The SOAR Goodman Spectrograph Red Camera is equipped with a 4096 x 4112 pixel, back-illuminated, deep-depletion, astro-multi-2 coating, e2v 231-84 CCD.  The CCD is read out through 1 amplifier using a Spectral Instruments [21] controller.  This CCD has excellent cosmetics.  Figure 1 shows a bias frame obtained in Spectroscopic 1x1 ROI mode and with the 344ATTN3 readout (Gain=1.48 e-/ADU, Readout Noise=3.89 e-). Figures 2 and 3 show a dome quartz lamp flat for the 400 l/mm grating in the 400M2 setup (505-905 nm).  Note the almost complete lack of fringing at the red end of the image, compared to the Blue Camera CCD [14] (Figure 4).

Figure 1. Goodman Red Camera bias frame (ROI: Spectroscopic 1x1; Readout: 344ATTN3)

Figure 2. Goodman Red Camera Dome Flat. Grating: 400, Mode: M2 + GG455 filter, ROI: Spectroscopic 1x1, Readout:344ATTN3, Dome lamps at 100%, Texp=20s

Figure 3. Plot of the above dome flat, along the wavelength direction (averaged 10 pixels across the spatial direction). Redder wavelengths to the right.

Figure 4. Comparison of dome flats obtained with the Blue and Red cameras, normalized at 5000A, using the 400M2+GG455 grating setup and 1.03 arcsec slit.

Click on this link for a PDF version of this info sheet [22]

We have obtained observations of standard stars in order to determine the system throughput with the Red Camera. Results will be posted soon.

Goodman Red Camera Cold Start page [23]

The SOAR Goodman Spectrograph Blue Camera features one 4096 x 4096 pixel Fairchild CCD.  The CCD is read out through 1 amplifier using a Spectral Instruments [21] controller.  This CCD has only minor flaws which has little impact on its scientific performance.  Figure 1 shows the combination of 20 bias frames taken with the 200ATTN0 readout mode (Readout Noise= 4.74 e-, Gain=1.4 e-/ADU), with the Spectroscopic 1x1 ROI.

Figure 1. Combined Bias frames in Spectroscopic 1x1 mode (average of 20 individual bias taken with the 200ATTN0 readout mode).

Figure 2 below shows an internal quartz lamp flat for the 400 l/mm grating in the 400M2 setup (505-905 nm).  Note the fringing pattern at the red end of the image. 

Figure 2: An internal quartz lamp flat of the 400l/mm grating in the 400M2 setup, taken with a Multi-Object Slit (MOS) Mask, The upper two and lower srtpes correspond to the square boxes for the alignment stars. The middle stripes are the quartz flats produced with the four science target slits.

Figure 3 shows the QE of the Goodman Blue Camera CCD.

Figure 3:  The QE curve of the Goodman CCD.

Below we provide the general characteristics of the Blue Camera detector and the available readout modes:

The default image size for imaging mode (1x1 binning) is 3096 x 3096 pixels and the default image size for spectroscopic mode is 4142 x 1896 pixels with 1x1 binning. These values were used calculate the read out times given above using one amplifier readout. Users should also expect 1 or 2 seconds of overhead on every exposure. 

Throughput: 
The imaging mode throughput of the GOODMAN BLUE CAMERA has been measured relative to the SOAR Optical Imager (SOI) for which we have good zero-points. As the table below shows, the throughput relative to SOI is better in the R, comparable in the V and lower in the B and U.
 
In the Goodman Throughput Information [16] page we show the measured the spectroscopic throughput of the Goodman BLUE CAMERA, obtained by taking spectra of spectrophotometric standards with the most commonly used preset setups. These curves show the overall system efficiency for the telescope+instrument+detector combination, with and without the Atmospheric Dispersion Corrector (ADC), commissioned in late 2014. That is, they show the fraction of photons striking the primary mirror of SOAR which are eventually detected by the CCD. The measurements were made using a very wide (~10 arcsec slit); slit losses will reduce the efficiency obtained when using a narrower slit by an amount which depends on the seeing. The measurements are corrected for atmospheric extinction; the efficiency obtained in an actual observation will be reduced by the atmospheric extinction for the airmass of observation.

Goodman Blue Camera Cold Start page [24]

Updated Apr 2018.

Up to three (3) gratings can be installed in the spectrograph at a time, in a linear stage which allows the rapid interchange of gratings. Installing different gratings is a day time operation. No grating installations are done during the night.

• 1200 line gratings: For observations in the UV use the 1200Blue grating + Blue Camera. Observations in the 450nm - 550nm range should use the 1200Blue grating, with either Blue or Red Cameras. For observations redward of ~600nm, use the 1200Red grating + Red Camera.

Configurations remain as listed in the table below.

Long Wavelength Limit for High Resolution Gratings
Because of limits in the camera rotation stage, it is not possible to use the 1800, 2100 and 2400 l/mm gratings beyond certain wavelength limits.

The table below shows the dispersion and the wavelength coverage for observations in our set spectroscopic modes.  Please note that the 1800, 2100, and 2400 l/mm gratings are operated in Custom mode where the observer selects the central wavelength for their observations.

The VPH gratings operate via Bragg scattering and their efficient operation requires Littrow or near-Littrow operation of the spectrograph. A grating rotation stage sets the incident angle to the desired value, which depends upon the line density of the grating and the central wavelength of interest. A concentric camera rotation stage must then be set to nearly twice this angle to intercept the diffracted beam.  A set of fixed observing modes for each grating are given below, where applicable.  All gratings can be used in the Custom mode.

The Goodman High Throughput Spectrograph (GHTS) has an assortment of long slits from which the user can choose, in addition to the possibility of creating custom Multi-Object Slit (MOS) masks.

The GHTS has a carrousel with 36 positions, of which 27 are available for longslits and/or Multi-Objects Masks (MOS).   Each long slit is approximately 3.9 arcmin long.
As of Aug 23, 2017, long slits which are always installed and available are the folllowing (all widths in arcsec; the unbinned pixel scale of the GHTS is 0.15 arcsec/pixel):

0.45", 0.6", 0.8", 0.95", 1.0", 1.2", 1.5", 1.9", 3.2", 4" and 10.2". 

The following table provides the old names of some of the slits.

We have 16 remaining positions are available for MOS masks. Installing MOS masks is a daytime task, like changing filters, and should be requested beforehand in the Instrument Setup Form [25], or by email to the Support Astronomer with copy (cc) to soarops@ctio.noao.edu [26], so our Observer Support staff also receives the request.

Note: the Goodman Acquisition Camera (GACAM) [27] has a FOV=1.8arcmin in its longest dimension, therefore, it does not span the full length of a Goodman long slit. If your science requires a full view of the long slit you will need to use the pre-imaging procedure for object acquisition (see the Step-by-step guide to Observing with Goodman [9]).

Instrument Overview

The Goodman High Throughput Spectrograph has been upgraded to provide users with the choice of one of two separate cameras.
One is the original UV-optimized Blue Camera, with a 4096x4096 Fairchid CCD.  The new device  is the Red Camera, equipped with an e2v 4096x4096 detector optimized for work at red wavelengths with negligible fringing redward of ~650nm  compared to the Blue Camera.  For both detectors the pixel scale is the same (0.15 arcsec per pixel).  This provides a 3096 x 3096 unbinned pixels (~7.2 arcmin diameter) FOV in imaging mode and a 4096 x 1896 unbinned pixels FOV in spectroscopic mode.  The long slit masks in spectroscopic mode are approximately 3.9 arcmin in length and cover ~1560 unbinned pixels, leaving enough pixels above and below the slit to obtain an estimate of the stray and scattered light.

In both cameras, the CCD is read by the Spectral Instruments [21] controller. In the Blue Camera through 1 amplifier. 
Blue Camera: Depending on binning and the gain setting, the CCD can be read in as little as 20 seconds (1x1 fast readout) to as long as 80 seconds (1x1 slow readout) in spectroscopic mode.  Please see the table given in the Goodman Overview [5] page for a more detailed description. 

The data are taken via a vncviewer on the Goodman data acquisition computer (soaric6 for the Red Camera and soaric2 for the Blue Camera) and examined via a vncviewer on the Goodman data analysis computer (soaric7).  From soaric7, one can transfer the data to their home institution using "scp".

Unbinned Goodman spectra plus overscan and header information are approximately 16 Mbytes each.  A typical night produces about 2-4 Gbytes of data and easily transferred over the internet.  This is the preferred method of the SOAR partners.  If this is unfeasible, please contact Sean Points prior to your run so that other options can be discussed.

The Goodman imaging (first) filter wheel contains space for 4 square 4x4 inch filters, plus one blank position. The second  filter wheel holds 4 inch diameter circular filters, and has 6 positions, 5 regularly equipped with the order sortting spectroscopic filters, and one open position. Filters may be up to 10mm thick. 
For the list of available filters look at the SOAR Filters page. [17] Special arrangements for installing filters should be consulted well in advance of an obsreving run with the Instrument Scientist.

Philosophy and Structure of this Manual

This manual is intended for an observer planning to use the Goodman spectrograph.  It is not intended to serve as a hardware or software reference document describing the inner workings of Goodman, although some details at that level may appear to help the observer plan observing strategies.  Also, we assume that the observer is already familiar with CCD cameras, spectroscopic observations, and data reductions.

The Goodman Overview [5] is at the front of this manual. If you've read this far, and don't plan to read any further, be sure you understand the Goodman Overview [5] pages.

Development of the Goodman High Throughput Spectrograph is a continuing process.  Throughout the lifetime of the instrument, filters will be added, old ones replaced, and software enhanced. This manual represents the status as of the date on the cover page. We expect to revise the manual occasionally to include information gained during engineering runs, as well as to reflect new filters.

Supplemental Information

A Beginner's Guide to Using IRAF [59] (IRAF Version 2.10), Jeannette Barnes, August 1993

A User's Guide to CCD Reductions with IRAF [60], Philip Massey, February 1997

A User's Guide to Reducing Slit Spectra with IRAF [61], Phil Massey, Frank Valdes, Jeannette Barnes, April 1992

Guide to the Slit Spectra Reduction Task DOSLIT [62], Francisco Valdes, February 1993

In this section  you will find a description of the hardware and main components of the Goodman HTS. Click on this link for a PDF file containing photos and further notes of each mechanism. [63]

The Goodman Spectrograph Control System (GSCS) is a system of Labview programs running on a Windows machine, with which observers control the spectrograph and take data using its CCD camera. To access this software, users must use a graphical desktop sharing system to connect to the spectrograph’s control computer. We recommend using a VNC connection (see the SOAR Remote Observer's Guide [65]), but other types of software may be used, such as Windows Remote Desktop. The following set of instructions for linking to the Goodman computer assumes that the user has established a secure VPN connection and will use a VNC or Remote Desktop session (click here to for a PDF document providing additional information on how to connect and run the Goodman GUI). [66] This dcument shows the example for the Blue Camera. For the Red Camera only the name of the computer changes (see below).
 

Logging on to the Data Acquisition and Data Analysis Computers

The data acquisition computers are:

• soaric2 if using the Goodman Blue Camera [14]
• soaric6 fif using the Goodman Red Camera. [15]

The data visualization computer running IRAF is soaric7. A number of different ways to logon to these machine exist, depending upon your preference. These methods are discussed below.

• From Cerro Pachón:
  • The mountain staff or your support scientist will show you the computer on which you can obtain and analyze your data. To open the Goodman user control panels:
    • Double click on the "Scroll Lock" Key
    • A window will open displaying the names of the computers to which you can connect
    • Use the "Up" and "Down" arrow keys to highlight a free machine.
    • If the Data Acquisition and Analysis windows are running, you can skip to the GUI Layout section of this manual. If these GUIs are not running, skip to the Starting and Stopping the Data Acquisition GUI and Starting and Stopping the Data Analysis GUI sections of this Manual.

• From the Remote Observing Center in La Serena:
  • Log on to the observing account using the username and password provided to you by the instrument scientist (Sean Points, César Briceño, Regis Cartier or Alfredo Zenteno if your time is through NOAO or Chile, or your Brazilian Support astronomer if you are observing through Brazil time). If forgotten, these are posted on a list near the door.
  • Start the Data Acquisition GUI by typing the following command from a terminal command line on the GNU/Linux computer in the remote observing center:
  • > vncviewer -Shared soaric2.ctio.noao.edu & (Blue Camera [14])
  • > vncviewer -Shared soaric6.ctio.noao.edu & (Red Camera [15])
    Log on to the vncviewer with the password provided by the instrument scientist.
  • Start the Data Analysis GUI by typing the following command from a terminal command line on the GNU/Linux computer in the remote observing center:
  • > vncviewer -Shared soaric7.ctio.noao.edu:4 &
    Log on to the vncviewer with the password provided by the instrument scientist.

• If you are a Remote Observer:
  • Start the VPN connection on your computer, using the username and password information provided by your Support Scientist: Sean Points or César Briceño if your time is through NOAO or Chile, your Brazilian Support astronomer if you are observing through Brazil time, or your SOAR Support person at UNC or MSU.
  • Start the Data Acquisition GUI by typing the following command from a terminal command line on the GNU/Linux computer in the remote observing center:
  • > vncviewer -Shared soaric2.ctio.noao.edu & (Blue Camera [14])
  • > vncviewer -Shared soaric6.ctio.noao.edu & (Red Camera [15])
  • Log on to the vncviewer with the password provided by the instrument scientist.  Set this GUI in one of your monitors.
  •  
  • Start the Data Analysis GUI by typing the following command from a terminal command line on the GNU/Linux computer in the remote observing center:
  • > vncviewer -Shared soaric7.ctio.noao.edu:4 &
    Log on to the vncviewer with the password provided by the instrument scientist. Set this GUI in another of your monitors. Remember that a minimum of 2 monitors is required to carry out remote observing at SOAR, and the recommended setup is 3 monitors (see the SOAR Remote Observer's Guide). [65]

In most cases the GUIs should be started and you will be presented with a data acquisition screen and data analysis screen as shown in Figure 4.

Figure 4: The Goodman Data Acquisition and Data Analysis GUI windows.

Starting and Stopping the Data Acquisition GUI

If the data acquisition GUI has not been started, then one should see a blue screen in the soaric2 VNC window. At the bottom of the screen, you should see that the SI Image SGL D and SI Image are minimized.  You may also see that the LabVIEW Transfer_To_SOARIC7 vi and the LabVIEW Goodman Spectrograph Control System vi are minimized.  If these are minimized, the you just need to click on them to start the data acquisition GUI.  Click here for a PDF file with additional information on the start-up of Goodman. [67]

To start the data acquisition software:

Figure 5: Selecting the CCD parameters (e.g., 1x1 imaging, 2x2 imaging, 1x1 spectroscopic, 2x2 spectroscopic, etc.)

Figure 6: Selecting the detector readout parameters.

• Click the Transfer_To_SOARIC7 LabVIEW shortcut on the Desktop and start the application by clicking on the white arrow.
• Open the Goodman controls by clicking on the GSP_Main LabView shortcut on the Desktop and start the application by clicking on the white arrow.
• Check the camera panel. If a green button is present for "Connection Open/Getting Data" in the upper left of the GUI, Goodman "sees" the SI Image camera control software and a TCP/IP connection is available to take data. You can confirm this by clicking on the "Obtain Camera Status" button. During a normal startup of the GSP_Main vi the CCD Temp will read "0". If the TCP/IP connection is operating, clicking on the "Obtain Camera Status" button will show the latest temperature measurement. If Goodman is cooled, the CCD Temp should be -106.5. If the CCD Temp does not update, you will need to check the SI Image SGL D window and make sure that a TCP/IP connection is open.
• Click on Main tab and logon;
  Use the account appropriate for your observing program (i.e., BRAZIL, CHILE, MSU, NOAO, OTHER, or UNC) with the password provided by your institution.
• Click the User tab, go to "Home Systems", and select "Home All". You should see the dark green lights change to yellow on the control panel as systems are being homed. Upon a successful homing of the systems, all lights should be bright green, except the Collimator Focus which well remain a dark green.  If there are any red lights, you will need to log out of GSP_Main and shutdown and cycle the power on the Goodman motor electronics.
• After the camera is homed, start the flexure correction by clicking the flexure LED. It should change from dark green to bright green.
• Select the imaging or spectroscopic mode in which you want to work.
• Select Gain and Readout Setting. These values are given in the Goodman Overview [5] and in the Goodman Cheat Sheet [28].   Usual values are 100 KHz ATTN0 with the Blue Camera, which provides gain=1.06 and readout noise= 3.72 e-, and 344KHz ATTN3 with the Red Camera, which provides gain=1.48 and read noise=3.89.
• Set up the grating and camera angles for your observations. The pre-defined modes are listed in the Goodman Overview [5].
• You are now ready to use Goodman.

If the data acquisition GUI needs to be stopped:

• Single click on the Main tab and log out.
• Click on the Main tab and Shutdown.  This will move all the systems back to their "Home" positions.
• After the shutdown has finished you should ask the TelOps staff to turn off the power to the Goodman electronics box.

A more detailed explanation of the Startup and Shutdown procedures can be found in the Goodman step-by-step User's Observing Guide (PDF). [9]
 

Starting and Stopping the Data Analysis GUI

The Goodman data analysis VNC window (soaric7:4) has a relatively simple layout. If the IRAF data analysis windows are not open, you should see an IRAF button in the lower right corner of the VNC window.  Single click on the IRAF button and an IRAF xgterm and a ds9 window will open.  Load any IRAF package you may need for your observing.  You will also want to make sure that you are in the correct directory to analyze your data.

> cd /home3/observer/today/
 

Basic GUI Layout

All observing with the Goodman Spectrograph is handled through the Data Acquisition GUI. Upon successful startup of the Goodman data acquisition GUI on soaric2, one should check that the Goodman data acquisition window looks something like that shown in Figure 4. 

The Goodman observing GUI can be divided into certain distinct regions as shown in Figure 7. These include the:
 

Figure 7: The Goodman data acquisition GUI with regions demarcated and labeled.

• TCS Status Region - This region shows various telemetry data from the instrument, as well as information obtained from the Telescope Control System (TCS) and the SOAR Environmental Station. These data include the current RA and Dec of the telescope, the airmass, the sidereal time, the ISB rotator angle, etc.

• Connection Info Region - This region shows if the LabVIEW GSP_Main vi has a TCP/IP connection to the SI Image software.  If the conection is active, then you should see a green box stating that the TCP/IP conection is open and that the SI Image software is receiving commands from the GSP_Main vi.  One method of checking this connection is to click on the "Obtain Camera Status" button while you are not taking an image.  This should update the "CCD Temp." and "Vacuum Pressure" fields above the camera status button.  Also included in this section of the GUI is the "General" tab.  If an observer selects this, they will be able to edit the "Observer" and "Proposal ID" keywords for the FITS headers.

• Acquisition and Exposure Status Region - This region of the GUI is complex and contains many items of which the observer should note. In this region, the observer can do the following:

• 

  Figure 8: Selecting the CCD binning and image size.

   

   

  Figure 9: Selecting the Goodman readout parameters.

   

  Figure 10: (a) Taking an internal calibration quartz spectrum.  In this image the internal quartz lamp is off. (b)  Taking an internal lamp quartz spectrum.  The quartz lamp has been turned on at the 70% level.

   

  • Change the OBSTYPE (OBJECT, FLAT, COMP, DARK, or ZERO) of the image by clicking on the appropriate tab.
  • Edit the "Object Name" for the FITS headers.
  • Set the number of exposures for each OBSTYPE.
  • Set the base name of the FITS file.
  • Set the exposure time.
  • Select the CCD binning and image size.  The default 1x1 imaging mode has an image size of 3096x3096 pixels.  The default 1x1 spectroscopic mode has an image size of 4142x1896 pixels.  Please note that no overscan region is written for imaging mode.  The overscan region is only read if the serial dimension is greater than 4096 pixels.
  • Select the CCD readout speed, gain and readnoise parameters.
  • Turn on/off calibration lamps (HgAr, CuHeAr, Ne, Ar, Quartz).  For example, select the "Flat" tab in the "Acquisition and Exposure Status" region of the GUI (see Figure 10).  All of the calibration lamp LEDs should be dark green (Figure 10a).  If you are using the internal quartz lamp, select the desired intensity value and then click the dark green box beneath the "Quartz" label.   The dark green box should now be bright green (Figure 10b).  You should always check with the telescope operators that the calibration lamp has been turned on.
  • Make a telescope offset.
  • View the exposure time and readout status.

  All of these features will be discussed in more detail in the Observing with Goodman [68] section of this manual.

• Instrument Status Region - This region of the GUI is equal in its complexity as the Acquisition and Exposure Status Region.  In this section, the observer controls the physical setup of the spectrograph. In this region, the observer can do the following:

•  

  Figure 11: Changing the primary filter.

   

   

  Figure 12: Changing the secondary filter.

   

   

  Figure 13: Selecting the slit mask assembly.

   

   

  Figure 14: Selecting the grating.

   

   

  Figure 15: Selecting the camera and grating angles (Wavelength Assembly).

   

   

  Figure 16: Selecting the camera focus.  The set camera focus region is located in the bottom right-hand corner of the GUI.  To change the camera focus, the observer should change the "Target" value to the desired camera focus and then press the "Set" button.

   

  • Check on the status of the motor sub-systems. This is indicated by the vertical column of round lights (LEDs) on the left of the display. If the lights are bright green, it signifies that the sus-systems are homed and/or in their proper positions as determined by the sub-displays in this region. If the lights are dark green, it indicates that the sub-system has not been homed. At present, only the status light for the Collimator Focus should be dark green (see below).  If the status light is yellow, it signifies that the sub-system is moving from one state to another. For example, if you change the Slit Mask from the 0.46" slit to the 1.03" slit, the light to the left of "Mask Assembly" will change from bright green to yellow and then back to bright green during the exchange of slit masks. If a motor light should be red, it indicates that an error has occurred and that the observer needs to shutdown the Data Acquisition GUI and restarted after the power to the instrument electronics box has been cycled.
  • Change the "Primary Filter".  The Goodman filter wheels can hold 5 +1 (empty) 4" diameter filters.  We have placed UBVR filters on the Kron-Cousins system in the primary filter wheel on Goodman (see Figure 11).
  • Change the "Secondary Filter".  The Goodman filter wheels can hold 5 + 1 (empty) 4" diameter filters.  We have placed GG-385, GG-455, GG-495, and OG-570 order blocking filters in the secondary filter wheel.
  • Change the "Slit Mask".  An observer can change the Slit Mask from that which is currently in place by clicking on the upper-most button under the "Mask" section of the GUI and select a different slit mask (see Figure 13).  After a successful startup of the GUI no slit mask will be in place.  The observer should then choose from among our current long-slit masks as given in the Goodman Overview [5].
  • Change the "Grating". An observer can choose from no grating, to any of the maximum of three gratings that can be installed at a given time, e.g., the 400l/mm, 600l/mm, or 1200l/mm by clicking on the grating selection button. For the updated list of available gratings see the Goodman Overview page [5].
  •  Select the "Camera and Grating" angles for the observations.  This feature allows the observer to select among the various predetermined spectroscopic modes of the instrument (see Figure 15).  These modes are listed in the Goodman Overview [5] section of this manual.  We provide examples of HgAr and CuHeAr spectra in the Comparison Lamp [31] section of the Goodman documentation.
  •  The "Camera Focus" depends upon the observing setup that the observer chooses. The TelOps staff have a list of the most recent camera foci that have been determined during an engineering run. If in doubt, the observer should determine the best camera foci for their run during afternoon calibrations. More information on determning the camera focus is given in the User's Guide to Observing with Goodman. [7]

Goodman High Throughput Spectrograph

Startup/Shutdown Guide

This is a step-by-step guide for the Goodman HTS users on the regular procedure for starting up the spectrograph GUI and related programs each evening. It assumes that the CCD camera SI Image SGL software is running, and hence that the camera cryostat is at the appropriate vacuum (Pressure=0, T=-106.7 C for the Blue Camera and Pressure=0, T=-100 C for the Red Camera).

Starting up the Goodman GUI programs

(the procedure is the same for both the Blue and Red Cameras)

Click here for a PDF document containing information and screenshots on the GUI-related startup procedures. [67]

Starting the LabView Applications
1) Make sure that the transfer to soaric7 is working.

2) Open the "My Computer" icon on the Desktop and see if "ic7home3" on "SOAR Data Samba Server" is present.

3) If it is not open, click on the "My Network Places" icon on the Desktop and then click on the "ic7home3 on SOAR Data Samba Server" icon. The Instrument Scientist has the logon and password information.

4) Click the "Remote Transfer to soaric7" LabView shortcut on the Desktop and start the application by clicking on the light grey arrow in the upper left corner of the LabView window.

5) Make sure the Symmetricon GPS Real Time clock is running, and minimize it. It should be left running. This will be the time signal that will be recorder in the Goodman FITS image headers:    

6) Make sure the Tray Time Application is running. Tray Time is the little globe icon indicated in the screenshot below. Tray Time is used to automatically sync the computer's system time with the symmetricom gps time. Even with symmetricom running GSCS still only reads the system time so without Tray Time running we are not actually recording GPS times in the header. Once you double click Tray Time, you should see the little globe icon appear down in the taskbar on the bottom right of the screen.  
 

7) Open the Goodman controls by clicking on the "GSP_Main" LabView shortcut on the Desktop and start the application by clicking on the light grey arrow in the upper left corner of the LabView window.

8) Check the camera panel. If a green button is present for "Connection Open/Getting Data" in the upper left of the GUI, Goodman "sees" the SI Image camera control software and a TCP/IP connection is available to take data. You can confirm this by clicking on the "Obtain Camera Status" button. During a normal startup of the GSP Main GUI the Camera Temp will read "0". If the TCP/IP connection is operating, clicking on the "Obtain Camera Status" will show the latest temperature. If Goodman is cooled, the CCD Temp should be -106.5. If the CCD Temp does not update, you will need to check the SI Image SGL D window and make sure that a TCP/IP connection is open.

9) Click on Main tab and logon;

Use the account appropriate for your observing program (i.e., BRAZIL, CHILE, MSU, NOAO, OTHER, or UNC) with the password provided by your institution.
 

10) Click the User tab and go to "Home Systems" Select Home all (WARNING NOTE: Always make sure with the Telescope Operator that it is ok to home systems, e.g., that the telescope is at Rotator Angle=0, the instrument is at PA=0, and that the Goodman electronics have been powered on. If you see a red warning sign displayed in the Goodman VNC, STOP, do not proceed under any circumstance and contact the Telescope Operator before continuing with any task). 
Once you have clicked on Home all you should see the dark green lights change to yellow on the control panel as systems are being homed. This process will take several minutes; the Slit Mask stage will take the longest. Upon a successful homing of the systems, all lights should be bright green.  If there are any red lights, you will need to log out of GSP Main and shutdown and ask the Telescope Operator to cycle the power on the Goodman motor electronics.

11) After the camera is homed, start the flexure correction by clicking the flexure LED. It should change from dark green to bright green.

12) Select Gain and Readout Setting. These values are given in the table below. The default is 100kHz ATTN3, but as with the Port readout, it needs to be changed to another value before it is initialized correctly.

13) Select the imaging or spectroscopic mode in which you want to work.
Make sure that the "Save As" type is "I16 FITS".

14) Set up the grating and camera angles for your observations. The pre-defined modes are listed in the Goodman Overview page. [5]

These steps are illustrated and explained in more detail in the User's step-by-step Guide to Observing with Goodman [7]. [55]

Shutdown

At the end of the night, the observer and TelOps staff should do the following:

1. Logout of the Goodman GUI. This is found under the Main tab.
2. Shutdown the instrument motors. This is also found under the Main tab and will store all of the mechanisms in their home position.
3. Create a directory on soaric4 (Goodman Data Acquisition computer) in C:\Data for the night of your observations (YYYY-MM-DD). Move all FITS files to this directory. Do not move the DO_NOT_DELETE_FROM_THIS_DIRECTORY file.
4. Create a directory on soaric7 (Goodman Data Anaylsis computer) in /home3/observer/GOODMAN_DATA/<PROGRAM> /YYYY-MM-DD, where <PROGRAM> is one of [BRAZIL, CHILE, MSU, NOAO, OTHER, or UNC].
5. Move the FITS files from /home3/observer/today to /home3/observer/GOODMAN_DATA/<PROGRAM> /YYYY-MM-DD.

Click on this link for a PDF with screenshots and additional information on the End-of-Night shutdown procedure. [83]
 

• After the logout and shutdown are done, the power to the Goodman Electronics box should be turned off on the remote power control panel.

IC7 Shutdown and/or Rebooted:
If soaric7 is rebooted or shutdown, the postproc (PPROC) process to move data to the NOAO Science Data Archive (SDA) needs to be restarted.

1. To restart PPROC, open a vncviewer to soaric7.ctio.noao.edu:8 (the VNC password is the same as for SOI).
2. Open a terminal window.
3. Execute the command
4. ~/APPROOT/PPROC/exe/PPROC &
5. The PPROC command should now be restarted. One can take a test image and see if it appears in the list of "Last Processed Files".

The need for faster target acquisition for relatively bright targets (V≤18) in the Goodman High Throughput Spectrograph (HTS) led to the development at CTIO of a slit-viewing acquisition camera, hereafter GACAM (Tokovinin 2015: Goodman Acquisition Camera Instructions, July 14, 2015 [84] [85]). GACAM is located inside the spectrograph. Its deployable arm places a diagonal mirror between the slit and the collimator. The image is captured by a Prosilica GigE camera of 659x493 (Horizontal xVertical) pixel format, with a scale 0.165”/pixel and field of view of 1.82' x 1.36'. The software was developed by R. Cantarruti. GACAM was designed to be simple to use and unobtrusive to the spectrograph. An added advantage of the GACAM is that all settings in the Goodman GUI can now stay fixed. In particular, there is no need to switch from imaging to spectroscopic mode
(i.e., grating and camera stay at fixed position), change the Region of Interest (ROI), readout mode, nor any other option in the spectrograph GUI

NEW - September 11, 2017 - GACam is now running on its own computer, and the IP address has changed to 139.229.15.30:5

NEWER - September 15, 2017 - GACam is back to running on a shared computer, IP address 139.229.15.32:5 . This situation is temporary. All other aspects of operation are unchanged. 

GACAM User's Manual (PDF) [86]

GACAM Cheat Sheet (PDF) [87]

[87]

Information and Tutorials:

• [28]Goodman Cheat Sheet [8]
• The step-by-step User's Guide to Observing with Goodman (PDF presentation) [9]
• Goodman User Startup/Shutdown Guide [92]

Observing with Goodman (PDF guides):

• Connecting to the Goodman GUI [66]
• Starting up the Goodman GUI [67]
• The Goodman GUI layout [81]
• Setting up the binning [75]
• Setting up the Region-of-Interest (ROI) [82]
• How to take a spectrum [77]
• How to take a direct image [78]
• Shutting down the  spectrograph [83]
• Measuring radial velocities with the Goodman HTS [57]
• Optimizing the CCD read out [10]

​Goodman Acquisition Camera (GACAM) [27] [87]

• Goodman Acquisition Camera (GACAM) User's Manual [86]
• GACAM CheatSheet [87]

Multi-Object Spectroscopy (MOS) [93]

• MOS Observing Tutorial (PDF document) [91]
• MOS Slit Design Software Manual (PDF document) [89]
• MOS Alignment User Manual (PDF document) [90]

• Click here to download the Goodman mask designing software (tested on Windows 7 and 10, 64-bit installations) [88]. Now users have the option to design their MOS masks by login into a CTIO machine which is already running the mask design software. Please contact your Support Astronomer for details on VPN access, procedure and passwords.

The SOAR Instrument Support Boxes (ISBs) contain facility calibration units containing both continuum sources for flat fielding and line sources for wavelength calibration. 

The wavelength calibration lamps normally used with the Goodman spectrograph are: HgAr, CuHeAr, Ne, and Ar.  An Fe lamp is also available.
The comparison lamps can be activated from the instrument GUI by you, or you can ask the Telescope Operator (TO) to do it for you from his technical GUI.
Note that you need to make a slow, substantial mouse click on the particular lamp in order for it to actually get the input and turn on or off (a quick click may make the green light go on or off but not turn on/off the lamp). If in doubt, check with the TO. The Fe lamp is not featured in the GUI and you need to ask the TO to rutn it ON/OFF for you. When obtaining comparison lamps, make sure you are in Spectroscopic Mode and that the TO has put the pickup mirror in.

In Figure 1 at below we show the CuHeAr arc lamp spectra for all of our pre-defined spectroscopic modes. NOTE: the 300 l/mm grating has now been replaced by the 400 l/mm grating.

In Figure 2 below we show the HgAr arc lamp spectra for all of our pre-defined spectroscopic modes. NOTE: the 300 l/mm grating has now been replaced by the 400 l/mm grating.

In the following table containing plots of the comparison lamps made with various gratings and setups. This library of comparison lamp spectra will be expanded and updated to make it include most, if not all of the setups available with the instrument.
 

Useful links:

The KPNO Spectral Atlas Central [119] is a useful resource for comparison lamp spectra

Typical Comparison Exposure Times:
 

See how to perform a spectroscopic focus measurement [120].

See how to perform an imaging focus measurement [76].

The folowing values are approximate and can change up to 500 units from run to run.
We recomend that you perform a focus sequence at the start of your run or even every afternoon.

Red Camera spectroscopic focus values:

Blue Camera spectroscopic focus values:

M. Hamuy led a group at CTIO to obtain observations of 10 secondary spectrophotometric standards from Taylor (1984) [121] and 19 tertiary spectrophotometric standards from Stone & Baldwin (1983) [122] and Stone (1977) [123]. These results were published in two papers:(1) Hamuy et al. (1992) [124] and (2) Hamuy et al. (1994) [125]. The former paper covers wavelengths from 3300Å to 7550Å and the latter paper covers wavelengths from 6000Å to 10500Å. The latter paper also combines both sets of observations and presents AB magnitudes for the 10 secondary standards at 16Å intervals from 3300Å to ~10400Å and for the 19 tertiary standards at 50Å intervals from 3300Å to ~10300Å. The AB magnitudes are converted to flux (erg cm^-2 s^-1Å^-1) using the formula:

AB Mag = -2.5 alog10(Fν) - 48.59 where Fν is in erg cm^-2 s^-1 Hz^-1.

One of the latest and most complete lists of radial velocity standard stars is that by Soubiran et al. 2013, A&A, 552A, 64 (ADS link [164]):

"The catalogue of radial velocity standard stars for Gaia. I. Pre-launch release."

This catalog contains 1420 stars with data over a baseline of over 6 yr,  with an overall stability of about 300 m/s

The data in their Table 4, can be accessed in the CDS service by click on this link. [165]

The Goodman Data-Reduction Pipeline (DRP) is a Python-based package for producing science-ready, wavelength-calibrated, one-dmiensional (1-D) spectra. The pipeline is an ongoing work aimed to provide SOAR users with an easy to use, documented software for reducing images and spectra obtained with the Goodman High-Throughput Spectrograph. Though the current implementation assumes offline data reduction, our goal is to provide the capability to run it in real time, so 1-D wavelength calibrated spectra can be produced shortly after the shutter closes.

The pipeline is primarily intended to be run on a data reduction dedicated computer. Please, check the instructions at the Running on SOAR Server [167] for more details.

The Goodman DRP project is hosted on GitHub at it’s GitHub Repository [170]. Currently, the pipeline is separated into two main components. The initial processing is done by redccd, which trims the images, and carries out bias and flat corrections, and apply cosmic ray rejection.

The spectroscopic processing is done by redspec and carries out the following steps:

• Identifies multiple point-source targets (spectra of more than one object in the slit);
• Trace the spectra
• Extract the spectra
• Estimate and subtract background
• Find the wavelength solution
• Linearize data (resample)
• Write wavelength solution to FITS header
• Create a new file for the wavelength calibrated 1-D spectrum

Goodman DRP Team:

Simón Torres (SOAR Data Analyst - main code developer), César Briceño (SOAR Telescope Scisntist - team lead), Bruno Quint (Brazil Support Astronomer - code development adviser). Contact page. [173]

Notes and caveats

• In this first release, the pipeline performs the wavelength calibration only for spectroscopy data obtained with the 400 l/mm grating with the 400M1 and 400M2+GG455 (order-blocking filter) modes.
• The pipeline has been tested with long-slit spectra and point source objects. In its present form it will not work for multi-object spectroscopy nor extended sources.
• Because the pipeline deals first with the basic CCD reductions, in the separate module redccd, it also suited for reducing Goodman imaging data.
• Data obtained with different modes are grouped into different sets and processed separately
• Comparison lamps for wavelength calibration are used in the following order: proximity to the science target coordinates and acquisition time. If no comparison lamp was obtained during the night, the pipeline will look for lamp files obtained in the previous afternoon or in the next morning as long as they are in the same folder.

Backward Compatibility

The Goodman Spectrograph Control Software (GSGC) has gone through a considerable amount of updates and improvements. Some of them changed the way that the data is saved into the FITS files (image data region of interest and keywords added/removed). For future releases we are working on making the Goodman DRP compatible with legacy data, but in its current inception the software is designed for processing data obtained since March 2018.

Available Spectroscopic Modes

Because this is an ongoing work, some modes are not yet available for general use. The limitations are mostly due to the availability of wavelength solutions in the redspec module. The automatic solution for wavelength calibration relies on having spectra obtained with comparison lamps that are already calibrated in wavelength. Here is the table with the available modes: 

If your data was obtained with a non-supported mode, the pipeline will not perform the wavelength calibration, but will output the other files (like the extracted 1D spectra). Please, contact us [173] if your data is not supported. We will give higher priority to the most popular modes.

SOAR has a dedicated machine with the most recent version of the pipeline that can be accessed by observers. This machine can only be accessed via VNC (Virtual Network Computing) from within the observatory's network. The network can be reached using VPN (Virtual Private Network) or accessing any computer within the observatory. 

The credentials for the VPN connections must be provided by your support scientist. The same person who supported you during your observing night.

The information to access the SOAR VNC machine will be only provided by audio using Skype or similar. Please, contact us [173] to request the access information.

Once you have access to the VNC machine, you can open a terminal by clicking the proper icon. The terminal will open and the Python Virtual Environment for the pipeline will be activated. You will have to access the home folder of the SOAR partner institute that you are associated with, where you can create a folder for your appropriate observation date(s). Enter that folder and copy your data to it. Once done, run redccd to perform the CCD standard corrections (BIAS subtraction, Flat normalization, Cosmic Ray rejection). The reduced data will be stored in the <path-to-your-data>/RED folder.

If your data was obtained in imaging mode, you are done. If your data was obtained in spectroscopic mode, you may want to have the spectra extracted and wavelength calibrated. That is done using redspec. For now, only a few modes are completely supported (see About [172]). The non-supported modes will not have wavelength calibration. Go to the <path-to-your-data>/RED folder and run the redspec command.

Please, check the Goodman Data-Reduction Pipeline User Manual [174] or the Run the Pipeline [175] page for more details.

See Also

Before sending any question, make sure you reviewed all the links below.

• SOAR Remote Observer Guide [65]

The Goodman DRP can be downloaded and run on machines running Unix-like Operating Systems (OS) like Ubuntu or Centos. All you need is to have Python and some libraries commonly used in astronomy. The pipeline should run also on MacOS systems, but it has not been fully tested yet on this OS. We expect it may also run in the latest versions of the Windows OS, but we have not tested this.
Here is what you need to have installed to run the pipeline:

• python 3.5+ [176]
• numpy [177]
• scipy [178]
• matplotlib 2.1+ [179]
• astropy 3.0+ [171]
• pandas 0.22+ [180]
• ccdproc [181] v1.3+  [181] 

If you choose to install the Goodman DRP on your machine, we highly recommend the use of a Python Virtual Environment. That will prevent any installation, update or upgrade, wreaking havoc with the Python installed in your Operational System, which may render your machine un-bootable, and require a full OS re-install. If you really want to install the pipeline natively on your system, you should be prepared for the possible consequences. ;-)

Before you start installing all the packages, consider download and install Anaconda, a manager for Python Virtual Environments [182]. (We actually recommend Miniconda [183], since it is cleaner).

Please, refer to the Goodman Data-Reduction Pipeline - User Manual [174] for more details on creating the proper environment to install the package.

Download the Goodman DRP

The links to download last stable version of the Goodman DRP can be found below:

• Goodman Data-Reduction Pipeline v1.0b (zip)  [184]
• Goodman Data-Reduction Pipeline v1.0b (tar.gz) [185]

The latest releases of the pipeline can be found at the SOAR Telescope GitHub Repository [186]. Please, download a stable version instead of cloning the whole repository. The Goodman DRP is an ongoing work and several changes are made every day. If you clone the repository, you might end up having inconsistencies between different times that you run it. 

Installing the Goodman DRP

If you are using Anaconda, you can simply follow the instructions below. If you already have created an environment, you can skip the step 3. 

1. Create a folder in your system, move the downloaded compressed files and decompress them.

$ mkdir <my_new_folder>
$ cd <my_new_folder>
$ mv <path_to_the_decompressed_files> ./

2. Decompress them.

$ tar xf goodman-v<version>.tar.gz

or

$ unzip goodman-v<version>.zip

then enter to the decompressed folder:

$ cd goodman-v<version>/

3. Use Conda to create a new environment using a pre-set environment that comes within the compressed files within the file "environment.yml":

$ conda env create -f environment.yml

4. Activate the environment now (and every time you want to use the pipeline):

$ source activate <virtual_environment_name>

If you created the environment using the file "environment.yml", the <virtual_environment_name> is "goodman".

5. Test if your installation will be successful:

$ python setup.py test

6. If no errors come up, install the pipeline:

$ python setup.py install

Now you are ready to Run the Pipeline [175].

If you have questions, requests, suggestions or want to get in touch with our team for any reason, please, write to the following e-mail

goodman-pipeline at ctio dot noao dot edu

and we will try to answer as possible.

The Goodman DRP Team: Simón Torres (SOAR Data Analyst - main code developer), César Briceño (SOAR Telescope Scisntist - team lead), Bruno Quint (Brazil Support Astronomer - code development adviser)

(Updated: Aug 29, 2017; C. Briceño)
ON-SITE STAFF IS NECESSARY TO PROCEED WITH A GOODMAN COLD START UP.

PDF version of this document [194]

1. Make sure that all of the lens covers are off.

2. Make sure that the Goodman Camera Electronics are on. This can be checked from the ECS VNC Viewer and Remote Power sub-panel. If the camera electronics are not on, turn them on. If this is successful, you should hear three rapid beeps over the dome microphone  You should also see the Remote Power sub-panel indicator for the camera electronics switch from "off" to "on".

3. Go to Room 109 and log the balance pressure of the CryoTiger. It should be at about 190 psi if the cooling has been turned off. The balance pressure should be around 0 psi if the cooling is on. Log this number and the date on the sheet provided.

4. Power up soaric2 (139.229.15.132).

  If this does not work, somebody will have to go up to the Nasmyth and manually cycle the power on soaric2 in the electronics box.

5. Log on to soaric2 using the vncviewer from some other computer. The linux example is:   vncviewer 139.229.15.132 -Shared &    (the password can be obtained from the TelOps staff: soaropsATctioDOTnoaoDOTedu, or the Instrument Scientist: spointsATctioDOTnoaoDOTedu).

Soaric2 should boot directly into the Desktop, there is only one user.

6. Starting SI Image SGL D:

Start the SI Image SGL II software by double-clicking on the appropriate icon in the Windows desktop of Soaric2. You will immediately be prompted with the pop-up “Do you want to open a camera now?”. Select “OK”. After a few seconds, the Blue Camera should appear as “Camera: 620-658”. Choose “Select Camera”. If “Camera 620-658” cannot be found, return to step 1 and verify the camera is on. If it is, and the camera cannot be found, contact the Instrument Scientist.

7.

Check that the Cooler is ON as indicated in the image below. If it is OFF, Click OK and open the Camera Status Panel. The pressure should be 0 or ~<0.001 Torr  (~< 10^-3 Torr or 1 mTorr), see image below.  If not, the Goodman cryostat (camera) needs pumping, which is done by the SOAR day crew, and usually requires a full day or so. WARNING: DO NOT START COOLING THE CAMERA IF THE VACUUM HAS NOT BEEN REACHED.

8.Click the “Open Settings File” button and select “Goodman_blue_new.SET” to load in the Blue Camera Set file.

 9.  Disable the “Auto Calc Postscan” by clicking on the button. Once disabled, the arrow within the button should be greyed out and not illuminated as shown below. Click “OK” in the top right corner of the panel to load in the changes.

10. From the SI Image front panel, open the Camera Status window to display the current CCD Temperature and Pressure. The operating Temperature and Pressure of the Blue Camera are -106.5 C and 0.000 Torr. Log the Temperature and Pressure

11. If the Chamber pressure is above 1.000 Torr, the camera head will need pumping which can only be done by the SOAR day crew. Do not proceed to step 12 until the chamber pressure is below 1.000 Torr.

12. Under the “Operate” Menu , enable the TCP/IP server so that it shows up as a yellow box with the status “Waiting”. Also under the “Operate” Menu open the “Configure” panel. Check that the “Min. Acquisition Time Out” is set to 30 seconds as shown below. Check that Image Transform 1 is set to “Flip Y”. Save the settings. Finally, change the acquisition mode in the top right corner of SI Image from “Light” to “Triggered”.

13. Minimize the SI Image SGL GUI. DO NOT CLICK ON THE RED "X" BUTTON since this will exit the GUI.  SI Image SGL II is now configured and should continue to run in the background.

14. Check the SAMBA server connection between soaric2 and soaric7: Open Computer on the Desktop. Under “Network Locations” you should find the three soarci7 folders cross-mounted. If the network drives show Red X’s, click on each drive on the left panel the window to ensure connection until they are all green.

15. Start the automatic file transfer program:  click on the "Transfer_To_ic7"  icon in the soaric2 desktop:  
 

16. Check whether the files from the latest observation night were transfered to soaric7. If they are still in soaric2 you should see them in the c:\DATA folder. If so, run the End-of-Night-Transfer DOS program on soaric2:

17. Start the Symmetricon GPS Real Time clock and Tray Time program. Symmetricom should be minimized and left running. The Tray Time program will run in the background and appear as a small globe in the tray in the bottom right of the desktop. These programs will ensure the GPS time signal will be recorded in the Goodman FITS image headers.

18. Double check with the Telescope Operator or day crew that:

a) The vacuum lines have been removed from Goodman (if pumping the instrument took place)
b) Instrument covers have been replaced (if applicable)
c) The Nazmyth rotator angle is ok and that nobody is working inside the instrument.  After these checks, ask the Telescope Operator to turn on the Goodman electronics, and start the Goodman GUI:

19. Log on to soaric7 using the vncviewer that is appropriate for your program. The linux example is:  vncviewer 139.229.15.137:<n> -Shared &  .The display number <n> and password can be obtained from the TelOps staff (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctioDOTnoaoDOTedu).

20. Check the disk space on soaric2 by double-clicking on the "My Computer" icon. Highlight "Local Disk (C:)". Right-click and select "Properties". If the disk is almost full, please contact TelOps (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctio.DOTnoaoDOTedu) so they can delete older data.

21. Check the disk space on soaric7 by issuing the command "df -h" from a terminal prompt. If the /home3/observer disk is close to full, contact TelOps staff (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctioDOTnoaoDOTedu).

(Updated: Aug 29, 2017; C. Briceño)
ON-SITE STAFF IS NECESSARY TO PROCEED WITH A GOODMAN COLD START UP.

PDF version of this document [195]

1. Go to Room 109 and verify that the Service Cabinet is powered on. The LCD display should read “Power On”. If the LCD display does not read “Power On”, open the cabinet door and verify that the switch is in the on position.

2. Once the power is on, log the pressure values on the Supply and Return lines. If cooling is not turned on (default state after complete power loss but not after computer loss), the pressures should be equal. If cooling is already enabled, typical operating pressures are approximately between 240-280 PSI for the Supply line and 30-50 PSI for the Return line.

3. Power up soaric6 (139.229.15.136). If this does not work, somebody will have to go up to the Nasmyth and manually cycle the power on soaric6 in the electronics box.

4. Log on to soaric6 using the vncviewer from some other computer. The linux example is : vncviewer 139.229.15.136 –Shared & (the password can be obtained from the TelOps staff: soaropsATctioDOTnoaoDOTedu, or the Instrument Scientist: spointsATctioDOTnoaoDOTedu).
Soaric6 should boot directly into the Desktop, there is only one user.

5. Starting SI Image SGL II: Start the SI Image SGL II software by double-clicking on the appropriate icon in the Windows desktop of soaric6. You will immediately be prompted with the pop-up “Do you want to open a camera now?”. Select “OK”. After a few seconds, the Red Camera should appear as “Camera: 1110-111”. Choose “Select Camera”. If “Camera 1110-111” cannot be found, return to step 1 and verify the camera is on. If it is, and the camera cannot be found, contact the Instrument Scientist.

6. Check that the Cooler is ON as indicated in the image below. If it is OFF, click the OFF button to turn cooling ON. DO NOT TURN ON COOLING IF THE CHAMBER PRESSURE IS ABOVE 1.000 Torr. If the camera has been allowed to warm up to ambient temperature it will take between 4-6 hours to reach operating temperature and pressure. During the initial cooling phase, significant condensation can form on the cryo-lines. Be sure the Nasmyth rotator angle is positioned at 90 degrees to avoid condensation dripping onto the camera head.

7. Click the “Open Settings File” button and select “GOODMAN_RED.SET” to load in the Red Camera Set file.

8. Disable the “Auto Calc Postscan” by clicking on the button. Once disabled, the arrow within the button should be greyed out and not illuminated as shown below. Click “OK” in the top right corner of the panel to load in the changes.

9. From the SI Image front panel, open the Camera Status window to display the current CCD Temperature and Pressure. The operating Temperature and Pressure of the Red Camera are -100.0 C and 0.000 Torr. The pressure sensor is known to bounce between 0.000 Torr and 0.050 Torr on minute timescales so refresh as needed. Log the Temperature and Pressure.

10. If the Chamber pressure is above 1.000 Torr, the camera head will need pumping which can only be done by the SOAR day crew. Do not proceed to step 9 until the chamber pressure is below 1.000 Torr.

11. Close the Camera Status panel and open the Camera Settings panel.

12. Under the “Operate” Menu , enable the TCP/IP server so that it shows up as a yellow box with the status “Waiting”. Also under the “Operate” Menu open the “Configure” panel. Check that the “Min. Acquisition Time Out” is set to 30 seconds as shown below. Save the settings.

13. Minimize the SI Image SGL GUI. DO NOT CLICK ON THE RED “X” Button since this will exit the GUI. SI Image SGL II is now configured and should continue to be run in the background.

14. Check the SAMBA server connection between soaric6 and soaric7: Open Computer on the Desktop. Under “Network Locations” you should find the three soarci7 folders cross-mounted. If the network drives show Red X’s, click on each drive on the left panel the window to ensure connection until they are all green.

15.  Start the automatic file transfer program: click on the “Transfer_To_ic7” icon on the soaric6 desktop.

16. Check whether the files from the latest observation night were transferred to soaric7. If they are still in soaric6 you should see them in the C:\DATA folder. If so, run the End-of-Night-Transfer DOS program on soaric6.

17. Start the Symmetricom GPS Real Time clock and Tray Time program. Symmetricom should be minimized and left running. The Tray Time program will run in the background and appear as a small globe in the tray in the bottom right of the desktop. These programs will ensure the GPS time signal will be recorded in the Goodman FITS image headers.

18. Double check with the Telescope Operator or day crew that nobody is working inside the instrument and the Nasmyth rotator angle is ok. After these checks, ask the Telescope Operator to turn on the Goodman electronics, and start the Goodman GUI.

19. Log on to soaric7 using the vncviewer that is appropriate for your program. The linux example is: vncviewer 139.229.15.137:<n> -Shared & .The display number <n> and password can be obtained from the TelOps staff (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctioDOTnoaoDOTedu).

20. Check the disk space on soaric6 by double-clicking on the "My Computer" icon. Highlight "Local Disk (C:)". Right-click and select "Properties". If the disk is almost full, please contact TelOps (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctio.DOTnoaoDOTedu) so they can delete older data.
21. Check the disk space on soaric7 by issuing the command "df -h" from a terminal prompt. If the /home3/observer disk is close to full, contact TelOps staff (soaropsATctioDOTnoaoDOTedu) or the Instrument Scientist (spointsATctioDOTnoaoDOTedu).

Updated Feb 10, 2016. C. Briceño

This page is intended to provide guidance on various error messages and problems that may be encountered when working with Goodman. It is aimed mostly for the Goodman support staff. Please note that by its very nature, this page is constantly under construction and will be updated as new issues arise, procedures change or updates in the instrument hardware/software take place.

1) Goodman GUI works fine, images are created in C:\DATA in soaric4, but are not transfered to /home3/observer/today/. [196]

2) The End-of-Night transfer program does not create the appropriate directory in soaric7:/home3/observer/GOODMAN_DATA/<institution>/  were <institution> is one of BRAZIL, CHILE, MSU, NOAO, OTHER or UNC, and transfer files: [197]

3) VNC to soaric7: suddenly the up/down left/right arrow keys in the keyboard stop working correctly -> e.g., up/down arrows change to anoher desktop workspace instead of scrolling up/down in the IRAF command window, or left/right change to another desktop workspace instead of allowing one to move the cursor on the ds9 window.
Solution: type either one of the Alt, CRTL or Shift keys in your keyboard.

4) RED light on the Goodman Camera/Grating LED
Solution: Shutdown and exit the Goodman GUI, power cycle the Goodman electronics, and restart GUI.
Procedure:  4.1) Telescope Operator should set the optical ISB to Rotator Angle=0 and instrument to PA=0.
                   4.2)  In the Goodman GUI click in the User menu and select Shutdown
                   4.3)  Go to File menu and click Exit to completely exit the application.
                   4.4)  Telescope Operator should TURN OFF the Goodman Electronics
                   4.5) After some 15 sec Telescope Operator can TURN ON again the Goodman Electronics
                   4.6) Restart the Goodman GUI  (see the Goodman Startup Guide [92])
                   4.7) Restart the "Transfer to soaric7" LabView application.   Resume observing.

5) GACAM fails to update the instrument position angle (IPA) in the GACAM GUI "Offsets" sub-window.
    GACAM communicates with the TCS through sockets that are opened only when the "Calculate" button is clicked, hence when communication problems like this one arise, the culprit is likely on the server side. 
Solution: The Telescope Operator should reboot the TCSAPP  application (TCS kernel machine: 132.229.15.2)

This page contains documents on technical issues related to the Cryo-Tiger closed circuit cooling system.

1. Pérdida de funcionamiento de un sistema Cryotiger por bloqueo de orificio en el 'cold head', y cómo purgar el sistema. [198]