curated interstellar bibliography
Extracting the multiphase structure of the neutral interstellar medium (ISM) is key to understand the star formation in galaxies. The radiative condensation of the diffuse warm neutral medium producing a
We investigate the physical properties of structures seen in channel map observations of 21 cm neutral hydrogen (H I) emission. H I intensity maps display prominent linear structures that are
The gases of the interstellar medium (ISM) possess orders of magnitude more mass than those of all the stars combined and are thus the prime component of the baryonic Universe.
Neutral hydrogen 21 cm transition is a useful tracer of the neutral interstellar medium. However, inferring physical condition from the observed 21 cm absorption and/or emission spectra is often not
We present a new map of interstellar reddening, covering the 39% of the sky with low H I column densities ({N}{{H}{{I}}}< 4× {10}20 cm-2 or E(B-V)≈ 45 mmag) at 16\buildrel{
We carried out synthetic observations of interstellar atomic hydrogen at 21 cm wavelength by utilizing the magnetohydrodynamic numerical simulations of the inhomogeneous turbulent interstellar medium. The cold neutral medium (CNM)
We have obtained deep HI observations in the direction of 22 continuum sources without previously detected cold neutral medium (CNM). 18 CNM clouds were detected with a typical HI column
The Galactic Arecibo L-band Feed Array H I (GALFA-H I) survey is mapping the entire Arecibo sky at 21 cm, over a velocity range of -700 to +700 km s-1
We present new L-band (1-2 GHz) observations of the nearby spiral galaxy M33 with 80 pc resolution obtained with the Karl G. Jansky Very Large Array. The H I observations,
Extragalactic astronomy relies on the accurate estimation of source photometry corrected for Milky Way dust extinction. This has motivated the creation of a number of “Galactic” dust maps. We investigate
New 21 cm H I observations made with the Green Bank Telescope show that the high-velocity cloud known as the Smith Cloud has a striking cometary appearance and many indications
We explore the relationship between dust-emission derived reddening E(B – V) and atomic hydrogen column density N(H I) derived from 21 cm emission surveys. We consider measurements at galactic latitudes
We identify a counterpart to a Galactic supershell in diffuse radio polarization, and use this to determine the magnetic fields associated with this object. GSH 006 – 15 + 7
We study infrared emission of 17 isolated, diffuse clouds with masses of order {10}2 {M}&sun; to test the hypothesis that grain property variations cause the apparently low gas-to-dust ratios that
Very little information exists concerning the properties of the interstellar medium (ISM)-induced starlight polarization at high Galactic latitudes. Future optopolarimetric surveys promise to fill this gap. We conduct a small-scale
Not Available van de Hulst, H. C.; Muller, C. A.; Oort, J. H. 1954, Bulletin of the Astronomical Institutes of the Netherlands, 12, 117 http://cdsads.u-strasbg.fr/abs/1954BAN….12..117V
We present methods and results from “21 cm Spectral Line Observations of Neutral Gas with the EVLA” (21-SPONGE), a large survey for Galactic neutral hydrogen (H i) absorption with the
Aims:We investigate the properties of the 21-cm radio-lines of galactic neutral hydrogen by decomposing, the profiles of “The Leiden/Argentine/Bonn (LAB) Survey of Galactic H I” into Gaussian components. The width
We report deep, high spectral resolution WSRT H I 21 cm observations of four high latitude compact radio sources, that have revealed a new population of tiny, discrete clouds in
We have carried out a sensitive high-latitude (|b| > 15?) HI 21 cm-line absorption survey towards 102 sources using the GMRT. With a 3sigma detection limit in optical depth of
We have used the Giant Meterwave Radio Telescope (GMRT) to measure the Galactic HI 21-cm line absorption towards 102 extragalactic radio continuum sources, located at high (|b| > 15?) Galactic
We consider the tiny-scale atomic structure (TSAS) on scales of tens of astronomical units, which has been detected by 21 cm absorption lines against quasars with VLBI techniques, against pulsars
Recent H I absorption surveys are used to derive H I temperatures T(H I) and their variation within a number of H I shells. In these shells T(H I) is