The Initial Mass Function of Low‐Mass Stars and Brown Dwarfs in Taurus

Luhman, K. L.

doi:10.1086/317232

Cited by 126 publications

(165 citation statements)

References 47 publications

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“…For the four systems described in this paper, we estimated T eff from the best-fit primary star template (x 4) and the spectral type-to-temperature conversion found in Luhman (2000;see Appendix B).…”

Section: Appendix a Primary Mass Determinations For Figurementioning

confidence: 99%

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The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

101

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Using high-resolution near-infrared spectroscopy with the Keck Telescope, we have detected the radial velocity signatures of the cool secondary components in four optically identified pre-main-sequence, singlelined spectroscopic binaries. All are weak-lined T Tauri stars with well-defined center-of-mass velocities. The mass ratio for one young binary, NTTS 160905À1859, is M 2 /M 1 = 0.18 AE 0.01, the smallest yet measured dynamically for a pre-main-sequence spectroscopic binary. These new results demonstrate the power of infrared spectroscopy for the dynamical identification of cool secondaries. Visible-light spectroscopy, to date, has not revealed any pre-main-sequence secondary stars with masses <0.5 M , while two of the young systems reported here are in that range. We compare our targets with a compilation of the published young, double-lined spectroscopic binaries and discuss our unique contribution to this sample.

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Section: Appendix a Primary Mass Determinations For Figurementioning

confidence: 99%

“…Typically, the same component velocities were determined, using a range of template spectral types. To convert to T eff , we used Figure 5 of Luhman (2000).…”

Section: Appendix B T Eff and Luminosity Estimates For Figurementioning

confidence: 99%

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Prato

Simon

Mazeh

et al. 2002

ApJ

101

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“…However, observations of young star forming regions indicate IMF variations even in the mass regime of brown dwarfs. The Taurus star forming region, for example, is significantly deficient in objects below 0.1 M ⊙ compared to the Trapezium [19]. If the IMF of both objects is normalised by the number of stars between 0.1 -1 M ⊙ , then ≈ 13 brown dwarfs with masses > 0.02 M ⊙ are found in the Trapezium, but only one in Taurus.…”

Section: Low-mass Stars In Young Clusters Globular Clusters and The mentioning

confidence: 99%

Evidence in Favour of IMF Variations

Eisenhauer

2001

Starburst Galaxies: Near and Far

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Abstract. The stellar initial mass function (IMF) determines the relative number of stars born at a given mass. Despite the tremendous effort to establish a universal IMF, the astronomical literature offers a wealth of diverse evidence for IMF variations. This review was prepared for a controversial debate at the conference "Starbursts -Near and Far" at Ringberg Castle, 2000, and gives a one-sided portrayal in favour of IMF variations. I will summarise the empirical evidence that the IMF varies with time, with environment, and for all stellar masses. While I see no obvious systematic trend in most regions of our Galaxy, there is at least an indication that the IMF is biased towards more massive stars in the early universe and in starbursts.

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“…The Taurus region in the nearby field may have a steep IMF at high mass too (Luhman 2000). The pre-stellar condensations there are peculiar anyway, showing more extended structures, like isothermal spheres, than those in Perseus or Ophiuchus which appear truncated (Motte & André 2001).…”

Section: Local Imfs the Fieldmentioning

confidence: 96%

The Initial Mass Function in Starbursts

Elmegreen

2005

Starbursts

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The history of the IMF in starburst regions is reviewed. The IMFs are no longer believed to be top-heavy, although some superstar clusters, whether in starburst regions or not, could be. Introduction: History of Starburst IMFsEarly starburst observations suggested the luminous mass from young massive stars is comparable to the dynamical mass from the rotation curve (see reviews in Telesco 1988; Scalo 1990; Zinnecker 1996; Leitherer 1999). This implied there was a deficit in low mass stars. The nearby starburst galaxy, M82, was one of the best cases. Rieke et al. (1980Rieke et al. ( , 1993 modeled M82's gas mass, luminous star mass, rotation curve mass, 2.2 µm flux, Lyman continuum flux, CO index for supergiants, and the Brα/Brγ ratio, giving an extinction A V = 25 mag. They concluded that only the usual IMF models with lower mass limits M L > 3 − 6 M ⊙ worked. Kronberg et al. (1985) used the Lyman continuum flux from radio emission in M82 to determine the star formation rate, and used the total gas mass combined with an efficiency estimate to conclude that the IMF is top-heavy compared to the Miller & Scalo (1979) IMF. Bernlohr (1992 fit the same M82 properties as Rieke et al., plus the heavy element abundance and FIR line ratios, and concluded that either the IMF slope is shallower than the Scalo (1986) IMF by 1, or there is a lower mass cutoff greater than 1.5-2

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The Initial Mass Function of Low‐Mass Stars and Brown Dwarfs in Taurus

Cited by 126 publications

References 47 publications

The Smallest Mass Ratio Young Star Spectroscopic Binaries

The Smallest Mass Ratio Young Star Spectroscopic Binaries

Evidence in Favour of IMF Variations

The Initial Mass Function in Starbursts

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