CSHELL manual v2.0WDBNMSWDvBJ&7# /"-ph`Yx{ *N1C'p(9 Infrared Telescope Facility Institute for Astronomy, University of Hawai`i 2680 Woodlawn Drive, Honolulu, HI 96822   CSHELL: NASA IRTF Cryogenic Echelle Spectrograph USER'S MANUAL Revision 2.0.1 16 August 1994 T. Greene A. Denault Lots of Mahalo to Alan Tokunaga for immeasurable guidance throughout the CSHELL project Table of Contents: IRTF CSHELL User's Manual I. Introduction 5 A. Preparations Before Coming to the IRTF 6 B. Instrument Description 6 Table1: General Specifications 7 Table 2: Key Technical Features 7 Predicted Sensitivity 8 Instrument Design Overview 9 Table 3: CSHELL SBRC 256 x 256 InSb Array Performance 10 II. Using CSHELL 13 A. Before Night Time Observing 14 System Checkout 14 Signal and Noise Checks 15 Wavelength Calibrations & Dispersion Measurement 15 Example: Setup for HI Br g, 2.16609 mm 17 B. Observing at the Telescope 17 General Observing Procedures 18 CSHELL Observing Checklist 19 Flat Field and Dark Frames 20 Astronomical Observations 20 Imaging 20 Spectroscopy 21 Command Files 21 Common VF Quick Look Techniques 22 III. CSHELL Instrument Reference 23 A. CSHELLXUI and VF Software Description and Reference 24 What is the IC and XUI? 25 Moving the IC computer between the Summit & Manoa 35 CSHELL XUI / IC Command Reference 36 What is VF? 44 VF Source and Docs from IRTF-online 61 VF Command Reference 64 B. Turning CSHELL and its CCD Camera On and Off 71 A. CSHELL Startup 71 B. CSHELL Shutdown 71 C. CCD Guider Camera 71 C. Observing Techniques 72 1. Setting IR Array Bias Voltages 72 2. Check For Read-Noise Limit and Saturation 72 3. Flat-fielding 73 4. Focus And Collimation 73 5. Tweaking the CVF for a Flatter Flat 73 6. Darks 74 7. Acquiring Objects 74 8. Slit Rotation 74 9. Integrations and Nodding 75 10. Observing Extended Objects 76 11. Command Files 76 D. Observing Spectral Lines 78 1. Popular Astronomical Line List 78 2. Night Sky OH Lines 79 3. Using Calibration Lamps and cal_lines 80 E. IRTF Computer Services 82 1. IRTF Mauna Kea Computer Facilities 82 2. Archiving Your Data 82 3. Anonymous FTP and WWW Site Information 84 F. CSHELL Data and its Reduction 85 1. CSHELL FITS File Header Example 85 2. Data Reduction Guide with IRAF Examples 86 G. Using the CSHELL CCD Guider Camera 88 GIC / GUIDER XUI Command Reference 89 IV. Appendices 90 A. Observing Log Sheet and Line Settup Form 90 B. CSHELL Hardware Reference 93 C. Troubleshooting 101 Filter and Slit Wheels 101 CSHELL Grating Equations 103 Verifying CSHELL Throughput 103 D. Temperatures and Controllers 104 Procedure A: Front Panel Configuration 104 Procedure B: Software Control 104 E. Summary of Upgrade Changes for Previous CSHELL Users 105 F. IR Array Linearity Data 107 I. Introduction This document is meant to be a reference to the CSHELL spectrometer for IRTF observers, operators, and staff. Sections I and II of this document are also intended to serve as a guide to introduce new users to the instrument. These first two sections prepare the user, describe the instrument, and cover the basics of system startup, wavelength calibration, and data acquisition. Section III is a detailed reference to instrument operation, observing techniques, spectral line selection, data archiving, and data reduction. The appendices in IV include data log sheets, spectral line setup forms, instrument hardware information, a troubleshooting guide, temperture controller setup instructions, and a summary of changes implemented in the 1994 CSHELL Upgrade. CSHELL users control the instrument through a Sun workstation computer using data acquisition and quick look reduction software under the Sun Open Windows graphical user interface (GUI). The Sun computer communicates via TCP/IP over the observatory Ethernet network to an instrument control (IC) computer mounted on the telescope with CSHELL. Normally the IC machine is always on and running the CSHELL software, but the observer logs onto the Sun machine each night to use the user interface software. Users must use a mouse, windows, and icons on the Sun computer to acquire and look at CSHELL data. The IRTF staff has endeavored to make the user interface programs as intuitive as possible, and they are fully documented in III A. Using the programs can be frustrating, however, if one is not familiar with the Open Windows mouse button conventions. Briefly, the left mouse button is used for selecting items such as text fields, buttons in windows, and default menu choices. The right mouse button is used to display a menu of choices by clicking it when the mouse is positioned on any object that displays a small down-pointing triangle indicative of further choices. A menu of options appears once this is done, and menu items are selected by again pressing the right mouse button when the mouse pointer is positioned on top of them. Default menu items are circled by ovals; they can be selected by either the above procedure or else by just clicking the left button when the mouse pointer is over the original object associated with the menu. Text can be selected with the left button in several ways. The mouse pointer can be positioned at the desired insertion point and the left mouse button clicked to select that point for text insertion. This selected position will be the active insertion point whenever the mouse pointer is positioned in the parent window of that text field. Alternatively, the mouse pointer can be positioned in a text field and the left mouse button can be double- or triple-clicked (rapidly) to select either a portion or all of the text in that field. Text can also be selected by positioning the pointer, clicking the left button, and dragging the pointer over the desired text. Selected text is highlighted and will be replaced by whatever new text is typed on the Sun keyboard. All text changes and commands must be followed by carriage returns to make them effective. This is a very important and often overlooked item! The two columns of keys at the left edge of the sun keyboard can also be used to manipulate windows that the mouse pointer is on top of. Most of these are toggles, so pressing the Front key will alternately place the window under the pointer either in front of or behind all other displayed windows. See III.A of this manual for further details on the CSHELL software. A. Preparations Before Coming to the IRTF a. Read this manual ( I and II) b. Contact your support scientist if you have any questions. c. Retrieve and read the cshellxui (CSHELL user interface) and vf (quick look data reduction) software guides if you are not a computer WIMP (Windows, Icons, and Mouse Person). If possible, get the vf quick look data reduction program installed at your home institution and practice using it. Instructions on how to obtain these user guides and programs electronically is given in III E. Alternatively, the vf programs is accessible at HP on the IRTFs Sun workstation. Practicing with this program before your run can greatly improve observer efficiency. Your support scientist will usually go over the operation of CSHELL and help you take calibration lamp data at Hale Pohaku in the first afternoon of your run. d. Bring the following with you: Offset guide stars if required. The offset guider has a field-of-view that is an annulus with inner radius 100" and outer radius ~200", and it can reach V= 12 mag in 1 second with no moon. Note that the CSHELL on-axis CCD camera permits guiding while integrating, has a field-of-view of ~60", and it can reach V= 16 mag stars under typical conditions. Contact your support scientist about using this camera to guide on visible objects. Slit rotation information. CSHELL can be rotated 90 to a few degrees accuracy, but the process takes up to half an hour. 8 mm or 4 mm tapes. It is recommended to bring one tape per night to permit backing up each night's data on a separate tape. Bring enough tapes for enough copies of the entire data set. We find the video grade tapes to be of insufficient quality; bring data grade tapes. B. Instrument Description CSHELL is a long-slit spectrograph which uses a 31.6 lines/mm, 63.5 echelle with narrow band circular variable filters that isolate a single order (orders from 11 to 56). The spectrograph can achieve resolving powers up to 42000, or 7 km/s, over the 1-5 mm spectral region. CSHELL originally had both Rockwell 256x256 NICMOS3 HgCdTe and Huhes SBRC 58x62 InSb detector arrays, but both have been now replaced with a single Huhes SBRC 256x256 InSb device sensitive from 1-5.5 mm. The instrument also has a direct imaging mode, described below. Further technical information on the design and performance can be found in Greene et al. (1993, Proc. SPIE, vol. 1946, p. 313) and Tokunaga et al. (1990, Proc. SPIE, vol. 1235, p.131). The Greene et al. (1993) paper must be cited in all publications of CSHELL data! CSHELL was constructed with funds from the NSF and NASA. Its design and construction was achieved by a team of IRTF and IfA personnel. The principal specifications and technical features of CSHELL are summarized below: Table1: General Specifications Array: SBRC InSb; 256 spectral by 160 spatial pixels Pixel Size: 0.20 arcsec; 2.7 km/s per pixel at blaze angle Wavelength Range: 1.08 - 5.6 mm Free Spectral Range: 2.5 10-3 l Resolving Power (R) 43000 21500 14300 10800 5400 Slit width (arcsec) 0.5 1.0 1.5 2.0 4.0 Pixels/slit 2.5 5 7.5 10 20 R = l / Dl Slit: 30" in length. Discrete slit widths of 0.5", 1.0", 1.5", 2.0" and 4.0". The 4" slit has been provided to permit spectrophotometry on point sources. The slit orientation may be changed by manually rotating the spectrograph with the instrument rotator on the telescope. Table 2: Key Technical Features Optics f/13.67 beam at the slit Collimator type Off-axis cassegrain Collimated beam diameter 8.0 cm Material Zerodur Grating Milton Roy 31.6 lines / mm echelle, 63.5 blaze angle Object acquisition capability Visible CCD and direct IR imaging of the focal plane Cooling method Closed-cycle cooler with Nitrogen regulation Overall dimensions Inner cold box 56 cm 19 cm 18 cm Outer vacuum case 64 cm 35 cm 27 cm Direct Imaging Mode CSHELL has a direct imaging mode in which a plane mirror substitutes for the grating and provides an image of the 30" field-of-view on the infrared array. This mode is useful for viewing the field in the infrared, acquiring sources, and centering them in the slit. Images of the field may be recorded for reference with either narrow band or standard photometric filters, though the system is not meant to provide high quality photometric images. Calibration Lamps Argon, krypton and xenon spectral lamps and a continuum lamp are provided for wavelength calibration and flat fields. Software On-line quick look data reduction software is available for use with the instrument. It allows examination of the data by providing sky subtraction, flat fielding, and simple spectral extraction. Raw or reduced FITS format data files are recorded in tar format on 4 mm or 8 mm tape. Predicted Sensitivity The spectrograph sensitivity F in W/m2/mm is given by  Other parameters are F0 = 2.410-19 l < 3 mm (16.5% throughput @ blaze angle) = 3.210-19 l > 3 mm S = signal-to-noise ratio R = resolving power l = wavelength in mm N = total number of pixels summed (spatial + spectral directions, including sky) nr = electronics noise (readout and other sources) in electrons nb = dark current and background in electrons/sec t = individual exposure time T = total observation time Below we present the sensitivity for S = 10, R = 21500 (1.0" slit), and T = 1 hour. Calculations are for a point source in which sky subtraction is achieved by nodding the telescope along the slit such that the object remains in the slit; for the surface brightness sensitivity, the telescope is nodded to blank sky. Pixels are summed 1" along the slit and over one resolution element along the dispersion direction; therefore, the results are per resolution element, not per pixel. The numbers below may be scaled to other cases using the above formula, but longer (guided) exposures can improve sensitivities. We use a system electronics noise of 35 electrons. This is representative of (almost) the entire array (including high dark current pixels) for 240 s exposures with 6 samples (Fowler MCS technique) at 325 mV applied bias. For wavelengths short of 2.5 mm we take nb = 5 electrons / sec and t = 240 sec. At 3.4 mm, nb = 28 electrons / sec and t = 120 sec. At 4.8 mm, nb = 1000 electrons / sec and t = 10 sec, usually short enough for good sky subtraction. We sum 5 pixels in the dispersion direction by 5 pixels (1'') in the spatial direction . Sensitivities with SBRC 256x256 InSb Array l mm Continuum Mag. Line Flux Surface Brightness (W/m2/mm) (W/m2 / resol) (W/m2/sq. arcsec) 1.25 9.6 10-15 13.8 5.6 10-19 7.9 10-19 1.65 5.6 10-15 13.3 4.3 10-19 6.1 10-19 2.2 3.2 10-15 12.8 3.2 10-19 4.6 10-19 3.4 3.2 10-15 10.9 5.1 10-19 7.2 10-19 4.8 8.2 10-15 8.5 1.8 10-18 2.6 10-18 NOTE: The above estimates do not account for observing overhead. Be sure to allow for acquiring objects, guiding inefficiencies, changing wavelengths, rotating the slit, observing the sky (you can not nod extended objects within the slit, so use the above Surface Brightness numbers), and calibrations (e.g. flats, lamp lines, and standard stars at each wavelength) when estimating the total time required for making a set of observations. CHECK IRTF ONLINE FOR UPDATED PERFORMANCE INFORMATION! Instrument Design Overview Figures 1 and 2 show the light path through the instrument. The incoming beam from the IRTF is f/35, and the beam is converted to f/13.67 by the input lens, a plano-convex BaF2 lens. The input lens forms an image of the focal plane at the slit while forming an image of the pupil at the secondary mirror of the collimator. Alignment with the optical axis of the telescope is achieved by translating and rotating the input lens and flat number 1 together as a unit. A dichroic mirror reflects the IR to the slit while permitting the visible light to be viewed with a visible CCD (not shown). This permits acquisition and guiding on objects with a visible light counterpart. The order-separating CircularVariable Filter (CVF) wheels are positioned at a suitable distance from the slit, such that the width of the incoming beam is not wider than a single resolution element of theCVF. This maintains the spectral purity of the beam through the CVF. The CVFs were selected from the stock catalog of Optical Coatings Lab Inc. These CVFs cause ripples in CSHELL spectra with amplitudes of 10 - 20% peak-to-peak and periods of 2 - 10 cycles per frame due to optical interference in their substrates. This is CSHELL's most severe remaining instrumental problem. However, we have constructed discrete He I 1.083 mm and HI Br g 2.167 mm filters which do not exhibit this fringing and are also investigating replacing the CVFs with ones that will not exhibit fringing. The l < 2.5 mm CVFs also have small leaks from adjacent grating orders, with maximum leak amplitudes at their shortest wavelenghts (2% at 1.1 mm). After the filter wheels, the beam passes through an off-axis Cassegrain collimator designed to produce a collimated beam 8.0 cm in diameter. The effective focal length of the collimator is 109 cm, and its design is such that its optical axis has been translated by 0.56 cm from that of the incoming beam. This produces a 1.12-cm displacement of the incoming and outgoing beams. The dispersed light is directed to flat number 3. The distance between the secondary and primary mirrors of the collimator is 12.6 cm, which is enough for installation of a "direct imaging mirror" (shown in Figure 2). When inserted into the beam, this mirror sends the beam back to the collimator, forming an image of the focal plane at the IR array. The telescope focal plane can thus be viewed directly in the IR, and the slit positioned before a spectrum is taken. It is also be possible to record an image of the field if desired. There is little room for placement of an IR array at the image of the spectrum, so we allow the dispersed light to expand to a spherical relay mirror via flat number 4. The relay mirror forms the final image of the spectrum on the IR array. A pupil image is located about 3 cm in front of the IR array where there is a stop and pupil mask to reject stray light. The closed-cycle cooler allows continuous operation for three weeks or longer on the telescope. We are using a CTI Cryogenics Model 350 CP closed-cycle cooler that provides acooling capacity of 20 watts at 77K and 2 watts at 13K. A vibration-damping mount was developed to reduce compressor-induced microphonics. CSHELL now uses a single Hughes SBRC 256 x 256 InSb pixel IR array to acquire all infrared photons. Its performance and operating parameters in CSHELL are tabulated below. See also Appendix F for linearity data. Table 3: CSHELL SBRC 256 x 256 InSb Array Performance Read Noise: 55 electrons @ 1 sample, 22 electrons @ 6 samples (Fowler MCS) Electrons / ADU: 11.0 Background Limit: ~ 100 ADU in 240 s exposure @ 6 samples Int. Time: 76 ms Fowler sampling; 50 ms Fast Mode Temperature: 30 K Dark Current: ~ 0.5 electrons / second Quantum Efficiency: ~ 80% for 1 mm < l < 3 mm; ~ 60% for 3 mm < l < 5.5 mm Pixel size: 30 mm 1% linear Well Size: 55,000 e- @ 325 mV bias; 92,400 e- @ 500 mV bias; 170,000 @ 800 mV bias; 234,000 e- @ 1.0 V bias (see III.C, IV.F) Device Artifacts: ~ 1000 icky pixels (high dark current), tachyons (re. Fowler)   II. Using CSHELL NOTE: This section assumes the user is familiar with the basic function of the cshellxui (data acquisition) and vf (quick look data reduction) programs. See the cshellxui and vf documentation ( III.A) for information on the details of this software. Powering up CSHELL and starting its software (explained in III.B) initializes the instrument in a safe state: the calibration lamps are off, the lamp mirror is out, the filters and slit are in closed blank positions, and the shutter is closed. This is done by the telescope operator, day crew, or support scientist. No light enters the spectrometer or falls on the infrared array in this initialized configuration, but the internal CCD can see out through the telescope. This configuration is graphically represented by the cshellxui Observing Parameters Window icons representing the elements in the instruments optical path. Icons representing elements exposed to light are colored yellow, ones not in the light path are gray, and the filter wheel is colored blue when the CVF has been manually changed to select a grating order different from the one of the entered wavelength. One must select the proper states of each mechanism by selecting from each icon's menu with the mouse (right button for menu). Typical mouse menu operations with the icons are turning the calibration lamps on and off, moving the lamp mirror in and out of the beam, selecting the desired filter, choosing a slit size, switching between imaging and spectroscopic modes, open and closing the shutter, and switching between the detector arrays. It is best to evaluate and change the states of the icons from right to left order as displayed in the window. Different observing modes are selected by changing the configurations of CSHELL's mechanisms. Open the shutter if you wish the detector array to be exposed to incident light, but close it if you wish to acquire dark images. The direct Imaging Mirror must be moved into the light path if one wants an image of the focal plane, and it must be out of the light path if one wishes to acquire a spectrum. Spectra are usually taken through a 30" long slit of selected width (the slit width determines flux and resolution), and images can be taken of a large field (30" 30") through the open slit position or else through a narrower slit . Filters must be selected for the desired wavelengths, and the grating is automatically positioned at the correct angle when wavelengths are entered into the cshellxui software. Calibration lamps must be turned on (and the lamp mirror moved in) to take wavelength calibration (e.g. Argon or Krypton lamp) or flat field (continuum lamp) frames. All lamps should be off (and the mirror moved out) when acquiring astronomical data. The calibration lamps and mirror are usually used just when taking spectral calibration data, and the lamp mirror is moved in and out by repeatedly selecting the lamp that is on. The filter wheels are usually set to the CVF / Open (l > 1.57 mm) or CVF / Blocker (l 1.57 mm) position unless one is observing lines for which we have discrete filters installed. Be sure to enter your name, institution, etc. in the Setup Parameters Frame (Window) each time you restart the cshellxui software. The (vacuum) wavelength or wave number to be observed is entered into the Observing Parameters Frame. Parameters such as integration time, the number of coadds per frame, and the number of frames (or Cycles) to be acquired are also entered into this window's text fields. Data can be acquired in either stare mode (single frame; .a appended to the filename) or else in nodding mode. The nodding mode moves the telescope between frames and stores each frame separately with a .a or .b name extension to indicate beam polarity. A single cycle in nodding mode acquires one frame in position A and another frame in position B. Multiples of two cycles cause data to be acquired in the ABBA... position sequence. The nod direction and magnitude are set to your request by the telescope operator. Newly acquired data goes into one of several buffers and may also be automatically saved. The LastFrame buffer in the Observing Parameters Frame indicates which buffer new data will go into. Buffer b0 is the default new data buffer, and the vf quick look program displays this buffer by default in its Canvas A. This is the standard configuration for data to be displayed in the top left canvas of the vf quick look program. A MeanFrame buffer can be selected so that a VF window shows the mean of a sequence of cycles (e.g. mean A-B in Nod mode or mean A frame in Stare mode). Autosave must be enabled for data to be automatically written with the concatenated filename and number shown on the bottom line of the Observing Parameters Frame. Autosave is enabled by checking its box; this ensures that the data files will be saved onto the Sun (XUI) computer's disk in FITS disk format. The data in a buffer can also be saved by the vf quick look program. The Save Data option of the vf File menu will save a selected buffer as a FITS data file, but will omit the instrument and telescope information from the file header. Therefore it is best to have Autosave enabled before acquiring any data if you wish to save it. The Object and Comment fields in the Observing parameters Frame are also written into the file header. One must issue a Go command to take an exposure. This is usually done by selecting Go Obs from the Go menu of the cshellxui Base Frame (main window). This is also the default for that menu so Go Obs can also be selected by clicking the left mouse button when the pointer is positioned over the Go menu. The data goes into the chosen buffer (default LastFrame buffer is b0) and is written to a disk file only if Autosave is enabled. The data buffer can be displayed in a canvas of the vf window (Canvas A displays buffer b0 by default). The current image coordinate and data value of the image pixel beneath the mouse cursor is displayed at the top of the image. The image can be zoomed, rescaled, or restretched in its vf display window canvas, and it can also be redisplayed as a spectral cut, histogram, or file header in any vf canvas. See the vf documentation in III.A for details. A. Before Night Time Observing System Checkout The IRTF day crew checks the basic wavelength calibration, sensitivity, and overall functionality of CSHELL each time it is mounted on the telescope, but you can also check these parameters when you do wavelength calibrations at the start of each night. The presence of the calibration lamp lines at the proper locations and intensities as well as the proper appearance of the flat field and dark frames are adequate assurances of the proper functioning of the instrument. The IRTF day crew and support staff have priority in using CSHELL between 9:00 am and 3:15 pm, while observers have usage priority at other times. Before the first night's observing (starting after 3:15 pm), we recommend that the signal and dark frame noise checks and the wavelength calibrations be performed either at HP or at the telescope. This will provide you with hands-on experience with using the instrument before taking astronomical data and allow you to spot any problems early on. Call the IRTF summit before starting any work with the instrument from Hale Pohaku - the day crew or other staff may be using it! First start up the cshellic, cshellxui, and vf software (see III.A-B or get assistance from the IRTF staff). Once the cshellxui software is up, you should check the main window's status panel for proper instrument operation. Remember to type xuihostname wien in the command line of the cshellxui window if observing from the IRTF workstation (wien) at Hale Pohaku. All of the status items should be "OK" or "READY" (green). The IR array temperature should be 30.0 0.2 K. The CCD array temperature should be 190 20 K. The coldbox temperature should be 72.5 2 K. There should not be any warning messages in the cshellxui feedback window. The IR array bias voltages must also be set (select Set Programmable Voltages button in Setup Parameters Window) whenever the software is started. Signal and Noise Checks Check the array noise performance by taking a 2.0 second dark (shutter closed) exposure. Check the array noise by selecting the stats item in the vf Options menu. Refer to Table 4 to see the means and standard deviations you should getting in a sub-region box of a given size. The array has adequate dark and noise performance if your numbers are consistent with the table values, and you can now evaluate its response to signals. Take a 2 second spectroscopic exposure of the 2.19085 mm Krypton line through the 1" slit and check if your peak signal values are consistent with those in Table 4. The Krypton line should be in column 128 5. Table 4: Signal & Noise Check Dark Frame Kr Line Frame Int. time (sec) 2.0 2.0 Slit Blank 1'' Mean (ADUs) 0.0 10 (50 x 50 pixel box) - Std. Dev. (ADUs) 3-5 (50 x 50 pixel box) - Peak Signal(ADUs) - ~ 1200 Wavelength Calibrations & Dispersion Measurement You must take wavelength calibration data each night by either observing rare gas discharge lamps or else by using telluric emission or absorption lines in your data itself. CSHELL uses vacuum wavelengths and vacuum wave numbers only. Be sure to correct rest wavelengths for any velocity shifts in your objects before entering them into the CSHELL software. The first step of the discharge lamp wavelength calibration process is selecting which calibration lamp lines to use. Lines must be selected for calculation of the spectral zero point and dispersion at each observational wavelength (grating position) selected. CSHELL's spectral range is only 1/400 of the central wavelength .This narrow range dictates that the lines of the calibration lamps rarely fall on the arrays when the instrument is set up to observe lines of astronomical interest. We can trick CSHELL into observing these calibration lines at the same grating position as used for astronomical lines, however. The procedure is to select the (vacuum) wavelength which you wish to fall near the center of the array for your astronomical observations, and then select a different grating order so that the desired calibration lines are visible without moving the grating. This is accomplished by moving the CVF filter to select different orders after the grating has already been positioned for the desired astronomical wavelength. This technique is explained below. An auxiliary program, cal_lines, is used to determine which calibration lamp lines are to be used at a given wavelength selected for observation. This program is run from either a UNIX command line window on an IRTF workstation, or else from the PC in the IRTF office at Hale Pohaku. Instructions on using the program and a description of its output are given in III.D. Which calibration lines should you observe? The purpose of the lines is to determine the wavelength zero point and dispersion for each observational wavelength (grating position). In practice, one should observe a single calibration line for each desired wavelength as well as several lines distributed across many columns of the array for at least one wavelength setting at the start of each night. The single line at each grating position (selected wavelength) directly allows the determination of the wavelength of the illuminated array column, and observing several lines over a range of columns on the array allows the determination of the dispersion at that grating setting. It is best to observe at least 3 lines which span at least half of the array (128 columns). We wish to observe these lines at the same grating position used for the object observation wavelength, so we must select the proper CVF wavelength for each line (see Cal_lines Table, III.D) without moving the grating. This is done by entering the new CVF wavelength into the proper text field of the Observing Parameters Frame. The calibration lines must also be sufficiently bright to observe in a reasonable amount of time (e.g. 60 seconds ). Line intensities can be looked up in the copy of the elemental spectral atlas (by M. Outred) kept with the CSHELL documentation at the telescope. Lines must be looked up within each element's listing by wave number (the atlas gives air wavelengths and we use vacuum ones), and we find that lines with intensities of 100 units or above can be adequately observed in 60 seconds or less. Most lines listed by cal_lines can be observed in 15 s or less. If you are observing in order nobs and the calibration line (wavelength ll) appears in some column in order nl , then lobs ,the wavelength of that column in the astronomical spectrum (order nobs), is: lobs = ll nl / nobs . lobs is given in column 3 and nl is given in column 4 of the Cal_lines Table (see also III.D). The expected position of a line on the SBRC 256 256 array is listed in col(SBRC256) in the table. The dispersion at one grating position is related to that at another position by:  where C is a different constant for each detector array and is the grating angle at each desired observational wavelength. The grating angle can be found in the cshellxui window and it is also recorded in the FITS file headers (see III.F). We recommend that you measure the zero-point for all observed wavelengths and the dispersion for at least one wavelength each night of your run. It is also a good idea to look at the CSHELL Atmospheric Atlas kept at the telescope (kindly provided by John Lacy @ UT) or the KPNO Solar Spectral Atlas (Livingston, W., and Wallace, L. An Atlas of the Solar Spectrum from 1850 - 9000 cm-1 (1.1 to 5.4 mm), NSO Technical Report #91-001, National Solar Observatory) as part of the wavelength calibration procedure. These atlases are useful for evaluating the strengths and locations of any telluric absorption lines in the wavelength ranges which you will observe. This will show you if any telluric lines will land on or near your astronomical ones, and these lines may also be used as accurate wavelength references for interpretation of your data while observing. You may also observe the sky at twilight to see if the telluric lines occur in their predicted places in your spectra. Finally, OH sky emission lines can be also used as a wavelength check (See III.D). Example: Setup for HI Br g, 2.16609 mm Suppose that you want to observe the HI Br g line at the 2.16609 mm wavelength (given as an example in III.D). First select CVF/ Open from the Filter icon menu, then type this wavelength into the Wavelen text field of the cshellxui Observing Parameters Frame. The grating is automatically positioned to the correct angle for observation, and the CVF is moved to the selected wavelength. Next choose the slit size you wish to observe with, and make sure that the grating is selected (e.g. direct imaging mirror is out of the optical path) and the shutter is open. Note that the Kr lamp has strong lines that are predicted to land at columns 50, 95, and 212 of the array (see Cal_lines Table in III.D). Each of these lines must be observed to adequately measure the dispersion at the 2.16609 mm wavelength. Remember to change the CVF wavelength to the correct value (see Cal_lines Table in III.D) before observing each calibration line. The spectral zero point and dispersion at the 2.16609 mm wavelength may be calculated by performing a linear fit to the apparent line wavelengths (lobs , column 3 of Cal_lines Table in III.D) and the array columns in which they appear at the row of interest. It is best to repeat this procedure for each wavelength you plan to observe, but it is possible to only observe single lines at each wavelength (for spectral zero-point information) and compute the dispersion from the Br g dispersion using the above formulae. Be sure to record the grating angle for each line, which can be read from the cshellxui program's main window. This angle is also in the FITS file headers (see III.F). Repeat this calibration procedure each night of your run. B. Observing at the Telescope Once you arrive at the telescope you may want to enter the coordinates of your target objects and standard stars into the user star catalog of the IRTF DAS. This will save you from doing so later while you are observing. Your telescope operator or support scientist can help you type in the coordinates. The Telescope Operator will fill CSHELL with liquid nitrogen and bring up the CSHELL software each night for you. Be sure to ask the telescope operator to rotate CSHELL to your desired slit angle (default is East - West with North to the left on the VF display) as well as configure the telescope focus, off-axis guider, and on-axis TV camera (focus and crosshair position) for CSHELL. Select the proper detector and perform the system, signal, and noise checks as well as the wavelength calibrations detailed in II.A if you have not already done so. General Observing Procedures The general observing procedure is to image the field of your object after completing a telescope slew. Next you must position the telescope so that your object is on the slit of the spectrometer and then switch to spectroscopic mode. Note the position of your object on the CCD camera display and ask the operator to start auto-guiding on it. You may use an off-axis guide star if your object is invisible on the CCD. You will usually acquire spectral data in frame pairs, with frames on and off of the object. It is convenient to nod the telescope by about 15" along the slit between the on and off frames. This allows the object to be observed in both frames of a pair if the object is not spatially extended. Be sure to nod far enough away from the object so that pixels seeing the object in the on frame see nothing but blank sky in the off frame. The telescope operator can enter the magnitude and direction of the nod for you, and the cshellxui software will automatically nod the telescope between exposures if you observe in nodding mode. Keep exposure times short initially (120-240 seconds per frame) to be sure that the telescope is tracking and guiding properly. The telescope operator can alter the tracking rates to correct for consistent drifts. You must select the CVF/Blocker Option and also use the shutter wheel blocker (SPF) when observing with the 1.1 - 1.57 mm CVF! This CVF transmits l > 2.5 mm radiation, causing significantly increased background in your data if not blocked as prescribed. The blockers impart about a 10% reduction in flux over the 1.1 - 1.6 mm region. You must observe celestial standard stars to correct for telluric absorption. Find a bright (V < 6) standard from either the Yale Bright Star Catalog or the IRTF standard tables. Be sure that the star is of a satisfactory spectral type so that it does not contain any spectral features that you are attempting to observe in your objects. You need to observe standards at a minimum of two different airmasses to be able to fit their telluric corrections to the airmass range of your objects. Also try to observe the standards at the same array location (row) as your objects; this will minimize CVF fringing in your data as well as simplify both your quick look and final data reductions. The SBRC InSb detector saturates at different count levels depending on its bias voltage (see table below); try to keep your data values below the 1% linearity deviation for your selected bias. Using a single fixed bias (as done with the old NICMOS array) is inappropriate because of non-linearities and icky pixel artifacts in the SBRC 256 x 256 InSb arrays. Larger biases allow more electrons to be collected before saturation, but they also cause increased numbers of high dark current pixels (icky pixels) and low-level non-linearities. Fortunately, the icky pixels mostly disappear when object and sky frames are subtracted. See III.C.1 and Appendix F for more information on selecting appropriate detector bias voltages. Remember to transfer your data to magnetic tapes; it is best to do this at the end of each night at Hale Pohaku. See III.E for details. Also remember that telescope operators are allowed to work no more than 12 hours at a time on the summit; plan your calibrations, observations, and data archiving accordingly. You may stay to archive data after the operator leaves. Be sure to set the CSHELL filter and slit wheels to their Blank positions and terminate the cshellxui software program at the end of each night. Ask the operator to shut down the instrument if there is a danger of lightning. See III.B for details. See the following Observing Checklist for more details. Next we consider some details of the observing procedure. We present a reference of observing techniques in III.C. CSHELL Observing Checklist Before Leaving Home Produce Objects, Standards, and Guide Stars Lists Calculate Integration Times for Desired Sensitivities Determine Slit Orientations Get one 4mm or 8 mm tape for each night of your run Read I and II of this manual Daytime at Hale Pohaku or the Summit Obtain an IRTF guest observer account (log into IRTF workstation as guests) Select Calibration Lamp lines with cal_lines Start the CSHELL Software and Check the System Status Set Programmable Voltages (Setup Parameters Frame) Take Signal and Noise Test Data Take Calibration Line Data for all Grating Settings that night At The Summit Request CSHELL Rotation, Focus, Guider, and Crosshair Configurations Enter Personal and Instrument Setup Information into CSHELLXUI and VF Software Select bias macro and Set Programmable Voltages (Setup Parameters Frame) Select First Wavelength Image Sky or Ar lamp through Slit and Record its Column Position (Direct Imaging Mode) Take Flat Field and Dark Frames (Spectroscopic Mode) Slew to Object Image Object Move Slit to Open and Select Direct Imaging Mode Choose Nod Vector for Imaging Take Image Frame Pair of Object Move to Slit using VF TCS Coordinates Window Take Object Spectra Insert Slit and Select Spectroscopic Mode Locate Object along Slit and Choose Nod Vector Guide with CCD Camera Take First Spectrum (short exposure) and Evaluate Signal Take More Spectra (longer exposures) Slew to Standard Image Standard Move Slit to Open and Select Direct Imaging Mode Choose Nod Vector for Imaging Take Image Frame Pair of Object Move to Slit using VF TCS Coordinates Window Take Standard Spectra, Darks, and Flats Insert Slit and Select Spectroscopic Mode Locate Standard along Slit and Choose Nod Vector Take Spectrum Close Shutter, Take Dark Frames, Open Shutter Select Continuum Lamp and Mirror Take Flat Field Frames Repeat Flat, Object, and Standard Observations at other Wavelengths Until Done Take any missing Calibration, Flat Field, or Dark Frame Data Blank CSHELL Filter and Slit from cshellxui Quit CSHELLXUI, VF , and Guider Software; logout from Sun Archive Data (4 mm tape drive at summit, 8 mm tape drive at Hale Pohaku) Flat Field and Dark Frames Uniform celestial illumination does not exactly illuminate the detector arrays uniformly due to imperfections in the telescope and instrument optics. Each detector pixel also responds to illumination differently, causing further departures from a uniform system response. However, dividing astronomical data by a flat field made by exposing CSHELL to a uniform illumination source should correct for these response abnormalities as long as the system responds to light linearly. The continuum lamp is a good source of spatially and spectrally uniform illumination, and CSHELL behaves linearly as long as each pixel has about the same number of counts in both object and flat filed data. Therefore we can take flat field frames by observing the continuum lamp with the same instrument state used for astronomical observations. In practice this means that you should acquire several frames of the continuum lamp's spectrum at each wavelength and slit size employed in your astronomical observations. Continuum lamp spectra exposure times of about 5 seconds result in about 2000 counts through a 1" slit. You may take many flat frames (10+) by typing the number of frames in the Cycles text field of the Observing Parameters Frame. The first step in this process is resetting the grating order or CVF wavelengths of CSHELL from those used for calibration lines to those used for your astronomical observations. All flat field and data frames should be taken without moving the grating or CVF between exposures. All exposures include a dark current contribution from the detector arrays. This current can be a significant fraction of the signal from astronomical objects since CSHELL operates at very high resolution. Objects are normally observed in frame pairs (on and off the source) which are subtracted to remove this dark current contribution from the data. We must observe separate dark frames to remove this component from the flat fields, however. This is done by turning off the calibration lamps and closing the shutter before acquiring frames of exposure time equal to the flat field frames. Again, many (5-10) dark frames should be acquired at a time in this manner. Astronomical Observations You are ready to acquire astronomical data once you have completed your calibration lamp, flat field, and dark frame observations. All flat field and data frames should be taken without moving the grating or CVF between exposures. The next step is to find the array column which corresponds to the location of the slit. Do this by acquiring a direct image of the slit; insert the direct imaging mirror (selecting imaging mode) into the light path. You may illuminate the sit with either they sky or a discharge lamp. Record the array column which the slit is centered on; you must position your objects on this column to observe them with the spectrometer. This is a good time to enter the slit position, the plate scale, and slit rotation angle into the TCS Coordinates frame of the VF program (Options menu item). VF will use this information to calculate position offsets to move the telescope so that your objects fall on the slit. Imaging Bright objects (K < 9) are easily imaged in single exposures of 1 second or less. Fainter objects require longer exposures and are best observed in a nodding mode in order to subtract the sky background. Be sure to check the focus several times a night by imaging non-saturated objects at different focus positions, using either a FWHM or peak pixel focus evaluation criterion. Evaluate several exposures or coadds at each focus position to integrate over seeing effects. You should be able to achieve a 1" or better FWHM source profile on nights of good seeing. You must position your object on the slit once you have found it in the imaging field (30" on each side). This is easily done by displaying the field in a pane of the VF program and selecting the TCS Coordinates item from the VF Option menu. Be sure that the plate scale, slit rotation angle, and slit position are correct, then click the left mouse button while the pointer is at the center of your object. Next press the F key on the Sun keyboard to enter the mouse coordinates, and click on the Calculate Offset button to calculate how far to offset the telescope. Then offset the telescope by pressing the Offset TCS button. It is a good idea to acquire a frame at the new telescope position to ensure that your object will be on the slit. Once this frame is acquired (and saved if desired) you should switch to your desired slit size and select spectroscopic observing mode (removing the direct imaging mirror). Spectroscopy It is best to move the telescope in the direction of the slit to position your object away from the array center and nod about half a slit length in the opposite direction in order to observe your source in both A and B beam positions. For example, if the slit is oriented East - West (default orientation), then you may wish to move the telescope 7.5" east and use a 15" West nod between frames if you are observing a point source. This would position your source spectrum nearly equally displaced from the array center in both the on and off (A and B) frames when observing in a nod mode. It is in your best interest to guide the telescope using a guide star in the field of either the internal CCD or offset guider camera. Guiding is required for good signal to noise ratios. The mean of the A-B data pairs can be accumulated in a buffer if you are taking many spectra of an object. The MeanFrame buffer is initially set to "N/A" to disable this feature. To turn it on, select an unused buffer from its list in the Observing Parameters Frame. This buffer will then contain the mean A-B for the current set of cycles. Command Files The cshellxui and VF programs can read command files which automatically configure CSHELL. This is a great advantage over the manual configuration of each mechanism for commonly used instrument setups. For example, one can create and execute a command file which selects a detector bias for spectroscopy, puts in a slit, switches to spectroscopic mode, and sets the integrations. This is in fact what the spect command does, and it can be used to automatically configure CSHELL for spectroscopic observations. Likewise, image will configure CSHELL for imaging, and a VF command file can subtract 2 buffers and divide the result by the Flat Field buffer. Command files maybe be created and edited in several ways. The current state of all CSHELL mechanisms may be recorded into a command file by selecting the Save Parameters item in the cshellxui Parameters menu. Command files may be loaded, edited, and saved with this window also. Commands may be entered into files by either recording your real-time manipulations of the spectrometer (check Record button in the Commands frame) or typing the text commands into the edit window of the Commands frame. Command syntax is identical to the cshellxui / cshellic and VF command line syntax; see III.A. Cshellxui command files are stored in the macro/cshellxui directory of your guest observer account, and VF command files are in the macro/vf directory . These are the default directories that the programs use to load and save command files. There are more macros in the ~cshell/macro directories, and you may copy ones from there to your guest account. The most commonly used command files are godark, goflat, image, and spect. These commands execute a series of dark exposures, a series of flat field exposures, set up for a pair of nodded images, and set up for a pair of nodded spectra, respectively. Command files starting with go (e.g. godark, goflat, godark) have Go Obs as their last commands so exposures are actually taken when they are executed Command file names without go (e.g. image, obs) do not contain Go Obs statements; exposure times or other parameters may be modified before starting exposures if you are using these files. The commands in these files are listed in III.C.11. Command file execution may be usually repeated by simply pressing the Go button in the cshellxui main menu; you need not re-load and re-execute the file since the state of CSHELL has already been set by the command file. It is most efficient to use command files for all of your observations, but keep a close eye on the exposure time, Autosave status, and other instrument parameters; it is quite easy to start an integration with the instrument in the wrong state. For example, you may wish to save images of the field, but the image command files turns Autosave off. Common VF Quick Look Techniques The data in any buffer can be examined using the VF program. For example, suppose a spectral frame is stored in buffer b0 and canvas A of VF is set to display an image of the buffer b0 data. Canvas C can also be set to point to buffer b0 and its display mode set to "SpectraA" or "Spectra B" in order to show a binned spectrum of the data over some range in coordinate values. Draw a box on the image in canvas A and select the "Obj Box" and the "X-scale" buttons in the canvas C panel to show the spectrum of the data in the canvas A box in a graph in canvas C. These and other techniques are described in the VF documentation, III.A. A hard copy of the image or the spectrum shown in the selected canvas can be obtained by selecting the print button at the bottom right of the VF window. You may also perform frame arithmetic on and rotate images with VF. For example, you can co-add images to evaluate the quality of your data, divide data by standard stars to remove telluric lines, or rotate a spectrum 180 so that you can compare it to a frequency spectrum. You can also combine the data of the A and B beams in a differenced spectrum with the Spectra A or Spectra B displays. If your object is in both beams in a differenced spectral image (you are nodding along the slit), then define a box enclosing the A beam as the object and a box enclosing the B beam as the sky and select "subtract sky" to see a display of the summed data. VF also can edit and execute command files. This feature is convenient for performing frame arithmetic on and displaying data once they are loaded into buffers. Several VF command files are provided for your use. III. CSHELL Instrument Reference A. CSHELLXUI and VF Software Description and Reference B. Turning CSHELL On and Off C. Observing Techniques D. Observing Spectral Lines E. IRTF Computer Services F. CSHELL Data and its Reduction G. Using the CSHELL CCD Guider Camera A. CSHELLXUI and VF Software Description and Reference What is the IC and XUI? The software for CSHELL consist of 2 applications, the Instrument Control (IC) program and the X User's Interface (XUI). The Instrument Control is named "cshellic", or commonly referred to as the IC. The IC executes on a 386PC computer located on the telescope platform, and is responsible for the real-time control of the instrument and its electronics. The user's interface is provided by the program named "cshellxui", or commonly referred to as the XUI. The XUI executes from a SUN workstation, and provides a friendly interface to the camera. These two programs communication over an ethernet network allowing you to control and view data produce by the instrument from any IRTF's SUN workstations. Figure 1 illustrates this setup.  Figure 1 -IC and XUI diagram A word about initialization files and environment variables. This section describes the initialization files for the IC and XUI program. Normally you will not need to modify these files since default values are automatically setup for your account. They are described here so that you may modify them as needed. Or so you can check them if thing are not working. An environment variable CSHELLXUI identifies the location of the XUI executable and associated information file. For example, if the cshellxui application is stored in /usr/local/cshell/XUI the following line in your .cshrc file would correctly setup this variable setenv CSHELLXUI /usr/local/cshell/XUI The IC, XUI, and VF all use a similar method to initialize parameters when starting up. Each program look for a special text file and execute the commands stored in that file. These file are plain text file which contain one command per line. You may modify them using your favorite UNIX editor. The available commands set are documented in the Command Dictionary for each application (IC, XUI, and VF). This IC program uses ".cshellic-init" from in your current working directory. The XUI program uses ".cshellxui-init" from your home directory. i.e.: ~/.cshellxui-init. The VF program uses ".vf-init" from your home directory. i.e.: ~/.vf-init. Starting the Software This section outlines the procedures for starting up the software. Note that there are two version of the software: 1. Observers version - This version is the last version of the software which has been tested in an actual observing night at the telescope. 2. Engineering version - This version is under development or testing. This version may contain new features, but has not been fully tested yet. You should use the observers version, unless you were specifically told by your support scientist to use the Engineering version of the software. The following sections describe how to start up both the observer and the engineering version. Starting the IC Normally the Instrument Technician will start the IC program for you. However, in case of computer crashes or other problems, the procedure is explained here. Note only one person at a time can start the IC program. Please check with the Telescope Operator or Instrument Tech before staring up the IC program. The procedures for starting the IC program are as follows: 1. Log in on the IC computer (host name is cshell) as the user 'cshellic'. a. Find the keyboard & screen for the cshell IC computer. Login as the user "cshellic". There is no password for this account. login: cshellic After hitting return, it takes about 90 seconds for the software to startup and display the status screen. See Figure 2 for an example of the IC's status screen. Once this screen is display and all mechanisms show "READY", you may go ahead and start the XUI. If any of the status show an "ERROR" state, you should try to reinitialize the item using the ??init command (i.e.: FilterInit, GOInit, GratingInit, etc..). If this fails, ask assistance from the T.O. or support scientist to trouble shoot this failure.  Figure 2 - IC program Sample Screen Starting the XUI Once the IC program is running and all status is READY, you may start the XUI program. The XUI program is an X windows applications. Here are the steps to start the cshellxui. 1. Login on the IRTF's sun workstation and start Openwindows. Your support scientist should have given you instruction on obtaining an account. To start Openwindows, type "openwin" at the UNIX prompt. % openwin 2. From OpenWindows, bring up the workspace menu by clicking the right mouse button on the workspace area. Under "CSHELL", select the "Cshell XUI" item.  Figure 3 - Starting the XUI from the Workspace Menu For those of you who were told to start up the engineering version, select the menu item " CShell XUI (ENG)" from the menu (Figure 3). If all goes well, the following window should appear on your screen.  Figure 4 - XUI program Sample Screen. 3. Start VF. At this point you should also start VF. Access the workspace menu, under the "CShell", select the "VF" menu item. VF should start up immediately. Shutting down the XUI & IC 1. To quit the XUI program by selecting the "Quit" button on the cshellxui window. 2. Backup your data (every night) with the 8 mm Exabyte tape drive to prevent data loss in case of a disk failure. ! Stop here. Normally quitting the XUI is enough. The T.O. or day crew can terminate the IC program. The remaining steps, will terminate the IC program. 3. Enter the "die" command on the IC computer. This will terminate the IC program. The message "CSHELL is down!" message is display when all programs are terminated. The CSHELLXUI Main Menu The Main Menu provides you access to the command frames and other functions. Figure 5 illustrates the menu's selections and give a brief summary of its purpose.  Figure 5 Main Menu Parameters - The select button selects the 'Change..' item. The menu button bring up the sub-menu. Change... - Brings up the 'Parameters' window which allow you to view and change the many CSHELL observing, Setup, and Engineering parameters. Save.. - Brings up the 'Save Parameters as a Macro File' dialog window. This window allows you to write the current setup as a macro file. Go - The select button select the 'Go Obs' item. The menu button brings up the GO sub menu. Go Obs -Starts an integration creating files with the '.a' or '.b' extensions, and IMAGETYP = object in the header. Go Dark - Starts an integration creating files with the '.dk' extension, and IMAGETYP = dark in the header. Go Flat - Starts an integration creating files with the '.fl' extension, and IMAGETYP = flat in the header. Go Comp - Starts an integration creating files with the '.cll' extension, and IMAGETYP = object in the header. Options - The select button selects the 'Execute Do Files' item. The menu button brings up the sub menu. Execute DO Files - Brings up the Edit Command Files window. This window provides the ability to create, edit, save, load, and execute macro files. Stop - The stop button will abort the current GO operation. Quit - The quit button will exit the application. The Status Canvas The Status Canvas is used to display the current state and configuration of CSHELL. A number of formats are available to you. To change the format, select an item from the status canvas menu panel item.  Figure 6 - Status Canvas display 'Status' Selecting 'status' from the status canvas menu, specifies a format similar to figure 4. This is the default selection. The information is grouped in 3 sections labeled STATUS, SET UP and TEMPERATURE. Under Status, there is a list of the various components of CSHELL which can take some time to change (moving the filter from point A to point B) or should be monitored (like the amount of time left in an integration). Each item may show 3 possible states. OK - This item is ready to receive commands. BUSY 99% - This item is currently in motion or in use. A new command concerning this item cannot be issued until it has completed its current motion. ERROR - A malfunction has occurred either in software or hardware. The software task should be initialized after inspecting the hardware related to that item. For example, a filter command will be accepted only when the filter status is OK. After the command is accepted, its status will change to BUSY. While the filter is moving, no new filter commands will be accepted and the percentage complete is updated to provide visual feedback. When the filter has reached its new position, the status will return to OK. The SETUP shows some important setup parameters. In the example, the CSHELL is currently using the SBRC array. TEMPERATURE displays the current temperature readings from the sensors. There are 4 sensors and their values are shown in Kelvin. Under the Status Canvas, there are 4 buttons labeled Status, Motors, TempCntl, About.... Selecting the different buttons will allow you to view the different status screen available. There different format are not explained in detailed here, but it is suggested you check them out. The Parameter's frame. The Parameters frame allows you to view and edit the most common CSHELL parameters. These parameter are separated into 3 groups: Observing, Setup, and Engineering. The first set of blue buttons on the Parameter's frame allows you to switch between these groups. You may view/edit each set of parameter by selecting the proper group. Each time you select a group the Parameter's frame appearance will change to display the appropriate parameters. The Observing Parameters. When you select the 'Observing' button on the Parameter's frame, it will display the most common parameters used while observing. Figure 6 is an illustration of the frame for Observing.  Figure 7 - Observing Parameter Frame The row of icons in the middle of the window represent mechanical components in the optical path. From left to right, each icon represents a component which can alter/redirect/block the light as it enters the CSHELL and travels through it. On top of each icon, the name of the component is shown. On the bottom, its current value or setting is shown. For example, look at the shutter's icon and you can see it is currently open. Each icon is colored gray or yellow. Yellow shows that an item is in the optical path, while gray shows you that an item is either blocked or moved out of the optical path. For example, if the Filter is set to blank, all the icons to the left will be gray since the filter is blocking the light. The other prompts and menu are usually self-explanatory. For a detailed explanation of each options, refer to the CSHELL Command Dictionary. For example if you wish to know what happens when you change the value for 'CVFWlen', look up 'CVFWlen' in the dictionary. A detailed explanation is provided. Special Notes: 1. Input a wavelength or wave number into the "Wavelen" parameter to move the grating to the desired wavelength. The CVF is also automatically changed to the proper wavelength. 2. Coadds is the number of coadds per beam. 3. Cycles determines the number of times an observing mode is repeated. 4. "ObsMode" determine how many beam switches are done. 5. After the 'Lastframe' label you are presented with 3 panel items: Buffer, -Dark, /Flat. These items control how the data is sent to the VF program upon reading out the array. In stare observing mode, data is sent to the buffer specified. In nod observing mode, after each object-sky pair, the difference frame is sent to the VF program. If the -Dark or /Flat is checked, a dark frame is subtracted from the data and it is divided by a flat frame. The 'MeanFrame' is also contain similar panels. If you do a GO with cycles greater than 1, you can calculate the mean of all the frames sent to VF. If a MeanBuffer is specified, each time data is placed into Lastframe-buffer, the mean of all the frame in the current cycle is calculated an placed into this buffer. The -Dark and /Flat, specifies the processing done when calculating the mean frame. In VF, there are two special buffers, a dark buffer and a flat buffer. You must load data into these buffers if you specify the -Dark or /Flat options. The Set Up Parameters. When you select the 'Setup' button on the Parameter's frame, it will display parameter not normally used while observing, but which should be reviewed during setup. Figure 7 is an illustration of the frame for 'Setup'.  Figure 8 - Calibration/Set Up Frame The items are usually self-explanatory. For a detailed explanation of each options, refer to the CSHELL Command Dictionary. Special Notes: Always select the Set Programmable Voltage button on the Setup page. The user's must set these voltages manually before take data with the SBRC array. The Engineering Parameters. When you select the 'Engineering' button on the Parameter's frame, the engineering parameter are displayed. These are parameters which should not be changed by casual observer. The Instrument Technician or support scientist can change them after inputting the password. You can view these parameters at anytime, but they can only be changed after the password has been entered. Figure 8 is an illustration of a sample frame.  Figure 9 - Engineering Parameters Frame For a detailed explanation of the options for each panel item, see the CSHELL Command Dictionary. The Save Parameters as a Macro File frame. Selecting the 'Save Parameter' menu item from the `Parameters' sub menu causes the Save Parameters as a Macro File command frame to appear. Through this frame, you can create a macro file of the current setting of the following parameters:  Figure 10 - Save Parameters Frame The panel items inside this frame are: DoPath - This text panel item identifies the sub directory used for accessing command or macro files. You may change this directory by editing this panel item. Filename - The macro file is created using this filename. You may change the filename by editing this field. Save - Selecting this button will execute the 'SaveSetUp' command, which crates a macro file using your current setup. Hide - Selecting this button will cause the frame to disappear from the computer screen. The Edit and Execute Files frame. XUI provides a way of creating and executing macro files. A macro file is a text file containing commands. There should be 1 command per line and the syntax for commands are defined in the CSHELL XUI Command Dictionary. In the Options sub menu, the choice 'Execute command files' brings up a command frame to create or edit files, and execute them.  Figure 11 - 'Do' Files command frame The following panel items will help you read, edit, and save the contents of macro file: DoPath - This text panel identifies the sub directory where your macro files are stored. DoFileMask - The file mask is a regular expression used with the path to determine the names of the files displayed in the file list. Selecting Update File List will re-initialize the list. Load File - Selecting this reads the file selected in the file list and places the text in the edit window. Clear text - Clear the edit windows buffer. Save as - Selecting this button writes the current text in the edit window into the filename shown in the text panel item. Record - This check box panel item controls the recording function. When the box is checked, any commands executed by XUI will also be written to the edit window. This allows you to write macro files using the mouse and panels items. The file list is identical to the one in the Execute Command Files frame. The sub directory and file mask is specified by the DoPath and DoFileMask variable which are shown in the Execute frame. To execute a command file, select the file in the list then click on the Execute button. XUI will read the file and execute each line. The commands and its error message ('Error None' when successfully executed) will be written to the Feedback panel on the Application's base frame so you can see what's happening. If you wish to abort a macro file in progress, click on the Cancel button. Moving the IC computer between the Summit & Manoa Because the PC is used both at the summit and Manoa, there are changes in some of the setup file which need to be done to allow it to work properly at each location. The manoa host name is 'cshell-manoa'. The summit host name is 'cshell'. This page identifies the changes required. This is mostly just a reminder for the IRTF programmer or technical staff. Cshell users can ignore this page. File: /bin/rc a. At the bottom of the file the rdate program is called to initialization the date and time at boot time. Additional line call programs at boot time to initialize the DIO board and PC-38 to mode friendly with CSHELL. Change the comment to use the approriation line. For example, on the summit it would be: #---------------------------------------------------------------- # Addition startup command added by Tony Denault, IRTF Programmer #---------------------------------------------------------------- /usr/local/bin/rdate herschel #/usr/local/bin/rdate wirth # These lines initializes the DIO48 board. It set the mode to # 0x82 (output, input, output) and write 0's to ports A, C. # /usr/local/bin/pc38io -o 643 -d 130 /usr/local/bin/pc38io -o 640 -d 0 /usr/local/bin/pc38io -o 642 -d 0 # This line initialize the PC-38 to power automatic mode. /usr/local/bin/pc38io ` rs;arpa;aspa;atpa;aupa;avpa;axpa;aypa;' File: /net/rc.network a. Insure the host name is correct. nsfpc is used on the summit. irlabpc is the manoa hostname. Look for the following lines and comment appropriately. hostname cshell #hostname cshell-manoa b. Look for the following line: # Mount remote NFS directories using the following format: # mount remhost:rem_dir_path_name local_dir_path_name mount wirth:/home/wirth /home/wirth The mount command should be commented on the summit. CSHELL XUI / IC Command Reference Array - Set the size and location of sub-arrays to be readout for r the next GO. These coordinate are relative to the physical device. You data is normally viewed rotated 90 clockwise. Prompt Array_icon on the Parameters screen, OBS page. Range x y wid hgt - The (x,y) location of the upper left corner and its width and hgt is specified. Please note that these values must be multiples of 8. Initial Full size (0 0 256 256). Syntax ARRAY x y wid hgt AutoSaveIC - Determines whether the data is saved by the IC program. Prompt Parameters window in the Setup page, Range Off - Data is not saved by the IC. On - The IC program on the PC saves the data. Initial Off Syntax AutoSaveIC { off | on } AutoSaveXUI - Determines whether the data is saved by the XUI program. Prompt 'AutosaveXUI' on the observing parameter's Obs page. Range Off - Data is not saved by the XUI. On - The XUI program on the SUN saves the data. Initial Off Syntax AutoSaveXUI { off | on } CamMode - Specifies the clocking and readout modes in the GO sequence. Prompt N/A Range Basic- Acquires single images with just the basic options. SIM- Simulation mode. Allows the software to be used with out the actual camera hardware. Initial Basic Syntax CAMMODE { basic | sim } ChgClkBias -.Changes the bias voltage to the clock/bias DAC. This is an engineering command. Prompt 'ChgClkBias' button on the Observing Parameter's Engineering page. Range Board 1 to 4. DAC 1 to 16. Volts: -10 to 10. Initial N/A Syntax CHGCLKBIAS board dac volt CoAdd - The number of intergrations summed together per beam or chop position in a GO. Prompt 'Coadd' on the observing parameter's Obs page. Range 1 ti 32000 Initial 1 Syntax COADD num Color - Indicate to the IC program whether the console supports color for text output. The character attributes for color or monochrome are selected based on this parameter. Prompt None Range OFF or ON. Initial OFF Syntax COLOR { off | on } Comment - Specifies a string to be place in the fits header of the saved file as a comment. Prompt 'Comment' on the observing parameter's Obs page. Range Any string up to 40 characters. Initial Undefined. Syntax COMMENT string Cycles - Cycles is a repeat factor in a GO sequence under basic mode. For the ObsMode NoiseImage, Cycles indicates how many frames will be used to calculate the noise. Prompt 'Cycles' on the observering parameter's Obs page. Range 1 to 1000. Initial 1 Syntax CYCLES num CVFwlen - When a CVF filter is selected, this parameter specifies the wavelenght for the CVF filter. Setting the CVFWlen update the user's order, which specifies which order to be used by grating to observe at the wavelen specified by CVFwlen. Prompt 'CVFWLen' on the Filter Wheel Dialog Box. Range 1.0 to 2.449, or 2.46 to 5.6 Initial 2.20 Syntax CVFWLEN num Die - This command stops the execution of the IC program. This command can only be executed from the IC program. Syntax DIE DiMirrorInit - The command to initialize the Direct Imaging Mirror. The DiMirror places the insturment in spectrscopic or imaging mode. Syntax DIMIRRORINIT Display - This command selects the various screen layouts on the IC program. This command can oly be executed form the IC program. Prompt XUi_PROMPTS Range 0 - Displays the most common observing parameters. 1 - Display the descriptive text parameters. 2 - Display the engineering parameters. Initial 0 Syntax DISPLAY num DoFastMode - Select the fast or slow clocking mode by setting Fastmode on or off. This is an engineering command. Prompt 'DoFastMode' on the observing parameter's Eng page. Range Off - Slow clocking mode. On - Fast clocking mode. Initial Off Syntax DOFASTMODE { off | on } DoFile - This command starts exection of a macro file. Prompt See Execute Command File in the XUI User's manual. Syntax DOFILE filename DoFileMask - This command sets the pattern string used in creating the file list on the Edit and Executed File window in the XUI program. This command can only be executed from the XUI program. Prompt 'DoFileMask' on the Execute Do Files window. Range Any string. Initial * Syntax DOFILEMASK string DoPath - This path identifies the subdirectory where the XUI program will search for DO or macro files. The $HOME and $DATE macros are supported. This command can only be executed from the XUI program. Prompt 'DoPath' on the Execute Do Files window. Range Any legal UNIX subdirectory Initial $HOME/macro/camxui Syntax DOPATH string DSPResetMSec - Specifies the amount of time in millisecond between array reset. Array resets are performed during idle periods. Prompt 'DSP Reset Msec' on the observing parameter's Eng page. Range 500 to 10000 milliseconds Initial 1000 Syntax DSPRESECMSEC num DSPSampleMode - Specifies the sampling mode used to readout the array during a GO. Prompt 'Sample Mode' on the observing parameter's Eng page. Range Single - A single sample is done by reseting the array. After the integration time has passed the array is readout to produce an image. Double - After an array reset, a pedestal image is readout. After the intergration time, a sample image is readout. The final image is the result of the sample minus the pedestal readout. Initial Double Syntax DSPSAMPLEMODE { single | Double } DTime - Specifies the dead time after a beam swith in seconds. Prompt 'Beamswitch DTime' on the observing parameter's Setup page. Range 0 to 10 seconds. Initial 2 Syntax DTIME sec EPassWord - The Epassword command allows you to enter a password. After entering the password sucessfully, any restrictive parameters (ie engineering) can be modified. Issing the command with an invalid password will cause those parameters to be restricted. Prompt 'epassword' on the observing parameter's Eng page. Range Any string Syntax EPASSWORD string Filename - The filename's prefix is used ot create filenames when saving data to disk. New filenames are constructed by concatendating Filename with the Image Number, then adding a file extension. For example, if Filename is '01jan' and image number is 45, the data file saved could be '01jan045.a'. Prompt 'Filename' on the observing parameter's Obs frame. Range A string of 8 characters Initial The current date in the form DDMMM Syntax FILENAME string Filter - Select a filter combination using the 2 filter wheels. The selection are indicated by the index values. Prompt Click on the FIlter Icon on the observing parameters window. Range 0 - CVF Wlen & Open 1 - 2.35 um NBF & Open 2 - 4.05 um NBF & Open 3 - He 1.083 & Open 4 - HI 2.167 & Open 5 - Both wheels blank 6 - CVF Wlen & Open 7 - 2.35 um NBF & Blocker 8 - 4.05 um NBF & Blocker 9 - 2.5 um Blocker 10 - 4.1 um Blocker Initial Blank Blank 2.20 Syntax FILTER { 0 | 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 | 10 } FilterInit - This command will initialize the filter wheels by moving them to their limit switches and then moving them to their initial position. Syntax FILTERINIT FIlterPos - Allows you to position the filter wheels to any step position. Normaily you may only offset the wheel position -100 or +100 steps from its normal location. After entering the engineering password, this restrictions is removed, but be careful of flashing the array in this mode. Range 1 to 40000 . Syntax FILTERPOS { A | B } step# [ {A|B} step# } ] Go - Performs a GO, which is a set of integrations. The GO command can take an optional parameter which determines the type extension for filenames in basic mode. Please read the section description of CamModes for a more complete description. Syntax GO [{ obs | dark | flat | comp }] GoInit - Initializies the go task in the IC program. The go task is responsible for controlling the DSPs and Array's electornics. Syntax GOINIT GoReset - Places the DSP in a reset operation mode. The go task's state will be change to ERROR. Syntax GORESET GratingInit - Initializes the grating. The grating is initialized by reading the step position from the encoder to set the step postion of the grating's stepper motor. Syntax GRATINGINIT GratingPos - Commands the grating's stepper motor to move to a specific step position. Syntax GRATINGPOS Range 100000 to 400000 GratingRMove - Moves the grating from its current position by a relative number of steps. Range -2000 to 2000 Syntax GRATINGRMOVE steps GWLen - Moves the grating to the indicated wavelenght. First the optimum order is calculated. The user's order is set to the optimum order. Then the step position of the grating is determined from the inputted wavelenght and this order. The grating is moved to this position. Prompt See 'WaveLen' command. Range 1.0 to 6.0. Syntax GWLEN micons ICHostName - The XUI program uses this hostname when initiating network communication to the IC program. This command can only be executed from the XUI program. Range Enter the hostname of the IC computer Initial cshell Syntax ICHOSTNAME name ICPath - The path identifies the subdirectory the IC program uses when writing data files. This command will create new subdirectories if path doesn't exist. Supports the $DATE and $HOME macors. Range Any legal unix subdirectory. 80 chars max. Initial $HOME/data/$DATE Syntax ICpath string ImageNumber - An ID number used to create the filename. See Filename for an example. Prompt 'Next Image Number' on the observing parameters Obs page. Range 1 to 9999 Initial 1 Syntax IMAGENUMBER num InstMode - Places the instrument in Spectrocopic or Direct Imaging mode by moving the Direct Imaging mirror out or in. Prompt 'Instrument Mode' menu is accessed by clicking on the Grating or DiMirror icon on Parameter's Observing page. Range S (Spectroscopic) Optical path is through grating. D (Direct Imaging) Blocks the grating Initial S Syntax INSTMODE { S | D } Itime - The amount of time the array is exposed between readouts, or the time interval for 1 Coadd. The minimum value is determined by the readout rate. Prompt 'Itime' on the observing parameter's Obs page. Range 0.1 to 3600.0 seconds Initial 1 Syntax ITIME sec Lamp - Turn off/on the calbration lamps This command automaticly move the lamp mirror out when the lamps are turned off, and in when the lamps are on. Prompt 'Cal_Lamp' icon on the Parameter window's Observing page. Range off AR - Argon Lamp KR - Krypton Lamp XE - Xenon Lamp Cont - Continuum Lamp Initial Blank Syntax LAMP { off | AR | KR | XE | Cont } LampInit - The command to initialize the lamp and lamp mirror by turning the lamp off and moving the mirror out of position. Syntax LAMPINIT LampMirror - More a mirror so the calibration lamp are out or in the optical light path. Range Out - lamps are out of optical path. In- lamp are in optical path. Syntax LAMPMIRROR { out | in } LastFrmBuf, LastFrmSubDark, LastFrmDivFlat - These are switches used by the XUI program to process each frame of data during a GO operation. LastFrmBuf identifies the buffer in the VF program which will display the data. When set, LastFrmSubDark and LastFrmDivFlat will cause some processing of the data frame by subtracting a dark and dividing by a flat. The dark and flat frames are identified by the VF program as the data loaded into buffer 5(Dark) and 6(Flat). Prompt 'LastFrame' on the Calibration/Setup frame. Range N/A Initial Buf = b0, -Dark and /Flat are off. Syntax LastFrmBuf {0 | 1 | 2 | 3 | 4 | 5 } LastFrmSubDark {off | on } LastFrmDivFlat { off | on } MeanFrmBuf, MeanFrmSubDark, MeanFrmDivFlat - During a GO you have the option of accumulating the data and displaying a mean frame at the end of each cycles. These parameters allow you control over this option. The MeanFrmBuf identifies the buffer in the VF program uses to display the mean frame. If set, MeanFrmSubDark and MeanFrmDivFlat will cause some processing of the mean frame by subtracting a dark and dividing by a flat frame. The dark and flat frame are identified by the vf program as the data loaded into buffers 5(Dark) and 6(Flat). Note: This option consumes much of the CPU's execution time and should only be used during GO with long integration times( greater than 15 seconds ). Prompt 'Meanframe' on the Calibration/Setup frame. Range N/A Initial Buf = N/A, -Dark and /Flat are off. Syntax MeanFrmBuf {0 | 1 | 2 | 3 | 4 | 5 } MeanFrmSubDark {off | on } MeanFrmDivFlat { off | on } Object Name - This information identifies the object you are observing and is placed in the fits header. Prompt 'Object' on the observing parameter's Obs page. Range Any string up to 40 characters. Initial 'Name of Object' Syntax OBJECT string Observer - This information identifies the observers and is placed in the fits header. Prompt 'Observer' on the observing parameter's Obs page. Range Any string up to 40 characters. Initial 'Your name' Syntax OBSERVER string ObsMode - The observing mode determines the beam switch pattern performed in a GO sequence and when in the sequence the files are saved. The obmode is identified by an index number Prompt 'Obs Mode' on the observing parameter's Obs page. Range 0 - Obj(A) integrates at the present beam position. This data is treated as an 'object' frame. 1 - Sky (B) integrates at the present beam position. This data is treated as a 'sky' frame. 3 - Pair (AB). In this mode, a pair of frames are taken. First the telescope is position at the A beam and a 'object' frame is taken. Then the telescope is positioned a the B beam and a 'sky' frame is taken. 4 - Noise Image. This is a special mode used to produce noise images. For each cycle a image is readout. Using these images, the standard deviation of each pixel is calculated. A frame is produced where each pixel position contains the standard deviation of that pixel position. These value are multipled by 100 to preserve decimal information. Initial 0 Syntax OBSMODE num Order - Set the user's order. The grating wavelenght is calculated based on the grating angle (step position) and an implied order. This implied order is called the user's order. Normal the user's order is set to the optimum order for a given wavelenght. This command allows you to change the user's order. Prompt None. Enter command at prompt. Range 8 to 60 Initial Optimum order Syntax ORDER num PVoltage - Sets the user programmable voltage's VDDUC and VDET on the clock bias board. Prompt The observing parameter's Setup page contains prompts for set the voltages. First input the appropriate values in VDDUC and VDET. Then select the 'Set Programmable Voltages' with the mouse to send these values. Range VDDUC range is -3.75 to -2.505 volts. VDET range is -3.75 to -2.505 volts. In addition, vdet >= vdduc and (vdet-vdduc)<=1.5 volts. Initial Undefined. You must initialize the voltage as part of your startup procedures. Syntax PVOLTAGE vdduc vdet PWindow - The PWindow variable indicates which parameter page should be displayed in the Observing Parameters frame. Prompt Set of Blue colored button in the upper-right corner of the Observing Parameter frame. Range 1 - Obs. Displays is most commonly changed Observing parameters. 2 - Setup. Displays the setup parameters. These parameters should be examine at the start of you observing session. 3 - Eng. Displays the engineering parameters. These are restricted parameters mostly dealing with the array electronics. Initial 0 Syntax PWINDOW { 0 | 1 | 2 } RotateImage - This option automaticly rotates the image clockwise 90 in the obsmode Stare and Nod. Prompt None. Enter command at command prompt. Range Off - No rotation performed. On - Rotates the image. Initial On Syntax ROTATEIMAGE { Off | ON } Samples - This parameter identifies the number of samples or times the array is readout to obtain the image for 1 coadd. Note that increased the number of samples will lower you noise, but will also increase you minimum integration time. This is a engineering or restricted command. Prompt 'Samples' on the Observing Parameter's Eng page. Range 1 to 256. Initial 1 Syntax SAMPLES num SaveSetUp - Ceates a macro file of some of the current parameter in the dofile directory. This command is used only by the XUI program. Prompt 'Save Parameters' on the main menu access the Save Parameters as a Macro file Frame. Syntax SaveSetUp filename SetMotorRdy - This command sets the status for all the motorized items (filter, dit, len, pplate) to the READY state. This command is intended for engineering purposes only. Since all item must in in a ready state before a GO is accepted, this command clears any ERROR condition due to mechincal failures. Do not attempt to move any motors which has been set ready using this command. This is an engineering or restricted command. Syntax SETMOTORDY Shutter - Selects a shutter wheel position. Prompt Shutter Range Open Close 2.5SPF Initial Close Syntax SHUTTER {Close | Open | 2.5SPF } ShutterInit - This command initializes the shutter wheel by searching for it limit switch, then moving the shutter to the closed position. Prompt None. Enter command at command prompt. Syntax ShutterInit ShutterPos - Allows you to move the shutter to an absolute step position. Prompt None. Enter command at command prompt. Range 0 to 4999 Syntax ShutterPos step# Slit - Select and moves to a slit wheel position. Prompt Slit Range 0.5, 1.0, 1.5, 2..0, 4.0, Blank, Open, J, H, K, L, L', M Initial Blank Syntax Slit {0.5 | 1.0 | 1.5 | 2..0 | 4.0 | Blank | Open | J | H | K | L | L' | M } SlitInit - Initializes the slit wheel by moving it into the limit and then setting it to BLANK. Prompt None. Enter command at command prompt. Syntax SlitInit SlitPos- Move the slit wheel to a step position Prompt None. Enter command at command prompt. Range 0 to 64000 Syntax SlitPos step# SlowCnt - When DoFastMode is OFF, the SlowCnt variable specifies the numbers of NOP's or delays in the DSP clocking algorithm. This effectively slows down the clocking pattern which lowers the readout rate and read noise. This is an engineering or restricted command. Prompt 'SlowCnt' on the Observing Parameter's Eng page. Range 1 to 100. Initial 1 Syntax SLOWCNT num Stop - During an integration or GO cycle, the stop command is used to abort the acquisition. Prompt 'Stop' button on the XUI's command frame. Syntax STOP SubArray - Load the size and position of the default subarray. These parameters are used when setting the subarray from the XUI's array icon on the Parameter's Observing page. These parameter refer to an unrotated image. This is an engineering command. Prompt 'SubArray' on the Parameter's Engineering Page. Range x, y, wid, hgt must be a multiple of 8. Syntax SUBARRAY x y wid hgt TCS - Using this command you may send a string to the Telescope Control System (TCS). This string is assumed to be a correct TCS command with a 40 character maximum limit. Range Any legal TCS command. Syntax TCS string TCSHostName - Identifies the computer host accepting TCS commands. Range The current TCS host is 'planck' Initial 'planck' Syntax TCSHOSTNAME name TempCmd - Sends a commands to any of CShell's two Temperature Controllers. Any string after the TempCmd is send to the temperature controller. Please refer to the Description of Hardware section or the temperature controller's manual for the correct syntax for the temperature control commands. Range Any legal controller command Syntax TEMPCMD { A | B } string TempRecord - TempRecord allows you to switch OFF/ON the recording to temperature information. When ON, the temperature information is appended to the file 'temper.log'. The recording interval is once every 5 minutes. Prompt 'TempRecord' on the Observing parameter's Eng page. Range OFF or ON. Initial OFF Syntax TEMPRECORD { off | on } VCCD - Selects the position for the visible CCD dichroic/Netural Density filter assembly. Prompt Click on the VCCD Icon on the observing parameters window. Range Out - VCCD Dichroic and ND filter out of light path. In - Places the VCCD Dichroic and ND filter in light path. Initial Out Syntax VCCD { out | in } VCCDInit - The command to initialize the visible CCD dichroic/Netural Density filter assembly. Syntax VCCDINIT VF - Commands VF from the XUI program. This command can only be executed from the XUI program. Range Any legal VF command. See the Command Dictionary for the VF program for syntax. Syntax VF command Wait - Sets the acquire or Go task busy for a time interval specified seconds. Range 0.1 to 60.0 seconds Initial N/A Syntax WAIT sec Wavelength- This command changes the value of the CVFWlen and GWLen. It is provide to allow the use to change the grating and CVF wavelenght with a single command. Prompt WaveLen on the Parameters window Observing Page. Range 1.10 to 2.449, 2.46 to 5.60 microns Syntax WAVELEN num XUIHostName - The IC program uses this hostname when initiating network communication to the XUI program. Range Enter the hostname of the workstation running the XUI interface. Initial Planck Syntax XUIHOSTNAME name XUIPath - This path identifies the subdirectory the XUI programs uses when reading and writing data file. Prompt 'XUIPath' on the Observing Parameter's Obs page. Range Any legal UNIX subdirectory Initial /scr1/nsfcam/data/DDMMM. Where DDMMM is the current date. For example, /scr/nsfcam/data/01jan. Syntax XUIPATH string Command - Describe_command. Prompt XUi_PROMPTS Range describe_parameters. Initial N/A Syntax SYNTAX What is VF? The VF software is a tool used to View Fits data files. A brief description of its capabilities are: Manipulate fits images of up to 2048 by 2048 pixels using 32 bits per pixel. Provides 8 buffers and 5 canvases for holding and viewing. Provide various mode of display such as imaging, histogram, line cut, plus other specialized modes. Allows the user to perform arithmetic operation on the fits data. Provides tools the calculate box photometry and statistics on pixels. Produces postscript files of graphics for hard copy output. Provides the ability for the instrument control software to send commands and data to VF. VF runs on a Sun Workstation under Sun's Openwindows software. It is an X windows application developed using the XView tool kit by the NASA Infrared Telescope Facility. The user interface conforms to the Openlook GUI Specifications. Before using VF, you should become familiar the Openlook User Interface. If you have questions or comments concerning VF, you may contact the author of the software via email at denault@.ifa.hawaii.edu or by calling the IRTF at (808)956-8101. Setting up your user account Since VF is an IRTF in-house software application, it is already installed on IRTF all workstations. If you wish to have this application installed on your own workstation, please see the IRTF computer staff for more information. This section will cover the setup information needed on you user account to run this application. To setup your account, you will need to know where the application is stored on the hard disk. Normally the IRTF will install it in /usr/local/VF, however you should check with the computing staff on this. The directory /usr/local/VF will be used as an example in this document. 1) Setting the environment variable $VFHOME. Create a environment variable $VFHOME to equal the name of the sub directory where the application is stored on your hard disk. For example, each user can place the following line in the .login file to set VFHOME to '/usr/local/VF': setenv VFHOME /usr/local/VF 2) Startup configuration file .vf-init. This step is optional, but highly recommended. When VF starts up, it searches for the file .vf-init in your home directory. If this file exist, VF expects it to contain VF commands. See VF Command Dictionary for the syntax. Using an text editor you can place instructions in this file to configure when it starts up VF. For example, the file may contain the following instruction to setup the directory paths and printer name. Path $HOME/protodat FileMask *.img DoPath $HOME/macro/vf DoFilemask * printer irlabpr Starting VF The VF program is a Xwindows application. You should be running an X server on your console. Openwindows is the default X server for sun workstations. There are two methods to start VF: 1. Starting VF using the workspace menu. The workspace menu has been configured to include a selection to start up an instance of the VF program. Press the menu (or right) mouse button on the workspace to bring up the workspace menu. Then click on 'Cshell" with the menu button to display its submenu. Select 'VF' with the select (left) button to begin execution of the VF program. 2. To start VF from a xterm or shelltool window, type 'vf' in the window. unix% vf & At this point the base window of the application should appear on your screen. Sometimes the following message may appear in your console window. Run VF without Sockets? (y or n) at the UNIX prompt 3) Hold down the right mouse button on the blue desktop 4) If the IC program is not already running (ASK a T.O. or Support Astronomer), Either: i) Select "Start CSHELL IC Software!" from the CSHELL menu or ii) Log into CSHELL IC console as "cshellic" 5) Select "Cshell XUI" from the CSHELL menu 6) Select "VF" from the CSHELL menu 7) Turn on the CSHELL Array Power Supplies (left on if cshellic is running) 8) Set Programmable Voltages in Setup Parameters XUI Window B. CSHELL Shutdown 1) Quit VF 2) Move Shutter, Slit, and Filter to "Blank" Position. Spectroscopic mode, turn lamps off. 3) Quit XUI software 4) Leave in this configuration unless powering off (proceed further only if powering off) 5) Turn off the CSHELL Array Power Supplies 6) Type "die" and in CSHELL IC window. Halt Lynx by logging in as "shutdown"; login as "reboot" if you only want to reboot the IC computer. C. CCD Guider Camera Startup: 1) Follow Steps A0 - A3. 2) Select "Login to CASSPC Guider PC" from CSHELL menu 3) Type "gic" and in the casspc window 4) Select "Guider XUI" from CSHELL menu Shutdown: 1) Quit Guider XUI 2) Type "die" and in GIC (casspc) window; exit window 3) Power Off Only: Login as oroot or sroot and type "reboot -ah" before power off or just type "reboot -a" to reboot only. C. Observing Techniques 1. Setting IR Array Bias Voltages The IR detector bias must be programmed to match the observing application. Using a single fixed bias (as done with the old NICMOS array) is inappropriate because of non-linearities and icky pixel artifacts in the SBRC 256 x 256 InSb arrays. Larger biases allow more electrons to be collected before saturation, but they also cause increased numbers of high dark current pixels (icky pixels) and low-level non-linearities. Fortunately, the icky pixels mostly disappear when object and sky frames are subtracted. Dark frames with exposure times equivalent to flat fields should be taken to subtract these pixels from your flats. The SBRC InSb arrays are not particularly linear near the tops or the bottoms of their integrating wells (see Appendix F), but linearity problems can be avoided if you expose your flats so that they have similar data counts to your object frames. You may coadd many flats to achieve high S/N. I recommend that you pick one of four following detector bias settings for you observations: ObservationBias (mV)WellVDDUCVDETXUI Do FileMost Spectroscopy3255000-3.7-3.375smallBright Thermal Spectroscopy5008400-3.7-3.200mediumBright or Thermal Imaging80015,500-3.7-2.900largeThermal Imaging with very high backgrounds100021,300-3.7-2.700huge Notes: Well: The maximum number of ADU counts (1 ADU = 11.0 electrons) that can be collected while not departing more than 1% from the linearity relation of the mid-well range. VDET & VDDUC are detector biases (Volts) that can be typed into the SETUP Parameters frame of the CSHELL XUI Application. XUI Do File is the name of a command file that can be executed from the Options menu of the CSHELL XUI application. These files automatically set the indicated bias levels. The bias voltages must also be set (execute DO File or push button in Setup Parameters Window) when the software is started. You must also use blockers if you ovbserve with the 1.10 - 1.57 mm CVF (see #9 this section). 2. Check For Read-Noise Limit and Saturation The minimum background-limited data value of each array is equal to the square of its read noise (in electrons) divided by the number of electrons per ADU. This value is approximately 100 for the SBRC InSb array in CSHELL as listed in I Table 3. Try to keep your data numbers above these values to avoid being limited by array read noise. The SBRC InSb array saturates at a level that is a function of detector bias as listed in the above table. Try to keep raw data values below the listed 1% linearity departure levels. It is good practice to check unsubtracted exposures for saturation. This may occur in frames with low mean counts if there is a bright OH line or thermal telluric line that is not seen in the A-B images. NOTE: When using the Direct Imaging Mode, you may find a black spot in the center of a bright star. This is a manifestation of gross saturation, and the numbers in the black area are meaningless. 3. Flat-fielding Flat-fielding is accomplished by taking spectra of a continuum source (usually a light bulb) that illuminates an integrating sphere (the same one that is used for the calibration lamps). One typically should obtain flats at the beginning of the night, whenever standards are measured, and at the end of the night. Flat fields should be taken for each observed wavelength observed. The grating and the CVF should not be moved between observing objects and flats in order to minimize wavelength shifts and ripples in spectra caused by interference in the CVFs. For most work, obtaining about 10 flats at an exposure of 1000 counts should suffice. They have similar data counts to your object frames if you are very concerned about linearity. For work requiring S/N 100 one should strive to get 25-30 flats at a time. Flats must be acquired with the same detector bias setting as your object data. We usually use the continuum lamp to generate flat fields at wavelengths l < 2.5 mm. The lamp does not produce many photons in the l ~ 3.5 mm range (due to opaque glass) but it usable. Its glass bulb is warm enough to provide an abundance of photons in the l > 4 mm region. You may also wish to try taking flats at l > 4 by using the thermal emission of the dome or mirror covers. You can try either taking long exposures of the continuum lamp or mirror covers for 3 mm < l < 4 mm, or else observing the dome target with the dome lights on. We do not yet have much experience in acquiring good flats at l > 3 mm wavelengths. 4. Focus And Collimation The collimation settings should be the same as that used for NSFCAM. Check with the T.O. to make sure that this is the case. The focus should be checked on a 7 - 9th magnitude star which the T. O. can find in the on-line SAO catalog. Use the Direct Imaging Mode, slit in the "open" position, and a few seconds of exposure time - using several coadds of shorter integrations if necessary - to integrate over seeing. At the beginning of the night, the focus is usually about +270 with the chipped secondary (~ +2.10 with the milled secondary) and it systematically drops (as the temperature drops) to about +2.30 (+1.85 with milled secondary) by the end of the night. The stellar image is typically less than 1 arcsec full-width-half-maximum (less than 5 pixels FWHM). 5. Tweaking the CVF for a Flatter Flat Whenever a new wavelength is entered, the grating and CVF are moved. The CVF suffers from internal reflections which cause an interference pattern in all spectra. The amplitude of this pattern varies from about 10 - 20% peak-to-peak, and it is quite sensitive to small changes in CVF position. If this fringing is particularly bad in your object or flat field data, you can try to minimize it by moving the CVF wheel (no more than 40 steps total) in small increments (5 or 10 steps). Be sure, however, to acquire all data (object and flats) for each wavelength at the exact same CVF and grating positions - do not move the grating or CVF in between data frames unless changing wavelengths. The CVF position can be seen in the Motors frame of the main cshellxui window. The CSHELL command Filterpos can be issued to move the CVF filter wheel a small amount. Consult the Hardware Reference (Appendix B) for the command syntax and to determine which CVF and wheel should be moved. 6. Darks Darks should be taken whenever flats are taken and the exposure time should be the same as the flats. Dark current is normally subtracted from object data when differencing object and sky frames acquired in Nod mode. Flat fields must have their dark current (and icky pixels) removed during the reduction process by subtracting separate dark frames. Darks must be acquired with the same detector bias setting as your object and flat field data. Close the shutter before taking dark frames. 7. Acquiring Objects To acquire objects, first determine the position of the slit on the array that you are using. Take an image of the slit in the Direct Imaging Mode looking at the sky or a discharge lamp (Kr or Ar).You should get an image of the slit with an integration time of a few seconds or less. Record the central column of the slit. It will change at each cool-down of the CSHELL, but it is usually near column 100. Move the telescope to the object you wish to acquire. Move the slit to the "open" position. Take an image of the field, and note the position of your object on the array (x,y coordinates). Use the Options menu of the VF program and select TCS. Use this window to compute the telescope offsets you need to center the object on the slit (the center of the slit will be near row 100). Note the position of the object in the CCD camera field when it is centered in the slit. You may mark this position on the TV monitor. Remember to insert the CCD filter (VCCD icon in CSHELLXUI) if the CCD bleeds due to excessive object brightness. 8. Slit Rotation The slit is normally positioned in the East-West direction. The primary reason for this is that tracking errors will not usually lead to a loss of signal. To obtain any other rotation angle, the entire instrument must be rotated using the IRTF instrument rotator. This requires manually rotating the instrument, a procedure taking at least 15 minutes and not something to do often. The default East-West slit position causes North to be located to the left and East down in the VF image display on the Sun workstation. The top of the slit (as seen in VF) is then rotated 270 East of North, and this angle is the default value in the VF TCS Coordinates frame. The slit location in the VF coordinate system is drawn on the bottom of the CSHELL cryostat for easy reference while rotating the instrument. Once the slit is rotated, enter the angle as defined in this convention in the TCS Coordinates frame of VF. This will allow you to easily position any object in the imaging field onto the slit by pushing the mouse buttons (see II.B and III.A for details). Please consult with your Support Scientist or Telescope Operator if you need to rotate the instrument. 9. Integrations and Nodding Prior to integrating, check the XUI path for the proper data location and change all of the appropriate parameters in the Setup Parameters window frame. These items need be checked only once each time the cshellxui software is started up. Next check and change (if necessary) the following parameters: Integration time: Seconds per exposure Coadds: Number of exposures per beam Cycles: Number of iterations of the selected observing mode Observing Mode: Stare or Nod LastFrame Buffer: Buffer into which the last exposure is stored MeanFrame Buffer: Buffer into which the average of the cycles are stored AutoSave: Check to have data stored into XUIpath directory EXAMPLE: Take the case of: Integration time: 2.0 Coadds: 1 Cycles: 4 Observing mode: Nod LastFrame Buffer: b0 MeanFrame Buffer: b1 This will generate 2.0 sec exposures, one exposure per beam, and 4 AB pairs (for a total of 8 separately stored exposures in ABBAABBA sequence). The last exposure is in buffer b0 and the running average of the AB pairs will appear in buffer b1. For each AB pair the telescope "nods" from position A to position B on the sky. The amount the telescope nods is set by the Telescope Operator, so inform him about how far you wish to nod (in arcsec). Motion E/W or N/S or both directions is possible for the nod. We recommend that you nod point sources along the slit with a throw of about 15'' in order to acquire object data in both the A and B frame positions. You must select the CVF/Blocker Option and also use the shutter wheel blocker (SPF) when observing with the 1.1 - 1.57 mm CVF! This CVF transmits l > 2.5 mm radiation, causing significantly increased background in your data if not blocked as prescribed. The blockers impart about a 10% reduction in flux over the 1.1 - 1.6 mm region. NOTE: Every exposure is stored onto the disk if the Autosave is enabled. The exposures are automatically named by the filename and the image number. For example if the filename is set to "data" and the image number is "0010", then the above example produces 8 files named "data0010.a", "data0011.b", "data0012.a", ..., "data0017.b". The extensions ".a" and ".b" refer to the A and B beams. 10. Observing Extended Objects When observing extended objects there will be additional concerns. First if the object fills the slit, the object must be moved off the slit for observations of the sky. Note that the sky exposure also contains ark current and other detector artifacts. These must be removed and therefore sky measurements are required. However, one loses about half of the total available observing time because of this. Second, any standard star measurement will cover only a few of the rows that the extended object covers. Hence the quality of the results may depend more on the quality of the flat-fields than anything else. It may be advantageous to use the Moon as a flat-field source if it is an appropriate standard, and you might want to drift-scan over it during exposures to smooth over any spatial features. However, keep in mind that the Moon has many solar absorption lines and it has albedo variations along the slit. It is far from being a satisfactory flat-field, but it may be handy for spectral regions that are relatively free of solar lines if you can find a relatively uniformly illuminated patch of the Moon. The moon should make a good telluric calibration source in the thermal IR (l > 3 mm). It is possible to automatically move the telescope a specified amount between exposures in order to map extended objects. For example, you can move in a vector parallel to the slit and 1 slit width in size between each exposure. This is done by writing CSHELLXUI macros (Do Files) that include TCS commands. Consult your support scientist or T.O. for help with this. 11. Command Files After taking data with the CSHELL you will find that many tasks are repetitive, such as switching to the imaging mode and back to the spectroscopic mode, setting up to peak up, setting up to observe, etc. These repetitive tasks can be put into an cshellxui "command file" and executed, thus saving time. More than saving typing, these command files can prevent loss of data by not having an important parameter set properly (like turning on auto save). See the CSHELLXUI and VF software guides (III.A) for more information on using command files. EXAMPLE: The following command files switch between imaging and spectroscopic modes and set the detector bias appropriately. They are the default image and spect macros: imagespect PVoltages -3.700 -3.200 ITIME 0.1 Cycles 1 Coadd 10 InstMode D Slit Open AutoSaveXUI Off PVoltages -3.700 -3.375 InstMode S Slit 1.0 ITIME 10 Coadd 1 Cycles 20 AutoSaveXUI On  Other commands may be included in command files, such as a Go command to actually start a sequence of exposures. The most commonly used command files, image, spect, goflat, and godark are in the directory ~cshell/macro/cshellxui . These files configure CSHELL to take images, take spectra, take flats, and take dark frames, respectively. The goflat and godark files contain a Go command, so they actually start a sequence of exposures once they are executed. Be sure to review the contents of a command file (by Loading it) before execution to make sure that it configures CSHELL properly and does exactly what you want. Commands to move the telescope (TCS commands) can also be included in CSHELLXUI Do Files. See the IRTF document, Computer to TCS ASCII Communications for a complete listing of TCS commands. As an example, the following macro will take an exposure, offset the telescope 1" N, expose again, offset again, expose again, and then return to the original position: tcs ABEAM tcs 1 0.0 0.0 -1 C.SCN echo Base Position go tcs 1 0.0 1.0 1 C.SCN wait 2 echo Moved 1 arcsec N of Base go tcs 1 0.0 2.0 1 C.SCN wait 2 echo Moved 2 arcsec N of Base go tcs 1 0.0 0.0 1 C.SCN echo Done; Returned to Base D. Observing Spectral Lines 1. Popular Astronomical Line List The following table lists the vacuum rest wavelengths of some commonly observed near-IR lines and band heads: MaterialTransitionNamel (mm)HI5-3Pb1.2822HI10-41.7367HI9-41.8179HI4-3Pa1.8756HI8-4Bd1.9451H21-0S(2)2.0388HeI2P-2S2.0587HeI4S-3P2.1126H21-0S(1)2.1218HI7-4Bg2.1661HeII10-72.1891H21-0S(0)2.2233H22-1S(1)2.2477CO2-0bh2.2935H21-0Q(3)2.4237HI10-53.0392HeII7-63.091H21-0O(5)3.2349HI9-5Pfd3.2970HI8-5Pfg3.7406H21-0O(7)3.8074H20-0S(13)3.8462HeI5-44.0490HI5-4Ba4.0522HI7-5Pfb4.6538H20-0S(9)4.6946 2. Night Sky OH Lines The following table list some night sky OH- lines in the J, H, and K windows that might be useful for wavelength calibration or other checks. Observed wavelengths are in vacuum, bl denotes a blend, and intensities are in units of photons s-1 arcsec-2. These data are taken from Ramsay, Mountain, and Geballe, 1992, M.N.R.A.S. 259, 751. Also see this reference for more lines. l (mm)Transitionv'' - v'Intensity1.0063Q9-53399.61.0263Q4-12276.31.0824Q5-2676.91.1430Q6-3825.71.2092Q7-4758.71.2660R branch8-5801.11.3072P(2) bl8-5602.51.4501P(1) bl2-0937.41.4582P(2) bl2-0929.91.4818P(4) bl2-0825.81.4873R(1)-R(7)bl3-11123.31.5170P2(1)3-11082.91.5235P1(1)3-13884.01.5319P(2) bl3-13556.21.5403P(3) bl3-12572.81.5524P(4) bl3-12259.91.5578R(2) bl4-21708.61.5622R(1) bl4-22483.41.5814Q4-26715.01.5946P2(1)4-21038.21.6018P1(1)4-23749.91.6059P2(2)4-21634.21.6108P1(2)4-24375.71.6217P(3) bl4-22960.21.6330P(4) bl4-21678.81.6434P(5) bl4-21574.5l (mm)Transitionv'' - v'Intensity1.6489R branch5-32021.51.6692Q5-36461.61.6891P1(1)5-33466.81.6944P2(2)5-31366.01.6992P1(2)5-33839.31.7061P2(3)5-31217.01.7101P1(3)5-32706.91.7235P(4),R bl5-3,6-41649.01.7367P(5), R(2)5-3,6-41917.21.7418R(1) bl6-41917.21.7639Q6-45821.01.9685R(1) bl8-61031.61.9756R1(0)8-61638.81.9845R2(0)8-6620.82.0270P1(1)8-62162.82.0315P2(2)8-61019.62.0400P1(2)8-62710.52.0897P1(5)8-6811.32.1110R(2) bl9-7853.52.1183R(1) bl9-7883.22.1250R1(0) bl9-71044.02.1518Q9-72201.22.1792P1(1)9-71533.72.1938P1(2)9-71550.62.2108P1(3)9-71461.32.2309P1(4)9-71081.7 3. Using Calibration Lamps and cal_lines CSHELL has three discharge lamps, Argon, Krypton, and Xenon. The Xenon lamp is mounted behind one of the other lamps, so its lines are very faint. Therefore the Ar and Kr calibration lamps in CSHELL are most useful for wavelength calibration of spectra. The following table lists their stronger lines (s = strong and m = medium intensity): Lampl (mm)Lampl (mm)Lampl (mm)Ar1.2706mAr2.154mAr23.1988mAr1.2806mKr2.1908sAr23.2882mAr1.2960sAr2.2083mAr23.3489mAr1.3012sKr2.2492mAr23.3890sAr1.6945sAr2.3140sAr23.490mAr1.7450mAr2.3852sAr23.5839sAr1.7920sAr2.3973sKr23.6345sKr1.8172sAr2.5132sAr33.8117mKr1.8701mKr22.8861sAr33.8419mAr1.9823mKr22.9477sAr34.0112sKr2.0215mAr2,H3.0101mAr34.0524sAr2.0323mAr23.0354mAr34.0879sAr2.0622sKr23.0488sAr24.6279sAr2.0992sKr23.0678sKr24.6694mKr2.1171sAr23.1808mAr24.7703s Beware that the discharge tube quartz envelopes absorb much of the radiation long-ward of 3 -4 mm; lines in the above table with wavelengths greater than 3 mm are difficult to detect due to this absorption as well as thermal emission by the envelopes. An auxiliary program, cal_lines, is used to determine which calibration lamp lines are to be used at a given wavelength selected for observation. The narrow spectral range of CSHELL usually prevents observing a calibration lamp in the same order as your object spectra, and cal_lines determines which order the lamp lines must be observed in. Position the mouse pointer in a UNIX text window on the Sun XUI computer, selecting it with the left button and bringing it forward if necessary. Type the following command in this window to display a list of calibration lamp lines which can fall on the InSb array when the grating is positioned for observing your astronomical line: cal_lines l(mm) | more where l (mm) is the desired central wavelength on the array. The list of available lines can be scrolled through by pressing the space bar on the keyboard. Alternately, this list can be printed by the laser printer with the following command in the UNIX window: cal_lines l(mm) | lpr These commands are also available on IRTF the workstation at H.P. One can print calibration line lists at H.P. by specifying the name of the H.P. laser printer (uh88pr) : cal_lines l(mm) | lpr -Puh88pr Now consider an example of using these commands to determine which calibration lines to observe if one is using the UNIX window on the Sun XUI computer. If we wish to observe HI Br g, l = 2.16609 mm wavelength, we issue the command: cal_lines 2.16609 | lpr which prints the following cal_lines table on the system printer: Central Vacuum Wavelength = 2.166090 microns: 4616.613 cm-1; order = 26 waveno line(vac. um) obs(um) order CVF(um) col(SBRC 256) Argon lines 6040.898 1.655383 2.164732 34 1.6564 56 6040.500 1.655492 2.164874 34 1.6564 63 7287.392 1.372233 2.163906 41 1.3736 15 7457.021 1.341018 2.166260 42 1.3409 133 7456.983 1.341025 2.166271 42 1.3409 134 Krypton lines 5321.816 1.879058 2.168144 30 1.8773 228 5321.150 1.879293 2.168415 30 1.8773 242 5502.887 1.817228 2.166695 31 1.8167 155 5502.884 1.817229 2.166696 31 1.8167 155 5856.639 1.707464 2.167166 33 1.7066 179 5856.272 1.707571 2.167302 33 1.7066 186 5856.275 1.707570 2.167300 33 1.7066 185 6032.254 1.657755 2.167833 34 1.6564 212 6393.989 1.563969 2.165496 36 1.5644 95 6573.027 1.521369 2.165025 37 1.5221 71 6929.652 1.443074 2.164611 39 1.4441 50 6929.652 1.443074 2.164611 39 1.4441 50 7276.638 1.374261 2.167104 41 1.3736 176 7276.638 1.374261 2.167104 41 1.3736 176 Xenon lines - Very Faint! 5321.059 1.879325 2.168452 30 1.8773 243 5856.272 1.707571 2.167302 33 1.7066 186 5856.275 1.707570 2.167300 33 1.7066 185 6039.008 1.655901 2.165409 34 1.6564 90 The first line of the output lists the central (vacuum) wavelength and wave number as well as the corresponding grating order for the astronomical line. The ensuing table lists the wave number, actual wavelength, apparent wavelength, grating order, CVF (order sorting filter) central wavelength, and approximate SBRC array column of each calibration lamp line. Note that no lines in the above example list fall in the same order (26) as the desired astronomical spectrum. We can observe lines in other orders by simply changing the CVF wavelength as explained in II.A. E. IRTF Computer Services 1. IRTF Mauna Kea Computer Facilities The current IRTF computer facilities on Mauna Kea include a Sun workstation, several PCs, and a PostScript laser printer on an ethernet network at the summit. These machines are also on a summit network that includes other Mauna Kea telescopes and the machines at Hale Pohaku. Currently the IRTF has a Sun workstation at Hale Pohaku that is available for data archiving, reduction, etc. during your run. These machines on the summit network are only reachable through U.H. Manoa machines via Internet, so you must make arrangements with your support astronomer if you need access to them before or after your CSHELL observing run. You should obtain a guest observer account when you arrive at Hale Pohaku by logging into the IRTF workstation as guests. Use this account for all activities while at the IRTF. It will expire 3 days after your run. 2. Archiving Your Data The recommended data archiving procedure is to copy each night's data files onto a separate 4 mm or 8 mm tape. Additionally, we recommend that you archive the data from all nights of your run onto a single tape if you have time at the end of your last night. This will ensure redundancy of your data in case some of your tapes are unreadable at your home institution. Our current housekeeping procedure is to keep data on the Sun computer's (herschel.ifa.hawaii.edu) disk for 1 week, then compress the data (UNIX format) and retain it for another week before erasing it. Be sure to read your data tapes as soon as you get back to your institution; your data will be completely erased from our computer two weeks from the date it was taken! Be sure to bring plenty of tapes (at least 1 per night + 1) for your run. We use the UNIX tar command (Tape ARchive) to transfer CSHELL data onto the tapes. Data are stored in FITS format and are readable by IRAF. The following procedures for data archiving, listing tape contents, and restoring tapes require that you issue their proper UNIX commands from the Sun console or other UNIX window. The 8 mm tape drive is located adjacent to the IRTF workstation named wien at Hale Pohaku, so 8 mm tapes must be written from Hale Pohaku. Wien's UNIX device name for the 8 mm tape drive is /dev/rst0 (or /dev/nrst0). The 4 mm tape drive is located adjacent to the IRTF summit workstation named Herschel, so 4 mm tapes must be written on the summit. Herschel's UNIX device name for the 4 mm tape drive without compression is /dev/rst0 (or /dev/nrst0). Tar writes data into 20 block records by default. The following examples show how to archive your data onto either drive. Sometimes we store data in other directories besides /scr1/cshell/data illustrated below; if your data is in a different directory you must substitute its name in the following commands. ARCHIVING 1 NIGHT'S DATA Commands: cd /scr1/cshell/data ls tar -cvf /dev/rst0 directory These commands will switch to the CSHELL data directory, list the nights there, and copy your night's data onto the tar tape. You must substitute your night's data directory name for directory in the above tar command. You should see the name of this directory when you execute the above ls command. These directory names are usually of the form ddmon, e.g. 30aug . ARCHIVING SEVERAL NIGHTS' DATA Commands: cd /scr1/cshell/data ls tar -cvf /dev/rst0 date1 date2 ... PRINTING A TAPE'S TABLE OF CONTENTS Commands: tar -tvf /dev/rst0 or: tar -tvf /dev/rst0 | lpr The first command will list the names of the files of a tape archive to the Sun computer screen. The second command will print the names of the files on the system (laser) printer. The second command may take 10 - 20 minutes to execute without any confirmation until the pages are printed and the tape is rewound - be patient! SEVERAL ARCHIVES ON 1 TAPE You may append data onto a pre-existing data tape, but this creates a new archive at the end of the existing one rather than appending the old one. This makes the tapes more confusing to write and read, and we do not recommend using his technique unless you must. It is most convenient to use the drive without rewinding it (use the /dev/nrst0 device name) if you go this route. Sequentially enter any of the above commands (once for each archive) using /dev/nrst0 instead of /dev/rst0. Rewind the tape manually when you are done: mt -f /dev/nrst0 rewind READING YOUR DATA TAPES You can usually read your data onto your home UNIX computer with the command: tar -xvf /dev/rstx where /dev/rstx is the device name of your 8 mm tape drive. 3. Anonymous FTP and WWW Site Information The IRTF maintains an anonymous FTP site called IRTF On-line, providing remote access to documentation and data reduction aids for IRTF observers. This site is on the machine irtf.ifa.hawaii.edu (128.171.79.135), and the information on it is accessible through the FTP (File Transfer Protocol) service of the Internet. If you have access to a machine on the Internet, then you may retrieve copies of this information. This archive is also reachable through the IRTF World Wide Web (WWW) home page (http://irtf.ifa.hawaii.edu/). Check it out! All CSHELL information is kept in the directory /pub/IRTF/CSHELL . This directory contains instrument documentation (including this manual), data reduction information, and some IRAF scripts and bad pixel masks that are useful in reducing CSHELL data. The current directory contents are kept in the README.txt file. Currently the CSHELL directory contains two directories, one for documentation and one for IRAF data reduction aids. The Docs directory contains the files: starting.ps I and II of this CSHELL User's Manual swref.ps.Z CSHELLXUI and VF documentation ( III.A of this manual) data.txt Text of Data Reduction Guide in III.F.2 of this manual line_form.ps CSHELL Line Set Up Form (from Appendix A of this manual) logsheet.ps CSHELL Logsheet (from Appendix A of this manual) manual_v2.ps.Z This entire CSHELL User's Manual manual_v2.word.Z CSHELL User's Manual in MS Word format (Macintosh 5.1) Here is how to access the information in IRTF On-line. First log on to IRTF On-line by typing the following commands on your Internet host: ftp irtf.ifa.hawaii.edu (or ftp 128.171.79.135) (use "anonymous" when prompted for "Name" and use your email address as a password) Now switch to the CSHELL directory: cd /pub/IRTF/CSHELL List the files in the directory: ls Retrieve the README.txt file which describes the CSHELL archive contents: get README.txt End your session: quit You may read the README.txt file on your local machine to see what is in the archive, and then FTP back to hubble.ifa.hawaii.edu to get the files you want. We plan to update the archive contents regularly, and we welcome your submissions. F. CSHELL Data and its Reduction 1. CSHELL FITS File Header Example SIMPLE = T / DATA IS IN FITS FORMAT BITPIX = 16 / bits per pixel. Two comp. Integers NAXIS = 2 / NUMBER OF AXIS NAXIS1 = 256 / PIXELS ON 1st MOST VARYING AXIS NAXIS2 = 256 / PIXELS ON 2nd MOST VARYING AXIS DATAMIN = -82 / MIN DATA VALUE IN FILE DATAMAX = 2795 / MAX DATA VALUE IN FILE DATAMEAN= 12 / MEAN DATA VALUE IN FILE ASEC_PIX= 0.20 / PLATE SCALE in arcseconds/pixel DIVISOR = 1 / Normalization value ORIGIN = 'Institute for Astronomy' TELESCOP= 'NASA IRTF' INSTRUME= 'CShell Spectrograph' OBSERVER= 'Your Name' OBJECT = 'HD129653 K=6.92' COMMENT = 'Comment for fits frame' IRAFNAME= 'hd1290019.a' BEAM = 'A' / Object(A) or sky(B) IMAGETYP= 'object' / Type of image TIME_OBS= '11:50:38.06' / UT TIME OF ACQISTION ('hh:mm:ss.ss') DATE_OBS= '07/05/94' / UT DATE OF ACQUISITION ('dd/mm/yy ') ITIME = 60.0000 / INTEGRATION TIME IN SECONDS CO_ADDS = 1 / NUMBER OF INTEGRATIONS OBSMODE = 1 / obsmode is Nod (AB) CYCLES = 1 / Number of cycles INSTMODE= 0 / Instrument Mode is S GPOS = 235523 / Grating step position GANGLE = 63.509 / Grating Angle ORDER = 26 / User's Order GWLEN = 2.17000 / Grating's wavelength FILTER = 0 / Filter is CVF Wlen/Open CVFWLEN = 2.1700 / CVF Wavelength FILTERA = 'AF4 (Open)' / StepPos 1166 FILTERB = 'BCVF1 (1.33 to 2.449 CVF)' / StepPos 4540 SLIT = 3 / Slit Wheel is 2.0 LMIRROR = 0 / Lamp Mirror is Out LAMP = 0 / Lamp is Off SHUTTER = 1 / Slit Wheel is Open VCCD = 0 / VCCD is Out ARRAY = 0,0,256,256 / x,y,wid,hgt of data array SAMPLES = 6 / Number of Samples SAM_MODE= 2 / 1=SINGLE, 2=DOUBLE FRM_RATE= 6 / In msec. Fastmode=Off SlowCnt=1 Samples=6 RESET_MS= 1000 / Idle Resets in msec. TEMP01 = 30.00 / A_T1 InSb Array Temp TEMP02 = 72.20 / A_T2 Grating Temp TEMP03 = 180.00 / B_T1 CCD Temp TEMP04 = 71.40 / B_T2 ColdBox Temp TPD = ' 14:40:38.81 36:58:26.5 01:49:28.21 1.143 1950.0 -O' RA = 14:40:38.81 / Right Ascension DEC = 36:58:26.5 / Declination HA = 01:49:28.21 / Hour Angle AIRMASS = 1.143 / Air Mass EPOCH = 1950.0 / Epoch VDDUC = -3.700 / Programmable voltage VVDUC VDET = -3.375 / Programmable voltage VDET END = / the end 2. Data Reduction Guide with IRAF Examples Point Source Data Reduction Note: Data should have been taken in nod mode (AB or ABBA, object is in both A and B beams and nodding along the slit) 1) Flat Fields a) combine the flat-field images: e.g. IRAF function 'imcombine' with avgsigclip b) combine dark images: e.g. IRAF 'imcombine' c) flat = a) - b) : e.g. IRAF 'imarith' d) fix badpixels using the badpixel mask: e.g. use fix.cl IRAF script e) normalize the flat-field, producing a frame called 'normflat' 2) Object Data a) form differences A1-B1, A2-B2, ...B1-A1, B2-A2, ...: e.g. IRAF 'imarith' b) combine the differences for each beam to give an A image and a B image: e.g. IRAF 'imcombine' c) divide each by the normalized flat-field: e.g. IRAF 'imarith' d) correct for badpixels with the mask: e.g. use fix.cl IRAF script e) Examine the images for any additional bad pixels or other problems f) You may save disk space by stripping out NICMOS image areas where there is no data e.g. use strip.cl IRAF script 3) Do the same for the standard star data, if any. 4) Extract the Spectra The IRAF noao.twodspec.apextract package is well-suited to this. The three extraction steps can be done interactively at once with the APALL task (dispaxis = 1) : a) EDIT the aperture and width (and any background regions subtract) b) TRACE the aperture, defining its position as a function of position across the frame c) EXTRACT the one-D spectrum from the frame 5) Extract Calibration Spectra (based on spectral lamp data) Assuming n>=1 images with n>=2 lamp lines (often in different orders): a) combine the images to be used: e.g. IRAF 'imcombine' or 'imcopy' b) extract a calibration spectrum for each beam (A,B) such that the calibration data are extracted from the same part of the image as the object data. Do this using APALL, setting 'referen' and 'profile' to the object data image, and do not edit or trace the aperture. We now have 1-dimensional spectra 6) Wavelength Scale Data (using noao.onedspec IRAF tasks) a) for each line in calibration spectra, convert the line wavelength to the equivalent wavelength in that order (done in cal_lines program) b) use 'IDENTIFY' to fit a wavelength scale to the spectrum c) use 'REFSPEC' to assign that wavelength scale to object spectrum (careful to apply the A calibration to the A spectrum, etc.) d) use 'DISPCOR' to produce a dispersion correct spectrum for each beam 7) Reduce the standard star data in the same way 8) Divide each object spectrum beam by the appropriate standard star beam 9) Combine All Spectra Since the A, B beams will have, in general, different wavelength scales, use the function 'COMBINE' (noao.onedspec IRAF task), which will resample the spectra and average them. This is the final spectrum. 10) Plot the final spectrum using SPLOT (noao.onedspec IRAF task), which can compute equivalent widths, display wavelenght and intensity units, etc. Extended Emission If your object is extended along the length of your slit, then the standard point source spectral extraction technique outlined above will probably not work optimally. First perform the frame arithmetic outlined in steps 1) - 3) above. Divide the object and standard star data by the normalized flat. Telluric correction: you may divide the flat-fielded object data by a flat-fielded standard star frame which has been artificially extended along the slit direction, but it is best to rotate the images first so that the slit is exactly perpindicular to the dispersion axis. Additional background subtraction can be done with BACKGROUND (IRAF noao.twodspec.longslit task), and then you should register all frames by moving them along the slit direction. IDENTIFY (IRAF noao.twodspec.longslit task) will allow you to measure the centroid of flux peaks interactively, and IMSHIFT (IRAF images task) allows you to shift the images to a common center. Combine all shifted images with IMCOMBINE (IRAF images task). What you do from here depends on what you want to get out of the data as well as its morphology. G. Using the CSHELL CCD Guider Camera The CSHELL CCD is now a scientific-grade Tektronix 512 x 512 pixel CCD which is operated via IC and XUI programs like other IRTF instruments. Its startup and shutdown instructions are given in III B. It can be operated in a continuous mode for acquisition, a single exposure mode, or an auto-guide mode. The CCD is clocked at a rate of 333,000 pixels / sec, so it takes just under 1 second to read a frame; this limits the minimum exposure time also. The CCD views the same field as the IR array and is not obstructed by the slit or other apertures. It looks through an IR-reflecting dichroic which has a pass band similar to an R-band filter. A 1000x attenuation filter can be switched in front of the CCD for observing bright objects (VCCD icon in CSHELLXUI). Pixels can be binned in software (1x1, 2x2, 4x4, or 8x8) to improve signal-to-noise. N is up and E is to the left on the CCD monitor (or in VF) when CSHELL is mounted in its normal E-W slit configuration. The CCD has a 55" (E-W) x 65" (N-S) FOV, 0.15"/pixel plate scale, and V=17 mag limit. CCD images can be automatically sent to VF for display by selecting the View IC Data checkbox. Once in VF, they can be saved as FITS files via the VF Save Data menu choice. It takes several seconds to send each frame to VF, so continuous readout mode will slow considerably if this option is selected. The guider should be operated as follows. 1) The TO should start the gic program (on max) at the start of each night. The observer should not start the gic. Starting the gic is done by logging into casspc with the login "guider" (no password). Then type "gic" and a carriage return to start the gic. 2) The observer should start the Guider XUI software (by selecting "Guider XUI" from the CSHELL OpenWindows menu) whenever he wishes to take images with the CCD for guider acquisition. He should optimize exposure time, set the proper binning (e.g. 2x2 or 4x4 for better sensitivity in bad seeing or 8x8 to be able to guide on Jupiter's or Saturn's large disk), select the 1000x CCD filter if needed (Cshell XUI), return the software to "Single Shot" frame mode, and then QUIT the Guider XUI before asking the TO to View or automatically guide with the CSHELL CCD. The observer should repeat this step whenever a new object is acquired. The observer will not be notified of CCD hardware timeouts or be annoyed by guider frame beeps when the Guider XUI is not running. This is a good thing! 3) The TO should use the IRTF guide program to autoguide with CSHELL. The rotation angle for the CSHELL CCD guider should now be approximately (within 3 degrees) the same as the CSHELL IR slit rotation angle entered into the VF TCS Coordinates Window by the observer. This angle is the position angle on the sky of the top of the CSHELL slit as seen in VF. 4) If the gic software has a hard failure (e.g. unrecoverable socket errors), then the TO should shut down the gic software (type "die" and a in the gic window) and restart the gic. If errors recur, then shut down the gic, exit from cass pc, login to cass pc as oroot, and then reboot casspc with the "reboot -a" command. Wait a minute or so and then login to casspc as guider and restart gic. The guider software commands follow: GIC / GUIDER XUI Command Reference do_stats() - Sets the calculation of stats on the DSP Syntax: stats { Off | On } do_array() - Sets the array type Syntax: array { 64 | 512 } do_scale() - Sets the type of scaling on the DSP Syntax: scale { None | Fixed | Auto | Slice} do_autodata() - Sets the transfer of 32 bit data from the DSP Syntax: autodata { Off | On} do_cammode() - specify clocking and readout program. Syntax: cammode {singleshot | simulation} do_coadd() - Set number of coadds on DSP Syntax: coadd {n} do_color - determine what character attributes the kbio process uses to update the parms window on stdout. syntax: color { no | yes } do_cycles() - Set the number of image cycles on the DSP Syntax: cycles {n} do_die() - quits the program. Syntax: die do_go() - Performs a GO. (starts integration sequence) syntax: go do_goinit() - send a init message to the GO task. GO can be initialized at anytime. syntax: GOInit do_goreset() - send a RESET message to the GO task. syntax: GoReset do_itime() - Set integration time in seconds Syntax: itime {seconds} do_zoom() - Sets the display window zoom factor Syntax: Zoom {mag} o_window() - Sets the size and location of the stats/display window. Only this part of the array will be scaled and displayed. Syntax: Window xoffset xsize yoffset ysize do_range() - Sets the range for fixed scaling Syntax: range {min} {max} ddo_senddata8() - Asks guider to send 8 bit data. Writes data to file "guider.img" Syntax: Senddata8 do_sendinfo() - Send status information. Just a dummy, since info is always sent. Syntax: Sendinfo do_register() - Set up the array control signals Syntax: register {0xnn} do_sync() - Synchronizes the DSP and TEK DEV. Syntax: sync do_slice() - Sets the LSB for slice. Syntax: Slice {bitslice} do_simulate() - Set the simulation on the DSP Syntax: simulate { Off | On } do_status() do_stop() - Stop the latest integration Syntax: stop do_tcs() - Send a string to the TCS computer. This string is assumed to be a correct TCS Command w/ 40 chars max. This command uses the GO task to communication with the TCS. Thus the GO task must be ready before continuing. Syntax: tcs {command string} do_tcshostname() - the host providing the data socket port. Sytnax: tcshostname {hostname} do_viewicdata() - Sets the viewicdata mode for the IC program Syntax: viewicdata { Off | On } do_wait() - Sets the acq task busy for N seconds. Syntax: wait {seconds} do_xuihostname() - the host providing the data socket port. Syntax: xuihostname {hostname}  IV. Appendices A. Observing Log Sheet and Line Settup Form  CSHELL Line Setup Form Line Name _________________ l __________ mm n __________ cm-1 Order __________ qg __________ Ng __________ Filt. Pos. ______________ Lampn (cm-1)l (mm)lobs (mm)OrderlCVF (mm)colpredcolobs________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________________Other Lines Line (telluric, object, or sky)l (mm)colobs_______________________________________________________________________________________________________________ Dispersion: _________________ (mm/pixel) _________________ (km/sec/pixel) Comments: _______________________________________________________________ ________________________________________________________________________ B. CSHELL Hardware Reference  Figure 1. CSHELL Filter Wheels. Inner numbers are degrees, outer ones are motor step positions. The filter wheel are controlled from the PC-38. Filter A is on the 'r' axis. Filter B is on the 's' axis. The following tables display the name and position of the filters on Filter A and FilterB: .   The filter menu selection and the position of wheel A & B are indicated by this table.  When menu index 0 or 7 are select in order to use the CVFs, the positions of the wheels are calculated from the following tables. Search the table until you found the first row which include the wavelenght you are using. The "CVF Used" column indicated which filter is used. The step position are calculated from the coefficients found in the columns "Motor Position Equations Terms". For the other filter, the Blocker or Open position is given by the "Position of Other Wheel" column.  Figure 2. CSHELL Slit Wheel. Inner numbers are degrees, outer ones are motor step positions.  The Slit wheel is control from the PC-38 from the 't' axis. Note the slit wheel has multiple Blank and Open positions. When selecting a Blank or Open, the software will move the wheel to the nearest Blank or Open.  Shutter Wheel  The Shutter wheel is controlled from the PC-38 from the 'v' axis.  RS-232 Devices To communication with serial devices the CSHELL IC computer is equipped with a 4-COM Serial Port Adapter by STB Systems, Inc (214-234-8750). The configuration of the serial board is as follows: Port I/O Base IRQ Comments COM1 0x3f8 IRQ4 Atttached to TC#1 COM2 0x2f8 IRQ3 Attached to TC#2 COM3 0x3e8 IRQ10 Attached to Encoder COM4 unassigned Temperature Controller CSHELL uses two series 9620 Temperature Controller by Scientific Instruments, Inc. The controller communicates to the IC computer via the serial ports. The TempCmd command allows you to communicate with the temperature controller using its native instructions outlined in its manual. These instructions are summaried here for your convinence. FUNCTION SYNTAX EXAMPLE Input the Setpoint Snnn 'S400' sets the setpoint to 40.0 Kelvin. Input Proportional Term Pnn 'P50' sets the proportional term to 50. Input Integral Term Inn 'I20' sets the integral term to 20. Input Derivative Term Dnn 'D20' sets the derivative term to 20. Get Temperature Setpoint S 'S' will return the Setpoint. Get Proportional Term P 'P' will return the proportional term. Get Integral Term I 'I' will return the integral term. Get the Derivative Term D 'D' will return the derivative term. Get Heater Ouput H 'H' will return the heater output. Get Temperature T1 T 'T' will return the T1 temperature. Get Temperature T2 t 't' will return the T2 temperature. Toggle Control Mode X 'X' will toggle the heater off/on. Please note that the syntax is case senitive. The syntax for the command to the IC to sent temperature commands is: TEMPCMD {A | B} command Encoder The default encoder parameters are: SN = 0 SP = 01 SE = 0 AR = 0 SD = 0 SO = 0 SF = 025000 CSHELL's RACKMOUNT SETUP CSHELL Instrument Control computer is a 20 slot 386/20 Rackmount PC-AT computer. This section attempts to documents the setup the various peripheral board install in the PC. Ethernet Card The ethernet card for the PC is a SMC EtherCard Plus Elite16. This is the default card supported by lynxOS. We have configured the board to be compatiable with Lynx. The board is setup as follows:  MM-96 Detailed Setup CSHELL uses two MM-96 DSP to provide clocking and buffer board functions. The clock DSP make no use of any DRAM. While the BCARD DSP uses the additional DRAM (up to 16Mwords) in speckle and movie mode.  The CSHELL project purchased the following DSP boards. Two full boards were initially purchased.  PC-38 Stepper Motor Controller An Oregon Micro System's PC38-8 board is installed to control the stepper motors for NSFCAM. The board is configured as follows:  J47 Limit sense jumpers: [:] : : : : : [:] [:] J15 Address Select Jumbers: [:] [:] [:] : [:] [:] : : = 0x320 J17 Interrupt and DMA Jumpers: : : : : : : : : No Ints. J67 User I/O Pull-up Jumpers: : : : : : : : : J57 I/O Configuration Jumpers: [:] : [:] 0-3 inputs 8-11 outputs 4-7 inputs DIO48 CSHELL make use the the DIO48 Digital I/O board to provide additional I/O bits. Cshell only utilities/programs 1 or the 2 available 8255 for digital I/O. The timera are not used. (Note: The wire wrap between the timer and some DIO lines are left in place from the echellc I project (NICMOS & SBRC 64 control). I/O Base: 0x280 Interrupts: None The 8255 #1 connected to J0 is initilaized using Mode 0x82. Port A - Output Port B - Input PB0 - Lamp_limit_off PB1 - Lamp_limit_on PB2 - vccd_limit_off PB3 - vccd_limit_on PB4 - dimirror_limit_off PB5 - dimirror_limit_off Port C - Output PC0 - Lamp_mirror_cntl PC1 - vccd_cntl PC2 - dimirror_cntl PC3 - UNUSED PC4 - AR Lamp* PC5 - KY Lamp* PC6 - Xe Lamp* PC7- Cont. Lamp* * Note currently the DIO48 is onlu used on control the Lamps. The additional definition are specified incase we switch the DC motor control from the PC-38 IO bits to the DIO48. SVGA Board CSHELL uses the SVGA board as a text only output device. Any generic VGA board will do. C. Troubleshooting CSHELL is a mighty instrument but is not immune to failure. We have attempted to identify common possible failures, and here we list their modes and possible fixes. Always get help from your support scientist, telescope operator, or other IRTF staff person. We now examine some possible failures and their fixes. Mojo Motor Madness Each CSHELL mechanism is controlled by a stepper motor or other actuator. Sometimes these motors, their mechanisms, or their electronics fail in various ways. Sometimes a mechanism will never become READY at startup of the cshellic software; it will stay in the INIT or ERROR modes instead. Most mechanisms may be initialized by commands typed in from the cshellic or cshellxui machine keyboards; see III.A for details. For example, if the Slit process shows an ERROR or INIT condition that never clears in the cshellxui status window at startup, then you can attempt to clear the condition by issuing the SlitInit command. Sometimes such initialization commands must be repeated several times to clear an ERROR or INIT state. These initialization commands may also be executed if a mechanism generates an ERROR or continuous INIT state during normal operation. INIT states sometimes take 2 or 3 minutes to clear to READY; wait some time before attempting to re-initialize the mechanism. If a more serious errors occurs, such as the filter or slit wheels not moving to the correct locations, the shut down and restart CSHELL as directed in III.B. If this clears your errors, then CSHELL is safe to operate. If it does not clear your errors, then you can force CSHELL to ignore the problem by issuing a setmotorrdy command (see III.A). CSHELL will be OK to use if you do not need to move the offending mechanism. The nature of a failure should be reported, investigated and documented Filter and Slit Wheels Positions of filter wheels and the grating can be examined from the cshellxui Motors frame of the program's main window pane. Motors can be commanded to go to specific step positions (see commands in III.A). It is useful to try to move them forward as well backward in order to isolate the failure. Beware that filter wheel A is labeled wheel 1 and filter wheel B is labeled wheel 2 on the CSHELL dewar. See Figure 1 in the CSHELL Hardware Description (Appendix B) for positions of the various filters on each wheel (also see the CSHELL Filters notebook), and see Figure 2 in the CSHELL Hardware Description (Appendix B) for positions of the slit wheel. The conversions between wavelength and step position are given for each CVF in the following table: CSHELL CVF Position Table CVFWavelength Range Wavelengths Used Motor Position EquationACVF11.10 - 1.57 (mm)1.10 - 1.569 (mm)13495.61l(mm) - 10609.83BCVF11.33 - 2.50 (mm)1.57 - 2.449 (mm)1.480l2(mm) + 2838.225l(mm) - 1625.656BCVF22.46 - 4.54 (mm)2.46 - 4.35 (mm)BCVF34.27 - 5.60 (mm)4.35 - 5.60 (mm) Other Problems CSHELL can experience other problems also. The following table lists some possible problems and suggested remedies. SymptomSolutionManual Sect.Array or Cold box Temperature is wrongCheck dewar for liquid nitrogen, make sure closed-cycle cooler is on, check controllers.  II.A, Appendix DNo Calibration Lamp linesCheck cshellxui status window, check filter wheel positions in Motors window, make sure lamps are on (look in holes in cal box), check instrument power and cablesIR Array Data Values are Funny or near-zeroProgram bias voltages with Set Programmable Voltages (Setup) II.CExcessive or Intermittent NoiseCheck cable connections, re-route data cables away from stepper motor cables.  CSHELL Grating Equations 1. Grating Step N as a function of angle q: N = -1,056,268 + 18,634.80q + 26.85632q2 ( ~ 22 steps / IR array pixel) 2. Wavelength to grating angle: l (mm) = 2ssinq ; n = order; s = groove spacing: 31.5195 mm cold n 3. Order Calculation: n = 2ssinq (nearest integer); l (mm) nopt = 2ssinqB = 56.416 cold (Integer Order closest to Blaze angle qB = 63.5) l (mm) l (mm) 4. Dispersion: Dl (mm/pixel) = Cl (mm) 2tan q Verifying CSHELL Throughput CSHELL is measured to have 16.5% total throughput (including telescope & atmosphere) at 1.25 - 2.2 mm (2% CVF), and 12% throughput at 3.4 (1% CVF) - 4.8 mm (2% CVF) in spectroscopic mode. You can use an Elias standard or the continuum lamp flux as a more convenient check. l (mm)Elias Std (2" slit, 63.5 gr)Image (* - sky ADU) spec (10w x20pxl)1.2537HD 161903 J= 7.1755558 in 2 sec3864 ADU in 60 sec2.1698HD 161903 K=7.02101,981 in 2 sec2906 ADU in 60 sec3.526HR 8143 L= 3.7140,500 in 0.25 sec26,400 ADU in 30 sec4.701HR 8143 M=3.728970 in 0.1 sec4323 ADU in 10 sec l (mm)Max ADU/pixel in 5 sec Spect of Continuum Lamp (1" slit)1.25371300 (with blockers in)1.6593 27092.169829063.52606354.701 3807 D. Temperatures and Controllers The CSHELL dewar and optics are cooled by a liquid nitrogen bath which must be filled once per day, usually at the start of each night. A closed cycle cooler provides additional cooling for the arrays. The arrays are maintained at their optimal operating temperatures by temperature controllers which apply small amounts of resistive heating to the devices. It is the user's responsibility to keep an eye on the array, cold box, and grating temperatures. The temperatures will drift if CSHELL runs out of liquid nitrogen, if the controllers get reset, or if the closed cycle cooler fails. The cold box should be 72.5 2 K. Temperatures any higher will cause focus and dispersion changes. The grating is cooled by the same bath as the cold box, so its temperature will usually follow the cold box. Follow the troubleshooting procedures in Appendix B if the cold box temperature is out of its range. The following procedures for resetting the temperature controllers should be performed by an IRTF operator or staff member only: The detector array temperature controllers are located on the front side of Box 5 which is mounted on the telescope along with CSHELL. The controllers usually have their set points reset to 0 K when powered off, and their heaters are off when the controllers are initially powered on. The arrays will cool to 20 K and will not be operational if the set points are not set and if the heaters are not turned on. The day crew properly sets the array temperatures and powers on the heaters when they mount CSHELL on the telescope, but you must set up the controllers if you have powered down Box 5 due to approaching lightning or as part of a troubleshooting procedure. The following procedure illustrates how to read the array temperatures, set the set points, and turn on the heaters. Controller A controls the SBRC InSb array temperature (30.0 K set point) and Controller B controls the TEK CCD array temperature (175 K set point). The controllers may be set up either via their front panel controls (Procedure A) or else via software (Procedure B). Procedure A: Front Panel Configuration Read Array Temperature on controller front panel LCD display (T1 probe). Press ENTER button until set point field is selected (S xxx.x on display) Press ENTER to change the set point temperature Press SCROLL to change current digit, press ENTER to accept and move to next digit Press RETURN to enter the displayed temperature as the set point. Press RETURN to activate the heater. The green HEATER LED should light. Procedure B: Software Control Alternatively, you can read and set the array temperatures via the cshellxui software: Read the array temperatures and set points in the cshellxui main window Change the set points by typing the tempcmd A S300 or tempcmd B S1750 commands on the cshellxui command line for the IR array and CCD, respectively. See III.A for details. Turn the heaters on or off by typing the tempcmd A X or tempcmd B X (see p. 98) command on the cshellxui command line. Heater status in the cshellxui window will display ERROR if the heater is off or the heater voltage if it is on. See III.A. E. Summary of Upgrade Changes for Previous CSHELL Users CSHELL Upgrade User Documentation Addendum I. New InSb Array CSHELL now has a single IR detector array, a 256 x 256 pixel Hughes SBRC InSb device. It performs at least as well as the old NICMOS-3 array in nearly all respects, while it also has increased spectral response, better quantum efficiency, and reduced artifacts (less residual image and no corner glow). The new array results in the following performance parameters: - 1 - 5.6 mm response; 16.5% total spectroscopic throughput @ 2.2 mm - 700 km/s spectral range per exposure when grating at blaze angle - 0.20 arcsec/pixel and 2.7 km/s/pixel - R.N. 33 e- - Idark @ 0.5 e-/ADU The new array also requires some operational changes. Foremost, the detector bias must be programmed to match the observing application. Using a single fixed bias (as done with the NICMOS array) is inappropriate because of non-linearities and icky pixel artifacts in the SBRC 256 x 256 InSb arrays. Larger biases allow more electrons to be collected before saturation, but they also cause increased numbers of high dark current pixels (icky pixels) and low-level non-linearities. Fortunately, the icky pixels mostly disappear when object and sky frames are subtracted. Dark frames with exposure times equivalent to flat fields should be taken to subtract these pixels from your flats. Linearity problems can be avoided if you expose your fats so that they have similar data counts to your object frames. You may coadd many flats to achieve high S/N. I recommend that you pick one of four following detector bias settings for you observations: ObservationBias (mV)WellVDDUCVDETXUI MACROMost Spectroscopy3255000-3.7-3.375smallBright Thermal Spectroscopy5008400-3.7-3.200mediumBright or Thermal Imaging80015,500-3.7-2.900largeThermal Imaging with very high backgrounds100021,300-3.7-2.700huge Notes: Well: The maximum number of ADU counts (1 ADU = 11.0 electrons) that can be collected while not departing more than 1% from the linearity relation of the mid-well range. VDET & VDDUC are detector biases (Volts) that can be typed into the SETUP Parameters frame of the CSHELL XUI Application. XUI MACRO is the name of a command file that can be executed from the Options menu of the CSHELL XUI application. These files automatically set the indicated bias levels. There are also some other operational changes resulting from the new array. Most importantly, you must select the CVF/Blocker Option and also use the shutter wheel blocker (SPF) when observing with the 1.1 - 1.57 mm CVF! This CVF transmits l > 2.5 mm radiation, causing significantly increased background in your data if not blocked as prescribed. The blockers impart about a 10% reduction in flux over the 1.1 - 1.6 mm region. Now exposures can be as short as .076 s or even less. The bias voltages must also be set (DO File or push button in Setup Parameters Window) when the software is started. II. New Tek 512 x 512 Acquisition & Guide CCD The old surveillance CCD has been replaced with a scientific-grade Tektronix 512 x 512 pixel CCD. The CCD is operated via IC and XUI programs like other IRTF instruments. It can be operated in a continuous mode for acquisition, a single exposure mode, or an auto-guide mode. Use of the guider software is described in III. G of this manual. The CCD is clocked at a rate of 333,000 pixels / sec, so it takes just under 1 second to read a frame; this limits the minimum exposure time also. A 1000x attenuation filter can be switched in front of the CCD for observing bright objects. Pixels can be binned (1x1, 2x2, 4x4, or 8x8) to improve signal-to-noise. N is up and E is to the left on the CCD monitor (or in VF) when CSHELL is mounted in its normal E-W slit configuration. The CCD has a 55" (E-W) x 65" (N-S) FOV, 0.15"/pixel plate scale, and V=15 mag limit. CCD frames may be viewed in VF and saved as FITS files. The CCD looks through an IR-reflecting dichroic which has a bandpass similar to an R band filter. III. Startup and Shutdown Software Notes All software can be started up from your user account on an IRTF Sun workstation at the summit (planck) or HP (wien). Just remember to type "xuihostname wien" in the command line of the CSHELL XUI program if running from that HP workstation. The CSHELL and CASSPC (the guider pc) Instrument control (IC) Intel architecture computers can also be logged into from their directly connected keyboard / monitor consoles. The new calibration lamp program is called cal_lines which should be typed in from a UNIX prompt. A. CSHELL Startup 0) Turn on CSHELL boxes #2 - #5 in numerical order 1) Log into your Guest Account 2) Type "openwin" and at the UNIX prompt 3) Hold down the right mouse button on the blue desktop 4) If the IC program is not already running (ASK a T.O. or Support Astronomer), Either: i) Select "Start CSHELL IC Software!" from the CSHELL menu or ii) Log into CSHELL IC console as "cshellic" 5) Select "Cshell XUI" from the CSHELL menu 6) Select "VF" from the CSHELL menu 7) Turn on the CSHELL Array Power Supplies 8) Set Programmable Voltages in Setup Parameters XUI window B. CSHELL Shutdown 1) Quit VF 2) Move Shutter, Slit, and Filter to "Blank" Position. Spectroscopic mode, turn lamps off. 3) Quit XUI software 4) Leave in this configuration unless powering off (proceed further only if powering off) 5) Turn off the CSHELL Array Power Supplies 6) Type "die" and in CSHELL IC window. Halt Lynx by logging in as "shutdown"; login as "reboot" if you only want to reboot the IC computer. 7) Turn off boxes #2 - #5 in reverse numerical order C. Guider Software Startup: 1) Follow Steps A0 - A3. 2) Select "Login to CASSPC Guider PC" from CSHELL menu 3) Type "gic" and in the casspc window 4) Select "Guider XUI" from CSHELL menu Shutdown: 1) Quit Guider XUI 2) Type "die" and in GIC (casspc) window; exit window F. IR Array Linearity Data   14 April 1994 lab data: CSHELL SBRC InSb SCA #052 Science Grade Array Vdduc -3.7 VGG -1.5/-1.0 switched off between rows V3 -2.9 11.0 e-/ADU VDET = -3.4 BIAS= -300 mV t (sec)ADU%e-0.1231.686.52539.550.25575.896.46313.770.5114499.812538.70.751706100.618706.712263100.824808.81.252811100.630823.21.53346100.136689.61.75386399.342358.62434397.8476222.25473795.051942.32.5500490.4548703525679.257633.25523847.557435.8slope2196ADU/soffset48.03r1 Charge Dump:178mVVDET=-3.38BIAS=-325mVt (sec)ADU%e-0.1224.783.72463.890.25559.595.36135.040.5111499.612209.80.751659100.618193.512203101.124156.41.53266100.735812.424307100.147227.22.25480799.452709.82.5527198.257797.73598793.165648.85625458.668576.5slope2124ADU/soffset55.93r1   VDET=-3.3BIAS=-400mVt (sec)ADU%e-0.1244.685.92682.090.25607.696.06662.470.5120999.613260.212397100.926283.61.53566100.83910224705100.251591.42.5583099.563927.23692398.675912.23.5799897.887699.85956582.010488210945040.6103621slope2323ADU/soffset52.43r1VDET=-3.2BIAS=-500mVt (sec)ADU%e-0.1255.377.12799.420.5126197.513827.112501100.2274241.53723100.740823.524928100.654036.62.56107100.166964.63727399.679750.13.5842199.092338.14954498.310465251171096.7128403101347155.8147712slope2405ADU/soffset90.53r1VDET=-3.1BIAS=-600mVt (sec)ADU%e-0.1264.667.22901.40.5130895.214339.21259399.828427.325113101.356065.237567101.082973.849943100.010902751225298.913434661446997.515865671650795.5181003151759047.7192878slope2448ADU/soffset148.8r1   VDET=-2.9BIAS=-800mVt (sec)ADU%e-0.1107683.311798.60.25267096.129277.10.55280100.4578920.757814101.085682.2110304100.91129861.2512719100.21394671.51505399.21650591.751728998.018957821936996.32123852.252088492.422899832358078.5258560slope9911ADU/soffset300.9r1VDET=-2.7BIAS=-1000mVt (sec)ADU%e-0.11217112.113344.70.55907112.464771.6111245110.11233041.516260107.21782941.7518678105.9204808220667102.72266182.252190296.92401602.52297391.625190452586651.9283626slope10861ADU/soffset0r0.995 IRTF CSHELL User's Guide  Page   Page  IRTF CSHELL User's Guide  Page   Page  IRTF CSHELL User's Guide  Page   Page  IRTF CSHELL User's Guide  Page  IRTF CSHELL User's Guide  Page  IRTF CSHELL User's Guide  Page  IRTF CSHELL User's Guide  Page   Page  IRTF CSHELL User's Guide 04/08/93 Page 80  uv} @@ wx @8wx 88v::uu 1cy1cy1d WORD 4!B  ?             @0?P @?  3?U 2T?0 P  30?U@3U? ̀3?U32??UT30?UP3  UU@̀33UT32? !UPL330UU@33?UU 332UUT330UUP 3 ???U@3U? 32UT30?UP?? 3U3?UT 30UP3 ?U3UT?30UP3 ?U@3????U????30?UP??30?U@?3U32UP?3 U@?3?U37U_3??U3U_3?U??3UW3??U?3U37?U_3;3UuU33??UU_??373?U_U33U_W33?UWU3?3 U@UWW 303033? ? 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8* d PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelv8* d PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelv4!&!! !d PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvdPPNTTms Rmn !,Times .+F d PPNTHelvdPPNTSymbol, Symbol) = d PPNTHelvdPPNTTms Rmn( F d PPNTHelvdPPNTTms Rmn +0 d PPNTHelvdPPNTSymbol ( % d PPNTHelvdPPNTTms Rmn)S d PPNTHelvdPPNTSymbol) d PPNTHelvdPPNTTms Rmn)R d PPNTHelvdPPNTSymbol(%l d PPNTHelvdPPNTTms Rmn (,2 "(d PPNTHelvdPPNTTms Rmn ( KN d PPNTHelvdPPNTSymbol)  d PPNTHelvdPPNTTms Rmn)( d PPNTHelvdPPNTTms Rmn)n d PPNTHelvdPPNTTms Rmn +r d PPNTHelvdPPNTTms Rmn(g2 d PPNTHelvdPPNTSymbol ++ d PPNTHelvdPPNTTms Rmn) n d PPNTHelvdPPNTTms Rmn +b d PPNTHelvdPPNTSymbol (  d PPNTHelvdPPNTTms Rmn)t d PPNTHelvdPPNTTms Rmn)) d PPNTHelvdPPNTTms Rmn(dT d PPNTHelvdPPNTSymbol)  d PPNTHelvdPPNTTms Rmn)t "IG"A"B "E#IdPPNTTms RmndPPNTTms RmndPPNTTms RmnR7R)R*d SPNTdSPNT * *"% P2-v17 - Copyright 1991 Aldus Corporation userdict/md known{currentdict md eq md/bu known and}{false}ifelse{bu}if currentdict/P2_d known not{/P2_b{P2_d begin}bind def/P2_d 33 dict def userdict/md known{currentdict md eq}{false}ifelse P2_b dup dup /mk exch def{md/pat known md/sg known md/gr known and and}{false}ifelse/pk exch def{md /setTxMode known}{false}ifelse/sk exch def mk{md/xl known}{false}ifelse/xk exch def/b{bind def}bind def/sa{matrix currentmatrix P2_tp concat aload pop}b/sb{matrix currentmatrix exch concat P2_tp matrix invertmatrix concat aload pop}b/se{matrix astore setmatrix}b/bb{gsave P2_tp concat newpath moveto}b/bc{curveto}b/bl {lineto}b/bx{closepath}b/bp{gsave eofill grestore}b/bf{scale 1 setlinewidth stroke}b/be {grestore}b/p{/gf false def}b p/g{/gf true def}b pk{/_pat/pat load def/_gr/gr load def}{/_gr {64.0 div setgray}b}ifelse sk{/_sTM/setTxMode load def}if/gx{/tg exch def}b 0 gx/x6{mk{av 68 gt {false}if}if}b/bps 8 string def/bpm[8 0 0 8 0 0]def/bpp{bps}def/obp{gsave setrgbcolor bps copy pop dup 0 get 8 div floor cvi 8 mul 1 index 2 get 8 div floor cvi 8 mul 2 index 1 get 8 div floor cvi 8 mul 8 4 index 3 get 8 div floor cvi 8 mul{2 index 8 3 index{1 index gsave translate 8 8 scale 8 8 false bpm/bpp load imagemask grestore}for pop}for pop pop pop grestore}b end P2_b pk end{/pat{P2_b gf{end pop sg P2_b mk end{av 68 gt{pop}if}if}{/_pat load end exec}ifelse}bind def}{/pat{P2_b pop _gr end}bind def}ifelse P2_b sk end{/setTxMode{P2_b/_sTM load end exec P2_b tg dup 0 ge{/_gr load end exec} {pop end}ifelse}bind def}{/setTxMode{pop P2_b tg dup 0 ge{/_gr load end exec}{pop end}ifelse}bind def}ifelse P2_b xk end{P2_d/_xl/xl load put/xl{P2_b 2 copy P2_tp 4 get add P2_tp 4 3 -1 roll put P2_tp 5 get add P2_tp 5 3 -1 roll put/_xl load end exec}bind def}if}if "+d SPNT *f27 42 1 index neg 1 index neg matrix translate 3 1 roll currentpoint 2 copy matrix translate 6 1 roll "d SPNT 512 721 currentpoint 1 index 6 index sub 4 index 9 index sub div 1 index 6 index sub 4 index 9 index sub div matrix scale 11 1 roll ~[ 9 1 roll cleartomark 3 2 roll matrix concatmatrix exch matrix concatmatrix /P2_tp exch def P2_b mk end{md/bn known{bn}if}if "d SPNT dSPNT &'d SPNT ,Times .(,YFigure 1. CSHELL optical layout. The CCD is mounted behind the dichroic but is not shown. UUUU",d SPNT d SPNT dSPNT &fd SPNT  *,  Helvetica ( Filter wheel #2  *" d SPNT  pd SPNT pQ^Q^d SPNT pQ^Q^d SPNT pttd SPNT pttd SPNT dSPNT U`UP*ŀcUPU`P2_b 253 386 bb 2251.00003 393.99988 244.6665 400.66675 234 406 bc .223.3335 411.33325 211.16646 414 197.5 414 bc ,183.83354 414 171.6665 411.33325 161 406 bc 2150.3335 400.66675 143.99997 393.99988 142 386 bc &p x6 end 0 pat P2_b 1 1 bf be end pd SPNT dSPNT }}UNU`UP*ŀcUPU`UN}}P2_b 253 381 bb 2251.00003 388.33322 244.6665 394.66675 234 400 bc .223.3335 405.33325 211.16646 408 197.5 408 bc ,183.83354 408 171.6665 405.33325 161 400 bc 2150.3335 394.66675 143.99997 388.33322 142 381 bc &p x6 end 0 pat P2_b 2 2 bf be end p|||d SPNT dSPNT URUJ[શ*Gŀ*UP U**YP2_b 253 409 bb !253 409 253 410.66672 253 414 bc /253 417.33328 247.33316 421.83342 236 427.5 bc /224.66684 433.16658 211.83311 436 197.5 436 bc /183.16689 436 170.49983 433.33325 159.5 428 bc 7148.50017 422.66675 142.83333 418.16661 142.5 414.5 bc '142.16667 410.83339 142 409 142 409 bc &p x6 end 0 pat P2_b 1 1 bf be end pd SPNT pd SPNT pd SPNT dSPNT hhkURp*v|OU`UF |Ovp**kURhSdaUR^^P2_b 249 360 bb /251.66663 363.33328 253 368.16676 253 374.5 bc ,253 380.83324 247.6665 387.00009 237 393 bc +226.3335 398.99991 213.3331 402 198 402 bc .182.6669 402 169.49983 398.99991 158.5 393 bc /147.50017 387.00009 142 380.83324 142 374.5 bc .142 368.16676 143.1667 363.33328 145.5 360 bc 2147.8333 356.66672 151.00006 353.33328 155 350 bc &p x6 end 0 pat P2_b 1 1 bf be end p^hjlnqswz}}zwsqnljhea^d SPNT dSPNT UT[**U`OUFO **[P2_b 251 391 bb /252.33331 393.66663 253 397.83342 253 403.5 bc .253 409.16658 247.6665 415.16676 237 421.5 bc +226.3335 427.83324 213.3331 431 198 431 bc 0182.6669 431 169.49983 427.83324 158.5 421.5 bc /147.50017 415.16676 142 409.16658 142 403.5 bc -142 397.83342 142.66669 393.66663 144 391 bc &p x6 end 0 pat P2_b 1 1 bf be end pd SPNT  q! pҡd SPNT  q    ! p    d SPNT pd SPNT pd SPNT p  d SPNT p  d SPNT  q 90 90 ! p 90 90 d SPNT  q(MNh(V-hN_IM(V! p(MNh(V-hN_IM(Vd SPNT p JO JOd SPNT  qxe}mxiym}i{e! pxe}mxiym}i{ed SPNT pNgykNgyiNkd SPNT pIId SPNT pJJd SPNT pJJJJd SPNT pd SPNT px3x3d SPNT dXSPNT xxxYz~*P2_b 384 120 bb /390.66656 120 395.83339 122.00006 399.5 126 bc -403.16661 129.99994 405 136.00012 405 144 bc &p x6 end 0 pat P2_b 1 1 bf be end p>xxxyz{|~d SPNT dXSPNT 444UP5Y*9=*QBJJP2_b 308 167 bb 1308 172.33325 309.83339 177.16673 313.5 181.5 bc 3317.16661 185.83327 322.66678 188.66669 330 190 bc &p x6 end 0 pat P2_b 1 1 bf be end p>4J444568:;>@CFJd SPNT dSPNT 3333UV333UX334UZ7:@UXJJP2_b 307 168 bb !307 168 307 168.33334 307 169 bc '307 169.66666 307 171.33337 307 174 bc .307 176.66663 308.50005 180.3334 311.5 185 bc 2314.49995 189.6666 320.66681 193.33337 330 196 bc &p x6 end 0 pat P2_b 1 1 bf be end pb3J33333333345689;>@BDFHJd SPNT pd SPNT pd SPNT pppd SPNT p:U:Ud SPNT p*E*Ed SPNT p*:*:١d SPNT pEUEUd SPNT p:o:od SPNT pVVd SPNT pood SPNT pd SPNT pd SPNT pd SPNT pEEgd SPNT d SPNT d SPNT q¡d SPNT Bpbb¡d SPNT d SPNT dSPNT ^^eULms媴x*|̀|c|ULxsme^^P2_b 253 350 bb -253 357.99988 248.33319 365.00009 239 371 bc /229.66681 376.99991 218.16646 380 204.5 380 bc -190.83354 380 179.33319 376.99991 170 371 bc -160.66681 365.00009 156 357.99988 156 350 bc &p x6 end 0 pat P2_b 1 1 bf be end p^|^bfikmnprstvwxyzz{{|||||{{zzyxwvtsrpnmkifb^d SPNT d SPNT  Q3o! Xd SPNT  QWf! Xd SPNT d SPNT d SPNT d SPNT q    d SPNT p ee d SPNT d SPNT d SPNT d SPNT q$#$"d SPNT p""d SPNT d SPNT d SPNT d SPNT q$$#"סd SPNT p""סd SPNT d SPNT d SPNT d SPNT q  šd SPNT pšd SPNT d SPNT Bp  d SPNT d SPNT d SPNT q;CC;CAܡd SPNT pAeeAܡd SPNT d SPNT Bp@@ݡd SPNT Bp;;d SPNT Bp  ֡d SPNT Bp""d SPNT d SPNT d SPNT q$,$,$&d SPNT p&&d SPNT d SPNT BdXSPNT &&'UTUV2F骪YdddP2_b 232 294 bb -232 295.33331 232.33334 306.00031 233 326 bc '233.66666 345.99969 234 356 234 356 bc &p x6 end 0 pat P2_b 0.25 0.25 bf be end p&d&&')*,/259;=?ADFHKMOQSWZ\_abcddd SPNT d SPNT d SPNT q]e]e]_d SPNT p__d SPNT d SPNT pd SPNT pyz{yd SPNT d SPNT d SPNT q"`*f*`"c*f(cd SPNT p(|c|?c(cd SPNT d SPNT d SPNT d SPNT q!O)U)O!R)U'Rd SPNT p'|R|8R'Rd SPNT d SPNT d SPNT d SPNT qO.V7Q.O7V1R2d SPNT pR}2}R2d SPNT d SPNT d SPNT d SPNT qrMzSrSzPrMtPd SPNT p`PtP`PtPd SPNT d SPNT BpuPPuPPd SPNT d SPNT d SPNT qMSSPMPd SPNT pPPPPd SPNT d SPNT d SPNT d SPNT q!!d SPNT pPPPd SPNT d SPNT d SPNT d SPNT qd SPNT pd SPNT d SPNT d SPNT d SPNT qekkhehd SPNT pfhfhd SPNT d SPNT d SPNT d SPNT q?fGl?lGi?fAid SPNT phAihAid SPNT d SPNT d SPNT d SPNT q\b\_b_d SPNT p2R_R2;\_d SPNT d SPNT Bp_d_dd SPNT BpBiwiBiwid SPNT dSPNT &j8cd SPNT  *(w=Echelle  * UUUU"=d SPNT dSPNT &)fd SPNT  *(. Secondary  *".d SPNT d SPNT  1d SPNT B! pd SPNT d SPNT d SPNT qd SPNT p;;d SPNT d SPNT d SPNT dSPNT S*UT*݀YSUTԀ*P2_b 234 251 bb .234 252.99997 232.8333 254.66669 230.5 256 bc .228.1667 257.33331 225.16661 258 221.5 258 bc .217.83339 258 214.8333 257.33331 212.5 256 bc ,210.1667 254.66669 209 252.99997 209 251 bc &p x6 end 0 pat P2_b 1 1 bf be end p>Ѡd SPNT pѡd SPNT d SPNT  Q! Xd SPNT dSPNT UT*W݀ڀ*րWUTP2_b 231 247 bb 1231 248.33331 230.16664 249.50002 228.5 250.5 bc /226.83336 251.49998 224.49995 252 221.5 252 bc 1218.50005 252 216.16664 251.49998 214.5 250.5 bc -212.83336 249.50002 212 248.33331 212 247 bc &p x6 end 0 pat P2_b 1 1 bf be end p>Ԡd SPNT pd SPNT pԡd SPNT d SPNT "d SPNT "d SPNT "d SPNT dSPNT UTUTS*UT*݀YSUTԀ*UTP2_b 232 243 bb -233.33331 244.33331 234 246.00003 234 248 bc .234 249.99997 232.8333 251.66669 230.5 253 bc .228.1667 254.33331 225.16661 255 221.5 255 bc .217.83339 255 214.8333 254.33331 212.5 253 bc ,210.1667 251.66669 209 249.99997 209 248 bc -209 246.00003 210.00003 244.33331 212 243 bc &p x6 end 0 pat P2_b 1 1 bf be end pVԠd SPNT d SPNT "d SPNT dSPNT &G(wd SPNT (T-Collimator primary  UUUU"c-d SPNT dSPNT &o1ed SPNT  *+ ( Slit wheel  *"6d SPNT dSPNT &gd SPNT  *(!Filter wheel #1  *"!d SPNT dSPNT &% d SPNT   *!+0 Dichroic* (Flat #2)  *"d SPNT dSPNT &3d SPNT  */+ Dewar window  *"d SPNT dSPNT &u0d SPNT  *( Flat #3  *" d SPNT dSPNT &*Zd SPNT  *V(7Flat #4  *"Fd SPNT dSPNT &d SPNT  *(Spherical relay mirror  *"d SPNT dSPNT &nd SPNT  *({IR detector array  *"d SPNT dSPNT &td SPNT  *(yIncoming light  *"yd SPNT dSPNT &d SPNT  *+* Input lens  *"d SPNT dSPNT &d SPNT  * +"Flat #1  *"d SPNT d SPNT d SPNT qd SPNT Bpd SPNT d SPNT d SPNT d SPNT qTXXTXWd SPNT BpWvvWd SPNT d SPNT d SPNT d SPNT qvryvyvxrvvxud SPNT Bpxuxxxud SPNT d SPNT d SPNT d SPNT q2s5w5w4s2w4vd SPNT Bp4v444vd SPNT d SPNT d SPNT d SPNT qqtqqtrd SPNT Bprrd SPNT d SPNT d SPNT d SPNT qrurtutd SPNT Bptbttbtd SPNT d SPNT d SPNT d SPNT qQTQRTRd SPNT BpRRRRd SPNT d SPNT d SPNT d SPNT qwzwxzxd SPNT Bpxdxxdxd SPNT d SPNT d SPNT d SPNT qd SPNT Bpeetd SPNT d SPNT d SPNT d SPNT qd SPNT Bpddyd SPNT d SPNT Bpۡd SPNT d SPNT d SPNT q١d SPNT Bp١d SPNT d SPNT d SPNT d SPNT q|~|~d SPNT Bp~~ ~ ~d SPNT d SPNT d SPNT d SPNT qۡd SPNT pۡd SPNT d SPNT d SPNT d SPNT q   d SPNT Bp   d SPNT d SPNT d SPNT P9hd SPNT P9gd SPNT d SPNT "hd SPNT d&SPNT YUuYVSd SPNT !drSPNT qՑ٣qՑ٣qՑ٣ngqىngqىngqىoE2oE2oE2pf؀pf؀pf؀d&SPNT cfYUuY_Sd SPNT P2_b 369.83424 473.63901 bb 366.40407 473.53775 bl 367.53621 469.19879 bl 368.40218 472.50366 bl &p x6 end 0 pat P2_b bp be end qnrrnppd SPNT bd>SPNT rrrpRpRpRd&SPNT eYUuY_SP2_b 393.78036 458.99393 bb 368.02696 472.32256 bl &p x6 end 0 pat P2_b 0.25 0.25 bf be end pppd SPNT d SPNT dSPNT/V/H/8>d SPNTdSPNT > > UUUU"% P2-v17 - Copyright 1991 Aldus Corporation userdict/md known{currentdict md eq md/bu known and}{false}ifelse{bu}if currentdict/P2_d known not{/P2_b{P2_d begin}bind def/P2_d 33 dict def userdict/md known{currentdict md eq}{false}ifelse P2_b dup dup /mk exch def{md/pat known md/sg known md/gr known and and}{false}ifelse/pk exch def{md /setTxMode known}{false}ifelse/sk exch def mk{md/xl known}{false}ifelse/xk exch def/b{bind def}bind def/sa{matrix currentmatrix P2_tp concat aload pop}b/sb{matrix currentmatrix exch concat P2_tp matrix invertmatrix concat aload pop}b/se{matrix astore setmatrix}b/bb{gsave P2_tp concat newpath moveto}b/bc{curveto}b/bl {lineto}b/bx{closepath}b/bp{gsave eofill grestore}b/bf{scale 1 setlinewidth stroke}b/be {grestore}b/p{/gf false def}b p/g{/gf true def}b pk{/_pat/pat load def/_gr/gr load def}{/_gr {64.0 div setgray}b}ifelse sk{/_sTM/setTxMode load def}if/gx{/tg exch def}b 0 gx/x6{mk{av 68 gt {false}if}if}b/bps 8 string def/bpm[8 0 0 8 0 0]def/bpp{bps}def/obp{gsave setrgbcolor bps copy pop dup 0 get 8 div floor cvi 8 mul 1 index 2 get 8 div floor cvi 8 mul 2 index 1 get 8 div floor cvi 8 mul 8 4 index 3 get 8 div floor cvi 8 mul{2 index 8 3 index{1 index gsave translate 8 8 scale 8 8 false bpm/bpp load imagemask grestore}for pop}for pop pop pop grestore}b end P2_b pk end{/pat{P2_b gf{end pop sg P2_b mk end{av 68 gt{pop}if}if}{/_pat load end exec}ifelse}bind def}{/pat{P2_b pop _gr end}bind def}ifelse P2_b sk end{/setTxMode{P2_b/_sTM load end exec P2_b tg dup 0 ge{/_gr load end exec} {pop end}ifelse}bind def}{/setTxMode{pop P2_b tg dup 0 ge{/_gr load end exec}{pop end}ifelse}bind def}ifelse P2_b xk end{P2_d/_xl/xl load put/xl{P2_b 2 copy P2_tp 4 get add P2_tp 4 3 -1 roll put P2_tp 5 get add P2_tp 5 3 -1 roll put/_xl load end exec}bind def}if}if "% P3 - v1 Copyright 1993 Aldus Corporation userdict/P3_d known not{userdict begin/P3_d 150 dict def P3_d begin /nulld { counttomark {null def} repeat pop} bind def mark /a /b /c /d /e /f /g /h /i /j /k /l /m /n /o /p /q /r /s /t /u /v /w /x /y /z /A /B /C /D /E /F /G /H /I /J /K /L /M /N /O /P /Q /R /S /T /U /V /W /X /Y /Z /aa /ab /ac /ad /ae /af /ag /ah /ai /aj /ak /al /am /an /ao /ap /aq /ar /as /at /au /av /aw /ax /ay /az /aA /aB /aC /aD /aE /aF /aG /aH /aI /aJ /aK /aL /aM /aN /aO /aP /aQ /aR /aS /aT /aU /aV /aW /aX /aY /aZ /ba /bb /bc /bd /be /bf /g /ia /iai nulld systemdict/currentpacking known dup{currentpacking exch true setpacking}if /a{bind def}bind def/b{exch def}a/d{0 def}a /aS{false def}a/c{null def}a/e{userdict begin P3_d end begin/f b/g b countdictstack save f 2 add 2 roll count f sub/h b/g load end{exec}stopped userdict begin P3_d end begin/i b count h sub{pop}repeat i 3 1 roll restore countdictstack exch sub{end}repeat end}a/r{/j b/k b /l b/m aS/n c/q load end{exec}stopped userdict begin P3_d end begin{clear/m aS}if m j restore }a/s{/t k def/u l def/v m def/w n def/k b/l b/m aS/n c/q load end exec userdict begin P3_d end begin /k t def/l u def/m v def/n w def}a/o{/j b/k b/l b/m aS/n c{currentfile token not{false exit}if dup dup type/nametype eq exch xcheck and{end load userdict begin P3_d end begin}if/q load end {exec}stopped userdict begin P3_d end begin{false exit}if m{true exit}if}loop currentrgbcolor currentlinewidth j restore setlinewidth setrgbcolor}a/x 10 array def/y d/z{dup/restore load eq{pop pop}{dup/save load eq{pop null}{dup dup dup dup/for load eq exch/forall load eq or exch/repeat load eq or exch/loop load eq or{/A b x y/n load put /y y 1 add def/n b{B}A/y y 1 sub def/n x y get def}{dup/exec load eq{pop/q load end exec userdict begin P3_d end begin}{dup/ifelse load eq{pop/C b/D b{/D}{/C}ifelse load/q load end exec userdict begin P3_d end begin}{dup/if load eq{pop/D b{/D load/q load end exec userdict begin P3_d end begin}if}{/E d l{dup systemdict exch known{load 1 index eq{pop k E get exec/m true def exit}if}{pop}ifelse/E E 1 add def}forall l length E eq {end exec userdict begin P3_d end begin}if}ifelse}ifelse}ifelse}ifelse}ifelse}ifelse}a/B{/n load/q load end exec userdict begin P3_d end begin}a/q{dup xcheck{dup dup type/arraytype eq exch type/packedarraytype eq or {{dup xcheck{dup type/nametype eq{load true}{false}ifelse userdict begin P3_d end begin/F b dup dup type /arraytype eq exch type/packedarraytype eq or{F{/q load end exec userdict begin P3_d end begin}if}{dup type /operatortype eq{z}{end exec userdict begin P3_d end begin}ifelse}ifelse end}if}forall}{dup type/operatortype eq {userdict begin P3_d end begin z end}{exec}ifelse}ifelse}if}a/p[/image/colorimage/imagemask]def /aF[{aG}{aH}{imagemask}bind]def/cim{userdict begin P3_d end begin p aF save o pop end}a/aI{aJ{gsave aK aL 3 index idtransform translate aM 1 4 index 4 index{aN}image grestore/aO d/aM d/aJ aS}if }a/aG{2 index 8 ne{image}{4 index cvi string/aN b/aP 0 string def/aQ d/aJ aS/aO d/aM d 0 1 5 index 1 sub{/aL b 0 1 6 index 1 sub{aQ aP length ge{1 index dup type/stringtype ne{exec}if /aP b/aQ d}if aP aQ get/aQ aQ 1 add def dup 255 eq{pop pop aI}{aN aO 3 -1 roll put/aO aO 1 add def/aM aM 1 add def aJ not{/aK b/aM 1 def/aJ true def}{pop}ifelse}ifelse}for aI}for pop 4{pop}repeat}ifelse}a/aR{aJ{gsave aK aL 5 index idtransform translate aM 1 6 index 6 index {aN}false 6 index colorimage grestore/aO d/aM d/aJ aS}if}a/aH{4 index 8 ne 2 index or{colorimage }{dup 1 eq{pop pop aG}{dup 3 eq{6 index cvi 3 mul string/aN b/aP 0 string def/aQ d/aJ aS/aO d /aM d 0 1 7 index 1 sub{/aL b 0 1 8 index 1 sub{aQ aP length ge{3 index dup type/stringtype ne {exec}if/aP b/aQ d}if aP aQ get/aQ aQ 1 add def aP aQ get/aQ aQ 1 add def aP aQ get/aQ aQ 1 add def dup 255 eq 2 index 255 eq and 3 index 255 eq and{4{pop}repeat aR}{aN aO 5 -1 roll put/aO aO 1 add def aN aO 4 -1 roll put/aO aO 1 add def aN aO 3 -1 roll put/aO aO 1 add def/aM aM 1 add def aJ not{/aK b/aM 1 def/aJ true def}{pop}ifelse}ifelse}for aR}for 7{pop}repeat}{ dup 4 eq{6 index cvi 4 mul string/aN b/aP 0 string def/aQ d/aJ aS/aO d/aM d 0 1 7 index 1 sub {/aL b 0 1 8 index 1 sub{aQ aP length ge{3 index dup type/stringtype ne{exec}if/aP b/aQ d}if aP aQ get/aQ aQ 1 add def aP aQ get/aQ aQ 1 add def aP aQ get/aQ aQ 1 add def aP aQ get/aQ aQ 1 add def dup 255 eq 2 index 255 eq and 3 index 255 eq and 4 index 255 eq and{5{pop}repeat aR}{aN aO 6 -1 roll put/aO aO 1 add def aN aO 5 -1 roll put/aO aO 1 add def aN aO 4 -1 roll put/aO aO 1 add def aN aO 3 -1 roll put/aO aO 1 add def/aM aM 1 add def aJ not{/aK b/aM 1 def/aJ true def }{pop}ifelse}ifelse}for aR}for 7{pop}repeat}{colorimage}ifelse}ifelse}ifelse}ifelse }a/G[/show/ashow/widthshow/awidthshow/kshow]def/H[{I}{0 0 0 6 3 roll J}bind{0 0 3 -1 roll J} bind{J}{exch /K b I}bind]def/ftp{/L b/M b/N b/K c/O M{2}{1}ifelse def G H 4 -1 roll r pop} a/I{5{0}repeat 6 -1 roll J}a/P[/show/setcachedevice/setcharwidth]def/Q[{userdict begin P3_d end begin/R R 1 add def/S currentfont def currentpoint transform/T b/U b R O eq{/V currentfont def/W U def/X T def/Y true def}if end pop}bind{6{pop}repeat}bind{pop pop}bind]def/Z( )def /au{moveto{ag setfont Z end gsave 0 setgray stringwidth grestore userdict begin P3_d end begin rmoveto/K load null ne {/ah ah 1 add def ah aa length le{ai aa ah get K}if}{ac ab rmoveto ai ad eq{af ae rmoveto }if}ifelse}stopped currentdict userdict begin P3_d ne{P3_d end begin}{end}ifelse}a/_doTexturePat aS /J{/aa b/ab b/ac b/ad b/ae b/af b gsave currentfont dup/V b/ag b/Y aS/S c/W d/X d/P3_dx d/P3_dy d ag begin FontType 3 eq end M N or and{gsave currentpoint newpath 1000 dup dup dup moveto lineto closepath clip moveto/R d ag begin FontMatrix concat 0 0 transform neg exch neg exch idtransform translate ag 65/BuildChar load end{exec}P Q s grestore Y{R M{6}{5}ifelse eq{/V S def/W U def/X T def}if R M{3}{2}ifelse ne{/S c}if/P3_dx W def/P3_dy X def W X idtransform/X b/W b/V V ag begin FontMatrix end makefont def S null ne{/S S ag begin FontMatrix end makefont def}if}{/S c}ifelse}if _doTexturePat{systemdict/makepattern known}{false}ifelse{matrix currentmatrix P3_tm setmatrix W X translate 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate settexturepat setmatrix W X translate W X rmoveto/ah d aa{/ai b Z 0 ai put V setfont currentpoint Z show au{exit}if}forall }{10 setlinewidth/ah d currentpoint newpath 0 0 moveto 0 0 lineto closepath moveto aa{/ai b Z 0 ai put currentpoint V setfont W X rmoveto count 1 add dup 1 roll Z true{charpath}stopped count count -1 roll sub{pop}repeat currentpoint{L}0 e pop newpath 0 dup dup dup moveto lineto closepath moveto au{exit}if}forall}ifelse grestore S null ne{gsave W X rmoveto 0 setgray/ah d aa{/ai b Z 0 ai put S setfont currentpoint Z show au{exit}if}forall grestore}if/K c/_doTexturePat aS}a/ax{5 index 4 index gt 8 index 3 index lt 6 index 5 index gt 9 index 4 index lt and and and[10 2 roll cleartomark }a/fp{tp{aload pop 1 1 4 index{gsave pop 3 index aload pop translate tr aload pop{clippath}stopped{-10000 dup dup dup} {pathbbox}ifelse ax{fsa{exec}forall}if 3 index aload pop 2 index add exch 3 index add exch 5 index astore pop grestore}for 4{pop}repeat}forall}a/aE{systemdict/vmreclaim known{1 vmreclaim}if vmstatus exch sub exch pop exch 10000 add lt{txrErrStr = flush stop}if}a/dia{userdict/P3_d get begin{{readstring}}{{readhexstring}}ifelse/aY b /ay b/ar ay{8}{exch}ifelse def/as b/at b/aT at ay{5 mul}{ar 1 eq{8 div ceiling}if}ifelse round cvi def /ba systemdict/colorimage known def/bb ay{ba{.8}{.2}ifelse}{1}ifelse def ay{/bc at 4 mul round cvi def /bd bc string def/be at round cvi def/bf be string def}if/az aT as mul round cvi def az bb mul aE /aU 30000 bb div aT div floor aT mul round cvi def/ia az aU div ceiling cvi array def/iai 0 def {/aA az aU le{az}{aU}ifelse def ia iai ay{/bg 0 def aA bb mul round cvi string aA aT div round cvi{ba {dup bg currentfile bd aY pop putinterval/bg bg bc add def currentfile bf aY pop pop}{ currentfile bd aY pop pop dup bg currentfile bf aY pop putinterval/bg bg be add def}ifelse }repeat}{currentfile aA string aY pop}ifelse put/iai iai 1 add def/az az aA sub def az 0 le{exit}if }loop end}a/aD{ia iai get/iai iai 1 add def}a/aV{ia iai get aW at getinterval/aW aW at add def}a /aZ{ia iai get length aW le{/iai iai 1 add def/aW 0 def}if}a/im{userdict/P3_d get begin /iai 0 def/aW 0 def ay{systemdict/colorimage known{{aV}{aV}{aV}{aV aZ}true 4 colorimage }{{aD}image}ifelse}{{aD}image}ifelse end}a/settexturepat{8 dict dup begin/PatternType 1 def /PaintType 1 def/TilingType 1 def/BBox tr def/XStep BBox 2 get BBox 0 get sub def/YStep BBox 3 get BBox 1 get sub def/PaintProc{pop save fsa{exec}forall restore}def end matrix gsave tp 0 get 0 get aload pop translate makepattern grestore setpattern}a/gofillit{systemdict/makepattern known{settexturepat {eofill}{fill}ifelse}{{eoclip}{clip}ifelse fp}ifelse}a{setpacking}if end end}if userdict begin P3_d begin/txrErrStr(A texture used in SuperPaint's draw layer is too large to print on this printer.)def end end "?d SPNT >g141 62 1 index neg 1 index neg matrix translate 3 1 roll currentpoint 2 copy matrix translate 6 1 roll "d SPNT 537 720 currentpoint 1 index 6 index sub 4 index 9 index sub div 1 index 6 index sub 4 index 9 index sub div matrix scale 11 1 roll ~[ 9 1 roll cleartomark 3 2 roll matrix concatmatrix exch matrix concatmatrix /P2_tp exch def P2_b mk end{md/bn known{bn}if}if Mmatrix currentmatrix aload pop count 6 roll P2_b mk end{md/bu known{bu}if}if Fuserdict begin P3_d begin count -6 roll matrix astore /P3_tm exch def )end end P2_b mk end{md/bn known{bn}if}if "d@SPNT Diagonal LinesSPNT 1did SPNT d SPNT  1rD! 8d SPNT 0+<`d SPNT  1(0S! 8d SPNT 0¡d SPNT 0'ݡd SPNT "١save gsave P2_b P2_tp concat end newpath 300.5 208.5 moveto 353.5 208.5 lineto 353.5 226.5 lineto 300.5 226.5 lineto 300.5 208.5 lineto 1 setlinewidth closepath flattenpath strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvx8]def /tr[0 0 40 40 ]def /tp[[[280 418 ]2 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore @,bd SPNT E,,b,b-a-a,b:,,@,@-@-@,@"-"/"1"3"5"7"9";"="?"A"C"E"G"I"K"M"O"Q"S,@b@b@a@a@b"U"W"Y"["]"_"a"c"e"g"i"k"m"o"q"s"u"w"y"{֠١d SPNT  >"١save gsave P2_b P2_tp concat end newpath 190.5 315.5 moveto 204.5 315.5 lineto 204.5 349.5 lineto 190.5 349.5 lineto 190.5 315.5 lineto 1 setlinewidth closepath flattenpath strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvxK]def /tr[0 0 40 40 ]def /tp[[[160 338 ]2 40 0 ][[160 298 ]2 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore @;^͠d SPNT E,;^;<]^:$;@;<@"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0".$;@;<@"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0".$@^@]^"|"z"x"v"t"r"p"n"l"j"h"f"d"b"`"^"\"Z"X"V$@^@]^"|"z"x"v"t"r"p"n"l"j"h"f"d"b"`"^"\"Z"X"V֠١d SPNT  >"١save gsave P2_b P2_tp concat end newpath 1 setlinewidth 206 192 moveto 206 182 lineto 230 182 lineto 230 249 lineto 222 249 lineto strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvx^]def /tr[0 0 40 40 ]def /tp[[[200 458 ]1 40 0 ][[200 418 ]1 40 0 ][[200 378 ]1 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore pޠd SPNT E42,"""""""""""""""""""" """"""""""""""""""""$","*"("&"$""" """""""""" " ""֠١d SPNT  >"١save gsave P2_b P2_tp concat end newpath 209.5 235.5 moveto 221.5 235.5 lineto 221.5 349.5 lineto 209.5 349.5 lineto 209.5 235.5 lineto 1 setlinewidth closepath flattenpath strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvxq]def /tr[0 0 40 40 ]def /tp[[[200 418 ]1 40 0 ][[200 378 ]1 40 0 ][[200 338 ]1 40 0 ][[200 298 ]1 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore @^ޠd SPNT E,^]^:(""""""""""""""""""""$","*"("&"$""" """""""""" " ""$@@"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0".(@^@]^"|"z"x"v"t"r"p"n"l"j"h"f"d"b"`"^"\"Z"X"V֠١d SPNT  >"١save gsave P2_b P2_tp concat end newpath 147.5 192.5 moveto 206.5 192.5 lineto 206.5 315.5 lineto 147.5 315.5 lineto 147.5 192.5 lineto 1 setlinewidth closepath flattenpath strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvxq]def /tr[0 0 40 40 ]def /tp[[[120 458 ]3 40 0 ][[120 418 ]3 40 0 ][[120 378 ]3 40 0 ][[120 338 ]3 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore @<Ϡd SPNT E,<;<:$"""""""""""""""""""" """"""""""""""""""""$"""""""""""""""""""" """""""""""""""""""" """""""""""""""""""" """""""""""""""""""" ","*"("&"$""" """""""""" " "" ","*"("&"$""" """""""""" " "" ","*"("&"$""" """""""""" " ""$<;<"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0". ;<"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0".$<;<"T"R"P"N"L"J"H"F"D"B"@">"<":"8"6"4"2"0".֠١d SPNT  >p;@;@@;d SPNT "١save {gsave P2_b P2_tp concat end newpath 1 setlinewidth 230 235 moveto 300 235 lineto 300 200 lineto 230 200 lineto strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvx8]def /tr[0 0 40 40 ]def /tp[[[200 418 ]3 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore p,,,d SPNT E,--,,-2-,"""""""""""""""""""",""" " " """"""""""!"#"%"'")"+,--,,-"-"/"1"3"5"7"9";"="?"A"C"E"G"I"K"M"O"Q"S֠١d SPNT  >pvvvd SPNT pСd SPNT pd SPNT 0d SPNT 0d SPNT 0d SPNT pd SPNT pBpplBBd SPNT QCFXd SPNT p.33..3d SPNT p$$$d SPNT pd SPNT pd SPNT p''''d SPNT p~  ~d SPNT pd SPNT p"CCB4d SPNT p*&&((((&d SPNT P ;Id SPNT Pʡd SPNT 0eld SPNT 0 d SPNT 0*2d SPNT 0?d SPNT 0c<d SPNT 0?d SPNT 0<)d SPNT p   ád SPNT p"("((d SPNT p *" " "*d SPNT p *  *d SPNT p͡d SPNT p222$͡d SPNT p .**.. Ρd SPNT p  Ρd SPNT p %( ( %%(d SPNT pd SPNT pd SPNT p5555d SPNT p6666d SPNT d SPNT 0dd SPNT  Q_! Xd SPNT  1b! 8d SPNT d SPNT p"d SPNT pyyΡd SPNT pd SPNT 0Xd SPNT pW-__[[-W-_d SPNT 0n6qd SPNT 0r6ud SPNT 0|6d SPNT pd SPNT p"VNVNZNZJJd SPNT pd SPNT pաd SPNT pd SPNT p.d SPNT p^ggg^աd SPNT p^ggg^d SPNT p.agbgagagagbd SPNT p[GyG[GyGd SPNT p[ggg[d SPNT p[[G[[Gd SPNT pnqnnqd SPNT p^yy^Ρd SPNT p"Wgb^^WWgd SPNT pW^W^^d SPNT pd SPNT py{y{{yd SPNT p:::d SPNT "١save gsave P2_b P2_tp concat end newpath 1 setlinewidth 326 189 moveto 321 189 lineto 321 195 lineto 326 200 lineto 326 156 lineto strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvx^]def /tr[0 0 40 40 ]def /tp[[[320 498 ]1 40 0 ][[320 458 ]1 40 0 ][[320 418 ]1 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore pAFFAAFFd SPNT EhAGFGAFBFBCABCDBCDECDEFDEEFFG2AG FG"U"W"Y"["]"_"a"c"e"g"i"k"m"o"q"s"u"w"y"{`AGFGAFBFBCABCDBCDECDEFDEEG"U"W"Y"["]"_"a"c"e"g"i"k"m"o"q"s"u"w"y"{ FG"U"W"Y"["]"_"a"c"e"g"i"k"m"o"q"s"u"w"y"{֠١d SPNT  >pBFBBFd SPNT  dSPNT &Qz d&SPNT j~+|d SPNT  ,  Helvetica .+gEchelle  >Qz Qz Qz PPPP UUUU"ud SPNT  dSPNT &C)z<d&SPNT j0}gd SPNT  (a Secondary  >C)z<C)z<C)z<`dPPPP` "od SPNT  dSPNT &J6z` d&SPNT j=md SPNT   (Y8Direct * imaging * mirror  >J6z`J6z`J6z`?"" >?@"@"PP**  >"}8d SPNT  dSPNT &>^z} d&SPNT jid SPNT  (XTPrimary * (collimator)  >>^z}>^z}>^z} >"""|`*d*  P P>"""""qTd SPNT  dSPNT &S}yd&SPNT j~d SPNT  +%Flat #3  >S}yS}yS}y` @@PP"vyd SPNT  dSPNT &Izd&SPNT j"d SPNT  (b Slit wheel  >IzIzIzPPPP00` "pd SPNT  dSPNT &>zd&SPNT j7!d SPNT  (]Filter wheels  >>z>z>z PPPPPP00PP"kd SPNT  dSPNT &Iz d&SPNT jE1d SPNT  + Incoming* light  >IzIzIz"|  >"""yd SPNT  dSPNT &P d&SPNT lPFd SPNT  +Dewar * vacuum * case  >PPP  >><PP>@@@<00"@"@@@PP*@*@  @@ "d SPNT  dSPNT &;d&SPNT l@6d SPNT  (\74 K cold box  >;;;@ @@@p"jd SPNT  dSPNT &4d&SPNT l&d SPNT # ([|IR Detector array  >444`dPPPPPPPP p"i|d SPNT  dSPNT &\~d&SPNT ld SPNT  (p{Flat #4  >\~\~\~@@@@PP"~{d SPNT  dSPNT &@(H d&SPNT .ud SPNT  (_Spherical relay * mirror  >@(H@(H@(H`dPPPPPP >PP"" > >`    >"xd SPNT  dSPNT &b  d&SPNT p Kd SPNT  (~Echelle drive * housing  >b b b PP0?""PP >P$P**><""  "d SPNT  dSPNT &$ d&SPNT Ad SPNT  ? (^dClosed-cycle cooler * (outline)  >$$$PPPP`d@@@** P>P PP"|><" " "wdd SPNT  dSPNT &6 d&SPNT O]d SPNT  +\ Incoming * light  >666"|  ?"""d SPNT  dSPNT &d&SPNT ,-d SPNT  (Echelle  >PPPP"d SPNT  dSPNT &d&SPNT d SPNT   ( Flex pivot  >0@PP"d SPNT  dSPNT &d&SPNT d SPNT   ( Echelle yoke  >PP@`dPPPP"d SPNT  dSPNT &d&SPNT d SPNT   ( Ball drive  >PP0PP`"d SPNT  dSPNT &d&SPNT gd SPNT   +Flat #1  >@@PP"d SPNT  dSPNT &e d&SPNT f'd SPNT   (hInput * lens  >eee $** >**"hd SPNT  dSPNT &Md&SPNT 8RVd SPNT ( (sClosed cycle cooler  >MMMPPPP`dPP PP  "-sd SPNT d SPNT d SPNT qd SPNT pd SPNT d SPNT d SPNT d SPNT qGRGRGJd SPNT p%J%Jd SPNT d SPNT d SPNT d SPNT qd SPNT pJJd SPNT d SPNT  dSPNT &dO d&SPNT Ud SPNT  +PDirect imaging * mirror  > dOdOdOPP >"" PP> >   > UUUU"Td SPNT  dSPNT &fd&SPNT kd SPNT   +Primary  >fff`dPP"md SPNT  dSPNT &sd&SPNT wd SPNT   )Flat #3  >sss` @@PP"{d SPNT  dSPNT &xd&SPNT -d SPNT   ( Slit wheel  >xxxPPPP00` "d SPNT  dSPNT &md&SPNT <d SPNT   (Filter wheels  >mmm PPPPPP00PP"d SPNT  dSPNT &d&SPNT Id SPNT   + Dichroic  > "d SPNT  dSPNT &c d&SPNT Ud SPNT  (p Dewar vacuum * case  > ccc  PP0PP**0$0**PP** """d SPNT d SPNT d SPNT qW[[W[Zd SPNT BpZccZd SPNT d SPNT d SPNT d SPNT q""! d SPNT Bp ~~ d SPNT d SPNT d SPNT d SPNT q:y>}>z:y=}<{d SPNT Bp<{mm<{d SPNT d SPNT d SPNT d SPNT q6o:r:o6o9r9pd SPNT Bp9pyy9pd SPNT d SPNT d SPNT d SPNT q h$j$h h#j#id SPNT Bp#iyy#id SPNT d SPNT d SPNT d SPNT q.Z2]2Z.[2]1\d SPNT Bp1\ll1\d SPNT d SPNT d SPNT d SPNT q0H4K4H0I4K3Id SPNT Bp3IeWeW3Id SPNT d SPNT dSPNT &+xg d SPNT  >c (:}{  > UUUU"M}d SPNT dSPNT & d SPNT  >({  >"d SPNT d SPNT d SPNT qd SPNT Bpzzd SPNT d SPNT d SPNT d SPNT qd SPNT Bpyyd SPNT d SPNT d SPNT d SPNT qd SPNT Bpzzd SPNT d SPNT d SPNT d SPNT qd SPNT Bpyyd SPNT d SPNT d SPNT d SPNT qy||zyzd SPNT Bpykzykzzd SPNT d SPNT d SPNT d SPNT qBEECBCd SPNT Bpy?Cy?CCd SPNT d SPNT d SPNT d SPNT q<??><>d SPNT Bpy4>y4>>d SPNT d SPNT d SPNT d SPNT qd SPNT Bpyyd SPNT d SPNT d SPNT d SPNT q=AA=A@d SPNT Bp@RR@d SPNT d SPNT d SPNT d SPNT q030131d SPNT Bp1>1>11d SPNT d SPNT d SPNT d SPNT q\__]\]d SPNT Bp]dd]]d SPNT d SPNT d SPNT d SPNT q      d SPNT Bp ZZ d SPNT d SPNT d SPNT d SPNT q    d SPNT Bp 11" d SPNT d SPNT d SPNT d SPNT q###"d SPNT Bp"AA"d SPNT d SPNT d SPNT d SPNT q*..*.-šd SPNT Bp-\\-šd SPNT d SPNT d SPNT d SPNT q   d SPNT Bp  d SPNT d SPNT d SPNT d SPNT qd SPNT Bpd SPNT d SPNT d SPNT d SPNT q١d SPNT Bp١d SPNT d SPNT d SPNT d SPNT q   ơd SPNT Bpơd SPNT d SPNT  dSPNT & d&SPNT d SPNT  (Rubber * damper  > >*P*P""?   > **p"" UUUU"d SPNT  dSPNT &d&SPNT d SPNT   (Bellows  > PP00PP`"d SPNT d SPNT d SPNT qˡd SPNT Bpˡd SPNT d SPNT d SPNT d SPNT qءd SPNT Bpءd SPNT d SPNT d SPNT d SPNT q\`\`]^d SPNT BpL^L^d SPNT d SPNT "?d SPNT #d SPNT #d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT "?d SPNT d SPNT pd SPNT Bpd SPNT d SPNT pd SPNT pd SPNT pd SPNT p2;2;d SPNT p2;;2d SPNT p=@=@@>d SPNT "yd SPNT "yd SPNT "yd SPNT "yd SPNT "yd SPNT "y d SPNT "yd SPNT "yd SPNT "yd SPNT "yd SPNT "yd SPNT "yd SPNT ""d SPNT ""d SPNT ""d SPNT ""d SPNT ""d SPNT ""d SPNT "" d SPNT "" d SPNT "" d SPNT "d SPNT #d SPNT "d SPNT "d SPNT "d SPNT "d SPNT " d SPNT " d SPNT " d SPNT "3d SPNT "3d SPNT "3d SPNT "3 d SPNT "3 d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3d SPNT "3!d SPNT "vd SPNT "vd SPNT "v d SPNT "v d SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "vd SPNT "v"d SPNT "v&d SPNT "_'d SPNT "yG$d SPNT #d SPNT #d SPNT #d SPNT "B-d SPNT "١save gsave P2_b P2_tp concat end newpath matrix currentmatrix 0.977 1 scale 333.671 157 43.5 0 90 arc setmatrix 1 setlinewidth flattenpath strokepath 0userdict begin P3_d end begin -658 /ph exch def %%BeginProcSet: Beachlet 1 0 userdict begin/Beachlet 2 dict def Beachlet end begin /oldmatrix 6 array def/newmatrix 6 array def end %%EndProcSetu /fsa[(gsave newpath 0 0 moveto 40 0 lineto 40 40 lineto 0 40 lineto closepath 1 setgray fill grestore 0 setgray)cvx (/showpage{}def %!PS-Adobe-2.0 EPSF-1.2 %%Creator: SuperPaint %%Title: Diagonal Lines %%CreationDate: 9/12/91 %%BoundingBox: 0 0 40 40 %%Pages 1 %%DocumentFonts: Symbol %%DocumentNeededFonts: Symbol )cvx(/showpage{}def  %%EndProlog %%BeginSetup userdict/Beachlet get begin %%EndSetup %%Page One 1 newpath 0 0 moveto 0 40 lineto 40 40 lineto 40 0 lineto closepath clip gsave 0 40 translate 1 -1 scale newpath 21.5 60.5 moveto -20.5 18.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 23.5 58.5 moveto -18.5 16.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 25.5 56.5 moveto -16.5 14.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 27.5 54.5 moveto -14.5 12.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 29.5 52.5 moveto -12.5 10.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 31.5 50.5 moveto -10.5 8.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 33.5 48.5 moveto -8.5 6.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 35.5 46.5 moveto -6.5 4.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 37.5 44.5 moveto -4.5 2.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 39.5 42.5 moveto -2.5 0.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 41.5 40.5 moveto -0.5 -1.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 43.5 38.5 moveto 1.5 -3.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 45.5 36.5 moveto 3.5 -5.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 47.5 34.5 moveto 5.5 -7.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 49.5 32.5 moveto 7.5 -9.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 51.5 30.5 moveto 9.5 -11.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 53.5 28.5 moveto 11.5 -13.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 55.5 26.5 moveto 13.5 -15.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 57.5 24.5 moveto 15.5 -17.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap newpath 59.5 22.5 moveto 17.5 -19.5 lineto 0 setgray currentlinecap 2 setlinecap 0.25 setlinewidth stroke setlinecap grestore showpage %%Trailer end )cvxq]def /tr[0 0 40 40 ]def /tp[[[280 538 ]3 40 0 ][[280 498 ]3 40 0 ][[280 458 ]3 40 0 ][[280 418 ]3 40 0 ]]def end userdict begin P3_d end begin 1 -1 scale 0 ph translate tr aload pop pop pop neg exch neg exch translate false gofillit end grestore restore `qqZZd SPNT E 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Front and side views of CSHELL. The length of the dewar vacuum case (tom to bottom) is 64 cm. + cThe inner cold box is thermally isolated and mechanically supported by fiberglass tabs (not shown). >{{{  `0@ pHH @ ?@ 0 @ ?    @H@H  @HHH H@_@P?@  @PHH ``?HH`` ` HH HH@  @@ _ **@ HHHHP P ? @0 H_8 @  @@ HH` ``HH@?`` _HHHH@P@HH _ H(@H`H@@@@`** UUUU" dSPNTum d PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelvd PPNTHelv "d*d PPNTHelvdPPNTSymbol, Symbol .+D d PPNTHelvdPPNTSymbol)l ) m ( il ) m +q d PPNTHelvd PPNTHelv,  Helvetica(( ) m ) / )pixel )) )C ( p( ) m ) ) d PPNTHelvdPPNTSymbol(L= ) +  d PPNTHelvd PPNTHelv(d2 ) tan )( ) ) d PPNTHelvd PPNTHelvd PPNTHelv 5 D 6 &  # AWj# H 1Xkl# 8  Qk# 1M# 8 1;J# 8#"B#"F#"? #" ;#";#"; 17# 8#"0#"0#" 0#"#" #" #"#"#"#"#"#""#"%#"(#"+#"/#"2 k # w#"W#"> 1>b# 8 19V# 8 1 3# 8 1C-O# 8#"b################################pJbq-bej j moopqqq!q&q&q)q-q-  r ",  Helvetica .* Observer on workstation*in observer's room  N #( "IC (Instrument Control) execute on*PC at telescope 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