0Assigned ID: 129
----- Attempting Submission 1 (Wed Apr 08 18:54:41 GMT 2015) -----
HST Phase I Proposal 129 (groups.apt) successfully submitted.
Receipt: # 129-1The number of orbits used exceeds the number allocated
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.
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.copied visit 14 to visit 16. 14 failed due to spacecraft anomaly.1439747065----- Attempting Submission 1 (Tue Jul 14 15:56:53 GMT 2015) -----
----- Attempting Submission 2 (Tue Jul 14 17:11:00 GMT 2015) -----
----- Attempting Submission 3 (Wed Jan 06 18:01:27 GMT 2016) -----
----- Attempting Submission 4 (Tue Jul 12 17:12:00 GMT 2016) -----
----- Attempting Submission 5 (Fri Mar 17 15:49:53 GMT 2017) -----We've picked Cenwave and FPPos settings intentionally.Probing Hot Gas in Spiral-Rich Galaxy GroupsApproximately 30% of the baryons in spiral galaxies like the Milky Way are "missing'' in the sense that while predicted to be present by numerical simulations and chemical evolution histories, this gas has not been detected as yet. Based on recent high-S/N (> 20) COS far-UV spectroscopy, this gas MAY have been detected as broad, shallow Ly alpha and OVI absorptions associated with foreground spiral-rich galaxy groups. These low-contrast features associated with T>10^5 K gas have not been detected by any other COS program probing galaxy, group or cluster halos due to insufficient S/N.
This proposal seeks to confirm or deny the presence of massive reservoirs of spiral group gas by obtaining high-S/N (>20) GOS G130M spectra of 10 bright QSOs behind 12 (two sightlines probe two groups each) low-z (0.1-0.2) galaxy groups selected from the SDSS using a consistent group-finding algorithm. Selecting the groups first, then searching for the absorptions provides a homogeneously-selected group sample to investigate and allows us to choose sightlines which probe these groups at a range of radii from their centers (0.3-1.4 R_virial) and which do not pass close to individual group galaxies. The redshift selection places the OVI doublet and Ly alpha in regions of highest COS sensitivity. The UV-initiative program to detect these subtle absorption features requires a total of 45 orbits to execute.Our set of group-selected absorption-line probes is composed of ten AGN sightlines which probe twelve spiral-rich galaxy groups at z=0.11-0.18. This redshift range was selected such that OVI 1031, 1038 doublet is redshifted into the sensitive COS/G130M spectral range (z>0.11), while Lya 1216 is has not yet redshifted onto the less sensitive COS/G160M grating. Much of this redshift range placed the OVI doublet blueward of Lya rest, making the identification of OVI mostly unambiguous. Additionally, we require that the AGN redshift be at least cz>3000 km/s greater than that of the group to minimize confusion with the signature of AGN outflow absorption. We further screened groups such that both Lya and the stronger OVI lines fall in spectral regions free of strong Galactic absorption. A range of fractional impact parameters and group richnesses are well-represented.
Using galaxy redshift information, we verified that the nearest individual group galaxy to the line of sight lies a minimum of 1.5 virial radii from the line of sight. This makes it most likely that any detected absorption is associated with the group not the halo of an individual galaxy (see e.g., Prochaska et al. 2011; Stocke et al. 2013).
We estimate the far-UV flux of each AGN from GALEX FUV-band photometry, or via previous low-resolution FUV spectra where available. The COS ETC was then used to estimate the exposure time neccessary for our required S/N=20 per resolution element and the results rounded up to the nearest HST orbit.QUASAR ABSORPTION LINES AND IGM6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOCoordinates checked with NED.SDSSJ102814.54+211955.2J2000J2000F(1500Ang)~3e-15 (GALEX FUV)GALAXYQSOQUASARNOSDSSJ1614.10.62+263250.4J2000J2000F(1500A)~2e-15 (GALEX FUV)GALAXYQSOQUASARNOSy1SDSSJ154019.57-020505.42MASXJ15401957-0205053J2000J2000F(1500A)~2e-15 (GALEX FUV), z=0.3205GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.SDSSJ083583.90+442602.3RXJ08359+4426J2000J2000F(1500A)~1e-14 (GALEX FUV), z=0.2546GALAXYQSOQUASARNOSy1SBS0956+510SDSSJ095931.66+504449.1J2000J2000F(1500A)=5e-15 (GALEX FUV), z=0.1434GALAXYQSOQUASARNOFSRQ, radio jetB21028+31SDSSJ103059.09+310255.8J2000J2000F(1500A)~2e-15 (GALEX FUV)GALAXYQSOQUASARNONLSy1, QSOFBQSJ151936.1+283827SDSSJ151936.15+283827.6J2000J2000F(1500A)~3e-15 (GALEX FUV), z=0.2700GALAXYQSOQUASARNOQSOSDSSJ150527.60+294718.31RXSJ150527.0+294722J2000J2000F(1500A)~4e-15 (GALEX FUV), z=0.5261GALAXYQSONOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Added to proposal Jan 6, 2016 after change request (substitute for target #5 in this proposal)J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.1459595025000115.87777999999997(Tic-Visit
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)true30The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.1458988357000136.51940677718449(Tic-Visit
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