MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?

K. Furusawa; A. Udalski; T. Sumi; D. P. Bennett; I. A. Bond; A. Gould; U. G. Jørgensen; C. Snodgrass; D. Dominis Prester; M. D. Albrow; F. Abe; C. S. Botzler; P. Chote; M. Freeman; A. Fukui; P. Harris; Y. Itow; C. H. Ling; K. Masuda; Y. Matsubara; N. Miyake; Y. Muraki; K. Ohnishi; N. J. Rattenbury; To. Saito; D. J. Sullivan; D. Suzuki; W. L. Sweatman; P. J. Tristram; K. Wada; P. C. M. Yock; M. K. Szymański; I. Soszyński; M. Kubiak; R. Poleski; K. Ulaczyk; G. Pietrzyński; Ł. Wyrzykowski; J.-Y. Choi; G. W. Christie; D. L. DePoy; Subo Dong; J. Drummond; B. S. Gaudi; C. Han; L.-W. Hung; K.-H. Hwang; C.-U. Lee; J. McCormick; D. Moorhouse; T. Natusch; M. Nola; E. Ofek; R. W. Pogge; I.-G. Shin; J. Skowron; G. Thornley; J. C. Yee; K. A. Alsubai; V. Bozza; P. Browne; M. J. Burgdorf; S. Calchi Novati; P. Dodds; M. Dominik; F. Finet; T. Gerner; S. Hardis; K. Harpsøe; T. C. Hinse; M. Hundertmark; Noé Kains; E. Kerins; C. Liebig; L. Mancini; M. Mathiasen; M. T. Penny; S. Proft; S. Rahvar; D. Ricci; G. Scarpetta; S. Schäfer; F. Schönebeck; J. Southworth; J. Surdej; J. Wambsganss; R. A. Street; D. M. Bramich; I. A. Steele; Y. Tsapras; K. Horne; J. Donatowicz; K. C. Sahu; E. Bachelet; V. Batista; T. G. Beatty; J.-P. Beaulieu; C. S. Bennett; C. Black; R. Bowens-Rubin; S. Brillant; J. A. R. Caldwell; A. Cassan; A. A. Cole; E. Corrales; C. Coutures; S. Dieters; P. Fouqué; J. Greenhill; C. B. Henderson; D. Kubas; J.-B. Marquette; R. Martin; J. W. Menzies; B. Shappee; A. Williams; D. Wouters; J. van Saders; R. Zellem; M. Zub

doi:10.1088/0004-637X/779/2/91

MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?

K. Furusawa, A. Udalski, T. Sumi, D. P. Bennett, I. A. Bond, A. Gould, U. G. Jørgensen, C. Snodgrass, D. Dominis Prester, M. D. Albrow, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, P. Harris, Y. Itow, C. H. Ling, K. Masuda, Y. MatsubaraN. Miyake, Y. Muraki, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, I. Soszyński, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzyński, Ł. Wyrzykowski, J.-Y. Choi, G. W. Christie, D. L. DePoy, Subo Dong, J. Drummond, B. S. Gaudi, C. Han, L.-W. Hung, K.-H. Hwang, C.-U. Lee, J. McCormick, D. Moorhouse, T. Natusch, M. Nola, E. Ofek, R. W. Pogge, I.-G. Shin, J. Skowron, G. Thornley, J. C. Yee, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, M. Dominik, F. Finet, T. Gerner, S. Hardis, K. Harpsøe, T. C. Hinse, M. Hundertmark, Noé Kains, E. Kerins, C. Liebig, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Southworth, J. Surdej, J. Wambsganss, R. A. Street, D. M. Bramich, I. A. Steele, Y. Tsapras, K. Horne, J. Donatowicz, K. C. Sahu, E. Bachelet, V. Batista, T. G. Beatty, J.-P. Beaulieu, C. S. Bennett, C. Black, R. Bowens-Rubin, S. Brillant, J. A. R. Caldwell, A. Cassan, A. A. Cole, E. Corrales, C. Coutures, S. Dieters, P. Fouqué, J. Greenhill, C. B. Henderson, D. Kubas, J.-B. Marquette, R. Martin, J. W. Menzies, B. Shappee, A. Williams, D. Wouters, J. van Saders, R. Zellem, M. Zub

School of Physics and Astronomy

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

Abstract

We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M _h = 0.11 ± 0.01 M _☉ and M_p = 9.2 ± 2.2 M _⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D _L = 0.81 ± 0.10 kpc with projected separation r _⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.

Original language	English
Article number	91
Number of pages	12
Journal	Astrophysical Journal
Volume	779
Issue number	2
Early online date	26 Nov 2013
DOIs	https://doi.org/10.1088/0004-637X/779/2/91
Publication status	Published - 20 Dec 2013

Keywords

Gravitational lensing: micro
Planetary systems

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10.1088/0004-637X/779/2/91

Horne_2013_TAJ_MOA
Copyright 2013. The American Astronomical Society. All rights reserved.
Final published version, 1.43 MB

AGN Echo mapping: AGN Echo Mapping and Mineral Clouds in Alien Atmospheres
Horne, K. D. (PI)
Science & Technology Facilities Council
1/04/12 → 31/08/12
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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Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jørgensen, U. G., Snodgrass, C., Dominis Prester, D., Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., ... Zub, M. (2013). MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf? Astrophysical Journal, 779(2), Article 91. https://doi.org/10.1088/0004-637X/779/2/91

@article{cc03b4f4aa4b437e8d8f3fd649bce0f7,

title = "MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?",

abstract = "We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M h = 0.11 ± 0.01 M ☉ and M p = 9.2 ± 2.2 M ⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D L = 0.81 ± 0.10 kpc with projected separation r ⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.",

keywords = "Gravitational lensing: micro, Planetary systems",

author = "K. Furusawa and A. Udalski and T. Sumi and Bennett, {D. P.} and Bond, {I. A.} and A. Gould and J{\o}rgensen, {U. G.} and C. Snodgrass and {Dominis Prester}, D. and Albrow, {M. D.} and F. Abe and Botzler, {C. S.} and P. Chote and M. Freeman and A. Fukui and P. Harris and Y. Itow and Ling, {C. H.} and K. Masuda and Y. Matsubara and N. Miyake and Y. Muraki 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 K. Wada and Yock, {P. C. M.} and Szyma{\'n}ski, {M. K.} and I. Soszy{\'n}ski and M. Kubiak and R. Poleski and K. Ulaczyk and G. Pietrzy{\'n}ski and {\L}. Wyrzykowski and J.-Y. Choi and Christie, {G. W.} and DePoy, {D. L.} and Subo Dong and J. Drummond and Gaudi, {B. S.} and C. Han and L.-W. Hung and K.-H. Hwang and C.-U. Lee and J. McCormick and D. Moorhouse and T. Natusch and M. Nola and E. Ofek and Pogge, {R. W.} and I.-G. Shin and J. Skowron and G. Thornley and Yee, {J. C.} and Alsubai, {K. A.} and V. Bozza and P. Browne and Burgdorf, {M. J.} and {Calchi Novati}, S. and P. Dodds and M. Dominik and F. Finet and T. Gerner and S. Hardis and K. Harps{\o}e and Hinse, {T. C.} and M. Hundertmark and No{\'e} Kains and E. Kerins and C. Liebig and L. Mancini and M. Mathiasen and Penny, {M. T.} and S. Proft and S. Rahvar and D. Ricci and G. Scarpetta and S. Sch{\"a}fer and F. Sch{\"o}nebeck and J. Southworth and J. Surdej and J. Wambsganss and Street, {R. A.} and Bramich, {D. M.} and Steele, {I. A.} and Y. Tsapras and K. Horne and J. Donatowicz and Sahu, {K. C.} and E. Bachelet and V. Batista and Beatty, {T. G.} and J.-P. Beaulieu and Bennett, {C. S.} and C. Black and R. Bowens-Rubin and S. Brillant and Caldwell, {J. A. R.} and A. Cassan and Cole, {A. A.} and E. Corrales and C. Coutures and S. Dieters and P. Fouqu{\'e} and J. Greenhill and Henderson, {C. B.} and D. Kubas and J.-B. Marquette and R. Martin and Menzies, {J. W.} and B. Shappee and A. Williams and D. Wouters and {van Saders}, J. and R. Zellem and M. Zub",

note = "K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. are thankful to Qatar National Research Fund (QNRF), a member of the Qatar Foundation, for support by grant NPRP 09-476-1-078. K.H. is supported by a Royal Society Leverhulme Trust Senior Research Fellowship.",

year = "2013",

month = dec,

day = "20",

doi = "10.1088/0004-637X/779/2/91",

language = "English",

volume = "779",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Furusawa, K, Udalski, A, Sumi, T, Bennett, DP, Bond, IA, Gould, A, Jørgensen, UG, Snodgrass, C, Dominis Prester, D, Albrow, MD, Abe, F, Botzler, CS, Chote, P, Freeman, M, Fukui, A, Harris, P, Itow, Y, Ling, CH, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Ohnishi, K, Rattenbury, NJ, Saito, T, Sullivan, DJ, Suzuki, D, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Szymański, MK, Soszyński, I, Kubiak, M, Poleski, R, Ulaczyk, K, Pietrzyński, G, Wyrzykowski, Ł, Choi, J-Y, Christie, GW, DePoy, DL, Dong, S, Drummond, J, Gaudi, BS, Han, C, Hung, L-W, Hwang, K-H, Lee, C-U, McCormick, J, Moorhouse, D, Natusch, T, Nola, M, Ofek, E, Pogge, RW, Shin, I-G, Skowron, J, Thornley, G, Yee, JC, Alsubai, KA, Bozza, V, Browne, P, Burgdorf, MJ, Calchi Novati, S, Dodds, P, Dominik, M, Finet, F, Gerner, T, Hardis, S, Harpsøe, K, Hinse, TC, Hundertmark, M, Kains, N, Kerins, E, Liebig, C, Mancini, L, Mathiasen, M, Penny, MT, Proft, S, Rahvar, S, Ricci, D, Scarpetta, G, Schäfer, S, Schönebeck, F, Southworth, J, Surdej, J, Wambsganss, J, Street, RA, Bramich, DM, Steele, IA, Tsapras, Y, Horne, K, Donatowicz, J, Sahu, KC, Bachelet, E, Batista, V, Beatty, TG, Beaulieu, J-P, Bennett, CS, Black, C, Bowens-Rubin, R, Brillant, S, Caldwell, JAR, Cassan, A, Cole, AA, Corrales, E, Coutures, C, Dieters, S, Fouqué, P, Greenhill, J, Henderson, CB, Kubas, D, Marquette, J-B, Martin, R, Menzies, JW, Shappee, B, Williams, A, Wouters, D, van Saders, J, Zellem, R & Zub, M 2013, 'MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?', Astrophysical Journal, vol. 779, no. 2, 91. https://doi.org/10.1088/0004-637X/779/2/91

TY - JOUR

T1 - MOA-2010-BLG-328Lb

T2 - a sub-Neptune orbiting very Late M dwarf?

AU - Furusawa, K.

AU - Udalski, A.

AU - Sumi, T.

AU - Bennett, D. P.

AU - Bond, I. A.

AU - Gould, A.

AU - Jørgensen, U. G.

AU - Snodgrass, C.

AU - Dominis Prester, D.

AU - Albrow, M. D.

AU - Abe, F.

AU - Botzler, C. S.

AU - Chote, P.

AU - Freeman, M.

AU - Fukui, A.

AU - Harris, P.

AU - Itow, Y.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Muraki, Y.

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 - Wada, K.

AU - Yock, P. C. M.

AU - Szymański, M. K.

AU - Soszyński, I.

AU - Kubiak, M.

AU - Poleski, R.

AU - Ulaczyk, K.

AU - Pietrzyński, G.

AU - Wyrzykowski, Ł.

AU - Choi, J.-Y.

AU - Christie, G. W.

AU - DePoy, D. L.

AU - Dong, Subo

AU - Drummond, J.

AU - Gaudi, B. S.

AU - Han, C.

AU - Hung, L.-W.

AU - Hwang, K.-H.

AU - Lee, C.-U.

AU - McCormick, J.

AU - Moorhouse, D.

AU - Natusch, T.

AU - Nola, M.

AU - Ofek, E.

AU - Pogge, R. W.

AU - Shin, I.-G.

AU - Skowron, J.

AU - Thornley, G.

AU - Yee, J. C.

AU - Alsubai, K. A.

AU - Bozza, V.

AU - Browne, P.

AU - Burgdorf, M. J.

AU - Calchi Novati, S.

AU - Dodds, P.

AU - Dominik, M.

AU - Finet, F.

AU - Gerner, T.

AU - Hardis, S.

AU - Harpsøe, K.

AU - Hinse, T. C.

AU - Hundertmark, M.

AU - Kains, Noé

AU - Kerins, E.

AU - Liebig, C.

AU - Mancini, L.

AU - Mathiasen, M.

AU - Penny, M. T.

AU - Proft, S.

AU - Rahvar, S.

AU - Ricci, D.

AU - Scarpetta, G.

AU - Schäfer, S.

AU - Schönebeck, F.

AU - Southworth, J.

AU - Surdej, J.

AU - Wambsganss, J.

AU - Street, R. A.

AU - Bramich, D. M.

AU - Steele, I. A.

AU - Tsapras, Y.

AU - Horne, K.

AU - Donatowicz, J.

AU - Sahu, K. C.

AU - Bachelet, E.

AU - Batista, V.

AU - Beatty, T. G.

AU - Beaulieu, J.-P.

AU - Bennett, C. S.

AU - Black, C.

AU - Bowens-Rubin, R.

AU - Brillant, S.

AU - Caldwell, J. A. R.

AU - Cassan, A.

AU - Cole, A. A.

AU - Corrales, E.

AU - Coutures, C.

AU - Dieters, S.

AU - Fouqué, P.

AU - Greenhill, J.

AU - Henderson, C. B.

AU - Kubas, D.

AU - Marquette, J.-B.

AU - Martin, R.

AU - Menzies, J. W.

AU - Shappee, B.

AU - Williams, A.

AU - Wouters, D.

AU - van Saders, J.

AU - Zellem, R.

AU - Zub, M.

N1 - K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. are thankful to Qatar National Research Fund (QNRF), a member of the Qatar Foundation, for support by grant NPRP 09-476-1-078. K.H. is supported by a Royal Society Leverhulme Trust Senior Research Fellowship.

PY - 2013/12/20

Y1 - 2013/12/20

N2 - We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M h = 0.11 ± 0.01 M ☉ and M p = 9.2 ± 2.2 M ⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D L = 0.81 ± 0.10 kpc with projected separation r ⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.

AB - We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M h = 0.11 ± 0.01 M ☉ and M p = 9.2 ± 2.2 M ⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D L = 0.81 ± 0.10 kpc with projected separation r ⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.

KW - Gravitational lensing: micro

KW - Planetary systems

U2 - 10.1088/0004-637X/779/2/91

DO - 10.1088/0004-637X/779/2/91

M3 - Article

SN - 0004-637X

VL - 779

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 91

ER -

MOA-2010-BLG-328Lb: a sub-Neptune orbiting very Late M dwarf?

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Keywords

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AGN Echo mapping: AGN Echo Mapping and Mineral Clouds in Alien Atmospheres

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

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