----- Attempting Submission 3 (Mon Jun 08 21:15:08 GMT 2009) ----- Phase II Proposal 11208 (11208.apt) successfully submitted. ----- Attempting Submission 4 (Tue Jun 09 22:26:15 GMT 2009) ----- Expected error. The co-evolution of spheroids and black holes in the last six billion years The masses of giant black holes are correlated with the luminosities, masses, and velocity dispersions of the bulges of their host galaxies. This empirical correlation of phenomena on widely different scales (from pcs to kpcs) suggests that the formation and evolution of galaxies and central black holes are closely linked. In Cycle 13, we have started a campaign to map directly the co-evolution of spheroids and black-holes by measuring in observationally favorable redshift windows the empirical correlations connecting their properties. By focusing on Seyfert 1s, where the nucleus and the stars contribute comparable fractions of total light, black hole mass and bulge dispersion are obtained from Keck spectroscopy. HST is required for accurate measurement of the non stellar AGN continuum, the morphology of the galaxy, and the structural parameters of the bulge. The results at z=0.36 indicate a surprisingly fast evolution of bulges in the past 4 Gyrs (significant at the 95%CL), in the sense that bulges were significantly smaller for a given black hole mass. Also, the large fraction of mergers and disturbed galaxies (4+2 out of 20) identifies gas-rich mergers as the mechanisms responsible for bulge-growth. Going to higher redshift -- where evolutionary trends should be stronger -- is needed to confirm these tantalizing results. We propose therefore to push our investigation to the next suitable redshift window z=0.57 (lookback-time 6 Gyrs). Fifteen objects are the minimum number required to map the evolution of the empirical correlations between bulge properties and black-hole mass, and to achieve a conclusive detection of evolution (>99%CL).
Our goal is to obtain high resolution photometry of a sample of 15 Seyfert 1s at z=0.57+-0.01 for which central black hole masses and bulge velocity dispersions are obtained from the ground. We need to determine the luminosity of the bulge and of the central point source, in order to extend our measurement of the M-L and M-\sigma relationships by 50\% in lookback time. We aim to measure bulge L with accuracy better than 0.2 dex, i.e. small with respect to the intrinsic uncertainty on the black hole mass (0.4 dex) from virial mass estimates. Measuring the nuclear luminosity to 20\% is needed to obtain unbiased estimates of the broad line region, and hence of the black hole mass. In addition, we will also derive effective radii (Re) and effective surface brightnesses (SBe) for the bulges, in order to derive their dynamical masses (sigma^2 Re) and probe the evolution of relationships involving more than one variable. Strategy The following strategy is based on our previous successful experience (Cycle 13). Camera. NIC-2 on NICMOS is the camera of choice, providing superior sensitivity to the NIC-1 camera at the low surface brightness levels needed to do bulge/disk decomposition, and better PSF sampling than NIC-3. PSF sampling will be further improved by obtaining dithered exposures with semi-integer pixel offsets (4 positions per pixel). This will also enable robust cosmic ray/defects removal. Note that the contrast between the central point source and the host galaxy in our sample is far more favorable than in other HST studies of QSOs hosts, where the AGN typically outshines the galaxy by a factor of 10 or more. Furthermore going to longer wavelength improves the contrast, since the host is redder than the nucleus. Therefore, in our case the modelling of the wings of the PSF is not nearly as crucial to obtain accurate parameters for the host galaxy. The residual PSF related uncertainties are estimated as described below. Filter. To minimize the size of the PSF, and preserving high sensitivity, we select the F110W filter. This filter is close in wavelength to the rest frame 5100\AA\ continuum -- used to estimate the size of the broad line region. Exposure time. The depth of the observations is chosen to obtain data of comparable quality to the ones we have obtained at z=0.36, which is adequate to meet our goals. Based on our previous extensive experience with structural parameters of distant bulges and AGN (e.g. Hunt et al.\ 1999; Treu et al. 2001), and confirmed by our study from Cycle 13 data (T07), the limiting factor is the signal to noise at the relatively low surface brightness typical of the disk and the outer bulge, i.e. F775W~22 mag arcsec^-2 at z=0.36. The intrinsic spatial resolution differs slightly between z=0.36 and z=0.57, but in any case is sufficient to resolve typical bulges (effective diameter 6~kpc) with NICMOS, even taking into account the slightly larger PSF at F110W than at F775W. Given cosmological dimming, we expect the surface brightness of our sources at z=0.57 to be fainter than that of those at z=0.36 by a factor (1.36/1.57)^4~0.56, corresponding to 0.6 mags arcsec^{-2}. Using a range of spectral energy distributions for the stellar and nuclear component we estimate that F775W~22 mag arcsec^{-2} at z=0.36, corresponds to F110W~21.3 (Vega) at z=0.57. According to the NICMOS ETC, 4133s are needed in order to obtain a signal-to-noise ratio of 10 per NIC2 pixel at this surface brightness. The same exposures will image the central point source at S/N>200, allowing for accurate determination of its luminosity, and the wings of the PSF. This is somewhat better than we obtained at cycle 13 (S/N=10 per 2x2 ACS pixel) to compensate for the larger amount of defects on the NICMOS detectors as compared to ACS. The exposure time corresponds to two orbits per object, including overhead. We will obtain our data in four separate pointings dithered by semi-integer pixels to help sampling the PSF and removing defects. 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CASM was run in Phase II mode. /tmp/OPVisit31291.xml 1218701736000 257.5887553370594 (Tic-Visit :proposal-id 11208 :visit-id "09" :proposal-version -1 :trans-version "20090130" :date "09-Jun-2009 15:23:40.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "23" :si-bright-earth-limb-angle 20.0 :data-volume 88336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11208 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11208 :visit-id "09" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2660 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3132 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11208 :visit-id "09" :orbit-number 2 :pcs-time 355 :si-vis-utilization 2634 :al-overhead-at-end 0 :internal-dur-at-end 136 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3132 :pcs-gap 0 ) true 2 0 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /tmp/OPVisit31292.xml 1210321307000 191.19134492703415 (Tic-Visit :proposal-id 11208 :visit-id "10" :proposal-version -1 :trans-version "20090130" :date "09-Jun-2009 15:23:41.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "23" :si-bright-earth-limb-angle 20.0 :data-volume 88336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11208 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11208 :visit-id "10" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2660 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11208 :visit-id "10" :orbit-number 2 :pcs-time 355 :si-vis-utilization 2634 :al-overhead-at-end 0 :internal-dur-at-end 136 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) true 2 0 The scheduling data was generated by CASM 17.2. 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