Open AccessThe energetics and mass loss of the dwarf starburst Markarian 33
Author(s) -
Summers Lesley K.,
Stevens Ian R.,
Strickland David K.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04722.x
Subject(s) - physics , astrophysics , rosat , galaxy , star formation , superbubble , astronomy , dwarf galaxy , interstellar medium
We present ROSAT HRI X‐ray data and optical imaging of the important dwarf starburst Markarian 33. We find an extended, complex, shell‐like morphology in the X‐ray emission, with an extent of ∼, coincident with the bright star‐forming regions at the centre of the galaxy. The physical extent of this X‐ray emission from Mrk 33 is very similar to the observed H α emission, and suggests that the bulk of the X‐ray emission is coming from an expanding superbubble. We estimate the age and mass of Mrk 33's starburst to be 5.8 Myr and respectively, with the energy injection rate in the central regions of the galaxy being ∼10 41 erg s −1 , while the associated mass‐loss rate from the star‐forming regions is estimated to be ∼0.2 M ⊙ yr −1 . We suggest that the X‐ray emission is predominantly powered by starburst‐type activity, and argue that a blow‐out in the form of a galactic wind is the most likely fate for Mrk 33, resulting in the loss of most of the galaxy's metal‐enriched material and a small fraction (<1 per cent) of the ISM.