N.B. If the computer have its builtin webcam (sometimes the case for laptops), the external mount webcam will be available on the USB device /dev/video1 instead of /dev/video0 .

As root do

Active archive

• SBIG Driver package from Jan Soldan 6 oct 2010 PUBLIC_SOFTWARE.tar.gz

Learn more about that

• Official nightview web site: http://www.physics.muni.cz/mb/nightview/
• nightview package already tested with SAND-3: nightview 2008-11-01

Skycalc

Skycalc allows ephemeris calculations that provide, among other time of the astronomical twilight ans sunset. These data will be used to manage the launch of observation requests. However a number of additional information will also be archived in the execution log file as the percentage of the lunar disk illuminated.

1. Download skycalc.c from link below and save file (probably in /home/sand/Downloads)

   • Source code of Skycalc 2010

2. As root do:

Lear more

skycalc manual

pyephem

Note: il manque des dependances a cette installation. Voir le journal des etudiants 2013-2014

Another ephemeris library using python.

• Download pyephem pyephem-3.7.5.1.tar.gz
• Uncompress the archive

• As root, compile the library

Servo city PT785-S Pan / Tilt mount with pololu Micro Maestro 6-Channel USB Servo Controller

Only do this step if you have this hardware. The default is the Meade's LXD-75 mount via autostar handpad 497. PT785-S is clearly less accurate (of the order of 1 deg) but it could be enough as light pollution do not varry at high angular frequencies.

1. As sand do:

• Download the pololu for linux package v 100507

1. As root do:

D-LINK router configuration

The router is useful when SAND is connected to the Internet and that the appropriate ports are open to take control of the instrument remotely. If the system is not connected to the internet, a simple network switch or hub is sufficient.

• Router local IP: 192.168.1.1
• Disable DHCP server and attribute Fixed IP as follow:
  • 192.168.1.100 = control computer
  • 192.168.1.101 = vebcam server
  • 192.168.1.other = any other computer connected temporarly or permanently to the router
• Create a virtual server to redirect port 2022 of the router toward SSH port 22 of 192.168.1.100
• Do the same for port 2080 to allow web access redirection (port 80)
• Create virtual server from port 2180 toward 192.168.1.101 port 80 (webcam server). This redirection will allow a user to see the webcam image from the web even if the computer is off.

Apache server

We are using the Apache web server. This server allow the remote control from a web interface. It allow also browsing the database.

To activate the web server, we must:

• Start httpd service and click on Boot startup (use drakconf via system-> Manage system services)
• Move to the security section and allow http (web server) from the firewall Services. Allow also port 2080 (Ports tab).
• As root, modify /etc/httpd/conf/httpd.conf .

• Restart httpd. As root do

• Be shure that the directory /home/sand is executable by all. As root do:

• As sand, create the directory /home/sand/public_html modify the permissions by doing:

• As sand do:

• Into /home/sand/public_html as sand, create the file .htaccess:

• Goto /home/sand/public_html/data , as sand, create the file .htaccess with this content:

• Go to /home/sand/ as sand do:

• As sand, install cgi scripts and thml pages:

• As sand, remove write permissions for other and group of all cgi scripts located in /home/sand/cgi-bin :

• Then if some files are not accessibles via the web interface, do as sand

Webcam server LINKSYS WVC54GC ou D-LINK DCS-920 et webcam logitech quickcam notebook

We are using a webcam server to track cloudiness and transparency of the window during day time. The webcam server is also usefull to measure the ambiant luminosity. This is obtained by taking the mean grey level of the image. If the mean grey level is higher that a given treshold (typically 10 or 20) then the observe script will pause for 15 min before make another verification of the mean grey level. Observe can also decide to begin observation if the ambiant luminosity is under the threshold when the starting observation time is more than 12 hours later.

• Giving that we can choose between 2 webcam server models, it is absolutely necessary to specify the model in the /usr/local/bin/webcamimg file.
• It is also required to set the network setting so that the DHCP is disabled. We are using fixed address 192.168.1.101 for the webcam server.
• You should add the sand user in the webcam configuration interface with password that fit the one in the /usr/local/bin/webcamimg script.
• Another webcam serve may be used to monitor the state of the mount. This device should have ip address 192.168.1.102. The user should use the web interface to see this image.
• Again giving that we can choose between 2 webcam server models, it is absolutely necessary to specify the model in the /home/sand/public_html/cgi-bin/print.cgi file.

crontab

The crond daemon is scheduling repetitive task on lilux system. Users who have the right to use crond can schedule their own tasks to crond. We are using crond to schedule a webcam acquisition every 15 min and to create an animated gif with the last 6 hours images.

Allow sand user to use crond

As root, allow sand to use cron by doing:

Add program webcamimg to the crond schedule

As sand, edit crontab

Add the following content:

Add program checkmysystem.bash and restartskycam.bash to the root crond schedule

As root, edit crontab

Add the following content:

USB GPS BU-353 from GlobalSat

The GPS is controlled by the gpsd server. The GPS startup may easily take 45 seconds (time to connect to available satallites). Sometime, the GPS do not succeed to connect to satellites. Most of the time this occur when satellites are masked by obstacles like mountains or buildings. The observe script is able to extract latitude and longitude from the GPS and use them for ephemeris calculations. To be shure that the gpsd server will startup with the system do the following steps.

As root create the script gpsstart into /etc/init.d .

As root do:

As root do:

UPS control

The UPS is a power battery backup. It will protect the system against power fluctuations and will allow the system to continue its ongoing tasks during short power failure.

• Use an APC UPS
• As root do:

• In drakconf->system->services and deamons et enable the apcupsd deamon on startup. Then startup the deamon.
• As root be shure that everything is working proberly by doing:

Monitoring system sensors

On a regular pc, we can use thermal sensors to monitor the internal temperature of obsand.

• As root do:

• The user sand can obtain sensors readout by doing:

• It is also possible to do the readout from the web interface.

System reboot

Now all the relevant software are installed, in order to activate all newly added functionalities, restart the computer.

Configuring the spectrometer

Opto-mechanical alignment and focussing

The spectrometer may be aligned following the procedure described in the document titled Operating instructions for the Santa Brabara Instrument Group Deep Space Spectrograph (DSS-7). In that case, it may be usefull to keep a windows partition since CCDOPS is convenient to make alignment with the focus mode.

We suggest here an alternative step by step procedure to make the optical alingment and focussion in linux.

The DSS-7 have a set of 4 air slits of various width. We are using the thinnest (the one giving the darkest spectrum and thinnest spectral lines). This slit possess a width of 50 microns of 1.45 mm in length.

Table 3: Field of view of the spectrometer:

SAND-4 version

To get the proper spectral image orientation on the CCd matrix (UV to the left and IR at right), the DSS-7 should be attached to the ST-402 camera according to the image below.

Figure 1: Proper orientation of the ST-402 relative to DSS-7

• Remove the top plate of the spectrometer and remove the rose foam inside. Then put back the top plate. *Point the spectrometer toward a white target illuminated with a fluocompact lamp.
• Focus the slit image on the camera. Unscrew the 2 screws on a small rectangle plate on top of the spectrometre (top defined according to Figure 1 orientation). Take a picture by doing:

Then move the small plate in a given way and take another picture. Repeat this step as long as the image of the slit is not the sharpest you can have. At the end, thighten the 2 screws.

• Open the top plate again and move the grating in the imaging position and turn the slit assembly to remove the slits from the field of view. Then put back the top plate.
• Attach the camera lens to tha CLA-7 adaptor and screw the adaptor into the DSS-7 spectrometer.
• Set the camera distace to infinity and apperture to F2.8
• Focus the image at infinity by reproducing the commands given in step 3 above. That time you want to obtain the sharpest image you can of a remote scenery located in front of the lens.
• When the image is sharp, tighten the 6 small screws of the CLA-7 adaptor.
• Open once again the top plate and move back the grating to spectral position and turn back the slits. Then put some hot glue on the arm of the grating assembly and on the slit assembly. Those two components should not move in the future. Put back the top plate.

Figure 2

• Now it is time to center the spectrum on the image. Ideally you should place the spectrometre in the orientation illustrated in fig 3 below.

Take note that at this step you should have the camera lens attached even if it is not shown on figure 3.

• Turn the DSS-7 relatively to the camera to obtain spectrum almost horizontal.
• Then unscrew the 3 brass screws and move the spectrometer in the camera lens direction and then in ist perpendicular direction. At the end of this step, the darkest spectrum should be more or less centered in the vertical axis of the image, and you should see two the two spectral lines at the left of the image. Thighten the 3 brass screw and glue that moving part to the rest of the spectrometer.
• Now we have to be shure that a spectral line is totally vertical on the image. To do so, you can rotate the spectrometer relatively to the camera. This step is very important since it will determine the signal to noise ratio. You can use the vertical edge of another window to be shure that the spectral line is really vertical on the image. When it is totally vertical, tighten the 3 screws attaching the DSS-7 to the camera D block and put some glue between the camera and the spectrometer.

At the end of the alignment procedure, the image of a white surface lighted by a fluocompact lamp, should be similar to image of table 4. We can clearly see on this image the 4 slits dispersion. These slits allow to cover a large span of sensitivity/spectral resolution. We are normally using the highest resolution that keep the signal to noise ratio at a reasonable level. On the same figure, we can notice that the spectral dispersion is correctly alligned horizontally (relative to the red rectangle). But the most important is to be shure that a given spectral line is precisely vertical on the image. This vertical alignment is crutial to get a maximum signal to noise ratio and an optimal spectral resolution. Sometimes the optical assembly is not perfectly done by SBIG and this may result in non perfect orthogonality between the spectral line and the spectral dispersion. This is not a big problem.

Securing moving components

The DSS-7 spectrometer contain some moving components (the air slit and the grating). Moreover, the grating is supported on a flexible shaft. These moving parts have the disadvantage that if we move the orientation of the spectrometer, there is some small change in grating orientation and then the spectrum moves on the CCD image. We decided to glue those moving parts. We used melted glue applied with a glue gun. That kind of glue may be remove (not without pain...) if required. Refer to figure 2 above to see where the glued spots should be applied. It should be also a good idea to glue the coupling fo the camera and the spectrometer and the spectrometer plate if you plan to travel with the instrument. This will prevent unwanted spectral calibration shifts.

Parameters for spectral calibration

In order to extract the spectral information of the desired air slit from the CCD image we should specify the line numbers of the beginning and end of the spectrum. As an example, on the image show in table 4, we had measured 136 and 218. This information have to appear in the spectral calibration file. There will be different values for different spectrometers units. More over these values may change if the instrument is violently shocked. It could be a good idea to keep an image of a uniform surface lighted by a fluocompact bulb as a reference. This image may be used later to confirm that the spectral calibration had not changed. The spectral calibration file name should allow to clearly identify the spectrometer unit and should contain the date of the calibration process.

Here is an example of a spectral calibration file

The conversion pixel to wavelength is done by doing: Wavelength(nm)=quad \times {pixel}^2 + gain \times pixel + oorigin

Table 4: Spectral alignment and calibration

Typical spectrum of a fluo-compact	Spetral line wavelength (nm)
	405.4 436.6 487.7 542.4 546.5 593.4 599.7 611.6 631.1 650.8 662.6 687.7 693.7 707 et 709 712.3 760.0 source

Note that the wavelengths provided in table above are for the peak of the spectral line as observed with a real fluocompact light bulb. This is why it is equal to the nominal wavelength of the given chemical element

To determine the spectral calibration parameters, you will need to identify the pixel position on the CCD image of spectral lines identified in table 4 above. The you can use a fitting application like fityk to fit a second order polynomial on the data assuming that x are the pixel position and y the wavelength in nm. But it is important to note that for us, the first pixel of the image is at position 1 (not 0 as it is in display program).

Figure 3: Example of spectral calibration with OpenOffice Calc. For that case we set the curve to linear since OpenOffice is not able to fit 2^nd order polynomials Download openoffice calc file.

For the case presented in figure 3, gain= 0.54056, oorigin= 397.8097 and quad= 0. .

OBSAND-2 automated observatory

The OBSAND-2 observatory is a protecting structure that keeps the spectrometer safe from the outdoor elements and from the extreme temperature variations. OBSAND-2’s objective is to allow the system to be continually operating with its robotized mounting. OBSAND-2 follows a first version called OBSAND and developed by mechanical engineering students (Université de Sherbrooke) and electrical engineering students (Cégep de Sherbrooke) supervised by Martin Aubé (Cégep/Université de Sherbrooke) and Chloé Legris (AstroLab du Mont-Mégantic). Due to the complexity of the construction and the maintenance of the OBSAND, we decided here to design a simplified observatory called OBSAND-2.

Figure 4: OBSAND-2 at Sherbrooke University, Quebec, Canada with SAND-3A inside

SAND-3A spectrometer

SAND-3A was optimized for a fixed installation but can be easily carried on a plane. It consists in a smaller box than OBSAND-2. It has the dimensions of a hand-luggage and can be carried in the cabin. SAND-3 is provided with a starphire glass that can be washed more times. This version was conceived for its installation in China. It has a power of 45 Watt, and can reach 65 Watt when its heating cable is in operation (less than 5 C). The system is controlled by an Acer Aspire One netbook. OBSAND-3 doesn’t include any mounting, and must be aligned in order to point at the zenith. SAND-3A includes less components than OBSAND-2. Here is a list of the revoved components:

• LXD-75 mount
• UPS
• The computer is substituted by a netbook (ASPIRE ONE de Acer).
• GPS
• Mount WEBcam
• The bathroom fan is substituted by a 1 1/2'' computer fan working on 12 V.
• Dessicant.

Img:obsand3-00.jpg

Figure 5: SAND-3A at AIOFM center Hefei, Anhui, China

For now, SAND-3 isn’t adapted to the very cold climatic conditions because its provided with a heating cable of 21 Watt only.

External size of the box:

height=13 po
width=9 po
depth=22 po

Mass:

SAND-3B spectrometer

This SAND version is intended for ponctual measurements but can be installed permanently. The main idea is to localize the computer-router tandem far from the webcam server and the spectrometer. The computer and the router are then safely set indoor, while only the spectrometer and the webcam server are exposed to the outdoor elements. In order to assure the communication between the outdoor unit and the indoor control center, we use a network cable for the webcam server and a USB->CAT5 converter for the spectrometer. The outdoor unit must also be powered by electricity. Here is a list of the non present components :

• LXD-75 mount
• GPS
• Mount WEBcam
• Fan
• Dessicant

The box protecting the spectrometer is the 516-0010 HAMMOND MFG model. Its dimensions are 8.5po x 14.38po x 9.25po (height). It has its own natural ventilating slits. A mosquito net has been placed on the interior side in front of those slits in order to repeal as much insects as possible.

Figure 6: SAND-3B at Sherbrooke University, Quebec, Canada

Development documentation

Here

Todo list

User's guide

Jump to SAND user's guide