----- Submission 1 (Thu May 01 20:10:49 GMT 2003) ----- ----- Submission 2 (Fri Jun 06 15:21:27 GMT 2003) ----- The proposal runs through fine, with just warning messages. ----- Submission 1 (Fri Jan 24 12:29:26 EST 2003) ----- Assigned ID: 732 Successfully submitted: Fri Jan 24 12:29:44 EST 2003 The Upper End of the Supermassive Black Hole Mass Function: Pushing the 10 Billion Solar Mass Limit. In 1994, HST provided the first secure detection of a supermassive black hole (SBH) in a galactic nucleus. The galaxy was M87, the black hole almost 4 billion solar masses. Since then, two dozen additional SBH detections have been the outcome of the several hundred orbits of HST time devoted to this cause. Yet, M87's black hole is still the most massive known, and in only two other galaxies have SBHs in excess of a billion solar masses been detected. The aim of this proposal is to characterize the high mass end of the local SBH mass function. Four brightest cluster galaxies have been carefully selected. Their large masses, luminosites and stellar velocity dispersions, as well as their having a merging history which is unmatched by galaxies in less crowded environments, make these galaxies the most promising hosts of the most massive SBHs in the local Universe. It is in the high mass regime that the unavoidable link between the evolution of supermassive black holes and the hierarchical build-up of galaxies leaves its clearest signature. It is these galaxies that are expected to be the relicts of the most luminous high redshift quasars, those so spectacularly targeted by the Sloan Digital Sky Survey. Expanding (and extending) the high mass end of the local SBH mass function is the next obligatory step we need to take to improve our understanding of how SBHs, and their hosts, formed and evolved.
\noindent{\bf STIS Observations, 21 orbits.} For each galaxy, we will perform high-resolution spectroscopy of the H$\alpha$+[NII] emission lines at 3 slit positions, to measure the central ionized gas kinematics. Three of the four galaxies will be observed for a total of six orbits each (2 orbits for each slit position), with the 52\sec$\times$0\Sec1E1 aperture. One galaxy, A3565-BCG, will be observed with the 52\sec$\times$0\Sec2 aperture for 3 orbits. The total number of orbits requested for spectroscopy is therefore 21. \vskip .2in \noindent{\it Grating selection.} We will use the G750M grating at the prime tilt $\lambda_{cen}=6768$ \AA. This covers the H$\alpha$+[NII] complex for all galaxies, and includes the [SII] doublet at $\lambda =6716,6731$ \AA. The FWHM of the spectral line-spread function will be of order 50 \kms~ for the 0\Sec2 slit, and 25 \kms~ for the 0\Sec1 slit. This is more than adequate for our purposes. \vskip .2in \noindent{\it Slit selection and position.} In order to produce unbiased mass measurements, it is imperative to use data which resolves the SBH sphere of influence (Merritt \& Ferrarese 2001b). This is the single most important consideration in selecting the slit width for our project. For each of the program galaxies, Figure 3 shows the SBH mass {\it versus} the diameter of the sphere of influence of the expected SBH. The SBH mass was estimated from the galaxy velocity dispersion (when available) or luminosity using the $\ms$ and $\ml$ correlations (Fig1). Based on these estimates, all of the galaxies {\it could} be observed with the 52\sec$\times$0\Sec2 slit. However, we {\it must} allow for the possibility that the SBH in these galaxies have smaller (or larger) masses than expected. Smaller masses, in particular, would obviously produce a proportionally smaller sphere of influence (for a given bulge stellar velocity dispersion). For this reason, we opt to use the smaller STIS aperture for all galaxies, with the exception A3565-BCG, whose central SBH would need to have been underestimated by a factor 5 for its sphere of influence to be unresolved by the 0\Sec2 wide slit. For each galaxy, the center and position angle of the major axis of the dust disk can be determined from the existing WFPC2 images (GO-8683). The STIS slit will be placed at three different positions, namely on the major axis of the dust disk, and on either side, displaced by plus/minus the slit width. This is a requirement in order to verify that the gas is indeed in Keplerian rotation in the SBH gravitational potential. \vskip .2in \noindent{\it Exposure times calculation and observing strategy}. Observed [NII]$\lambda6593$ line fluxes for the project galaxies are of order of a few$\times10^{-15}$ erg cm$^{-2}$ s$^{-1}$ \AA$^{-1}$ (Owen et al. 1995, Crawford et al. 1999). Based on previous experience (Ferrarese et al. 1996, Ferrarese \& Ford 1999), we require a S/N of 10 per resolution element at the peak of the [NII]$\lambda6593$ line, which is normally the brightest in the H$\alpha$+[NII] complex. According to the on-line STIS exposure time calculator, this can be achieved in 5000s and 2500s of integration with the 0\Sec1 and 0\Sec2 slits respectively. For each target, the first orbit will include the initial guide star acquisition (6m) and target acquisition (8m, see below). Assuming a 52m orbit, this leaves a total of 32m for one CR-SPLIT scientific exposure (6m overhead). A CCD fringe flat exposure will be performed during occultation if necessary. The overhead on any additional orbit on the same galaxy will be 5m for GS re-acquisition and 6m for each CR-split science exposure, leaving 41m for science observations. We therefore require a total of 1 orbit for each slit position for A3565-BCG (with the 0\Sec2 slit, three orbits total), and two orbits per slit position for all other galaxies (6 orbits per galaxy). Exposures at the same slit position but taken in consecutive orbits will be dithered by a few pixels in the spatial direction to allow for accurate removal of hot pixels and CCD defects. \vskip .2in \noindent{\it Target Acquisition} We will perform the target acquisition directly on the nucleus. The use of three adjacent slit positions allows us to by-pass the need of an acquisition peakup even for the 0\Sec1 slit (notice that this strategy was used successfully for GO-8236). The precise position of the slit aperture at the time of the observations will be recovered from the acquisition images. \vskip .2in \noindent{\bf ACS/HRC Observations, $B$ (F435W) and $r$ (F625W) bands, 4 orbits.} These observations, combined with the WFPC2/F814W data already existing in the HST archive, will be used to determine the optical depth of the dust (which strongly affects the surface brightness profiles in the inner 1\sec) and the stellar mass distribution near the nucleus. The latter is needed to build the dynamical models to fit the spectroscopic data (see below). The $r-$band (F625W) exposure is useful but not strictly necessary for this purpose, however it is needed as an off-band continuum image to derive a H$\alpha$+[NII] narrow band map of the ionized gas (see below). Exposure times were calculated using the on-line ACS ETC, given the surface brightness profile measured by Laine et al. (2002). Exposure times of 560s in F625W and 1800s in F435W will give S/N of 100 and 80 respectively. Adding a total of 13 minute overhead (6m for initial GS acquisition, and 3.5m for each set of CR-split exposures), each galaxy can be observed with both filters in one orbit (52m). \vskip .2in \noindent{\bf ACS/HRC Observations, H$\alpha$+[NII] narrow band, 4 orbits.} These observations are needed to characterize the morphology and spatial distribution of the line emission from the ionized gas associated with the nuclear dust disks. The observations will make use of the F656N ramp filter, centered at the wavelength corresponding to the redshifted H$\alpha$ emission in each galaxy (6630 \AA~to 6810 \AA). At these wavelengths, the filter has a $\sim$130 \AA~wide bandpass, covering not only H$\alpha$ but also the adjacent [NII] emission. As a continuum exposure we will use the F625W data described in the previous paragraph. The line emission is included in the F625W bandpass (1500 \AA~wide), but its contribution to the total transmitted flux is insignificant compared to that of the underlying stellar continuum. Color gradients between the F656N and F625W bandpass, which could affect the continuum subtraction, should be minimal in the innermost $1-2$\sec~were the line emission is expected to be concentrated, and can be modeled by constructing F814W-F625W-F435 color profiles. \vskip .2in \noindent{\bf Data analysis and modeling.} We have extensive experience of analyzing both ACS and STIS data, and the dataset proposed here should not present unexpected challenges. The dynamical modeling of the gas kinematics will be done following the procedure outlined in Ferrarese \& Ford (1999) and refined in Barth et al. (2001, see also van der Marel \& van den Bosch 1998). The gas kinematic will be interpreted by constructing axisymmetric models in which the gas and dust reside in a disk in the equatorial plane of the stellar body. The mass model will incorporate a central point mass (the SBH) and the stellar mass distribution. After accounting for dust obscuration (as outlined in Ferrarese et al. 1996 and Ferrarese \& Ford 1999), the ACS and WFPC2 surface brightness profiles will be deconvolved to give a luminosity density as a function of radius, the mass density follows once a mass-to-light ratio is chosen. The resulting velocity field is projected onto the plane of the disk - the inclination of the disk, as well as the SBH mass and the stellar M/L ratio, being free parameters in the models. Before comparing the model to the observations, the model velocity field is `observed' to simulate the actual parameters of the STIS observations. The line profiles will be weighted by the emission line surface brightness at each point in the disk, as derived from the F656N-F625W ACS/HRC images. As described in Barth et al. (2001), this step is important in order to assess whether irregularities in the measured velocity field are due to departures from Keplerian rotation (which would bias the SBH mass estimate), or simply to an inhomogeneous spatial distribution of the ionized gas. In addition, the effects of line broadening (produced by light passing through different parts of the slit), as well as instrumental broadening due to the telescope PSF and the finite slit width, will be accounted for. The SBH mass is determined by finding the model parameters that produce the best match to the observed velocity curves. GALAXIES 12 false 2 false false false SUPPORTED GALAXY ELLIPTICAL J2000 GALAXY ELLIPTICAL J2000 GALAXY ELLIPTICAL J2000 GALAXY ELLIPTICAL J2000 13 36 39.05 -33 57 58.0 J2000 STIS/CCD ACCUM Spectroscopic No STIS/CCD ACCUM 13 36 39.05 -33 57 58.0 J2000 ACS/HRC ACCUM Imaging No ACS/HRC ACCUM 13 36 39.05 -33 57 58.0 J2000 ACS/HRC ACCUM RampFilter No ACS/HRC ACCUM 23 24 20.1 +14 38 49.2 J2000 STIS/CCD ACCUM Spectroscopic No STIS/CCD ACCUM 23 24 20.1 +14 38 49.2 J2000 ACS/HRC ACCUM Imaging No ACS/HRC ACCUM 23 24 20.1 +14 38 49.2 J2000 ACS/HRC ACCUM RampFilter No ACS/HRC ACCUM 15 16 44.59 +07 01 17.6 J2000 STIS/CCD ACCUM Spectroscopic No STIS/CCD ACCUM 15 16 44.59 +07 01 17.6 J2000 ACS/HRC ACCUM Imaging No ACS/HRC ACCUM 15 16 44.59 +07 01 17.6 J2000 ACS/HRC ACCUM RampFilter No ACS/HRC ACCUM 14 01 41.85 -11 36 25.0 J2000 STIS/CCD ACCUM Spectroscopic No STIS/CCD ACCUM 14 01 41.85 -11 36 25.0 J2000 ACS/HRC ACCUM Imaging No ACS/HRC ACCUM 14 01 41.85 -11 36 25.0 J2000 ACS/HRC ACCUM RampFilter No ACS/HRC ACCUM (Tic-Visit :proposal-id 9838 :visit-id "10" :proposal-version -1 :trans-version "20030422" :date "28-Apr-2003 15:58:21.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 110416 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "10" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2848 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "10" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2914 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) false /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v10.xml (Tic-Visit :proposal-id 9838 :visit-id "20" :proposal-version -1 :trans-version "20030422" :date "01-May-2003 14:14:43.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 276752 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "20" :obset-id "20" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "20" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2844 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "20" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2911 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "20" :orbit-number 3 :pcs-time 300 :si-vis-utilization 2911 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) true /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v20.xml Acquisition for exposures 5-7. No ACQ/PEAK is performed since three adjacient slit positions will be obtained (one one the nucleus and two on either side). CR-split exposures 0.2 arcsec (one slit width) on one side of the nucleus. CR-Split exposure 0.2 arcsec (one slit width) on the other side of the nucleus. (Tic-Visit :proposal-id 9838 :visit-id "30" :proposal-version -1 :trans-version "20030422" :date "01-May-2003 15:48:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 110416 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "30" :obset-id "30" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "30" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2838 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "30" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2904 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) true /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v30.xml /var/tmp/OPVisit63357.xml (Tic-Visit :proposal-id 9838 :visit-id "40" :proposal-version -1 :trans-version "20030422" :date "06-Jun-2003 11:19:22.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 6 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 570944 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "40" :obset-id "40" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2838 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2894 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 3 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 4 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 5 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "40" :orbit-number 6 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) true /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v40.xml Acquisition for exposures 5-13. No ACQ/PEAK is performed since three adjacient slit positions will be obtained (one one the nucleus and two on either side). First of two exposures on the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures on the nucleus. First of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. First of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus. (Tic-Visit :proposal-id 9838 :visit-id "10" :proposal-version -1 :trans-version "20030422" :date "28-Apr-2003 15:58:21.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 110416 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "10" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2848 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "10" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2914 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3214 :pcs-gap 0 ) false /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v50.xml (Tic-Visit :proposal-id 9838 :visit-id "60" :proposal-version -1 :trans-version "20030422" :date "01-May-2003 14:13:44.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 6 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 570976 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "60" :obset-id "60" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2726 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2894 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 3 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 4 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 5 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "60" :orbit-number 6 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3206 :pcs-gap 0 ) true /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v60.xml Acquisition for exposures 5-13. No ACQ/PEAK is performed since three adjacient slit positions will be obtained (one one the nucleus and two on either side). First of two exposures on the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures on the nucleus. First of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. First of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus. (Tic-Visit :proposal-id 9838 :visit-id "70" :proposal-version -1 :trans-version "20030422" :date "28-Apr-2003 17:30:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 110416 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "70" :obset-id "70" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "70" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2836 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "70" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2898 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) false /export/laura/proposals/HST/cycle12/BCG/OP-cache/bcg-v70.xml (Tic-Visit :proposal-id 9838 :visit-id "80" :proposal-version -1 :trans-version "20030422" :date "01-May-2003 14:16:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 6 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 570944 :tdrss-contact-duration 0 ) (Tic-Obset :proposal-id 9838 :visit-id "80" :obset-id "80" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2828 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2894 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 3 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 4 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 5 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) (Tic-Orbit :proposal-id 9838 :visit-id "80" :orbit-number 6 :pcs-time 300 :si-vis-utilization 2897 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3201 :pcs-gap 0 ) false /var/tmp/OPVisit35999.xml Acquisition for exposures 5-13. No ACQ/PEAK is performed since three adjacient slit positions will be obtained (one one the nucleus and two on either side). First of two exposures on the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures on the nucleus. First of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on one side of the nucleus. First of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus. The two exposures are moved by 4 pixels with respect to each other in the spacial direction to allow for accurate removal of hot pixels and cosmic rays. Second of two exposures 0.2 arcsec (one slit width) on the other side of the nucleus.