OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis

Y. H. Ryu; C. Han; K. H. Hwang; R. Street; A. Udalski; T. Sumi; A. Fukui; J. P. Beaulieu; A. Gould; M. Dominik; F. Abe; D. P. Bennett; I. A. Bond; C. S. Botzler; K. Furusawa; F. Hayashi; J. B. Hearnshaw; S. Hosaka; Y. Itow; K. Kamiya; P. M. Kilmartin; A. Korpela; W. Lin; C. H. Ling; S. Makita; K. Masuda; Y. Matsubara; N. Miyake; Y. Muraki; K. Nishimoto; K. Ohnishi; Y. C. Perrott; N. Rattenbury; To Saito; L. Skuljan; D. J. Sullivan; D. Suzuki; W. L. Sweatman; P. J. Tristram; K. Wada; P. C.M. Yock; M. K. Szymański; M. Kubiak; G. Pietrzyński; R. Poleski; I. Soszyński; O. Szewczyk; Wyrzykowski; K. Ulaczyk; M. Bos; G. W. Christie; D. L. Depoy; A. Gal-Yam; B. S. Gaudi; S. Kaspi; C. U. Lee; D. Maoz; J. McCormick; B. Monard; D. Moorhouse; R. W. Pogge; D. Polishook; Y. Shvartzvald; A. Shporer; G. Thornley; J. C. Yee; M. D. Albrow; V. Batista; S. Brillant; A. Cassan; A. Cole; E. Corrales; Ch Coutures; S. Dieters; P. Fouqué; J. Greenhill; J. Menzies; A. Allan; D. M. Bramich; P. Browne; K. Horne; N. Kains; C. Snodgrass; I. Steele; Y. Tsapras; V. Bozza; M. J. Burgdorf; S. Calchi Novati; S. Dreizler; F. Finet; M. Glitrup; F. Grundahl; K. Harpsøe; F. V. Hessman; T. C. Hinse; M. Hundertmark; U. G. Jørgensen; C. Liebig; G. Maier; L. Mancini; M. Mathiasen; S. Rahvar; D. Ricci; G. Scarpetta; J. Skottfelt; J. Surdej; J. Southworth; J. Wambsganss; F. Zimmer

doi:10.1088/0004-637X/723/1/81

OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis

Y. H. Ryu, C. Han, K. H. Hwang, R. Street, A. Udalski, T. Sumi, A. Fukui, J. P. Beaulieu, A. Gould, M. Dominik, F. Abe, D. P. Bennett, I. A. Bond, C. S. Botzler, K. Furusawa, F. Hayashi, J. B. Hearnshaw, S. Hosaka, Y. Itow, K. KamiyaP. M. Kilmartin, A. Korpela, W. Lin, C. H. Ling, S. Makita, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Nishimoto, K. Ohnishi, Y. C. Perrott, N. Rattenbury, To Saito, L. Skuljan, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C.M. Yock, M. K. Szymański, M. Kubiak, G. Pietrzyński, R. Poleski, I. Soszyński, O. Szewczyk, Wyrzykowski, K. Ulaczyk, M. Bos, G. W. Christie, D. L. Depoy, A. Gal-Yam, B. S. Gaudi, S. Kaspi, C. U. Lee, D. Maoz, J. McCormick, B. Monard, D. Moorhouse, R. W. Pogge, D. Polishook, Y. Shvartzvald, A. Shporer, G. Thornley, J. C. Yee, M. D. Albrow, V. Batista, S. Brillant, A. Cassan, A. Cole, E. Corrales, Ch Coutures, S. Dieters, P. Fouqué, J. Greenhill, J. Menzies, A. Allan, D. M. Bramich, P. Browne, K. Horne, N. Kains, C. Snodgrass, I. Steele, Y. Tsapras, V. Bozza, M. J. Burgdorf, S. Calchi Novati, S. Dreizler, F. Finet, M. Glitrup, F. Grundahl, K. Harpsøe, F. V. Hessman, T. C. Hinse, M. Hundertmark, U. G. Jørgensen, C. Liebig, G. Maier, L. Mancini, M. Mathiasen, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, J. Surdej, J. Southworth, J. Wambsganss, F. Zimmer

School of Physics and Astronomy

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Abstract

We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ∼100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events.With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system.We find that the event occurred on a bulge clump giant and itwas produced by a binary lens composed of a K- and M-type main-sequence stars. The estimated masses of the binary components are M₁ = 0.69±0.11M_⊙ and M₂ = 0.36±0.06M⊙, respectively, and they are separated in projection by r⊥ = 10.9±1.3AU. The measured distance to the lens is D_L = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system.

Original language	English
Pages (from-to)	81-88
Number of pages	8
Journal	Astrophysical Journal
Volume	723
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/723/1/81
State	Published - 1 Nov 2010

Keywords

Gravitational lensing: micro

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10.1088/0004-637X/723/1/81

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Ryu, Y. H., Han, C., Hwang, K. H., Street, R., Udalski, A., Sumi, T., Fukui, A., Beaulieu, J. P., Gould, A., Dominik, M., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., ... Zimmer, F. (2010). OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis. Astrophysical Journal, 723(1), 81-88. https://doi.org/10.1088/0004-637X/723/1/81

@article{cdb4d2020e554d0895c4370a980e891f,

title = "OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis",

abstract = "We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ∼100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events.With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system.We find that the event occurred on a bulge clump giant and itwas produced by a binary lens composed of a K- and M-type main-sequence stars. The estimated masses of the binary components are M1 = 0.69±0.11M⊙ and M2 = 0.36±0.06M⊙, respectively, and they are separated in projection by r⊥ = 10.9±1.3AU. The measured distance to the lens is DL = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system.",

keywords = "Gravitational lensing: micro",

author = "Ryu, {Y. H.} and C. Han and Hwang, {K. H.} and R. Street and A. Udalski and T. Sumi and A. Fukui and Beaulieu, {J. P.} and A. Gould and M. Dominik and F. Abe and Bennett, {D. P.} and Bond, {I. A.} and Botzler, {C. S.} and K. Furusawa and F. Hayashi and Hearnshaw, {J. B.} and S. Hosaka and Y. Itow and K. Kamiya and Kilmartin, {P. M.} and A. Korpela and W. Lin and Ling, {C. H.} and S. Makita and K. Masuda and Y. Matsubara and N. Miyake and Y. Muraki and K. Nishimoto and K. Ohnishi and Perrott, {Y. C.} and N. Rattenbury and To Saito and L. Skuljan and Sullivan, {D. J.} and D. Suzuki and Sweatman, {W. L.} and Tristram, {P. J.} and K. Wada and Yock, {P. C.M.} and Szyma{\'n}ski, {M. K.} and M. Kubiak and G. Pietrzy{\'n}ski and R. Poleski and I. Soszy{\'n}ski and O. Szewczyk and Wyrzykowski and K. Ulaczyk and M. Bos and Christie, {G. W.} and Depoy, {D. L.} and A. Gal-Yam and Gaudi, {B. S.} and S. Kaspi and Lee, {C. U.} and D. Maoz and J. McCormick and B. Monard and D. Moorhouse and Pogge, {R. W.} and D. Polishook and Y. Shvartzvald and A. Shporer and G. Thornley and Yee, {J. C.} and Albrow, {M. D.} and V. Batista and S. Brillant and A. Cassan and A. Cole and E. Corrales and Ch Coutures and S. Dieters and P. Fouqu{\'e} and J. Greenhill and J. Menzies and A. Allan and Bramich, {D. M.} and P. Browne and K. Horne and N. Kains and C. Snodgrass and I. Steele and Y. Tsapras and V. Bozza and Burgdorf, {M. J.} and Novati, {S. Calchi} and S. Dreizler and F. Finet and M. Glitrup and F. Grundahl and K. Harps{\o}e and Hessman, {F. V.} and Hinse, {T. C.} and M. Hundertmark and J{\o}rgensen, {U. G.} and C. Liebig and G. Maier and L. Mancini and M. Mathiasen and S. Rahvar and D. Ricci and G. Scarpetta and J. Skottfelt and J. Surdej and J. Southworth and J. Wambsganss and F. Zimmer",

year = "2010",

month = nov,

day = "1",

doi = "10.1088/0004-637X/723/1/81",

language = "אנגלית",

volume = "723",

pages = "81--88",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

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Ryu, YH, Han, C, Hwang, KH, Street, R, Udalski, A, Sumi, T, Fukui, A, Beaulieu, JP, Gould, A, Dominik, M, Abe, F, Bennett, DP, Bond, IA, Botzler, CS, Furusawa, K, Hayashi, F, Hearnshaw, JB, Hosaka, S, Itow, Y, Kamiya, K, Kilmartin, PM, Korpela, A, Lin, W, Ling, CH, Makita, S, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Nishimoto, K, Ohnishi, K, Perrott, YC, Rattenbury, N, Saito, T, Skuljan, L, Sullivan, DJ, Suzuki, D, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Szymański, MK, Kubiak, M, Pietrzyński, G, Poleski, R, Soszyński, I, Szewczyk, O, Wyrzykowski, Ulaczyk, K, Bos, M, Christie, GW, Depoy, DL, Gal-Yam, A, Gaudi, BS, Kaspi, S, Lee, CU, Maoz, D, McCormick, J, Monard, B, Moorhouse, D, Pogge, RW, Polishook, D, Shvartzvald, Y, Shporer, A, Thornley, G, Yee, JC, Albrow, MD, Batista, V, Brillant, S, Cassan, A, Cole, A, Corrales, E, Coutures, C, Dieters, S, Fouqué, P, Greenhill, J, Menzies, J, Allan, A, Bramich, DM, Browne, P, Horne, K, Kains, N, Snodgrass, C, Steele, I, Tsapras, Y, Bozza, V, Burgdorf, MJ, Novati, SC, Dreizler, S, Finet, F, Glitrup, M, Grundahl, F, Harpsøe, K, Hessman, FV, Hinse, TC, Hundertmark, M, Jørgensen, UG, Liebig, C, Maier, G, Mancini, L, Mathiasen, M, Rahvar, S, Ricci, D, Scarpetta, G, Skottfelt, J, Surdej, J, Southworth, J, Wambsganss, J & Zimmer, F 2010, 'OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis', Astrophysical Journal, vol. 723, no. 1, pp. 81-88. https://doi.org/10.1088/0004-637X/723/1/81

TY - JOUR

T1 - OGLE-2009-BLG-092/MOA-2009-BLG-137

T2 - A dramatic repeating event with the second perturbation predicted by real-time analysis

AU - Ryu, Y. H.

AU - Han, C.

AU - Hwang, K. H.

AU - Street, R.

AU - Udalski, A.

AU - Sumi, T.

AU - Fukui, A.

AU - Beaulieu, J. P.

AU - Gould, A.

AU - Dominik, M.

AU - Abe, F.

AU - Bennett, D. P.

AU - Bond, I. A.

AU - Botzler, C. S.

AU - Furusawa, K.

AU - Hayashi, F.

AU - Hearnshaw, J. B.

AU - Hosaka, S.

AU - Itow, Y.

AU - Kamiya, K.

AU - Kilmartin, P. M.

AU - Korpela, A.

AU - Lin, W.

AU - Ling, C. H.

AU - Makita, S.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Muraki, Y.

AU - Nishimoto, K.

AU - Ohnishi, K.

AU - Perrott, Y. C.

AU - Rattenbury, N.

AU - Saito, To

AU - Skuljan, L.

AU - Sullivan, D. J.

AU - Suzuki, D.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Wada, K.

AU - Yock, P. C.M.

AU - Szymański, M. K.

AU - Kubiak, M.

AU - Pietrzyński, G.

AU - Poleski, R.

AU - Soszyński, I.

AU - Szewczyk, O.

AU - Wyrzykowski,

AU - Ulaczyk, K.

AU - Bos, M.

AU - Christie, G. W.

AU - Depoy, D. L.

AU - Gal-Yam, A.

AU - Gaudi, B. S.

AU - Kaspi, S.

AU - Lee, C. U.

AU - Maoz, D.

AU - McCormick, J.

AU - Monard, B.

AU - Moorhouse, D.

AU - Pogge, R. W.

AU - Polishook, D.

AU - Shvartzvald, Y.

AU - Shporer, A.

AU - Thornley, G.

AU - Yee, J. C.

AU - Albrow, M. D.

AU - Batista, V.

AU - Brillant, S.

AU - Cassan, A.

AU - Cole, A.

AU - Corrales, E.

AU - Coutures, Ch

AU - Dieters, S.

AU - Fouqué, P.

AU - Greenhill, J.

AU - Menzies, J.

AU - Allan, A.

AU - Bramich, D. M.

AU - Browne, P.

AU - Horne, K.

AU - Kains, N.

AU - Snodgrass, C.

AU - Steele, I.

AU - Tsapras, Y.

AU - Bozza, V.

AU - Burgdorf, M. J.

AU - Novati, S. Calchi

AU - Dreizler, S.

AU - Finet, F.

AU - Glitrup, M.

AU - Grundahl, F.

AU - Harpsøe, K.

AU - Hessman, F. V.

AU - Hinse, T. C.

AU - Hundertmark, M.

AU - Jørgensen, U. G.

AU - Liebig, C.

AU - Maier, G.

AU - Mancini, L.

AU - Mathiasen, M.

AU - Rahvar, S.

AU - Ricci, D.

AU - Scarpetta, G.

AU - Skottfelt, J.

AU - Surdej, J.

AU - Southworth, J.

AU - Wambsganss, J.

AU - Zimmer, F.

PY - 2010/11/1

Y1 - 2010/11/1

N2 - We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ∼100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events.With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system.We find that the event occurred on a bulge clump giant and itwas produced by a binary lens composed of a K- and M-type main-sequence stars. The estimated masses of the binary components are M1 = 0.69±0.11M⊙ and M2 = 0.36±0.06M⊙, respectively, and they are separated in projection by r⊥ = 10.9±1.3AU. The measured distance to the lens is DL = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system.

AB - We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ∼100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events.With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system.We find that the event occurred on a bulge clump giant and itwas produced by a binary lens composed of a K- and M-type main-sequence stars. The estimated masses of the binary components are M1 = 0.69±0.11M⊙ and M2 = 0.36±0.06M⊙, respectively, and they are separated in projection by r⊥ = 10.9±1.3AU. The measured distance to the lens is DL = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system.

KW - Gravitational lensing: micro

UR - http://www.scopus.com/inward/record.url?scp=78349234630&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/723/1/81

DO - 10.1088/0004-637X/723/1/81

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

AN - SCOPUS:78349234630

VL - 723

SP - 81

EP - 88

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -

OGLE-2009-BLG-092/MOA-2009-BLG-137: A dramatic repeating event with the second perturbation predicted by real-time analysis

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