OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING

A. Fukui, A. Gould, T. Sumi, D. P. Bennett, I. A. Bond, C. Han, D. Suzuki, J. P. Beaulieu, V. Batista, A. Udalski, R. A. Street, Y. Tsapras, M. Hundertmark, F. Abe, A. Bhattacharya, M. Freeman, Y. Itow, C. H. Ling, N. Koshimoto, K. MasudaY. Matsubara, Y. Muraki, K. Ohnishi, L. C. Philpott, N. Rattenbury, T. Saito, D. J. Sullivan, P. J. Tristram, A. Yonehara, J. Y. Choi, G. W. Christie, D. L. Depoy, Subo Dong, J. Drummond, B. S. Gaudi, K. H. Hwang, A. Kavka, C. U. Lee, J. Mccormick, T. Natusch, H. Ngan, H. Park, R. W. Pogge, I. G. Shin, T. G. Tan, J. C. Yee, M. K. Szymański, G. Pietrzyński, I. Soszyński, R. Poleski, S. Kozłowski, P. Pietrukowicz, K. Ulaczyk, [No Value] Wyrzykowski, D. M. Bramich, P. Browne, M. Dominik, K. Horne, S. Ipatov, N. Kains, C. Snodgrass, I. A. Steele

Research output: Contribution to journalArticle

27 Citations (Scopus)

Abstract

We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of ∼1 ×10-3. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3 0.6 0.8 kpc from us, and consists of an M dwarf (0.34 0.12 0.20 M) orbited by a Saturn-mass planet (0.39 0.14 0.23 MJup) at the projected separation of 0.74 0.26 0.42 AU (close model) or 4.3 1.5 2.5 AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J - Ks ) and (H - Ks ) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 ≤ mp MJup

Original languageEnglish
Article number74
JournalAstrophysical Journal
Volume809
Issue number1
DOIs
Publication statusPublished - 10 Aug 2015

Fingerprint

Saturn
planets
planet
stars
magnification
metallicity
Jupiter
planetary systems
parallax
high resolution
extrasolar planets
Jupiter (planet)
mass ratios
light curve
spectrographs
contamination
cameras
lenses
color
estimates

Keywords

  • planetary systems
  • planets and satellites: detection
  • planets and satellites: gaseous planets
  • stars: late-type
  • techniques: high angular resolution
  • techniques: photometric

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Fukui, A., Gould, A., Sumi, T., Bennett, D. P., Bond, I. A., Han, C., ... Steele, I. A. (2015). OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING. Astrophysical Journal, 809(1), [74]. https://doi.org/10.1088/0004-637X/809/1/74

OGLE-2012-BLG-0563Lb : A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING. / Fukui, A.; Gould, A.; Sumi, T.; Bennett, D. P.; Bond, I. A.; Han, C.; Suzuki, D.; Beaulieu, J. P.; Batista, V.; Udalski, A.; Street, R. A.; Tsapras, Y.; Hundertmark, M.; Abe, F.; Bhattacharya, A.; Freeman, M.; Itow, Y.; Ling, C. H.; Koshimoto, N.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Ohnishi, K.; Philpott, L. C.; Rattenbury, N.; Saito, T.; Sullivan, D. J.; Tristram, P. J.; Yonehara, A.; Choi, J. Y.; Christie, G. W.; Depoy, D. L.; Dong, Subo; Drummond, J.; Gaudi, B. S.; Hwang, K. H.; Kavka, A.; Lee, C. U.; Mccormick, J.; Natusch, T.; Ngan, H.; Park, H.; Pogge, R. W.; Shin, I. G.; Tan, T. G.; Yee, J. C.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Poleski, R.; Kozłowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, [No Value]; Bramich, D. M.; Browne, P.; Dominik, M.; Horne, K.; Ipatov, S.; Kains, N.; Snodgrass, C.; Steele, I. A.

In: Astrophysical Journal, Vol. 809, No. 1, 74, 10.08.2015.

Research output: Contribution to journalArticle

Fukui, A, Gould, A, Sumi, T, Bennett, DP, Bond, IA, Han, C, Suzuki, D, Beaulieu, JP, Batista, V, Udalski, A, Street, RA, Tsapras, Y, Hundertmark, M, Abe, F, Bhattacharya, A, Freeman, M, Itow, Y, Ling, CH, Koshimoto, N, Masuda, K, Matsubara, Y, Muraki, Y, Ohnishi, K, Philpott, LC, Rattenbury, N, Saito, T, Sullivan, DJ, Tristram, PJ, Yonehara, A, Choi, JY, Christie, GW, Depoy, DL, Dong, S, Drummond, J, Gaudi, BS, Hwang, KH, Kavka, A, Lee, CU, Mccormick, J, Natusch, T, Ngan, H, Park, H, Pogge, RW, Shin, IG, Tan, TG, Yee, JC, Szymański, MK, Pietrzyński, G, Soszyński, I, Poleski, R, Kozłowski, S, Pietrukowicz, P, Ulaczyk, K, Wyrzykowski, NV, Bramich, DM, Browne, P, Dominik, M, Horne, K, Ipatov, S, Kains, N, Snodgrass, C & Steele, IA 2015, 'OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING', Astrophysical Journal, vol. 809, no. 1, 74. https://doi.org/10.1088/0004-637X/809/1/74
Fukui, A. ; Gould, A. ; Sumi, T. ; Bennett, D. P. ; Bond, I. A. ; Han, C. ; Suzuki, D. ; Beaulieu, J. P. ; Batista, V. ; Udalski, A. ; Street, R. A. ; Tsapras, Y. ; Hundertmark, M. ; Abe, F. ; Bhattacharya, A. ; Freeman, M. ; Itow, Y. ; Ling, C. H. ; Koshimoto, N. ; Masuda, K. ; Matsubara, Y. ; Muraki, Y. ; Ohnishi, K. ; Philpott, L. C. ; Rattenbury, N. ; Saito, T. ; Sullivan, D. J. ; Tristram, P. J. ; Yonehara, A. ; Choi, J. Y. ; Christie, G. W. ; Depoy, D. L. ; Dong, Subo ; Drummond, J. ; Gaudi, B. S. ; Hwang, K. H. ; Kavka, A. ; Lee, C. U. ; Mccormick, J. ; Natusch, T. ; Ngan, H. ; Park, H. ; Pogge, R. W. ; Shin, I. G. ; Tan, T. G. ; Yee, J. C. ; Szymański, M. K. ; Pietrzyński, G. ; Soszyński, I. ; Poleski, R. ; Kozłowski, S. ; Pietrukowicz, P. ; Ulaczyk, K. ; Wyrzykowski, [No Value] ; Bramich, D. M. ; Browne, P. ; Dominik, M. ; Horne, K. ; Ipatov, S. ; Kains, N. ; Snodgrass, C. ; Steele, I. A. / OGLE-2012-BLG-0563Lb : A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING. In: Astrophysical Journal. 2015 ; Vol. 809, No. 1.
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title = "OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING",
abstract = "We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of ∼1 ×10-3. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3 0.6 0.8 kpc from us, and consists of an M dwarf (0.34 0.12 0.20 M) orbited by a Saturn-mass planet (0.39 0.14 0.23 MJup) at the projected separation of 0.74 0.26 0.42 AU (close model) or 4.3 1.5 2.5 AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17{\%}. This possibility can be tested by future high-resolution imaging. We also estimate the (J - Ks ) and (H - Ks ) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 ≤ mp MJup",
keywords = "planetary systems, planets and satellites: detection, planets and satellites: gaseous planets, stars: late-type, techniques: high angular resolution, techniques: photometric",
author = "A. Fukui and A. Gould and T. Sumi and Bennett, {D. P.} and Bond, {I. A.} and C. Han and D. Suzuki and Beaulieu, {J. P.} and V. Batista and A. Udalski and Street, {R. A.} and Y. Tsapras and M. Hundertmark and F. Abe and A. Bhattacharya and M. Freeman and Y. Itow and Ling, {C. H.} and N. Koshimoto and K. Masuda and Y. Matsubara and Y. Muraki and K. Ohnishi and Philpott, {L. C.} and N. Rattenbury and T. Saito and Sullivan, {D. J.} and Tristram, {P. J.} and A. Yonehara and Choi, {J. Y.} and Christie, {G. W.} and Depoy, {D. L.} and Subo Dong and J. Drummond and Gaudi, {B. S.} and Hwang, {K. H.} and A. Kavka and Lee, {C. U.} and J. Mccormick and T. Natusch and H. Ngan and H. Park and Pogge, {R. W.} and Shin, {I. G.} and Tan, {T. G.} and Yee, {J. C.} and Szymański, {M. K.} and G. Pietrzyński and I. Soszyński and R. Poleski and S. Kozłowski and P. Pietrukowicz and K. Ulaczyk and Wyrzykowski, {[No Value]} and Bramich, {D. M.} and P. Browne and M. Dominik and K. Horne and S. Ipatov and N. Kains and C. Snodgrass and Steele, {I. A.}",
year = "2015",
month = "8",
day = "10",
doi = "10.1088/0004-637X/809/1/74",
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volume = "809",
journal = "Astrophysical Journal",
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TY - JOUR

T1 - OGLE-2012-BLG-0563Lb

T2 - A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING

AU - Fukui, A.

AU - Gould, A.

AU - Sumi, T.

AU - Bennett, D. P.

AU - Bond, I. A.

AU - Han, C.

AU - Suzuki, D.

AU - Beaulieu, J. P.

AU - Batista, V.

AU - Udalski, A.

AU - Street, R. A.

AU - Tsapras, Y.

AU - Hundertmark, M.

AU - Abe, F.

AU - Bhattacharya, A.

AU - Freeman, M.

AU - Itow, Y.

AU - Ling, C. H.

AU - Koshimoto, N.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Ohnishi, K.

AU - Philpott, L. C.

AU - Rattenbury, N.

AU - Saito, T.

AU - Sullivan, D. J.

AU - Tristram, P. J.

AU - Yonehara, A.

AU - Choi, J. Y.

AU - Christie, G. W.

AU - Depoy, D. L.

AU - Dong, Subo

AU - Drummond, J.

AU - Gaudi, B. S.

AU - Hwang, K. H.

AU - Kavka, A.

AU - Lee, C. U.

AU - Mccormick, J.

AU - Natusch, T.

AU - Ngan, H.

AU - Park, H.

AU - Pogge, R. W.

AU - Shin, I. G.

AU - Tan, T. G.

AU - Yee, J. C.

AU - Szymański, M. K.

AU - Pietrzyński, G.

AU - Soszyński, I.

AU - Poleski, R.

AU - Kozłowski, S.

AU - Pietrukowicz, P.

AU - Ulaczyk, K.

AU - Wyrzykowski, [No Value]

AU - Bramich, D. M.

AU - Browne, P.

AU - Dominik, M.

AU - Horne, K.

AU - Ipatov, S.

AU - Kains, N.

AU - Snodgrass, C.

AU - Steele, I. A.

PY - 2015/8/10

Y1 - 2015/8/10

N2 - We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of ∼1 ×10-3. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3 0.6 0.8 kpc from us, and consists of an M dwarf (0.34 0.12 0.20 M) orbited by a Saturn-mass planet (0.39 0.14 0.23 MJup) at the projected separation of 0.74 0.26 0.42 AU (close model) or 4.3 1.5 2.5 AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J - Ks ) and (H - Ks ) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 ≤ mp MJup

AB - We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of ∼1 ×10-3. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3 0.6 0.8 kpc from us, and consists of an M dwarf (0.34 0.12 0.20 M) orbited by a Saturn-mass planet (0.39 0.14 0.23 MJup) at the projected separation of 0.74 0.26 0.42 AU (close model) or 4.3 1.5 2.5 AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J - Ks ) and (H - Ks ) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 ≤ mp MJup

KW - planetary systems

KW - planets and satellites: detection

KW - planets and satellites: gaseous planets

KW - stars: late-type

KW - techniques: high angular resolution

KW - techniques: photometric

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