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Table 5

Spectral types and photometry for stars in the region.

Star Spectral type V B − V U − B (B − V)0 (U − B)0 E(B − V) E(U − B) V 0

a801 B1  V 12.559 0.682  −0.171  −0.260  −0.950 0.942 0.779 9.639
a802 B1  II 11.525 1.211 0.101  −0.240  −0.990 1.451 1.091 7.027
a803 B2  III-IV 12.152 0.712  −0.068  −0.240  −0.930 0.952 0.863 9.201
a805 O7  II 12.827 1.833 0.446  −0.320  −1.170 2.153 1.616 6.153
A507 B1  V 14.733 1.554 0.373  −0.260  −0.950 1.814 1.323 9.110
A263 B1  V 14.719 1.546 0.360  −0.260  −0.950 1.806 1.310 9.120
A253 B0.5 V 14.646 1.582 0.406  −0.280  −1.000 1.862 1.406 8.874
A197 B1  V 14.900 1.630 0.504  −0.260  −0.950 1.890 1.454 9.041
A514 B0.5  V 14.674 1.923 0.641  −0.280  −1.000 2.203 1.641 7.845
A515 B0.5  V 14.414 1.881 0.624  −0.280  −1.000 2.161 1.624 7.715
b201 O7  V 12.434 1.261 0.059  −0.320  −1.170 1.581 1.229 7.533
C81 O7  V 12.605 1.726 0.390  −0.320  −1.170 2.046 1.560 6.262
C84 B1  V 12.636 0.863  −0.075  −0.260  −0.950 1.123 0.876 9.155
C129 B7  III 13.025 0.785 0.235  −0.120  −0.440 0.905 0.675 10.220

Notes. Stars marked with “*” have been observed with grism #14. Stars not marked have been observed with grism #16. The intrinsic colours from Fitzgerald (1970) are used to derive excesses and dereddened magnitudes. These agree well with those obtained from CHORIZOS, which should be considered more accurate, as the code takes colour terms into full account.

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