Revised submission ----- Attempting Submission 1 (Thu Jul 03 17:30:16 GMT 2008) ----- ----- Attempting Submission 2 (Tue Oct 13 21:12:28 GMT 2009) ----- Assigned ID: 527 ----- Attempting Submission 1 (Fri Mar 07 19:52:43 GMT 2008) ----- Phase I Proposal 527 (hostgalaxies.apt) successfully submitted. The radius-luminosity (R-L) relationship is currently the fundamental basis for all techniques used to estimate black hole masses in AGNs, in both the nearby and distant universe. However, the current R-L relationship is based on 34 objects that cover a limited range in black hole mass and luminosity. To improve our understanding of black hole growth and evolution, the R-L relationship must be extended to cover a broader range of black hole masses using the technique known as reverberation mapping. To this end, we have been awarded an unprecedented 64 nights on the Lick Observatory 3-m telescope between March 24 and May 31, 2008, to spectroscopically monitor 12 AGNs in order to measure their black hole masses. To properly determine the luminosities of these 12 AGNs, we must correct them for their host-galaxy starlight contributions using high-resolution images. Previous work by Bentz et al. (2006) has shown that the starlight correction to AGN luminosity measurements is an essential component to interpreting the R-L relationship. The correction will be substantial for each of the 12 sources we will monitor, as the AGNs are relatively faint and embedded in nearby, bright galaxies. Starlight corrections are not possible with ground-based images, as the PSF and bulge contributions become indistinguishable under typical seeing conditions, and adaptive optics are not yet operational in the spectral range where the corrections are needed. In addition, spectral decompositions are very model-dependent and are limited by the degree of accuracy to which we understand emission processes and stellar populations in galaxies. Without correcting for starlight, we will be unable to apply the results of our Spring 2008 campaign to the body of knowledge from previous reverberation mapping work. Therefore, we propose to obtain high resolution, high dynamic range images of the host galaxies of the 12 AGNs in our ground-based monitoring sample, as well as one white dwarf which will be used as a PSF model.

We propose to obtain Wide Field Camera 3 UVIS images of the host-galaxies of 12 nearby, low-luminosity AGNs through the F547M (medium-band V ) filter. Each object will only require a single orbit. In addition, we also propose to image the white dwarf EGGR 102 with the same instrument configuration, in order to create a PSF model with a very high dynamic range. The proposed images will allow us to determine the host-galaxy starlight contribution to the optical luminosity measured from the spectrum of each AGN. The F547M filter ensures that we will have a continuum- only image of each host galaxy in a flat part of the spectrum, which will facilitate the correction of the continuum luminosity at 5100A. Removing the starlight contribution to the luminosity of each of these 12 objects is an essential component of the ground-based reverberation-mapping study we are carrying out at Lick Observatory during Spring 2008. Due to our experiences with the previous HST programs to correct AGN luminosities (GO 9851, 10516, 10833), we can slightly improve upon the methods that were employed. In previous programs, starlight corrections were determined using the Advanced Camera for Surveys High Resolution Channel (ACS HRC) through the F550M filter. The main consideration in choosing the HRC over the Wide Field Channel was the smaller pixel size of the HRC, allowing a more accurate determination of the AGN PSF contribution to the surface brightness profile of each galaxy. However, for nearby galaxies, the small field of view of the HRC turned out to cause two issues – namely, that the sky background was not well constrained for galaxies that filled the entire field of view, and the scalelengths of some galaxy components were on the order of the size of the detector. The first has the effect of causing instabilities in the Sersic index for small-scale components in the center of the galaxy near the AGN PSF, and the second causes difficulties in disentangling the disk component from distinct inner-galaxy structures. In choosing WFC3 over ACS HRC, we will be making a slight sacrifice in our ability to determine the PSF contribution to a high degree of accuracy, as WFC3 has slightly larger pixels (0.04′′ vs. 0.025′′). However, we will be gaining the higher sensitivity of WFC3 as well as the larger field of view necessary for the accurate determination of both the sky level and extended host-galaxy features in the images of these nearby objects. One of the main considerations in this project is to maximize the dynamic range achieved by replacing the saturated pixels in deeper exposures with pixels from shallower, unsaturated exposures that are scaled by the exposure time ratio. This method was shown to work extremely well in the previous programs. In those cases, dithering was not employed between images, as the PSF is known to change shape at different locations on the detector. However, dithering has many useful features, including facilitating the rejection of cosmic rays and detector artifacts (such as transient warm pixels), as well as filling any gaps between detectors that would otherwise result in a loss of information. Therefore, we will use one of the standard 2-point dithering patterns for our program with WFC3, yet in a slightly different way, as explained below. For the brightest object in our sample, the WFC3 exposure time calculator estimate a time to saturation of 47s. This is actually a lower limit on the time to saturation, as it assumes that all of the flux in the spectrum is due to the AGN point source, which we know is not the case for any of these objects. In order to obtain the dynamic range necessary to decompose the host galaxy and AGN surface brightness profiles, we must properly replace saturated pixels in deep exposures using shallower, unsaturated exposures. To this end, we will take two sets of exposures separated by a dithering maneuver, where each set of exposures will be graduated in time, for example 30s, 300s, and 690s. The exposures will be ordered such that two full parallel buffer dumps (which require 664 s each to transfer two full images to the SSR) will occur during the long exposures and will not create any additional overheads. For 11 of our 12 AGN targets, the FOV provided by a single WFC3 chip will be sufficient for measuring the structure of the host galaxy. For these objects, the UVIS1 aperture will be used for centering the galaxy, and the WFC3-UVIS-DITHER-LINE pattern with the standard dither size and orientation will be used. Three of these objects are somewhat elongated, so their orientations have been constrained to ensure that they will fit within the FOV provided by a single chip. The 12th AGN host galaxy (NGC 6814) is more spatially extended than the others, so we have elected to use the UVIS aperture with the WFC3-UVIS-MOST-DITH-LINE pattern with the following modifications to the defaults for this pattern: 2 pointings rather than 3 and no subpattern. The default orientation and offset will allow us to dither across the gap, thereby ensuring that we do not lose any information in the host galaxy structure. In a similar manner, we propose to image EGGR 102, an isolated white dwarf with V = 12.8 to create a high-dynamic range PSF model. Its moderate apparent brightness makes EGGR 102 a suitable star to use with HST imaging, as it will not saturate in short exposures but also requires little time to achieve a high S/N. In addition, its spectral shape in the optical is similar to the spectral shape of AGNs. EGGR 102 has been used extensively as a PSF model for HST imaging (e.g., McLure et al. 1999), as it more accurately fits both the bright core and the extended PSF wings than do TinyTim models of the PSF. We will again use two sets of graduated exposures to maximize the dynamic range. The WFC3 exposure time calculator estimates a time to saturation of 6.8 s for EGGR 102. We will take exposures that are 4s, 40s, and 600s in length. In this case, two of the buffer dumps will be in serial with the exposures. Two full buffer dumps of 664 s each must occur within the unrestricted visibility time of the object. The exposures for EGGR 102 will be centered with the UVIS1 aperture, and the WFC3-UVIS-DITHER-LINE pattern will be used, such that the pointings and dithers match the majority of the observations within this proposal. As a final note, WFC3 is the best choice for this project, because of its high sensitivity, wide field of view, and relatively small pixels. However, should WFC3 not be available for use, the observations proposed here may be successfully carried out with the same number of requested orbits using ACS WFC, or even WFPC2, if necessary. AGN/QUASARS 12 false 0.0 0.0 false false false false false false SUPPORTED GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. g= 15.8 J2000 10 25 31.3000 +51 40 35.00 J2000 GALAXY SEYFERT g=15.7 J2000 11 18 57.7000 +58 03 24.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. g=16.0 J2000 11 25 36.2000 +54 22 57.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. g= 14.8 J2000 12 01 14.3000 -03 40 41.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. g=15.4 J2000 12 17 55.0000 +58 39 35.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=13.7 J2000 12 18 26.5000 +29 48 46.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=14.27 J2000 12 52 12.4000 -13 24 53.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=14.6 J2000 13 17 3.4000 -02 15 41.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=13.9 J2000 13 35 53.8000 -34 17 44.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. g=15.1 J2000 15 35 52.3000 +57 54 9.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=15.20 J2000 16 08 36.4000 +12 19 51.00 J2000 GALAXY SEYFERT This object was generated by the targetselector and retrieved from the NED database. B=11.9 J2000 19 42 40.6000 -10 19 25.00 J2000 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. white dwarf J2000 13 38 50.4743 +70 17 7.62 J2000 WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F547M POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 1 false POS-TARG DITHER DITHER 2 4.0 WFC3-UVIS-MOS-DITH-LINE false true 0.119 2 85.754 POS-TARG WFC3-UVIS-MOS-DITH-LINE 33.606 2 false The scheduling data was generated by CASM 17.2. 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