English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We report the results of spectroscopic mapping observations carried outtoward small (1 x 1 arcmin) regions within the supernova remnants W44, W28,IC443, and 3C391 using the Infrared Spectrograph of the Spitzer SpaceTelescope. These observations, covering the 5.2 - 37 micron spectral region,have led to the detection of a total of 15 fine structure transitions of Ne+,Ne++, Si+, P+, S, S++, Cl+, Fe+, and Fe++; the S(0) - S(7) pure rotationallines of molecular hydrogen; and the R(3) and R(4) transitions of hydrogendeuteride. In addition to these 25 spectral lines, the 6.2, 7.7, 8.6, 11.3 and12.6 micron PAH emission bands were also observed. Most of the detected linetransitions have proven strong enough to map in several sources, providing acomprehensive picture of the relative distribution of the various lineemissions observable in the Spitzer/IRS bandpass. A principal componentanalysis of the spectral line maps reveals that the observed emission linesfall into five distinct groups, each of which may exhibit a distinct spatialdistribution: (1) lines of S and H2 (J > 2); (2) the H2 S(0) line; (3) lines ofions with appearance potentials less than 13.6 eV; (4) lines of ions withappearance potentials greater than 13.6 eV, not including S++; (5) lines ofS++. Lines of group (1) likely originate in molecular material subject to aslow, nondissociative shock that is driven by the overpressure within thesupernova remnant, and lines in groups (3) - (5) are associated primarily withdissociative shock fronts with a range of (larger) shock velocities. The H2S(0) line shows a low-density diffuse emission component, and - in some sources- a shock-excited component.

Spitzer spectral line mapping of supernova remnants: I. Basic data and principal component analysis