain an open question. This class of objects, being cold and neutral, have long been believed to be critical in the formation of galaxies and ideal staging grounds for new star formation. In fact, many studies suggest they may arise in galaxy disks or, due to their low metallicity nature, dwarf galaxies. The distinction is of great importance and requires the identification of as many host galaxies as possible, which is easiest at low-z due to the decrease in surface brightness with distance.
We present a sample of 10 FUV-bright QSOs probing the disks of foreground galaxies at z<0.14 from the SDSS. These galaxies have known star formation rates, E(B-V), and most importantly: imaging detections detailing their morphology and orientation relative to the QSO line of sight. We propose to use HST/COS to determine the neutral hydrogen column density of these galaxies in order to constrain the host environments of DLAs and sub-DLAs. We will use the spectra to determine metallicity gradients and HI covering fraction at z<0.14. Finally, we will determine correlations between the HI absorption strength with the galaxy orientation and morphology that have been found in the literature for Mg II and Na I D.Since we are looking specically for sub-DLAs and DLAs (with 19.0<log NHI<20.3 and log NHI>20.3, respectively), a spectral resolution of Delta-lambda = 10A would be suffcient. At the wavelengths we are considering (~1350A), COS has a resolving power of approximately 1500 with the G140L grating, corresponding to a spectral resolution of Delta-lambda ~ 1A, which is more than suitable for our purposes.
We plan COS observations of 10 QSO sight lines that coincide with foreground galaxies in the SDSS. We have chosen our sample from our survey of 103 GOTOQs based on their FUV brightness (> 30 microJy in GALEX) and redshifts z < 2. We estimate using the COS ETC that we can reach a S/N~10 per resolution element in two orbits per QSO (4x1200s exposures) using the G140L_1105 grating. In our simulation, we have assumed a FOS-based QSO spectrum and FUV flux (> 30 microJy) from GALEX data. The emission redshifts of the QSO and the foreground galaxy are known from SDSS and our previous study of the GOTOQs (York+12; Straka+13,15). The QSOs we target are faint enough to avoid saturation during our exposures on COS.
TARGET ACQUISITION:
Each object will have target acquisition as follows:
COS ACQ/IMAGE - We use the ETC to determine the exposure time required to reach S/N~40. Because these QSOs have galaxies directly on top of them, the galaxies may be contributing UV flux to the GALEX flux measurements and magnitudes. Therefore, we conservatively estimate that the QSOs have half the flux reported by GALEX for the purposes of target acquisition in order to account for QSO variability and foreground galaxy contamination. We use the PSA and Mirror A for our settings. We assume a FOS-based QSO spectrum.
We also ran acquisition simulations at STScI in order to determine if the foreground galaxies would cause acquisition problems. The simulations came back with no problems centering on the QSOs.
EXPOSURE SETUP:
We will use the default FLASH = YES for all of our observations, which are taken in TIME-TAG PSA mode, in order to maximize science integration times. In addition, we will use all 4 FP-POS settings, manually set across four exposures (2 exposures per orbit, 2 orbits). This will minimize fixed position noise and detector artifacts. The FP-POS settings are arranged in increasing order for each visit (1, 2, 3, and 4) to minimize overhead.
BRIGHT OBJECTS AND BUFFER TIMES:
We have checked the GALEX FUV and NUV images for foreground galaxy contribution to the flux and found no detection of the foreground galaxies for any of our targets. We have used the APT Bright Object Tracker to determine if there are any field objects that might pose a health or safety threat while using COS/FUV. We used the GALEX database for this search and found that all of our fields return safe.
We have used the ETC to determine the buffer time for each of our science frames. In each case, the ETC buffer time exceeds the science exposure time. Therefore, we take 2/3 of the ETC buffer time as our APT buffer time input for each science frame. The typical 2/3 ETC buffer time fore our sample is ~7000s.
OBSERVING FORMAT:
Our COS observations will proceed on average as follows (with some variability depending on target visibility):
First orbit: Guide star acquisition + ACQ/IMAGE + science (~20 minutes) + science overhead (5 minutes first exposure) + science (~20 minutes) + science overhead during occult (2 minutes subsequent exposure otherwise).
Second orbit: Guide star re-acquisition (~4 minutes) + science (~24 minutes) + science overhead (2 minutes) + science (~24 minutes) + science overhead (2 minutes) + occult.
Total science for 2 orbits : ~80 minutes
Total overhead for 2 orbits: ~20 minutes
Total orbits for 10 targets: 20 orbitsQUASAR ABSORPTION LINES AND IGM12falsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOJ2000J2000FUV=38microJy, NUV=102microJyGALAXYQSOQUASARNOJ2000J2000FUV=63microJy, NUV=115microJyGALAXYQSOQUASARNOJ2000J2000FUV=53microJy, NUV=59microJyGALAXYQSOQUASARNOJ2000J2000FUV=35microJy, NUV=36microJyGALAXYQSOQUASARNOJ2000J2000FUV=113microJy, NUV=155microJyGALAXYQSOQUASARNOJ2000J2000FUV=40microJy, NUV=46microJyGALAXYQSOQUASARNOJ2000J2000FUV=48microJy, NUV=82microJyGALAXYQSOQUASARNOJ2000J2000FUV=39microJy, NUV=99microJyGALAXYQSOQUASARNOJ2000J2000FUV=119microJy, NUV=146microJyGALAXYQSOQUASARNOJ2000J2000FUV=70microJy, NUV=120microJyCOS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105/private/var/folders/ny/y2rfgxpn4k37g754z2ph3gd00001bc/T/OPVisit7101585912100299059.xmlThe scheduling data was generated by CASM 24.0.CASM was run in Phase II mode.GALEX FUV flux halved for ETC in order to account for QSO variability and foreground galaxy contamination.(Tic-Visit
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:low-sky "N"
:pcs-visibility 3210
:pcs-gap 0
)true20