Candidate gravitational microlensing events for future direct lens imaging

C. B. Henderson; H. Park; T. Sumi; A. Udalski; A. Gould; Y. Tsapras; C. Han; B. S. Gaudi; V. Bozza; F. Abe; D. P. Bennett; I. A. Bond; C. S. Botzler; M. Freeman; A. Fukui; D. Fukunaga; Y. Itow; N. Koshimoto; C. H. Ling; K. Masuda; Y. Matsubara; Y. Muraki; S. Namba; K. Ohnishi; N. J. Rattenbury; To Saito; D. J. Sullivan; D. Suzuki; W. L. Sweatman; P. J. Tristram; N. Tsurumi; K. Wada; N. Yamai; P. C. M. Yock; A. Yonehara; M. K. Szymanski; M. Kubiak; G. Pietrzynski; I. Soszynski; J. Skowron; S. Kozlowski; R. Poleski; Daniel Martyn Bramich; Paul Browne; Martin Dominik; Keith Douglas Horne; Markus Peter Gerhard Hundertmark; Roberto Jose Figuera Jaimes; Noé Kains; Rachel Amanda Street; MOA Collaboration; OGLE Collaboration; μFUN Collaboration; RoboNet Collaboration

doi:10.1088/0004-637X/794/1/71

Candidate gravitational microlensing events for future direct lens imaging

C. B. Henderson, H. Park, T. Sumi, A. Udalski, A. Gould, Y. Tsapras, C. Han^*, B. S. Gaudi, V. Bozza, F. Abe, D. P. Bennett, I. A. Bond, C. S. Botzler, M. Freeman, A. Fukui, D. Fukunaga, Y. Itow, N. Koshimoto, C. H. Ling, K. MasudaY. Matsubara, Y. Muraki, S. Namba, K. Ohnishi, N. J. Rattenbury, To Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, N. Tsurumi, K. Wada, N. Yamai, P. C. M. Yock, A. Yonehara, M. K. Szymanski, M. Kubiak, G. Pietrzynski, I. Soszynski, J. Skowron, S. Kozlowski, R. Poleski, Daniel Martyn Bramich, Paul Browne, Martin Dominik, Keith Douglas Horne, Markus Peter Gerhard Hundertmark, Roberto Jose Figuera Jaimes, Noé Kains, Rachel Amanda Street, MOA Collaboration, OGLE Collaboration, μFUN Collaboration, RoboNet Collaboration

^*Corresponding author for this work

School of Physics and Astronomy

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

Abstract

The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with μ ≥ 8 mas yr^–1.
Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In ≤12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events.

Original language	English
Article number	71
Number of pages	11
Journal	Astrophysical Journal
Volume	794
Issue number	1
Early online date	24 Sept 2014
DOIs	https://doi.org/10.1088/0004-637X/794/1/71
Publication status	Published - 10 Oct 2014

Keywords

Binaries: general
Gravitational lensing: micro
Galactic bulge
Binary-lens
Chemical evolution
Planetary companion
Orbital motion
Optical depth
Mass planet
Brown dwarf
OGLE-III
Parallax

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10.1088/0004-637X/794/1/71

CandidateEventsImaging
© 2014. 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/794/1/71
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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
Planet population statistics: Planet population statistics from fully-deterministic microlensing campaigns
Dominik, M. (PI)
The Royal Society
1/10/11 → 30/09/15
Project: Fellowship

Cite this

Henderson, C. B., Park, H., Sumi, T., Udalski, A., Gould, A., Tsapras, Y., Han, C., Gaudi, B. S., Bozza, V., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Ling, C. H., ... RoboNet Collaboration (2014). Candidate gravitational microlensing events for future direct lens imaging. Astrophysical Journal, 794(1), Article 71. https://doi.org/10.1088/0004-637X/794/1/71

@article{472d3aefd1c34a5581e90a31c76e40b2,

title = "Candidate gravitational microlensing events for future direct lens imaging",

abstract = "The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with μ ≥ 8 mas yr–1. Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In ≤12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events.",

keywords = "Binaries: general, Gravitational lensing: micro, Galactic bulge, Binary-lens, Chemical evolution, Planetary companion, Orbital motion, Optical depth, Mass planet, Brown dwarf, OGLE-III, Parallax",

author = "Henderson, {C. B.} and H. Park and T. Sumi and A. Udalski and A. Gould and Y. Tsapras and C. Han and Gaudi, {B. S.} and V. Bozza and F. Abe and Bennett, {D. P.} and Bond, {I. A.} and Botzler, {C. S.} and M. Freeman and A. Fukui and D. Fukunaga and Y. Itow and N. Koshimoto and Ling, {C. H.} and K. Masuda and Y. Matsubara and Y. Muraki and S. Namba and K. Ohnishi and Rattenbury, {N. J.} and To Saito and Sullivan, {D. J.} and D. Suzuki and Sweatman, {W. L.} and Tristram, {P. J.} and N. Tsurumi and K. Wada and N. Yamai and Yock, {P. C. M.} and A. Yonehara and Szymanski, {M. K.} and M. Kubiak and G. Pietrzynski and I. Soszynski and J. Skowron and S. Kozlowski and R. Poleski and Bramich, {Daniel Martyn} and Paul Browne and Martin Dominik and Horne, {Keith Douglas} and Hundertmark, {Markus Peter Gerhard} and {Figuera Jaimes}, {Roberto Jose} and No{\'e} Kains and Street, {Rachel Amanda} and {MOA Collaboration} and {OGLE Collaboration} and {μFUN Collaboration} and {RoboNet Collaboration}",

note = "This material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship Program under grant No. DGE-0822215, awarded to C.B.H., and an international travel allowance through the Graduate Research Opportunities Worldwide, also awarded to C.B.H. and taken to Cheongju, Korea. T.S. is supported by the grant JSPS23340044 and JSPS24253004. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471 and from NASA grant NNX12AB99G. 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 J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. M.D., K.H., M.H., C.S., R.A.S., and Y.T. acknowledge grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). This publication was made possible by NPRP grant #X-019-1-006 from the Qatar National Research Fund (a member of the Qatar Foundation). ",

year = "2014",

month = oct,

day = "10",

doi = "10.1088/0004-637X/794/1/71",

language = "English",

volume = "794",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Henderson, CB, Park, H, Sumi, T, Udalski, A, Gould, A, Tsapras, Y, Han, C, Gaudi, BS, Bozza, V, Abe, F, Bennett, DP, Bond, IA, Botzler, CS, Freeman, M, Fukui, A, Fukunaga, D, Itow, Y, Koshimoto, N, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Namba, S, Ohnishi, K, Rattenbury, NJ, Saito, T, Sullivan, DJ, Suzuki, D, Sweatman, WL, Tristram, PJ, Tsurumi, N, Wada, K, Yamai, N, Yock, PCM, Yonehara, A, Szymanski, MK, Kubiak, M, Pietrzynski, G, Soszynski, I, Skowron, J, Kozlowski, S, Poleski, R, Bramich, DM, Browne, P, Dominik, M , Horne, KD, Hundertmark, MPG, Figuera Jaimes, RJ, Kains, N, Street, RA, MOA Collaboration, OGLE Collaboration, μFUN Collaboration & RoboNet Collaboration 2014, 'Candidate gravitational microlensing events for future direct lens imaging', Astrophysical Journal, vol. 794, no. 1, 71. https://doi.org/10.1088/0004-637X/794/1/71

TY - JOUR

T1 - Candidate gravitational microlensing events for future direct lens imaging

AU - Henderson, C. B.

AU - Park, H.

AU - Sumi, T.

AU - Udalski, A.

AU - Gould, A.

AU - Tsapras, Y.

AU - Han, C.

AU - Gaudi, B. S.

AU - Bozza, V.

AU - Abe, F.

AU - Bennett, D. P.

AU - Bond, I. A.

AU - Botzler, C. S.

AU - Freeman, M.

AU - Fukui, A.

AU - Fukunaga, D.

AU - Itow, Y.

AU - Koshimoto, N.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Namba, S.

AU - Ohnishi, K.

AU - Rattenbury, N. J.

AU - Saito, To

AU - Sullivan, D. J.

AU - Suzuki, D.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Tsurumi, N.

AU - Wada, K.

AU - Yamai, N.

AU - Yock, P. C. M.

AU - Yonehara, A.

AU - Szymanski, M. K.

AU - Kubiak, M.

AU - Pietrzynski, G.

AU - Soszynski, I.

AU - Skowron, J.

AU - Kozlowski, S.

AU - Poleski, R.

AU - Bramich, Daniel Martyn

AU - Browne, Paul

AU - Dominik, Martin

AU - Horne, Keith Douglas

AU - Hundertmark, Markus Peter Gerhard

AU - Figuera Jaimes, Roberto Jose

AU - Kains, Noé

AU - Street, Rachel Amanda

AU - MOA Collaboration

AU - OGLE Collaboration

AU - μFUN Collaboration

AU - RoboNet Collaboration

N1 - This material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship Program under grant No. DGE-0822215, awarded to C.B.H., and an international travel allowance through the Graduate Research Opportunities Worldwide, also awarded to C.B.H. and taken to Cheongju, Korea. T.S. is supported by the grant JSPS23340044 and JSPS24253004. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471 and from NASA grant NNX12AB99G. 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 J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. M.D., K.H., M.H., C.S., R.A.S., and Y.T. acknowledge grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). This publication was made possible by NPRP grant #X-019-1-006 from the Qatar National Research Fund (a member of the Qatar Foundation).

PY - 2014/10/10

Y1 - 2014/10/10

N2 - The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with μ ≥ 8 mas yr–1. Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In ≤12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events.

AB - The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with μ ≥ 8 mas yr–1. Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In ≤12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events.

KW - Binaries: general

KW - Gravitational lensing: micro

KW - Galactic bulge

KW - Binary-lens

KW - Chemical evolution

KW - Planetary companion

KW - Orbital motion

KW - Optical depth

KW - Mass planet

KW - Brown dwarf

KW - OGLE-III

KW - Parallax

U2 - 10.1088/0004-637X/794/1/71

DO - 10.1088/0004-637X/794/1/71

M3 - Article

SN - 0004-637X

VL - 794

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 71

ER -

Candidate gravitational microlensing events for future direct lens imaging

Abstract

Keywords

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Projects

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

Planet population statistics: Planet population statistics from fully-deterministic microlensing campaigns

Cite this