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Difference imaging photometry of blended gravitational microlensing events with a numerical kernel

Identifieur interne : 000D50 ( Istex/Corpus ); précédent : 000D49; suivant : 000D51

Difference imaging photometry of blended gravitational microlensing events with a numerical kernel

Auteurs : M. D. Albrow ; K. Horne ; D. M. Bramich ; P. Fouqué ; V. R. Miller ; J. Beaulieu ; C. Coutures ; J. Menzies ; A. Williams ; V. Batista ; D. P. Bennett ; S. Brillant ; A. Cassan ; S. Dieters ; D. Dominis Prester ; J. Donatowicz ; J. Greenhill ; N. Kains ; S. R. Kane ; D. Kubas ; J. B. Marquette ; K. R. Pollard ; K. C. Sahu ; Y. Tsapras ; J. Wambsganss ; M. Zub

Source :

RBID : ISTEX:47D7065FE5601F3E5B7E324BF6189A1AD3FE2D28

English descriptors

Abstract

The numerical kernel approach to difference imaging has been implemented and applied to gravitational microlensing events observed by the PLANET collaboration. The effect of an error in the source‐star coordinates is explored and a new algorithm is presented for determining the precise coordinates of the microlens in blended events, essential for accurate photometry of difference images. It is shown how the photometric reference flux need not be measured directly from the reference image but can be obtained from measurements of the difference images combined with the knowledge of the statistical flux uncertainties. The improved performance of the new algorithm, relative to isis2, is demonstrated.

Url:
DOI: 10.1111/j.1365-2966.2009.15098.x

Links to Exploration step

ISTEX:47D7065FE5601F3E5B7E324BF6189A1AD3FE2D28

Le document en format XML

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<term>Accurate photometry</term>
<term>Acta astron</term>
<term>Alard lupton</term>
<term>Albrow</term>
<term>Algorithm</term>
<term>Arellano ferro</term>
<term>Astrometric reference</term>
<term>Blended events</term>
<term>Blended microlensing events</term>
<term>Bramich</term>
<term>Convolution kernel</term>
<term>Correct coordinates</term>
<term>Correct position</term>
<term>Cubic interpolation</term>
<term>Data points</term>
<term>Difference image</term>
<term>Difference images</term>
<term>Difference imaging</term>
<term>Difference imaging photometry</term>
<term>Effective number</term>
<term>Error bars</term>
<term>Galactic bulge</term>
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<term>Gravitational microlensing</term>
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<term>Isis code</term>
<term>Journal compilation</term>
<term>Kernel</term>
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<term>Light curve</term>
<term>Light curves</term>
<term>Microlensing</term>
<term>Microlensing event</term>
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<term>Microlensing events</term>
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<p>The numerical kernel approach to difference imaging has been implemented and applied to gravitational microlensing events observed by the PLANET collaboration. The effect of an error in the source‐star coordinates is explored and a new algorithm is presented for determining the precise coordinates of the microlens in blended events, essential for accurate photometry of difference images. It is shown how the photometric reference flux need not be measured directly from the reference image but can be obtained from measurements of the difference images combined with the knowledge of the statistical flux uncertainties. The improved performance of the new algorithm, relative to
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