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Current measurements indicate that the deuterium abundance in diffuse interstellar gas varies spatially by a factor of ~4 among sightlines extending beyond the Local Bubble. One plausible explanation ...
The quantity of dust in a spiral disk can be estimated using the dust's typical emission or the extinction of a known source. In this paper we compare two techniques, one based on emission and one on ...
We present a compelling case for a systematic and comprehensive study of the resolved and unresolved stellar populations, ISM, and immediate environments of galaxies throughout the local volume, defin...
We present a compelling case for a systematic and comprehensive study of the resolved and unresolved stellar populations, ISM, and immediate environments of galaxies throughout the local volume, defin...
We apply Support Vector Machines -- a machine learning algorithm -- to the task of classifying structures in the Interstellar Medium. As a case study, we present a position-position velocity data cube...
RX J1713.7-3946 is the most remarkable TeV {\gamma}-ray SNR which emits {\gamma}-rays in the highest energy range 10-100 TeV. We made a combined analysis of CO and HI in the SNR and derived the total ...
The ISM, powered by SNe, is turbulent and permeated by a magnetic field (with a mean and a turbulent component). It constitutes a frothy medium that is mostly out of equilibrium and is ram pressure do...
The fate of metals after they are released in starburst episodes is still unclear. What phases of the interstellar medium are involved, in which timescales?
We analyse SPI/INTEGRAL data on the 511 keV line from the Galactic Centre, accumulated over ~6 years of observations.
We present the results of the search for candidate Planetary Nebulae interacting with the interstellar medium (PN-ISM) in the framework of the INT Photometric H$\alpha$ Survey (IPHAS) and located in t...
Diagnostics of the Ionized ISM:The Importance of Density Fluctuations。
Winds from Low Mass Stars:impact on the ISM
HD 192281 and HD 10125:A Study of their Local ISM using Radio and Infrared Data。
Numerical Simulations of the Interaction of Colliding Stellar Winds with the ISM
[WC] Stellar wind turbulent outflows feeding the ism

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