0Assigned ID: 344
----- Attempting Submission 1 (Fri Apr 11 02:54:59 GMT 2014) -----
HST Phase I Proposal 344 (n3510.apt) successfully submitted.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.Effort made to include as many FP-POS as possible, but shorter visits don't always cover all 4 FP-POS because of time lost with grating change.
Two CENWAVES used for all objects (1291 & 1327), however. All ACQ times are based on GALEX NUV mags, but assuming flux is only half
that cataloged (-0.75 mags) to account for any variability in souce.
Observing strategy based largely on experience with C20 COS program -- please let me know if there are changes I should have considered!1386612810----- Attempting Submission 1 (Fri Jul 11 19:26:55 GMT 2014) -----Two CENWAVES are included for every object, 1291 & 1327, to cover the inter-chip gap, and to provide
more 'FP-SPLIT' between each exposures. Each CENWAVE has at least 2 FP-POS, but for single orbit
visits, the grating change between FP-POS takes a significant fraction of the exposure time, so only
2 or 3 FP-POS positions have been used. The S/N of each exposure is modest, so FP-POS's aren't
crucial for reducing fixed-pattern noise. We recognize, however, that they are important for removing
gain-sag effects, and assume that the combination of 2 or 3 FP-POS, and two CENWAVE settings, will
be enough to mitigate gain-sag features.Baryon Structures Around Nearby Galaxies: Using an Edge-On Disk to Assess Inflow/Outflow ModelsWe propose observing 6 QSOs whose sightlines pass through the halo of the highly inclined galaxy NGC 3510 at impact parameters of 62-139 kpc. This galaxy has the highest available surface density of UV-bright QSOs behind high-inclination spirals in the nearby Universe. Our principal goal is to use the projected positions and kinematics of gas clouds seen in absorption towards the QSOs in conjunction with the high inclination of the galaxy to differentiate between gas flowing into the galaxy from intergalactic medium filaments ("cold-flow" accretion), and gas flowing out of the galaxy from galactic winds. We will search primarily for Lyman-alpha, SiIII, and SiIV absorption from gas in the galactic halo, as well as NV from hot gas, and any other lower ionization species. These data will answer the basic questions of how absorber column density, covering fraction, and temperature all decline with impact parameter. More importantly, the data will show whether gas is found preferentially along the major or minor axis of the galaxy, and whether absorption line velocities conform to those expected from inflow or outflow models. NGC 3510 is undergoing a recent burst of star formation, and is likely at a young stage of its evolution. Our observations will address whether the current paradigm that has QSO absorption line systems arising primarily from star-forming galaxies holds when a single galactic halo is probed along multiple sightlines.Our aim is to use the G130M grating of COS to search for absorption lines from gas in the halo of NGC3510, towards 6 background UV probes. Exposures towards individual sightlines are split into two halves with different central wavelengths (1291 and 1327A) in order to cover the gap in the COS detectors. For each central wavelength, multiple FP-POS positions are used. All targets have known GALEX fluxes. We expect to obtain a S/N of at least 10 per resolution element in the data.QUASAR ABSORPTION LINES AND IGMDefaultfalsetruefalsefalsefalseSUPPORTEDGALAXYQSOQUASARJ2000J2000GALEX FUV = 69 micro-Jy, or 19.1 mag; sdss g=18.24GALAXYQSOQUASARJ2000J2000GALEX FUV = 61 micro-Jy, or 19.5 mag; sdss g=18.14GALAXYLINERNLRSTARBURSTgalaxy is resolved in SDSS images; fluxes are integrated over sourceJ2000J2000GALEX FUV = 219 micro-Jy, or 18.1 mag; sdss g=16.68GALAXYQSOQUASARJ2000J2000GALEX FUV = 79 micro-Jy, or 19.0 mag; sdss g=18.94GALAXYQSOQUASARJ2000J2000GALEX FUV = 177 micro-Jy, or 17.5 mag; sdss g=17.30GALAXYQSOQUASARJ2000J2000GALEX FUV = 109 micro-Jy, or 18.8 mag; sdss g=17.90COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291/private/var/folders/q_/glfmvhmj0mq4qm_yvhs134lh0003lp/T/OPVisit1520134257569526670.xmlThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.All 4 FP-POS used; FP-POS=3 split over orbit(Tic-Visit
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