On the 1 m RCC telescope:
On the 50 cm Cassegrain telescope:
The camera itself can be controlled via a GUI, therefore the optimal way to reach the controlling computer (in case of the RCC)
m16 is by VNC protocol, e.g.:
xvncviewer -bgr233 -via root@m16 :42
m16 can only be reached from the internal network. Screen 42 should be used. The switch
bgr233 reduces the color depth resulting in lower latency.
m16, the program
ixon-server should always be running. Usually, the user does not have to start it. In case of a power failure, or software crash, it can be started with the command (via
ixon-server has to be stopped. It can be carried out via telnet:
telnet localhost 32768
After connecting to the server, the command
shutdown stops the server itself. The connection can be terminated by
closeconn. Do this only, if you are absolutely sure about the results!
The camera controlling program can be started by the following command:
The FITS viewing program
DS9 has to be started by the user as well. A typical screen of
ixon-gui can be seen below.
First of all, the connection can be established by pressing the
Connect button at the lower-left corner of the window. The camera cooling can be controlled via the the
Set Temp input field. Note that the power usage of the cooler is not indicated explicitly. If the current temperature is indicated by blue numbers, then the temperature set can be hold safely. Without the water cooler, a temperature of can be reached. With the circulatory system installed, the threshold is around .
CCD Readout Control section on the above figre typical settings are shown. Change these only if you are certain about what you are doing!
The camera can be used in non-EM mode as well, in this case, the
Output Amp field should be set to
Conventional. Otherwise, set it to
EM. The typical value of the
EM gain is 40.
For dark frames, the field
Shutter mode should be set to closed. The exposure time is given in milliseconds. Also note that the lowest achievable time depends on the trimming (it can be set in the input fields
Image Size) and the binning. 2x2 binning is resonable to use in most cases. While doing lucky imaging 1x1 binning might be a better choice.
Observing sequences can be defined on the panel
Observing Blocks in a self-explanatory way. The filter field should be left on U. The filters can be set via the program
acectrl running on
m5. In the spectrograph frontend, there are two built-in filter wheels. Currently a Johnson-Cousins BVRI set is installed. The filter can be changed with the following command
acectrl --filter-1 n
where n indicates the number of the filter:
- 0: empty - 1: B - 2: V - 3: R - 4: I - 5: clear
For a more detailed description of acectrl, see article ACE spectrograph.
The EMCCD mounted on the RCC telescope (photo by Miklós Rácz).
The EMCCD mounted on the Cassegrain telescope (photo by Miklós Rácz).