Spitzer microlens measurement of a massive remnant in a well-separated binary

Y. Shvartzvald; A. Udalski; A. Gould; C. Han; V. Bozza; M. Friedmann; Markus Peter Gerhard Hundertmark; C. Beichman; G. Bryden; S. Calchi Novati; S. Carey; M. Fausnaugh; B. S. Gaudi; C. B. Henderson; T. Kerr; R. W. Pogge; W. Varricatt; B. Wibking; J. C. Yee; W. Zhu; R. Poleski; M. Pawlak; M. K. Szymański; J. Skowron; P. Mróz; S. Kozłowski; Ł. Wyrzykowski; P. Pietrukowicz; G. Pietrzyński; I. Soszyński; K. Ulaczyk; J.-Y. Choi; H. Park; Y. K. Jung; I.-G. Shin; M. D. Albrow; B.-G. Park; S.-L. Kim; C.-U. Lee; S.-M. Cha; D.-J. Kim; Y. Lee; D. Maoz; S. Kaspi; R. A. Street; Y. Tsapras; E. Bachelet; Martin Dominik; D. M. Bramich; Keith Douglas Horne; C. Snodgrass; I. A. Steele; J. Menzies; Roberto Jose Figuera Jaimes; J. Wambsganss; R. Schmidt; A. Cassan; C. Ranc; S. Mao; Subo Dong; G. D’Ago; G. Scarpetta; P. Verma; U. G. Jørgensen; E. Kerins; J. Skottfelt

doi:10.1088/0004-637X/814/2/111

Spitzer microlens measurement of a massive remnant in a well-separated binary

Y. Shvartzvald, A. Udalski, A. Gould, C. Han, V. Bozza, M. Friedmann, Markus Peter Gerhard Hundertmark, C. Beichman, G. Bryden, S. Calchi Novati, S. Carey, M. Fausnaugh, B. S. Gaudi, C. B. Henderson, T. Kerr, R. W. Pogge, W. Varricatt, B. Wibking, J. C. Yee, W. ZhuR. Poleski, M. Pawlak, M. K. Szymański, J. Skowron, P. Mróz, S. Kozłowski, Ł. Wyrzykowski, P. Pietrukowicz, G. Pietrzyński, I. Soszyński, K. Ulaczyk, J.-Y. Choi, H. Park, Y. K. Jung, I.-G. Shin, M. D. Albrow, B.-G. Park, S.-L. Kim, C.-U. Lee, S.-M. Cha, D.-J. Kim, Y. Lee, D. Maoz, S. Kaspi, R. A. Street, Y. Tsapras, E. Bachelet, Martin Dominik, D. M. Bramich, Keith Douglas Horne, C. Snodgrass, I. A. Steele, J. Menzies, Roberto Jose Figuera Jaimes, J. Wambsganss, R. Schmidt, A. Cassan, C. Ranc, S. Mao, Subo Dong, G. D’Ago, G. Scarpetta, P. Verma, U. G. Jørgensen, E. Kerins, J. Skottfelt

School of Physics and Astronomy

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Abstract

We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the “microlens parallax” effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.

Original language	English
Pages (from-to)	111
Journal	Astrophysical Journal
Volume	814
Issue number	2
Early online date	23 Nov 2015
DOIs	https://doi.org/10.1088/0004-637X/814/2/111
Publication status	Published - 1 Dec 2015

Keywords

Binaries: general
Black hole physics
Galaxy: bulge
Gravitational lensing: micro
Stars: neutron

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10.1088/0004-637X/814/2/111

Dominik_2015_TAJ_SpitzerMicrolens
© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/0004-637X/814/2/111.
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http://adsabs.harvard.edu/abs/2015ApJ...814..111S

Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018
Jardine, M. M. (PI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Horne, K. D. (CoI) & Wood, K. (CoI)
Science & Technology Facilities Council
1/04/15 → 31/03/18
Project: Standard
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

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Shvartzvald, Y., Udalski, A., Gould, A., Han, C., Bozza, V., Friedmann, M., Hundertmark, M. P. G., Beichman, C., Bryden, G., Novati, S. C., Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, C. B., Kerr, T., Pogge, R. W., Varricatt, W., Wibking, B., Yee, J. C., ... Skottfelt, J. (2015). Spitzer microlens measurement of a massive remnant in a well-separated binary. Astrophysical Journal, 814(2), 111. https://doi.org/10.1088/0004-637X/814/2/111

@article{49bc8ce1a0a44debb416cadebe38ae0b,

title = "Spitzer microlens measurement of a massive remnant in a well-separated binary",

abstract = "We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the “microlens parallax” effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.",

keywords = "Binaries: general, Black hole physics, Galaxy: bulge, Gravitational lensing: micro, Stars: neutron",

author = "Y. Shvartzvald and A. Udalski and A. Gould and C. Han and V. Bozza and M. Friedmann and Hundertmark, {Markus Peter Gerhard} 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 T. Kerr and Pogge, {R. W.} and W. Varricatt and B. Wibking and Yee, {J. C.} and W. Zhu and R. Poleski and M. Pawlak and Szyma{\'n}ski, {M. K.} and J. Skowron and P. Mr{\'o}z and S. Koz{\l}owski and {\L}. Wyrzykowski and P. Pietrukowicz and G. Pietrzy{\'n}ski and I. Soszy{\'n}ski and K. Ulaczyk and J.-Y. Choi and H. Park and Jung, {Y. K.} and I.-G. Shin and Albrow, {M. D.} and B.-G. Park and S.-L. Kim and C.-U. Lee and S.-M. Cha and D.-J. Kim and Y. Lee and D. Maoz and S. Kaspi and Street, {R. A.} and Y. Tsapras and E. Bachelet and Martin Dominik and Bramich, {D. M.} and Horne, {Keith Douglas} and C. Snodgrass and Steele, {I. A.} and J. Menzies and {Figuera Jaimes}, {Roberto Jose} and J. Wambsganss and R. Schmidt and A. Cassan and C. Ranc and S. Mao and Subo Dong and G. D{\textquoteright}Ago and G. Scarpetta and P. Verma and J{\o}rgensen, {U. G.} and E. Kerins and J. Skottfelt",

note = "Work by Y.S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. L.W. acknowledges support from the Polish NCN Harmonia grant No. 2012/06/M/ST9/00172. D.M. and A.G. acknowledge support by a grant from the US Israel Binational Science Foundation. Work by D.M. is supported by the I-CORE program of the Israel Science Foundation and the Planning and Budgeting Committee. This publication was made possible by NPRP grant # X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). S.D. is supported by {"}the Strategic Priority Research Program—The Emergence of Cosmological Structures{"} of the Chinese Academy of Sciences (grant No. XDB09000000). Work by S.M. has been supported by the Strategic Priority Research Program {"}The Emergence of Cosmological Structures{"} of the Chinese Academy of Sciences Grant No. XDB09000000, and by the National Natural Science Foundation of China (NSFC) under grant numbers 11333003 and 11390372. M.P.G.H. acknowledges support from the Villum Foundation. ",

year = "2015",

month = dec,

day = "1",

doi = "10.1088/0004-637X/814/2/111",

language = "English",

volume = "814",

pages = "111",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

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Shvartzvald, Y, Udalski, A, Gould, A, Han, C, Bozza, V, Friedmann, M, Hundertmark, MPG, Beichman, C, Bryden, G, Novati, SC, Carey, S, Fausnaugh, M, Gaudi, BS, Henderson, CB, Kerr, T, Pogge, RW, Varricatt, W, Wibking, B, Yee, JC, Zhu, W, Poleski, R, Pawlak, M, Szymański, MK, Skowron, J, Mróz, P, Kozłowski, S, Wyrzykowski, Ł, Pietrukowicz, P, Pietrzyński, G, Soszyński, I, Ulaczyk, K, Choi, J-Y, Park, H, Jung, YK, Shin, I-G, Albrow, MD, Park, B-G, Kim, S-L, Lee, C-U, Cha, S-M, Kim, D-J, Lee, Y, Maoz, D, Kaspi, S, Street, RA, Tsapras, Y, Bachelet, E, Dominik, M, Bramich, DM, Horne, KD, Snodgrass, C, Steele, IA, Menzies, J, Figuera Jaimes, RJ, Wambsganss, J, Schmidt, R, Cassan, A, Ranc, C, Mao, S, Dong, S, D’Ago, G, Scarpetta, G, Verma, P, Jørgensen, UG, Kerins, E & Skottfelt, J 2015, 'Spitzer microlens measurement of a massive remnant in a well-separated binary', Astrophysical Journal, vol. 814, no. 2, pp. 111. https://doi.org/10.1088/0004-637X/814/2/111

TY - JOUR

T1 - Spitzer microlens measurement of a massive remnant in a well-separated binary

AU - Shvartzvald, Y.

AU - Udalski, A.

AU - Gould, A.

AU - Han, C.

AU - Bozza, V.

AU - Friedmann, M.

AU - Hundertmark, Markus Peter Gerhard

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 - Kerr, T.

AU - Pogge, R. W.

AU - Varricatt, W.

AU - Wibking, B.

AU - Yee, J. C.

AU - Zhu, W.

AU - Poleski, R.

AU - Pawlak, M.

AU - Szymański, M. K.

AU - Skowron, J.

AU - Mróz, P.

AU - Kozłowski, S.

AU - Wyrzykowski, Ł.

AU - Pietrukowicz, P.

AU - Pietrzyński, G.

AU - Soszyński, I.

AU - Ulaczyk, K.

AU - Choi, J.-Y.

AU - Park, H.

AU - Jung, Y. K.

AU - Shin, I.-G.

AU - Albrow, M. D.

AU - Park, B.-G.

AU - Kim, S.-L.

AU - Lee, C.-U.

AU - Cha, S.-M.

AU - Kim, D.-J.

AU - Lee, Y.

AU - Maoz, D.

AU - Kaspi, S.

AU - Street, R. A.

AU - Tsapras, Y.

AU - Bachelet, E.

AU - Dominik, Martin

AU - Bramich, D. M.

AU - Horne, Keith Douglas

AU - Snodgrass, C.

AU - Steele, I. A.

AU - Menzies, J.

AU - Figuera Jaimes, Roberto Jose

AU - Wambsganss, J.

AU - Schmidt, R.

AU - Cassan, A.

AU - Ranc, C.

AU - Mao, S.

AU - Dong, Subo

AU - D’Ago, G.

AU - Scarpetta, G.

AU - Verma, P.

AU - Jørgensen, U. G.

AU - Kerins, E.

AU - Skottfelt, J.

N1 - Work by Y.S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. L.W. acknowledges support from the Polish NCN Harmonia grant No. 2012/06/M/ST9/00172. D.M. and A.G. acknowledge support by a grant from the US Israel Binational Science Foundation. Work by D.M. is supported by the I-CORE program of the Israel Science Foundation and the Planning and Budgeting Committee. This publication was made possible by NPRP grant # X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). S.D. is supported by "the Strategic Priority Research Program—The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant No. XDB09000000). Work by S.M. has been supported by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences Grant No. XDB09000000, and by the National Natural Science Foundation of China (NSFC) under grant numbers 11333003 and 11390372. M.P.G.H. acknowledges support from the Villum Foundation.

PY - 2015/12/1

Y1 - 2015/12/1

N2 - We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the “microlens parallax” effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.

AB - We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the “microlens parallax” effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.

KW - Binaries: general

KW - Black hole physics

KW - Galaxy: bulge

KW - Gravitational lensing: micro

KW - Stars: neutron

U2 - 10.1088/0004-637X/814/2/111

DO - 10.1088/0004-637X/814/2/111

M3 - Article

SN - 0004-637X

VL - 814

SP - 111

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

Spitzer microlens measurement of a massive remnant in a well-separated binary

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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

Astrophysics at St Andrews:2012 - 2014: Astrophysics at St Andrews: 2012 - 2014

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