0Assigned ID: 548
----- Attempting Submission 1 (Fri Apr 10 16:17:55 GMT 2015) -----For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.0----- Attempting Submission 1 (Tue Jul 21 15:38:56 GMT 2015) -----
----- Attempting Submission 2 (Tue Dec 15 16:34:29 GMT 2015) -----
----- Attempting Submission 3 (Thu Jun 16 16:33:30 GMT 2016) -----We require “contiguous spectral coverage” and that some FP-POS are split among different visits.Characterizing Circumgalactic Gas around Passive GalaxiesLuminous Red Galaxies (LRGs) are passive galaxies found in dark matter halos of ~1E13 Msun with little to no on-going star formation detected. Our group noted in 2009 that a significant fraction of LRGs at z ~ 0.5 display coincident strong MgII absorbers in their halos. This finding is now confirmed with a new and larger sample of LRGs available from SDSS DR12. The presence of cool gas in these massive halos challenges predictions from both numerical simulations and analytic models that halo gas around massive galaxies is hot (T>1E6 K) and cold clumps would evaporate quickly. The quiescent state of the galaxy also makes starburst outflows an unlikely explanation for the observed MgII absorbers. However, direct and quantitative comparisons with theoretical predictions require knowledge of HI column density and metallicity. To determine these quantities at z ~ 0.5, FUV spectra of the QSOs are necessary. We have searched SDSS and GALEX archives and found a total of 9 LRGs with a UV bright QSO (FUV<18.5 mag) at projected distances < 150 kpc. This close LRG-QSO pair sample offers a unique and important opportunity to gain a deeper understanding of halo gas content around LRGs. Four of the QSOs have COS spectra already available in the HST archive, and an initial analysis of the data indicates a modest scatter in the physical properties. Here we propose to obtain high-resolution COS G130M and G160M spectra for the remaining five QSO. The proposed and archival COS spectra together will enable a detailed study of the ionization state and metallicity of halo gas around quiescent galaxies, and offer key insights into the physical origin of cool gas in massive halos.We will obtain high-resolution FUV spectra of five UV bright QSOs located at projected distance d<150 kpc from a foreground luminous red galaxy (LRG), using COS and the G130M and G160M gratings. The goal of the proposed observations is to determine the neutral hydrogen column density, N(HI), and metallicity of the cool clouds found in quiescent LRG halos. The redshifts of the LRGs are ideally suited for the COS wavelength coverage enabling observations of the full HI Lyman series and a suite of heavy element transitions for accurate measurements of N(HI), gas ionization state, and metallicity.
Exposure Time Estimate:
Based on our previous experience with COS data, we estimate that a signal-to-noise ratio (SNR) of >7 per resolution element is required to place constraints on the ionization-state and metallicity of the absorbing gas. Observations of this moderate SNR will enable 2-sigma rest-frame detection limits of better than W=0.1 Ang, for absorption features at the LRG redshift between the Lyman-limit and Lya features. The equivalent width limit corresponds to sensitive column density limits of, for example, 2e13 cm^{-2} for HI & SiII and lower for SiIII and CIII, accounting for the broad wings of the COS line spread function. Achieving the desired signal-to-noise ratio of these transitions will result in a higher SNR of 15 per resolution element at the expected positions of the CII and OVI transitions enabling detection limits of 3e13 cm^{-2} for these weaker absorbers. To estimate the exposure time to reach the desired SNR, we used the COS spectroscopic ETC and GALEX FUV magnitudes of the QSOs which range from AB(FUV)=18.0 to AB(FUV)=18.4. We estimate required exposures times of 2 orbits for G130M and 4-5 orbits for G160M.
COS Configuration:
The desired spectral coverage can be provided by the G130M and G160M gratings with standard central wavelength settings. These two gratings also provide sufficient resolution (FWHM ~ 18 km/s) for detecting weak, narrow absorption systems. We use two central wavelength settings to obtain contiguous spectral coverage and choose the combination to minimize the chances of critical absorption features falling in the low S/N gap. For each central wavelength setting, we use between two and three FP-POS offsets to minimize fixed pattern noise. Combining two central wavelength settings per grating and 2-3 FP-POS offsets per central wavelength setting leads to at least 4 different FP-POS offsets per grating.
Target Acquisition:
The COS entrance aperture is 2.5" in diameter. To center the quasar in the aperture at the beginning of each visit, we will obtain an FUV image in ACQ/IMAGE mode. No ACQ/SEARCH is necessary because the quasar coordinates are known to better than 0.1". The GALEX FUV magnitudes of the quasars range from AB(FUV)=18 to AB(FUV)=18.4. Using the COS Target Acquisition ETC, we find that for two QSOs, J0946+5123 and J1243+3539, we can obtain S/N greater than 40 in less than 10 sec using MIRROR A. For the other three, we need to use MIRROR B to avoid exceeding the bright limit.QUASAR ABSORPTION LINES AND IGM12falsetruefalsefalsefalsefalseSUPPORTEDGALAXYLYMAN ALPHA CLOUDQSONOJ2000J2000AB(FUV)=18.44; AB(NUV)=18.01GALAXYLYMAN ALPHA CLOUDQSONOJ2000J2000AB(FUV)=18.32; AB(NUV)=17.24GALAXYLYMAN ALPHA CLOUDQSONOJ2000J2000AB(FUV)=18.09; AB(NUV)=17.54GALAXYLYMAN ALPHA CLOUDQSONOJ2000J2000AB(FUV)=18.37; AB(NUV)=17.84GALAXYLYMAN ALPHA CLOUDQSONOJ2000J2000AB(FUV)=18.03; AB(NUV)=17.62COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.(Tic-Visit
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