RISE is a fast-readout camera developed in collaboration with the Queens University Belfast for the precision measurement of transiting exoplanet timing. The camera optics were designed by John Meaburn. Mechanical design work was done at Liverpool JMU, and mechanical and software build done at QUB.

The CCD camera in use with RISE is an Andor DW485 which houses an E2V CCD 47-20 frame transfer device.


  • Single fixed filter
  • Pixel Scale: 0.54 arcsec/pixel (unbinned)
  • Field of view 9.2 x 9.2 arcmin (11 arcmin unvignetted circle - see diagram below)
  • Minimum exposure Time 1.2 seconds (1x1 binning)
  • Minimum exposure Time 0.6 seconds (2x2 binning)
  • No readout overhead.
  • Gain (2x2 binning) 2.3 electrons/count
  • Read noise (2x2 binning) 10 electrons
  • Mean dark current (2x2 binning) 0.0143 counts/sec
  • Saturation Limit (1x1 binning) 20,000 counts
  • Saturation limit (2x2 binning) 40,000 counts

RISE field of view

Above: Sketch of the RISE unvignetted field-of-view (the circle) superimposed onto the square CCD field.


RISE uses a single fixed filter. Since science commisioning and up until the end of semester 2017A, the filter offered is a "V+R" filter comprising 3mm OG515 + 2mm KG3.

RISE Filter transmission 

Above: A calculated filter transmission curve for the RISE system with the V+R filter installed.

We plan to change the filter in semester 2017B. The replacement will be a 720nm longpass filter, which can be thought of as approximately "I+Z". We are currently working on an analysis of some test data obtained with this filter, and the results will appear here shortly. However, there are two main consequences to bear in mind when preparing proposals for semester 2017B.

  • The instrument will have a reduced sensitivity due to the lower quantum efficiency of the chip at this wavelength range. We estimate the effect to be a decrease of approximately 1 magnitude in zeropoint. Whether this change will have a positive or negative impact on signal-to-noise will of course depend on the SED of the target.
  • Some fringing is apparent in our test data. The amplitude of the fringes seems to be approximately 2 to 4 per cent peak-to-trough in normal dark sky. Our initial analyses show that it is fairly straightforward to subtract the fringes from the data (see below).

RISE fringe 

Above: A test RISE frame using the "I+Z" filter, before and after a basic fringe correction.

Photometric Standards

As the majority of RISE data are taken for the purpose of relative photometry using secondary standards within the field of view, no routine nightly photometric standards are obtained with this instrument. If you require standards you must request them explicitly in your Phase 1 proposal (and include the time needed for these in your time request); you should also upload observing groups for them in your Phase 2 submission.

Sensitivity, Saturation & Defocus

The sensitivity of RISE is similar to that of IO:O (and RATCam before it) with an SDSS r'-band filter. Even so, those preparing proposals should use our Exposure Time Calculator as a guide to the signal-to-noise ratio expected with a given exposure time, seeing, sky brightness, etc.

RISE is, however, typically used with very short exposure times on bright targets, often with the telescope defocused to avoid saturation and to minimise uncertainties associated with flat-fielding. We STRONGLY RECOMMEND that users planning long groups (more than 10-20 minutes) submit a test observation to establish the best exposure time and telescope focus setting for their needs.

As a guide, on a 10th magnitude star in a 4 second exposure with 2x2 binning, the following has been measured in "typical" observing conditions:

Telescope defocus (mm): 0.5 1 2
Peak counts (ADU): 20,000-35,000 6,000-20,000 5,000

Note that saturation occurs at around 40,000 counts with 2x2 binning.

The following plots illustrate the PSF diameter and peak count rate you can expect as a function of defocus. The diameters are derived directly from the optical prescription of the telescope and instrument optics. The relative peak height is derived empirically from data similar to the table above and must only be treated as a rough guide since the result is so dependent on seeing conditions.

Line plot relating RISE defocus to image diameter Line plot relating RISE defocus to peak count rate
Above: General guide to effect you may expect as a function of RISE defocus.

Data Pipeline

All RISE data are run through a modified version of the RATCam data pipeline during the following working day after data taking. The pipeline debiases, removes a scaled dark frame, and flat-fields the data using a library flat which is updated every few months. An automated email is sent when reduced data are available for download, either from the Quicklook, Recent Data, or Archival Data web pages..

Phase 1 information

No filter-change or readout time overheads need be applied when applying for RISE time; a simple 60 second slew overhead is all that is required. No filter changes are possible, and the readout time is negligible.

Phase 2 information

Guidelines on how to prepare observations are given in the Phase 2 web pages. Note in particular the instrument-specific User Interface Instructions. The phase 2 "Wizard" should always be used to prepare observations. Groups that can not be prepared with the wizard should be discussed with LT Phase 2 support. Note that LT staff do not routinely check observing groups, and that observing groups are potentially active as soon as they are submitted. Please do contact us if you have any questions about your observations.

In general we recommend 2x2 binning is used for all RISE observing due to the better linearity and cycle time in this mode. For bright targets you must be very careful of saturation and may well need to defocus the telescope.

Users are also encouraged to use MULTRUN exposures with RISE.