The initial mass function 50 years later
By E. Corbelli, F. Palla, H. Zinnecker. 2005
366 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Oceanography
View Paper: https://www.semanticscholar.org/paper/dd8ea4617de0fc74e47ddddeb5e9a7cc0912e2c8
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Citations in the corpus
- Age-dating luminous red galaxies observed with the Southern African Large Telescope (2016, background): “…1997; Leitherer et al. 1999; Bruzual & Charlot 2003; Le Borgne et al. 2004; Jimenez et al. 2004; González Delgado et al. 2005; Maraston 2005; Tantalo 2005; Coelho et al. 2007; Schiavon 2007; Conroy, Gunn, & White 2009; Eldridge & Stanway 2009; Kotulla et al. 2009; Mollá, García-Vargas, &…”
- STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, background): “There is no compelling reason to abandon the Salpeter IMF (Renzini 2005), but it is a possibility explored in the literature.”
- FIRE-2 simulations: physics versus numerics in galaxy formation (2017, background): “In each case, the shape of the mass function is, as expected, a power-law with slope dN/dM ∝ M−(1.6−1.8) (very similar to observed; see Blitz & Rosolowsky 2005; Rice et al. 2016), and turnover at a maximum mass about the Toomre mass MToomre defined above (also as expected from observations and…”
- The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, background): “Van Dokkum & van der Marel (2007) find that it is easier to understand early-type fundamental plane evolution at z 1 with a slightly top-heavy IMF (as also argued by Renzini 2005).”
- The lifecycle of molecular clouds in nearby star-forming disc galaxies (2019, methodology): “They sample stars stochastically from a Chabrier (2005) initial mass function (IMF) and use Geneva stellar evolutionary tracks (Schaller et al. 1992) with STARBURST99 spectral synthesis (Leitherer et al. 2014).8 Haydon et al. (2018) calibrate tstar,ref using an SPS model describing an instantaneous…”
- A unified model for galactic discs: star formation, turbulence driving, and mass transport (2017, methodology): “The observations have been homogenized to a Chabrier (2005) IMF and the convention for αCO suggested by Daddi et al. (2010a); see Appendix A and Krumholz et al. (2012) for details. and without transport.7 The physical origin of this difference is easy to understand.”
- A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey (2015, methodology): “For comparison, the lognormal part of the Chabrier (2005) system IMF has a central mass of 0.25 M and a standard deviation of 0.55 in log10M.”
- Evidence for TP-AGB Stars in High-Redshift Galaxies, and Their Effect on Deriving Stellar Population Parameters (2006, background): “…evidence, from the redshift evolution of the fundamental plane to theM/L of local Es to the metal content of the intergalactic medium strongly favor a Salpeter-like IMF down to 1 M but flatter below as required to agree with the dynamically estimatedM/L ratios of earlytype galaxies (Renzini 2005).”
- Theory of Star Formation (2007, background): “Research on formal turbulence theory is quite active (see Elmegreen & Scalo, 2004 for a review of the recent theoretical literature relevant to the ISM), although a comprehensive framework remains elusive.”
- The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, background): “From these constraints and from the metal abundance in the clusters’ interstellar medium, Renzini (2005) concluded that elliptical galaxies as a class must have an IMF close to Salpeter for stellar masses m > 1 M , while the IMF must flatten at lower masses, similar to the Kroupa IMF.”