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. Szymański, G. Pietrzyński, I. Soszyński, 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. Fouqué, 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

Research output: Contribution to journalArticle

11 Citations (Scopus)

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 DL = 3.11 ± 0.39kpc and total mass ML = 1.40 ± 0.18 M ⊙; this leads to the primary and secondary components having masses of M 1 = 1.06 ± 0.13 M ⊙ and M 2 = 0.34 ± 0.04 M ⊙, 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+4.6 -0.3 M ⊙ and it is at a distance of D L = 2.6+3.8 -0.9kpc. Given the secure mass ratio measurement, the companion mass is therefore M 2 = 0.2+1.2 -0.1 M ⊙. 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 languageEnglish
Article number82
JournalAstrophysical Journal
Volume752
Issue number2
DOIs
Publication statusPublished - 20 Jun 2012
Externally publishedYes

Fingerprint

magnification
lenses
parallax
orbits
mass ratios
Bayesian analysis
Earth motion
main sequence stars
observatory
neutron stars
light curve
observatories
radii
estimates
effect

Keywords

  • binaries: general
  • Galaxy: bulge
  • gravitational lensing: micro

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

A possible binary system of a stellar remnant in the high-magnification gravitational microlensing event OGLE-2007-BLG-514. / Miyake, N.; Udalski, A.; Sumi, T.; Bennett, D. P.; Dong, S.; Street, R. A.; Greenhill, J.; Bond, I. A.; Gould, A.; Kubiak, M.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Ulaczyk, K.; Wyrzykowski, L.; Abe, F.; Fukui, A.; Furusawa, K.; Holderness, S.; Itow, Y.; Korpela, A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagayama, T.; Ohnishi, K.; Rattenbury, N.; Saito, To; Sako, T.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Yock, P. C M; Allen, W.; Christie, G. W.; Depoy, D. L.; Gaudi, B. S.; Han, C.; Lee, C. U.; McCormick, J.; Monard, B.; Natusch, T.; Park, B. G.; Pogge, R. W.; Allan, A.; Bode, M.; Bramich, D. M.; Clay, N.; Dominik, M.; Horne, K. D.; Kains, N.; Mottram, C.; Snodgrass, C.; Steele, I.; Tsapras, Y.; Albrow, M. D.; Batista, V.; Beaulieu, J. P.; Brillant, S.; Burgdorf, M.; Caldwell, J. A R; Cassan, A.; Cole, A.; Cook, K. H.; Coutures, Ch; Dieters, S.; Prester, D. Dominis; Donatowicz, J.; Fouqué, P.; Jorgensen, U. G.; Kane, S.; Kubas, D.; Marquette, J. B.; Martin, R.; Menzies, J.; Pollard, K. R.; Sahu, K. C.; Wambsganss, J.; Williams, A.; Zub, M.

In: Astrophysical Journal, Vol. 752, No. 2, 82, 20.06.2012.

Research output: Contribution to journalArticle

Miyake, N, Udalski, A, Sumi, T, Bennett, DP, Dong, S, Street, RA, Greenhill, J, Bond, IA, Gould, A, Kubiak, M, Szymański, MK, Pietrzyński, G, Soszyński, 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, CU, McCormick, J, Monard, B, Natusch, T, Park, BG, 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, Fouqué, 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
Miyake, N. ; Udalski, A. ; Sumi, T. ; Bennett, D. P. ; Dong, S. ; Street, R. A. ; Greenhill, J. ; Bond, I. A. ; Gould, A. ; Kubiak, M. ; Szymański, M. K. ; Pietrzyński, G. ; Soszyński, I. ; Ulaczyk, K. ; Wyrzykowski, L. ; Abe, F. ; Fukui, A. ; Furusawa, K. ; Holderness, S. ; Itow, Y. ; Korpela, A. ; Ling, C. H. ; Masuda, K. ; Matsubara, Y. ; Muraki, Y. ; Nagayama, T. ; Ohnishi, K. ; Rattenbury, N. ; Saito, To ; Sako, T. ; Sullivan, D. J. ; Sweatman, W. L. ; Tristram, P. J. ; Yock, P. C M ; Allen, W. ; Christie, G. W. ; Depoy, D. L. ; Gaudi, B. S. ; Han, C. ; Lee, C. U. ; McCormick, J. ; Monard, B. ; Natusch, T. ; Park, B. G. ; Pogge, R. W. ; Allan, A. ; Bode, M. ; Bramich, D. M. ; Clay, N. ; Dominik, M. ; Horne, K. D. ; Kains, N. ; Mottram, C. ; Snodgrass, C. ; Steele, I. ; Tsapras, Y. ; Albrow, M. D. ; Batista, V. ; Beaulieu, J. P. ; Brillant, S. ; Burgdorf, M. ; Caldwell, J. A R ; Cassan, A. ; Cole, A. ; Cook, K. H. ; Coutures, Ch ; Dieters, S. ; Prester, D. Dominis ; Donatowicz, J. ; Fouqué, P. ; Jorgensen, U. G. ; Kane, S. ; Kubas, D. ; Marquette, J. B. ; Martin, R. ; Menzies, J. ; Pollard, K. R. ; Sahu, K. C. ; Wambsganss, J. ; Williams, A. ; Zub, M. / A possible binary system of a stellar remnant in the high-magnification gravitational microlensing event OGLE-2007-BLG-514. In: Astrophysical Journal. 2012 ; Vol. 752, No. 2.
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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 DL = 3.11 ± 0.39kpc and total mass ML = 1.40 ± 0.18 M ⊙; this leads to the primary and secondary components having masses of M 1 = 1.06 ± 0.13 M ⊙ and M 2 = 0.34 ± 0.04 M ⊙, 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+4.6 -0.3 M ⊙ and it is at a distance of D L = 2.6+3.8 -0.9kpc. Given the secure mass ratio measurement, the companion mass is therefore M 2 = 0.2+1.2 -0.1 M ⊙. 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.",
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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 Szymański, {M. K.} and G. Pietrzyński and I. Soszyński 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. Fouqu{\'e} 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",
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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 - Szymański, M. K.

AU - Pietrzyński, G.

AU - Soszyński, 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 - Fouqué, 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 DL = 3.11 ± 0.39kpc and total mass ML = 1.40 ± 0.18 M ⊙; this leads to the primary and secondary components having masses of M 1 = 1.06 ± 0.13 M ⊙ and M 2 = 0.34 ± 0.04 M ⊙, 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+4.6 -0.3 M ⊙ and it is at a distance of D L = 2.6+3.8 -0.9kpc. Given the secure mass ratio measurement, the companion mass is therefore M 2 = 0.2+1.2 -0.1 M ⊙. 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 DL = 3.11 ± 0.39kpc and total mass ML = 1.40 ± 0.18 M ⊙; this leads to the primary and secondary components having masses of M 1 = 1.06 ± 0.13 M ⊙ and M 2 = 0.34 ± 0.04 M ⊙, 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+4.6 -0.3 M ⊙ and it is at a distance of D L = 2.6+3.8 -0.9kpc. Given the secure mass ratio measurement, the companion mass is therefore M 2 = 0.2+1.2 -0.1 M ⊙. 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

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