Computer Science
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009eimw.confe..39m&link_type=abstract
"The Evolving ISM in the Milky Way and Nearby Galaxies, The Fourth Spitzer Science Center Conference, Proceedings of the confere
Computer Science
Galaxies: Ism, Infrared: Galaxies, Infrared: Ism, Dust, Extinction, Galaxies: Individual (Ngc 1569)
Scientific paper
We report the results of recent near- to mid-infrared imaging and spectroscopic observations of the starburst dwarf galaxy NGC 1569 with the Infrared Camera (IRC) on board AKARI. Infrared imaging observations with 6 bands of the IRC (3, 4, 7, 11, 15, and 24 μm) indicate that super star clusters (SSCs) are faint at 7 μm (S7 band) relative to 15 and 24 μm, while a structure associated with a Hα filament is clearly seen at S7. Since the S7 band efficiently probes the 6.2 and 7.7 μm unidentified infrared (UIR) band emissions, which are attributed to polycyclic aromatic hydrocarbons (PAHs), the filament should contain an appreciable amount of PAHs. Follow-up observations of near- to mid-infrared spectroscopy (2--13 μm) also with the IRC indeed confirm the presence of the 6.2, 7.7, and 11.2 μm band features in the filament for the first time. The spectrum has a strong 11.2 μm band relative to the 7.7 μm band compared to that of SSC A taken with IRS on Spitzer. The filament encloses the X-ray emitting gas and is thought to be created by the outflow from the galaxy. Because the destruction time scale of PAHs in the plasma gas is quite short, it is suggested that the PAHs in the filament are produced from the fragmentation of large carbonaceous grains in the shock. The near-infrared spectrum also suggests the presence of excess emission in 3--5 μm in the filament for the first time, which may come from very small grains.
Matsumoto Haru
Onaka Takashi
Sakon Itsuki
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