Characterizing HR 3549 B using SPHERE

D. Mesa; A. Vigan; V. D'Orazi; C. Ginski; S. Desidera; M. Bonnefoy; R. Gratton; M. Langlois; F. Marzari; S. Messina; J. Antichi; B. Biller; M. Bonavita; E. Cascone; G. Chauvin; R. U. Claudi; I. Curtis; D. Fantinel; M. Feldt; A. Garufi; R. Galicher; Th Henning; S. Incorvaia; A. M. Lagrange; M. Millward; C. Perrot; B. Salasnich; S. Scuderi; E. Sissa; Z. Wahhaj; A. Zurlo

doi:10.1051/0004-6361/201628740

Characterizing HR 3549 B using SPHERE

D. Mesa, A. Vigan, V. D'Orazi, C. Ginski, S. Desidera, M. Bonnefoy, R. Gratton, M. Langlois, F. Marzari, S. Messina, J. Antichi, B. Biller, M. Bonavita, E. Cascone, G. Chauvin, R. U. Claudi, I. Curtis, D. Fantinel, M. Feldt, A. GarufiR. Galicher, Th Henning, S. Incorvaia, A. M. Lagrange, M. Millward, C. Perrot, B. Salasnich, S. Scuderi, E. Sissa, Z. Wahhaj, A. Zurlo

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Abstract

Aims. In this work, we characterize the low-mass companion of the A0 field star HR 3549. Methods. We observed HR 3549B in imaging mode with the near-infrared branch (IFS and IRDIS) of SPHERE at the VLT, with IFS in YJ mode and IRDIS in the H band. We also acquired a medium-resolution spectrum with the IRDIS long-slit spectroscopy mode. The data were reduced using the dedicated SPHERE GTO pipeline, which is custom-designed for this instrument. We employed algorithms such as PCA and TLOCI to reduce the speckle noise. Results. The companion was clearly visible with both IRDIS and IFS. We obtained photometry in four different bands and also the astrometric position for the companion. Based on our astrometry, we confirm that it is a bound object and set constraints on its orbit. Although several uncertainties still remain, we estimate an age of ∼100-150 Myr for this system, yielding a most probable mass for the companion of 40-50 M_Jup and T_eff ∼ 2300-2400 K. Compared with template spectra, this points to a spectral type between M9 and L0 for the companion, commensurate with its position on the color-magnitude diagram.

Original language	English
Article number	A119
Pages (from-to)	1-12
Number of pages	12
Journal	Astronomy and Astrophysics
Volume	593
DOIs	https://doi.org/10.1051/0004-6361/201628740
Publication status	Published - 1 Sept 2016

Bibliographical note

Keywords

Instrumentation: spectrographs
Methods: data analysis
Planetary systems
Techniques: imaging spectroscopy

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10.1051/0004-6361/201628740

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Mesa, D., Vigan, A., D'Orazi, V., Ginski, C., Desidera, S., Bonnefoy, M., Gratton, R., Langlois, M., Marzari, F., Messina, S., Antichi, J., Biller, B., Bonavita, M., Cascone, E., Chauvin, G., Claudi, R. U., Curtis, I., Fantinel, D., Feldt, M., ... Zurlo, A. (2016). Characterizing HR 3549 B using SPHERE. Astronomy and Astrophysics, 593, 1-12. Article A119. https://doi.org/10.1051/0004-6361/201628740

@article{8ac60dc196b04bab9a7b9c25e336cdfe,

title = "Characterizing HR 3549 B using SPHERE",

abstract = "Aims. In this work, we characterize the low-mass companion of the A0 field star HR 3549. Methods. We observed HR 3549B in imaging mode with the near-infrared branch (IFS and IRDIS) of SPHERE at the VLT, with IFS in YJ mode and IRDIS in the H band. We also acquired a medium-resolution spectrum with the IRDIS long-slit spectroscopy mode. The data were reduced using the dedicated SPHERE GTO pipeline, which is custom-designed for this instrument. We employed algorithms such as PCA and TLOCI to reduce the speckle noise. Results. The companion was clearly visible with both IRDIS and IFS. We obtained photometry in four different bands and also the astrometric position for the companion. Based on our astrometry, we confirm that it is a bound object and set constraints on its orbit. Although several uncertainties still remain, we estimate an age of ∼100-150 Myr for this system, yielding a most probable mass for the companion of 40-50 MJup and Teff ∼ 2300-2400 K. Compared with template spectra, this points to a spectral type between M9 and L0 for the companion, commensurate with its position on the color-magnitude diagram.",

keywords = "Instrumentation: spectrographs, Methods: data analysis, Planetary systems, Techniques: imaging spectroscopy",

author = "D. Mesa and A. Vigan and V. D'Orazi and C. Ginski and S. Desidera and M. Bonnefoy and R. Gratton and M. Langlois and F. Marzari and S. Messina and J. Antichi and B. Biller and M. Bonavita and E. Cascone and G. Chauvin and Claudi, {R. U.} and I. Curtis and D. Fantinel and M. Feldt and A. Garufi and R. Galicher and Th Henning and S. Incorvaia and Lagrange, {A. M.} and M. Millward and C. Perrot and B. Salasnich and S. Scuderi and E. Sissa and Z. Wahhaj and A. Zurlo",

note = "Copyright 2016 ESO. First published in Astronomy and Astrophysics, 593, A119, 2016, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201628740.",

year = "2016",

month = sep,

day = "1",

doi = "10.1051/0004-6361/201628740",

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Mesa, D, Vigan, A, D'Orazi, V, Ginski, C, Desidera, S, Bonnefoy, M, Gratton, R, Langlois, M, Marzari, F, Messina, S, Antichi, J, Biller, B, Bonavita, M, Cascone, E, Chauvin, G, Claudi, RU, Curtis, I, Fantinel, D, Feldt, M, Garufi, A, Galicher, R, Henning, T, Incorvaia, S, Lagrange, AM, Millward, M, Perrot, C, Salasnich, B, Scuderi, S, Sissa, E, Wahhaj, Z & Zurlo, A 2016, 'Characterizing HR 3549 B using SPHERE', Astronomy and Astrophysics, vol. 593, A119, pp. 1-12. https://doi.org/10.1051/0004-6361/201628740

TY - JOUR

T1 - Characterizing HR 3549 B using SPHERE

AU - Mesa, D.

AU - Vigan, A.

AU - D'Orazi, V.

AU - Ginski, C.

AU - Desidera, S.

AU - Bonnefoy, M.

AU - Gratton, R.

AU - Langlois, M.

AU - Marzari, F.

AU - Messina, S.

AU - Antichi, J.

AU - Biller, B.

AU - Bonavita, M.

AU - Cascone, E.

AU - Chauvin, G.

AU - Claudi, R. U.

AU - Curtis, I.

AU - Fantinel, D.

AU - Feldt, M.

AU - Garufi, A.

AU - Galicher, R.

AU - Henning, Th

AU - Incorvaia, S.

AU - Lagrange, A. M.

AU - Millward, M.

AU - Perrot, C.

AU - Salasnich, B.

AU - Scuderi, S.

AU - Sissa, E.

AU - Wahhaj, Z.

AU - Zurlo, A.

N1 - Copyright 2016 ESO. First published in Astronomy and Astrophysics, 593, A119, 2016, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201628740.

PY - 2016/9/1

Y1 - 2016/9/1

N2 - Aims. In this work, we characterize the low-mass companion of the A0 field star HR 3549. Methods. We observed HR 3549B in imaging mode with the near-infrared branch (IFS and IRDIS) of SPHERE at the VLT, with IFS in YJ mode and IRDIS in the H band. We also acquired a medium-resolution spectrum with the IRDIS long-slit spectroscopy mode. The data were reduced using the dedicated SPHERE GTO pipeline, which is custom-designed for this instrument. We employed algorithms such as PCA and TLOCI to reduce the speckle noise. Results. The companion was clearly visible with both IRDIS and IFS. We obtained photometry in four different bands and also the astrometric position for the companion. Based on our astrometry, we confirm that it is a bound object and set constraints on its orbit. Although several uncertainties still remain, we estimate an age of ∼100-150 Myr for this system, yielding a most probable mass for the companion of 40-50 MJup and Teff ∼ 2300-2400 K. Compared with template spectra, this points to a spectral type between M9 and L0 for the companion, commensurate with its position on the color-magnitude diagram.

AB - Aims. In this work, we characterize the low-mass companion of the A0 field star HR 3549. Methods. We observed HR 3549B in imaging mode with the near-infrared branch (IFS and IRDIS) of SPHERE at the VLT, with IFS in YJ mode and IRDIS in the H band. We also acquired a medium-resolution spectrum with the IRDIS long-slit spectroscopy mode. The data were reduced using the dedicated SPHERE GTO pipeline, which is custom-designed for this instrument. We employed algorithms such as PCA and TLOCI to reduce the speckle noise. Results. The companion was clearly visible with both IRDIS and IFS. We obtained photometry in four different bands and also the astrometric position for the companion. Based on our astrometry, we confirm that it is a bound object and set constraints on its orbit. Although several uncertainties still remain, we estimate an age of ∼100-150 Myr for this system, yielding a most probable mass for the companion of 40-50 MJup and Teff ∼ 2300-2400 K. Compared with template spectra, this points to a spectral type between M9 and L0 for the companion, commensurate with its position on the color-magnitude diagram.

KW - Instrumentation: spectrographs

KW - Methods: data analysis

KW - Planetary systems

KW - Techniques: imaging spectroscopy

UR - http://www.scopus.com/inward/record.url?scp=84990206091&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201628740

DO - 10.1051/0004-6361/201628740

M3 - Article

AN - SCOPUS:84990206091

SN - 0004-6361

VL - 593

SP - 1

EP - 12

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A119

ER -

Characterizing HR 3549 B using SPHERE

Abstract

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Keywords

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