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The 37 pages that link to Initial mass function, each with the reason it gives.

• Stellar evolutionRelated: It determines how many stars enter each mass-dependent evolutionary pathway.

• Interstellar mediumRelated: Conditions in star-forming interstellar gas influence which stellar masses are produced.

• Star formationRelated: It records the range of stellar masses produced by a star-forming population.

• Stellar populationRelated: It determines which stellar masses were initially represented in a population.

• Brown dwarfRelated: Brown dwarf counts test whether this distribution continues smoothly below stellar masses.

• Stellar feedbackRelated: It sets how many massive, short-lived stars supply strong feedback per unit stellar mass.

• Stellar massRelated: It quantifies how many stars form at each mass.

• Massive starRelated: Its high-mass end determines how many massive stars enrich and energize a stellar population.

• Galactic chemical evolutionRelated: It determines how many stars of each mass contribute to later enrichment.

• Population III starRelated: Its form for metal-free stars determines whether they were mostly massive or included smaller survivors.

• Cosmic star-formation historyRelated: Converting light into formed stellar mass depends on assumptions about stellar birth masses.

• Star clusterRelated: It describes the range of stellar masses born in a cluster.

• T Tauri starRelated: It places T Tauri stars among the common low-mass products of star formation.

• Star formation rateRelated: Rate estimates infer total stellar mass from luminous stars by assuming a distribution of stellar birth masses.

• Free-floating planetRelated: Counts of isolated planetary-mass objects can test how far this distribution extends.

• Mass–luminosity relationRelated: Combining it with the relation predicts how a population’s stars contribute light.

• O-type starRelated: Its steep decline at high masses explains why O-type stars are rare.

• Star formation efficiencyCompared with: Efficiency counts total stellar mass, while the initial mass function describes its division among stellar masses.

• Pair-instability supernovaRelated: The scarcity of sufficiently massive progenitors depends on how frequently the highest-mass stars form.

• Planetary-mass objectRelated: Its low-mass end tests whether isolated planetary-mass objects form like stars or planets.

• Tarantula NebulaRelated: Its unusually rich massive-star population helps test whether this distribution changes in intense environments.

• Bok globuleRelated: Globule studies help test whether isolated clouds produce stars across a range of masses.

• Hayashi trackRelated: Track-based masses and ages help correct observed young populations when estimating this distribution.

• R136Related: The cluster helps test whether unusually dense star formation changes the high-mass end of this distribution.

• Rho Ophiuchi cloud complexRelated: Census of young objects in the complex can constrain the masses produced by a cloud.

• Stellar black holeRelated: It helps determine how many massive stars are available to produce black holes.

• Sub-brown dwarfRelated: Its low-mass end helps establish whether sub-brown dwarfs form as a continuation of stellar populations.

• Super star clusterRelated: It determines how many massive, short-lived stars a newly formed cluster contains.

• Interstellar cloudRelated: Cloud conditions and feedback help shape the masses of stars formed from them.

• Trapezium ClusterRelated: The cluster’s mixture of massive and lower-mass young stars informs studies of stellar birth populations.

• Young stellar objectRelated: How young objects gain and lose mass helps determine this birth-mass distribution.

• Astronomical masses and mass distributionsRelated: It connects the masses of individual stars to the total stellar mass of a population.

• Edwin E. SalpeterRelated: Salpeter’s 1955 formulation became a foundational model for stellar birth masses.

• Formation and evolution of stars and galaxiesRelated: Its form determines how many massive, short-lived stars drive feedback and enrich galaxies.

• Starburst regionRelated: Starburst rate estimates depend on how many massive stars form per unit stellar mass.

• Stochastic self-propagating star formation modelRelated: The model’s formation events ultimately contribute stars drawn from an initial mass distribution.

• Westerhout 40Related: The young population in Westerhout 40 provides evidence for studying the masses of newly formed stars.