Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant

Bo Ma, Jian Ge, Rory Barnes, Justin R. Crepp, Nathan De Lee, Leticia Dutra-Ferreira, Massimiliano Esposito, Bruno Femenia, Scott W. Fleming, B. Scott Gaudi, Luan Ghezzi, Leslie Hebb, Jonay I. Gonzalez Hernandez, Brian L. Lee, G. F.Porto De Mello, Keivan G. Stassun, Ji Wang, Johnp Wisniewski, Eric Agol, Dmitry Bizyaev & 28 others Phillip Cargile, Liang Chang, Luiz Nicolaci Da Costa, Jasond Eastman, Bruce Gary, Peng Jiang, Stephen R. Kane, Rui Li, Jian Liu, Suvrath Mahadevan, Marcioa G. Maia, Demitri Muna, Duy Cuong Nguyen, Ricardo L.C. Ogando, Daniel Oravetz, Joshua Pepper, Martin Paegert, Carlos Allende Prieto, Rafael Rebolo, Basilio X. Santiago, Donald P. Schneider, Alaina Shelden, Audrey Simmons, Thirupathi Sivarani, J. C. Van Eyken, Xiaoke Wan, Benjamin A. Weaver, Bo Zhao

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

We present an eccentric, short-period brown dwarf candidate orbiting the active, slightly evolved subgiant star TYC2087-00255-1, which has effective temperature T eff = 5903 ± 42K, surface gravity log (g) = 4.07 ± 0.16(cgs), and metallicity [Fe/H] = -0.23 ± 0.07. This candidate was discovered using data from the first two years of the Multi-object APO Radial Velocity Exoplanets Large-area Survey, which is part of the third phase of Sloan Digital Sky Survey. From our 38 radial velocity measurements spread over a two-year time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 3.571 ± 0.041kms-1, period P = 9.0090 ± 0.0004days, and eccentricity e = 0.226 ± 0.011. Adopting a mass of 1.16 ± 0.11 M· for the subgiant host star, we infer that the companion has a minimum mass of 40.0 ± 2.5 M ·Jup. Assuming an edge-on orbit, the semimajor axis is 0.090 ± 0.003AU. The host star is photometrically variable at the sim;1% level with a period of sim;13.16 ± 0.01 days, indicating that the host star spin and companion orbit are not synchronized. Through adaptive optics imaging we also found a point source 643 ± 10 mas away from TYC2087-00255-1, which would have a mass of 0.13 M· if it is physically associated with TYC2087-00255-1 and has the same age. Future proper motion observation should be able to resolve if this tertiary object is physically associated with TYC2087-00255-1 and make TYC2087-00255-1 a triple body system. Core Ca II H and K line emission indicate that the host is chromospherically active, at a level that is consistent with the inferred spin period and measured v rotsin i, but unusual for a subgiant of this T eff. This activity could be explained by ongoing tidal spin-up of the host star by the companion.

Original languageEnglish (US)
Article number20
JournalAstronomical Journal
Volume145
Issue number1
DOIs
StatePublished - Jan 1 2013

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subgiant stars
stars
radial velocity
H lines
orbits
K lines
eccentrics
proper motion
extrasolar planets
eccentricity
adaptive optics
velocity measurement
point sources
metallicity
gravitation
orbitals
point source
gravity
temperature

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ma, Bo ; Ge, Jian ; Barnes, Rory ; Crepp, Justin R. ; De Lee, Nathan ; Dutra-Ferreira, Leticia ; Esposito, Massimiliano ; Femenia, Bruno ; Fleming, Scott W. ; Gaudi, B. Scott ; Ghezzi, Luan ; Hebb, Leslie ; Gonzalez Hernandez, Jonay I. ; Lee, Brian L. ; De Mello, G. F.Porto ; Stassun, Keivan G. ; Wang, Ji ; Wisniewski, Johnp ; Agol, Eric ; Bizyaev, Dmitry ; Cargile, Phillip ; Chang, Liang ; Da Costa, Luiz Nicolaci ; Eastman, Jasond ; Gary, Bruce ; Jiang, Peng ; Kane, Stephen R. ; Li, Rui ; Liu, Jian ; Mahadevan, Suvrath ; Maia, Marcioa G. ; Muna, Demitri ; Nguyen, Duy Cuong ; Ogando, Ricardo L.C. ; Oravetz, Daniel ; Pepper, Joshua ; Paegert, Martin ; Allende Prieto, Carlos ; Rebolo, Rafael ; Santiago, Basilio X. ; Schneider, Donald P. ; Shelden, Alaina ; Simmons, Audrey ; Sivarani, Thirupathi ; Van Eyken, J. C. ; Wan, Xiaoke ; Weaver, Benjamin A. ; Zhao, Bo. / Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant. In: Astronomical Journal. 2013 ; Vol. 145, No. 1.
@article{799027dea97346eb9e9916ddc2515201,
title = "Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant",
abstract = "We present an eccentric, short-period brown dwarf candidate orbiting the active, slightly evolved subgiant star TYC2087-00255-1, which has effective temperature T eff = 5903 ± 42K, surface gravity log (g) = 4.07 ± 0.16(cgs), and metallicity [Fe/H] = -0.23 ± 0.07. This candidate was discovered using data from the first two years of the Multi-object APO Radial Velocity Exoplanets Large-area Survey, which is part of the third phase of Sloan Digital Sky Survey. From our 38 radial velocity measurements spread over a two-year time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 3.571 ± 0.041kms-1, period P = 9.0090 ± 0.0004days, and eccentricity e = 0.226 ± 0.011. Adopting a mass of 1.16 ± 0.11 M· for the subgiant host star, we infer that the companion has a minimum mass of 40.0 ± 2.5 M ·Jup. Assuming an edge-on orbit, the semimajor axis is 0.090 ± 0.003AU. The host star is photometrically variable at the sim;1{\%} level with a period of sim;13.16 ± 0.01 days, indicating that the host star spin and companion orbit are not synchronized. Through adaptive optics imaging we also found a point source 643 ± 10 mas away from TYC2087-00255-1, which would have a mass of 0.13 M· if it is physically associated with TYC2087-00255-1 and has the same age. Future proper motion observation should be able to resolve if this tertiary object is physically associated with TYC2087-00255-1 and make TYC2087-00255-1 a triple body system. Core Ca II H and K line emission indicate that the host is chromospherically active, at a level that is consistent with the inferred spin period and measured v rotsin i, but unusual for a subgiant of this T eff. This activity could be explained by ongoing tidal spin-up of the host star by the companion.",
author = "Bo Ma and Jian Ge and Rory Barnes and Crepp, {Justin R.} and {De Lee}, Nathan and Leticia Dutra-Ferreira and Massimiliano Esposito and Bruno Femenia and Fleming, {Scott W.} and Gaudi, {B. Scott} and Luan Ghezzi and Leslie Hebb and {Gonzalez Hernandez}, {Jonay I.} and Lee, {Brian L.} and {De Mello}, {G. F.Porto} and Stassun, {Keivan G.} and Ji Wang and Johnp Wisniewski and Eric Agol and Dmitry Bizyaev and Phillip Cargile and Liang Chang and {Da Costa}, {Luiz Nicolaci} and Jasond Eastman and Bruce Gary and Peng Jiang and Kane, {Stephen R.} and Rui Li and Jian Liu and Suvrath Mahadevan and Maia, {Marcioa G.} and Demitri Muna and Nguyen, {Duy Cuong} and Ogando, {Ricardo L.C.} and Daniel Oravetz and Joshua Pepper and Martin Paegert and {Allende Prieto}, Carlos and Rafael Rebolo and Santiago, {Basilio X.} and Schneider, {Donald P.} and Alaina Shelden and Audrey Simmons and Thirupathi Sivarani and {Van Eyken}, {J. C.} and Xiaoke Wan and Weaver, {Benjamin A.} and Bo Zhao",
year = "2013",
month = "1",
day = "1",
doi = "10.1088/0004-6256/145/1/20",
language = "English (US)",
volume = "145",
journal = "Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "1",

}

Ma, B, Ge, J, Barnes, R, Crepp, JR, De Lee, N, Dutra-Ferreira, L, Esposito, M, Femenia, B, Fleming, SW, Gaudi, BS, Ghezzi, L, Hebb, L, Gonzalez Hernandez, JI, Lee, BL, De Mello, GFP, Stassun, KG, Wang, J, Wisniewski, J, Agol, E, Bizyaev, D, Cargile, P, Chang, L, Da Costa, LN, Eastman, J, Gary, B, Jiang, P, Kane, SR, Li, R, Liu, J, Mahadevan, S, Maia, MG, Muna, D, Nguyen, DC, Ogando, RLC, Oravetz, D, Pepper, J, Paegert, M, Allende Prieto, C, Rebolo, R, Santiago, BX, Schneider, DP, Shelden, A, Simmons, A, Sivarani, T, Van Eyken, JC, Wan, X, Weaver, BA & Zhao, B 2013, 'Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant', Astronomical Journal, vol. 145, no. 1, 20. https://doi.org/10.1088/0004-6256/145/1/20

Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant. / Ma, Bo; Ge, Jian; Barnes, Rory; Crepp, Justin R.; De Lee, Nathan; Dutra-Ferreira, Leticia; Esposito, Massimiliano; Femenia, Bruno; Fleming, Scott W.; Gaudi, B. Scott; Ghezzi, Luan; Hebb, Leslie; Gonzalez Hernandez, Jonay I.; Lee, Brian L.; De Mello, G. F.Porto; Stassun, Keivan G.; Wang, Ji; Wisniewski, Johnp; Agol, Eric; Bizyaev, Dmitry; Cargile, Phillip; Chang, Liang; Da Costa, Luiz Nicolaci; Eastman, Jasond; Gary, Bruce; Jiang, Peng; Kane, Stephen R.; Li, Rui; Liu, Jian; Mahadevan, Suvrath; Maia, Marcioa G.; Muna, Demitri; Nguyen, Duy Cuong; Ogando, Ricardo L.C.; Oravetz, Daniel; Pepper, Joshua; Paegert, Martin; Allende Prieto, Carlos; Rebolo, Rafael; Santiago, Basilio X.; Schneider, Donald P.; Shelden, Alaina; Simmons, Audrey; Sivarani, Thirupathi; Van Eyken, J. C.; Wan, Xiaoke; Weaver, Benjamin A.; Zhao, Bo.

In: Astronomical Journal, Vol. 145, No. 1, 20, 01.01.2013.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Very-low-mass stellar and substellar companions to solar-like stars from marvels. III. A short-period brown dwarf candidate around an active g0iv subgiant

AU - Ma, Bo

AU - Ge, Jian

AU - Barnes, Rory

AU - Crepp, Justin R.

AU - De Lee, Nathan

AU - Dutra-Ferreira, Leticia

AU - Esposito, Massimiliano

AU - Femenia, Bruno

AU - Fleming, Scott W.

AU - Gaudi, B. Scott

AU - Ghezzi, Luan

AU - Hebb, Leslie

AU - Gonzalez Hernandez, Jonay I.

AU - Lee, Brian L.

AU - De Mello, G. F.Porto

AU - Stassun, Keivan G.

AU - Wang, Ji

AU - Wisniewski, Johnp

AU - Agol, Eric

AU - Bizyaev, Dmitry

AU - Cargile, Phillip

AU - Chang, Liang

AU - Da Costa, Luiz Nicolaci

AU - Eastman, Jasond

AU - Gary, Bruce

AU - Jiang, Peng

AU - Kane, Stephen R.

AU - Li, Rui

AU - Liu, Jian

AU - Mahadevan, Suvrath

AU - Maia, Marcioa G.

AU - Muna, Demitri

AU - Nguyen, Duy Cuong

AU - Ogando, Ricardo L.C.

AU - Oravetz, Daniel

AU - Pepper, Joshua

AU - Paegert, Martin

AU - Allende Prieto, Carlos

AU - Rebolo, Rafael

AU - Santiago, Basilio X.

AU - Schneider, Donald P.

AU - Shelden, Alaina

AU - Simmons, Audrey

AU - Sivarani, Thirupathi

AU - Van Eyken, J. C.

AU - Wan, Xiaoke

AU - Weaver, Benjamin A.

AU - Zhao, Bo

PY - 2013/1/1

Y1 - 2013/1/1

N2 - We present an eccentric, short-period brown dwarf candidate orbiting the active, slightly evolved subgiant star TYC2087-00255-1, which has effective temperature T eff = 5903 ± 42K, surface gravity log (g) = 4.07 ± 0.16(cgs), and metallicity [Fe/H] = -0.23 ± 0.07. This candidate was discovered using data from the first two years of the Multi-object APO Radial Velocity Exoplanets Large-area Survey, which is part of the third phase of Sloan Digital Sky Survey. From our 38 radial velocity measurements spread over a two-year time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 3.571 ± 0.041kms-1, period P = 9.0090 ± 0.0004days, and eccentricity e = 0.226 ± 0.011. Adopting a mass of 1.16 ± 0.11 M· for the subgiant host star, we infer that the companion has a minimum mass of 40.0 ± 2.5 M ·Jup. Assuming an edge-on orbit, the semimajor axis is 0.090 ± 0.003AU. The host star is photometrically variable at the sim;1% level with a period of sim;13.16 ± 0.01 days, indicating that the host star spin and companion orbit are not synchronized. Through adaptive optics imaging we also found a point source 643 ± 10 mas away from TYC2087-00255-1, which would have a mass of 0.13 M· if it is physically associated with TYC2087-00255-1 and has the same age. Future proper motion observation should be able to resolve if this tertiary object is physically associated with TYC2087-00255-1 and make TYC2087-00255-1 a triple body system. Core Ca II H and K line emission indicate that the host is chromospherically active, at a level that is consistent with the inferred spin period and measured v rotsin i, but unusual for a subgiant of this T eff. This activity could be explained by ongoing tidal spin-up of the host star by the companion.

AB - We present an eccentric, short-period brown dwarf candidate orbiting the active, slightly evolved subgiant star TYC2087-00255-1, which has effective temperature T eff = 5903 ± 42K, surface gravity log (g) = 4.07 ± 0.16(cgs), and metallicity [Fe/H] = -0.23 ± 0.07. This candidate was discovered using data from the first two years of the Multi-object APO Radial Velocity Exoplanets Large-area Survey, which is part of the third phase of Sloan Digital Sky Survey. From our 38 radial velocity measurements spread over a two-year time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 3.571 ± 0.041kms-1, period P = 9.0090 ± 0.0004days, and eccentricity e = 0.226 ± 0.011. Adopting a mass of 1.16 ± 0.11 M· for the subgiant host star, we infer that the companion has a minimum mass of 40.0 ± 2.5 M ·Jup. Assuming an edge-on orbit, the semimajor axis is 0.090 ± 0.003AU. The host star is photometrically variable at the sim;1% level with a period of sim;13.16 ± 0.01 days, indicating that the host star spin and companion orbit are not synchronized. Through adaptive optics imaging we also found a point source 643 ± 10 mas away from TYC2087-00255-1, which would have a mass of 0.13 M· if it is physically associated with TYC2087-00255-1 and has the same age. Future proper motion observation should be able to resolve if this tertiary object is physically associated with TYC2087-00255-1 and make TYC2087-00255-1 a triple body system. Core Ca II H and K line emission indicate that the host is chromospherically active, at a level that is consistent with the inferred spin period and measured v rotsin i, but unusual for a subgiant of this T eff. This activity could be explained by ongoing tidal spin-up of the host star by the companion.

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U2 - 10.1088/0004-6256/145/1/20

DO - 10.1088/0004-6256/145/1/20

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JO - Astronomical Journal

JF - Astronomical Journal

SN - 0004-6256

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