Table 9
Detection rates of CO first overtone bandhead emission (CO emission) in YSOs of different masses and stages of formation.
| Mass (a) | Object type | Detection rate | Sample size | Comments | Reference |
|---|---|---|---|---|---|
| Low | Class 0 | 67% | 6 | 1 | |
| Low | Class I | 15% | 52 | 2 | |
| Low | Class I | 22% | 110 | 3 | |
| Low | T Tauri | 0% | 100 | Sample from Lupus region. Authors find 3 cl TTS with CO emission in literature. | 4 |
| Low to intermediate | Variable, embedded (EXors, FUors, MNors) | 38% | 28 | 60% among objects identified as eruptive YSOs undergoing an episode of accretion. | 5 |
| Intermediate | Herbig AeBe | 5–21% | 36 | 6 | |
| Intermediate | Herbig AeBe | 7% | 91 | Strong preference for higher-mass objects. | 7 |
| High | MYSO | 17% | 195 | Red MSX Source (RMS) survey; low resolution spectroscopy. | 8 |
| High | MYSO (without HII region) | 34% | 36 | Subsample RMS, selected to be luminous and radio quiet; intermediate resolution spectroscopy. | 9 |
| High | MYSO (with and without H II region) | 18% | 11 | Sources associated with a disk (candidate) in sub-mm/radio and with a bright NIR counterpart. | 10 |
| Intermediate to high | PMS stars in M17 | 63–83% | 6–8 | Sample from which the objects in this study were taken. | RT17 |
Notes. (a)The mass categories refer to expected ZAMS masses of approximately ≲2 M⊙ (low), 2–8 M⊙ (intermediate) and ≳8 M⊙ (high). Since mass estimates are not always available or derived in the same way the numbers are approximate.
References. (1) Laos et al. (2021); (2) Doppmann et al. (2005); (3) Connelley & Greene (2010); (4) Koutoulaki et al. (2019); (5) Contreras Peña et al. (2017); (6) Ishii et al. (2001); (7) Ilee et al. (2014); (8) Cooper et al. (2013); (9) Pomohaci et al. (2017); (10) Hsieh et al. (2021).
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