First microlens mass measurement: Planet photometry of EROS BLG-2000-5

Jin H. An; 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. W. Pogge; K. R. Pollard; P. D. Sackett; K. C. Sahu; P. Vermaak; R. Watson; A. Williams

doi:10.1086/340191

First microlens mass measurement: Planet photometry of EROS BLG-2000-5

Jin H. An^*, 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. W. Pogge, K. R. Pollard, P. D. Sackett, K. C. Sahu, P. Vermaak, R. Watson, A. Williams

^*Corresponding author for this work

Research output: Contribution to journal › Review article › peer-review

161 Citations (Scopus)

Abstract

We analyze PLANET photometric observations of the caustic-crossing binary lens microlensing event, EROS BLG-2000-5, and find that modeling the observed light curve requires incorporation of the microlens parallax and the binary orbital motion. The projected Einstein radius (r̃_E = 3.61 ± 0.11 AU) is derived from the measurement of the microlens parallax, and we are also able to infer the angular Einstein radius (θ_E = 1.38 ± 0.12 mas) from the finite source effect on the light curve, combined with an estimate of the angular size of the source given by the source position in a color-magnitude diagram. The lens mass, M = 0.612 ± 0.057 M_⊙, is found by combining these two quantities. This is the first time that parallax effects are detected for a caustic-crossing event and also the first time that the lens mass degeneracy has been completely broken through photometric monitoring alone. The combination of r̃_E and θ_E also allows us to conclude that the lens lies in the near side of the disk, within 2.6 kpc of the Sun, while the radial velocity measurement indicates that the source is a Galactic bulge giant.

Original language	English
Pages (from-to)	521-539
Number of pages	19
Journal	Astrophysical Journal
Volume	572
Issue number	1 I
DOIs	https://doi.org/10.1086/340191
Publication status	Published - 10 Jun 2002
Externally published	Yes

Access to Document

10.1086/340191

Cite this

An, J. H., 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., Pogge, R. W., Pollard, K. R., Sackett, P. D., Sahu, K. C., Vermaak, P., Watson, R., & Williams, A. (2002). First microlens mass measurement: Planet photometry of EROS BLG-2000-5. Astrophysical Journal, 572(1 I), 521-539. https://doi.org/10.1086/340191

@article{6763fa335713438ab858faa427e0239e,

title = "First microlens mass measurement: Planet photometry of EROS BLG-2000-5",

abstract = "We analyze PLANET photometric observations of the caustic-crossing binary lens microlensing event, EROS BLG-2000-5, and find that modeling the observed light curve requires incorporation of the microlens parallax and the binary orbital motion. The projected Einstein radius ({\~r}E = 3.61 ± 0.11 AU) is derived from the measurement of the microlens parallax, and we are also able to infer the angular Einstein radius (θE = 1.38 ± 0.12 mas) from the finite source effect on the light curve, combined with an estimate of the angular size of the source given by the source position in a color-magnitude diagram. The lens mass, M = 0.612 ± 0.057 M⊙, is found by combining these two quantities. This is the first time that parallax effects are detected for a caustic-crossing event and also the first time that the lens mass degeneracy has been completely broken through photometric monitoring alone. The combination of {\~r}E and θE also allows us to conclude that the lens lies in the near side of the disk, within 2.6 kpc of the Sun, while the radial velocity measurement indicates that the source is a Galactic bulge giant.",

keywords = "Binaries: general, Gravitational lensing, Stars: fundamental parameters",

author = "An, {Jin H.} and 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 Pogge, {R. W.} and Pollard, {K. R.} and Sackett, {P. D.} and Sahu, {K. C.} and P. Vermaak and R. Watson and A. Williams",

year = "2002",

month = jun,

day = "10",

doi = "10.1086/340191",

language = "English",

volume = "572",

pages = "521--539",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 I",

}

An, JH, Albrow, MD, Beaulieu, JP, Caldwell, JAR, DePoy, DL, Dominik, M, Gaudi, BS, Gould, A, Greenhill, J, Hill, K, Kane, S, Martin, R, Menzies, J, Pogge, RW, Pollard, KR, Sackett, PD, Sahu, KC, Vermaak, P, Watson, R & Williams, A 2002, 'First microlens mass measurement: Planet photometry of EROS BLG-2000-5', Astrophysical Journal, vol. 572, no. 1 I, pp. 521-539. https://doi.org/10.1086/340191

TY - JOUR

T1 - First microlens mass measurement

T2 - Planet photometry of EROS BLG-2000-5

AU - An, Jin H.

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 - 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 - 2002/6/10

Y1 - 2002/6/10

N2 - We analyze PLANET photometric observations of the caustic-crossing binary lens microlensing event, EROS BLG-2000-5, and find that modeling the observed light curve requires incorporation of the microlens parallax and the binary orbital motion. The projected Einstein radius (r̃E = 3.61 ± 0.11 AU) is derived from the measurement of the microlens parallax, and we are also able to infer the angular Einstein radius (θE = 1.38 ± 0.12 mas) from the finite source effect on the light curve, combined with an estimate of the angular size of the source given by the source position in a color-magnitude diagram. The lens mass, M = 0.612 ± 0.057 M⊙, is found by combining these two quantities. This is the first time that parallax effects are detected for a caustic-crossing event and also the first time that the lens mass degeneracy has been completely broken through photometric monitoring alone. The combination of r̃E and θE also allows us to conclude that the lens lies in the near side of the disk, within 2.6 kpc of the Sun, while the radial velocity measurement indicates that the source is a Galactic bulge giant.

AB - We analyze PLANET photometric observations of the caustic-crossing binary lens microlensing event, EROS BLG-2000-5, and find that modeling the observed light curve requires incorporation of the microlens parallax and the binary orbital motion. The projected Einstein radius (r̃E = 3.61 ± 0.11 AU) is derived from the measurement of the microlens parallax, and we are also able to infer the angular Einstein radius (θE = 1.38 ± 0.12 mas) from the finite source effect on the light curve, combined with an estimate of the angular size of the source given by the source position in a color-magnitude diagram. The lens mass, M = 0.612 ± 0.057 M⊙, is found by combining these two quantities. This is the first time that parallax effects are detected for a caustic-crossing event and also the first time that the lens mass degeneracy has been completely broken through photometric monitoring alone. The combination of r̃E and θE also allows us to conclude that the lens lies in the near side of the disk, within 2.6 kpc of the Sun, while the radial velocity measurement indicates that the source is a Galactic bulge giant.

KW - Binaries: general

KW - Gravitational lensing

KW - Stars: fundamental parameters

UR - http://www.scopus.com/inward/record.url?scp=0038475555&partnerID=8YFLogxK

U2 - 10.1086/340191

DO - 10.1086/340191

M3 - Review article

SN - 0004-637X

VL - 572

SP - 521

EP - 539

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

First microlens mass measurement: Planet photometry of EROS BLG-2000-5

Abstract

Access to Document

Other files and links

Fingerprint

Cite this