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Journal articles on the topic 'Stellar initial mass function'

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Published: 10 December 2022

Last updated: 29 January 2023

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1

Hopkins, Andrew. "Measuring the stellar initial mass function." Proceedings of the International Astronomical Union 15, S352 (June 2019): 98. http://dx.doi.org/10.1017/s1743921320001155.

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AbstractThe birth of stars and the formation of galaxies are cornerstones of modern astrophysics. While much is known about how galaxies globally and their stars individually form and evolve, one fundamental property that affects both remains elusive. This is problematic because this key property, the stellar initial mass function (IMF), is a key tracer of the physics of star formation that underpins almost all of the unknowns in galaxy and stellar evolution. It is perhaps the greatest source of systematic uncertainty in star and galaxy evolution. The past decade has seen a growing number and variety of methods for measuring or inferring the shape of the IMF, along with progressively more detailed simulations, paralleled by refinements in the way the concept of the IMF is applied or conceptualised on different physical scales. This range of approaches and evolving definitions of the quantity being measured has in turn led to conflicting conclusions regarding whether or not the IMF is universal. Here I summarise the growing wealth of approaches to our understanding of this fundamental property that defines so much of astrophysics, and highlight the importance of considering potential IMF variations, reinforcing the need for measurements to quantify their scope and uncertainties carefully. I present a new framework to aid the discussion of the IMF and promote clarity in the further development of this fundamental field.

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2

Larson, R. B. "Towards understanding the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 256, no. 4 (June 15, 1992): 641–46. http://dx.doi.org/10.1093/mnras/256.4.641.

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3

Ferreras, Ignacio, Francesco La Barbera, and Alexandre Vazdekis. "Is the stellar initial mass function universal?" Astronomy & Geophysics 57, no. 2 (March 30, 2016): 2.32–2.36. http://dx.doi.org/10.1093/astrogeo/atw074.

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4

Chabrier, Gilles. "Galactic Stellar and Substellar Initial Mass Function." Publications of the Astronomical Society of the Pacific 115, no. 809 (July 2003): 763–95. http://dx.doi.org/10.1086/376392.

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5

Maschberger, T. "On the function describing the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 429, no. 2 (December 20, 2012): 1725–33. http://dx.doi.org/10.1093/mnras/sts479.

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6

Schaerer, Daniel. "The massive star Initial Mass function." Symposium - International Astronomical Union 212 (2003): 642–51. http://dx.doi.org/10.1017/s007418090021303x.

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We review our current knowledge on the IMF in nearby environments, massive star forming regions, super star clusters, starbursts and alike objects from studies of integrated light, and discuss the various techniques used to constrain the IMF. In most cases, including UV-optical studies of stellar features and optical-IR analysis of nebular emission, the data is found to be compatible with a ‘universal’ Salpeter-like IMF with a high upper mass cut-off over a large metallicity range. In contrast, near-IR observations of nuclear starbursts and LIRG show indications of a lowerMupand/or a steeper IMF slope, for which no alternate explanation has yet been found. Also, dynamical mass measurements of seven super star clusters provide so far no simple picture of the IMF. Finally, we present recent results of a direct stellar probe of the upper end of the IMF in metal-rich H ii regions, showing no deficiency of massive stars at high metallicity, and determining a lower limit ofMup≳ 60 – 90 M⊙.

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7

Padoan, P., A. Nordlund, and B. J. T. Jones. "The universality of the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 288, no. 1 (June 11, 1997): 145–52. http://dx.doi.org/10.1093/mnras/288.1.145.

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8

Nakamura, Fumitaka, and Masayuki Umemura. "The Stellar Initial Mass Function in Primordial Galaxies." Astrophysical Journal 569, no. 2 (April 20, 2002): 549–57. http://dx.doi.org/10.1086/339392.

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9

Larson, Richard B. "Some processes influencing the stellar initial mass function." Symposium - International Astronomical Union 147 (1991): 261–73. http://dx.doi.org/10.1017/s0074180900239600.

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Current evidence suggests that the stellar initial mass function has the same basic form everywhere, and that its fundamental features are (1) the existence of a characteristic stellar mass of order one solar mass, and (2) the existence of an apparently universal power-law form for the mass spectrum of the more massive stars. The characteristic stellar mass may be determined in part by the typical mass scale for the fragmentation of star forming clouds, which is predicted to be of the order of one solar mass. The power-law extension of the mass spectrum toward higher masses may result from the continuing accretional growth of some stars to much larger masses; the fact that the most massive stars appear to form preferentially in cluster cores suggests that such continuing accretion may be particularly important at the centers of clusters. Numerical simulations suggest that forming systems of stars may tend to develop a hierarchical structure, possibly self-similar in nature. If most stars form in such hierarchically structured systems, and if the mass of the most massive star that forms in each subcluster increases as a power of the mass of the subcluster, then a mass spectrum of power-law form is predicted. Some possible physical effects that could lead to such a relation are briefly discussed, and some observational tests of the ideas discussed here are proposed.

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10

Leitherer, Claus. "The Stellar Initial Mass Function in Starburst Galaxies." Symposium - International Astronomical Union 186 (1999): 243–50. http://dx.doi.org/10.1017/s0074180900112707.

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Starburst galaxies are currently forming massive stars at prodigious rates. I discuss the star-formation histories and the shape of the initial mass function, with particular emphasis on the high- and on the low-mass end. The classical Salpeter IMF is consistent with constraints from observations of the most massive stars, irrespective of environmental properties. The situation at the low-mass end is less clear: direct star counts in nearby giant H II regions show stars down to ~1 M⊙, whereas dynamical arguments in some starburst galaxies suggest a deficit of such stars.

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11

Larson, Richard B. "Some processes influencing the stellar initial mass function." Symposium - International Astronomical Union 147 (1991): 261–73. http://dx.doi.org/10.1017/s0074180900198985.

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Current evidence suggests that the stellar initial mass function has the same basic form everywhere, and that its fundamental features are (1) the existence of a characteristic stellar mass of order one solar mass, and (2) the existence of an apparently universal power-law form for the mass spectrum of the more massive stars. The characteristic stellar mass may be determined in part by the typical mass scale for the fragmentation of star forming clouds, which is predicted to be of the order of one solar mass. The power-law extension of the mass spectrum toward higher masses may result from the continuing accretional growth of some stars to much larger masses; the fact that the most massive stars appear to form preferentially in cluster cores suggests that such continuing accretion may be particularly important at the centers of clusters. Numerical simulations suggest that forming systems of stars may tend to develop a hierarchical structure, possibly self-similar in nature. If most stars form in such hierarchically structured systems, and if the mass of the most massive star that forms in each subcluster increases as a power of the mass of the subcluster, then a mass spectrum of power-law form is predicted. Some possible physical effects that could lead to such a relation are briefly discussed, and some observational tests of the ideas discussed here are proposed.

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12

Padoan, Paolo, and Ake Nordlund. "The Stellar Initial Mass Function from Turbulent Fragmentation." Astrophysical Journal 576, no. 2 (September 10, 2002): 870–79. http://dx.doi.org/10.1086/341790.

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13

Hennebelle, Patrick, and Gilles Chabrier. "Theories of the initial mass function." Proceedings of the International Astronomical Union 6, S270 (May 2010): 159–68. http://dx.doi.org/10.1017/s1743921311000329.

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AbstractWe review the various theories which have been proposed along the years to explain the origin of the stellar initial mass function. We pay particular attention to four models, namely the competitive accretion and the theories based respectively on stopped accretion, MHD shocks and turbulent dispersion. In each case, we derive the main assumptions and calculations that support each theory and stress their respective successes and failures or difficulties.

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14

Weisz, Daniel R., L. Clifton Johnson, Daniel Foreman-Mackey, Andrew E. Dolphin, Lori C. Beerman, Benjamin F. Williams, Julianne J. Dalcanton, et al. "THE HIGH-MASS STELLAR INITIAL MASS FUNCTION IN M31 CLUSTERS." Astrophysical Journal 806, no. 2 (June 18, 2015): 198. http://dx.doi.org/10.1088/0004-637x/806/2/198.

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15

Shetty, Shravan, and Michele Cappellari. "Initial Mass Function for Massive Galaxies at z ~ 1." Proceedings of the International Astronomical Union 10, S311 (July 2014): 136–39. http://dx.doi.org/10.1017/s1743921315003543.

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AbstractWe present the results on the stellar Initial Mass Function (IMF) normalisation of 68 massive (M* = 1011 - 1012M⋖) Early-Type Galaxies (ETGs) at redshift of ~1. This was achieved by deriving the stellar Mass-to-Light ratio (M/L) of the galaxies through axis-symmetric dynamical modelling and comparing it to the same derived via stellar population modelling through full spectrum fitting. The study also employs an Abundance Matching technique to account for the dark matter within the galaxies. The results demonstrate that massive ETGs at high redshifts on average have a Salpeter-like IMF normalisation, while providing observational evidence supporting previous predictions of low dark matter fraction in the inner regions (<1Re) of galaxies at higher redshift.

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16

Hopkins, Philip F. "The stellar initial mass function, core mass function and the last-crossing distribution." Monthly Notices of the Royal Astronomical Society 423, no. 3 (May 23, 2012): 2037–44. http://dx.doi.org/10.1111/j.1365-2966.2012.20731.x.

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17

Riaz, Rafeel, Dominik R. G. Schleicher, Siegfried Vanaverbeke, and Ralf S. Klessen. "Stellar initial mass function over a range of redshifts." Astronomische Nachrichten 342, no. 1-2 (January 2021): 157–63. http://dx.doi.org/10.1002/asna.202113897.

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18

Bonnell, I. A., C. J. Clarke, M. R. Bate, and J. E. Pringle. "Accretion in stellar clusters and the initial mass function." Monthly Notices of the Royal Astronomical Society 324, no. 3 (June 21, 2001): 573–79. http://dx.doi.org/10.1046/j.1365-8711.2001.04311.x.

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19

de Freitas, D. B., R. T. Eufrásio, M. M. F. Nepomuceno, and J. R. P. da Silva. "A nonextensive insight into the stellar initial mass function." EPL (Europhysics Letters) 125, no. 6 (May 7, 2019): 69002. http://dx.doi.org/10.1209/0295-5075/125/69002.

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20

Wyse, Rosemary F. G. "The Intracluster Medium: An Invariant Stellar Initial Mass Function." Astrophysical Journal 490, no. 1 (November 20, 1997): L69—L72. http://dx.doi.org/10.1086/311021.

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21

Yan, Zhiqiang, Tereza Jerabkova, and Pavel Kroupa. "The optimally sampled galaxy-wide stellar initial mass function." Astronomy & Astrophysics 607 (November 2017): A126. http://dx.doi.org/10.1051/0004-6361/201730987.

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22

Hartwig, Tilman, Volker Bromm, Ralf S. Klessen, and Simon C. O. Glover. "Constraining the primordial initial mass function with stellar archaeology." Monthly Notices of the Royal Astronomical Society 447, no. 4 (January 29, 2015): 3892–908. http://dx.doi.org/10.1093/mnras/stu2740.

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23

Li, Jiadong, Chao Liu, Zhi-Yu Zhang, Hao Tian, Xiaoting Fu, Jiao Li, and Zhi-Qiang Yan. "Stellar initial mass function varies with metallicity and time." Nature 613, no. 7944 (January 18, 2023): 460–62. http://dx.doi.org/10.1038/s41586-022-05488-1.

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24

Zinnecker, Hans. "The Initial Mass Function in Young Star Clusters." Highlights of Astronomy 7 (1986): 489–99. http://dx.doi.org/10.1017/s1539299600006821.

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AbstractThis review discusses both the earlier and the most recent work on the IMF in young star clusters. It is argued that the study of the stellar content of young star clusters offers the best chance of developing a theory of star formation and of the IMF.

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25

Dabringhausen, J. "Simple interpolation functions for the galaxy-wide stellar initial mass function and its effects in early-type galaxies." Monthly Notices of the Royal Astronomical Society 490, no. 1 (September 13, 2019): 848–67. http://dx.doi.org/10.1093/mnras/stz2562.

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ABSTRACT The galaxy-wide stellar initial mass function (IGIMF) of a galaxy is thought to depend on its star formation rate (SFR). Using a catalogue of observational properties of early-type galaxies (ETGs) and a relation that correlates the formation time-scales of ETGs with their stellar masses, the dependencies of the IGIMF on the SFR are translated into dependencies on more intuitive parameters like present-day luminosities in different passbands. It is found that up to a luminosity of approximately 109 L⊙ (quite independent of the considered passband), the total masses of the stellar populations of ETGs are slightly lower than expected from the canonical stellar initial mass function (IMF). However, the actual mass of the stellar populations of the most luminous ETGs may be up to two times higher than expected from a simple stellar population model with the canonical IMF. The variation of the IGIMF with the mass of ETGs is presented here also as convenient functions of the luminosity in various passbands.

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26

Rubin, Douglas, and Abraham Loeb. "Constraining the Stellar Mass Function in the Galactic Center via Mass Loss from Stellar Collisions." Advances in Astronomy 2011 (2011): 1–19. http://dx.doi.org/10.1155/2011/174105.

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The dense concentration of stars and high-velocity dispersions in the Galactic center imply that stellar collisions frequently occur. Stellar collisions could therefore result in significant mass loss rates. We calculate the amount of stellar mass lost due to indirect and direct stellar collisions and find its dependence on the present-day mass function of stars. We find that the total mass loss rate in the Galactic center due to stellar collisions is sensitive to the present-day mass function adopted. We use the observed diffuse X-ray luminosity in the Galactic center to preclude any present-day mass functions that result in mass loss rates>10-5M⨀yr−1in the vicinity of~1″. For present-day mass functions of the form,dN/dM∝M-α, we constrain the present-day mass function to have a minimum stellar mass≲7M⨀and a power-law slope≳1.25. We also use this result to constrain the initial mass function in the Galactic center by considering different star formation scenarios.

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27

Goodwin, S. P., D. Nutter, P. Kroupa, D. Ward-Thompson, and A. P. Whitworth. "The relationship between the prestellar core mass function and the stellar initial mass function." Astronomy & Astrophysics 477, no. 3 (November 6, 2007): 823–27. http://dx.doi.org/10.1051/0004-6361:20078452.

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28

Holman, K., S. K. Walch, S. P. Goodwin, and A. P. Whitworth. "Mapping the core mass function on to the stellar initial mass function: multiplicity matters." Monthly Notices of the Royal Astronomical Society 432, no. 4 (May 21, 2013): 3534–43. http://dx.doi.org/10.1093/mnras/stt705.

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29

Davé, Romeel. "The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function?" Monthly Notices of the Royal Astronomical Society 385, no. 1 (February 7, 2008): 147–60. http://dx.doi.org/10.1111/j.1365-2966.2008.12866.x.

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30

Malkov, O. Yu. "On the Mass Distribution of Stellar-Mass Black Holes." Open Astronomy 23, no. 3-4 (December 1, 2014): 267–71. http://dx.doi.org/10.1515/astro-2017-0190.

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AbstractThe observational stellar-mass black hole mass distribution exhibits a maximum at about 8 M⊙. It can be explained via the details of the massive star evolution, supernova explosions, or consequent black hole evolution. We propose another explanation, connected with an underestimated influence of the relation between the initial stellar mass and the compact remnant mass. We show that an unimodal observational mass distribution of black holes can be produced by a power-law initial mass function and a monotonic “remnant mass versus initial mass” relation.

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31

Webb, Jeremy J., and Jo Bovy. "Variation in the stellar mass function along stellar streams." Monthly Notices of the Royal Astronomical Society 510, no. 1 (December 1, 2021): 774–85. http://dx.doi.org/10.1093/mnras/stab3451.

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ABSTRACT Stellar streams are the inevitable end product of star cluster evolution, with the properties of a given stream being related to its progenitor. We consider how the dynamical history of a progenitor cluster, as traced by the evolution of its stellar mass function, is reflected in the resultant stream. We generate model streams by evolving star clusters with a range of initial half-mass relaxation times and dissolution times via direct N-body simulations. Stellar streams that dissolve quickly show no variation in the stellar mass function along the stream. Variation is, however, observed along streams with progenitor clusters that dissolve after several relaxation times. The mass function at the edges of a stream is approximately primordial, as it is populated by the first stars to escape the cluster before segregation occurs. Moving inwards the mass function steepens as the intermediate parts of the stream consist of mostly low-mass stars that escaped the cluster after some segregation has occurred. The centre of the stream is then marked by a flatter mass function, as the region is dominated by high-mass stars that quickly segregated to the progenitor cluster’s centre and were the last stars to become unbound. We further find that the maximum slope of the mass function along the stream and the rate at which it decreases with distance from the dissolved progenitor serve as proxies for the dynamical state reached by the progenitor cluster before dissolution; this may be able to be applied to observed streams with near-future observations.

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32

Elmegreen, Bruce G. "Modeling a High‐Mass Turn‐Down in the Stellar Initial Mass Function." Astrophysical Journal 539, no. 1 (August 10, 2000): 342–51. http://dx.doi.org/10.1086/309204.

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33

Ballesteros-Paredes, Javier, Lee W. Hartmann, Nadia Pérez-Goytia, and Aleksandra Kuznetsova. "Bondi–Hoyle–Littleton accretion and the upper-mass stellar initial mass function." Monthly Notices of the Royal Astronomical Society 452, no. 1 (July 6, 2015): 566–74. http://dx.doi.org/10.1093/mnras/stv1285.

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34

Sharda, Piyush, and Mark R. Krumholz. "When did the initial mass function become bottom-heavy?" Monthly Notices of the Royal Astronomical Society 509, no. 2 (October 9, 2021): 1959–84. http://dx.doi.org/10.1093/mnras/stab2921.

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ABSTRACT The characteristic mass that sets the peak of the stellar initial mass function (IMF) is closely linked to the thermodynamic behaviour of interstellar gas, which controls how gas fragments as it collapses under gravity. As the Universe has grown in metal abundance over cosmic time, this thermodynamic behaviour has evolved from a primordial regime dominated by the competition between compressional heating and molecular hydrogen cooling to a modern regime where the dominant process in dense gas is protostellar radiation feedback, transmitted to the gas by dust–gas collisions. In this paper, we map out the primordial-to-modern transition by constructing a model for the thermodynamics of collapsing, dusty gas clouds at a wide range of metallicities. We show the transition from the primordial regime to the modern regime begins at metallicity $Z\sim 10^{-4} \,\rm {Z_\odot }$, passes through an intermediate stage where metal line cooling is dominant at $Z \sim 10^{-3}\, \rm {Z_{\odot }}$, and then transitions to the modern dust- and feedback-dominated regime at $Z\sim 10^{-2}\, \rm {Z_\odot }$. In low pressure environments like the Milky Way, this transition is accompanied by a dramatic change in the characteristic stellar mass, from ${\sim}50\, \rm {M_\odot }$ at $Z \sim 10^{-6}\, \rm {Z_{\odot }}$ to ${\sim}0.3\, \rm {M_\odot }$ once radiation feedback begins to dominate, which marks the appearance of the modern bottom-heavy Milky Way IMF. In the high pressure environments typical of massive elliptical galaxies, the characteristic mass for the modern, dust-dominated regime falls to ${\sim}0.1\, \rm {M_{\odot }}$, thus providing an explanation for the more bottom-heavy IMF observed in these galaxies. We conclude that metallicity is a key driver of variations in the characteristic stellar mass, and by extension, the IMF.

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35

Larson, Richard B. "Fragmentation and the Initial Mass Function." International Astronomical Union Colloquium 120 (1989): 44–55. http://dx.doi.org/10.1017/s0252921100023472.

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A central problem in the theory of star formation is to understand the spectrum of masses, or Initial Mass Function, with which stars are formed. The fundamental role of the IMF in galactic evolution has been described by Tinsley (1980), and an extensive review of evidence concerning the IMF and its possible variability has been presented by Scalo (1986). Although the IMF derived from the observations is subject to many uncertainties, two basic features seem reasonably well established. One is that the typical stellar mass, defined such that equal amounts of matter condense into stars above and below this mass, is within a factor of 3 of one solar mass. A theory of star formation should therefore be able to explain why most stars are formed with masses of order one solar mass. The second apparently universal feature is that the IMF for relatively massive stars can be approximated by a power law with a slope not greatly different from that originally proposed by Salpeter (1955). Thus we also need to understand why the IMF always has a similar power-law tail toward higher masses.

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36

Nam, Donghee G., Christoph Federrath, and Mark R. Krumholz. "Testing the turbulent origin of the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 503, no. 1 (February 26, 2021): 1138–48. http://dx.doi.org/10.1093/mnras/stab505.

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ABSTRACT Supersonic turbulence in the interstellar medium (ISM) is closely linked to the formation of stars; hence, many theories connect the stellar initial mass function (IMF) with the turbulent properties of molecular clouds. Here, we test three turbulence-based IMF models (by Padoan and Nordlund, Hennebelle and Chabrier, and Hopkins) that predict the relation between the high-mass slope (Γ) of the IMF, dN/d log M ∝ MΓ, and the exponent n of the velocity power spectrum of turbulence, Ev(k) ∝ k−n, where n ≈ 2 corresponds to typical ISM turbulence. Using hydrodynamic simulations, we drive turbulence with an unusual index of n ≈ 1, measure Γ, and compare the results with n ≈ 2. We find that reducing n from 2 to 1 primarily changes the high-mass region of the IMF (beyond the median mass), where we measure high-mass slopes within the 95 per cent confidence interval of −1.5 < Γ < −1 for n ≈ 1 and −3.7 < Γ < −2.4 for n ≈ 2, respectively. Thus, we find that n = 1 results in a significantly flatter high-mass slope of the IMF, with more massive stars formed than for n ≈ 2. We compare these simulations with the predictions of the three IMF theories. We find that while the theory by Padoan and Nordlund matches our simulations with fair accuracy, the other theories either fail to reproduce the main qualitative outcome of the simulations or require some modifications. We conclude that turbulence plays a key role in shaping the IMF, with a shallower turbulence power spectrum producing a shallower high-mass IMF, and hence more massive stars.

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37

Kuperman, Ethan. "The Significance and Evolution of the Stellar Initial Mass Function." International Journal of High School Research 3, no. 5 (November 1, 2021): 11–15. http://dx.doi.org/10.36838/v3i5.3.

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38

Sung, Hwankyung, and Michael S. Bessell. "The Initial Mass Function and Stellar Content of NGC 3603." Astronomical Journal 127, no. 2 (February 2004): 1014–28. http://dx.doi.org/10.1086/381297.

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39

Chary, Ranga‐Ram. "The Stellar Initial Mass Function at the Epoch of Reionization." Astrophysical Journal 680, no. 1 (June 10, 2008): 32–40. http://dx.doi.org/10.1086/587737.

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40

Yoshii, Y., and H. Saio. "A fragmentation-coalescence model for the initial stellar mass function." Astrophysical Journal 295 (August 1985): 521. http://dx.doi.org/10.1086/163396.

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41

Riaz, R., D. R. G. Schleicher, S. Vanaverbeke, and R. S. Klessen. "Do fragmentation and accretion affect the stellar initial mass function?" Monthly Notices of the Royal Astronomical Society 494, no. 2 (March 20, 2020): 1647–57. http://dx.doi.org/10.1093/mnras/staa787.

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ABSTRACT While the stellar initial mass function (IMF) appears to be close to universal within the Milky Way galaxy, it is strongly suspected to be different in the primordial universe, where molecular hydrogen cooling is less efficient and the gas temperature can be higher by a factor of 30. In between these extreme cases, the gas temperature varies depending on the environment, metallicity, and radiation background. In this paper we explore if changes of the gas temperature affect the IMF of the stars considering fragmentation and accretion. The fragmentation behaviour depends mostly on the Jeans mass at the turning point in the equation of state (EOS) where a transition occurs from an approximately isothermal to an adiabatic regime due to dust opacities. The Jeans mass at this transition in the EOS is always very similar, independent of the initial temperature, and therefore the initial mass of the fragments is very similar. Accretion on the other hand is strongly temperature dependent. We argue that the latter becomes the dominant process for star formation efficiencies above 5–7 per cent, increasing the average mass of the stars.

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42

van Dokkum, Pieter G. "Evidence of Cosmic Evolution of the Stellar Initial Mass Function." Astrophysical Journal 674, no. 1 (February 10, 2008): 29–50. http://dx.doi.org/10.1086/525014.

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43

Jermyn, Adam S., Charles L. Steinhardt, and Christopher A. Tout. "The cosmic microwave background and the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 480, no. 3 (August 6, 2018): 4265–72. http://dx.doi.org/10.1093/mnras/sty2123.

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44

Larson, R. B. "Thermal physics, cloud geometry and the stellar initial mass function." Monthly Notices of the Royal Astronomical Society 359, no. 1 (May 1, 2005): 211–22. http://dx.doi.org/10.1111/j.1365-2966.2005.08881.x.

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45

de Souza, R. S., E. E. O. Ishida, D. J. Whalen, J. L. Johnson, and A. Ferrara. "Probing the stellar initial mass function with high-z supernovae." Monthly Notices of the Royal Astronomical Society 442, no. 2 (June 16, 2014): 1640–55. http://dx.doi.org/10.1093/mnras/stu984.

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46

Mollá, Mercedes, Oscar Cavichia, Marta Gavilán, and Brad K. Gibson. "Galactic chemical evolution: stellar yields and the initial mass function." Monthly Notices of the Royal Astronomical Society 451, no. 4 (June 29, 2015): 3693–708. http://dx.doi.org/10.1093/mnras/stv1102.

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47

Cisewski-Kehe, Jessi, Grant Weller, and Chad Schafer. "A preferential attachment model for the stellar initial mass function." Electronic Journal of Statistics 13, no. 1 (2019): 1580–607. http://dx.doi.org/10.1214/19-ejs1556.

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Dib, Sami, and Shantanu Basu. "The emergence of the galactic stellar mass function from a non-universal IMF in clusters." Astronomy & Astrophysics 614 (June 2018): A43. http://dx.doi.org/10.1051/0004-6361/201732490.

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We investigate the dependence of a single-generation galactic mass function (SGMF) on variations in the initial stellar mass functions (IMF) of stellar clusters. We show that cluster-to-cluster variations of the IMF lead to a multi-component SGMF where each component in a given mass range can be described by a distinct power-law function. We also show that a dispersion of ≈0.3 M⊙ in the characteristic mass of the IMF, as observed for young Galactic clusters, leads to a low-mass slope of the SGMF that matches the observed Galactic stellar mass function even when the IMFs in the low-mass end of individual clusters are much steeper.

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Sneppen, Albert, Charles L. Steinhardt, Hagan Hensley, Adam S. Jermyn, Basel Mostafa, and John R. Weaver. "Implications of a Temperature-dependent Initial Mass Function. I. Photometric Template Fitting." Astrophysical Journal 931, no. 1 (May 1, 2022): 57. http://dx.doi.org/10.3847/1538-4357/ac695e.

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Abstract A universal stellar initial mass function (IMF) should not be expected from theoretical models of star formation, but little conclusive observational evidence for a variable IMF has been uncovered. In this paper, a parameterization of the IMF is introduced into photometric template fitting of the COSMOS2015 catalog. The resulting best-fit templates suggest systematic variations in the IMF, with most galaxies exhibiting top-heavier stellar populations than in the Milky Way. At fixed redshift, only a small range of IMFs are found, with the typical IMF becoming progressively top-heavier with increasing redshift. Additionally, subpopulations of ULIRGs, quiescent and star-forming galaxies are compared with predictions of stellar population feedback and show clear qualitative similarities to the evolution of dust temperatures.

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McGee, Sean L., Ryosuke Goto, and Michael L. Balogh. "The stellar mass function and efficiency of galaxy formation with a varying initial mass function." Monthly Notices of the Royal Astronomical Society 438, no. 4 (January 22, 2014): 3188–204. http://dx.doi.org/10.1093/mnras/stt2426.

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