Table 3.
Properties of MUSE members of the overdensity.
| ID | M2800 | β | SFR | log(M*) | log(sSFR) |
|---|---|---|---|---|---|
| (AB) | (M⊙ yr−1) | (M⊙) | (Gyr−1) | ||
| (1) | (2) | (3) | (4) | (5) | (6) |
| m1 | −19.52 | −1.33 | 20.2 ± 3.4 | 9.36 |
0.94 ± 0.55 |
| m2 | −19.53 | −1.45 | 18.1 ± 3.4 | 9.69 |
0.57 ± 0.11 |
| m3 | −21.25 | −1.88 | 57.1 ± 6.2 | 10.09 |
0.67 ± 0.08 |
| m4 | −20.08 | −2.22 | 13.8 ± 1.1 | 9.33 |
0.81 ± 0.23 |
| m5 | −19.96 | −2.70 | 7.6 ± 1.1 | 9.54 |
0.34 ± 0.28 |
| m6 | −19.94 | −0.35 | 13.1 ± 1.0 (a) | 10.48 |
−0.37 ± 0.04 |
Notes. Columns: (1) source identifier; (2) absolute magnitude at 2800Å rest-frame (not corrected for extinction); (3) slope of the optical spectrum (fλ ∝ λβ); (4) extinction-corrected star formation rate based on the UV spectrum; (5) stellar mass; and (6) specific star formation rate.
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