CAMELOT2

Current Filter Wheel Configuration

 

Introduction

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 0.336 arcsec/pix. The theoretical field of view must be 23 x 23 arcsminutes² but, due to the vignetting caused by the filters, the useful field of view is 12.3 x 12.3 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.


 

Physical characteristics

  • Total CCD size: 4096 (horizontal) x 4112 (vertical) pixels
  • Pixel size: 13.5×13.5 µm
  • Pixel scale: 0.336 “/pixel
  • Total CCD field: 22.9 x 23 “²
  •  Useful CCD size (squared): 2200 (h) x 2200 (v) pixels
  • Useful CCD field (squared): 12.3 x 12.3 “²
  • Read modes: 15
  • Quantum Efficiency

 

Readout modes

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
2 709 7.2 22000 16000
3 100 43.6 60000 42000
4 855 6.6 12000 8000

 

 


 

Vignetting:

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.

vineteo

The circle has a field of 17.3 arcmin of diameter and the square has a field of 12.3×12.3 arcmin².


 

Linearity:

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.

 

 mode0_engmode1_eng

mode2_engmode3_eng

mode4_eng


 

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:

Captura de pantalla de 2020-12-26 17-57-39They need a pair or flat images and a pair of bias images. The results for the 5 readout speeds, for the 4 channel readout mode are in the following table:

 

Mode Gain (e- / ADU) RON (ADU)
0 (344 kHz, Attn 0) 4.11 6.76
1 (344 kHz, Attn 0) 7.76 10.99
2 (709 kHz) 9.78 13.99
3 (100 kHz) 0.78 6.27

4 (855 kHz)

19.94 25.27

 

This values are computed with the media of the results for each of the four channels.


 

Darks:

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.

darks_3_derk


 

Shutter:

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.

shutter

 

In the next animation is clearly seen how the leafs of the shutter open.

shutter

 

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.

shutter_speed_eng

 


 

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.

FOV_PSF_I 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.

I_eje_x_engI_eje_y_eng

 Finally, the ellipticity along both axis can see in better way plotting they in a 3D plot.

I_3d_eng

 This anomaly is due to a king of misalignment in the optical path that will be fixed in the future.


 

Written by Alberto Madrigal Aguado

Detector Characterization lUser’s Manual Frequently Asked Questions (F.A.Q.)