Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020

Tianshu Wang; Wei Zhu; Shude Mao; I. A. Bond; A. Gould; A. Udalski; T. Sumi; V. Bozza; C. Ranc; A. Cassan; J. C. Yee; C. Han; F. Abe; Y. Asakura; R. Barry; D. P. Bennett; A. Bhattacharya; M. Donachie; P. Evans; A. Fukui; Y. Hirao; Y. Itow; K. Kawasaki; N. Koshimoto; M. C. A. Li; C. H. Ling; K. Masuda; Y. Matsubara; S. Miyazaki; Y. Muraki; M. Nagakane; K. Ohnishi; N. Rattenbury; To Saito; A. Sharan; H. Shibai; D. J. Sullivan; D. Suzuki; P. J. Tristram; T. Yamada; A. Yonehara; S. KozŁowski; P. Mroz; M. Pawlak; P. Pietrukowicz; R. Poleski; J. Skowron; I. Soszyński; M. K. Szymanski; K. Ulaczyk; C. Beichman; G. Bryden; S. Calchi Novati; S. Carey; M. Fausnaugh; B. S. Gaudi; C. B. Henderson; Y. Shvartzvald; B. Wibking; M. D. Albrow; S. -J. Chung; K. -H. Hwang; Y. K. Jung; Y. -H. Ryu; I. -G. Shin; S. -M. Cha; D. -J. Kim; H. -W. Kim; S. -L. Kim; C. -U. Lee; Y. Yee; B. -G. Park; R. W. Pogge; R. A. Street; Y. Tsapras; M. Hundertmark; E. Bachelet; M. Dominik; K. Horne; R. Figuera Jaimes; J. Wambsganss; D. M. Bramich; R. Schmidt; C. Snodgrass; I. A. Steele; J. Menzies

doi:10.3847/1538-4357/aa813b

Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020

Tianshu Wang, Wei Zhu, Shude Mao, I. A. Bond, A. Gould, A. Udalski, T. Sumi, V. Bozza, C. Ranc, A. Cassan, J. C. Yee, C. Han, F. Abe, Y. Asakura, R. Barry, D. P. Bennett, A. Bhattacharya, M. Donachie, P. Evans, A. FukuiY. Hirao, Y. Itow, K. Kawasaki, N. Koshimoto, M. C. A. Li, C. H. Ling, K. Masuda, Y. Matsubara, S. Miyazaki, Y. Muraki, M. Nagakane, K. Ohnishi, N. Rattenbury, To Saito, A. Sharan, H. Shibai, D. J. Sullivan, D. Suzuki, P. J. Tristram, T. Yamada, A. Yonehara, S. KozŁowski, P. Mroz, M. Pawlak, P. Pietrukowicz, R. Poleski, J. Skowron, I. Soszyński, M. K. Szymanski, K. Ulaczyk, C. Beichman, G. Bryden, S. Calchi Novati, S. Carey, M. Fausnaugh, B. S. Gaudi, C. B. Henderson, Y. Shvartzvald, B. Wibking, M. D. Albrow, S. -J. Chung, K. -H. Hwang, Y. K. Jung, Y. -H. Ryu, I. -G. Shin, S. -M. Cha, D. -J. Kim, H. -W. Kim, S. -L. Kim, C. -U. Lee, Y. Yee, B. -G. Park, R. W. Pogge, R. A. Street, Y. Tsapras, M. Hundertmark, E. Bachelet, M. Dominik, K. Horne, R. Figuera Jaimes, J. Wambsganss, D. M. Bramich, R. Schmidt, C. Snodgrass, I. A. Steele, J. Menzies

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

Abstract

We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (~63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses M₁= 0.606 ± 0.028 M_⊙ and M₂= 0.125 ± 0.006 M⊙ in the Galactic disk. Assuming that the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance D_L= 2.44 ± 0.10 kpc. We also provide a summary and short discussion of all of the published microlensing events in which the annual parallax effect is confirmed by other independent observations.

Original language	English
Article number	129
Number of pages	11
Journal	Astrophysical Journal
Volume	845
Issue number	2
Early online date	18 Aug 2017
DOIs	https://doi.org/10.3847/1538-4357/aa813b
Publication status	Published - 20 Aug 2017

Keywords

Binaries: general
Galaxy: bulge
Gravitational lensing: micro

Access to Document

10.3847/1538-4357/aa813b

Wang-2017-Ground-based-APJ-AAM
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org / https://doi.org/10.3847/1538-4357/aa813b
Accepted author manuscript, 11.2 MB

Cite this

Wang, T., Zhu, W., Mao, S., Bond, I. A., Gould, A., Udalski, A., Sumi, T., Bozza, V., Ranc, C., Cassan, A., Yee, J. C., Han, C., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., ... Menzies, J. (2017). Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020. Astrophysical Journal, 845(2), Article 129. https://doi.org/10.3847/1538-4357/aa813b

@article{df21f40bb1164c40a3b1323c8eef32cd,

title = "Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020",

abstract = "We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (~63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses M1 = 0.606 ± 0.028 M⊙ and M2 = 0.125 ± 0.006 M⊙ in the Galactic disk. Assuming that the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance DL = 2.44 ± 0.10 kpc. We also provide a summary and short discussion of all of the published microlensing events in which the annual parallax effect is confirmed by other independent observations.",

keywords = "Binaries: general, Galaxy: bulge, Gravitational lensing: micro",

author = "Tianshu Wang and Wei Zhu and Shude Mao and Bond, {I. A.} and A. Gould and A. Udalski and T. Sumi and V. Bozza and C. Ranc and A. Cassan and Yee, {J. C.} and C. Han and F. Abe and Y. Asakura and R. Barry and Bennett, {D. P.} and A. Bhattacharya and M. Donachie and P. Evans and A. Fukui and Y. Hirao and Y. Itow and K. Kawasaki and N. Koshimoto and Li, {M. C. A.} and Ling, {C. H.} and K. Masuda and Y. Matsubara and S. Miyazaki and Y. Muraki and M. Nagakane and K. Ohnishi and N. Rattenbury and To Saito and A. Sharan and H. Shibai and Sullivan, {D. J.} and D. Suzuki and Tristram, {P. J.} and T. Yamada and A. Yonehara and S. Koz{\L}owski and P. Mroz and M. Pawlak and P. Pietrukowicz and R. Poleski and J. Skowron and I. Soszy{\'n}ski and Szymanski, {M. K.} and K. Ulaczyk and C. Beichman and G. Bryden and Novati, {S. Calchi} and S. Carey and M. Fausnaugh and Gaudi, {B. S.} and Henderson, {C. B.} and Y. Shvartzvald and B. Wibking and Albrow, {M. D.} and Chung, {S. -J.} and Hwang, {K. -H.} and Jung, {Y. K.} and Ryu, {Y. -H.} and Shin, {I. -G.} and Cha, {S. -M.} and Kim, {D. -J.} and Kim, {H. -W.} and Kim, {S. -L.} and Lee, {C. -U.} and Y. Yee and Park, {B. -G.} and Pogge, {R. W.} and Street, {R. A.} and Y. Tsapras and M. Hundertmark and E. Bachelet and M. Dominik and K. Horne and Jaimes, {R. Figuera} and J. Wambsganss and Bramich, {D. M.} and R. Schmidt and C. Snodgrass and Steele, {I. A.} and J. Menzies",

year = "2017",

month = aug,

day = "20",

doi = "10.3847/1538-4357/aa813b",

language = "English",

volume = "845",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Wang, T, Zhu, W, Mao, S, Bond, IA, Gould, A, Udalski, A, Sumi, T, Bozza, V, Ranc, C, Cassan, A, Yee, JC, Han, C, Abe, F, Asakura, Y, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Evans, P, Fukui, A, Hirao, Y, Itow, Y, Kawasaki, K, Koshimoto, N, Li, MCA, Ling, CH, Masuda, K, Matsubara, Y, Miyazaki, S, Muraki, Y, Nagakane, M, Ohnishi, K, Rattenbury, N, Saito, T, Sharan, A, Shibai, H, Sullivan, DJ, Suzuki, D, Tristram, PJ, Yamada, T, Yonehara, A, KozŁowski, S, Mroz, P, Pawlak, M, Pietrukowicz, P, Poleski, R, Skowron, J, Soszyński, I, Szymanski, MK, Ulaczyk, K, Beichman, C, Bryden, G, Novati, SC, Carey, S, Fausnaugh, M, Gaudi, BS, Henderson, CB, Shvartzvald, Y, Wibking, B, Albrow, MD, Chung, S-J, Hwang, K-H, Jung, YK, Ryu, Y-H, Shin, I-G, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, C-U, Yee, Y, Park, B-G, Pogge, RW, Street, RA, Tsapras, Y, Hundertmark, M, Bachelet, E, Dominik, M , Horne, K, Jaimes, RF, Wambsganss, J, Bramich, DM, Schmidt, R, Snodgrass, C, Steele, IA & Menzies, J 2017, 'Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020', Astrophysical Journal, vol. 845, no. 2, 129. https://doi.org/10.3847/1538-4357/aa813b

TY - JOUR

T1 - Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020

AU - Wang, Tianshu

AU - Zhu, Wei

AU - Mao, Shude

AU - Bond, I. A.

AU - Gould, A.

AU - Udalski, A.

AU - Sumi, T.

AU - Bozza, V.

AU - Ranc, C.

AU - Cassan, A.

AU - Yee, J. C.

AU - Han, C.

AU - Abe, F.

AU - Asakura, Y.

AU - Barry, R.

AU - Bennett, D. P.

AU - Bhattacharya, A.

AU - Donachie, M.

AU - Evans, P.

AU - Fukui, A.

AU - Hirao, Y.

AU - Itow, Y.

AU - Kawasaki, K.

AU - Koshimoto, N.

AU - Li, M. C. A.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyazaki, S.

AU - Muraki, Y.

AU - Nagakane, M.

AU - Ohnishi, K.

AU - Rattenbury, N.

AU - Saito, To

AU - Sharan, A.

AU - Shibai, H.

AU - Sullivan, D. J.

AU - Suzuki, D.

AU - Tristram, P. J.

AU - Yamada, T.

AU - Yonehara, A.

AU - KozŁowski, S.

AU - Mroz, P.

AU - Pawlak, M.

AU - Pietrukowicz, P.

AU - Poleski, R.

AU - Skowron, J.

AU - Soszyński, I.

AU - Szymanski, M. K.

AU - Ulaczyk, K.

AU - Beichman, C.

AU - Bryden, G.

AU - Novati, S. Calchi

AU - Carey, S.

AU - Fausnaugh, M.

AU - Gaudi, B. S.

AU - Henderson, C. B.

AU - Shvartzvald, Y.

AU - Wibking, B.

AU - Albrow, M. D.

AU - Chung, S. -J.

AU - Hwang, K. -H.

AU - Jung, Y. K.

AU - Ryu, Y. -H.

AU - Shin, I. -G.

AU - Cha, S. -M.

AU - Kim, D. -J.

AU - Kim, H. -W.

AU - Kim, S. -L.

AU - Lee, C. -U.

AU - Yee, Y.

AU - Park, B. -G.

AU - Pogge, R. W.

AU - Street, R. A.

AU - Tsapras, Y.

AU - Hundertmark, M.

AU - Bachelet, E.

AU - Dominik, M.

AU - Horne, K.

AU - Jaimes, R. Figuera

AU - Wambsganss, J.

AU - Bramich, D. M.

AU - Schmidt, R.

AU - Snodgrass, C.

AU - Steele, I. A.

AU - Menzies, J.

PY - 2017/8/20

Y1 - 2017/8/20

N2 - We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (~63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses M1 = 0.606 ± 0.028 M⊙ and M2 = 0.125 ± 0.006 M⊙ in the Galactic disk. Assuming that the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance DL = 2.44 ± 0.10 kpc. We also provide a summary and short discussion of all of the published microlensing events in which the annual parallax effect is confirmed by other independent observations.

AB - We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (~63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses M1 = 0.606 ± 0.028 M⊙ and M2 = 0.125 ± 0.006 M⊙ in the Galactic disk. Assuming that the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance DL = 2.44 ± 0.10 kpc. We also provide a summary and short discussion of all of the published microlensing events in which the annual parallax effect is confirmed by other independent observations.

KW - Binaries: general

KW - Galaxy: bulge

KW - Gravitational lensing: micro

U2 - 10.3847/1538-4357/aa813b

DO - 10.3847/1538-4357/aa813b

M3 - Article

SN - 0004-637X

VL - 845

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 129

ER -

Ground-based parallax confirmed by Spitzer. Binary microlensing event MOA-2015-BLG-020

Abstract

Keywords

Access to Document

Fingerprint

Cite this