Linked from

The 19 pages that link to Molecular hydrogen, each with the reason it gives.

• Star formationRelated: Its presence marks the cold molecular environments where collapse commonly occurs.

• Molecular cloudRelated: Its rotational emission reveals molecular gas, though the molecule itself is difficult to observe directly.

• Interstellar dustRelated: Dust surfaces catalyze the formation of molecular hydrogen from atomic hydrogen.

• Galaxy quenchingRelated: Its abundance tracks the fuel available for ongoing star formation.

• Herbig–Haro objectRelated: Near-infrared molecular-hydrogen emission traces cooler regions of some outflows.

• Population III starRelated: It was the principal coolant allowing primordial gas clouds to fragment and collapse.

• Star formation rateRelated: Its distribution is commonly used to estimate the gas reservoir available for star formation.

• Interstellar chemistryRelated: H₂ dominates molecular gas and influences the pathways that build heavier molecules.

• Astrophysical maserRelated: It dominates molecular clouds, though its lack of a permanent dipole makes it difficult to observe directly.

• Sagittarius B2Related: It makes up most of Sagittarius B2’s molecular gas, though astronomers often trace that gas with other molecules.

• Kennicutt–Schmidt lawRelated: Molecular gas often tracks star-forming material more directly than total gas.

• Rho Ophiuchi cloud complexRelated: It dominates the cloud mass, although it is difficult to observe directly.

• Interstellar cloudRelated: It is the most abundant molecule in cold, dense clouds, though difficult to observe directly.

• NGC 7027Related: Infrared observations trace molecular hydrogen in the nebula's dense outer regions.