OGLE-2017-BLG-1434Lb: eighth q <1 x 10-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function

A. Udalski; Y-H Ryu; S. Sajadian; A. Gould; P. Mroz; R. Poleski; M. K. Szymanski; J. Skowron; null Soszynski; S. Kozlowski; P. Pietrukowicz; K. Ulaczyk; M. Pawlak; K. Rybicki; P. Iwanek; M. D. Albrow; S-J Chung; C. Han; K-H Hwang; Y. K. Jung; I-G Shin; Y. Shvartzvald; J. C. Yee; W. Zang; W. Zhu; S-M Cha; D-J Kim; H-W Kim; S-L Kim; C-U Lee; D-J Lee; Y. Lee; B-G Park; R. W. Pogge; null Bozza; M. Dominik; C. Helling; M. Hundertmark; U. G. Jorgensen; P. Longa-Pena; S. Lowry; M. Burgdorf; J. Campbell-White; S. Ciceri; D. Evans; R. Figuera Jaimes; Y. Fujii; L. K. Haikala; T. Henning; T. C. Hinse; L. Mancini; N. Peixinho; S. Rahvar; M. Rabus; J. Skottfelt; C. Snodgrass; J. Southworth; C. von Essen

OGLE-2017-BLG-1434Lb: eighth q <1 x 10^-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function

A. Udalski^*, Y-H Ryu, S. Sajadian, A. Gould, P. Mroz, R. Poleski, M. K. Szymanski, J. Skowron, Soszynski, S. Kozlowski, P. Pietrukowicz, K. Ulaczyk, M. Pawlak, K. Rybicki, P. Iwanek, M. D. Albrow, S-J Chung, C. Han, K-H Hwang, Y. K. JungI-G Shin, Y. Shvartzvald, J. C. Yee, W. Zang, W. Zhu, S-M Cha, D-J Kim, H-W Kim, S-L Kim, C-U Lee, D-J Lee, Y. Lee, B-G Park, R. W. Pogge, Bozza, M. Dominik, C. Helling, M. Hundertmark, U. G. Jorgensen, P. Longa-Pena, S. Lowry, M. Burgdorf, J. Campbell-White, S. Ciceri, D. Evans, R. Figuera Jaimes, Y. Fujii, L. K. Haikala, T. Henning, T. C. Hinse, L. Mancini, N. Peixinho, S. Rahvar, M. Rabus, J. Skottfelt, C. Snodgrass, J. Southworth, C. von Essen

^*Corresponding author for this work

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

Abstract

We report the discovery of a cold Super-Earth planet (m(p) = 4.4 +/- 0.5 M⊙) orbiting a low-mass (M = 0.23 +/- 0.03 M_⊙) M dwarf at projected separation a⊥ = 1.18 ± 0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, D_L = 0.86 ± 0.09 kpc. Indeed, it was the large lens-source relative parallax Π_rel = 1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" π_E ∝ (Π_rel/M)^1/2 that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q <1 x 10^-4.

We apply a new planet-detection sensitivity method, which is a variant of "V/V_max", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN / d lnq ∝ q^P , with p =1.05(-0.68)(+0.78), which confirms the "turnover" in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 ± 0.13 at higher mass ratios q greater than or similar to 2 x 10^-4. We combine our result with that of Suzuki et al. to obtain p = 0.73(-0.34)(+0.42).

Original language	English
Pages (from-to)	1-42
Journal	Acta Astronomica
Volume	68
Issue number	1
Publication status	Published - 2018

Keywords

Gravitational lensing: micro
Planetary systems

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OGLE-2017-BLG-1434Lb: Eighth q<1x10-4 Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function v(dataset)
Udalski, A. (Creator), Ryu, Y.-H. (Creator), Sajadian, S. (Creator), Gould, A. (Creator), Mroz, P. (Creator), Poleski, R. (Creator), Szymanski, M. K. (Creator), Skowron, J. (Creator), Soszynski (Creator), Kozlowski, S. (Creator), Pietrukowicz, P. (Creator), Ulaczyk, K. (Creator), Pawlak, M. (Creator), Rybicki, K. (Creator), Iwanek, P. (Creator), Albrow, M. D. (Creator), Chung, S.-J. (Creator), Han, C. (Creator), Hwang, K.-H. (Creator), Jung, Y. K. (Creator), Shin, I.-G. (Creator), Shvartzvald, Y. (Creator), Yee, J. C. (Creator), Zang, W. (Creator), Zhu, W. (Creator), Cha, S.-M. (Creator), Kim, D.-J. (Creator), Kim, H.-W. (Creator), Kim, S.-L. (Creator), Lee, C.-U. (Creator), Lee, D.-J. (Creator), Lee, Y. (Creator), Park, B.-G. (Creator), Pogge, R. W. (Creator), Bozza (Creator), Dominik, M. (Creator), Helling, C. (Creator), Hundertmark, M. P. G. (Creator), Jorgensen, U. G. (Creator), Longa-Pena, P. (Creator), Lowry, S. (Creator), Burgdorf, M. (Creator), Campbell-White, J. (Creator), Ciceri, S. (Creator), Evans, D. (Creator), Figuera Jaimes, R. J. (Creator), Fujii, Y. (Creator), Haikala, L. K. (Creator), Henning, T. (Creator), Hinse, T. C. (Creator), Mancini, L. (Creator), Peixinho, N. (Creator), Rahvar, S. (Creator), Rabus, M. (Creator), Skottfelt, J. (Creator), Snodgrass, C. (Creator), Southworth, J. (Creator) & von Essen, C. (Creator), NASA Exoplanet Science Institute, 2018
https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=OGLE-2017-BLG-1434L+b
Dataset

Cite this

Udalski, A., Ryu, Y.-H., Sajadian, S., Gould, A., Mroz, P., Poleski, R., Szymanski, M. K., Skowron, J., Soszynski, Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S.-J., Han, C., Hwang, K.-H., ... von Essen, C. (2018). OGLE-2017-BLG-1434Lb: eighth q <1 x 10^-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function. Acta Astronomica, 68(1), 1-42. https://arxiv.org/abs/1802.02582

@article{ee8029646b6345b18fc2aa1062f2df57,

title = "OGLE-2017-BLG-1434Lb: eighth q <1 x 10-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function",

abstract = "We report the discovery of a cold Super-Earth planet (m(p) = 4.4 +/- 0.5 M⊙) orbiting a low-mass (M = 0.23 +/- 0.03 M⊙) M dwarf at projected separation a⊥ = 1.18 ± 0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, DL = 0.86 ± 0.09 kpc. Indeed, it was the large lens-source relative parallax Πrel = 1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, {"}microlens parallax{"} πE ∝ (Πrel/M)1/2 that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q <1 x 10-4.We apply a new planet-detection sensitivity method, which is a variant of {"}V/Vmax{"}, to seven of these eight planets to derive the mass-ratio function in this regime. We find dN / d lnq ∝ qP , with p =1.05(-0.68)(+0.78), which confirms the {"}turnover{"} in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 ± 0.13 at higher mass ratios q greater than or similar to 2 x 10-4. We combine our result with that of Suzuki et al. to obtain p = 0.73(-0.34)(+0.42).",

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

author = "A. Udalski and Y-H Ryu and S. Sajadian and A. Gould and P. Mroz and R. Poleski and Szymanski, {M. K.} and J. Skowron and Soszynski and S. Kozlowski and P. Pietrukowicz and K. Ulaczyk and M. Pawlak and K. Rybicki and P. Iwanek and Albrow, {M. D.} and S-J Chung and C. Han and K-H Hwang and Jung, {Y. K.} and I-G Shin and Y. Shvartzvald and Yee, {J. C.} and W. Zang and W. Zhu and S-M Cha and D-J Kim and H-W Kim and S-L Kim and C-U Lee and D-J Lee and Y. Lee and B-G Park and Pogge, {R. W.} and Bozza and M. Dominik and C. Helling and M. Hundertmark and Jorgensen, {U. G.} and P. Longa-Pena and S. Lowry and M. Burgdorf and J. Campbell-White and S. Ciceri and D. Evans and Jaimes, {R. Figuera} and Y. Fujii and Haikala, {L. K.} and T. Henning and Hinse, {T. C.} and L. Mancini and N. Peixinho and S. Rahvar and M. Rabus and J. Skottfelt and C. Snodgrass and J. Southworth and {von Essen}, C.",

note = "Work by WZ, YKJ, and AG were supported by AST-1516842 from the US NSF. WZ, IGS, and AG were supported by JPL grant 1500811. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. Work by YS was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association through a contract with NASA.",

year = "2018",

language = "English",

volume = "68",

pages = "1--42",

journal = "Acta Astronomica",

issn = "0001-5237",

publisher = "COPERNICUS FOUNDATION POLISH ASTRONOMY",

number = "1",

}

Udalski, A, Ryu, Y-H, Sajadian, S, Gould, A, Mroz, P, Poleski, R, Szymanski, MK, Skowron, J, Soszynski, Kozlowski, S, Pietrukowicz, P, Ulaczyk, K, Pawlak, M, Rybicki, K, Iwanek, P, Albrow, MD, Chung, S-J, Han, C, Hwang, K-H, Jung, YK, Shin, I-G, Shvartzvald, Y, Yee, JC, Zang, W, Zhu, W, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, C-U, Lee, D-J, Lee, Y, Park, B-G, Pogge, RW, Bozza, , Dominik, M, Helling, C, Hundertmark, M, Jorgensen, UG, Longa-Pena, P, Lowry, S, Burgdorf, M, Campbell-White, J, Ciceri, S, Evans, D, Jaimes, RF, Fujii, Y, Haikala, LK, Henning, T, Hinse, TC, Mancini, L, Peixinho, N, Rahvar, S, Rabus, M, Skottfelt, J, Snodgrass, C, Southworth, J & von Essen, C 2018, 'OGLE-2017-BLG-1434Lb: eighth q <1 x 10^-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function', Acta Astronomica, vol. 68, no. 1, pp. 1-42. <https://arxiv.org/abs/1802.02582>

TY - JOUR

T1 - OGLE-2017-BLG-1434Lb

T2 - eighth q <1 x 10-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function

AU - Udalski, A.

AU - Ryu, Y-H

AU - Sajadian, S.

AU - Gould, A.

AU - Mroz, P.

AU - Poleski, R.

AU - Szymanski, M. K.

AU - Skowron, J.

AU - Soszynski, null

AU - Kozlowski, S.

AU - Pietrukowicz, P.

AU - Ulaczyk, K.

AU - Pawlak, M.

AU - Rybicki, K.

AU - Iwanek, P.

AU - Albrow, M. D.

AU - Chung, S-J

AU - Han, C.

AU - Hwang, K-H

AU - Jung, Y. K.

AU - Shin, I-G

AU - Shvartzvald, Y.

AU - Yee, J. C.

AU - Zang, W.

AU - Zhu, W.

AU - Cha, S-M

AU - Kim, D-J

AU - Kim, H-W

AU - Kim, S-L

AU - Lee, C-U

AU - Lee, D-J

AU - Lee, Y.

AU - Park, B-G

AU - Pogge, R. W.

AU - Bozza, null

AU - Dominik, M.

AU - Helling, C.

AU - Hundertmark, M.

AU - Jorgensen, U. G.

AU - Longa-Pena, P.

AU - Lowry, S.

AU - Burgdorf, M.

AU - Campbell-White, J.

AU - Ciceri, S.

AU - Evans, D.

AU - Jaimes, R. Figuera

AU - Fujii, Y.

AU - Haikala, L. K.

AU - Henning, T.

AU - Hinse, T. C.

AU - Mancini, L.

AU - Peixinho, N.

AU - Rahvar, S.

AU - Rabus, M.

AU - Skottfelt, J.

AU - Snodgrass, C.

AU - Southworth, J.

AU - von Essen, C.

N1 - Work by WZ, YKJ, and AG were supported by AST-1516842 from the US NSF. WZ, IGS, and AG were supported by JPL grant 1500811. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. Work by YS was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association through a contract with NASA.

PY - 2018

Y1 - 2018

N2 - We report the discovery of a cold Super-Earth planet (m(p) = 4.4 +/- 0.5 M⊙) orbiting a low-mass (M = 0.23 +/- 0.03 M⊙) M dwarf at projected separation a⊥ = 1.18 ± 0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, DL = 0.86 ± 0.09 kpc. Indeed, it was the large lens-source relative parallax Πrel = 1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" πE ∝ (Πrel/M)1/2 that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q <1 x 10-4.We apply a new planet-detection sensitivity method, which is a variant of "V/Vmax", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN / d lnq ∝ qP , with p =1.05(-0.68)(+0.78), which confirms the "turnover" in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 ± 0.13 at higher mass ratios q greater than or similar to 2 x 10-4. We combine our result with that of Suzuki et al. to obtain p = 0.73(-0.34)(+0.42).

AB - We report the discovery of a cold Super-Earth planet (m(p) = 4.4 +/- 0.5 M⊙) orbiting a low-mass (M = 0.23 +/- 0.03 M⊙) M dwarf at projected separation a⊥ = 1.18 ± 0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, DL = 0.86 ± 0.09 kpc. Indeed, it was the large lens-source relative parallax Πrel = 1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" πE ∝ (Πrel/M)1/2 that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q <1 x 10-4.We apply a new planet-detection sensitivity method, which is a variant of "V/Vmax", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN / d lnq ∝ qP , with p =1.05(-0.68)(+0.78), which confirms the "turnover" in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 ± 0.13 at higher mass ratios q greater than or similar to 2 x 10-4. We combine our result with that of Suzuki et al. to obtain p = 0.73(-0.34)(+0.42).

KW - Gravitational lensing: micro

KW - Planetary systems

M3 - Article

SN - 0001-5237

VL - 68

SP - 1

EP - 42

JO - Acta Astronomica

JF - Acta Astronomica

IS - 1

ER -

OGLE-2017-BLG-1434Lb: eighth q <1 x 10-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function

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OGLE-2017-BLG-1434Lb: Eighth q<1x10-4 Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function v(dataset)

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OGLE-2017-BLG-1434Lb: eighth q <1 x 10^-4 mass-ratio microlens planet confirms turnover in planet mass-ratio function