The galaxy-wide initial mass function of dwarf late-type to massive early-type galaxies

Weidner, C.; Kroupa, Pavel; Pflamm-Altenburg, Jan; Vazdekis, Alexandre

doi:10.1093/mnras/stt1806

Cited by 95 publications

(111 citation statements)

References 108 publications

(152 reference statements)

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“…There are theoretical reasons to expect that the fates of massive stars could be determined in part by metallicity (e.g., Langer 2012;Smith 2014;Yoon 2015) or SFR conditions (e.g., because galaxies with high sSFRs may have altered IMFs or because they may possess dense clusters with a high number of dynamical interactions; Habergham et al 2010;Gunawardhana et al 2011;Sana et al 2012;Geha et al 2013;Weidner et al 2013;Pastorello et al 2014), but it is not clear how the total mass of the galaxy would impact the death of one or two massive local stars. On their own, though, our data do not allow us to either prove or disprove these claims.…”

Section: Correlation Vs Causationmentioning

confidence: 99%

LOSS Revisited. I. Unraveling Correlations between Supernova Rates and Galaxy Properties, as Measured in a Reanalysis of the Lick Observatory Supernova Search

Graur

Bianco

Huang

et al. 2017

ApJ

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Most types of supernovae (SNe) have yet to be connected with their progenitor stellar systems. Here, we reanalyze the 10-year SN sample collected during 1998-2008 by the Lick Observatory Supernova Search (LOSS) in order to constrain the progenitors of SNe Ia and stripped-envelope SNe (SE SNe, i.e., SNe IIb, Ib, Ic, and broad-lined Ic). We matched the LOSS galaxy sample with spectroscopy from the Sloan Digital Sky Survey and measured SN rates as a function of galaxy stellar mass, specific star formation rate, and oxygen abundance (metallicity). We find significant correlations between the SN rates and all three galaxy properties. The SN Ia correlations are consistent with other measurements, as well as with our previous explanation of these measurements in the form of a combination of the SN Ia delay-time distribution and the correlation between galaxy mass and age. The ratio between the SE SN and SN II rates declines significantly in low-mass galaxies. This rules out single stars as SE SN progenitors, and is consistent with predictions from binary-system progenitor models. Using well-known galaxy scaling relations, any correlation between the rates and one of the galaxy properties examined here can be expressed as a correlation with the other two. These redundant correlations preclude us from establishing causality-that is, from ascertaining which of the galaxy properties (or their combination) is the physical driver for the difference between the SE SN and SN II rates. We outline several methods that have the potential to overcome this problem in future works.

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Section: Correlation Vs Causationmentioning

confidence: 99%

LOSS Revisited. I. Unraveling Correlations between Supernova Rates and Galaxy Properties, as Measured in a Reanalysis of the Lick Observatory Supernova Search

Graur

Bianco

Huang

et al. 2017

ApJ

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“…The existence of a physical m max -M ecl relation is thus taken to be established (Weidner et al 2014). Although the theory has been successful in describing the stellar contents of whole galaxies (e.g., Weidner et al 2013b), it has been debated if the relation exists (see Section 2.1 in Weidner et al 2013a for details) or if star formation is a purely stochastic process (e.g., Krumholz 2015). This is a fundamental issue for understanding galaxy-wide IMFs and how massive stars form, and we here thus stress that the data do not support the hypothesis that star formation is stochastic (see Section 7 of Kroupa 2015).…”

Section: The Binary Fraction Among the Ejected O Star Systemsmentioning

confidence: 99%

Dependency of Dynamical Ejections of O Stars on the Masses of Very Young Star Clusters

Kroupa

Pflamm-Altenburg

2015

ApJ

106

149

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Massive stars can be efficiently ejected from their birth star clusters through encounters with other massive stars. We study how the dynamical ejection fraction of O star systems varies with the masses of very young star clusters, M ecl , by means of direct N-body calculations. We include diverse initial conditions by varying the half-mass radius, initial mass segregation, initial binary fraction, and orbital parameters of the massive binaries. The results show robustly that the ejection fraction of O star systems exhibits a maximum at a cluster mass offor all models, even though the number of ejected systems increases with cluster mass. We show that lower mass clusters) are the dominant sources for populating the Galactic field with O stars by dynamical ejections, considering the mass function of embedded clusters. About 15% (up to ≈38%, depending on the cluster models) of O stars of which a significant fraction are binaries, and which would have formed in a ≈10 Myr epoch of star formation in a distribution of embedded clusters, will be dynamically ejected to the field. Individual clusters may eject 100% of their original O star content. A large fraction of such O stars have velocities up to only 10 km s −1 . Synthesising a young star cluster mass function, it follows, given the stellar-dynamical results presented here, that the observed fractions of field and runaway O stars, and the binary fractions among them, can be well understood theoretically if all O stars form in embedded clusters.

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“…The IMF of a whole object would thus be less top-heavy (e.g. Pflamm-Altenburg et al 2009;Weidner et al 2013;Fontanot et al 2017;Yan et al 2017), leading to smaller M/L V ratios at older ages (Figs. 4 and 5).…”

Section: Where To Lookmentioning

confidence: 99%

The formation of ultra compact dwarf galaxies and massive globular clusters

Jeřabková

Kroupa

Dabringhausen

et al. 2017

A&A

Self Cite

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The stellar initial mass function (IMF) has been described as being invariant, bottom-heavy, or top-heavy in extremely dense starburst conditions. To provide usable observable diagnostics, we calculate redshift dependent spectral energy distributions of stellar populations in extreme star-burst clusters, which are likely to have been the precursors of present day massive globular clusters (GCs) and of ultra compact dwarf galaxies (UCDs). The retention fraction of stellar remnants is taken into account to assess the mass to light ratios of the ageing star-burst. Their redshift dependent photometric properties are calculated as predictions for James Webb Space Telescope (JWST) observations. While the present day GCs and UCDs are largely degenerate concerning bottom-heavy or top-heavy IMFs, a metallicity-and density-dependent top-heavy IMF implies the most massive UCDs, at ages <100 Myr, to appear as objects with quasar-like luminosities with a 0.1-10% variability on a monthly timescale due to core collapse supernovae.

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The galaxy-wide initial mass function of dwarf late-type to massive early-type galaxies

Cited by 95 publications

References 108 publications

LOSS Revisited. I. Unraveling Correlations between Supernova Rates and Galaxy Properties, as Measured in a Reanalysis of the Lick Observatory Supernova Search

LOSS Revisited. I. Unraveling Correlations between Supernova Rates and Galaxy Properties, as Measured in a Reanalysis of the Lick Observatory Supernova Search

Dependency of Dynamical Ejections of O Stars on the Masses of Very Young Star Clusters

The formation of ultra compact dwarf galaxies and massive globular clusters

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