OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★

V. Bozza; M. Dominik; N. J. Rattenbury; U. G. Jørgensen; Y. Tsapras; D. M. Bramich; A. Udalski; I. A. Bond; C. Liebig; A. Cassan; P. Fouqué; A. Fukui; M. Hundertmark; I.‐G. Shin; S. H. Lee; J.‐Y. Choi; S.‐Y. Park; A. Gould; A. Allan; S. Mao; Ł. Wyrzykowski; R. A. Street; D. Buckley; T. Nagayama; M. Mathiasen; T. C. Hinse; S. Calchi Novati; K. Harpsøe; L. Mancini; G. Scarpetta; T. Anguita; M. J. Burgdorf; K. Horne; Allan Hornstrup; N. Kains; E. Kerins; P. Kjærgaard; G. Masi; S. Rahvar; D. Ricci; C. Snodgrass; J. Southworth; I. A. Steele; J. Surdej; C. C. Thöne; J. Wambsganss; M. Zub; M. D. Albrow; V. Batista; J.‐P. Beaulieu; D. P. Bennett; J. A. R. Caldwell; A. A. Cole; K. H. Cook; C. Coutures; S. Dieters; D. Dominis Prester; J. Donatowicz; J. Greenhill; S. R. Kane; D. Kubas; J.‐B. Marquette; R. Martin; J. Menzies; K. R. Pollard; K. C. Sahu; A. Williams; M. K. Szymański; M. Kubiak; G. Pietrzyński; I. Soszyński; R. Poleski; K. Ulaczyk; D. L. DePoy; Subo Dong; C. Han; J. Janczak; C.‐U. Lee; R. W. Pogge; F. Abe; K. Furusawa; J. B. Hearnshaw; Y. Itow; P. M. Kilmartin; A. V. Korpela; W. Lin; C. H. Ling; K. Masuda; Y. Matsubara; N. Miyake; Y. Muraki; K. Ohnishi; Y. C. Perrott; To. Saito; L. Skuljan; D. J. Sullivan; T. Sumi; D. Suzuki; W. L. Sweatman; P. J. Tristram; K. Wada; P. C. M. Yock; A. Gulbis; Y. Hashimoto; A. Kniazev; P. Vaisanen

doi:10.1111/j.1365-2966.2012.21233.x

OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★

V. Bozza, M. Dominik, N. J. Rattenbury, U. G. Jørgensen, Y. Tsapras, D. M. Bramich, A. Udalski, I. A. Bond, C. Liebig, A. Cassan, P. Fouqué, A. Fukui, M. Hundertmark, I.‐G. Shin, S. H. Lee, J.‐Y. Choi, S.‐Y. Park, A. Gould, A. Allan, S. MaoŁ. Wyrzykowski, R. A. Street, D. Buckley, T. Nagayama, M. Mathiasen, T. C. Hinse, S. Calchi Novati, K. Harpsøe, L. Mancini, G. Scarpetta, T. Anguita, M. J. Burgdorf, K. Horne, Allan Hornstrup, N. Kains, E. Kerins, P. Kjærgaard, G. Masi, S. Rahvar, D. Ricci, C. Snodgrass, J. Southworth, I. A. Steele, J. Surdej, C. C. Thöne, J. Wambsganss, M. Zub, M. D. Albrow, V. Batista, J.‐P. Beaulieu, D. P. Bennett, J. A. R. Caldwell, A. A. Cole, K. H. Cook, C. Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, J. Greenhill, S. R. Kane, D. Kubas, J.‐B. Marquette, R. Martin, J. Menzies, K. R. Pollard, K. C. Sahu, A. Williams, M. K. Szymański, M. Kubiak, G. Pietrzyński, I. Soszyński, R. Poleski, K. Ulaczyk, D. L. DePoy, Subo Dong, C. Han, J. Janczak, C.‐U. Lee, R. W. Pogge, F. Abe, K. Furusawa, J. B. Hearnshaw, Y. Itow, P. M. Kilmartin, A. V. Korpela, W. Lin, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Ohnishi, Y. C. Perrott, To. Saito, L. Skuljan, D. J. Sullivan, T. Sumi, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, A. Gulbis, Y. Hashimoto, A. Kniazev, P. Vaisanen

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Abstract

The microlensing event OGLE‐2008‐BLG‐510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary‐lens and binary‐source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real‐time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the ‘favourite model’ is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown‐dwarf companions and binary‐source microlensing events might hide here.

Original language	English
Journal	Royal Astronomical Society. Monthly Notices
Volume	424
Issue number	2
Pages (from-to)	902-918
ISSN	0035-8711
DOIs	https://doi.org/10.1111/j.1365-2966.2012.21233.x
Publication status	Published - 2012

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Bozza, V., Dominik, M., Rattenbury, N. J., Jørgensen, U. G., Tsapras, Y., Bramich, D. M., Udalski, A., Bond, I. A., Liebig, C., Cassan, A., Fouqué, P., Fukui, A., Hundertmark, M., Shin, I. G., Lee, S. H., Choi, J. Y., Park, S. Y., Gould, A., Allan, A., ... Vaisanen, P. (2012). OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★. Royal Astronomical Society. Monthly Notices, 424(2), 902-918. https://doi.org/10.1111/j.1365-2966.2012.21233.x

@article{0132ae78bdb448dfaef58a9b9e96a46c,

title = "OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★",

abstract = "The microlensing event OGLE‐2008‐BLG‐510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary‐lens and binary‐source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real‐time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the {\textquoteleft}favourite model{\textquoteright} is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown‐dwarf companions and binary‐source microlensing events might hide here.",

author = "V. Bozza and M. Dominik and Rattenbury, {N. J.} and J{\o}rgensen, {U. G.} and Y. Tsapras and Bramich, {D. M.} and A. Udalski and Bond, {I. A.} and C. Liebig and A. Cassan and P. Fouqu{\'e} and A. Fukui and M. Hundertmark and I.‐G. Shin and Lee, {S. H.} and J.‐Y. Choi and S.‐Y. Park and A. Gould and A. Allan and S. Mao and {\L}. Wyrzykowski and Street, {R. A.} and D. Buckley and T. Nagayama and M. Mathiasen and Hinse, {T. C.} and Novati, {S. Calchi} and K. Harps{\o}e and L. Mancini and G. Scarpetta and T. Anguita and Burgdorf, {M. J.} and K. Horne and Allan Hornstrup and N. Kains and E. Kerins and P. Kj{\ae}rgaard and G. Masi and S. Rahvar and D. Ricci and C. Snodgrass and J. Southworth and Steele, {I. A.} and J. Surdej and Th{\"o}ne, {C. C.} and J. Wambsganss and M. Zub and Albrow, {M. D.} and V. Batista and J.‐P. Beaulieu and Bennett, {D. P.} and Caldwell, {J. A. R.} and Cole, {A. A.} and Cook, {K. H.} and C. Coutures and S. Dieters and Prester, {D. Dominis} and J. Donatowicz and J. Greenhill and Kane, {S. R.} and D. Kubas and J.‐B. Marquette and R. Martin and J. Menzies and Pollard, {K. R.} and Sahu, {K. C.} and A. Williams and Szyma{\'n}ski, {M. K.} and M. Kubiak and G. Pietrzy{\'n}ski and I. Soszy{\'n}ski and R. Poleski and K. Ulaczyk and DePoy, {D. L.} and Subo Dong and C. Han and J. Janczak and C.‐U. Lee and Pogge, {R. W.} and F. Abe and K. Furusawa and Hearnshaw, {J. B.} and Y. Itow and Kilmartin, {P. M.} and Korpela, {A. V.} and W. Lin and Ling, {C. H.} and K. Masuda and Y. Matsubara and N. Miyake and Y. Muraki and K. Ohnishi and Perrott, {Y. C.} and To. Saito and L. Skuljan and Sullivan, {D. J.} and T. Sumi and D. Suzuki and Sweatman, {W. L.} and Tristram, {P. J.} and K. Wada and Yock, {P. C. M.} and A. Gulbis and Y. Hashimoto and A. Kniazev and P. Vaisanen",

year = "2012",

doi = "10.1111/j.1365-2966.2012.21233.x",

language = "English",

volume = "424",

pages = "902--918",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

Bozza, V, Dominik, M, Rattenbury, NJ, Jørgensen, UG, Tsapras, Y, Bramich, DM, Udalski, A, Bond, IA, Liebig, C, Cassan, A, Fouqué, P, Fukui, A, Hundertmark, M, Shin, IG, Lee, SH, Choi, JY, Park, SY, Gould, A, Allan, A, Mao, S, Wyrzykowski, Ł, Street, RA, Buckley, D, Nagayama, T, Mathiasen, M, Hinse, TC, Novati, SC, Harpsøe, K, Mancini, L, Scarpetta, G, Anguita, T, Burgdorf, MJ, Horne, K, Hornstrup, A, Kains, N, Kerins, E, Kjærgaard, P, Masi, G, Rahvar, S, Ricci, D, Snodgrass, C, Southworth, J, Steele, IA, Surdej, J, Thöne, CC, Wambsganss, J, Zub, M, Albrow, MD, Batista, V, Beaulieu, JP, Bennett, DP, Caldwell, JAR, Cole, AA, Cook, KH, Coutures, C, Dieters, S, Prester, DD, Donatowicz, J, Greenhill, J, Kane, SR, Kubas, D, Marquette, JB, Martin, R, Menzies, J, Pollard, KR, Sahu, KC, Williams, A, Szymański, MK, Kubiak, M, Pietrzyński, G, Soszyński, I, Poleski, R, Ulaczyk, K, DePoy, DL, Dong, S, Han, C, Janczak, J, Lee, CU, Pogge, RW, Abe, F, Furusawa, K, Hearnshaw, JB, Itow, Y, Kilmartin, PM, Korpela, AV, Lin, W, Ling, CH, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Ohnishi, K, Perrott, YC, Saito, T, Skuljan, L, Sullivan, DJ, Sumi, T, Suzuki, D, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Gulbis, A, Hashimoto, Y, Kniazev, A & Vaisanen, P 2012, 'OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★', Royal Astronomical Society. Monthly Notices, vol. 424, no. 2, pp. 902-918. https://doi.org/10.1111/j.1365-2966.2012.21233.x

TY - JOUR

T1 - OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★

AU - Bozza, V.

AU - Dominik, M.

AU - Rattenbury, N. J.

AU - Jørgensen, U. G.

AU - Tsapras, Y.

AU - Bramich, D. M.

AU - Udalski, A.

AU - Bond, I. A.

AU - Liebig, C.

AU - Cassan, A.

AU - Fouqué, P.

AU - Fukui, A.

AU - Hundertmark, M.

AU - Shin, I.‐G.

AU - Lee, S. H.

AU - Choi, J.‐Y.

AU - Park, S.‐Y.

AU - Gould, A.

AU - Allan, A.

AU - Mao, S.

AU - Wyrzykowski, Ł.

AU - Street, R. A.

AU - Buckley, D.

AU - Nagayama, T.

AU - Mathiasen, M.

AU - Hinse, T. C.

AU - Novati, S. Calchi

AU - Harpsøe, K.

AU - Mancini, L.

AU - Scarpetta, G.

AU - Anguita, T.

AU - Burgdorf, M. J.

AU - Horne, K.

AU - Hornstrup, Allan

AU - Kains, N.

AU - Kerins, E.

AU - Kjærgaard, P.

AU - Masi, G.

AU - Rahvar, S.

AU - Ricci, D.

AU - Snodgrass, C.

AU - Southworth, J.

AU - Steele, I. A.

AU - Surdej, J.

AU - Thöne, C. C.

AU - Wambsganss, J.

AU - Zub, M.

AU - Albrow, M. D.

AU - Batista, V.

AU - Beaulieu, J.‐P.

AU - Bennett, D. P.

AU - Caldwell, J. A. R.

AU - Cole, A. A.

AU - Cook, K. H.

AU - Coutures, C.

AU - Dieters, S.

AU - Prester, D. Dominis

AU - Donatowicz, J.

AU - Greenhill, J.

AU - Kane, S. R.

AU - Kubas, D.

AU - Marquette, J.‐B.

AU - Martin, R.

AU - Menzies, J.

AU - Pollard, K. R.

AU - Sahu, K. C.

AU - Williams, A.

AU - Szymański, M. K.

AU - Kubiak, M.

AU - Pietrzyński, G.

AU - Soszyński, I.

AU - Poleski, R.

AU - Ulaczyk, K.

AU - DePoy, D. L.

AU - Dong, Subo

AU - Han, C.

AU - Janczak, J.

AU - Lee, C.‐U.

AU - Pogge, R. W.

AU - Abe, F.

AU - Furusawa, K.

AU - Hearnshaw, J. B.

AU - Itow, Y.

AU - Kilmartin, P. M.

AU - Korpela, A. V.

AU - Lin, W.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Muraki, Y.

AU - Ohnishi, K.

AU - Perrott, Y. C.

AU - Saito, To.

AU - Skuljan, L.

AU - Sullivan, D. J.

AU - Sumi, T.

AU - Suzuki, D.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Wada, K.

AU - Yock, P. C. M.

AU - Gulbis, A.

AU - Hashimoto, Y.

AU - Kniazev, A.

AU - Vaisanen, P.

PY - 2012

Y1 - 2012

N2 - The microlensing event OGLE‐2008‐BLG‐510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary‐lens and binary‐source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real‐time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the ‘favourite model’ is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown‐dwarf companions and binary‐source microlensing events might hide here.

AB - The microlensing event OGLE‐2008‐BLG‐510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary‐lens and binary‐source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real‐time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the ‘favourite model’ is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown‐dwarf companions and binary‐source microlensing events might hide here.

U2 - 10.1111/j.1365-2966.2012.21233.x

DO - 10.1111/j.1365-2966.2012.21233.x

M3 - Journal article

SN - 0035-8711

VL - 424

SP - 902

EP - 918

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

IS - 2

ER -

OGLE‐2008‐BLG‐510: first automated real‐time detection of a weak microlensing anomaly – brown dwarf or stellar binary?★

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