Table 3
Physical parameters for a subset of YSO Candidates in the IRAS 22147 region with at least five photometry points, including one at a wavelength longer than 12 µm.
| Nr | IRAC designation ‘SSTSMOGA’ | Model Set(a) | Class(b) init | Class(c) SED | Selection method(d) | R* (R⊙) | T* (K) | L (e) (L⊙) |  (M⊙) |
Age(f) (Myr) |
|---|---|---|---|---|---|---|---|---|---|---|
| YSO candidates at ~5.6kpc | ||||||||||
| 1 | G104.6697+02.9357 | sp–smi | II | II+III | ML | 2.8 | 11340 | 120 | 3.0 | 2.3 |
| 2 | G104.6895+02.7945 | sp–smi | I | II+III | CC | 54.5 | 6760 | 5600 | – | – |
| 3 | G104.6968+02.7925 | s-ubsmi | II | 0 | ML | 4.2 | 10690 | 210 | – | – |
| 4 | G104.7003+02.7923 | spubsmi | I | I | CC | 16.4 | 5070 | 160 | – | – |
| 5 | G104.7062+02.7895(ɡ) | sp–h-i | II | II+III | ML | 32.9 | 6500 | 1750 | – | – |
| 6 | G104.7118+02.7921 | sp–h-i | II | II+III | ML | 58.9 | 4050 | 840 | – | – |
| 7 | G104.7153+02.7979 | sp–h-i | II | II+III | ML | 5.4 | 11280 | 430 | 4.4 | 0.8 |
| 8 | G104.7241+02.8075 | sp–h-i | II | II+III | ML | 11.2 | 5630 | 110 | – | – |
| 9 | G104.7270+02.8003 | sp–smi | I | II+III | CC | 11.5 | 14370 | 5050 | – | – |
| 10 | G104.7934+02.6942 | sp–s-i | I | II+III | CC | 3.6 | 10150 | 120 | 3.0 | 2.2 |
| 11 | G104.8126+02.6920 | sp–s-i | I | II+III | CC | 6.4 | 11760 | 700 | – | – |
| 12 | G104.8206+02.7026 | sp–smi | I | II+III | CC | 1.5 | 6980 | 5 | – | – |
| 13 | G104.8383+02.7091 | sp–s-i | II | II+III | CC | 13.8 | 4790 | 90 | – | – |
| YSO candidates at ~2.2 kpc | ||||||||||
| 1 | G104.5582+02.8857 | sp–s-i | II | II+III | CC | 2.8 | 5560 | 7 | 2.1 | 2.4 |
| 2 | G104.6829+02.6173 | sp–s-i | II | II+III | CC | 2.0 | 4220 | 1 | 0.7 | 1.0 |
| 3 | G104.7009+02.6186 | sp–s-i | II | II+III | CC | 1.1 | 5770 | 1 | – | – |
| 4 | G104.7538+02.8964(ɡ) | sp–hmi | II | II+III | ML | 1.4 | 6490 | 3 | – | – |
| 5 | G104.7544+02.6101 | sp–s-i | I | II+III | CC | 6.7 | 4160 | 12 | – | – |
| 6 | G104.7622+02.7179 | spu-hmi | I | I | CC | 4.1 | 4400 | 6 | 0.8 | 0.2 |
| 7 | G104.8225+02.8393 | sp–s-i | I | II+III | CC | 1.5 | 5150 | 2 | 1.4 | 4.1 |
| 8 | G104.8429+02.6522(ɡ) | sp–s-i | I | II+III | CC | 0.6 | 3840 | 0.1 | – | – |
| 9 | G104.8436+02.7289 | sp–s-i | I | II+III | CC | 1.4 | 4450 | 0.6 | – | – |
| 10 | G104.8510+02.7998 | sp–s-i | I | II+III | CC | 2.9 | 5580 | 7 | 2.1 | 2.3 |
| 11 | G104.8965+02.7124 | sp–smi | II | II+III | ML | 1.9 | 5650 | 3 | – | – |
| 12 | G104.9084+02.7625(ɡ) | sp–s-i | II | II+III | CC | 2.5 | 8270 | 27 | – | – |
| 13 | G104.9180+02.7798 | sp–hmi | II | II+III | ML | 0.9 | 4800 | 0.4 | – | – |
Notes. (a)See Table 2 footnotes for the meaning of characters in the model set names. (b)YSO class as initially determined using color–color diagrams and machine learning algorithms (Sects. 3.2 and 3.3, respectively). (c)YSO class as determined from the SED fitting (see Sect. 3.7). (d)Initial selection methods used in this work are the color–color/color–magnitude diagrams (CC; Sect. 3.2) and machine learning algorithms (ML; Sect. 3.3).(e) Stellar luminosities are calculated using the formula 
, where σSB is the Stefan–Boltzmann constant.(f)We provide stellar masses (M*) and ages (Age) only for sources with the most reliable estimates of these parameters (see Sect. 3.7).(ɡ) A more reliable distance for this source is provided by Gaia; see Appendix A for the SED model adopting the Gaia DR3 distance from Bailer-Jones et al. (2021).
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