| GOODMAN NEWS - Feb 2019: During the recent Feb 19, 2019 the round GG-385 order-sorting filter broke beyond repair. While we obtain a replacement, we have available a 4x4 inch GG-395 on loan from the COSMOS instrument [4] on the CTIO 4m Blanco telescope. Users interested in this filter should request it specifically in the Instrument Setup form. |
The Goodman High Throughput Spectrograph (GTHS) was built in the Goodman
Laboratory at the University of North Carolina [5]under the leadership of Prof. J. Christopher Clemens. It is an imaging spectrograph, capable of producing excellent image quality across a 7.2 arcmin diameter FOV (with a 0.15 arcsec/pixel scale), and spectra at various resolutions from the atmospheric UV cutoff all the way out to 850nm. It employs all transmissive optics, and Volume Phase Holographic (VPH) Gratings to achieve the highest possible throughput for low resolution spectroscopy over the 320-850 nm wavelength range. The paper describing the instrument is Clemens et al. (2004) [6]
Observing with Goodman
Data Reduction and Publishing Results
Also, be aware of SOAR limits, overheads and efficiency [24].
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 [25] 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 [18] (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 [26]
We have obtained observations of standard stars in order to determine the system throughput with the Red Camera. Results will be posted soon.
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 [25] 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 [20] 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.
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.
New 600 and 1200 l/mm gratings were delivered to SOAR in April 2017. Based on tests at the telescope, we are offering the new gratings, with recommendations as follows:
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 [29], or by email to the Support Astronomer with copy (cc) to soarops@ctio.noao.edu [30], so our Observer Support staff also receives the request.
Note: the Goodman Acquisition Camera (GACAM) [31] 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 [12]).
[32]
At least read this!
Optics:
The Goodman optics are designed to transmit down to the atmospheric cutoff at 320 nm, and include lenses made of CaF2 and of NaCl. The latter are the center elements of fluid-coupled triplets. None of the multiplets are over 4" in diameter which reduced the difficulty compared to spectrographs with larger pupil sizes. Each of the multiplets is sealed on one end with a face-mounted o-ring that imposes a known axial load, and on the other end with a rim-mounted o-ring that imposes a radial load, and finally held captive axially with a retaining ring that incorporates a third o-ring. This last o-ring does not participate in the sealing of fluid, but avoids a metal glass interface that would be undesirable for the CaF2 lenses. The salt lenses are held by the other optics and are never in contact with a seal.
Filters:
There are two independent filter wheels: One holds 4 x 4 inch square filters, and can be fit with 4 filters. The second wheel holds 4 inch diameter filters, and normally holds the 5 order-sorting filters.
The full list of available filters can be accessed in the SOAR filter list page. [21]
The filters are in the collimated beam (tilted to avoid ghosts). Installing different filters is straight forward, but is a day-time operation. Special arrangements for fillter installations should be consulted with the Instrument Scientist well in advance of the observing run.
Imaging Mode
In imaging mode the plate scale is 0.15 arcsec/pixel and the field of view is 7.2 arcmin in diameter (3096 x 3096 unbinned pixels). Filters available include Bessell UBVRI, SDSS ugriz, and VR. See the SOAR filter list [21]for other filters
Spectroscopic Mode
In Spectroscopic mode the Goodman Spectrograph can obtain both single, longslit spectra and spectra of multiple objects simultaneously over a field of 3.0 x 5.0 arcminutes using multi-slit masks. A carousel style mask changer, holding up to 36 masks allows the slit plates to be interchanged and located at the instrument entrance aperture.
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 changes are done during the night.
Goodman has now different Blue and Red-optimized options for the 1200 l/mm grating. Please check the updated list of currently available gratings in the Goodman Spectrograph Gratings page. [22]
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. Because of limits in the camera rotation stage, it is not possible to use the 2100 and 2400 l/mm gratings beyond certain wavelength limits.
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.
Calibration Lamps:
We have a quartz lamp for spectral flats and HgAr, Ne, Ar, and CuHeAr lamps for wavelength calibration. Plots of these spectra with the lines identified in each of our standard spectroscopic modes can be found in the Goodman Comparison lamp web page. [35]
With the 400, 600 and 930 line gratings we recommend also taking Dome Flats during your afternoon calibrations.
Choice of Detectors
If science program requires:
[18]
[19]
Most programs requiring wavelengths redward of ~4500 A will benefit from the enhanced red throughput and minimum fringing provided by the red camera.
Use of blocking filters:
Those taking spectra to the red of ~600nm should be aware that, depending on the spectrum of their target, there may be significant contamination from second order blue light superposed on the first order red spectrum (a blue leak). The blue leak will change the apparent shape of the red continuum, "fill in absorption features in the red, and may "imprint" emission or absorption features occurring in the blue spectrum at roughly twice their wavelength. This second order contamination can be eliminated by use of an appropriate blocking filter. However, this does entail a loss of efficiency in the red since the "in-band" transmission of the available blocking filters is not 100%.
Those needing spectrophotometric calibration should note that essentially all spectrophotometric standards are quite blue, so there will be a significant blue leak if they are measured without a blocking filter, which will invalidate the calibration of science target spectra, even if the targets themselves have no blue flux. A possible approach would be to measure the science targets without a blocking filter, the standards with one, and then correct the standards for the blocking filter transmission. However, we currently do not have measurements of the blocking filter transmission which we consider sufficiently reliable for these purposes. In the meantime observers who plan to do this should measure there own by observing a red star with and without blocking filter.
In principle contamination by the blue leak will also effect arc lamp calibrations (superposing blue lines on the red spectrum at roughly twice their wavelength) and flat fields. However, with the exception of the HgAr lamp the blue lines in all the calibration sources are very weak compared to the red lines, and similarly the flat field sources are much brighter in the red than the blue.
Scattered (and Stray) Light:
Measured to be small in imaging mode by comparing imaging FOV and surroundings with a bright star illuminating the pupil. Some scattered and stray light is seen in the Goodman spectroscopic mode. We currently see 0.06e/s of stray and/or scattered light in the spectroscopic mode with 1x1 pixel binning and the 100kHz ATTN2 readout. Efforts are underway to replace the tent that covers Goodman with a light-tight box. We are also looking for low-level emitting LEDs on all of the Goodman motors and covering them with metallic tape as we find them.
Calibration Issues:
Obtaining good quartz spectra over the entire wavelength range with the 400 l/mm grating is difficult because of the different spectral response at the red and blue ends. The most noticeable effect is that to obtain sufficient counts in the blue end, the red end becomes saturated. A blocking filter is on order so that composite quartz flats can be made. This effect is not as great with the other gratings because the wavelength range isn't as large.
There also exists contamination of the flats by scattering from the back of the second filter wheel. Use of the blocking filter mentioned above mitigates this contamination. Finally, with the BLUE CAMERA fringing appears in the spectra to the red of the Hα line. With the availability of the RED CAMERA, fringing at red wavelengths is greatly reduced, as can be seen in this plot below.
Flexure:
The instrument has active flexure compensation based on the Nasmyth rotator angle. The corrections are succesful at the fraction of a pixel level for the full range of rotator angles.
Goodman High Throughput Spectrograph
User Manual
Updated Mar 2017
C. Briceño/S. Points
Contents
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 [25] 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 [8] 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. [21] 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 [8] 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 [8] 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.
A Beginner's Guide to Using IRAF [63] (IRAF Version 2.10), Jeannette Barnes, August 1993
A User's Guide to CCD Reductions with IRAF [64], Philip Massey, February 1997
A User's Guide to Reducing Slit Spectra with IRAF [65], Phil Massey, Frank Valdes, Jeannette Barnes, April 1992
Guide to the Slit Spectra Reduction Task DOSLIT [66], 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. [67]
Both the Blue [18] and Red [19] cameras are installed on an articulated stage, which is moved by a wormdriven annular stage directly encoded with a resolution of 0.6 μ-radians. To minimize flexure the camera platform rides on a concentric 400mm curved bearing rail. The platform that holds the camera optics and dewar is attached at two points to the central stage and at two points to the bearings on the curved rail. The coupling between the bearing assembly and the camera platform is through tuned flexures that both relieve the overconstraint between the central bearing and the rail, and act as a restoring spring for two piezo-electric actuators that can move the whole platform up and down to compensate for instrument flexures. These flexures are pre-loaded with 100kg of tension, which is more than twice the total weight of the camera assemblies, to insure that the bearings on the curved rail remain on the same contact surface (the underside of the rail) during rotation of the instrument. Flexure compensation on the orthogonal axis uses the articulation motion at very low speed.
The camera optics tube rides on lead-screwdriven crossed roller bearing stages. The camera stage is a custom low profile design that had to be incorporated into the articulation assembly. The camera focus stage incorporates external temperature sensors, constructed from temperature-to-voltage converters that feed built-in analog-to-digital converters in the Silvermax motors driving the stage. The optics mounts do not include passive thermal compensation, so measurements are required to correct for focus changes with temperature.
The clear aperture at the front of the camera is 4” and it is 2.8” at the last optic, which doubles as a dewar window. The shutter adds only ¼” to the width of the camera optics (except for a strategically positioned motor), and adds only 1” in length to the front of the camera. It consists of a friction driven curved stainless plate 0.010” thick that rides in a curved teflon track to cover the 4” entrance to the camera optics. The stepper motor can open or close the shutter in under 200 msec.
We have available VPH gratings of 400, 600, 930, 1200, 1800, 2100 and 2400 l/mm, that have been produced in a holographic exposure facility at UNC that is currently capable of making 4” size VPH gratings. These gratings are of quality equal to or exceeding those produced by most vendors.
The Grating Rotation and Translation Stages
The grating changer can position any of three gratings at the 75 mm pupil, or lower them out of the way for imaging mode. This translation is subordinate to the grating rotation, so that the grating can be inserted and removed quickly from the pupil without resetting the angle. The rotation is driven by a Newport rotary stage at the bottom and a matching bearing at the top. This stage was retrofitted with a Silvermax motor. The stage is directly encoded with a resolution of 0.9 μ-radians, and the Silvermax motor uses feedback from this encoder for fine position control. Gratings are mounted in frames that are held by ball detents in the translation mechanism.
The Goodman spectrograph uses two filters wheels.
The first filter wheel is used mostly for imaging. It can hold up to 4 holds 4x4 inch square filters. The SOAR filter page [21] shows the list of available filters.
The second filter wheel has 6 positions for 4-inch diameter circular filters. It normally holds the 5 spectroscopic order sorting filters, and an open position.
Filters are placed in the collimated beam where they cause a pupil shift instead of a more irritating refocus, but this made them large, to accommodate the 75 mm pupil, and difficult to place. The wheels are suspended from a plate mounted to a cantilevered extension to the truss. The wheels are tilted enough to place any reflection ghosts the filters generate outside of the imaging field. Filters are mounted in rings that are held in the wheels using spring loaded ball detents. This allows exchange of filters without tools or fasteners that get lost or dropped in the instrument. Likewise, the wheels are held on their bearings by a hub that can be removed by hand. The wheels have teeth around their perimeter and are driven by smaller gears engaged by a spring loaded mechanism.
The Goodman Spectrograph collimator has a set position at this time and cannot be moved. The collimator focus value is 1000.
Goodman slit masks are 3x5 arcmin on the sky. Single longslits are available in widths ranging from 0.46 to 10 arcsec. They are all roughly 3.9 arcmin long. See the Goodman longslit page for more details. [68] Slit masks are installed on a 36 position carrousel.
Multiobject slit masks are also 3x5 arcmin on the sky. At present the mask carrousel can hold 17 MOS masks at one time, the remaining 19 positions are used by longslits, image slicers, and a few non-operative slots. Changing MOS masks is a daytime operation.
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 [69]), 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). [70] 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:
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.
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.
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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. [71]
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.
If the data acquisition GUI needs to be stopped:
A more detailed explanation of the Startup and Shutdown procedures can be found in the Goodman step-by-step User's Observing Guide (PDF). [12]
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/
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.
Figure 8: Selecting the CCD binning and image size.
Figure 9: Selecting the Goodman readout parameters.
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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.
All of these features will be discussed in more detail in the Observing with Goodman [72] section of this manual.
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.
In this section the users will find the procedures and recommendations to carry out a successful observing night with Goodman. We strongly recommend that after going through this web page, you download and study the Step-by-step User's Guide to Observing with Goodman.
Prior to your run at SOAR with the Goodman Spectrograph, you should have completed the Instrument Setup Form [29]. When using Goodman, it is important to send in this form well ahead of time so that any specific needs can be addressed before your run. In the instrument setup form you can also specify what binning you will use during your run. The default readout is for 1x1 binning with the 100kHz ATTN3 readout. Information on the gain settings and readout noise for various readout options can be found in the Goodman Overview [8].
In addition to filling out the Instrument Setup Form [29], visiting observers should read the SOAR Visiting Astronomer's [73] webpage for general information about traveling to and within Chile. Furthermore, visiting investigators should fill out the Travel Information Questionaire [74] so that your transportation and lodgings can be arranged.
Observing logs for your run can be downloaded here [75].
Setting Up for the Start of Your Night/Run
Before you begin observing with Goodman, you should first make sure that the data acquisition GUI and the data analysis GUI are running as shown here in Figure 1.
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Figure 1: The Goodman Data Acquisition and Data Analysis GUI windows.
If these GUIs are not running, please refer to the sections about Starting and Stopping the Data Acquisition GUI [76] and Starting and Stopping the Data Analysis GUI [77] in the Software [50] section of the Goodman Manual. [9] If you have problems with starting either of these, please contact the Telescope Operators or the Goodman instrument scientist (Sean Points). They will be able to help you with this task.
After the GUIs are running, you should check that:
You are now ready to use the Goodman Spectrograph.
Daytime Calibration Data
Performing a focus:
Figure 2: Selecting the CCD geometry (i.e., 1x1 imaging, 2x2 imaging, etc.)
Figure 3: Selecting the CCD geometry (user-defined ROI)
Figure 4: Selecting the CCD readout speed. Please see the Overview section of this manual for the gains (e/ADU), read noise (e), and readout times for 1x1 spectroscopic binning.
Figure 5: Selecting the slit mask to be used.
Figure 6: Selecting the order-sorting filter (secondary filter), if any, to be used.
Figure 7: Selecting the grating.
Figure 8: Selecting the camera and wavelength angles.
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Figure 9: Taking an arc lamp spectrum.
Figure 10: Changing the camera focus.
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Figure 11: Determining the best camera focus value with the specfocus task within IRAF.
Taking Bias Frames
Select the "Zero" tab in the Acquisition and Exposure Status region of the GUI. Make sure that the CCD binning and readout parameters are set to the values that you will use for your science observations. Select how many bias frames you want to take. You will want to take bias frames for as many different observing modes you plan on using during the night. That is to say, if you plan on observing during the night in 1x1 spectroscopic mode with the 300 l/mm grating 100kHz ATTN3 readout and the the 600 l/mm grating (mid) 200kHz ATTN2 readout, you should take bias frames for both the 1x1 spectroscopic 100kHz ATTN3 and 200kHz ATTN2 readouts.
Taking Comparison Lamp Spectra
Select the "Comp" tab in the Acquisition and Exposure Status region of the GUI. Select the CCD binning and readout parameters to the values that you will use for the night. We advise that observers take a set of comparison lamp spectra using the 0.45" slit mask as well as the slit mask they will be using during the night. This may help the observer in deblending any lines when using the wider slit masks. We also note that it can be difficult to obtain a sufficient number of lines to determine an accurate wavelength solution in the blue preset modes using the HgAr lamp. Therefore, we also recommend taking some spectra of the CuHeAr lamp.
Taking Quartz Flats
Select the "Flat" tab in the Acquisition and Exposure Status region of the GUI. Select the CCD binning and readout parameters to the values that you will use for the night. Take the quartz flats you need for all of the observing modes you will use during the night.
Nighttime Observing
1) Slew to target
2) Move to "image mask" mode
3) Withdraw slit
4) Take image of field and note x,y coordinates of object in current position field (in "Current Pixel Values")
5) Move slit back into place
6) Take image of slit and note x,y coordinates of slit center in desired position field (in "Desired Pixel Values")
7) Make offset ("Calulate Required Offset" -> "Apply SOAR Offset")
8) Take image of object on slit. Is it centered? If not, perform another offset with slit in place.
9) Repeat 8 as needed
10) Change readout speed and move grating and camera into spectroscopic mode
11) Take spectrum
12) For faster target acquisition for relatively bright targets (V≤18), the GACAM [31] may be used.
Click here for additional information and tips on how to get your target spectrum [81].
Click here for tips and advice on how to take direct images with Goodman. [82]
At the end of your observing night, please fill out the End-of-Night [83] report for the telescope. Please make note of any problems that were encountered during the night so that they may be resolved before the next night's observing.
Also, at the end of your night observing with Goodman, you may want to transfer your data back to your home institution. To do so, open a local Terminal in your home institution, and scp the data from soaric7.
After your run is complete, please fill out the End-of-Run [84] report.
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).
(the procedure is the same for both the Blue and Red Cameras)
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. [8]
These steps are illustrated and explained in more detail in the User's step-by-step Guide to Observing with Goodman [10]. [59]
At the end of the night, the observer and TelOps staff should do the following:
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.
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 [88]
[89]). 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 - August 3, 2018 - GACam is now running on its own computer, and the IP address has changed to 139.229.15.168:1. All other aspects of operation are unchanged.
GACAM User's Manual (PDF) [90]
[91]
Goodman Multi-Object Spectroscopy (MOS) mode brings multiplex capability over a field of view of 3' x 5'.
Custom MOS masks are designed with a Mask Designing software, developed at UNC.
Goodman carrousel has 16 available positions for MOS masks.
Installing MOS masks is a daytime task, like changing filters, and should be requested beforehand in the Instrument Setup Form [29], or by email to the Support Astronomer with copy (cc) to soarops@ctio.noao.edu [30], so our Observer Support staff also receives the request.
Click here to download the Goodman Mask Designing software (tested on Windows 7 and 10, 64-bit installations) [92].
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.
See the PDF tutorials:
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.
| Grating | Setup | Lamp | Wavelength Coverage of the Plot |
|---|---|---|---|
| 400 | M1 | HgAr | 3000-7000 (Full range) [100] |
| 400 | M1 | HgAr | 3000-5000 (Zoom) [101] |
| 400 | M1 | HgAr | 5000-7000 (Zoom) [102] |
| 400 | M2 | HgAr | 5000-9000 (Full range) [103] |
| 400 | M2 | HgAr | 5000-9000 (Zoomed/split) [104] |
| 600 | UV,Blue,Mid,Red | HgAr | 3600-9000 (6 plots) [105] |
| 600 | UV,Blue,Mid | CuHeAr | 3600-6500 [106] |
| 930 | M1 | HgAr | 3000-4500 (Full range & zoom) [107] |
| 930 | M2 | HgAr | 3750-5500 (Full range & zoom) [108] |
| 930 | M3 | HgAr | 4750-6250 (Full range & zoom) [109] |
| 930 | M4 | HgAr | 5500-7200 (Full range & zoom) [110] |
| 930 | M5 | HgAr | 6400-8000 (Full range & zoom) [111] |
| 930 | M6 | HgAr | 7250-8750 (Full range & zoom) [112] |
| 930 | M2 | CuHeAr | 3750-5500 (Full range & zoom) [113] |
| 930 | M3 | CuHeAr | 4750-6250 (Full range & zoom) [114] |
| 930 | M4 | CuHeAr | 5500-7200 [115] |
| 930 | M5 | CuHeAr | 6400-8000 [116] |
| 930 | M6 | CuHeAr | 7250-8750 [117] |
| 1200 | M5 | HgArNe | 3600-8700 (7 plots) [118] |
| 1200 | M1,M2,M3,M4,M5,M6,M7 | CuHeAr | 3600-8700 (7 plots) [119] |
| 2100 | 650nm (Littrow) | Ne | 6150-6720 [120] |
Useful links:
The KPNO Spectral Atlas Central [121] is a useful resource for comparison lamp spectra
Typical Comparison Exposure Times:
| Grating | Mode | Slit | Lamp (%) / Exp (s) |
|---|---|---|---|
| 400 | M1 | ||
| 400 (+GG455) | M2 | ||
| 600 | UV | ||
| 600 | Blue | ||
| 600 (+GG-385) | Mid | ||
| 600 (+GG-495) | Red | ||
See how to perform a spectroscopic focus measurement [122].
See how to perform an imaging focus measurement [80].
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.
| Grating | Mode | Camera Temp (C) |
Focus |
|---|---|---|---|
| 400 | M1 | 16 | -600 |
| 400 (+GG455) | M2 | 16 | -1200 |
| 600 | UV | 18 | -400 |
| 600 | Blue | 18 | -300 |
| 600 (+GG385) | Mid | 18 | -1100 |
| 600 (+GG495) | Red | 18 | -400 |
| 1200 | M2 | 17 | -700 |
| Grating | Mode | Camera Temp (C) |
Focus |
|---|---|---|---|
| 400 | M1 | ||
| 400 (+GG455) | M2 | ||
| 600 | UV | 17 | 1650 |
| 600 | Blue | 17 | 1650 |
| 600 (+GG385) | Mid | 17 | 820 |
| 600 (+GG495) | Red | 17 | 1650 |
M. Hamuy led a group at CTIO to obtain observations of 10 secondary spectrophotometric standards from Taylor (1984) [123] and 19 tertiary spectrophotometric standards from Stone & Baldwin (1983) [124] and Stone (1977) [125]. These results were published in two papers:(1) Hamuy et al. (1992) [126] and (2) Hamuy et al. (1994) [127]. 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.
| Secondary Spectrophotometric Standard Stars | |||||||||
| HR# | Star | RA (J2000) |
Dec (J2000) |
MKType | (U-B) | (B-V) | V | (V-R)KC | (V-I)KC |
| 718 | ξ2 Cet | 02:28:09.54 | +08:27:36.2 | B9 III | -0.107 | -0.056 | 4.279 | -0.023 | -0.063 |
| 1544 | π2 Ori | 04:50:36.69 | +08:54:00.7 | A1 V | ... | 0.01 | 4.355 | 0.014 | 0.039 |
| 3454 | η Hya | 08:43:13.46 | +03:23:55.1 | B3 V | -0.743 | -0.200 | 4.295 | -0.083 | -0.200 |
| 4468 | θ Crt | 11:36:40.91 | -09:48:08.2 | B9.5 V | -0.18 | -0.07 | 4.700 | -0.023 | -0.063 |
| 4963 | θ Vir | 13:09:56.96 | -05:32:20.5 | A1 IV | -0.01 | -0.00 | 4.375 | 0.003 | 0.010 |
| 5501 | 108 Vir | 14:45:30.25 | +00:43:02.7 | B9.5 V | -0.080 | -0.023 | 5.681 | 0.004 | -0.026 |
| 7001 | α Lyr | 18:36:56.33 | +38:47:01.1 | A0 V | 0.00 | 0.00 | 0.03 | -0.037 | -0.045 |
| 7596 | 58 Aql | 19:54:44.80 | +00:16:24.6 | A0 II1 | -0.01 | 0.10 | 5.62 | ... | ... |
| 7950 | ε Aqr | 20:47:40.55 | -09:29:44.7 | A1 V | 0.029 | -0.001 | 3.778 | -0.005 | -0.010 |
| 8634 | ζ Peg | 22:41:27.64 | +10:49:53.2 | B8 V | -0.24 | -0.09 | 3.40 | -0.037 | -0.079 |
| 9087 | 29 Psc | 00:01:49.42 | -03:01:39.0 | B7 III-IV | -0.501 | -0.136 | 5.120 | -0.052 | -0.122 |
| Tertiary Spectrophotometric Standard Stars | |||||||||||
| Star | RA (J2000) |
Dec (J2000) |
Type | (U-B) | (B-V) | V | (V-R)KC | (R-I)KC | PM (RA) (" yr-1) |
PM (Dec) (" yr-1) |
Plots |
| 1CD-34 241 | 00:41:46.9 | -33:39:09 | f | -0.065 | +0.478 | 11.229 | +0.295 | +0.289 | -0.45 | -0.25 | finder [128]/spectrum [129] |
| LTT 1020 | 01:54:49.7 | -27:28:29 | g | -0.186 | +0.557 | 11.522 | +0.361 | +0.364 | 0.33 | -0.21 | finder [130]/spectrum [131] |
| EG 21 | 03:10:30.4 | -68:36:05 | DA | -0.661 | +0.039 | 11.379 | -0.093 | -0.064 | 0.00 | -0.30 | finder [132]/spectrum [133] |
| LTT 1788 | 03:48:22.2 | -39:08:35 | f | -0.281 | +0.469 | 13.155 | +0.317 | +0.332 | 0.24 | -0.19 | finder [134]/spectrum [135] |
| LTT 2415 | 05:56:24.2 | -27:51:26 | ... | -0.215 | +0.400 | 12.214 | +0.267 | +0.293 | 0.30 | -0.18 | finder [136]/spectrum [137] |
| Hiltner 600 | 06:45:13.5 | +02:08:15 | B1 | -0.574 | +0.179 | 10.441 | +0.120 | +0.140 | ... | ... | finder [138]/spectrum [139] |
| LTT 3218 | 08:41:32.4 | -32:56:33 | DA | -0.574 | +0.220 | 11.858 | +0.096 | +0.111 | -1.10 | 1.34 | finder [140]/spectrum [141] |
| LTT 3864 | 10:32:13.8 | -35:37:42 | f | -0.167 | +0.495 | 12.171 | +0.323 | +0.329 | -0.34 | -0.01 | finder [142]/spectrum [143] |
| LTT 4364 | 11:45:42.9 | -64:50:29 | C2 | -0.664 | +0.162 | 11.504 | +0.173 | +0.127 | 6.19 | -0.33 | finder [144]/spectrum [145] |
| 2Feige 56 | 12:06:47.3 | +11:40:13 | B5p | ... | ... | ... | ... | ... | ... | ... | finder [146]/spectrum [147] |
| LTT 4816 | 12:38:50.7 | -49:47:58 | DA | -0.656 | +0.166 | 13.794 | +0.013 | +0.027 | -0.86 | -0.13 | finder [148]/spectrum [149] |
| CD-32 9927 | 14:11:46.3 | -33:03:15 | A0 | ... | ... | ... | ... | ... | 0.01 | -0.02 | finder [150]/spectrum [151] |
| LTT 6248 | 15:38:59.8 | -28:35:34 | a | -0.197 | +0.491 | 11.797 | +0.319 | +0.345 | -0.25 | -0.18 | finder [152]/spectrum [153] |
| EG 274 | 16:23:33.7 | -39:13:48 | DA | -0.969 | -0.144 | 11.029 | -0.093 | -0.096 | 0.10 | -0.01 | finder [154]/spectrum [155] |
| LTT 7379 | 18:36:26.2 | -44:18:37 | G0 | -0.020 | +0.605 | 10.225 | +0.366 | +0.366 | -0.22 | -0.16 | finder [156]/spectrum [157] |
| LTT 7987 | 20:10:57.1 | -30:13:03 | DA | -0.670 | +0.046 | 12.230 | -0.062 | -0.078 | -0.43 | -0.24 | finder [158]/spectrum [159] |
| LTT 9239 | 22:52:40.9 | -20:35:27 | f | -0.110 | +0.609 | 12.068 | +0.397 | +0.372 | 0.10 | -0.33 | finder [160]/spectrum [161] |
| Feige 110 | 23:19:58.3 | -05:09:56 | sdO | ... | ... | ... | ... | ... | ... | ... | finder [162]/spectrum [163] |
| LTT 9491 | 23:19:35.2 | -17:05:28 | DC | -0.843 | +0.007 | 14.112 | +0.045 | +0.031 | 0.27 | 0.05 | finder [164]/spectrum [165] |
| Notes: 1CD-34 241 is mistakenly named LTT 377 in Stone and Baldwin (1983) and Hamuy et al. (1992 & 1994). 2The coordinates of Feige 56 are given incorrectly in Hamuy et al. (1992). |
|||||||||||
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 [166]):
"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. [167]
Latest release [168]
The Goodman Data-Reduction Pipeline is a Python-based package developed with the goal of processing raw spectra obtained with the Goodman High Throughput Spectrograph [169] at SOAR, and producing one-dimensional, wavelength-calibrated, science quality spectra, in a highly automated way, with minimal user intervention.
The pipeline is divided into two scripts:
After some minimal data organization, the user needs only run a single command-line instruction.
The pipeline has been designed to be run without having to perform any installation, by using a dedicated machine available at SOAR via VNC (Virtual Network Computing) for users that have access to the SOAR private network. However, users can download the software and install it locally.
For further information, details on how to run the software and the full documentation, please click this link [170] go to the official Goodman Data Reduction Pipeline documentation.
Goodman DRP team [171]
These are pages containing technical documentation intended only for SOAR Support Staff.
Users are asked not to carry out any of these procedures. If in doubt, always consult with the SOAR Support Scientist.
(Updated: Aug 29, 2017; C. Briceño)
ON-SITE STAFF IS NECESSARY TO PROCEED WITH A GOODMAN COLD START UP.
PDF version of this document [179]
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 [180]
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.
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 [183])
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.
Links
[1] mailto:spoints@ctio.noao.edu
[2] mailto:spoints@ctio.noao.edu, cbriceno@ctio.noao.edu, rcartier@ctio.noao.edu, azenteno@ctio.noao.edu
[3] mailto:tarmond@ctio.noao.edu
[4] http://www.ctio.noao.edu/noao/node/7167
[5] http://physics.unc.edu/
[6] http://adsabs.harvard.edu/abs/2004SPIE.5492..331C
[7] http://www.ctio.noao.edu/soar/content/instrument-characteristics
[8] http://www.ctio.noao.edu/soar/content/goodman-spectrograph-overview
[9] http://www.ctio.noao.edu/soar/content/goodman-hts-manual
[10] http://www.ctio.noao.edu/soar/content/observing-goodman
[11] http://www.ctio.noao.edu/soar/content/goodman-cheat-sheet
[12] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Goodman_Tutorial_2017.pdf
[13] http://www.ctio.noao.edu/soar/content/optimizing-goodman-ccd-read-out
[14] http://www.ctio.noao.edu/soar/content/calibration-information
[15] http://www.ctio.noao.edu/soar/content/soar-staff
[16] http://www.ctio.noao.edu/soar/content/goodman-data-reduction-pipeline
[17] http://www.ctio.noao.edu/soar/sites/default/files/images/Instruments/mos_data_reduction_with_goodman.pdf
[18] http://www.ctio.noao.edu/soar/content/goodman-blue-camera
[19] http://www.ctio.noao.edu/soar/content/goodman-red-camera
[20] http://www.ctio.noao.edu/soar/content/goodman-spectrograph-blue-camera-throughput-information
[21] http://www.ctio.noao.edu/soar/content/filters-available-soar
[22] http://www.ctio.noao.edu/soar/content/goodman-spectrograph-gratings
[23] http://www.ctio.noao.edu/soar/content/goodman-long-slits
[24] http://www.ctio.noao.edu/soar/content/observing-soar-limits-overheads-and-efficiency
[25] http://www.specinst.com/
[26] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Redcam_cheat_sheet.pdf
[27] http://www.ctio.noao.edu/soar/content/goodman-red-camera-cold-start-procedure-soar-support-staff
[28] http://www.ctio.noao.edu/soar/content/goodman-blue-camera-cold-start-procedure-soar-support-staff
[29] http://www.ctio.noao.edu/SOAR/Forms/INST/setup.php
[30] mailto:soarops@ctio.noao.edu
[31] http://www.ctio.noao.edu/soar/content/goodman-acquisition-camera-gacam
[32] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Images/New_Goodman_Cheat_Sheet.pdf
[33] http://www.ctio.noao.edu/soar/sites/default/files/images/Instruments/Slitmask_Guide.pdf
[34] mailto:goodman_mos@ctio.noao.edu
[35] http://www.ctio.noao.edu/soar/content/goodman-comparison-lamps-updated
[36] http://www.ctio.noao.edu/soar/user/login?destination=node/225%23comment-form
[37] http://www.ctio.noao.edu/soar/content/introduction-goodman-hts
[38] http://www.ctio.noao.edu/soar/node/226/#I1
[39] http://www.ctio.noao.edu/soar/node/226/#I2
[40] http://www.ctio.noao.edu/soar/node/226/#I3
[41] http://www.ctio.noao.edu/soar/node/227
[42] http://www.ctio.noao.edu/soar/node/227/#H2
[43] http://www.ctio.noao.edu/soar/node/227/#H3
[44] http://www.ctio.noao.edu/soar/node/227/#H4
[45] http://www.ctio.noao.edu/soar/node/227/#H5
[46] http://www.ctio.noao.edu/soar/node/227/#H6
[47] http://www.ctio.noao.edu/soar/node/227/#H7
[48] http://www.ctio.noao.edu/soar/node/227/#H8
[49] http://www.ctio.noao.edu/soar/node/227/#H9
[50] http://www.ctio.noao.edu/soar/content/goodman-software
[51] http://www.ctio.noao.edu/soar/node/228/#S1
[52] http://www.ctio.noao.edu/soar/node/228/#S2
[53] http://www.ctio.noao.edu/soar/node/228/#S3
[54] http://www.ctio.noao.edu/soar/node/228/#S4
[55] http://www.ctio.noao.edu/soar/content/observing-goodman/#S5a
[56] http://www.ctio.noao.edu/soar/content/observing-goodman/#S5b
[57] http://www.ctio.noao.edu/soar/content/observing-goodman/#S5c
[58] http://www.ctio.noao.edu/soar/content/observing-goodman/#S5d
[59] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Goodman2013_EngVersion.pdf
[60] http://www.ctio.noao.edu/soar/content/observing-goodman/#S6
[61] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/RV.pdf
[62] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/goodman_rv.pdf
[63] http://iraf.noao.edu/iraf/ftp/pub/beguide.ps.Z
[64] http://iraf.noao.edu/iraf/ftp/iraf/docs/ccduser3.ps.Z
[65] http://iraf.noao.edu/iraf/ftp/iraf/docs/spect.ps.Z
[66] http://iraf.noao.edu/iraf/ftp/iraf/docs/doslit.ps.Z
[67] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/where_does_the_light_go.pdf
[68] http://www.ctio.noao.edu/soar/content/ghts-long-slits
[69] http://www.ctio.noao.edu/soar/content/soar-remote-observers-guide
[70] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/connecting_to_goodman.pdf
[71] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/starting_up_spectrograph.pdf
[72] http://www.ctio.noao.edu/soar/content/goodman-observing-guide
[73] http://www.ctio.noao.edu/soar/content/visiting-astronomers-guide
[74] http://www.ctio.noao.edu/travel/itinerary.php
[75] http://www.ctio.noao.edu/soar/content/soar-observing-logs
[76] http://www.ctio.noao.edu/soar/content/goodman-software#S2
[77] http://www.ctio.noao.edu/soar/content/goodman-software#S3
[78] http://www.ctio.noao.edu/soar/content/goodman-software#S4
[79] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/binning.pdf
[80] http://www.ctio.noao.edu/soar/content/imaging-focus
[81] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/how_do_I_take_a_spectrum.pdf
[82] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/how_to_take_images.pdf
[83] http://www.ctio.noao.edu/SOAR/Forms/EON/Form.php?telescope=SOAR
[84] http://www.ctio.noao.edu/new/Tools/Forms/EOR/Form.php?telescope=SOAR
[85] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/control_panel_layout.pdf
[86] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/ROI.pdf
[87] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/shutting_down_the_spectrograph.pdf
[88] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Instruction.pdf
[89] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/AcqCam_User_Guide_Dec2015.pdf
[90] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/AcqCam_User_Guide_Sep2017.pdf
[91] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/AcqCam_Cheat_Sheet_Dec2015.pdf
[92] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/NewSlitDesigner.zip
[93] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Slitmask_Guide.pdf
[94] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Manual_for_Goodman_MOS_v2.pdf
[95] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/mos_observing_with_goodman_Sep2015.pdf
[96] http://www.ctio.noao.edu/soar/content/goodman-comps-and-quartz-exposure-times
[97] http://www.ctio.noao.edu/soar/content/goodman-spectrograph-typical-focus-values
[98] http://www.ctio.noao.edu/soar/content/hamuy-spectrophotometric-standards
[99] http://www.ctio.noao.edu/soar/content/radial-velocity-standards
[100] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/400m1_HgAr_3000-7000.pdf
[101] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/400m1_HgAr_3000-5000.pdf
[102] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/400m1_HgAr_5000-7000.pdf
[103] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/HgArNe_400M2_GG455_full.pdf
[104] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/HgArNe_400M2_GG455_split.pdf
[105] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/hgar_600.pdf
[106] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/CuHeAr_600_Blue_full.pdf
[107] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m1.pdf
[108] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m2.pdf
[109] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m3.pdf
[110] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m4.pdf
[111] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m5.pdf
[112] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/HgAr_930m6.pdf
[113] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/CuHeAr_930m2.pdf
[114] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/CuHeAr_930m3.pdf
[115] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/CuHeAr_930m4.pdf
[116] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/CuHeAr_930m5.pdf
[117] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/CuHeAr_930m6.pdf
[118] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/HgArNe_1200M5_GG455_full.pdf
[119] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/cuhear_1200.pdf
[120] http://www.ctio.noao.edu/soar/sites/default/files/Instrument_Plots/GHTS_2100_650nm_Ne.2.pdf
[121] http://iraf.noao.edu/specatlas/
[122] http://www.ctio.noao.edu/soar/content/observing-goodman#S5c
[123] http://adsabs.harvard.edu/abs/1984ApJS...54..259T
[124] http://adsabs.harvard.edu/abs/1983MNRAS.204..347S
[125] http://adsabs.harvard.edu/abs/1977ApJ...218..767S
[126] http://adsabs.harvard.edu/abs/1992PASP..104..533H
[127] http://adsabs.harvard.edu/abs/1994PASP..106..566H
[128] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/cd-34241_dss.pdf
[129] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/cd-34241_spec.pdf
[130] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt1020_dss.pdf
[131] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt1020_spec.pdf
[132] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/eg21_dss.pdf
[133] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/eg21_spec.pdf
[134] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt1788_dss.pdf
[135] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt1788_spec.pdf
[136] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt2415_dss.pdf
[137] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt2415_spec.pdf
[138] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/hiltner600_dss.pdf
[139] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/hiltner600_spec.pdf
[140] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt3218_dss.pdf
[141] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt3218_spec.pdf
[142] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt3864_dss.pdf
[143] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt3864_spec.pdf
[144] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt4364_dss.pdf
[145] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt4364_spec.pdf
[146] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/feige56_dss.pdf
[147] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/feige56_spec.pdf
[148] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt4816_dss.pdf
[149] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt4816_spec.pdf
[150] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/cd-329927_dss.pdf
[151] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/cd-329927_spec.pdf
[152] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt6248_dss.pdf
[153] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt6248_spec.pdf
[154] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/eg274_dss.pdf
[155] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/eg274_spec.pdf
[156] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt7379_dss.pdf
[157] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt7379_spec.pdf
[158] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt7987_dss.pdf
[159] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt7987_spec.pdf
[160] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt9239_dss.pdf
[161] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt9239_spec.pdf
[162] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/feige110_dss.pdf
[163] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/feige110_spec.pdf
[164] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt9491_dss.pdf
[165] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Hamuy/ltt9491_spec.pdf
[166] https://ui.adsabs.harvard.edu/?#abs/2013A%26A...552A..64S
[167] http://vizier.u-strasbg.fr/viz-bin/VizieR-3?-source=J/A%2bA/552/A64/table4
[168] https://github.com/soar-telescope/goodman/releases
[169] http://www.ctio.noao.edu/soar/content/goodman-high-throughput-spectrograph
[170] https://goodman.readthedocs.io/en/latest/index.html
[171] https://goodman.readthedocs.io/en/latest/authors.html
[172] http://www.ctio.noao.edu/soar/content/goodman-troubleshooting
[173] http://www.ctio.noao.edu/soar/content/cryotiger-help-page
[174] http://www.ctio.noao.edu/soar/sites/default/files/SOAR_ADC_Nasmyth_Optic-1.3.pdf
[175] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/acam-integration.pdf
[176] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/installing_and_removing_slit_masks.pdf
[177] http://www.ctio.noao.edu/soar/sites/default/files/CAMBIO%20DE%20MASCARAS%20EN%20CARRUSEL%20GOODMAN.pdf
[178] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Goodman_Maintenance_Manual.pdf
[179] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Images/ColdStart/BlueColdStart/Goodman_New_Blue_Cold_Start_rev1.pdf
[180] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Images/ColdStart/Goodman_Red_Camera_Cold_Start.pdf
[181] http://www.ctio.noao.edu/soar/content/ghts-troubleshooting-1
[182] http://www.ctio.noao.edu/soar/content/ghts-troubleshooting-2
[183] http://www.ctio.noao.edu/soar/content/goodman-user-startupshutdown-guide
[184] http://www.ctio.noao.edu/soar/sites/default/files/GOODMAN/Fwd_%20CCD-world_%20Cryotiger%20lost%20of%20cooling%20power.eml