0Assigned ID: 833
----- Attempting Submission 1 (Fri Apr 08 21:07:10 GMT 2016) -----
HST Phase I Proposal 833 (all.apt) successfully submitted.
Receipt: # 833-10POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp filters as central wavelengths & transmission efficiencies vary within the apertures.0----- Attempting Submission 1 (Thu Jul 21 13:37:40 GMT 2016) -----there are warning regarding the use of pos targs with LRFs.
But the dither is needed to get clean images and the offsets are small.Imaging BALQSO outflows: a critical step in assessing AGN feedbackQuasar outflows are increasingly invoked as a major contributor to the formation and evolution of supermassive black holes, their host galaxies, the surrounding IGM, and cluster cooling flows. Using spectral data, our group has determined the distance of the outflows from the central source in a sample of objects. Some of these outflows are found to be at ~10 kpc from the nucleus and thus can be imaged directly using ACS at redshifts 1-3. We therefore propose to obtain the first ever imaging of BALQSO outflows at high redshifts. This project will uncover the spatial geometry of the outflows, which is the final piece needed to derive their kinetic luminosities, and therefore a direct measurement of their importance to AGN feedback processes. We will image each object with filters corresponding to deep absorption troughs. Such configuration will detect light scattered from the same ionic transitions that cause the trough, which are outflowing in directions other than our line of sight. The natural coronagraph supplied by the absorption trough will greatly reduce the flux of the quasar in that narrow spectral region, facilitating the detection of the outflow. To distinguish between the outflow features and the underlying galaxy we will use two narrow band filters at wavelengths of deep troughs as well as a broader band filter that does not cover significant troughs and therefore should show only the underlying galaxy and not the outflowing material.Imaging outflows. For the narrow band imaging at the wavelength of the chosen
troughs, we will use the Linear Ramp Filter (LRF) on ACS/WFC, which has a continuous
tunable central wavelength ranging from about 3700 Ang to 11000 Ang. The full width at half
maximum of the filter is dependent upon the location of the center of the bandpass via
/ = 0.02. For SDSS J0318-0600, Fig. 2 shows the SDSS spectrum and the coverage of
the LRF for the Civ (observed at about 4500 Ang and Al iii trough (observed at about 5450 Ang). As
explained on page 2, we assume that the outflow will scatter ~10% of the light from the
quasar continuum level adjacent to the Civ and Al iii troughs into our line of sight (11 and
16 x10^17 ergs s^-1 cm$-2 Ang^-1, respectively). With residual flux of 1.4 and 4x10^17 ergs s^-1
cm^-2 Ang^-1, respectively, these absorption troughs provide a "natural coronagraph"
for imaging the outflows by suppressing the quasar glare by a factor of 4 - 8.
We estimate the surface brightness of the wind by assuming uniform emission over 1 arcsec^2
for the scattered fluxes. In the LRF images, read noise is comparable to (or larger than) the
source noise and sky background noise. We will take two exposures per orbit with position
offsets to create a 4-point dither over the course of the total exposure. This will allow us to
remove cosmic rays and CCD imperfections. We require an average S/N=5 per 2x2 pixels
(a resolution downgraded to this level remains sufficient for our science goal) in both the
Civ and the Al iii features in order to deal with expected image complexity, due to e.g.,
non-uniformity in the outflow surface brightness, wind sizes larger than 1 arcsec^2, confusion
by features in the host galaxy and nuclear PSF residuals. Using the on-line ACS ETC we
calculate the exposure time required to achieve a S/N=5 per 2x2 pixels in the Al iii and
Civ lines.
Imaging host galaxies. We will use the wide-band filter F625W to image the host
galaxies in a trough-free continuum region redward of the Al iii trough (Fig. 3). The
feasibility of such imaging and PSF subtraction involved has been demonstrated for z=2
galaxies hosting quasars (Floyd et al. 2013). Taking SDSS J0318-0600 as an example, the
quasar continuum flux in this region is ~ 21x10^-17 ergs s^-1 cm^-2 Ang^-1 , and we expect the host
galaxy to be ~ 50 times fainter. Requiring a S/N=5 per 2x2 pixels, this flux level necessitates
an exposure time of 2.2 kilo-seconds (ks) for a source extended over 4 arcsec^2. Thus, the
total exposure time for the two narrow band filters and the wide bandpass filter is 8.7 ks. A
typical HST orbit includes 6 minutes for guide star acquisition (5 for re-acquisition), 4 min
overhead (2.5 min for subsequent exposures), which leaves about 40 minutes observing time.
Therefore, the total observing time of 8.7 ks translates to 4 HST orbits for SDSS J0318-0600.
Table 1 shows our second target, with a similar observing method of 2 absorption troughs
observed with the LRFs and the continuum observed through a wide filter. We will calibrate
the ACS/LRFs using flat fields interpolated from non-LRF filters close in wavelength as
described by Tremblay et al. (2009).
PSF observation. Past experience has demonstrated that the success of modeling the
QSO/host combination hinges on obtaining an accurate empirical PSF (e.g., McLure et al. 1999,
Floyd et al. 2004, 2013). As in those programs, we need to obtain both unsaturated and very
deep images of a star using the same filter and positioned on the same part of the detector as our
target QSOs. We will observe the HST standard star GRW+70D5824 which has colors similar to
those of a typical QSO over the wavelength intervals of interest. We will perform the a 2-point
dither pattern to attain a clean and well-sampled PSF. These PSF observations will be carried out
for the bluers of the LRFs for each target and the broad band filter. the obtained PSF will be at the same location on the
chip as our targets. Because of the large number of short exposures, overhead is significant including buffer dumps and additional GS acqs.Massive Black Holes and their HostsGalaxies12falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYBLRQUASARWINDThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000r = 17.6GALAXYBLRQUASARWINDThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000r = 17.7CALIBRATIONPOINT SPREAD FUNCTIONThis object was generated by the targetselector and retrieved from the GSC 2.3 database.This object was generated by the targetselector and retrieved from the GSC 2.3 database.J2000J2000ACS/WFCRampFilterNoNoFR462NACS/WFCRampFilterNoNoFR551NACS/WFCImagingNoNoF625WACS/WFCRampFilterNoNoFR423NACS/WFCRampFilterNoNoFR462NACS/WFCImagingNoNoF625WACS/WFCRampFilterNoNoFR462NACS/WFCRampFilterNoNoFR551NACS/WFCRampFilterNoNoFR423NACS/WFCImagingNoNoF625WPOS-TARGDITHER0.262LINE0.192falsefalse68.14418.39ACS-WFC-DITHER-BOX1falsePOS-TARGDITHER3.034LINEfalsefalse285.29ACS-WFC-DITHER-LINE2falseC:\Users\Administrator\Documents\Proposals\HST\2016\BALQSO\PhaseII\OP-cache\HST-Cy24_PHII-v01.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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