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The HARPS-N Rocky Planet Search: I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun

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The HARPS-N Rocky Planet Search : I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun. / Motalebi, F.; Udry, S.; Gillon, M.; Lovis, C.; Ségransan, D.; Buchhave, Lars A.; Demory, B. O.; Malavolta, L.; Dressing, C. D.; Sasselov, D.; Rice, K.; Charbonneau, D.; Collier Cameron, A.; Latham, D.; Molinari, E.; Pepe, F.; Affer, L.; Bonomo, A. S.; Cosentino, R.; Dumusque, X.; Figueira, P.; Fiorenzano, A. F M; Gettel, S.; Harutyunyan, A.; Haywood, R. D.; Johnson, J.; Lopez, E.; Lopez-Morales, M.; Mayor, M.; Micela, G.; Mortier, A.; Nascimbeni, V.; Philips, D.; Piotto, G.; Pollacco, D.; Queloz, D.; Sozzetti, A.; Vanderburg, A.; Watson, C. A.

I: Astronomy & Astrophysics, Bind 584, A72, 2015.

Publikation: Bidrag til tidsskriftTidsskriftartikelForskningfagfællebedømt

Harvard

Motalebi, F, Udry, S, Gillon, M, Lovis, C, Ségransan, D, Buchhave, LA, Demory, BO, Malavolta, L, Dressing, CD, Sasselov, D, Rice, K, Charbonneau, D, Collier Cameron, A, Latham, D, Molinari, E, Pepe, F, Affer, L, Bonomo, AS, Cosentino, R, Dumusque, X, Figueira, P, Fiorenzano, AFM, Gettel, S, Harutyunyan, A, Haywood, RD, Johnson, J, Lopez, E, Lopez-Morales, M, Mayor, M, Micela, G, Mortier, A, Nascimbeni, V, Philips, D, Piotto, G, Pollacco, D, Queloz, D, Sozzetti, A, Vanderburg, A & Watson, CA 2015, 'The HARPS-N Rocky Planet Search: I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun', Astronomy & Astrophysics, bind 584, A72. https://doi.org/10.1051/0004-6361/201526822

APA

Motalebi, F., Udry, S., Gillon, M., Lovis, C., Ségransan, D., Buchhave, L. A., Demory, B. O., Malavolta, L., Dressing, C. D., Sasselov, D., Rice, K., Charbonneau, D., Collier Cameron, A., Latham, D., Molinari, E., Pepe, F., Affer, L., Bonomo, A. S., Cosentino, R., ... Watson, C. A. (2015). The HARPS-N Rocky Planet Search: I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun. Astronomy & Astrophysics, 584, [A72]. https://doi.org/10.1051/0004-6361/201526822

Vancouver

Motalebi F, Udry S, Gillon M, Lovis C, Ségransan D, Buchhave LA o.a. The HARPS-N Rocky Planet Search: I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun. Astronomy & Astrophysics. 2015;584. A72. https://doi.org/10.1051/0004-6361/201526822

Author

Motalebi, F. ; Udry, S. ; Gillon, M. ; Lovis, C. ; Ségransan, D. ; Buchhave, Lars A. ; Demory, B. O. ; Malavolta, L. ; Dressing, C. D. ; Sasselov, D. ; Rice, K. ; Charbonneau, D. ; Collier Cameron, A. ; Latham, D. ; Molinari, E. ; Pepe, F. ; Affer, L. ; Bonomo, A. S. ; Cosentino, R. ; Dumusque, X. ; Figueira, P. ; Fiorenzano, A. F M ; Gettel, S. ; Harutyunyan, A. ; Haywood, R. D. ; Johnson, J. ; Lopez, E. ; Lopez-Morales, M. ; Mayor, M. ; Micela, G. ; Mortier, A. ; Nascimbeni, V. ; Philips, D. ; Piotto, G. ; Pollacco, D. ; Queloz, D. ; Sozzetti, A. ; Vanderburg, A. ; Watson, C. A. / The HARPS-N Rocky Planet Search : I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun. I: Astronomy & Astrophysics. 2015 ; Bind 584.

Bibtex

@article{22799ca16c8d415c81f441954dc73b3d,
title = "The HARPS-N Rocky Planet Search: I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun",
abstract = "We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V = 5.5) and close-by (6.5 pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935 ± 0.0003 days, on a quasi-circular orbit with a semi-major axis of 0.0382 ± 0.0003 AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date. From the amplitude of the radial velocity variation (2.25 ± 0.22 ms-1) and observed depth of the transit (359 ± 38 ppm), the planet mass and radius are estimated to be 4.36 ± 0.44 M⊕ and 1.606 ± 0.086 R⊕, leading to a mean density of 5.76 ± 1.09 g cm-3, suggesting a rocky composition. One additional planet with minimum-mass of 2.78 ± 0.65 M⊕ moves on a close-in, quasi-circular orbit with a period of 6.767 ± 0.004 days. The third planet in the system has a period of 46.66 ± 0.08 days and a minimum-mass of 8.94 ± 1.13 M⊕, at 0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ± 0.11. The period of this planet is close to the rotational period of the star estimated from variations of activity indicators (42.3 ± 0.1 days). The planetary origin of the signal is, however, thepreferred solution as no indication of variation at the corresponding frequency is observed for activity-sensitive parameters. Finally, a fourth additional longer-period planet of mass of 71 M⊕ orbits the star in 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at a distance of 2.56 AU.",
keywords = "Binaries: eclipsing, Instrumentation: spectrographs, Stars: individual: HD 219134, Techniques: photometric, Techniques: radial velocities",
author = "F. Motalebi and S. Udry and M. Gillon and C. Lovis and D. S{\'e}gransan and Buchhave, {Lars A.} and Demory, {B. O.} and L. Malavolta and Dressing, {C. D.} and D. Sasselov and K. Rice and D. Charbonneau and {Collier Cameron}, A. and D. Latham and E. Molinari and F. Pepe and L. Affer and Bonomo, {A. S.} and R. Cosentino and X. Dumusque and P. Figueira and Fiorenzano, {A. F M} and S. Gettel and A. Harutyunyan and Haywood, {R. D.} and J. Johnson and E. Lopez and M. Lopez-Morales and M. Mayor and G. Micela and A. Mortier and V. Nascimbeni and D. Philips and G. Piotto and D. Pollacco and D. Queloz and A. Sozzetti and A. Vanderburg and Watson, {C. A.}",
year = "2015",
doi = "10.1051/0004-6361/201526822",
language = "English",
volume = "584",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - The HARPS-N Rocky Planet Search

T2 - I. HD219134 b: a transiting rocky planet in a multi-planet system at 6.5 pc from the Sun

AU - Motalebi, F.

AU - Udry, S.

AU - Gillon, M.

AU - Lovis, C.

AU - Ségransan, D.

AU - Buchhave, Lars A.

AU - Demory, B. O.

AU - Malavolta, L.

AU - Dressing, C. D.

AU - Sasselov, D.

AU - Rice, K.

AU - Charbonneau, D.

AU - Collier Cameron, A.

AU - Latham, D.

AU - Molinari, E.

AU - Pepe, F.

AU - Affer, L.

AU - Bonomo, A. S.

AU - Cosentino, R.

AU - Dumusque, X.

AU - Figueira, P.

AU - Fiorenzano, A. F M

AU - Gettel, S.

AU - Harutyunyan, A.

AU - Haywood, R. D.

AU - Johnson, J.

AU - Lopez, E.

AU - Lopez-Morales, M.

AU - Mayor, M.

AU - Micela, G.

AU - Mortier, A.

AU - Nascimbeni, V.

AU - Philips, D.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Sozzetti, A.

AU - Vanderburg, A.

AU - Watson, C. A.

PY - 2015

Y1 - 2015

N2 - We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V = 5.5) and close-by (6.5 pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935 ± 0.0003 days, on a quasi-circular orbit with a semi-major axis of 0.0382 ± 0.0003 AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date. From the amplitude of the radial velocity variation (2.25 ± 0.22 ms-1) and observed depth of the transit (359 ± 38 ppm), the planet mass and radius are estimated to be 4.36 ± 0.44 M⊕ and 1.606 ± 0.086 R⊕, leading to a mean density of 5.76 ± 1.09 g cm-3, suggesting a rocky composition. One additional planet with minimum-mass of 2.78 ± 0.65 M⊕ moves on a close-in, quasi-circular orbit with a period of 6.767 ± 0.004 days. The third planet in the system has a period of 46.66 ± 0.08 days and a minimum-mass of 8.94 ± 1.13 M⊕, at 0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ± 0.11. The period of this planet is close to the rotational period of the star estimated from variations of activity indicators (42.3 ± 0.1 days). The planetary origin of the signal is, however, thepreferred solution as no indication of variation at the corresponding frequency is observed for activity-sensitive parameters. Finally, a fourth additional longer-period planet of mass of 71 M⊕ orbits the star in 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at a distance of 2.56 AU.

AB - We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V = 5.5) and close-by (6.5 pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935 ± 0.0003 days, on a quasi-circular orbit with a semi-major axis of 0.0382 ± 0.0003 AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date. From the amplitude of the radial velocity variation (2.25 ± 0.22 ms-1) and observed depth of the transit (359 ± 38 ppm), the planet mass and radius are estimated to be 4.36 ± 0.44 M⊕ and 1.606 ± 0.086 R⊕, leading to a mean density of 5.76 ± 1.09 g cm-3, suggesting a rocky composition. One additional planet with minimum-mass of 2.78 ± 0.65 M⊕ moves on a close-in, quasi-circular orbit with a period of 6.767 ± 0.004 days. The third planet in the system has a period of 46.66 ± 0.08 days and a minimum-mass of 8.94 ± 1.13 M⊕, at 0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ± 0.11. The period of this planet is close to the rotational period of the star estimated from variations of activity indicators (42.3 ± 0.1 days). The planetary origin of the signal is, however, thepreferred solution as no indication of variation at the corresponding frequency is observed for activity-sensitive parameters. Finally, a fourth additional longer-period planet of mass of 71 M⊕ orbits the star in 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at a distance of 2.56 AU.

KW - Binaries: eclipsing

KW - Instrumentation: spectrographs

KW - Stars: individual: HD 219134

KW - Techniques: photometric

KW - Techniques: radial velocities

U2 - 10.1051/0004-6361/201526822

DO - 10.1051/0004-6361/201526822

M3 - Journal article

AN - SCOPUS:84946930604

VL - 584

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A72

ER -

ID: 154795999