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 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 Supergiant Sequence (O VI, C III)

Optical O Luminosity Sequence (He II λ4686, N III λ4640)

UV O Luminosity Sequence (Si IV! 45 eV)

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

Vz Stars

J. Maiz Apellaniz in prep.

Vn/nn/nnn Stars (red)

H. Sana

VISTA Blue J Spitzer Green 4.5 Red 8 micron R. Barba et al in prep.

N11 LMC

NGC 5471 M101

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 G B. Whitmore et al. (2010)

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 ! Region B

Antennae SpitzerHST/ACS

<1 Myr 1-2 Myr 3-4 Myr 4-5 Myr 7-9 Myr B S G