New Neighbors: Parallaxes of 18 Nearby Stars Selected From the LSPM-North Catalog

Lépine, Sébastien; Thorstensen, J. R.; Shara, Michael M.; Rich, R. Michael

doi:10.1088/0004-6256/137/5/4109

Cited by 68 publications

(54 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The RECONS stellar compilation was next completed with the Palomar/Michigan State University survey catalogue of nearby stars (PMSU -Reid et al 1995Hawley et al 1996;Gizis et al 2002). Afterwards, we gave special attention to the comprehensive proper-motion catalogues of Lépine et al (2003Lépine et al ( , 2009Lépine et al ( , 2013 and Lépine & Gaidos (2011), and the "Meeting the Cool Neighbors" series of papers (Cruz & Reid 2002;Cruz et al 2003Cruz et al , 2007Reid et al 2003Reid et al , 2004Reid et al , 2008. Table 2 provides the sources of our information on M dwarfs.…”

Section: Carmenes Samplementioning

confidence: 99%

CARMENES input catalogue of M dwarfs

Alonso-Floriano¹,

Morales²,

Caballero³

et al. 2015

A&A

185

178

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

Section: Carmenes Samplementioning

confidence: 99%

CARMENES input catalogue of M dwarfs

Alonso-Floriano¹,

Morales²,

Caballero³

et al. 2015

A&A

185

178

View full text Add to dashboard Cite

show abstract

“…Law et al (2006) estimated a spectral type of M6 for LSPMJ1314 +1320 from its V − K color and discovered that it was a binary with a separation of 130 mas and flux ratios of Δi′=0.93±0.25 mag and Δz′=0.97±0.25 mag. Meanwhile, Lépine (2005) had identified LSPMJ1314+1320 as a potential nearby star with an estimated distance of 9.7 pc, leading them to obtain spectra and astrometry that revealed a spectral type of M7, Hα in emission, and a parallactic distance of 16.4±0.8 pc (Lépine et al 2009). They concluded that their original photometric distance estimate was much smaller than the parallactic distance due to unresolved binarity and/or extreme youth.…”

Section: Introductionmentioning

confidence: 99%

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

Dupuy

Forbrich

Rizzuto

et al. 2016

ApJ

View full text Add to dashboard Cite

We present novel tests of pre-main-sequence models based on individual dynamical masses for the M7 binary LSPMJ1314+1320AB. Joint analysis of Keck adaptive optics astrometric monitoring along with Very Long Baseline Array radio data from a companion paper yield component masses of 92.8±0.6 M Jup (0.0885±0.0006 M ☉ ) and 91.7±1.0 M Jup (0.0875±0.0010 M ☉ ) and a parallactic distance of 17.249±0.013 pc. We find component luminosities consistent with the system being coeval at 80.8±2.5 Myr, according to BHAC15 evolutionary models. The presence of lithium is consistent with model predictions, marking the first test of the theoretical lithium depletion boundary using ultracool dwarfs of known mass. However, we find that the evolutionary model-derived average effective temperature (2950±5 K) is 180 K hotter than that given by a spectral type-T eff relation based on BT-Settl models (2770±100 K). We suggest that the dominant source of this discrepancy is model radii being too small by ≈13%. In a test mimicking the typical application of models by observers, we derive masses on the H-R diagram using luminosity and BT-Settl temperature. The estimated masses are lower by -(2.0σ) than we measure dynamically and would imply that this is a system of ≈50 M Jup brown dwarfs, highlighting the large systematic errors possible in H-R diagram properties. This is the first time masses have been measured for ultracool ( M6) dwarfs displaying spectral signatures of low gravity. Based on features in the infrared, LSPMJ1314+1320AB appears to have higher gravity than typical Pleiades and ABDor members, opposite the expectation given its younger age. The components of LSPMJ1314+1320AB are now the nearest, lowest mass pre-main-sequence stars with direct mass measurements.

show abstract

“…From the images, we derive J = 14.8 ± 0.1 and K = 14.5 ± 0.2 for the primary and J = 15.8 ± 0.1, K = 15.4 ± 0.2 for the secondary. Figure 4 shows the absolute brightness in the J-band (M J ), and the J − K colours, assuming that the two objects are at the same distance, together with the absolute brightness and colours of stars taken from Lépine et al (2009), Henry et al (2006, and Bilir et al (2009).The brightness as well as the J − K-colours of the secondary is in agreement with being a physical G9V-companion at a projected distance of ∼1900 AU. If the CC were either bluer or redder, we would know that it is an unrelated star.…”

Section: A2 Lra01_e1_4719mentioning

confidence: 52%

“…The J − K colours are derived from the observations. For comparison, we also show the brightness and J − K colour of standard stars (small dots) as given in Lépine et al (2009), Henry et al (2006, and Bilir et al (2009). In all cases the J − K colours are consistent with physical companions.…”

Section: Stars With Companion Candidatesmentioning

confidence: 85%

High angular resolution imaging and infrared spectroscopy of CoRoT candidates

Guenther¹,

Fridlund²,

Alonso³

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Studies of transiting extrasolar planets are of key importance for understanding the nature of planets outside our solar system because their masses, diameters, and bulk densities can be measured. An important part of transit-search programmes is the removal of false-positives. In the case of the CoRoT space mission, the majority of the false-positives are removed by a detailed analysis of the light curves and by seeing-limited imaging in-and out-of-transit. However, the critical question is how many of the candidates that passed all these tests are false-positives. Such false-positives can be caused by eclipsing binaries, which are either related or unrelated to the targets. Aims. For our study we selected 25 CoRoT candidates that have already been screened against false-positives using detailed analysis of the light curves and seeing-limited imaging, which has transits that are between 0.7 and 0.05% deep. Our aim is to search for companion candidates that had not been recognized in previous observations. Methods. We observed 20 candidates with the adaptive optics imager NaCo and 18 with the high-resolution infrared spectrograph CRIRES. Results. We found previously unknown stars within 2 of the targets in seven of the candidates. All of these are too faint and too close to the targets to have been previously detected with seeing-limited telescopes in the optical. Our study thus leads to the surprising results that if we remove all candidates excluded by the sophisticated analysis of the light-curve, as well as carrying out deep imaging with seeing-limited telescopes, still 28−35% of the remaining candidates are found to possess companions that are bright enough to be false-positives. Conclusions. Given that the companion candidates cluster around the targets and that the J − K colours are consistent with physical companions, we conclude that the companion candidates are more likely to be physical companions rather than unrelated field stars.

show abstract

New Neighbors: Parallaxes of 18 Nearby Stars Selected From the LSPM-North Catalog

Cited by 68 publications

References 72 publications

CARMENES input catalogue of M dwarfs

CARMENES input catalogue of M dwarfs

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

High angular resolution imaging and infrared spectroscopy of CoRoT candidates

Contact Info

Product

Resources

About