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A Reanalysis of the UVES M Dwarf Planet Search Program

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A Reanalysis of the UVES M Dwarf Planet Search Program. / Butler, R. P. ; Jones, Hugh; Feng, F. ; Escude, G. Anglada; Tuomi, M.; Keiser, Sandy .

In: The Astronomical Journal, Vol. 158, No. 6, 251, 02.12.2019.

Research output: Contribution to journalArticlepeer-review

Harvard

Butler, RP, Jones, H, Feng, F, Escude, GA, Tuomi, M & Keiser, S 2019, 'A Reanalysis of the UVES M Dwarf Planet Search Program', The Astronomical Journal, vol. 158, no. 6, 251. https://doi.org/10.3847/1538-3881/ab4905

APA

Butler, R. P., Jones, H., Feng, F., Escude, G. A., Tuomi, M., & Keiser, S. (2019). A Reanalysis of the UVES M Dwarf Planet Search Program. The Astronomical Journal, 158(6), [251]. https://doi.org/10.3847/1538-3881/ab4905

Vancouver

Author

Butler, R. P. ; Jones, Hugh ; Feng, F. ; Escude, G. Anglada ; Tuomi, M. ; Keiser, Sandy . / A Reanalysis of the UVES M Dwarf Planet Search Program. In: The Astronomical Journal. 2019 ; Vol. 158, No. 6.

Bibtex

@article{256f90ebc4974d0aad451a40b2a286c0,
title = "A Reanalysis of the UVES M Dwarf Planet Search Program",
abstract = "The UVES (Ultraviolet and Visible Spectrometer) M Dwarf Planet Search program surveyed 40 M dwarfs and 1 M giant from 2000 through 2007 March. Two of the M dwarfs were double-lined spectroscopic binaries. The 38 single-lined M dwarfs in this survey are among the nearest and brightest M dwarfs. Starting with the reduced 1D spectra provided by the UVES team, we reanalyzed the UVES velocities of Proxima Cen as part of the {"}Pale Red Dot{"} program. The velocity rms decreased from 3.6 to 2.3 m s−1. Motivated by this result, we have harvested all of the raw data from the UVES M Dwarf Planet Search from the European Southern Observatory (ESO) archives and have written custom packages to generate 1D spectra from the raw data, and velocities from the 1D spectra. The median improvement in the velocity rms from the new analysis is 1.8 m s−1. Six of the 38 M dwarfs from the original study had a velocity rms < 4 m s−1. In the reanalysis presented here, 22 of these stars have a velocity rms < 4 m s−1. We improve the upper limits on possible planets orbiting these stars by a factor of typically two to three. For many of these M dwarfs, these observations represent the first epoch of high-precision velocity measurements",
author = "Butler, {R. P.} and Hugh Jones and F. Feng and Escude, {G. Anglada} and M. Tuomi and Sandy Keiser",
note = "{\textcopyright} 2019. The American Astronomical Society. All rights reserved. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.3847/1538-3881/ab4905",
year = "2019",
month = dec,
day = "2",
doi = "10.3847/1538-3881/ab4905",
language = "English",
volume = "158",
journal = "The Astronomical Journal ",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "6",

}

RIS

TY - JOUR

T1 - A Reanalysis of the UVES M Dwarf Planet Search Program

AU - Butler, R. P.

AU - Jones, Hugh

AU - Feng, F.

AU - Escude, G. Anglada

AU - Tuomi, M.

AU - Keiser, Sandy

N1 - © 2019. The American Astronomical Society. All rights reserved. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.3847/1538-3881/ab4905

PY - 2019/12/2

Y1 - 2019/12/2

N2 - The UVES (Ultraviolet and Visible Spectrometer) M Dwarf Planet Search program surveyed 40 M dwarfs and 1 M giant from 2000 through 2007 March. Two of the M dwarfs were double-lined spectroscopic binaries. The 38 single-lined M dwarfs in this survey are among the nearest and brightest M dwarfs. Starting with the reduced 1D spectra provided by the UVES team, we reanalyzed the UVES velocities of Proxima Cen as part of the "Pale Red Dot" program. The velocity rms decreased from 3.6 to 2.3 m s−1. Motivated by this result, we have harvested all of the raw data from the UVES M Dwarf Planet Search from the European Southern Observatory (ESO) archives and have written custom packages to generate 1D spectra from the raw data, and velocities from the 1D spectra. The median improvement in the velocity rms from the new analysis is 1.8 m s−1. Six of the 38 M dwarfs from the original study had a velocity rms < 4 m s−1. In the reanalysis presented here, 22 of these stars have a velocity rms < 4 m s−1. We improve the upper limits on possible planets orbiting these stars by a factor of typically two to three. For many of these M dwarfs, these observations represent the first epoch of high-precision velocity measurements

AB - The UVES (Ultraviolet and Visible Spectrometer) M Dwarf Planet Search program surveyed 40 M dwarfs and 1 M giant from 2000 through 2007 March. Two of the M dwarfs were double-lined spectroscopic binaries. The 38 single-lined M dwarfs in this survey are among the nearest and brightest M dwarfs. Starting with the reduced 1D spectra provided by the UVES team, we reanalyzed the UVES velocities of Proxima Cen as part of the "Pale Red Dot" program. The velocity rms decreased from 3.6 to 2.3 m s−1. Motivated by this result, we have harvested all of the raw data from the UVES M Dwarf Planet Search from the European Southern Observatory (ESO) archives and have written custom packages to generate 1D spectra from the raw data, and velocities from the 1D spectra. The median improvement in the velocity rms from the new analysis is 1.8 m s−1. Six of the 38 M dwarfs from the original study had a velocity rms < 4 m s−1. In the reanalysis presented here, 22 of these stars have a velocity rms < 4 m s−1. We improve the upper limits on possible planets orbiting these stars by a factor of typically two to three. For many of these M dwarfs, these observations represent the first epoch of high-precision velocity measurements

U2 - 10.3847/1538-3881/ab4905

DO - 10.3847/1538-3881/ab4905

M3 - Article

VL - 158

JO - The Astronomical Journal

JF - The Astronomical Journal

SN - 0004-6256

IS - 6

M1 - 251

ER -