Table 1
Taurus multiplicity surveys.
| Binary-fraction (%) | |||||
| Mass (M⊙) | Separation (AU) | obs | Model | Comment | Reference |
|
|
|||||
| – | 50 − 5000 | 64 ± 8 | – | Class 0 protostars | Chen et al. (2013) |
|
|
|||||
| 0.01 − 0.1 | 10-4 − 3 | – | 11 | T Tauri, prediction | – |
| 0.1 − 2.0 | 10-4 − 3 | – | 19 | T Tauri, prediction | – |
| 0.2 − 2.3 | 16 − 252 | 37 ± 9 | 28 | T Tauri | Ghez et al. (1993) |
| 0.5 − 1 | 3 − 1400 | 55 ± 11 | 59 | T Tauri; lower bound | Simon et al. (1995) |
| solar | 18 − 1800 | 42.5 ± 7.9 | 47 | T Tauri | Kohler & Leinert (1998) |
|
|
|||||
| 0.01 − 0.1 | 10-4 − 3 | – | 9 | model prediction | – |
| 0.1 − 2.0 | 10-4 − 3 | – | 18 | model prediction | – |
| 0.015 − 0.14 | >4 |
|
18 | VLMOs; >M5.5 | Kraus et al. (2006) |
| < 0.1 | > 10 |
|
6 | >M6 | Todorov et al. (2014) |
| 0.1 − 0.3 | > 10 |
|
21 | M4 − M6 | Todorov et al. (2014) |
| 0.5 − 2.0 | 500 − 5000 |
|
15 | – | Kraus & Hillenbrand (2009) |
| 0.25 − 0.7 | 3 − 5000 | ( ) |
50 | CSF1 | Kraus et al. (2011) |
| 0.7 − 2.5 | 3 − 5000 | ( ) |
59 | CSF1 | Kraus et al. (2011) |
| 0.2 − 3.0 | 10 − 1500 |
|
38 | raw | Daemgen et al. (2015) |
| 0.7 − 1.4 | all | 62 ± 14 | 84 | corrected for full range | Daemgen et al. (2015) |
Notes. Observationally inferred binary fractions are compared to those resulting from the model. For the T Tauri observations the initial model population is used, for the other sub-populations an initial density of 350 M⊙ pc-3 (as in Marks & Kroupa 2011) for Taurus-Auriga embedded clusters is used to account for little dynamical evolution; see Sect. 3.2.1. We provide predictions for binary-fractions in the separation range < 3 AU where currently no observations are available. (1) CSF denotes that the original paper stated the companion star frequency (number of companions per target) which is larger than the corresponding binary fraction (number of targets with at least one companion) used otherwise throughout this paper.
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