Difference imaging photometry of blended gravitational microlensing events with a numerical kernel
Identifieur interne : 002C22 ( PascalFrancis/Corpus ); précédent : 002C21; suivant : 002C23Difference imaging photometry of blended gravitational microlensing events with a numerical kernel
Auteurs : M. D. Albrow ; K. Home ; D. M. Bramich ; P. Fouque ; V. R. Miller ; J.-P. 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. ZubSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009.
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English descriptors
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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.
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NO : | PASCAL 09-0360685 INIST |
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ET : | Difference imaging photometry of blended gravitational microlensing events with a numerical kernel |
AU : | ALBROW (M. D.); HOME (K.); BRAMICH (D. M.); FOUQUE (P.); MILLER (V. R.); BEAULIEU (J.-P.); COUTURES (C.); MENZIES (J.); WILLIAMS (A.); BATISTA (V.); BENNETT (D. P.); BRILLANT (S.); CASSAN (A.); DIETERS (S.); DOMINIS PRESTER (D.); DONATOWICZ (J.); GREENHILL (J.); KAINS (N.); KANE (S. R.); KUBAS (D.); MARQUETTE (J. B.); POLLARD (K. R.); SAHU (K. C.); TSAPRAS (Y.); WAMBSGANSS (J.); ZUB (M.) |
AF : | Beatrice Tinsley Institute, †Department of Physics and Astronomy, University of Canterbury, Private Bag 4800/Christchurch/Nouvelle-Zélande (1 aut., 5 aut., 22 aut.); SUPA, School of Physics and Astronomy, University of St. Andrews/North Haugh, St Andrews, KY16 9SS/Royaume-Uni (2 aut., 18 aut.); Isaac Newton Group of Telescopes, Apartado de Correos 321/38700 Santa Cruz de la Palma, Canary Islands/Espagne (3 aut.); LATT, Universite de Toulouse, CNRS, 14 avenue Edouard Belin/31400 Toulouse/France (4 aut.); Institut dAstrophysique de Paris, CNRS - UMR 7095, Univensite Pierre & Marie Curie, 98bis Bd Arago/75014 Paris/France (6 aut., 7 aut., 10 aut., 14 aut., 21 aut.); CEA, DSM, DAPNIA, Centre d'Études de Saclay/91791 Gif sur-Yvette/France (7 aut.); South African Astronomical Observatory, PO Box 9/7935 Observatory/Afrique du Sud (8 aut.); Perth Observatory, Walnut Road/Bickley, Perth 6076/Australie (9 aut.); University of Notre Dame, Department of Physics, 225 Nieuwland Science Hall/Notre Dame, IN 46556/Etats-Unis (11 aut.); European Southern Observatory, Casilla 19001, Vitacura 19/Santiago/Chili (12 aut., 20 aut.); Astronomisches Rechen-Institut (ARI), Zentrum fur Astronomie (ZAH), Heidelberg University, Monchhofstrasse 12-14/69120 Heidelberg/Allemagne (13 aut., 25 aut., 26 aut.); Department of Physics, University of Rijeka, Omladinska 14/51000 Rijeka/Croatie (15 aut.); Technical University of Vienna, Department of Computing, Wiedner Hauptstrasse 10/Vienna/Autriche (16 aut.); University of Tasmania, School of Maths and Physics, Private bag 37, GPO Hobart/Tasmania 7001/Australie (17 aut.); NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue/Pasadena, CA 91725/Etats-Unis (19 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (23 aut.); Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102/Goleta, CA 93117/Etats-Unis (24 aut.); Astrophysics Research Institute, Liverpool John Moores University/Liverpool CH41 1LD/Royaume-Uni (24 aut.) |
DT : | Publication en série; Niveau analytique |
SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2009; Vol. 397; No. 4; Pp. 2099-2105; Bibl. 1/4 p. |
LA : | Anglais |
EA : | 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. |
CC : | 001E03 |
FD : | Photométrie; Microlentille; Planète; Algorithme; Incertitude; Performance; Méthode statistique; Traitement image |
ED : | Photometry; Microlenses; Planets; Algorithms; Uncertainty; Performance; Statistical method; Image processing |
SD : | Incertidumbre; Método estadístico |
LO : | INIST-2067.354000187577090360 |
ID : | 09-0360685 |
Links to Exploration step
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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Difference imaging photometry of blended gravitational microlensing events with a numerical kernel</title>
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<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Algorithms</term>
<term>Image processing</term>
<term>Microlenses</term>
<term>Performance</term>
<term>Photometry</term>
<term>Planets</term>
<term>Statistical method</term>
<term>Uncertainty</term>
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<keywords scheme="Pascal" xml:lang="fr"><term>Photométrie</term>
<term>Microlentille</term>
<term>Planète</term>
<term>Algorithme</term>
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<term>Performance</term>
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<front><div type="abstract" xml:lang="en">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.</div>
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<fA08 i1="01" i2="1" l="ENG"><s1>Difference imaging photometry of blended gravitational microlensing events with a numerical kernel</s1>
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<ET>Difference imaging photometry of blended gravitational microlensing events with a numerical kernel</ET>
<AU>ALBROW (M. D.); HOME (K.); BRAMICH (D. M.); FOUQUE (P.); MILLER (V. R.); BEAULIEU (J.-P.); COUTURES (C.); MENZIES (J.); WILLIAMS (A.); BATISTA (V.); BENNETT (D. P.); BRILLANT (S.); CASSAN (A.); DIETERS (S.); DOMINIS PRESTER (D.); DONATOWICZ (J.); GREENHILL (J.); KAINS (N.); KANE (S. R.); KUBAS (D.); MARQUETTE (J. B.); POLLARD (K. R.); SAHU (K. C.); TSAPRAS (Y.); WAMBSGANSS (J.); ZUB (M.)</AU>
<AF>Beatrice Tinsley Institute, †Department of Physics and Astronomy, University of Canterbury, Private Bag 4800/Christchurch/Nouvelle-Zélande (1 aut., 5 aut., 22 aut.); SUPA, School of Physics and Astronomy, University of St. Andrews/North Haugh, St Andrews, KY16 9SS/Royaume-Uni (2 aut., 18 aut.); Isaac Newton Group of Telescopes, Apartado de Correos 321/38700 Santa Cruz de la Palma, Canary Islands/Espagne (3 aut.); LATT, Universite de Toulouse, CNRS, 14 avenue Edouard Belin/31400 Toulouse/France (4 aut.); Institut dAstrophysique de Paris, CNRS - UMR 7095, Univensite Pierre & Marie Curie, 98bis Bd Arago/75014 Paris/France (6 aut., 7 aut., 10 aut., 14 aut., 21 aut.); CEA, DSM, DAPNIA, Centre d'Études de Saclay/91791 Gif sur-Yvette/France (7 aut.); South African Astronomical Observatory, PO Box 9/7935 Observatory/Afrique du Sud (8 aut.); Perth Observatory, Walnut Road/Bickley, Perth 6076/Australie (9 aut.); University of Notre Dame, Department of Physics, 225 Nieuwland Science Hall/Notre Dame, IN 46556/Etats-Unis (11 aut.); European Southern Observatory, Casilla 19001, Vitacura 19/Santiago/Chili (12 aut., 20 aut.); Astronomisches Rechen-Institut (ARI), Zentrum fur Astronomie (ZAH), Heidelberg University, Monchhofstrasse 12-14/69120 Heidelberg/Allemagne (13 aut., 25 aut., 26 aut.); Department of Physics, University of Rijeka, Omladinska 14/51000 Rijeka/Croatie (15 aut.); Technical University of Vienna, Department of Computing, Wiedner Hauptstrasse 10/Vienna/Autriche (16 aut.); University of Tasmania, School of Maths and Physics, Private bag 37, GPO Hobart/Tasmania 7001/Australie (17 aut.); NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue/Pasadena, CA 91725/Etats-Unis (19 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (23 aut.); Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102/Goleta, CA 93117/Etats-Unis (24 aut.); Astrophysics Research Institute, Liverpool John Moores University/Liverpool CH41 1LD/Royaume-Uni (24 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2009; Vol. 397; No. 4; Pp. 2099-2105; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
<CC>001E03</CC>
<FD>Photométrie; Microlentille; Planète; Algorithme; Incertitude; Performance; Méthode statistique; Traitement image</FD>
<ED>Photometry; Microlenses; Planets; Algorithms; Uncertainty; Performance; Statistical method; Image processing</ED>
<SD>Incertidumbre; Método estadístico</SD>
<LO>INIST-2067.354000187577090360</LO>
<ID>09-0360685</ID>
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