Near-Infrared Adaptive Optics Spectroscopy of Binary Brown Dwarfs HD 130948B and HD 130948C

Goto, Miwa; Kobayashi, Naoto; Terada, Hiroshi; Gäessler, Wolfgang; Kanzawa, Tomio; Takami, Hideki; Takato, Naruhisa; Hayano, Yutaka; Kamata, Yukiko; Iye, Masanori; Saint-Jacques, David; Tokunaga, A. T.; Potter, D.; Cushing, Michael C.

doi:10.1086/339800

Cited by 54 publications

(38 citation statements)

References 15 publications

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“…None of these template spectra matched well the continua of the GSC 08047-00232 B spectrum which appeared to be too steep. As already evoked by Goto et al (2002), the main plausible explanation seems to be a chromatical dependency of the flux transmitted through the narrow slit in case of a difference of centering between GSC 08047-00232 B and the standard star. This results in a decrease of the continuum slope going from short to long wavelengths, well represented by a linear function which is effectively observed in the case the GSC 08047-00232 B spectrum.…”

Section: Spectral Characterization Of Gsc 08047-00232 Bmentioning

confidence: 78%

Astrometric and spectroscopic confirmation of a brown dwarf companion to GSC 08047-00232

Chauvin¹,

Lagrange²,

Lacombe

et al. 2005

A&A

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Abstract. We report VLT/NACO imaging observations of the stars GSC 08047-00232 and HIP 6856, probable members of the large Tucana-Horologium association. During our previous ADONIS/SHARPII deep imaging survey, a substellar candidate companion was discovered around each star. Based on VLT/NACO astrometric measurements, we find that GSC 08047-00232 and the faint candidate companion near to it share the same proper motion with a significance of 3.1 σ. On the contrary, the candidate companion to HIP 6856 is probably a background object with a significance of 4.3 σ. We also detect a new fainter and closer candidate companion to HIP 6856, but which is likely a background object too with a significance of 4 σ. Recent VLT/NACO spectroscopic measurements of GSC 08047-00232 finally confirm the substellar nature of this young brown dwarf with a derived spectral type M 9.5±1. GSC 08047-00232 B, with an estimated mass of 25±10 M Jup and an effective temperature of 2100 ± 200 K, is presently the third substellar companion identified among young, nearby associations.

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Section: Spectral Characterization Of Gsc 08047-00232 Bmentioning

confidence: 78%

Astrometric and spectroscopic confirmation of a brown dwarf companion to GSC 08047-00232

Chauvin¹,

Lagrange²,

Lacombe

et al. 2005

A&A

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“…We are searching for sub-stellar companions also on the southern sky, with speckle and normal imaging at the ESO NTT, and now also with AO (NAOS-CONICA at the ESO VLT). Four sub-stellar companions to young (nearby) stars have been confirmed by both proper motion and spectroscopy: The ∼12 Myrs young TWA-5 B (Lowrance et al 1999;Neuhäuser et al 2000), the ∼300 Myrs old Gl 569 B, C Lane et al 2001), the ∼35 Myrs young HR 7239 B (Lowrance et al 2000;Guenther et al 2001), and the ∼300 Myrs old HD 130948 B, C (Potter et al 2002;Goto et al 2002).…”

Section: Introductionmentioning

confidence: 85%

HD 77407 and GJ 577: Two new young stellar binaries

Mugrauer

Neuhäuser

Guenther

et al. 2004

A&A

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Abstract. We present the first results from our search for close stellar and sub-stellar companions to young nearby stars on the northern sky. Our infrared imaging observations are obtained with the 3.5 m Calar Alto telescope and the AO system ALFA. With two epoch observations which were separated by about one year, we found two co-moving companion candidates, one close to HD 77407 and one close to GJ 577. For the companion candidate near GJ 577, we obtained an optical spectrum showing spectral type M 4.5; this candidate is a bound low-mass stellar companion confirmed by both proper motion and spectroscopy. We estimate the masses for HD 77407 B and GJ 577 B to be ∼0.3 to 0.5 M and ∼0.16 to 0.2 M , respectively. Compared to Siess et al. (2000) models, each of the two pairs appears co-eval with HD 77407 A, B being 10 to 40 Myrs and GJ 577 A, B being ≥100 Myrs old. We also took multi-epoch high-resolution spectra of HD 77407 to search for sub-stellar companions, but did not find any with 3 M Jup as upper mass (m sin i) limit (for up to 4 year orbits); however, we detected a long-term radial velocity trend in HD 77407 A, consistent with a ∼0.3 M companion at ∼50 AU separation, i.e. the one detected by the imaging. Hence, HD 77407 B is confirmed to be a bound companion to HD 77407 A. We also present limits for undetected, but detectable companions using a deep image of HD 77407 A and B, also observed with the Keck NIRC2 AO system; any brown dwarfs were detectable outside of 0.5 arcsec (17 AU at HD 77407), giant planets with masses from ∼6.5 to 12 M Jup were detectable at ≥1.5 arcsec.

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“…From spectroscopy, we decided to consider only the K-band portion of the AB Pic b spectrum which is less subject than the H-band to chromatical effects, mainly due to differential slit centering and/or differential AO corrections between the science source and the telluric standard (see Goto et al 2002;Chauvin et al 2004). Based on the template spectra for late-M, L and T dwarfs of Leggett et al (2001) and Geballe et al (2002), we used a minimum χ 2 adjustment to find the best template spectra matching the broad water-band absorptions of the AB Pic b spectrum.…”

Section: Spectral Type Determinationmentioning

confidence: 99%

A companion to AB Pic at the planet/brown dwarf boundary

Chauvin

Lagrange²,

Zuckerman

et al. 2005

A&A

232

213

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Abstract. We report deep imaging observations of the young, nearby star AB Pic, a member of the large Tucana-Horologium association. We have detected a faint, red source 5.5 South of the star with JHK colors compatible with that of a young substellar L dwarf. Follow-up observations at two additional epochs confirm, with a confidence level of 4.7σ, that the faint red object is a companion to AB Pic rather than it being a stationary background object. A low resolution K-band spectrum indicates an early-L spectral type for the companion. Finally, evolutionary model predictions based on the JHK photometry of AB Pic b indicate a mass of 13 to 14 M Jup if its age is ∼30 Myr. Is AB Pic b a massive planet or a minimum mass brown dwarf?

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Near-Infrared Adaptive Optics Spectroscopy of Binary Brown Dwarfs HD 130948B and HD 130948C

Cited by 54 publications

References 15 publications

Astrometric and spectroscopic confirmation of a brown dwarf companion to GSC 08047-00232

Astrometric and spectroscopic confirmation of a brown dwarf companion to GSC 08047-00232

HD 77407 and GJ 577: Two new young stellar binaries

A companion to AB Pic at the planet/brown dwarf boundary

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