Table 1
WISE and 2MASS magnitudes of the point sources at the heads of the G1–G3 filaments.
| Pillar | 2MASS Source | J | H | KS | w1 | w2 | w3 | w2 – w3 | w1 – w2 | Class | Lbol |
|---|---|---|---|---|---|---|---|---|---|---|---|
| G1 | J02521697+6003170 | 16.498 | 14.94 | 14.546 | 10.895 | 8.659 | 4.961 | 3.698 | 2.236 | I | 0.37 |
| G2 | J02515380+6006581 | 15.934 | 13.625 | 11.776 | 8.883 | 7.018 | 4.889 | 2.129 | 1.865 | I | 0.81 |
| G3 | J02513283+6003542 | 13.005 | 11.523 | 10.447 | 9.261 | 8.112 | 5.562 | 2.550 | 1.149 | I/II | 0.86 |
Notes. Entries in the table are: 2MASS source identifier, 2MASS J, H, and KS magnitudes (1.235, 1.662, and 2.159 µm), WISE w1 – w3 magnitudes (3.4, 4.6, and 12 µm), WISE colors, the resulting classification (Koenig & Leisawitz 2014; Kang et al. 2017), and an estimate of the bolometric luminosity (in solar luminosities) based on the KS magnitude (González Hernández & Bonifacio 2009). We assume a distance of 1.9 kpc corresponding to the distance modulus of 11.39 mag, a Vega KS -band magnitude of 0.043 and a flux of 1.1e-7 erg s−1 cm−2 (Table 3 of González Hernández & Bonifacio 2009).
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