User's Guide to the Nickel Spectrograph

Table of Contents

Hardware Overview
Aperture Wheel
Filter Wheel
CCD Stage
Detector Characteristics
Software Overview
CCD User Interface
Motor Controller
Observing Hints
Calibration Lamp Spectra

Data Archive
Mt. Hamilton Homepage

CCD User Interface

The CCD User Interface (also called the Data-Taker) is started either by clicking on its icon (labeled "Spect") or typing nickel_spect_client at the Linux command line. The interface consists of those software components for controlling the direct-imaging camera's CCD, including setting array parameters, controlling exposures, and displaying raw images:

Starting the CCD User Interface also invokes the Motor Control GUI, described in the Motor Control section of this manual.

Click for a full-sized image in a separate window.

The top level of the GUI allows one to set various detector parameters in advance, and to control exposures. Parameters are briefly described here. Commands for controlling exposures - start, pause, stop, and abort - are self explanatory.

Immediately below the Quit button is the identification of the CCD. For the Nickel Spectrograph the chip identification should be Reticon 400x1200. If it indicates another detector, contact a support astronomer for assistance.

Saved Setup Parameters are stored as one of ten "saved setups." No active "save" is required to make current parameters part of a saved setup, instead, current parameters automatically become part of the currently active saved setup. Saved setups may be named on the 2nd level of the GUI (see below).

Exposure Time Zero-second exposures and fractional seconds are allowed. Due to shutter timing errors and fly time, open shutter exposures of less than 1 second for data are not recommended.

CCD Window This is the section of the CCD which is atually read out. Smaller windows read out more quickly. The window size may be defined graphically from the image display (using the XVideo b command to define the region), or by entering rows, columns, and origin. Clicking "Whole CCD" restores readout of the whole chip. Note that the XVideo display origin is the upper left hand corner of the image.

Shutter Open for normal exposure, close for darks and bias frames.

Binning CCD9 is generally used unbinned for normal observations (see Detector Characteristics).

Read Speed Fast is about a third the time of slow, gained at the price of an increase in readnoise (see Detector Characteristics).

Observation Number and Recording The observation number increments with each recorded exposure. It can be set manually, but be careful, it is possible to overwrite existing data by setting the number back. Note that the last unrecorded exposure is saved in /scratch/nickel/scr.fits. More on recording images in "2nd Level", below.

Object You may enter up to 64 characters, including white spaces. The string will appear in the "OBJECT" field of the FITS header.

Click for a full-sized image in a separate window.

Clicking on the 2nd level tab on the GUI's left margin presents parameters that are usually only set once in the course of a night, if at all. Only the first few of these are for observer use. MPP and Amplifier selection should remain as set by default, unless there is a clearly understood reason to change them.

Saved Setup Name This allows a name to be associated with a saved setup (see Top Level).

Record Count Whether an image is recorded or not is controlled from the Top Level by turning recording on of off. The record count parameter is generally set to 1 or -1 so that all images are saved whenever recording is turned on.

Directory This parameter should be set to /data so that recorded images are saved in the /data directory. It is important to save them there so that they will be found and saved to Lick's on-line data archive, Data are copied to the archive shortly after being acquired. If you need to set or reset your data archive password, please contact a Support Astronomer. If there are data in the directory from a previous observer, contact a Support Astronomer or Telescope Technician so they can confirm that data are properly in the archive before clearing the directory for you. It is possible to overwrite data using the same observation number, so do not take any recorded data or use observation numbers different from the existing data until the data directory is properly cleared.

Root The string entered here becomes the root of the image file names, prepended to a unique image number. E.g., using the parameters shown here, the first recorded image will become /data/d1.fits, the second d2.fits, and so on. The root may be whatever you wish, but we recommend you use the default "d" root.

Suffix You may choose the suffix to be appended to your image file names, but it must be one recognized by our automatic archiver: fits, ccd, fts.

Observer's Name You may enter any number of first or last names up to a total of 64 characters. White space and comma separation are permitted. The string will appear in the "OBSERVER" field of the FITS header.

Support Astronomers (
Last modified: Tue Jul 17 18:55:42 PDT 2012