A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy, M.; Chauvin, G.; Lagrange, A.-M.; Rojo, P.; Allard, F.; Pinte, C.; Dumas, Christophe; Homeier, D.

doi:10.1051/0004-6361/201118270

Cited by 143 publications

(230 citation statements)

References 190 publications

(409 reference statements)

Supporting

Mentioning

204

Contrasting

Order By: Relevance

“…This indicates a photosphere with temperature around 2800 K (see e.g. Bonnefoy et al 2014, and references therein). Even if HS 0220+0603 followed the semi-empirical sequence of Knigge et al (2011) and had a donor mass of 0.25 M , the spectral type would still be cooler than expected.…”

Section: The M-type Companionmentioning

confidence: 91%

Dynamical masses of a nova-like variable on the edge of the period gap

Rodríguez‐Gil

Shahbaz

Marsh

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present the first dynamical determination of the binary parameters of an eclipsing SW Sextantis star in the 3-4 hour orbital period range during a low state. We obtained time-resolved optical spectroscopy and photometry of HS 0220+0603 during its 2004-2005 low brightness state, as revealed in the combined SMARTS, IAC80 and M1 Group long-term optical light curve.The optical spectra taken during primary eclipse reveal a secondary star spectral type of M5.5±0.5 as derived from molecular band-head indices. The spectra also provide the first detection of a DAB white dwarf in a cataclysmic variable. By modelling its optical spectrum we estimate a white dwarf temperature of 30 000 ± 5 000 K.By combining the results of modelling the white dwarf eclipse from ULTRA-CAM light curves with those obtained by simultaneously fitting the emission-and absorption-line radial velocity curves and I-band ellipsoidal light curves, we measure the stellar masses to be M 1 = 0.87 ± 0.09 M and M 2 = 0.47 ± 0.05 M for the white dwarf and the M dwarf, respectively, and an inclination of the orbital plane of i ≈ 79 o . A radius of 0.0103 ± 0.0007 R is obtained for the white dwarf. The secondary star in HS 0220+0603 is likely too cool and undersized for its mass.

show abstract

Section: The M-type Companionmentioning

confidence: 91%

Dynamical masses of a nova-like variable on the edge of the period gap

Rodríguez‐Gil

Shahbaz

Marsh

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The third sample is made of spectra of members of 1−150 Myr old young moving groups and clusters (Lodieu et al 2008;Rice et al 2010;Bonnefoy et al 2014;Gagné et al 2014). The fourth sample is composed of spectra of young MLT companions (Patience et al 2010;Lafrenière et al 2010;Wahhaj et al 2011;Bonnefoy et al 2010Bonnefoy et al , 2014). …”

Section: Appendix A: Details On the Orbital Fitmentioning

confidence: 99%

“…The SED and spectral-fitting procedures are described in Bonnefoy et al (2013) and Bonnefoy et al (2014), respectively.…”

Section: Appendix A: Details On the Orbital Fitmentioning

confidence: 99%

Physical and orbital properties ofβPictoris b

Bonnefoy

Marleau

Galicher

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

The intermediate-mass star β Pictoris is known to be surrounded by a structured edge-on debris disk within which a gas giant planet was discovered orbiting at 8−10 AU. The physical properties of β Pic b were previously inferred from broad-and narrow-band 0.9−4.8 µm photometry. We used commissioning data of the Gemini Planet Imager (GPI) to obtain new astrometry and a lowresolution (R ∼ 35−39) J-band (1.12−1.35 µm) spectrum of the planet. We find that the planet has passed the quadrature. We constrain its semi-major axis to ≤10 AU (90% prob.) with a peak at 8.9 +0.4 −0.6 AU. The joint fit of the planet astrometry and the most recent radial velocity measurements of the star yields a planet dynamical mass lower than 20 M Jup (≥96% prob.). The extracted spectrum of β Pic b is similar to those of young L1 +1 −1.5 dwarfs. We used the spectral type estimate to revise the planet luminosity to log(L/L ) = −3.90±0.07. The 0.9−4.8 µm photometry and spectrum are reproduced for T eff = 1650 ± 150 K and a log g ≤ 4.7 dex by 12 grids of PHOENIX-based and LESIA atmospheric models. For the most recent system age estimate (21 ± 4 Myr), the bolometric luminosity and the constraints on the dynamical mass of β Pic b are only reproduced by warm-and hot-start tracks with initial entropies S i > 10.5 k B /baryon. These initial conditions may result from an inefficient accretion shock and/or a planetesimal density at formation higher than in the classical core-accretion model. Considering a younger age for the system or a conservative formation time for β Pic b does not change these conclusions.

show abstract

“…Gorlova et al 2003;McGovern et al 2004;Kirkpatrick et al 2006 2007). We measured the equivalent widths (EW) of the gravity sensitive Na I doublet at 1.138µm and the K I doublets at 1.169, 1.177µm and 1.243, 1.253µm with associated errors as described in Bonnefoy et al (2014), with the psuedocontinuum wavelength regions reported therein. For a given spectral subtype, low surface gravity, hence youth, can be seen in the reduced strength of the alkali lines compared to main sequence stars.…”

Section: Surface Gravity and Chromospheric Activitymentioning

confidence: 99%

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

Bergfors¹,

Brandner²,

Bonnefoy³

et al. 2015

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We present VLT/SINFONI J, H + K spectra of seven close visual pairs in M dwarf binary/triple systems, discovered or observed by the AstraLux M dwarf survey. We determine the spectral types to within ±1.0 subclasses from comparison to template spectra and the strength of K-band water absorption, and derive effective temperatures. The results are compared to optical spectral types of the unresolved binary/multiple systems, and we confirm that our photometric method to derive spectral types in the AstraLux M dwarf survey is accurate. We look for signs of youth such as chromospheric activity and low surface gravity, and find an age in the range 0.25 − 1 Gyr for the GJ 852 system. Strong Li absorption is detected in optical spectra of the triple system J024902 obtained with FEROS at the ESO-MPG 2.2 m telescope. The equivalent width of the absorption suggests an age consistent with the β Pic moving group. However, further observations are needed to establish group membership. Ongoing orbital monitoring will provide dynamical masses and thus calibration of evolutionary models for low mass stars.

show abstract

A library of near-infrared integral field spectra of young M–L dwarfs

Cited by 143 publications

References 190 publications

Dynamical masses of a nova-like variable on the edge of the period gap

Dynamical masses of a nova-like variable on the edge of the period gap

Physical and orbital properties ofβPictoris b

Characterization of close visual binaries from the AstraLux Large M Dwarf Survey

Contact Info

Product

Resources

About