²⁶Al kinematics: superbubbles following the spiral arms?

Constraints from the statistics of star clusters and HI supershells

¹ Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany
e-mail: krause@mpe.mpg.de
² Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, 85741 Garching, Germany
³ Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
⁴ Netherlands Institute for Radio Astronomy, Postbus 2, 7990 Dwingeloo, The Netherlands
⁵ Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
⁶ Universitäts-Sternwarte München, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 München, Germany
⁷ François Arago Centre, APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France

Received: 9 February 2015
Accepted: 13 April 2015

Abstract

Context. High-energy resolution spectroscopy of the 1.8 MeV radioactive decay line of ²⁶Al with the SPI instrument onboard the INTEGRAL satellite has recently revealed that diffuse ²⁶Al has higher velocities than other components of the interstellar medium in the Milky Way. ²⁶Al shows Galactic rotation in the same sense as the stars and other gas tracers, but reaches excess velocities of up to 300 km s^-1.

Aims. We investigate whether this result can be understood in the context of superbubbles, taking into account the statistics of young star clusters and HI supershells as well as the association of young star clusters with spiral arms.

Methods. We derived energy output and ²⁶Al mass of star clusters as a function of the cluster mass by population synthesis from stellar evolutionary tracks of massive stars. Using the limiting cases of weakly and strongly dissipative superbubble expansion, we linked this to the size distribution of HI supershells and assessed the properties of possible ²⁶Al-carrying superbubbles.

Results. ²⁶Al is produced by star clusters of all masses above ≈200 M_⊙, is roughly equally contributed over a logarithmic star cluster mass scale and strongly linked to the injection of feedback energy. The observed superbubble size distribution cannot be related to the star cluster mass function in a straightforward manner. To avoid the added volume of all superbubbles exceeding the volume of the Milky Way, individual superbubbles have to merge frequently. If any two superbubbles merge, or if ²⁶Al is injected off-centre into a larger HI supershell, we expect the hot ²⁶Al-carrying gas to obtain velocities of the order of the typical sound speed in superbubbles, ≈300 km s^-1 before decay. For star formation coordinated by the spiral arm pattern which, inside co-rotation, is overtaken by the faster moving stars and gas, outflows from spiral arm star clusters would preferentially flow into the cavities that are inflated by previous star formation associated with this arm. These cavities would preferentially be located towards the leading edge of a given arm.

Conclusions. This scenario might explain the ²⁶Al kinematics. The massive-star ejecta are expected to survive ≥10⁶ yr before being recycled into next-generation stars.