Journal
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
Volume 194, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0067-0049/194/1/16
Keywords
H II regions; X-rays: individual (Carina, M17, NGC 3576, NGC 3603, 30 Doradus)
Categories
Funding
- Chandra [GO8-9131X, GO8-9006X, AR9-0001X, GO6-7006X, GO5-6080X, GO4-5007X]
- ACIS Instrument Team [SV4-74018]
- NASA [NAS8-03060]
- STFC [ST/F002092/1, ST/I001557/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002092/1, ST/I001557/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908038] Funding Source: National Science Foundation
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The Chandra Carina Complex Project (CCCP) has shown that the Carina Nebula displays bright, spatially-complex soft diffuse X-ray emission. Here, we sum up the CCCP diffuse emission work by comparing the global morphology and spectrum of Carina's diffuse X-ray emission to other famous sites of massive star formation with pronounced diffuse X-ray emission: M17, NGC 3576, NGC 3603, and 30 Doradus. All spectral models require at least two diffuse thermal plasma components to achieve adequate spectral fits, a softer component with kT = 0.2-0.6 keV and a harder component with kT = 0.5-0.9 keV. In several cases these hot plasmas appear to be in a state of non-equilibrium ionization that may indicate recent and current strong shocks. A cavity north of the embedded giant H II region NGC 3576 is the only region studied here that exhibits hard diffuse X-ray emission; this emission appears to be nonthermal and is likely due to a recent cavity supernova, as evidenced by a previously-known pulsar and a newly-discovered pulsar wind nebula also seen in this cavity. All of these targets exhibit X-ray emission lines that are not well modeled by variable-abundance thermal plasmas and that might be attributed to charge exchange at the shock between the hot, tenuous, X-ray-emitting plasma and cold, dense molecular material; this is likely evidence for dust destruction at the many hot/cold interfaces that characterize massive star-forming regions.
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