Table 3.
Overview of average radial velocities as determined from YSOs and gas for the 14 subregions and Orion X.
| YSOs |
Gas |
||||||||
|---|---|---|---|---|---|---|---|---|---|
| Subregion | NRV | vHEL | σv, yso | vLSR(c) | Ref. (a) | vLSR | σv, gas | vHEL(d) | Ref. (b) |
| km s−1 | km s−1 | km s−1 | km s−1 | km s−1 | km s−1 | ||||
| L1647-S | 9 | 20.84 | 0.77 | 3.28 | 1 | 3.04 | 1.20 | 21.64 | 4 |
| L1647-N | 16 | 20.77 | 1.39 | 3.26 | 1 | 3.50 | 1.33 | 21.99 | 4 |
| L1641-S | 46 | 22.75 | 2.02 | 5.31 | 1 | 4.35 | 1.39 | 22.71 | 4 |
| L1641-S/C | 16 | 22.59 | 2.14 | 5.20 | 1 | 5.41 | 1.42 | 23.66 | 4 |
| L1641-C | 37 | 24.06 | 2.68 | 6.74 | 1 | 6.51 | 1.43 | 24.65 | 4 |
| L1641-N | 72 | 25.65 | 1.96 | 8.39 | 1 | 8.15 | 1.45 | 26.18 | 4 |
| OMC-4/5 | 48 | 26.26 | 2.41 | 9.06 | 1 | 8.54 | 1.57 | 26.48 | 4 |
| OMC-1 | 112 | 27.21 | 2.09 | 10.04 | 1 | 9.22 | 1.77 | 27.11 | 4 |
| OMC-2/3 | 38 | 28.33 | 2.60 | 11.19 | 1 | 10.46 | 1.54 | 28.30 | 4 |
| L1630-S | 37 | 27.68 | 1.61 | 10.86 | 1 | 10.12 | 1.48 | 26.82 | 4 |
| L1630-N | 45 | 27.98 | 1.37 | 11.40 | 1 | 9.46 | 1.28 | 26.51 | 4 |
| L1622 (e) | 4 | 19.28 | 1.17 | 2.91 | 2 | 1.17 | 0.71 | 17.96 | 5 |
| L1616 (f) | 4 | 24.50 | 2.70 | 7.80 | 3 | 7.70 | 1.05 | 22.59 | 6 |
| IC 2118 | – | – | – | – | – | −2.20 | 1.77 | 15.40 | 7 |
| Orion X | 4 | 19.63 | 0.28 | 2.68 | 1 | – | – | – | – |
Notes. The listed values are average values for each subregion with σ referring to the velocity dispersion. NRV lists the number of YSOs used to estimate the average stellar radial velocity.
The average vHEL of the YSOs is converted to vLSR using the standard solar motion from Schönrich et al. (2010).
The vLSR of the gas is converted to vHEL using the standard solar motion from Kerr & Lynden-Bell (1986) for all except for L1616, for which we used Mihalas & Binney (1981), since the data is from Maddalena et al. (1986).
The four sources in L1622 were observed by Kounkel et al. (2017b) with lower resolution (observational errors between 0.8 to 1.2 km s−1) compared to APOGEE-2 (typical observational error of about 0.05 km s−1).
The four sources in L1616 were observed by Alcalá et al. (2004) with lower resolution (observational errors between 2.0 to 2.3 km s−1) compared to APOGEE-2.
References. (1) APOGEE-2 SDSS-DR16; (2) Kounkel et al. (2017b); (3) Alcalá et al. (2004); (4) Nishimura et al. (2015)12CO(2-1); (5) Kun et al. (2008)12CO(1-0); (6) Maddalena et al. (1986)12CO(1-0); (7) Kun et al. (2001)12CO(1-0).
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