Dustwind closes after launch4/12/2023 We searched for X-ray supernova remnants (SNRs) in the starburst region of M 82, using archival data from the Chandra X-ray Observatory with a total effective exposure time of 620 ks with an X-ray spectroscopic selection. The spatial distribution of the $F_\mathrm$ regions are spatially confined by the HI ridge that is considered to be a birthplace of the SSCs, the spatial coincidences may indicate that dust grains around the SSCs are grains of relatively high crystallinity injected by massive stars originating from starburst activities and that those grains are blown away along the HI ridge and thus the western arm. The most prominent filamentary structure seen in the diffuse IR emission is spatially in good agreement with the western H$\alpha$ filament (western arm). Images show a diffuse infrared (IR) emission extending from the galactic disk into the halo region. We used a data set from AKARI and Herschel images at wavelengths from 7 $\mu$m to 500 $\mu$m to catch the evidence of dust processing in galactic winds in NGC 1569. Therefore, this galaxy hosts both the enshrouded compact core and the superwind-driving circumnuclear starburst. On the basis of comparison between this starburst–superwind scenario and the observations in terms of the burst age, stellar mass, infrared luminosity, and obscuration in the optical bands, we argue that this superwind-driving starburst is separate from the submillimeter core even if the core is a very young star cluster. It is powerful enough to drive the superwind within the dynamical age of the superwind (10 Myr). We also detected a moderately extinct starburst population in the Sloan Digital Sky Survey nuclear spectrum with a burst age of 10 Myr and stellar mass of 1 × 10⁷M ☉. ![]() This superwind shows basic characteristics similar to those of the prototypical superwind in the starburst galaxy M82, such as a kiloparsec-scale extended structure of gas and dust along the disk minor axis, outflowing components (multiphase gas and dust), physical conditions of the ionized gas, and monotonically blueshifting radial velocity field with increasing distance from the nucleus on the front side of the superwind. We detected dusty superwind outflow at 1 kpc scale along the disk semiminor axis in both shock-heated emission lines and enhanced interstellar Na D absorption. This galaxy has been known to host a compact obscured nucleus, showing distinct characteristics such as a very compact (~20 pc) submillimeter and mid-infrared core and dusty circumnuclear region with massive molecular gas concentration. We report our optical spectroscopic study of the nucleus and its surrounding region of a nearby luminous infrared galaxy NGC 4418. The infall of these new clumps back into the galaxy and their subsequent re-entrainment into the galactic outflow form a loop process of galactic material recycling. These are advected into the circumgalactic environment, where their remnants would seed condensation of the circumgalactic medium to form new clumps. We have shown that some clumps could survive their passage along a galactic outflow. Our findings are consistent with numerical simulations that have shown that cold dense clumps in galactic outflows can be compressed by ram pressure, and also progressively ablated and stripped before complete disintegration. They are stripped material torn from the slow-moving dense clumps by the faster moving ionized fluid, which are subsequently warmed and stretched into elongated shapes. The observed filamentary H α features are therefore not prime charge-exchange line emitters. From the charge-exchange lines observed in the nearby starburst galaxy M82, we conduct surfaceto-volume analyses and deduce that the cold dense clumps in its galactic outflow have flattened shapes, resembling a hamburger or a pancake morphology rather than elongated shapes. Chargeexchange lines that originate from the interfacing surface between the neutral and ionized components are a useful diagnostic of the cold dense structures in the galactic outflow. Large-scale outflows from starburst galaxies are multiphase, multicomponent fluids.
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