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

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

doi:10.1111/j.1365-2966.2009.15098.x

Cited by 205 publications

(153 citation statements)

References 36 publications

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“…All reductions for the light-curve analysis were conducted using variants of difference image analysis (DIA; Alard & Lupton 1998), specifically Woźniak (2000) and Albrow et al (2009).…”

Section: Full Kepler Orbits In Microlensingmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

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“…All reductions for the light-curve analysis were conducted using variants of difference image analysis (DIA; Alard & Lupton 1998), specifically Woźniak (2000) and Albrow et al (2009).…”

Section: Full Kepler Orbits In Microlensingmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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“…OGLE data were reduced using the OGLE Difference Image Analysis software and optimal centroid method (Wozniak 2000;Udalski 2003). The μFUN photometry was produced using a modified version of the PySIS package (Albrow et al 2009). Robonet data were reduced using the DanDIA package (Bramich 2008).…”

Section: Data Reductionmentioning

confidence: 99%

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

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We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong lightcurve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with -=  V I 1.48 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at =  D 6.9 1.1 kpc , and a projected star-planet separation of = -+ a 1.75 0.33 0.34 au. The lens-source relative proper motion is m =  6.5 1.1 rel mas yr −1 . The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6-8 yr after the peak magnification. So, by 2020-2022, we can hope to detect the lens star with deep, high-resolution images.

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“…RoboNet/LCOGT data were reduced using an automatic image subtraction package, and reduced again off-line. PLANET telescopes also use image subtraction: at telescope an on-line version called WISIS, based on Alard's ISIS package, then off-line version 3.0 of pySIS (Albrow et al 2009), based on a numerical kernel (Bramich 2008). SAAO I photometry obtained with pySIS has been checked independently using a DIA package.…”

Section: Data Sets: Observations and Data Reductionsmentioning

confidence: 99%

OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

Fouqué

Heyrovsky

Dong

et al. 2010

A&A

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Context. Not only is gravitational microlensing a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event.Aims. In high-magnification events, the lens caustic may cross over the source disk, which allows determination of the angular size of the source and measurement of its limb darkening. Methods. When such extended-source effects appear close to maximum magnification, the resulting light curve differs from the characteristic Paczyński point-source curve. The exact shape of the light curve close to the peak depends on the limb darkening of the source. Dense photometric coverage permits measurement of the respective limb-darkening coefficients.Results. In the case of the microlensing event OGLE 2008-BLG-290, the K giant source star reached a peak magnification at about 100. Thirteen different telescopes have covered this event in eight different photometric bands. Subsequent light-curve analysis yielded measurements of linear limb-darkening coefficients of the source in six photometric bands. The best-measured coefficients lead to an estimate of the source effective temperature of about 4700 +100 −200 K. However, the photometric estimate from colour-magnitude diagrams favours a cooler temperature of 4200 ± 100 K. Conclusions. Because the limb-darkening measurements, at least in the CTIO/SMARTS2 V s -and I s -bands, are among the most accurate obtained, the above disagreement needs to be understood. A solution is proposed, which may apply to previous events where such a discrepancy also appeared.

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

Cited by 205 publications

References 36 publications

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

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