Potential Direct Single‐Star Mass Measurement | Zendy

H. Ghosh | Zendy; D. L. DePoy | Zendy; A. GalYam | Zendy; B. S. Gaudi | Zendy; Andrew Gould | Zendy; Cheongho Han | Zendy; Y. Lipkin | Zendy; Dan Maoz | Zendy; E. O. Ofek | Zendy; B.G. Park | Zendy; Richard W. Pogge | Zendy; Samir Salim | Zendy; F. Abe | Zendy; D. P. Bennett | Zendy; I. A. Bond | Zendy; S. Eguchi | Zendy; Y. Furuta | Zendy; J. B. Hearnshaw | Zendy; K. Kamiya | Zendy; P. M. Kilmartin | Zendy; Y. Kurata | Zendy; K. Masuda | Zendy; Y. Matsubara | Zendy; Y. Muraki | Zendy; S. Noda | Zendy; Kazuhisa Okajima | Zendy; Nicholas J. Rattenbury | Zendy; T. Sako | Zendy; Tomohiko Sekiguchi | Zendy; D. J. Sullivan | Zendy; T. Sumi | Zendy; P. J. Tristram | Zendy; Tatsuya Yanagisawa | Zendy; P. C. M. Yock | Zendy; A. Udalski | Zendy; I. Soszyński | Zendy; Ł. Wyrzykowski | Zendy; M. Kubiak | Zendy; M. K. Szymański | Zendy; G. Pietrzyński | Zendy; O. Szewczyk | Zendy; K. Żebruń | Zendy; Michael D. Albrow | Zendy; JeanPhilippe Beaulieu | Zendy; J. A. R. Caldwell | Zendy; A. Cassan | Zendy; C. Coutures | Zendy; M. Dominik | Zendy; J. Donatowicz | Zendy; P. Fouqué | Zendy; J. Greenhill | Zendy; K. Hill | Zendy; K. Horne | Zendy; U. G. Jørgensen | Zendy; Stephen R. Kane | Zendy; D. Kubas | Zendy; R. Martin | Zendy; J. Menzies | Zendy; K. R. Pollard | Zendy; K. C. Sahu | Zendy; J. Wambsganß | Zendy; R. Watson | Zendy; A. Williams | Zendy

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Potential Direct Single‐Star Mass Measurement

Author(s) -

H. Ghosh,

D. L. DePoy,

A. GalYam,

B. S. Gaudi,

Andrew Gould,

Cheongho Han,

Y. Lipkin,

Dan Maoz,

E. O. Ofek,

B.G. Park,

Richard W. Pogge,

Samir Salim,

F. Abe,

D. P. Bennett,

I. A. Bond,

S. Eguchi,

Y. Furuta,

J. B. Hearnshaw,

K. Kamiya,

P. M. Kilmartin,

Y. Kurata,

K. Masuda,

Y. Matsubara,

Y. Muraki,

S. Noda,

Kazuhisa Okajima,

Nicholas J. Rattenbury,

T. Sako,

Tomohiko Sekiguchi,

D. J. Sullivan,

T. Sumi,

P. J. Tristram,

Tatsuya Yanagisawa,

P. C. M. Yock,

A. Udalski,

I. Soszyński,

Ł. Wyrzykowski,

M. Kubiak,

M. K. Szymański,

G. Pietrzyński,

O. Szewczyk,

K. Żebruń,

Michael D. Albrow,

JeanPhilippe Beaulieu,

J. A. R. Caldwell,

A. Cassan,

C. Coutures,

M. Dominik,

J. Donatowicz,

P. Fouqué,

J. Greenhill,

K. Hill,

K. Horne,

U. G. Jørgensen,

Stephen R. Kane,

D. Kubas,

R. Martin,

J. Menzies,

K. R. Pollard,

K. C. Sahu,

J. Wambsganß,

R. Watson,

A. Williams

Publication year - 2004

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/423665

Subject(s) - gravitational microlensing , light curve , physics , astrometry , einstein radius , proper motion , lens (geology) , distortion (music) , event (particle physics) , radius , astrophysics , optics , stars , astronomy , gravitational lens , amplifier , computer security , optoelectronics , redshift , cmos , galaxy , computer science

We analyze the lightcurve of the microlensing eventOGLE-2003-BLG-175/MOA-2003-BLG-45 and show that it has two properties that,when combined with future high resolution astrometry, could lead to a direct,accurate measurement of the lens mass. First, the lightcurve shows clear signsof distortion due to the Earth's accelerated motion, which yields a measurementof the projected Einstein radius \tilde r_E. Second, from precise astrometricmeasurements, we show that the blended light in the event is coincident withthe microlensed source to within about 15 mas. This argues strongly that thisblended light is the lens and hence opens the possibility of directly measuringthe lens-source relative proper motion \vec\mu_\rel and so the massM=(c^2/4G)\mu_\rel t_E \tilde r_E, where t_E is the measured Einsteintimescale. While the lightcurve-based measurement of \tilde r_E is, by itself,severely degenerate, we show that this degeneracy can be completely resolved bymeasuring the direction of proper motion \vec\mu_\rel.Comment: 28 pages including 7 figures. Submitted to Ap

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