The MEIA instrument is the optical imager of TJO. It consists in two components: the CCD camera and the filter wheel. In addition, a system to acquire dome flats is available. Please, read the full information provided here when preparing observations for the TJO.

CCD camera

The CCD camera is a ProLine 4240 (model PL4240-1-B), with a back-illuminated 2k×2k chip manufactured by Finger Lakes Instrumentation (FLI):

  • Model: CCD42-40-1-B
  • Sensor Manufacturer: E2V
  • Sensor Type: Back Illuminated
  • Coating: Basic Midband
  • Number of pixels: 2048x2048
  • Pixel Size: 13.5x13.5 μm (0.36x0.36 arcsec @ TJO)
  • Field of view at TJO: 12.3x12.3 arcmin
  • Sensor Diagonal: 39.1mm
  • Peak Quantum Efficiency: 96%
  • Typical Working Temperature: -30º C
  • Temperature Stability: 0.1º C
  • Typical Gain: 1.53 e-/ADU
  • Typical Dark Current: <1 e-/pixel/sec. @ -30º C
  • Typical Readout Noise: 8 e- RMS @ 500 kHz
  • Non linearity: <1%
  • Read-out time: 10 seconds

Filter wheel

The filter wheel is physically coupled to the telescope at the back of the primary mirror support. It can hold up to 12 3-inch filters that are placed at the optical axis of the telescope by rotating the filter wheel. Currently, 5 Johnson-Cousins photometric filters (manufactured by Custom Scientific) are installed: U, B, V, Rc, and Ic.

The limiting magnitude of MEIA for an exposure time of 300 seconds (the maximum recommended) to reach S/N=100 for each one of the five Johnson-Cousins filters is (preliminary results):

U B V Rc Ic
13.2 17.0 17.0 17.2 17.0

The maximum S/N that can be reached with MEIA in a single exposure strongly depends on seeing and sky brightness. However, values with a S/N=750 should ensure an optimum S/N within linerarity regime of the CCD, except in cases with very good seeing.

The time required to change from one filter to another is 30 seconds.

Dome flats

Although currently only sky flats are being obtained, dome flat-field images are expected to be routinely obtained with a homogeneity better than 1% RMS using the following instrumental set-up:

  • A white screen mounted on the inside of the dome.
  • A full-spectrum light source that illuminates the screen.
  • A control system to turn on the light when required by the observatory control system.

Standard calibration procedure

The TJO control system is designed to periodically run the acquisition of calibration images, including bias, darks and sky flat-fields:

  • Bias. Bias frames are usually taken in multiples of 5 after the acquisition of sky flats or between two science sequences along the night. Usually, a minimum number of ten bias frames are provided to the observers.
  • Dark. Dark current frames are usually taken just before or after the acquisition of bias frames. The exposure time for the dark frames depends on the exposure time of science images. Usually, the exposure time for the dark frames, corresponds to the maximum exposure time for the science frames.
  • Sky flat-fields. Sky flats are routinely taken by pointing to several blank fields during twilight. When sky conditions do not allow the acquisition of sky flat exposures, images taken previously can also be provided to the observers. Flat-field images are routinely obtained with an illumination that provides a homogeneity better than 1% RMS.

Calibration exposures are expected to be used for an on-the-fly evaluation of the quality of the science images taken with MEIA2. All the calibration images are provided to the observers having science sequences during the night.

Generalitat de CatalunyaUniversitat de BarcelonaUniversitat Autònoma de BarcelonaUniversitat Politècnica de CatalunyaConsejo Superior de Investigaciones CientíficasCentres de Recerca de Catalunya