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
Galactic bars can affect the evolution of galaxies by redistributing gas in galaxies, possibly contributing to the cessation of star formation. Recent works point to ‘bar quenching’ playing an important
We utilize the multi-wavelength data of M33 to study the origin of turbulence in its interstellar medium. We find that the HI turbulent energy surface density inside 8 kpc is
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,
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 present results from multi-epoch neutral hydrogen (H I) absorption observations of six bright pulsars with the Arecibo telescope. Moving through the interstellar medium (ISM) with transverse velocities of 10-150
Context. In the previous papers of this series, we decomposed all the H I 21-cm line profiles of the Leiden-Argentina-Bonn (LAB) database into Gaussian components (GCs), and studied the statistical
We confirm and discuss recently discovered cold H I clouds with column densities among the lowest ever detected. The column densities of the cold neutral medium (CNM) toward 3C 286
We use the Gaussian fit results of Paper I to investigate the properties of interstellar H I in the solar neighborhood. The warm and cold neutral media (WNM and CNM)
The properties of interstellar H I are investigated using high-velocity resolution, Arecibo emission-absorption spectra in the direction of 40 radio continuum sources, including 21 at low Galactic latitude. Comparison of
Arecibo 3-arcsec beam neutral hydrogen emission-absorption observations are analyzed, and spin temperature results in the direction of ‘small’ and ‘large’ extragalactic sources are found to be statistically similar. The variations
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