MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?

We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary massesof Mh = 0.11 ± 0.01M and Mp = 9.2 ± 2.2M?, corresponding to a very late M dwarf and sub-Neptune-massplanet, respectively. The system lies at DL = 0.81 ± 0.10 kpc with projected separation r? =...

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Main Authors:	Furusawa, K., Udalski, A., Sumi, T., Bennett, D., Bond, I., Gould, A., Jørgensen, U., Snodgrass, C., Dominis Prester, D., Albrow, M., Abe, F., Botzler, C., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Suzuki, D., Sweatman, W., Tristram, P., Wada, K., Yock, P., Szymanski, M., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J., Christie, G., DePoy, D., Dong, S., Drummond, J., Gaudi, B., Han, C., Hung, L., Hwang, K., Lee, C., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Pogge, R., Shin, I., Skowron, J., Thornley, G., Yee, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R., Bramich, D., Steele, I., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K., Bachelet, E., Batista, V., Beatty, T., Beaulieu, J., Bennett, C., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C., Kubas, D., Marquette, J., Martin, R., Menzies, J., Shappee, B., Williams, Andrew, Wouters, D., van Saders, J., Zellem, R., Zub, M.
Format:	Journal Article
Published:	IOP Publishing Ltd. 2013
Subjects:	gravitational lensing micro planetary systems
Online Access:	http://iopscience.iop.org/0004-637X/779/2/91/pdf/0004-637X_779_2_91.pdf http://hdl.handle.net/20.500.11937/16718

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author	Furusawa, K. Udalski, A. Sumi, T. Bennett, D. Bond, I. Gould, A. Jørgensen, U. Snodgrass, C. Dominis Prester, D. Albrow, M. Abe, F. Botzler, C. Chote, P. Freeman, M. Fukui, A. Harris, P. Itow, Y. Ling, C. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Rattenbury, N. Saito, T. Sullivan, D. Suzuki, D. Sweatman, W. Tristram, P. Wada, K. Yock, P. Szymanski, M. Soszynski, I. Kubiak, M. Poleski, R. Ulaczyk, K. Pietrzynski, G. Wyrzykowski, L. Choi, J. Christie, G. DePoy, D. Dong, S. Drummond, J. Gaudi, B. Han, C. Hung, L. Hwang, K. Lee, C. McCormick, J. Moorhouse, D. Natusch, T. Nola, M. Ofek, E. Pogge, R. Shin, I. Skowron, J. Thornley, G. Yee, J. Alsubai, K. Bozza, V. Browne, P. Burgdorf, M. Calchi Novati, S. Dodds, P. Dominik, M. Finet, F. Gerner, T. Hardis, S. Harpsoe, K. Hinse, T. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Mancini, L. Mathiasen, M. Penny, M. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schafer, S. Schonebeck, F. Southworth, J. Surdej, J. Wambsganss, J. Street, R. Bramich, D. Steele, I. Tsapras, Y. Horne, K. Donatowicz, J. Sahu, K. Bachelet, E. Batista, V. Beatty, T. Beaulieu, J. Bennett, C. Black, C. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cassan, A. Cole, A. Corrales, E. Coutures, C. Dieters, S. Fouque, P. Greenhill, J. Henderson, C. Kubas, D. Marquette, J. Martin, R. Menzies, J. Shappee, B. Williams, Andrew Wouters, D. van Saders, J. Zellem, R. Zub, M.
author_facet	Furusawa, K. Udalski, A. Sumi, T. Bennett, D. Bond, I. Gould, A. Jørgensen, U. Snodgrass, C. Dominis Prester, D. Albrow, M. Abe, F. Botzler, C. Chote, P. Freeman, M. Fukui, A. Harris, P. Itow, Y. Ling, C. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Rattenbury, N. Saito, T. Sullivan, D. Suzuki, D. Sweatman, W. Tristram, P. Wada, K. Yock, P. Szymanski, M. Soszynski, I. Kubiak, M. Poleski, R. Ulaczyk, K. Pietrzynski, G. Wyrzykowski, L. Choi, J. Christie, G. DePoy, D. Dong, S. Drummond, J. Gaudi, B. Han, C. Hung, L. Hwang, K. Lee, C. McCormick, J. Moorhouse, D. Natusch, T. Nola, M. Ofek, E. Pogge, R. Shin, I. Skowron, J. Thornley, G. Yee, J. Alsubai, K. Bozza, V. Browne, P. Burgdorf, M. Calchi Novati, S. Dodds, P. Dominik, M. Finet, F. Gerner, T. Hardis, S. Harpsoe, K. Hinse, T. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Mancini, L. Mathiasen, M. Penny, M. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schafer, S. Schonebeck, F. Southworth, J. Surdej, J. Wambsganss, J. Street, R. Bramich, D. Steele, I. Tsapras, Y. Horne, K. Donatowicz, J. Sahu, K. Bachelet, E. Batista, V. Beatty, T. Beaulieu, J. Bennett, C. Black, C. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cassan, A. Cole, A. Corrales, E. Coutures, C. Dieters, S. Fouque, P. Greenhill, J. Henderson, C. Kubas, D. Marquette, J. Martin, R. Menzies, J. Shappee, B. Williams, Andrew Wouters, D. van Saders, J. Zellem, R. Zub, M.
author_sort	Furusawa, K.
building	Curtin Institutional Repository
collection	Online Access
description	We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary massesof Mh = 0.11 ± 0.01M and Mp = 9.2 ± 2.2M?, corresponding to a very late M dwarf and sub-Neptune-massplanet, respectively. The system lies at DL = 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 considerthe possibility that the microlens parallax signal, which determines the host mass and distance, is actually due toxallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallaxsolution, even given its close host distance. We show that future high-resolution astrometric measurements coulddecisively resolve the remaining ambiguity of these solutions.
first_indexed	2025-11-14T07:18:03Z
format	Journal Article
id	curtin-20.500.11937-16718
institution	Curtin University Malaysia
institution_category	Local University
last_indexed	2025-11-14T07:18:03Z
publishDate	2013
publisher	IOP Publishing Ltd.
recordtype	eprints
repository_type	Digital Repository
spelling	curtin-20.500.11937-167182017-05-30T08:13:23Z MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf? Furusawa, K. Udalski, A. Sumi, T. Bennett, D. Bond, I. Gould, A. Jørgensen, U. Snodgrass, C. Dominis Prester, D. Albrow, M. Abe, F. Botzler, C. Chote, P. Freeman, M. Fukui, A. Harris, P. Itow, Y. Ling, C. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Rattenbury, N. Saito, T. Sullivan, D. Suzuki, D. Sweatman, W. Tristram, P. Wada, K. Yock, P. Szymanski, M. Soszynski, I. Kubiak, M. Poleski, R. Ulaczyk, K. Pietrzynski, G. Wyrzykowski, L. Choi, J. Christie, G. DePoy, D. Dong, S. Drummond, J. Gaudi, B. Han, C. Hung, L. Hwang, K. Lee, C. McCormick, J. Moorhouse, D. Natusch, T. Nola, M. Ofek, E. Pogge, R. Shin, I. Skowron, J. Thornley, G. Yee, J. Alsubai, K. Bozza, V. Browne, P. Burgdorf, M. Calchi Novati, S. Dodds, P. Dominik, M. Finet, F. Gerner, T. Hardis, S. Harpsoe, K. Hinse, T. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Mancini, L. Mathiasen, M. Penny, M. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schafer, S. Schonebeck, F. Southworth, J. Surdej, J. Wambsganss, J. Street, R. Bramich, D. Steele, I. Tsapras, Y. Horne, K. Donatowicz, J. Sahu, K. Bachelet, E. Batista, V. Beatty, T. Beaulieu, J. Bennett, C. Black, C. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cassan, A. Cole, A. Corrales, E. Coutures, C. Dieters, S. Fouque, P. Greenhill, J. Henderson, C. Kubas, D. Marquette, J. Martin, R. Menzies, J. Shappee, B. Williams, Andrew Wouters, D. van Saders, J. Zellem, R. Zub, M. gravitational lensing micro planetary systems We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary massesof Mh = 0.11 ± 0.01M and Mp = 9.2 ± 2.2M?, corresponding to a very late M dwarf and sub-Neptune-massplanet, respectively. The system lies at DL = 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 considerthe possibility that the microlens parallax signal, which determines the host mass and distance, is actually due toxallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallaxsolution, even given its close host distance. We show that future high-resolution astrometric measurements coulddecisively resolve the remaining ambiguity of these solutions. 2013 Journal Article http://hdl.handle.net/20.500.11937/16718 http://iopscience.iop.org/0004-637X/779/2/91/pdf/0004-637X_779_2_91.pdf IOP Publishing Ltd. restricted
spellingShingle	gravitational lensing micro planetary systems Furusawa, K. Udalski, A. Sumi, T. Bennett, D. Bond, I. Gould, A. Jørgensen, U. Snodgrass, C. Dominis Prester, D. Albrow, M. Abe, F. Botzler, C. Chote, P. Freeman, M. Fukui, A. Harris, P. Itow, Y. Ling, C. Masuda, K. Matsubara, Y. Miyake, N. Muraki, Y. Ohnishi, K. Rattenbury, N. Saito, T. Sullivan, D. Suzuki, D. Sweatman, W. Tristram, P. Wada, K. Yock, P. Szymanski, M. Soszynski, I. Kubiak, M. Poleski, R. Ulaczyk, K. Pietrzynski, G. Wyrzykowski, L. Choi, J. Christie, G. DePoy, D. Dong, S. Drummond, J. Gaudi, B. Han, C. Hung, L. Hwang, K. Lee, C. McCormick, J. Moorhouse, D. Natusch, T. Nola, M. Ofek, E. Pogge, R. Shin, I. Skowron, J. Thornley, G. Yee, J. Alsubai, K. Bozza, V. Browne, P. Burgdorf, M. Calchi Novati, S. Dodds, P. Dominik, M. Finet, F. Gerner, T. Hardis, S. Harpsoe, K. Hinse, T. Hundertmark, M. Kains, N. Kerins, E. Liebig, C. Mancini, L. Mathiasen, M. Penny, M. Proft, S. Rahvar, S. Ricci, D. Scarpetta, G. Schafer, S. Schonebeck, F. Southworth, J. Surdej, J. Wambsganss, J. Street, R. Bramich, D. Steele, I. Tsapras, Y. Horne, K. Donatowicz, J. Sahu, K. Bachelet, E. Batista, V. Beatty, T. Beaulieu, J. Bennett, C. Black, C. Bowens-Rubin, R. Brillant, S. Caldwell, J. Cassan, A. Cole, A. Corrales, E. Coutures, C. Dieters, S. Fouque, P. Greenhill, J. Henderson, C. Kubas, D. Marquette, J. Martin, R. Menzies, J. Shappee, B. Williams, Andrew Wouters, D. van Saders, J. Zellem, R. Zub, M. MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title	MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title_full	MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title_fullStr	MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title_full_unstemmed	MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title_short	MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?
title_sort	moa-2010-blg-328lb: a sub-neptune orbiting very late m dwarf?
topic	gravitational lensing micro planetary systems
url	http://iopscience.iop.org/0004-637X/779/2/91/pdf/0004-637X_779_2_91.pdf http://hdl.handle.net/20.500.11937/16718

MOA-2010-BLG-328Lb: A sub-Neptune orbiting very late M dwarf?

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