The Kinematics and Ages of Stars in Gliese’s Catalogue

Wielen, Roland

doi:10.1017/s1539299600002100

Cited by 68 publications

(78 citation statements)

References 13 publications

(1 reference statement)

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“…The models are based on different combinations of the disc and halo luminosity functions and the kinematics of the halo. Our result gives a value which falls between the predictions of models A and D and excludes models B amd C. Model A is based largely on the results of Wielen (1974), whilst model D uses the Luyten (1968) disc luminosity function, a "mean globular" halo luminosity function and the halo kinematics of Oort (1965). This analysis is described in more detail in Pokorny et al (2002) (in preparation).…”

Section: Discussionsupporting

confidence: 64%

The Liverpool-Edinburgh high proper motion survey

Pokorny

Jones

Hambly

2002

A&A

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Abstract. We present a catalogue of 6206 stars which have proper motions exceeding 0.18 yr −1 with an R-band faint magnitude limit of 19.5 mag. This catalogue has been produced using SuperCOSMOS digitized R-band ESO and UK Schmidt Plates in 131 Schmidt fields covering more than 3 000 square degrees (>7.5% of the whole sky) at the South Galactic Cap. The survey is ≥90% complete within the nominal limits of the Luyten Two Tenths Catalogue of m R ≤ 18.5 mag and 0.2 ≤ µ ≤ 2.5 yr −1 , and is ≥80% complete for m R ≤ 19.5 mag and µ ≤ 2.5 yr −1 .

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Section: Discussionsupporting

confidence: 64%

The Liverpool-Edinburgh high proper motion survey

Pokorny

Jones

Hambly

2002

A&A

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“…b Their adopted LF was averaged from the LFs of McCuskey (1966), Luyten (1968) and Wielen (1974). c The "8 parsec" sample was compiled by Reid & Gizis (1997), with later additions from Reid et al (1999), Reid et al (2003), andCruz et al (2007).…”

Section: Sample Selectionmentioning

confidence: 99%

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

Bochanski¹,

Hawley²,

Covey³

et al. 2010

The Astronomical Journal

322

305

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We report on new measurements of the luminosity function (LF) and mass function (MF) of field low-mass dwarfs derived from Sloan Digital Sky Survey (SDSS) Data Release 6 (DR6) photometry. The analysis incorporates ∼ 15 million low-mass stars (0.1 M ⊙ < M < 0.8M ⊙ ), spread over 8,400 square degrees. Stellar distances are estimated using new photometric parallax relations, constructed from ugriz photometry of nearby low-mass stars with trigonometric parallaxes. We use a technique that simultaneously measures Galactic structure and the stellar LF from 7 < M r < 16. We compare the LF to previous studies and convert to a MF using the mass-luminosity relations of Delfosse et al. (2000). The system MF, measured over −1.0 < log M/M ⊙ < −0.1, is well-described by a log-normal distribution with M • = 0.25 M ⊙ . We stress that our results should not be extrapolated to other mass regimes. Our work generally agrees with prior low-mass stellar MFs and places strong constraints in future star-formation studies of the Milky Way.

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“…2). In Table 3, we present the most used values derived from observations: Wielen (1974), hereafter referred as LMD1, and Jahreiß & Wielen (1997), which are obtained using Hipparcos data and are referred here as LMD2. As can be seen in Table 3, this last value is in good agreement with the value derived by Reid et al (2002), which is also from Hipparcos data.…”

Section: The Local Stellar and Ism Mass Densitiesmentioning

confidence: 99%

The Besançon Galaxy model renewed

Czekaj

Robin

Figueras

et al. 2014

A&A

132

219

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Context. The understanding of Galaxy evolution can be facilitated by the use of population synthesis models, which allows us to test hypotheses on the star formation history, star evolution, and chemical and dynamical evolution of the Galaxy. Aims. The new version of the Besançon Galaxy model (BGM) aims to provide a more flexible and powerful tool to investigate the initial mass function (IMF) and star formation rate (SFR) of the Galactic disc. Methods. We present a new strategy for the generation of thin disc stars, which assumes the IMF, SFR and evolutionary tracks as free parameters. We have updated most of the ingredients for the star count production and, for the first time, binary stars are generated in a consistent way. The local dynamical self-consistency is maintained in this new scheme. We then compare simulations from the new model with Tycho-2 data and the local luminosity function, as a first test to verify and constrain the new ingredients. The effects of changing thirteen different ingredients of the model are systematically studied. Results. For the first time, a full sky comparison is performed between BGM and data. This strategy allows us to constrain the IMF slope at high masses, which is found to be close to 3.0 and excludes a shallower slope such as Salpeter's one. The SFR is found decreasing whatever IMF is assumed. The model is compatible with a local dark matter density of 0.011 M pc −3 implying that there is no compelling evidence for the significant amount of dark matter in the disc. While the model is fitted to Tycho-2 data, which is a magnitude limited sample with V < 11, we check that it is still consistent with fainter stars. Conclusions. The new model constitutes a new basis for further comparisons with large scale surveys and is being prepared to become a powerful tool for the analysis of the Gaia mission data.

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The Kinematics and Ages of Stars in Gliese’s Catalogue

Cited by 68 publications

References 13 publications

The Liverpool-Edinburgh high proper motion survey

The Liverpool-Edinburgh high proper motion survey

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk. Ii. The Field

The Besançon Galaxy model renewed

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