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OB Spectral and Spatial Morphology from Carina to the Antennae. Nolan R. Walborn Space Telescope Science Institute HotSci STScI August 17, 2011. Walborn Diagram. Optical O Main Sequence N IV/III He II/I. UV O Main Sequence (No Si IV). UV OB Main Sequence (No Si IV). Optical
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OB Spectral and Spatial Morphologyfrom Carina to the Antennae Nolan R. Walborn Space Telescope Science Institute HotSci STScI August 17, 2011
Optical O Main Sequence N IV/III He II/I
Optical Early O Supergiant Sequence N IV/III
Optical OB Supergiant Sequence Si IV/III/II
UV O Supergiant Sequence Si IV!
UV B Supergiant Sequence Si IV!
FUV O Luminosity Sequence(S IV 47 eV, C III 48 eV, P V 65 eV but low abundance!)
X-Ray OB Supergiant Sequence Si XIV/XIII Mg XII/XI Ne X/IX O VIII/VII
X-Ray OB Main Sequence Si XIV/XIII Mg XII/XI Ne X/IX O VIII/VII
New Of?p Stars GOSSS J. Maiz Apellaniz et al. ApJS 193, 24 (2011)
Ofc Spectra GOSSS
ONn Spectra GOSSS
VFTS C. Evans et al., A&A 530, A108 (2011) All Single O Stars
J. Maiz Apellaniz in prep.
Vn/nn/nnn Stars (red)
VISTA Blue J Spitzer Green 4.5 Red 8 micron R. Barba et al in prep.
N11 LMC
Region G B. Whitmore et al. (2010) Region G has only a single dominant central cluster (brightest in the Antennae), but again shows evidence for some weak triggering. The mass in the intermediate age clusters is only about 5 % of the mass of the central cluster, hence the triggered star formation is a relatively minor effect. Note the beautiful H_alpha shells, which have expanded unimpeded to the left, but have run into material and appear to have formed clusters in other directions
Region B We find a smooth gradient in the ages! In addition, the supershell is centered on the old cluster, and the young clusters are located where the shell intersects the dust lane ! The young clusters have a total mass of 4 E6 Msolar, 5 times more than the cluster that appears to have triggered their formation. Triggering is not always weak !
Antennae Spitzer HST/ACS
4-5 Myr 7-9 Myr G 1-2 Myr S <1 Myr 3-4 Myr B