!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! ! ! ! This is a slightly modified version of the Phase II proposal for Cycle ! ! 5 project 5847 submitted earlier. This version overrides all previous ! ! ones. ! ! ! ! R. van der Marel, July 19, 1995. ! ! ! !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! ! ! ! Any suggestions for improvement in this program are welcome and should ! ! be reported to the Principal Investigator and Program Coordinator. ! ! ! ! ABSOLUTELY NOTHING SHOULD BE MODIFIED IN THIS PROPOSAL WITHOUT FIRST ! ! CONSULTING THE PRINCIPAL INVESTIGATOR. ! ! ! !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal ID: 5847 ! Anything after a "!" is comment ! ! Principal Investigator: Roeland P. van der Marel ! Phone: 609 734 8082 (office) , E-mail: marel@sns.ias.edu ! Phone: 609 279 2839 (home) ! ! Program Coordinator: William Workman ! Phone: 410 338 4495 , E-mail: workman@stsci.edu Proposal_Information Title: Stellar kinematics near the nucleus of M32: the central black hole confirmed? Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: Roeland P. van der Marel PI_Institution: Institute for Advanced Study, USA CoI_Name: P. Tim de Zeeuw CoI_Institution: Leiden Observatory, The Netherlands Contact: N CoI_Name: Hans-Walter Rix CoI_Institution: Steward Observatory, Tucson, USA Contact: N CoI_Name: Simon D. M. White CoI_Institution: Max-Planck Institut fuer Astrophysik, Muenchen, Germany Contact: N Abstract: Ground-based stellar kinematical data and HST photometry suggest that M32 might have a massive central black hole. In several recent papers we presented a comprehensive study of the dynamical structure of M32. We obtained high spatial resolution ground-based kinematical data, and determined the deviations of the stellar line-of-sight velocity distributions from Gaussians. We constructed detailed axisymmetric models and found a model with a 1.8 x 10^6 solar mass black hole that fits the HST photometry and all ground-based kinematical data. This makes M32 one of the best cases for a central black hole in a quiescent galaxy. We will obtain HST absorption-line spectra of M32, using the FOS/RD with the G570H grating and various apertures at 6 different positions near the nucleus. The target will be acquired with a five-stage peakup into the 0.1-PAIR aperture. With this aperture our black hole model predicts a stellar velocity dispersion of 116 km/s on the nucleus, and a stellar rotation velocity of 42 km/s at 0.086" along the major axis. Detailed simulations show that these effects are measurable with the FOS, in spite of the relatively large instrumental dispersion and wavelength calibration uncertainties. Wavelength calibration spectra will be taken at the end of each orbit. All observations will be done in one visit of nine orbits. One pointing verification FOS/IMAGE will be obtained at the end of the visit. Questions Observing_Description: SUMMARY: We will obtain HST absorption-line spectra of M32, using the FOS/RD with the G570H grating and various apertures at 6 different positions near the nucleus. The target will be acquired with a five-stage peakup into the 0.1-PAIR aperture. Wavelength calibration images will be taken at the end of each orbit. All observations will be done in one visit of nine orbits. A pointing verification FOS/IMAGE will be obtained at the end of the visit. TARGET COORDINATES: For the target acquisition it is essential to have the best possible estimate of the coordinates of the nucleus of M32. We therefore analyzed HST images of M32, obtained with the FOC/48 (pre-COSTAR; PID: 2719, 3105), the FOC/96 (pre-COSTAR; PID: 1277), the WFPC1 (pre-COSTAR; PID: 1118) and the WFPC2 (post-COSTAR; PID: 5464). In each case the position of the galaxy nucleus was determined using the header information and the software in STSDAS. The resulting coordinates are in the GSC-coordinate system with equinox J2000.0. The coordinates of the nucleus defined for Target 10 below is the average of the values thus obtained. The maximum difference between the positions determined from the different observations was 2.04", with a RMS spread of 1.08". Coordinates determined at STScI using the GASP system are within 1" from the coordinates listed here. ACQUISITION: The smallest aperture to be used for our observations is the 0.1-PAIR. The surface brightness distribution of M32 is very smooth, and increases sharply towards the nucleus. The standard acquisition procedure is therefore a sequence of ACQ/PEAK stages. The default way of doing this is a four-stage peak-up, starting with a 1x3 dwell pattern of the 4.3 aperture, followed by dwells using the 1.0-PAIR, 0.25-PAIR and 0.1-PAIR apertures, respectively. In the present case, the position of the M32 nucleus is not known accurately enough to be confident that it will fall in the 4.3 aperture. We must start with at least a 2x6 dwell pattern of the 4.3 aperture to make sure that the nucleus is found with >99% probability. If we do this and stick to the default four-stage peak-up, then only the first two stages will fit in the first orbit of the visit. Only the third stage will fit in the second orbit, and the fourth and final stage will take up most of the third orbit. This is then an extremely inefficient procedure that leaves much unused target visibility at the end of the first and second orbit. We have therefore devised an alternative scheme based on five stages that can be executed entirely in only two orbits and yields the same pointing accuracy as the default four-stage peak-up. It uses a 2x7 dwell of the 4.3 aperture, a 6x2 dwell of the 1.0-PAIR aperture, a 3x3 dwell of the 0.5-PAIR aperture, a 3x3 dwell of the 0.25-PAIR aperture, and finally, a 5x5 dwell of the 0.1-PAIR aperture. For each stage the parameters SCAN-STEP-X and SCAN-STEP-Y are chosen such that apertures at different dwell positions overlap slightly, and in addition cover entirely the aperture chosen in the previous stage. The first three stages fill the first orbit of the visit, the final two stages fill the second orbit of the visit. M32 is too bright to be acquired with the MIRROR, and we therefore acquire it with the G570H grating, which is also used for all galaxy exposures. The success of our project hinges critically on a proper acquisition. We have therefore developed software that simulates the target acquisition process. The model of Lauer et al. (AJ 104, 552, 1992) for the M32 surface brightness was used, which is based on WFPC photometry. The main issues we wanted to test are: (i) the influence of shot noise associated with the finite exposures time at each dwell point; (ii) the influence of y-location errors on the results of the first acquisition stage; and (iii) the influence of telescope jitter. Uncertainties in the y-location of spectra, combined with the fact that the onboard GIMP-correction scheme is not working during peak-up acquisitions, can lead to systematic errors in the first peak-up stage. The detected photons at each dwell point can come from a region that is up to 0.25" away from where the telescope is actually pointing. To make sure that this doesn't lead to acquisition failure one must choose a sufficiently large overlap between apertures at different dwell points in the first stage. The effects of jitter are small. Unless there is a guide star reacquisition, the target will not be lost. Jitter only adds to the final pointing accuracy. Our software indicates that our planned 5-stage peak-up should work, and yield a RMS final pointing accuracy of 0.020". The expected total number of counts at each stage of the acquisition can be calculated from the Table on page 39 of the FOS Handbook (using the entry that has the same B-V as M32) and the total V-magnitude as observed through the given aperture. A correction of -30% was applied to the total number of counts (Tony Keyes, STScI, private communication). The results are listed in the comments to the individual acquisition exposures. Since HST slews are extremely accurate, and since changes of aperture do not influence the telescope pointing, we will need only one target acquisition. GALAXY EXPOSURES: We will obtain galaxy exposures on and near the nucleus of M32 using the FOS/RD with the G570H grating. The wavelength range is 4569-6818 Angstrom, with a scale of 4.37 Angstrom/diode. The nucleus itself will be observed with the apertures: 0.1-PAIR (which is 0.086" square) and 0.25-PAIR (which is 0.215" square). In addition, the 0.1-PAIR will be used to observe the positions along the M32 major axis at 0.086" from the nucleus, at either side of it. The 0.25-PAIR will be used to observe the positions along the M32 major axis at 0.215" from the nucleus, at either side of it, and at 0.43", at one side of it. The off-nuclear positions are all defined as small offsets with respect to the nucleus. No additional acquisitions are required. The 0.25-PAIR spectrum at 0.43" from the nucleus will be used as template in the stellar kinematical analysis of the other spectra. For example, the nuclear observation with the 0.1-PAIR aperture will be compared to this template to study whether the stellar velocity dispersion on the nucleus is larger than at 0.43" from the nucleus. The choice of aperture positionings was chosen to obtain uniform coverage along the major axis without overlap, for both the 0.1-PAIR and the 0.25-PAIR apertures. For this to work we require the square apertures to be aligned parallel to the major axis. Hence we require a special requirement on the ORIENTation of the telescope (see below). There are four possible ORIENTation options, since square apertures are four-fold symmetric. We are not interested in `chopping' or sky observations and all exposures are therefore done using STEP-PATT=SINGLE. For each target position and aperture the total V-magnitude was calculated by integrating the surface brightness model of Lauer et al. over the given aperture. These magnitudes are listed under `Flux' in the target definitions below. The keyword `SIZE' indicates the size of the aperture to which the given magnitude applies. From these V-magnitudes and the B-V color of M32 the expected count rates per diode at 5000 Angstrom were calculated using the SYNPHOT package and the figures and tables in the FOS Handbook. The resulting S/N per diode for each exposure and exposure time are listed below in the comments to each individual exposure. Different physical models for M32 discern themselves by predicting stellar rotation velocities that differ by less than 40 km/s. To be able to measure such velocities it is necessary to do the wavelength calibration as accurately as possible. The pipeline wavelength calibration is only accurate to of order 70 km/s. We therefore require wavelength calibration exposures at the end of each orbit. These can be obtained during occultation, and therefore do not take up any visibility time. IMAGE: In addition to the spectra we will take one `white light' IMAGE of the FOS aperture field with the MIRROR, to allow an a posteriori check of the pointing accuracy. The total V-magnitude of M32 on a strip of diodes of size 3.7x1.3" is 11.94. This exceeds the brightness limit of the MIRROR. Hence the image must be obtained with a smaller aperture. We will use the 1.0-PAIR. The total V-magnitude through this aperture (when placed on the nucleus) is 12.99, which does not exceed the MIRROR brightness limit. When using this aperture there is no point in using the default dwell pattern of the mode `ACQ', which scans a region of approximately 5x5". We have therefore adopted a non-standard pattern. This has SUB-STEP=8 and Y-SPACE=8, hence yielding pixels that are a factor of two smaller than the default pixels of the mode ACQ (which uses SUB-STEP=4 and Y-SPACE=16). We use the same value for Y-SPACE, namely 64. A vertical region of 2.6" is then scanned, thus properly covering the entire 1.0-PAIR aperture. We use overscanning by setting COMB=YES, and use no Y-OFFSET. The expected number of counts in the diode on the galaxy nucleus is listed in the comment to the IMAGE exposure. PROJECT COMPLEXITY: The effects that we hope to measure are near the limit of what is possible with the HST/FOS: (i) The success of our project relies heavily on the correct pointing of the telescope. Any mispointing at the 0.05" level could seriously limit the information that can be derived from the data. To date, the 0.1-PAIR aperture has not been used for science exposures (although some exposures have been planned for Cycle 4). (ii) With the 0.1-PAIR aperture we expect a stellar velocity dispersion of 116 km/s on the nucleus, if a black hole is present. This is of the same order as the instrumental velocity dispersion of the FOS, which is of order 100 km/s (Gaussian dispersion of the line-spread function). The analysis of the data will involve deconvolution with the line-spread function through the use of a template, hence allowing velocity dispersions near 100 km/s to be measured accurately. However, this does require high S/N (of order 50-100 per diode), and consequently also very accurate flat-fielding to the <1% level. (iii) We expect rotation velocities of 40 km/s near the nucleus, if a black hole is present. This is only little larger than the RMS error in the FOS wavelength calibration, which can be of order 20 km/s. Accurate wavelength calibration is thus required. MINIMIZING INSTRUMENTAL EFFECTS: The previous discussion demonstrates that it is essential that instrumental effects are minimized as much as possible. (i) Motion of the filter grating wheel introduces errors of up to 70 km/s in the wavelength calibration. Hence, there should be ABSOLUTELY NO motion of the filter grating wheel, other than that indicated below. That is, the G570H should be installed before the first (acquisition) exposure of the visit. It should then remain in place until all ACCUM exposures have been obtained. Then it should be replaced by the MIRROR to take the verification IMAGE. This IMAGE should be the last exposure of the visit. (ii) There is a possibility that motion of the aperture wheel influences the wavelength scale (see instrument report CAL/FOS-131). Therefore, the exposures should be obtained in EXACTLY the sequence listed below, without any additional motion of the aperture wheel. The sequence of exposures below was adopted because it minimizes the number of aperture changes. (iii) The wavelength calibration exposures are essential to monitor small changes in the wavelength scale during the visit. The number and sequence of the wavelength calibration exposures should not be changed, from what is listed below. (iv) The exposure times for the galaxy exposures were all chosen to yield a S/N of 50-100 per diode, which is essential to infer stellar kinematical quantities from the data. Any error in the flat-fielding of the data, even at the <1% level, will reduce the accuracy of the inferences that can be made from the data. It is therefore essential that accurate flat fields are obtained for all apertures to be used in our project (i.e., 0.1-PAIR and 0.25-PAIR). This is especially true for the 0.1-PAIR aperture, for which no flat-fields are currently available. If this were to remain unchanged, it would render part of our Cycle 5 data useless. Likewise, the absence of accurate inverse-sensitivity (IVS) files for any of the apertures to be used in our project could seriously affect the stellar kinematical information that we can derive from it. UNCALIBRATED STATUS OF 0.1-PAIR APERTURE: As indicated by RPS2 in a feasibility diagnostic, the 0.1-PAIR aperture has currently not been fully calibrated. We have conferred with the FOS instrument scientists Tony Keyes and Anuradha Koratkar, and have decided that this should not preclude the use of this aperture in our program. We do require accurate flat-fields and inverse-sensitivity (IVS) frames for this aperture, as discussed below. However, the instrument scientists have expressed their intent to obtain the required calibration exposures during Cycle 4 or 5. Real_Time_Justification: Calibration_Justification: We will obtain wavelength calibration spectra at the end of each orbit of the visit. As explained above, this is absolutely essential to be able to measure rotation velocities of the order 40 km/s in M32. These calibration exposures do not take up any visibility time, since they can be done during occultation. To extract stellar kinematical information from our data it is essential that accurate flat-field and IVS files are available for the 0.1-PAIR and 0.25-PAIR apertures, combined with the G570H grating on the red detector (as discussed above). WE HEREBY VERY STRONGLY REQUEST THAT THE NECESSARY CALIBRATION OBSERVATIONS ARE PERFORMED BY THE FOS INSTRUMENT SCIENTISTS, prior to or during Cycle 5. This is especially important for the 0.1-PAIR aperture, for which no flat-field or IVS files are currently available. In this context we would like to point out that the projects of Ford et al (PID: 5432) and Bower et al (PID: 5433) in Cycle 4 will also use the 0.1-PAIR aperture, and would also strongly benefit from accurate flat-field and IVS files. Other Cycle 5 projects might also wish to use the 0.1-PAIR aperture. After all: this is the smallest aperture available on the HST, and it is likely that this aperture will yield some of the most interesting science ! Additional_Comments: We only have time for one target acquisition in the 9 orbits allocated to this program. It should thus be attempted to schedule our program in ONE VISIT OF 9 SAA FREE ORBITS (which was mentioned also in our Phase I proposal). If this is not possible, we will need to restructure our program. We have an ORIENTation special requirement to make sure that the square apertures align parallel to the major axis of M32, as explained under `GALAXY EXPOSURES' above. This ORIENTation is only determined modulo 90D. We tolerate a difference of +/-10D, to allow more flexible scheduling. It was proposed originally by Ford et al. to use the FOS to determine the stellar kinematics near the nucleus of M32 (proposal type: GTO/FOS; ID 1044; Cycle 0). However, this group has given up its protected rights on these observations. Hence, our proposed observations are not duplications, and they do not violate any GTO protections. Our FOS ACQ image of M32 is no duplication of existing FOC and WFPC2 images of M32: we require it only for an a posteriori check of the positioning of our apertures. ABSOLUTELY NO CHANGES OR MODIFICATIONS, NOT EVEN MINOR ONES, SHOULD BE MADE TO THIS PROGRAM WITHOUT CONSULTING THE PI FIRST. Fixed_Targets Target_Number: 10 Target_Name: NGC221-NUC Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA = 0H 42M 41.824S +/- 0.075S, DEC = +40D 51' 53.91" +/- 0.67", PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 16.73 +/- 0.2 , SIZE = 0.10 , V = 15.09 +/- 0.2 , SIZE = 0.24 , V = 13.85 +/- 0.2 , SIZE = 0.60 , V = 12.99 +/- 0.2 , SIZE = 0.97 , V = 11.23 +/- 0.2 , SIZE = 4.16 Comments: Coordinates of nucleus determined from HST images of M32. V magnitudes obtained by integrating M32 surface brightness over apertures of given `SIZE' (corresponding to FOS apertures: 0.1-PAIR, 0.25-PAIR, 0.25x2.0, 1.0-PAIR and 4.3, respectively). Target_Number: 20 Target_Name: NGC221-MAJ1 Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: R = 0.086" , PA = 161D, FROM 10, PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 17.10 +/- 0.2 , SIZE = 0.10 Comments: V-magnitude is total magnitude as observed through aperture of given `SIZE'. Target_Number: 30 Target_Name: NGC221-MAJ2 Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: R = 0.086" , PA = 341D, FROM 10, PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 17.10 +/- 0.2 , SIZE = 0.10 Comments: V-magnitude is total magnitude as observed through aperture of given `SIZE'. Target_Number: 40 Target_Name: NGC221-MAJ3 Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: R = 0.215" , PA = 161D, FROM 10, PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 15.67 +/- 0.2 , SIZE = 0.24 Comments: V-magnitude is total magnitude as observed through aperture of given `SIZE'. Target_Number: 50 Target_Name: NGC221-MAJ4 Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: R = 0.215" , PA = 341D, FROM 10, PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 15.67 +/- 0.2 , SIZE = 0.24 Comments: V-magnitude is total magnitude as observed through aperture of given `SIZE'. Target_Number: 60 Target_Name: NGC221-MAJ5 Alternate_Names: M32 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: R = 0.430" , PA = 161D, FROM 10, PLATE-ID=0738 Equinox: J2000.0 RV_or_Z: V = -205 Flux: B-V = 0.95 +/- 0.02 , V = 16.24 +/- 0.2 , SIZE = 0.24 Comments: V-magnitude is total magnitude as observed through aperture of given `SIZE'. Visits Visit_Number: 1 Visit_Requirements: ORIENT 242.8D TO 242.8D On_Hold_Comments: Visit_Comments: [1] We only have time for one target acquisition in the 9 orbits allocated to this program. It should thus be attempted to schedule our program in ONE VISIT OF 9 SAA FREE ORBITS. If this is not possible, we will need to restructure our program. [2] The following ORIENTations are also OK: 142.8D TO 162.8D; 52.8D TO 72.8D; 322.8D TO 342.8D. These orientations ensure that the square FOS apertures align parallel with the M32 major axis, which has PA = 341D or 161D. Preferably the midpoint of the orientation range should be used, but we tolerate a difference of +/-10D to allow for more flexible scheduling. The angle between the +U3-axis and the FOS +Y-axis was assumed to be 81.8D. [3] Any possible changes to this visit should first be discussed with the PI. Exposure_Number: 10 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 3.36, SCAN-STEP-Y = 0.80, SEARCH-SIZE-X = 2, SEARCH-SIZE-Y = 7, TYPE = UP, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 4.7s Special_Requirements: ONBOARD ACQ FOR 20 NO SPLIT Comments: M32 nucleus falls in this 2*7 search pattern with >99% probability. Exposure time yields 100000 counts on the nucleus. Total V mag. through 4.3 aperture is 11.23, much fainter than G570H red side brightness limit. Exposure_Number: 20 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACQ/PEAK Aperture: 1.0-PAIR Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.61, SCAN-STEP-Y = 0.65, SEARCH-SIZE-X = 6, SEARCH-SIZE-Y = 2, TYPE = UP, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 7.4s Special_Requirements: ONBOARD ACQ FOR 30 NO SPLIT Comments : Exposure time yields 60000 counts on the nucleus. This is a paired aperture, but no sky-chopping should be used. Exposure_Number: 30 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.5-PAIR Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.2867, SCAN-STEP-Y = 0.2867, SEARCH-SIZE-X = 3, SEARCH-SIZE-Y = 3, TYPE = UP, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 9.1s Special_Requirements: ONBOARD ACQ FOR 40 NO SPLIT END ORBIT Comments : Exposure time yields 30000 counts on the nucleus. Exposures 10,20,30 must be completed in first orbit of visit. This is a paired aperture, but no sky-chopping should be used. Exposure_Number: 40 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.1433, SCAN-STEP-Y = 0.1433, SEARCH-SIZE-X = 3, SEARCH-SIZE-Y = 3, TYPE = UP, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 8.5s Special_Requirements: ONBOARD ACQ FOR 50 NO SPLIT Comments : Exposure time yields 10000 counts on the nucleus. This is a paired aperture, but no sky-chopping should be used. Exposure_Number: 50 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.043, SCAN-STEP-Y = 0.043, SEARCH-SIZE-X = 5, SEARCH-SIZE-Y = 5, TYPE = UP, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 38.7s Special_Requirements: ONBOARD ACQ FOR 52-200 NO SPLIT Comments : Exposure time yields 10000 counts on the nucleus. This is a paired aperture, but no sky-chopping should be used. Exposure_Number: 52 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 40,50,52 must be completed in second orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 100 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 49 (i.e., 2400 counts) per diode expected at 5000 Ang. Exposure_Number: 102 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 100,102 must be completed in third orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 110 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 49 per diode expected at 5000 Ang. Exposure_Number: 112 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 110,112 must be completed in the fourth orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 120 Target_Name: NGC221-MAJ1 Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 42 per diode expected at 5000 Ang. Exposure_Number: 122 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 120,122 must be completed in fifth orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 130 Target_Name: NGC221-MAJ2 Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 42 per diode expected at 5000 Ang. Exposure_Number: 132 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.1-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT Comments : Exposure_Number: 134 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 130,132,134 must be completed in sixth orbit of visit. Wave-cals can be done during occultation. Exposure_Number: 140 Target_Name: NGC221-MAJ3 Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 1105S Special_Requirements: NO SPLIT Comments : S/N = 56 per diode expected at 5000 Ang. Exposure_Number: 150 Target_Name: NGC221-MAJ4 Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 1105S Special_Requirements: EXPAND MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 56 per diode expected at 5000 Ang. Exposure_Number: 152 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 140,150,152 must be completed in seventh orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 160 Target_Name: NGC221-NUC Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 1395S Special_Requirements: EXPAND MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 80 per diode expected at 5000 Ang. Exposure_Number: 170 Target_Name: NGC221-MAJ5 Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 800S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT Comments : S/N = 36 per diode expected at 5000 Ang. Exposure_Number: 172 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments : Exposures 160,170,172 must be completed in eigth orbit of visit. Wave-cal can be done during occultation. Exposure_Number: 180 Target_Name: NGC221-MAJ5 Config: FOS/RD Opmode: ACCUM Aperture: 0.25-PAIR Sp_Element: G570H Optional_Parameters: STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 1790S Special_Requirements: EXPAND MIN DUR 90% MAX DUR NO SPLIT Comments : S/N = 54 per diode expected at 5000 Ang. Exposures 180,200 must be completed in ninth and final orbit of visit. Exposure_Number: 200 Target_Name: NGC221-NUC Config: FOS/RD Opmode: IMAGE Aperture: 1.0-PAIR Sp_Element: MIRROR Optional_Parameters: COMB = YES, SUB-STEP = 8, Y-OFFSET = 0, Y-SIZE = 64, Y-SPACE = 8, STEP-PATT = SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 235.4S Special_Requirements: MIN DUR 85% MAX DUR NO SPLIT END ORBIT Comments : Verification image of nucleus. Total V magnitude through aperture is 12.99. Will not `SAFE' the FOS. Exp. time is 0.46S per (x,y) dwell point. Yields 2500 counts in the diode on the nucleus. Data_Distribution Medium: 8MM Blocking_Factor: 10 Ship_To: PI_Address ! (i.e.: Olden Lane, Princeton, NJ 08540) Ship_Via: UPS