first submit April 6
second submit April 8, updated figures and text
third submit April 8, updated abstract583138744Assigned ID: 176
----- Attempting Submission 1 (Wed Apr 06 23:07:44 GMT 2016) -----
HST Phase I Proposal 176 (straka_blindqso_24.apt) successfully submitted.
Receipt: # 176-1
----- Attempting Submission 2 (Fri Apr 08 17:48:59 GMT 2016) -----
HST Phase I Proposal 176 (straka_blindqso_24.apt) successfully submitted.
Receipt: # 176-2
----- Attempting Submission 3 (Fri Apr 08 21:09:23 GMT 2016) -----July 20: First submission.1317483910----- Attempting Submission 1 (Wed Jul 20 10:10:52 GMT 2016) -----
HST Phase II Proposal 14660 (hst24_blindqso_phaseII.apt) successfully submitted.
Receipt: # 14660-1Morphology and Orientation of QSO Absorber Host Galaxies at z<1.5 Detected with VLT/MUSE1/stGas accretion and galactic winds are two of the most important, but also most poorly understood ingredients of models for the evolution of galaxies. QSO absorption line spectroscopy enables us to study the gas around galaxies, nearly all of which is far too diffuse to see in emission. This unbiased method allows us to probe even low-mass galaxies, which dominate the galaxy number counts and are likely to be closest to absorbers, and is ideal for studying metal-enriched gas in galaxy outflows or inflows. Because outflowing gas is thought to be most prominent in the directions perpendicular to the disk, while infalling gas may be strongest in the plane of the disk, knowing the orientiation of the galaxy relative to the line of sight of the QSO is critical. However, the usefulness of absorption line studies is generally limited by the small number of galaxies at close impact parameters to the QSO line of sight for which redshifts are available. To remedy this, we have successfully used the MUSE integral field unit on the Very Large Telescope to detect and obtain redshifts for hundreds of galaxies < 250 kpc from the sight lines to 16 luminous QSOs at 0.4<z<1.5 for which high-quality archival HST/COS data (~200 orbits) is available. While MUSE is highly efficient at detecting and localizing galaxies close to QSO sight lines, the image quality is insufficient to determine the morphologies and orientations of the detected objects. We propose to use ACS/WFC to obtain high-resolution images of our MUSE fields in order to determine the relation between QSO absorbers (including HI, OVI, SiIV, CIV, NV, and MgII), and galaxy position angle and morphology.We request a total of 6 orbits for this program, covering 7 fields total, with two of these fields being obtained in one ACS pointing. The objects PB6291 and Q0107-0235 are QSOs within 1arcmin of one another on the sky, and therefore we require only a single pointing to cover both. For these two objects (PB6291 and Q0107-0235), we must arrange the orientation at 32 degrees in order to fit both MUSE fields of view within the ACS field of view without overlapping the chip gap. We account for dithering in this fit. This heavily restricts the window in which this visit can be completed.
Each of the 7 QSOs at 0.4<z(QSO)<1.5 requested here will be observed for one orbit with ACS/WFC in the F814W filter. The F814W filter is chosen to probe the optical continuum and for its high sensitivity of the galaxies in the range $z<1.5$, which are detected by MUSE in optical nebular emission (one or more of H-alpha, [O III](4959,5007), and [O II](3727). The approximate transmission range of this filter is 6625A-9495A, for which the corresponding rest wavelength range is 6022A-8630A for a z~0.1 galaxy and 3312A-4747A for a z=1 galaxy. These galaxies are correlated with hydrogen and metal absorption line systems detected in high-quality UV spectra of the QSOs with HST/COS (R~18,000, S/N=10-20), particularly HI, C IV, O VI, and Si IV.
We use the ACS ETC to determine the S/N of the faintest objects we will detect in a single orbit (~2400 sec integration time) in the F814W band, based on magnitudes measured in the available archival fields. A spiral type galaxy at z~0.1 with an I-band magnitude of 26 spanning 2 arcsec in diameter can be detected in a single orbit at a S/N~6, while the same galaxy at z~1 can be detected in a single orbit at a S/N~8. These numbers are supported by the detections we have already made in the archival fields.
In a single orbit, we will obtain four images with a standard four point line dither. This offset will allow us to eliminate detector artifacts and cosmic rays in addition to offering a better sampling of the ACS chip gap (minimum of three exposures at each pixel with this pattern). The MUSE field of view is 1 arcmin x 1 arcmin. Therefore, we will position the QSO within the ACS field of view (3 arcmin x 3 arcmin) at the WFC1 focal point.
We propose standard observations as laid out in the ACS handbook. The single orbit observations for a visibility time of 54 minutes will proceed as follows:
Guide star acquisition (6 minutes) - WFC overhead for the first exposure (4 minutes) - Spacecraft slew (0.5 minutes) - First science exposure (20 minutes) - WFC overhead for subsequent science exposure (2.5 minutes) - Second science exposure (21 minutes)
This is a total on-source integration time of 41 minutes, and a total orbit time of 54 minutes.GalaxiesIntergalactic Medium and Cosmology12falsefalsefalsefalsefalsefalseSUPPORTEDISMABSORPTION LINE SYSTEM - EXTRAGALACTICIGMSTAR FORMING REGIONJ2000J2000z=0.631ISMABSORPTION LINE SYSTEM - EXTRAGALACTICIGMSTAR FORMING REGIONJ2000J2000z=0.669ISMABSORPTION LINE SYSTEM - EXTRAGALACTICIGMSTAR FORMING REGIONPB6291Q0107-0235J2000J2000z=0.956ISMABSORPTION LINE SYSTEM - EXTRAGALACTICIGMSTAR FORMING REGIONJ2000J2000z=1.234ISMABSORPTION LINE SYSTEM - EXTRAGALACTICIGMSTAR FORMING REGIONJ2000J2000z=1.128ACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF814WPOS-TARGDITHER2.994LINEfalsefalse485.27ACS-WFC-DITHER-LINE2falseThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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