Table 1
Distribution of PMS objects in our sample across the six NGC 2264 subregions discussed in Sung et al. (2009), and disk fraction, accretors fraction and distribution in age of the population of each subregion.
| Region | Tot # | Class II (%) | CTTS (%) | # in each isochronal age bin (Myr) | # with no age estimate in our sample | ||||||||||
| <1 | 1–2 | 2–3 | 3–4 | 4–6 | 6–8 | >8 | ↙ 1 Gyr a | ↖ 1.4 M⊙b | (Teff,Lbol) c | ||||||
|
|
|||||||||||||||
| Spokes | 44 | 47.7+18.2 | 52.3+4.5 | 7 | 8 | 4 | 3 | 3 | 1 | 4 | 0 | 8 | 6 | ||
| Cone (C) | 80 | 41.3+12.5 | 37.5+11. | 14 | 16 | 8 | 6 | 6 | 4 | 10 | 0 | 3 | 13 | ||
| Cone (H) | 70 | 28.6+14.3 | 32.9+4.3 | 4 | 14 | 6 | 7 | 9 | 3 | 11 | 1 | 4 | 11 | ||
| S Mon | 195 | 31.3+11.8 | 23.6+14. | 11 | 33 | 23 | 16 | 14 | 16 | 16 | 2 | 10 | 54 | ||
| Halo | 175 | 20.6+10.9 | 22.3+8.0 | 6 | 27 | 14 | 21 | 29 | 22 | 16 | 2 | 10 | 28 | ||
| Field | 91 | 28.6+12.1 | 28.6+3.3 | 0 | 5 | 6 | 8 | 9 | 14 | 8 | 1 | 4 | 36 | ||
Notes. “Class II (%)” = percentage of disk-bearing objects in the total number of sources located onto the corresponding region (the superscript corresponds to the percentage of objects with no IR information within the region, hence potentially adding to the estimated disk fraction). “CTTS (%)” = percentage of accreting objects in the total number of sources located onto the corresponding region (the superscript corresponds to the percentage of objects with no UV/Hα information within the region, hence potentially adding to the estimated accretors fraction).
Objects whose location on the HR diagram falls below the 1 Gyr isochrone from Baraffe et al.’s (2015) PMS model grid.
Objects whose location on the HR diagram falls above the highest mass track (1.4 M⊙) included in Baraffe et al.’s (2015) PMS model grid.
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