A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514

N. Miyake; A. Udalski; T. Sumi; D. P. Bennett; S. Dong; R. A. Street; J. Greenhill; I. A. Bond; A. Gould; M. Kubiak; M. K. Szymanski; G. Pietrzynski; I. Soszynski; K. Ulaczyk; L. Wyrzykowski; F. Abe; A. Fukui; K. Furusawa; S. Holderness; Y. Itow; A. Korpela; C. H. Ling; K. Masuda; Y. Matsubara; Y. Muraki; T. Nagayama; K. Ohnishi; N. Rattenbury; To Saito; T. Sako; D. J. Sullivan; W. L. Sweatman; P. J. Tristram; P. C. M. Yock; W. Allen; G. W. Christie; D. L. DePoy; B. S. Gaudi; C. Han; C. -U. Lee; J. McCormick; B. Monard; T. Natusch; B. -G. Park; R. W. Pogge; A. Allan; M. Bode; D. M. Bramich; N. Clay; M. Dominik; K. D. Horne; N. Kains; C. Mottram; C. Snodgrass; I. Steele; Y. Tsapras; M. D. Albrow; V. Batista; J. P. Beaulieu; S. Brillant; M. Burgdorf; J. A. R. Caldwell; A. Cassan; A. Cole; K. H. Cook; Ch Coutures; S. Dieters; D. Dominis Prester; J. Donatowicz; P. Fouque; U. G. Jorgensen; S. Kane; D. Kubas; J. B. Marquette; R. Martin; J. Menzies; K. R. Pollard; K. C. Sahu; J. Wambsganss; A. Williams; M. Zub

doi:10.1088/0004-637X/752/2/82

A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514

N. Miyake^*, A. Udalski, T. Sumi, D. P. Bennett, S. Dong, R. A. Street, J. Greenhill, I. A. Bond, A. Gould, M. Kubiak, M. K. Szymanski, G. Pietrzynski, I. Soszynski, K. Ulaczyk, L. Wyrzykowski, F. Abe, A. Fukui, K. Furusawa, S. Holderness, Y. ItowA. Korpela, C. H. Ling, K. Masuda, Y. Matsubara, Y. Muraki, T. Nagayama, K. Ohnishi, N. Rattenbury, To Saito, T. Sako, D. J. Sullivan, W. L. Sweatman, P. J. Tristram, P. C. M. Yock, W. Allen, G. W. Christie, D. L. DePoy, B. S. Gaudi, C. Han, C. -U. Lee, J. McCormick, B. Monard, T. Natusch, B. -G. Park, R. W. Pogge, A. Allan, M. Bode, D. M. Bramich, N. Clay, M. Dominik, K. D. Horne, N. Kains, C. Mottram, C. Snodgrass, I. Steele, Y. Tsapras, M. D. Albrow, V. Batista, J. P. Beaulieu, S. Brillant, M. Burgdorf, J. A. R. Caldwell, A. Cassan, A. Cole, K. H. Cook, Ch Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, P. Fouque, U. G. Jorgensen, S. Kane, D. Kubas, J. B. Marquette, R. Martin, J. Menzies, K. R. Pollard, K. C. Sahu, J. Wambsganss, A. Williams, M. Zub

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.

Original language	English
Article number	82
Number of pages	12
Journal	Astrophysical Journal
Volume	752
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/752/2/82
Publication status	Published - 20 Jun 2012

Keywords

binaries: general
Galaxy: bulge
gravitational lensing: micro
GALACTIC BULGE
CHEMICAL EVOLUTION
LENSING EXPERIMENT
MASS-DISTRIBUTION
BLACK-HOLES
DWARF
PHOTOMETRY
PLANET
STARS
ATMOSPHERE

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10.1088/0004-637X/752/2/82

Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014
Horne, K. D. (PI)
Science & Technology Facilities Council
1/10/11 → 31/03/12
Project: Standard

Cite this

Miyake, N., Udalski, A., Sumi, T., Bennett, D. P., Dong, S., Street, R. A., Greenhill, J., Bond, I. A., Gould, A., Kubiak, M., Szymanski, M. K., Pietrzynski, G., Soszynski, I., Ulaczyk, K., Wyrzykowski, L., Abe, F., Fukui, A., Furusawa, K., Holderness, S., ... Zub, M. (2012). A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514. Astrophysical Journal, 752(2), Article 82. https://doi.org/10.1088/0004-637X/752/2/82

@article{8d9d7b5b37254ed6ae3f6fa97591e043,

title = "A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514",

abstract = "We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.",

keywords = "binaries: general, Galaxy: bulge, gravitational lensing: micro, GALACTIC BULGE, CHEMICAL EVOLUTION, LENSING EXPERIMENT, MASS-DISTRIBUTION, BLACK-HOLES, DWARF, PHOTOMETRY, PLANET, STARS, ATMOSPHERE",

author = "N. Miyake and A. Udalski and T. Sumi and Bennett, {D. P.} and S. Dong and Street, {R. A.} and J. Greenhill and Bond, {I. A.} and A. Gould and M. Kubiak and Szymanski, {M. K.} and G. Pietrzynski and I. Soszynski and K. Ulaczyk and L. Wyrzykowski and F. Abe and A. Fukui and K. Furusawa and S. Holderness and Y. Itow and A. Korpela and Ling, {C. H.} and K. Masuda and Y. Matsubara and Y. Muraki and T. Nagayama and K. Ohnishi and N. Rattenbury and To Saito and T. Sako and Sullivan, {D. J.} and Sweatman, {W. L.} and Tristram, {P. J.} and Yock, {P. C. M.} and W. Allen and Christie, {G. W.} and DePoy, {D. L.} and Gaudi, {B. S.} and C. Han and Lee, {C. -U.} and J. McCormick and B. Monard and T. Natusch and Park, {B. -G.} and Pogge, {R. W.} and A. Allan and M. Bode and Bramich, {D. M.} and N. Clay and M. Dominik and Horne, {K. D.} and N. Kains and C. Mottram and C. Snodgrass and I. Steele and Y. Tsapras and Albrow, {M. D.} and V. Batista and Beaulieu, {J. P.} and S. Brillant and M. Burgdorf and Caldwell, {J. A. R.} and A. Cassan and A. Cole and Cook, {K. H.} and Ch Coutures and S. Dieters and Prester, {D. Dominis} and J. Donatowicz and P. Fouque and Jorgensen, {U. G.} and S. Kane and D. Kubas and Marquette, {J. B.} and R. Martin and J. Menzies and Pollard, {K. R.} and Sahu, {K. C.} and J. Wambsganss and A. Williams and M. Zub",

year = "2012",

month = jun,

day = "20",

doi = "10.1088/0004-637X/752/2/82",

language = "English",

volume = "752",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Miyake, N, Udalski, A, Sumi, T, Bennett, DP, Dong, S, Street, RA, Greenhill, J, Bond, IA, Gould, A, Kubiak, M, Szymanski, MK, Pietrzynski, G, Soszynski, I, Ulaczyk, K, Wyrzykowski, L, Abe, F, Fukui, A, Furusawa, K, Holderness, S, Itow, Y, Korpela, A, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Nagayama, T, Ohnishi, K, Rattenbury, N, Saito, T, Sako, T, Sullivan, DJ, Sweatman, WL, Tristram, PJ, Yock, PCM, Allen, W, Christie, GW, DePoy, DL, Gaudi, BS, Han, C, Lee, C-U, McCormick, J, Monard, B, Natusch, T, Park, B-G, Pogge, RW, Allan, A, Bode, M, Bramich, DM, Clay, N, Dominik, M , Horne, KD, Kains, N, Mottram, C, Snodgrass, C, Steele, I, Tsapras, Y, Albrow, MD, Batista, V, Beaulieu, JP, Brillant, S, Burgdorf, M, Caldwell, JAR, Cassan, A, Cole, A, Cook, KH, Coutures, C, Dieters, S, Prester, DD, Donatowicz, J, Fouque, P, Jorgensen, UG, Kane, S, Kubas, D, Marquette, JB, Martin, R, Menzies, J, Pollard, KR, Sahu, KC, Wambsganss, J, Williams, A & Zub, M 2012, 'A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514', Astrophysical Journal, vol. 752, no. 2, 82. https://doi.org/10.1088/0004-637X/752/2/82

TY - JOUR

T1 - A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514

AU - Miyake, N.

AU - Udalski, A.

AU - Sumi, T.

AU - Bennett, D. P.

AU - Dong, S.

AU - Street, R. A.

AU - Greenhill, J.

AU - Bond, I. A.

AU - Gould, A.

AU - Kubiak, M.

AU - Szymanski, M. K.

AU - Pietrzynski, G.

AU - Soszynski, I.

AU - Ulaczyk, K.

AU - Wyrzykowski, L.

AU - Abe, F.

AU - Fukui, A.

AU - Furusawa, K.

AU - Holderness, S.

AU - Itow, Y.

AU - Korpela, A.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Nagayama, T.

AU - Ohnishi, K.

AU - Rattenbury, N.

AU - Saito, To

AU - Sako, T.

AU - Sullivan, D. J.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Yock, P. C. M.

AU - Allen, W.

AU - Christie, G. W.

AU - DePoy, D. L.

AU - Gaudi, B. S.

AU - Han, C.

AU - Lee, C. -U.

AU - McCormick, J.

AU - Monard, B.

AU - Natusch, T.

AU - Park, B. -G.

AU - Pogge, R. W.

AU - Allan, A.

AU - Bode, M.

AU - Bramich, D. M.

AU - Clay, N.

AU - Dominik, M.

AU - Horne, K. D.

AU - Kains, N.

AU - Mottram, C.

AU - Snodgrass, C.

AU - Steele, I.

AU - Tsapras, Y.

AU - Albrow, M. D.

AU - Batista, V.

AU - Beaulieu, J. P.

AU - Brillant, S.

AU - Burgdorf, M.

AU - Caldwell, J. A. R.

AU - Cassan, A.

AU - Cole, A.

AU - Cook, K. H.

AU - Coutures, Ch

AU - Dieters, S.

AU - Prester, D. Dominis

AU - Donatowicz, J.

AU - Fouque, P.

AU - Jorgensen, U. G.

AU - Kane, S.

AU - Kubas, D.

AU - Marquette, J. B.

AU - Martin, R.

AU - Menzies, J.

AU - Pollard, K. R.

AU - Sahu, K. C.

AU - Wambsganss, J.

AU - Williams, A.

AU - Zub, M.

PY - 2012/6/20

Y1 - 2012/6/20

N2 - We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.

AB - We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.

KW - binaries: general

KW - Galaxy: bulge

KW - gravitational lensing: micro

KW - GALACTIC BULGE

KW - CHEMICAL EVOLUTION

KW - LENSING EXPERIMENT

KW - MASS-DISTRIBUTION

KW - BLACK-HOLES

KW - DWARF

KW - PHOTOMETRY

KW - PLANET

KW - STARS

KW - ATMOSPHERE

U2 - 10.1088/0004-637X/752/2/82

DO - 10.1088/0004-637X/752/2/82

M3 - Article

SN - 0004-637X

VL - 752

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 82

ER -

A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514

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