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A molecular cloud, sometimes called a stellar nursery (if star formation is occurring within), is a type of interstellar cloud, the density and size of which permit absorption nebulae, the formation of molecules (most commonly molecular hydrogen, H 2), and the formation of H II regions.
These filaments of cloud have dense "cores" of gas embedded within them—many of which are likely to gravitationally collapse and form stars. The Herschel results for this region, and subsequently reported results for other star-forming regions, imply that fragmentation of molecular-cloud filaments are fundamental to the star-formation process.
Map of the Vela Molecular Ridge. The Vela Molecular Ridge appears as a sequence of bright and dark nebulae, located on the northwestern side of Vela.The main sequence of nebulae that compose it is located a few degrees northwest of the star Lambda Velorum, while some dark ramifications also extend south of it, reaching the central areas of the constellation.
The cloud in the top left corner is LBN 1093 and Sh2-1 with the bright star being Pi Scorpii and the yellowish cloud in the middle on the left being Sh2-7 with Dschubba at its center. A starchart of the Galactic Center area, with the Rho Ophiuchi cloud complex marked as large green area in the middle of the right half of the chart.
Maggie is a vast cloud of hydrogen gas observed within our own Milky Way galaxy. It is a filament of hydrogen 3,900 light-years long and 130 light-years wide. It is a single coherent structure with all parts showing similar velocity with respect to the local standard of rest. It is one of the biggest structures within the Milky Way.
The molecular cloud at these wavelengths is traced by emission from warm dust in the clouds, allowing the structure of the clouds to be probed. Wavelet analysis of the molecular clouds in the approximately 11 square degree Herschel field of view breaks up the clouds into numerous filaments, mostly in and around the Westerhout 40 region. [20]
In astronomy, the initial mass function (IMF) is an empirical function that describes the initial distribution of masses for a population of stars during star formation. [1] IMF not only describes the formation and evolution of individual stars, it also serves as an important link that describes the formation and evolution of galaxies.
An MeerKAT image of the Galactic Center showing a number of filaments Radio image of a number of parallel filaments in the Galactic Center; Sagittarius A*, the Milky Way's central black hole, is located in the bright region in the bottom right [1] [2] Nonthermal radio filaments from the 4'' resolution MeerKAT mosaic; oriented vertically for space; scales given assuming a distance of 8.2 kpc