! Proposal 6667, submission 1 ! PI: Henry C. Ferguson ! Received Fri Apr 26 13:48:25 EDT 1996 ! From: ferguson@stsci.edu ! +====================+ ! | PED OUTPUT PRODUCT | ! +====================+ ! ! /planxty/data2/cyc6prop/egalz/6667/6667.prop ! Generated by PREPROCESSOR, version 6.0e ! Date: Fri Apr 26 13:24:12 EDT 1996 Proposal_Information Title: The Far-UV Evolution of Elliptical Galaxies Proposal_Category: GO Scientific_Category: COSMOLOGY Cycle: 6 Investigators PI_Name: Henry C. Ferguson PI_Institution: Space Telescope Science Institute CoI_Name: Arthur Davidsen CoI_Institution: Johns Hopkins University Contact: CoI_Name: Thomas Brown CoI_Institution: Johns Hopkins University Contact: CoI_Name: Robert Jedrzejewski CoI_Institution: Space Telescope Science Institute Contact: CoI_Name: Jean-Michel Deharveng CoI_Institution: CNRS Laboratoire d'Astronomie Spatiale Contact: Abstract: The far-UV spectra of nearby giant elliptical galaxies are characterized by a ``UV rising branch," which varies greatly in strength from galaxy to galaxy. Studies with IUE, HUT, and HST suggest that the UV flux arises from the advanced phases of evolution in low-mass stars in these systems. While there are several different models to explain the presence such stars in elliptical galaxies, a common feature of the models is that the number of hot stars is a sensitive function of the main-sequence turnoff mass. Because of this, the models in general predict rapid evolution of the far-UV upturn with lookback time. We propose to observe a sample of galaxies in the cluster Abell 370 (z=0.37) with the FOC using the F130LP and F370LP filters. The difference between the two images will effectively provide the flux that would be measured through a broad, very high throughput far-UV filter. Tests on simulated data indicate that these observations will provide a sensitive measure of the strength of the UV rising branch, and decisive upper limits if the galaxies are not detected. Questions Observing_Description: Instrument Configuration We propose to observe four galaxies with the FOC F130LP and F370LP filters. Calibration of the relative throughputs of the two filters will allow measurement of the flux shortward of 3700Angstrom (rest frame 2690Angstrom). This instrument configuration has the highest total throughput in the far UV (Fig. 2) of any HST observing mode, and thus provides the most efficient way to carry out a reconnaissance of elliptical galaxy evolution in the ultraviolet at moderate redshift. beginfigureh parbox3.5in figure=fig1.ps,height=2.8in,width=3.2in parbox3in Fig. 2. --- Comparison of F13-37 bandpass to other bandpasses. WFPC bandpasses are shown as dashed lines. Johnson U appears as a dotted line (normalized arbitrarily to peak at 10%). The key to our proposal is that the much greater integrated throughput in the F13-37 bandpass overcomes the additional noise introduced by having to subtract the F370LP observation. endfigure To verify that this wide bandpass is still sensitive to the UV upturn, we have taken IUE and optical spectra of a sample of nearby ellipticals, redshifted them to z = 0.375 and folded them through the filter bandpasses. The resultant color index varies over 1 magnitude for a 1.7 mag change in rest-frame 1550-V color (Fig. 3). beginfigureh centerline figure=fig2.ps,height=4.5in parbox6.5in Fig. 3. --- Sensitivity of F13-37 to the strength of the far-UV upturn. Composite IUE, optical, and HUT spectra for galaxies in the Virgo and Fornax Cluster have been redshifted to z=0.375 and folded through the F13-37 bandpass. The resulting UV-F370LP color is plotted vs. rest-frame 1550- V, demonstrating that variations in the strength of the UV upturn should be easily detected, even though most of the variation occurs at wavelengths shortward of the peak of the filter bandpass. endfigure Exposure times and Signal- to-Noise Ratio Our galaxy sample consists of the four brightest spectroscopically confirmed normal E/S0 galaxies from the survey of Aragon-Salamanca et al. (1991). The galaxies span 1 magnitude in the K-band, and are similar in luminosity to the galaxies used in Fig. 3. Our exposure times are dictated by the desire to provide significant constraints on models in the event of a null detection. We have therefore adopted a spectrum with 1550-V color of 3.7, and have set exposure times such that the formal uncertainty in the F13-37 flux is 10\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\%. The table below shows count rates and noise contributions from dark current and counting statistics within a 3^ aperture for each galaxy. begintabularcccccccc multicolumn1cGalaxy & multicolumn1cV mag & multicolumn3cCount Rates ( s^-1) & multicolumn3cNoise Contributions (\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\%), Number & (3^ ) & F130LP & F370LP & F13-37 & Dark & F130LP & F370LP , 10 & 20.72 & 6.57 & 8.18 & 1.63 & 77.4 & 12.5 & 10.1, 9 & 20.58 & 7.47 & 9.31 & 1.85 & 75.1 & 13.8 & 11.1, 41 & 21.22 & 4.15 & 5.16 & 1.03 & 84.4 & 8.6 & 6.9, 34 & 21.05 & 4.85 & 6.04 & 1.20 & 82.3 & 9.8 & 7.9, endtabular sectionCalibration The major source of systematic error in these observations will be uncertainties in the relative throughput of the F370LP and F130LP filters. Here, we are helped immensely by the long wavelength cutoff of the FOC. At z = 0.37 the 4000Angstrom break is redshifted well past the peak in the FOC response curve. For a galaxy with rest-frame 1550-V=3.7 at z=0.4, 20\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\% of the counts through F130LP come from photons shortward of 3700Angstrom. To measure the UV flux to 10\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\% accuracy requires that we know the relative throughputs of the two filters to about 2\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\%. The objective prism can be placed in the optical path of both filters, so such calibration is in principle straightforward. Because only a differential measurement is needed at long wavelengths, the low dispersion offered by the prism is not a problem. However, the nonlinearity of the detector at count rates greater than ~ 1 per pixel limits the choice of stars to stars fainter than B ~ 18.7 (or 17.7 with the F1ND filter). We have identified candidate calibrators among the O and B subdwarfs in the outskirts of globular clusters (Chan & Richer 1986; Drukier et al. 1989), and have tentatively chosen M4 CR-831. Crowding does not appear to be a problem. The exposure time is set to achieve <1\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! 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\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\! \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\% uncertainty due to counting statistics in 20Angstrom intervals near 4000Angstrom. To test the calibration, we propose to observe the red spectrophotometric standard G138-31 (spectral type DA7) through F130LP and F370LP (+ F8ND). Real_Time_Justification: Calibration_Justification: Additional_Comments: The calibration observations should be done early in the cycle, and the other observations placed on hold until we review the calibrations. Fixed_Targets Target_Number: 1 Target_Name: A370-10 Alternate_Names: A370-CN-1,A370-SMFC-20 Description: GALAXY,ELLIPTICAL,CLUSTER OF GALAXIES,HIGH REDSHIFT CLUSTER,GRAVITATIONAL LENS Position: RA=02H 39M 52.7S +/- 1S,DEC=-1D 34' 17.54" +/- 1" Equinox: J2000 RV_or_Z: Z = 0.3785 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 19.78+/-0.1 Comments: Positions for A370 galaxies measured from WFPC-1 images, proposal 4719; confirmed to within 3" on digitized sky survey. Target_Number: 2 Target_Name: A370-24 Alternate_Names: A370-CN-42,A370-SMFC-9 Description: GALAXY,ELLIPTICAL,CLUSTER OF GALAXIES,HIGH REDSHIFT CLUSTER,GRAVITATIONAL LENS Position: RA=02H 39M 52.44S +/- 1S,DEC=-1D 33' 41.57" +/- 1" Equinox: J2000 RV_or_Z: Z = 0.377 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 20.25+/-0.1 Comments: This is actually two galaxies, both of which fit in the FOC field of view. We are putting the field center between the two galaxies. Target_Number: 3 Target_Name: A370-34 Alternate_Names: A370-CN-47,A370-SMFC-13 Description: GALAXY,ELLIPTICAL,CLUSTER OF GALAXIES,HIGH REDSHIFT CLUSTER,GRAVITATIONAL LENS Position: RA=2H 39M 50.8S +/- 1S,DEC=-1D 33' 51.78" +/- 1" Equinox: J2000 RV_or_Z: Z = 0.378 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 20.50+/-0.1 Comments: Target_Number: 4 Target_Name: A370-9 Alternate_Names: A370-CN-107,A370-SMFC-35 Description: GALAXY,ELLIPTICAL,CLUSTER OF GALAXIES,HIGH REDSHIFT CLUSTER,GRAVITATIONAL LENS Position: RA=2H 39M 53.02S +/- 1S,DEC=-1D 34' 54.66" +/- 1" Equinox: J2000 RV_or_Z: Z = 0.374 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 19.70+/-0.1 Comments: Target_Number: 5 Target_Name: M4-CR-831 Alternate_Names: Description: STAR,WDO,STELLAR CLUSTER,GLOBULAR CLUSTER Position: RA=16H 24M 10.2S +/- 3S,DEC=-26D 33' 12.2" +/- 3" Equinox: J2000 RV_or_Z: Z = 0 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 20.33 Comments: This star is being observed to calibrate the relative sensitivities of F130LP and F370LP. It is a hot star in the globular cluster M4. It was identified by Chan & Richer 1986, ApJ, 302, 257. There is a spectrum in ApJ, 342, L27, 1989. Target_Number: 6 Target_Name: G158-100 Alternate_Names: OKE-1 Description: STAR,DA,CALIBRATION,THROUGHPUT TEST,INSTRUMENT SENSITIVITY TEST Position: RA=00H 33M 54.32S +/- 1S,DEC=-12D 07' 57.8" +/- 1" Equinox: J2000 RV_or_Z: Z = 0 RA_PM: 0.0 Dec_PM: 0.0 Epoch: J2000 Annual_Parallax: 0.0 Flux: V = 14.89+/-0.01 Comments: This target tests the calibration of the relative throughputs of F130LP and F370LP. It is a red spectrophotometric standard from Oke 1990, AJ, 99, 1621. Position taken from an FOC observation (GO-2583), with a 0.8" correction for proper motion. G158-100 replaces the star G138-31 specified in phase-1. Solar_System_Targets Generic_Targets Scan_Data Visits Visit_Number: 01 Visit_Requirements: ! BEFORE 01-Jan-1997 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 Target_Name: M4-CR-831 Config: FOC/96 Opmode: IMAGE Aperture: 512X512 Sp_Element: F130LP,PRISM2 Wavelength: Optional_Parameters: PIXEL=25X25 Number_of_Iterations: 1 Time_Per_Exposure: 18M Special_Requirements: POS TARG 0,2 Comments: This is a calibration of the F130LP and F370LP relative throughputs. The star is in the globular cluster M4. Exposure_Number: 20 Target_Name: M4-CR-831 Config: FOC/96 Opmode: IMAGE Aperture: 512X512 Sp_Element: F370LP,PRISM2 Wavelength: Optional_Parameters: PIXEL=25X25 Number_of_Iterations: 1 Time_Per_Exposure: 18M Special_Requirements: SAME POS AS 10 Comments: This is a calibration of the relative throughputs of the F370LP and the F130LP filters. The star is in the globular cluster M4. Visit_Number: 02 Visit_Requirements: ! BEFORE 01-Jan-1997 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 Target_Name: G158-100 Config: FOC/96 Opmode: IMAGE Aperture: 512X512 Sp_Element: F130LP,F6ND Wavelength: Optional_Parameters: PIXEL=25X25 Number_of_Iterations: 1 Time_Per_Exposure: 18M Special_Requirements: Comments: Predicted total flux from SYNPHOT is 9.36 counts/s. In 512x512 mode, for a red star, that probably results in less than 0.7 counts/s in the central pixel, comfortably below non-linearity. Exposure_Number: 20 Target_Name: G158-100 Config: FOC/96 Opmode: IMAGE Aperture: 512X512 Sp_Element: F370LP,F6ND Wavelength: Optional_Parameters: PIXEL=25X25 Number_of_Iterations: 1 Time_Per_Exposure: 18M Special_Requirements: SAME POS AS 10 Comments: Visit_Number: 03 Visit_Requirements: AFTER 02 BY 60D TO 180D On_Hold_Comments: Visit_Comments: Visits to the A370 galaxies should be scheduled at least 60 days after the calibration observations, to allow time to modify our observing strategy in the event that the calibration is not successful. Exposure_Number: 10 Target_Name: A370-10 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 42M Special_Requirements: EXPAND Comments: Exposure_Number: 20 Target_Name: A370-10 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Exposure_Number: 30 Target_Name: A370-10 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: SAME POS AS 10 EXPAND Comments: Exposure_Number: 40 Target_Name: A370-10 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Visit_Number: 04 Visit_Requirements: AFTER 02 BY 60D TO 180D On_Hold_Comments: Visit_Comments: Visits to the A370 galaxies should be scheduled at least 60 days after the calibration observations, to allow time to modify our observing strategy in the event that the calibration is not successful. Exposure_Number: 10 Target_Name: A370-9 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 42M Special_Requirements: EXPAND Comments: Exposure_Number: 20 Target_Name: A370-9 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: EXPAND Comments: Exposure_Number: 30 Target_Name: A370-9 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: EXPAND Comments: Visit_Number: 05 Visit_Requirements: AFTER 02 BY 60D TO 180D On_Hold_Comments: Visit_Comments: Visits to the A370 galaxies should be scheduled at least 60 days after the calibration observations, to allow time to modify our observing strategy in the event that the calibration is not successful. Exposure_Number: 10 Target_Name: A370-34 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 42M Special_Requirements: EXPAND Comments: Exposure_Number: 20 Target_Name: A370-34 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Exposure_Number: 30 Target_Name: A370-34 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: SAME POS AS 10 EXPAND Comments: Exposure_Number: 40 Target_Name: A370-34 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: SAME POS AS 10 EXPAND Comments: Exposure_Number: 50 Target_Name: A370-34 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Visit_Number: 06 Visit_Requirements: AFTER 02 BY 60D TO 180D On_Hold_Comments: Visit_Comments: Visits to the A370 galaxies should be scheduled at least 60 days after the calibration observations, to allow time to modify our observing strategy in the event that the calibration is not successful. Exposure_Number: 10 Target_Name: A370-24 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 42M Special_Requirements: EXPAND Comments: Exposure_Number: 20 Target_Name: A370-24 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F130LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Exposure_Number: 30 Target_Name: A370-24 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: SAME POS AS 10 EXPAND Comments: Exposure_Number: 40 Target_Name: A370-24 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 46M Special_Requirements: SAME POS AS 10 EXPAND Comments: Exposure_Number: 50 Target_Name: A370-24 Config: FOC/96 Opmode: IMAGE Aperture: 512X1024 Sp_Element: F370LP Wavelength: Optional_Parameters: PIXEL=50X25 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: POS TARG 0.2,0.2 EXPAND Comments: Data_Distribution ! Defaults indicated; change if desired Medium: 8MM Blocking_Factor: 10 Ship_To: PI_Address Ship_Via: Recipient_Email: ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator