Results 1 to 10 of about 1,909 (165)
Organic molecules in translucent interstellar clouds. [PDF]
Orig Life Evol Biosph, 2014 Absorption spectra of translucent interstellar clouds contain many known molecular bands of CN, CH+, CH, OH, OH(+), NH, C2 and C3. Moreover, one can observe more than 400 unidentified absorption features, known as diffuse interstellar bands (DIBs), commonly believed to be carried by complex, carbon-bearing molecules.
Krełowski J.
europepmc +4 more sources
CaFe interstellar clouds* [PDF]
Monthly Notices of the Royal Astronomical Society, 2007 A new kind of interstellar cloud is proposed. These are rare (just a few examples among ∼300 lines of sight) objects with the Ca I 4227-Å, Fe I 3720-Å and 3860-Å lines stronger than those of K I (near 7699 Å) and Na I (near 3302 Å). We propose the name ‘CaFe’ for these clouds.
A. Bondar +5 more
openaire +2 more sources
Dust evolution, a global view I. Nanoparticles, nascence, nitrogen and natural selection … joining the dots [PDF]
Royal Society Open Science, 2016 The role and importance of nanoparticles for interstellar chemistry and beyond is explored within the framework of The Heterogeneous dust Evolution Model for Interstellar Solids (THEMIS), focusing on their active surface chemistry, the effects of ...
A. P. Jones
doaj +1 more source
Presumed Detection of C5 Molecule in the Interstellar Medium
The Astrophysical Journal, 2022 The paper suggests the presence of the carbon chain C _5 molecule in translucent, interstellar H i clouds. This species, the only five atom interstellar molecule, observable in dark, translucent clouds, seems to be observable in reasonably dense clouds ...
J. Krełowski, R. Hakalla, W. Szajna
doaj +1 more source
Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
The Astrophysical Journal Supplement Series, 2023 In this paper we present the distribution of molecular gas in the Milky Way Galactic plane from l = [59.75, 74.75]° and b = [−5.25, +5.25]°, using the MWISP ^12 CO/ ^13 CO/C ^18 O emission-line data.
Chunxue Li +8 more
doaj +1 more source
Neutral Atomic and Molecular Clouds and Star Formation in the Outer Carina Arm
The Astrophysical Journal, 2023 We present a comprehensive investigation of H i (super)clouds, molecular clouds (MCs), and star formation in the Carina spiral arm of the outer Galaxy.
Geumsook Park +3 more
doaj +1 more source
The mass spectrum of interstellar clouds [PDF]
International Astronomical Union Colloquium, 1989 AbstractThe abundance of 21-cm absorption lines seen in surveys at high latitudes can be translated into a line of sight abundance of clouds vs. column density using an empirical relationship between temperature and optical depth. As VLA surveys of 21-cm absorption at low latitudes are now becoming available, it is possible to study the variation of ...
John M. Dickey, Robert W. Garwood
openaire +1 more source
Measuring the fractal structure of interstellar clouds [PDF]
Symposium - International Astronomical Union, 1991 To study the structure of interstellar clouds we used the so-called perimeter-area relation to estimate fractal dimensions. We studied the reliability of the method by applying it to artificial fractals and discuss some of the problems and pitfalls. Results for two different cloud types (high-
Vogelaar, M.G.R +2 more
openaire +2 more sources
Turbulence in Interstellar Clouds [PDF]
International Astronomical Union Colloquium, 1989 Above masses of the order of lOO M⊙, molecular clouds have masses and sizes which scale like those of self-gravitating polytropes bounded by an external pervading pressure. It is unlikely that this scaling is due to mere observational bias. But the physics underlying this behaviour is far from being understood.
openaire +1 more source
A Search for OH 18 cm Emission from Intermediate-velocity Gas at High Galactic Latitudes
The Astrophysical Journal, 2023 We present search results of 22 high-latitude (∣ b ∣ > 25°) sightlines for OH 18 cm emission using the 305 m radio telescope at the Arecibo Observatory. These sightlines appear in neutral hydrogen emission at intermediate velocities −90 ≤ V _LSR ≤ −20 km
Allison J. Smith, D. Anish Roshi
doaj +1 more source