Difference between revisions of "Detection system"

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(Sampling properties of Gaia)
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[[File:scanning_law_gal.png|400px|right|thumb|Number of observations per source over entire mission.]]
 
[[File:scanning_law_gal.png|400px|right|thumb|Number of observations per source over entire mission.]]
 
Detections will be strongly affected by sampling properties of the Gaia. These are induced by characteristic "scanning law" (see figure).
 
Detections will be strongly affected by sampling properties of the Gaia. These are induced by characteristic "scanning law" (see figure).
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Gaia will be equipped with 2 telescopes, therefore there will usually be two subsequent observations of an object, separated by 106 minutes. Next scan comes after 6h after the first (4.5h after the last observation), so there may be another set of two fields of view observations, unless the satellite precesses enough to move to another bit of the sky. Then, the same object may be observed after 40-70 days, depending on the location.
  
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Such cadence allows for detection and immediate confirmation of an anomaly using closely spaced observations, but after the sequence, the object is gone for a long time from Gaia's view.
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On the Gaia focal plane there are 8 or 9 (depending on alignment of the source on the plane) separate CCDs. The source will be observed by each of them with 4.4 seconds integration time. This feature can be very helpful in rejecting spurious anomalies, like cosmic rays, etc. Also, it will provide closely spaced observations, useful in detecting very rapid changes in brightness.
  
 
== Photometric precision ==
 
== Photometric precision ==

Revision as of 14:37, 6 November 2009

Detailed description (in draft version) of the Java code is available from Gaia WebSVN (Gaia password required), or here.



Detection

Detection will be conducted in almost entire range of available magnitudes from Gaia. Limiting magnitude for Gaia is equivalent of V=20mag, but for detection we will require signal above at least 19mag, to avoid spurious anomalies at high noise level. The saturation limit for Gaia is around 5 mag.

  • Detection system employs the following data:
    • G-flux observations - all available in given cycle
    • accumulated G-flux: mean and scatter
    • accumulated BP and RP colours
    • low-dispersion BP and RP spectrometry
    • morphology of the source
    • source motion flags
    • later in the mission: CU3, CU4, CU7 and CU8’s deliverables (information on motion, variability, astrophysical parameters)

Sampling properties of Gaia

Number of observations per source over entire mission.

Detections will be strongly affected by sampling properties of the Gaia. These are induced by characteristic "scanning law" (see figure). Gaia will be equipped with 2 telescopes, therefore there will usually be two subsequent observations of an object, separated by 106 minutes. Next scan comes after 6h after the first (4.5h after the last observation), so there may be another set of two fields of view observations, unless the satellite precesses enough to move to another bit of the sky. Then, the same object may be observed after 40-70 days, depending on the location.

Such cadence allows for detection and immediate confirmation of an anomaly using closely spaced observations, but after the sequence, the object is gone for a long time from Gaia's view.

On the Gaia focal plane there are 8 or 9 (depending on alignment of the source on the plane) separate CCDs. The source will be observed by each of them with 4.4 seconds integration time. This feature can be very helpful in rejecting spurious anomalies, like cosmic rays, etc. Also, it will provide closely spaced observations, useful in detecting very rapid changes in brightness.

Photometric precision

Photometric precision.png From M. Varadi et al. 2009.

Classification

At this stage all additional information from Gaia and later from other catalogues will be used for narrowing down the sample of interesting alerts.

Cross-matching with existing catalogues

List of catalogues to cross-match