We present initial XMM–Newton EPIC observations of the prototypical starburst galaxy M82. The superwind is seen to extend continuously from the starburst region to the X‐ray emission associated with the Hα‘cap’. We also find evidence for a ridge feature, probably associated with the superwind interacting with an H i streamer. Narrow‐band images, centred on individual X‐ray lines, show differences in morphology, with higher energy lines being less spatially extended, and a systematic shift with energy in the region of peak emission. Spectral fits with two thermal and one power‐law component provide a good fit to the spectra of the nuclear and inner wind regions, indicating a multiphase superwind. We discuss the implications of these observations on our understanding of superwinds.
We present results from a 30 ksec Chandra observation of the important starburst galaxy NGC 2782, covering the 0.3-10 keV energy band. We find evidence of a superwind of small extent, that is likely in an early stage of development.We find a total of 27 X-ray point sources within a region of radius 2D 25 of the galaxy centre and which are likely associated with the galaxy. Of these, 13 are ULXs (L X 10 39 erg s −1 ) and a number have likely counterparts. The X-ray luminosities of the ULX candidates are 1.2 − 3.9 × 10 39 erg s −1 . NGC 2782 seems to have an unusually large number of ULXs.Central diffuse X-ray emission extending to ∼ 3 kpc from the nuclear region has been detected. We also find an X-ray structure to the south of the nucleus, coincident with Hα filaments and with a 5 GHz radio source. We interpret this as a blow-out region of a forming superwind. This X-ray bubble has a total luminosity (0.3-10 keV) of 5 × 10 39 erg s −1 (around 15% of the total luminosity of the extended emission), and an inferred wind mass of 1.5 × 10 6 M . We also discuss the nature of the central X-ray source in NGC 2782, and conclude that it is likely a low-luminosity AGN (LLAGN), with a total X-ray luminosity of L X = 6 × 10 40 erg s −1 , with strong Fe line emission at 6.4 keV.
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