Lithium abundances of nearby young solar-type stars based on optical high-resolution spectroscopy

Xing, Qianfan

doi:10.1051/0004-6361/201117133

Cited by 16 publications

(12 citation statements)

References 45 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The W velocity is matched to a few MGs, however, both the U and V are at least ∼ 15 km s −1 from any MG.Target P -Using Li, an age of 30 − 150 Myr was estimated and Hα measurements suggest an age of 65 − 125 Myr. It has a U, V and W velocity at least 10 km s −1 from any MG Xing & Xing (2012). include this target as a young K4V object (we calculate K5) with a Li EW of 17 m Å which is almost 150 m Å lower than the measurement in this work.…”

mentioning

confidence: 77%

“…It has a U, V and W velocity at least 10 km s −1 from any MG. Xing & Xing (2012) include this target as a young K4V object (we calculate K5) with a Li EW of 17 mÅ which is almost 150 mÅ lower than the measurement in this work. It is listed as a possible visual binary in Makarov (2003), however, two consistent RV measurements in this analysis suggest the object is not a close binary.…”

Section: Individual Objects Not Linked To Any Mgmentioning

confidence: 91%

See 1 more Smart Citation

A kinematically unbiased search for nearby young stars in the Northern hemisphere selected using SuperWASP rotation periods

Binks

Jeffries

Maxted

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a kinematically-unbiased search to identify young, nearby low-mass members of kinematic moving groups (MGs). Objects with both rotation periods shorter than 5 days in the SuperWASP All-Sky Survey and X-ray counterparts in the ROSAT All-Sky Survey were chosen to create a catalog of several thousand rapidly-rotating, X-ray active FGK stars. These objects are expected to be either young single stars or tidally-locked spectroscopic binaries. We obtained optical spectra for a sub-sample of 146 stars to determine their ages and kinematics, and in some cases repeat radial velocity (RV) measurements were used to identify binarity. Twenty-six stars are found to have lithium abundances consistent with an age of 200 Myr, and show no evidence for binarity and in most cases measurements of Hα and v sin i support their youthful status. Based on their youth, their radial velocities and estimates of their 3-dimensional kinematics, we find 11 objects that may be members of known MGs, 8 that do not appear associated with any young MG and a further 7 that are close to the kinematics of the recently proposed "Octans-Near" MG, and which may be the first members of this MG found in the northern hemisphere. The initial search mechanism was ∼ 18 per cent efficient at identifying likely-single stars younger than 200 Myr, of which 80 per cent were early-K spectral types.

show abstract

mentioning

confidence: 77%

Section: Individual Objects Not Linked To Any Mgmentioning

confidence: 91%

A kinematically unbiased search for nearby young stars in the Northern hemisphere selected using SuperWASP rotation periods

Binks

Jeffries

Maxted

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…It is J03332+462 (M0.0 V, pEW(Hα) = -3.4 +0.5 −0.3 Å, V577 Per B), a confirmed member of the ∼70 Ma-old AB Doradus moving group da Silva et al 2009;Schlieder et al 2012a). Its relatively bright primary at about 9 arcsec is a young K2 V star with strong ultraviolet and X-ray emission and lithium in absorption (Pounds et al 1993;Jeffries 1995;Montes et al 2001;Xing & Xing 2012). …”

Section: Hα Emissionmentioning

confidence: 99%

CARMENES input catalogue of M dwarfs

Cortés-Contreras

Béjar

Caballero

et al. 2016

A&A

View full text Add to dashboard Cite

Context. CARMENES is a stabilised, high-resolution, double-channel spectrograph at the 3.5 m Calar Alto telescope. It is optimally designed for radial-velocity surveys of M dwarfs with potentially habitable Earth-mass planets. Aims. We prepare a list of the brightest, single M dwarfs in each spectral subtype observable from the northern hemisphere, from which we will select the best planet-hunting targets for CARMENES. Methods. In this first paper on the preparation of our input catalogue, we compiled a large amount of public data and collected lowresolution optical spectroscopy with CAFOS at the 2.2 m Calar Alto telescope for 753 stars. We derived accurate spectral types using a dense grid of standard stars, a double least-squares minimisation technique, and 31 spectral indices previously defined by other authors. Additionally, we quantified surface gravity, metallicity, and chromospheric activity for all the stars in our sample. Results. We calculated spectral types for all 753 stars, of which 305 are new and 448 are revised. We measured pseudo-equivalent widths of Hα for all the stars in our sample, concluded that chromospheric activity does not affect spectral typing from our indices, and tabulated 49 stars that had been reported to be young stars in open clusters, moving groups, and stellar associations. Of the 753 stars, two are new subdwarf candidates, three are T Tauri stars, 25 are giants, 44 are K dwarfs, and 679 are M dwarfs. Many of the 261 investigated dwarfs in the range M4.0-8.0 V are among the brightest stars known in their spectral subtype. Conclusions. This collection of low-resolution spectroscopic data serves as a candidate target list for the CARMENES survey and can be highly valuable for other radial-velocity surveys of M dwarfs and for studies of cool dwarfs in the solar neighbourhood.

show abstract

“…More recently, Xing (2010) derived a spectral type of K0 and measured the Li equivalent width of only 39 mÅ. In addition, Xing & Xing (2012) detected Hα in absorption, and Rebull et al (2010) found no significant infrared excess for this source based on Spitzer photometry. Altogether, these properties are consistent with V1110Tau being a young foreground dwarf not related to the Taurus population of YSOs (see also Briceno et al 1997).…”

Section: V1110taumentioning

confidence: 99%

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Galli

Loinard

Ortiz-León

et al. 2018

ApJ

100

View full text Add to dashboard Cite

We present new trigonometric parallaxes and proper motions of young stellar objects in the Taurus molecular cloud complex from observations collected with the Very Long Baseline Array as part of the Gould's Belt Distances Survey. We detected 26 young stellar objects and derived trigonometric parallaxes for 18 stars with an accuracy of 0.3% to a few percent. We modeled the orbits of six binaries and determined the dynamical masses of the individual components in four of these systems (V1023 Tau, T Tau S, V807 Tau, and V1000 Tau). Our results are consistent with the first trigonometric parallaxes delivered by the Gaia satellite and reveal the existence of significant depth effects. We find that the central portion of the dark cloud Lynds1495 is located at d= 129.5±0.3 pc, while the B216 clump in the filamentary structure connected to it is at d=158.1±1.2 pc. The closest and remotest stars in our sample are located at d=126.6±1.7 pc and d=162.7±0.8 pc, yielding a distance difference of about 36pc. We also provide a new distance estimate for HLTau that was recently imaged. Finally, we compute the spatial velocity of the stars with published radial velocity and investigate the kinematic properties of the various clouds and gas structures in this region.

show abstract

Lithium abundances of nearby young solar-type stars based on optical high-resolution spectroscopy

Cited by 16 publications

References 45 publications

A kinematically unbiased search for nearby young stars in the Northern hemisphere selected using SuperWASP rotation periods

A kinematically unbiased search for nearby young stars in the Northern hemisphere selected using SuperWASP rotation periods

CARMENES input catalogue of M dwarfs

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Contact Info

Product

Resources

About