0Assigned ID: 1115
----- Attempting Submission 1 (Fri Apr 07 23:29:26 GMT 2017) -----FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserThis version includes orientation requirements for visit 7, to avoid bleeding and diffraction spikes from
nearby bright star.-1305786616----- Attempting Submission 1 (Thu Jul 20 16:13:00 GMT 2017) -----
----- Attempting Submission 2 (Tue Sep 05 22:39:57 GMT 2017) -----
----- Attempting Submission 3 (Fri Sep 08 15:07:25 GMT 2017) -----We have specified post flash levels so as to reach a background of 15 e-/pixel, as
recommended by the contact scientist.Revealing the circum-nuclear torus: HST imaging of active galaxies observed during a Spitzer reverberation mapping campaignWe are currently analyzing data from a recently completed ~2.5 year
monitoring campaign, during which 12 low-redshift broad-line AGN were
observed at 3.6 and 4.5 microns with the Spitzer Space Telescope, with
supporting optical observations from several ground-based telescopes.
The objective is to "reverberation map" the circumnuclear torus of
dusty molecular gas that is a key element of the AGN unification scheme;
that is, infer its size and structure from the temporal
response of the dusty torus IR emission to changes in the AGN optical
luminosity. However, a critical unknown is the contribution of
host galaxy starlight to the measured optical luminosity.
The objective of this proposal is to obtain WFC3/UVIS images of 8 of our
Spitzer galaxies in order to decompose the host galaxy and AGN
contributions within the photometric apertures used for the monitoring
campaign. Removing the host galaxy contribution is an
essential step in the analysis and interpretation of this unique
time-series dataset, since it will allow the intrinsic luminosity and
variability amplitude of the AGN optical continuum to be determined.
This, in turn, will yield more precise measurements of the optical-IR
lags and better estimates of the dust sublimation radius and undiluted
optical light curves. These are essential for our torus reverberation
simulations, since the amplitude of the luminosity variations can
strongly modify the torus response through the effects of dust sublimation.We propose to obtain WFC3/UVIS images of 8 nearby active galaxies observed during our Spitzer Space Telescope torus reverberation-mapping campaign, using the F621M filter. We will require a single orbit for each of the 8 targets.
The images will allow us to determine the constant host galaxy starlight contribution to the measured optical flux. For the redshift range spanned by our targets, the F621M filter samples the spectrum in a region which is free of strong emission lines, between the strong Hbeta and [OIII]4959, 5007 lines to the blue and Halpha + [NII]6548,83 lines to red, ensuring that the images will be dominated by continuum light. It is important, in particular, that the variable broad Halpha and Hbeta lines are excluded so that we can recover the constant host galaxy contribution. Note that after reviewing the filter pass bands, it was decided that F621M is a better choice for our targets than the F547M filter, which was selected for the phase I proposal.
As relatively large photometric apertures (5'') were necessarily used for many of our ground-based measurements (with typical seeing ~1'' and for some instruments, low angular resolution), the starlight contribution to the measured optical fluxes is substantial for all 8 AGNs, but it is not possible to accurately quantify this contribution using our existing data. Removing this host galaxy contribution to the measured fluxes is an essential step in the analysis and interpretation of this unique time-series dataset, since it will allow the intrinsic luminosity and variability amplitude of the AGN optical continuum to be determined. Our goal is to measure the integrated host starlight flux to ~10%, which requires the high-resolution and stable PSF of WFC3/UVIS images.
The observing strategy and analysis methodology adopted here follows that of Bentz et al. (2013, ApJ 767, 149; GO-11662). We will maximize the dynamic range of the data by obtaining two sequences of 3 exposures of approximately 40s, 400s and 800s for each of our targets. The short (~40s) exposure is below the saturation point for all our targets as estimated by the ETC, while the 400s and 800s exposures will maximize the S/N of the host galaxy and the wings of the nuclear PSF. We will replace saturated pixels in and around the nucleus in the long exposure images using corresponding pixels from the shallower, unsaturated exposures, scaling the counts by the exposure time ratio. We will use a 2-point dither pattern to improve the WFC3 point spread function (PSF), with a sequence of 3 exposures being executed at each dither position. The short exposure times differ slightly between objects to ensure that the nuclear point sources in the brightest objects will not saturate. The target having the brightest nucleus is M876, for which B ~ 14.4. The ETC indicates a time to saturation of 49s. This is a lower limit, since we assumed that the nucleus emits all the light. However, to allow for possible variability we limited the exposure to 30s. We use 40 - 44s exposures for the remaining targets, which have B ~ 16-17.
The ETC indicates that the short, medium and long exposures require different post-flash levels to mitigate CTE losses. We therefore implement the dither pattern as two sets of individual exposures, with the second set having a POS-TARG offset of 0.099,0.106, equivalent to the standard WFC3 UVIS 2-point line dither pattern, We will use the UVIS2 aperture. As all our targets comfortably fit into the CCD 2 field of view, it is not necessary to perform a larger dither to fill in the chip gap. The exposures have been ordered so that the 668s and 352s buffer dumps occur in parallel with long and intermediate exposures respectively.
On the recommendation of the contact scientist, we have adjusted the post flash level for each exposure so as to reach a background level of 15 electrons/pix to reduce CTE losses.
The GALFIT 2-D image decomposition software (Peng et al. 2002, 2010) will be used to model the surface brightness distribution of each target, in order to separate the host galaxy and AGN components. We will use TinyTim (Krist, 1993) to model the unresolved AGN PSF. Each target image also contains 2-4 field stars comparable in brightness to the AGN. These will be used to estimate color corrections and can also be combined to construct an alternative PSF model. The end product will be an intrinsic, host galaxy subtracted, light curve for each of the AGN in our sample.Massive Black Holes And Their Host Galaxies6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYNUCLEUSSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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