HAT-P-11b: A super-neptune planet transiting a bright K star in the kepler field

G. Á Bakos, G. Torres, A. Pál, J. Hartman, Géza Kovács, R. W. Noyes, D. W. Latham, D. D. Sasselov, B. Sipõcz, G. A. Esquerdo, D. A. Fischer, J. A. Johnson, G. W. Marcy, R. P. Butler, H. Isaacson, A. Howard, S. Vogt, Gbor Kovács, J. Fernandez, A. MoórR. P. Stefanik, J. Lázár, I. Papp, P. Sári

Research output: Contribution to journalArticle

211 Citations (Scopus)

Abstract

We report on the discovery of HAT-P-11b, the smallest radius transiting extrasolar planet (TEP) discovered from the ground, and the first hot Neptune discovered to date by transit searches. HAT-P-11b orbits the bright (V= 9.587) and metal rich ([Fe/H] = +0.31±0.05) K4 dwarf star GSC 03561-02092 with P = 4.8878162±0.0000071days and produces a transit signal with depth of 4.2mmag, the shallowest found by transit searches that is due to a confirmed planet. We present a global analysis of the available photometric and radial velocity (RV) data that result in stellar and planetary parameters, with simultaneous treatment of systematic variations. The planet, like its near-twin GJ436b, is somewhat larger than Neptune (17 M, 3.8 R ) both in mass Mp = 0.081±0.009 M J(25.8±2.9 M) and radius Rp = 0.422±0.014 R J(4.73±0.16 R). HAT-P-11b orbits in an eccentric orbit with e = 0.198 0.046 and ω = 3552 173, causing a reflex motion of its parent star with amplitude 11.6±1.2m s-1, a challenging detection due to the high level of chromospheric activity of the parent star. Our ephemeris for the transit events is T c = 2454605.89132 0.00032 (BJD), with duration 0.0957 0.0012days, and secondary eclipse epoch of 2454608.96 0.15days (BJD). The basic stellar parameters of the host star are M = 0.809+0.020 -0.027 M*, R* = 0.752 0.021 R, and T eff* = 4780±50K. Importantly, HAT-P-11 will lie on one of the detectors of the forthcoming Kepler mission; this should make possible fruitful investigations of the detailed physical characteristic of both the planet and its parent star at unprecedented precision. We discuss an interesting constraint on the eccentricity of the system by the transit light curve and stellar parameters. This will be particularly useful for eccentric TEPs with low-amplitude RV variations in Kepler's field. We also present a blend analysis, that for the first time treats the case of a blended transiting hot Jupiter mimicking a transiting hot Neptune, and proves that HAT-P-11b is not such a blend.

Original languageEnglish
Pages (from-to)1724-1745
Number of pages22
JournalAstrophysical Journal
Volume710
Issue number2
DOIs
Publication statusPublished - 2010

Fingerprint

K stars
Neptune (planet)
Neptune
transit
planet
planets
stars
radial velocity
transparent exopolymer particle
Kepler mission
orbits
dwarf stars
eccentric orbits
reflexes
eccentricity
radii
Jupiter
eccentrics
eclipses
extrasolar planets

Keywords

  • Planetary systems
  • Stars: individual (HAT-P-11, GSC 03561 02092)
  • Techniques: photometric
  • Techniques: spectroscopic

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics
  • Nuclear and High Energy Physics

Cite this

HAT-P-11b : A super-neptune planet transiting a bright K star in the kepler field. / Bakos, G. Á; Torres, G.; Pál, A.; Hartman, J.; Kovács, Géza; Noyes, R. W.; Latham, D. W.; Sasselov, D. D.; Sipõcz, B.; Esquerdo, G. A.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Butler, R. P.; Isaacson, H.; Howard, A.; Vogt, S.; Kovács, Gbor; Fernandez, J.; Moór, A.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.

In: Astrophysical Journal, Vol. 710, No. 2, 2010, p. 1724-1745.

Research output: Contribution to journalArticle

Bakos, GÁ, Torres, G, Pál, A, Hartman, J, Kovács, G, Noyes, RW, Latham, DW, Sasselov, DD, Sipõcz, B, Esquerdo, GA, Fischer, DA, Johnson, JA, Marcy, GW, Butler, RP, Isaacson, H, Howard, A, Vogt, S, Kovács, G, Fernandez, J, Moór, A, Stefanik, RP, Lázár, J, Papp, I & Sári, P 2010, 'HAT-P-11b: A super-neptune planet transiting a bright K star in the kepler field', Astrophysical Journal, vol. 710, no. 2, pp. 1724-1745. https://doi.org/10.1088/0004-637X/710/2/1724
Bakos, G. Á ; Torres, G. ; Pál, A. ; Hartman, J. ; Kovács, Géza ; Noyes, R. W. ; Latham, D. W. ; Sasselov, D. D. ; Sipõcz, B. ; Esquerdo, G. A. ; Fischer, D. A. ; Johnson, J. A. ; Marcy, G. W. ; Butler, R. P. ; Isaacson, H. ; Howard, A. ; Vogt, S. ; Kovács, Gbor ; Fernandez, J. ; Moór, A. ; Stefanik, R. P. ; Lázár, J. ; Papp, I. ; Sári, P. / HAT-P-11b : A super-neptune planet transiting a bright K star in the kepler field. In: Astrophysical Journal. 2010 ; Vol. 710, No. 2. pp. 1724-1745.
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T1 - HAT-P-11b

T2 - A super-neptune planet transiting a bright K star in the kepler field

AU - Bakos, G. Á

AU - Torres, G.

AU - Pál, A.

AU - Hartman, J.

AU - Kovács, Géza

AU - Noyes, R. W.

AU - Latham, D. W.

AU - Sasselov, D. D.

AU - Sipõcz, B.

AU - Esquerdo, G. A.

AU - Fischer, D. A.

AU - Johnson, J. A.

AU - Marcy, G. W.

AU - Butler, R. P.

AU - Isaacson, H.

AU - Howard, A.

AU - Vogt, S.

AU - Kovács, Gbor

AU - Fernandez, J.

AU - Moór, A.

AU - Stefanik, R. P.

AU - Lázár, J.

AU - Papp, I.

AU - Sári, P.

PY - 2010

Y1 - 2010

N2 - We report on the discovery of HAT-P-11b, the smallest radius transiting extrasolar planet (TEP) discovered from the ground, and the first hot Neptune discovered to date by transit searches. HAT-P-11b orbits the bright (V= 9.587) and metal rich ([Fe/H] = +0.31±0.05) K4 dwarf star GSC 03561-02092 with P = 4.8878162±0.0000071days and produces a transit signal with depth of 4.2mmag, the shallowest found by transit searches that is due to a confirmed planet. We present a global analysis of the available photometric and radial velocity (RV) data that result in stellar and planetary parameters, with simultaneous treatment of systematic variations. The planet, like its near-twin GJ436b, is somewhat larger than Neptune (17 M⊕, 3.8 R ⊕) both in mass Mp = 0.081±0.009 M J(25.8±2.9 M⊕) and radius Rp = 0.422±0.014 R J(4.73±0.16 R⊕). HAT-P-11b orbits in an eccentric orbit with e = 0.198 0.046 and ω = 3552 173, causing a reflex motion of its parent star with amplitude 11.6±1.2m s-1, a challenging detection due to the high level of chromospheric activity of the parent star. Our ephemeris for the transit events is T c = 2454605.89132 0.00032 (BJD), with duration 0.0957 0.0012days, and secondary eclipse epoch of 2454608.96 0.15days (BJD). The basic stellar parameters of the host star are M = 0.809+0.020 -0.027 M*, R* = 0.752 0.021 R, and T eff* = 4780±50K. Importantly, HAT-P-11 will lie on one of the detectors of the forthcoming Kepler mission; this should make possible fruitful investigations of the detailed physical characteristic of both the planet and its parent star at unprecedented precision. We discuss an interesting constraint on the eccentricity of the system by the transit light curve and stellar parameters. This will be particularly useful for eccentric TEPs with low-amplitude RV variations in Kepler's field. We also present a blend analysis, that for the first time treats the case of a blended transiting hot Jupiter mimicking a transiting hot Neptune, and proves that HAT-P-11b is not such a blend.

AB - We report on the discovery of HAT-P-11b, the smallest radius transiting extrasolar planet (TEP) discovered from the ground, and the first hot Neptune discovered to date by transit searches. HAT-P-11b orbits the bright (V= 9.587) and metal rich ([Fe/H] = +0.31±0.05) K4 dwarf star GSC 03561-02092 with P = 4.8878162±0.0000071days and produces a transit signal with depth of 4.2mmag, the shallowest found by transit searches that is due to a confirmed planet. We present a global analysis of the available photometric and radial velocity (RV) data that result in stellar and planetary parameters, with simultaneous treatment of systematic variations. The planet, like its near-twin GJ436b, is somewhat larger than Neptune (17 M⊕, 3.8 R ⊕) both in mass Mp = 0.081±0.009 M J(25.8±2.9 M⊕) and radius Rp = 0.422±0.014 R J(4.73±0.16 R⊕). HAT-P-11b orbits in an eccentric orbit with e = 0.198 0.046 and ω = 3552 173, causing a reflex motion of its parent star with amplitude 11.6±1.2m s-1, a challenging detection due to the high level of chromospheric activity of the parent star. Our ephemeris for the transit events is T c = 2454605.89132 0.00032 (BJD), with duration 0.0957 0.0012days, and secondary eclipse epoch of 2454608.96 0.15days (BJD). The basic stellar parameters of the host star are M = 0.809+0.020 -0.027 M*, R* = 0.752 0.021 R, and T eff* = 4780±50K. Importantly, HAT-P-11 will lie on one of the detectors of the forthcoming Kepler mission; this should make possible fruitful investigations of the detailed physical characteristic of both the planet and its parent star at unprecedented precision. We discuss an interesting constraint on the eccentricity of the system by the transit light curve and stellar parameters. This will be particularly useful for eccentric TEPs with low-amplitude RV variations in Kepler's field. We also present a blend analysis, that for the first time treats the case of a blended transiting hot Jupiter mimicking a transiting hot Neptune, and proves that HAT-P-11b is not such a blend.

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KW - Stars: individual (HAT-P-11, GSC 03561 02092)

KW - Techniques: photometric

KW - Techniques: spectroscopic

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