Since mid of 2019, CAMELOT2 has replace the previous common use instrument CAMELOT. CAMELOT2 (from in spanish ‘CAmara MEjorada LIgera del Observatorio del Teide’) is the common user instrument of the IAC80 telescope, at the Teide Observatory. The IAC80 telescope has 82 cm of aperture and at its cassegrain focus is placed CAMELOT2, an instrument with a detector made by Spectral Instruments. It is a 4kx4k back illuminated CCD which operates in the optical wavelength range. It has a huge collection of filters which includes SDSS griz, Johnson UBVRI, Strömgrem uvby standards and many narrow filters. The pixels size is 15 μm which implies a pixel scale on-sky of 0.322 arcsec/pix. The theoretical field of view must be 22 x 22 arcsminutes² but, due to the vignetting caused by the filters, the useful field (squared) of view is 11.8 x 11.8 arcminutes².
From 2009 we are publishing the CAMELOT data at the Virtual Observatory service. These images, already reduced and astrometrized, are now available to the general user. Requests can be done using the standard VO tools, as Aladin or Topcat, or using our own Server Query Form.
Total CCD size: 4096 (horizontal) x 4112 (vertical) pixels
Pixel size: 15×15 µm
Pixel scale: 0.322 “/pixel
Total CCD field: 21.98 x 22.06 arcmin²
- Useful CCD size (squared): 2200 (h) x 2200 (v) pixels
- Useful CCD field (squared): 11.8 x 11.8 arcmin²
- Useful CCD field (circular area): 16.7 arcmin radius
- Read modes: 15
- Quantum Efficiency
CAMELOT2 has 3 different readout modes (1, 2 or 4 channels) and each one has 4 readout speeds (100kHz, 344 kHz, 709 kHz and 855 kHz). The usual readout mode is the one with 4 channels, and the usual readout speeds are 709 kHz and 344 kHz. Some useful information for each readout speed is shown in the table below.
|Mode||Readout speed (kHz)||Readout time (s)||Dynamic range (counts)||Recommended flat counts|
|0||344 (Attn 0)||13.5||56000||39000|
|1||344 (Attn 1)||13.5||40000||28000|
As a result of having recicled CAMELOT’s filter wheel, a vignneting appears in CAMELOT2 images, reducing its field of view. In the image below, an example is shown.
The circle has a field of 16.7 arcmin of diameter and the square has a field of 11.8×11.8 arcmin².
The figures below shows the linearity of the CCD for the 5 readout speeds. The dynamic range of the CCD and the recommended flat count in each readout speed is set from these figures.
Gain and RON (ReadOut Noise):
The gain and the RON (readout noise) can be know from each night calibration images (bias and flat) for each readout speed. It can be done with the following equations:
|Mode||Gain (e- / ADU)||RON (e-)|
|0 (344 kHz, Attn 0)||4.23||6.01|
|1 (344 kHz, Attn 0)||8.54||11.62|
|2 (709 kHz)||8.98||12.11|
|3 (100 kHz)||0.79||5.31|
4 (855 kHz)
This values are computed with the media of the results for each of the four channels.
Althought the CCD is cooled to -105ºC, a test of the darkd calibration images are perfomed. It is only teste in 344 kHz Attn 0 readout speed.
The shutter is the mecanishm tha allows light to pass or not. In Camelot2, it is made of leafs that open radially. During the time it takes to open and close, it block partially some light. In the figure below is shown the difference bewteen two zones in the unviggneting detector and a zone where firstly reach the light. This effect is visible due to for this test, a strong dome flats lights were used. In a common scenario of astronomical observation, the shutter effect is negligible.
In the next animation is clearly seen how the leafs of the shutter open.
Also, the time that the shutter spend open and close can be found. In the figure below are represented the ADU in each zone versus the time. Is clearly seen the strange behaviour until, approximately, 70 miliseconds, where the open and close shutter effects finish.
PSF (Point Spread Function):
The shape of the PSF (Point Spread Function) along the detector is revised. As is clearly seen in the figure below, the stars begin to appear elongated as they approach to the lower left corner of the detector.
In a more quantitative way, we can measure the elipticity of the stars that, in the above figure, are rounded with an orange circle. Doing this, two figures can make to see how the ellipticity of the stars evolved along each axis.
Finally, the ellipticity along both axis can see in better way plotting they in a 3D plot.
This anomaly is due to a king of misalignment in the optical path that will be fixed in the future.
Using a dark photometric night, the photometric calibration of the CCD was performed in the Johnson-Bessell filters by fitting a curve of the type: m = M + Z + K*AIRMASS + C*COLOR. The zeropoint magnitude adopted in Sextractor was zmag = 25. The results obtained were the following:
Filter: zero_point +/- error, airmass_term +/- error, color_term +/- error
B: 20.760 +/- 0.010 , 0.22 +/- 0.010 , -0.139 +/- 0.004
V: 21.060 +/- 0.007 , 0.125 +/- 0.007 , 0.028 +/- 0.006
R: 21.504 +/- 0.008 , 0.082 +/- 0.008 , 0.046 +/- 0.005
I: 21.578 +/- 0.009 , 0.051+/- 0.009 , -0.057 +/- 0.003
Signal-to-Noise ratio (S/N):
To estimate the empirical S/N from CAMELOT2 images, the following equation can be used:
Where flux is the noise-subtracted flux contained into a circular aperture, gain is the one corresponding to the CCD mode used, rad is the radius of the aperture, bgr is the background estimation from sky, and ron, the read-out noise of the CCD mode used. Flux, rad, and bgr can be obtained with the keystroke ‘r’ in IRAF/imexam.