Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14

M. D. Albrow; J. P. Beaulieu; J. A.R. Caldwell; D. L. Depoy; M. Dominik; B. S. Gaudi; A. Gould; J. Greenhill; K. Hill; S. Kane; R. Martin; J. Menzies; R. M. Naber; R. W. Pogge; K. R. Pollard; P. D. Sackett; K. C. Sahu; P. Vermaak; R. Watson; A. Williams

doi:10.1086/308842

Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14

M. D. Albrow^*, J. P. Beaulieu, J. A.R. Caldwell, D. L. Depoy, M. Dominik, B. S. Gaudi, A. Gould, J. Greenhill, K. Hill, S. Kane, R. Martin, J. Menzies, R. M. Naber, R. W. Pogge, K. R. Pollard, P. D. Sackett, K. C. Sahu, P. Vermaak, R. Watson, A. Williams

^*Corresponding author for this work

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Abstract

We present the PLANET photometric data set for OGLE-1998-BUL-14, a high-magnification (A_max ∼ 16) event alerted by the OGLE collaboration toward the Galactic bulge in 1998. The PLANET data set consists a total of 461 I-band and 139 V-band points, the majority of which was taken over a 3 month period. The median sampling interval during this period is about 1 hr, and the 1 σ scatter over the peak of the event is 1.5%. The excellent data quality and high maximum magnification of this event make it a prime candidate to search for the short-duration, low-amplitude perturbations that are signatures of a planetary companion orbiting the primary lens. The observed light curve for OGLE-1998-BUL-14 is consistent with a single lens (no companion) within photometric uncertainties. We calculate the detection efficiency of the light curve to lensing companions as a function of the mass ratio and angular separation of the two components. We find that companions of mass ratio ≥ 0.01 are ruled out at the 95% significance level for projected separations between 0.4 and 2.4r_E, where r_E is the Einstein ring radius of the primary lens. Assuming that the primary is a G dwarf with r_E ∼ 3 AU, our detection efficiency for this event is ∼60% for a companion with the mass and separation of Jupiter and ∼5% for a companion with the mass and separation of Saturn. Our efficiencies for planets like those around v And and 14 Her are > 75%.

Original language	English
Pages (from-to)	176-189
Number of pages	14
Journal	Astrophysical Journal
Volume	535
Issue number	1 PART 1
DOIs	https://doi.org/10.1086/308842
Publication status	Published - 20 May 2000
Externally published	Yes

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Albrow, M. D., Beaulieu, J. P., Caldwell, J. A. R., Depoy, D. L., Dominik, M., Gaudi, B. S., Gould, A., Greenhill, J., Hill, K., Kane, S., Martin, R., Menzies, J., Naber, R. M., Pogge, R. W., Pollard, K. R., Sackett, P. D., Sahu, K. C., Vermaak, P., Watson, R., & Williams, A. (2000). Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14. Astrophysical Journal, 535(1 PART 1), 176-189. https://doi.org/10.1086/308842

@article{e87006996e9f4494a0b1698cb83997e1,

title = "Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14",

abstract = "We present the PLANET photometric data set for OGLE-1998-BUL-14, a high-magnification (Amax ∼ 16) event alerted by the OGLE collaboration toward the Galactic bulge in 1998. The PLANET data set consists a total of 461 I-band and 139 V-band points, the majority of which was taken over a 3 month period. The median sampling interval during this period is about 1 hr, and the 1 σ scatter over the peak of the event is 1.5%. The excellent data quality and high maximum magnification of this event make it a prime candidate to search for the short-duration, low-amplitude perturbations that are signatures of a planetary companion orbiting the primary lens. The observed light curve for OGLE-1998-BUL-14 is consistent with a single lens (no companion) within photometric uncertainties. We calculate the detection efficiency of the light curve to lensing companions as a function of the mass ratio and angular separation of the two components. We find that companions of mass ratio ≥ 0.01 are ruled out at the 95% significance level for projected separations between 0.4 and 2.4rE, where rE is the Einstein ring radius of the primary lens. Assuming that the primary is a G dwarf with rE ∼ 3 AU, our detection efficiency for this event is ∼60% for a companion with the mass and separation of Jupiter and ∼5% for a companion with the mass and separation of Saturn. Our efficiencies for planets like those around v And and 14 Her are > 75%.",

keywords = "Dark matter, Gravitational lensing, Planetary systems",

author = "Albrow, {M. D.} and Beaulieu, {J. P.} and Caldwell, {J. A.R.} and Depoy, {D. L.} and M. Dominik and Gaudi, {B. S.} and A. Gould and J. Greenhill and K. Hill and S. Kane and R. Martin and J. Menzies and Naber, {R. M.} and Pogge, {R. W.} and Pollard, {K. R.} and Sackett, {P. D.} and Sahu, {K. C.} and P. Vermaak and R. Watson and A. Williams",

note = "{\textcopyright} 2000 The Author(s)",

year = "2000",

month = may,

day = "20",

doi = "10.1086/308842",

language = "English",

volume = "535",

pages = "176--189",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 PART 1",

}

Albrow, MD, Beaulieu, JP, Caldwell, JAR, Depoy, DL, Dominik, M, Gaudi, BS, Gould, A, Greenhill, J, Hill, K, Kane, S, Martin, R, Menzies, J, Naber, RM, Pogge, RW, Pollard, KR, Sackett, PD, Sahu, KC, Vermaak, P, Watson, R & Williams, A 2000, 'Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14', Astrophysical Journal, vol. 535, no. 1 PART 1, pp. 176-189. https://doi.org/10.1086/308842

TY - JOUR

T1 - Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14

AU - Albrow, M. D.

AU - Beaulieu, J. P.

AU - Caldwell, J. A.R.

AU - Depoy, D. L.

AU - Dominik, M.

AU - Gaudi, B. S.

AU - Gould, A.

AU - Greenhill, J.

AU - Hill, K.

AU - Kane, S.

AU - Martin, R.

AU - Menzies, J.

AU - Naber, R. M.

AU - Pogge, R. W.

AU - Pollard, K. R.

AU - Sackett, P. D.

AU - Sahu, K. C.

AU - Vermaak, P.

AU - Watson, R.

AU - Williams, A.

PY - 2000/5/20

Y1 - 2000/5/20

N2 - We present the PLANET photometric data set for OGLE-1998-BUL-14, a high-magnification (Amax ∼ 16) event alerted by the OGLE collaboration toward the Galactic bulge in 1998. The PLANET data set consists a total of 461 I-band and 139 V-band points, the majority of which was taken over a 3 month period. The median sampling interval during this period is about 1 hr, and the 1 σ scatter over the peak of the event is 1.5%. The excellent data quality and high maximum magnification of this event make it a prime candidate to search for the short-duration, low-amplitude perturbations that are signatures of a planetary companion orbiting the primary lens. The observed light curve for OGLE-1998-BUL-14 is consistent with a single lens (no companion) within photometric uncertainties. We calculate the detection efficiency of the light curve to lensing companions as a function of the mass ratio and angular separation of the two components. We find that companions of mass ratio ≥ 0.01 are ruled out at the 95% significance level for projected separations between 0.4 and 2.4rE, where rE is the Einstein ring radius of the primary lens. Assuming that the primary is a G dwarf with rE ∼ 3 AU, our detection efficiency for this event is ∼60% for a companion with the mass and separation of Jupiter and ∼5% for a companion with the mass and separation of Saturn. Our efficiencies for planets like those around v And and 14 Her are > 75%.

AB - We present the PLANET photometric data set for OGLE-1998-BUL-14, a high-magnification (Amax ∼ 16) event alerted by the OGLE collaboration toward the Galactic bulge in 1998. The PLANET data set consists a total of 461 I-band and 139 V-band points, the majority of which was taken over a 3 month period. The median sampling interval during this period is about 1 hr, and the 1 σ scatter over the peak of the event is 1.5%. The excellent data quality and high maximum magnification of this event make it a prime candidate to search for the short-duration, low-amplitude perturbations that are signatures of a planetary companion orbiting the primary lens. The observed light curve for OGLE-1998-BUL-14 is consistent with a single lens (no companion) within photometric uncertainties. We calculate the detection efficiency of the light curve to lensing companions as a function of the mass ratio and angular separation of the two components. We find that companions of mass ratio ≥ 0.01 are ruled out at the 95% significance level for projected separations between 0.4 and 2.4rE, where rE is the Einstein ring radius of the primary lens. Assuming that the primary is a G dwarf with rE ∼ 3 AU, our detection efficiency for this event is ∼60% for a companion with the mass and separation of Jupiter and ∼5% for a companion with the mass and separation of Saturn. Our efficiencies for planets like those around v And and 14 Her are > 75%.

KW - Dark matter

KW - Gravitational lensing

KW - Planetary systems

UR - http://www.scopus.com/inward/record.url?scp=0034690344&partnerID=8YFLogxK

U2 - 10.1086/308842

DO - 10.1086/308842

M3 - Article

AN - SCOPUS:0034690344

SN - 0004-637X

VL - 535

SP - 176

EP - 189

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 1

ER -

Limits on stellar and planetary companions in microlensing event OGLE-1998-BUL-14

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