SLUG – stochastically lighting up galaxies – III. A suite of tools for simulated photometry, spectroscopy, and Bayesian inference with stochastic stellar populations

Krumholz, Mark R.; Fumagalli, Michele; Silva, Robert L. da; Rendahl, Theodore; Parra, Jonathan

doi:10.1093/mnras/stv1374

Cited by 142 publications

(159 citation statements)

References 90 publications

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“…For a given cluster mass, the clustered_SNe code uses the SLUG code (da Silva et al 2012;da Silva et al 2014;Krumholz et al 2015) to directly sample a Kroupa (2002) IMF of stars, and then explodes any stars with an initial mass greater than 8M after a mass-dependent lifetime predicted by the Geneva stellar evolution models (Ekström et al 2012). Explosion mass and metal yields follow the results of Woosley & Heger (2007), while each explosion is assumed to yield a constant E blast = 10 51 erg of energy (unless otherwise specified by a feedback model).…”

Section: Methodsmentioning

confidence: 99%

Momentum injection by clustered supernovae: testing subgrid feedback prescriptions

Gentry

Madau

Krumholz

2019

Monthly Notices of the Royal Astronomical Society

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Using a 1D Lagrangian code specifically designed to assess the impact of multiple, time-resolved supernovae (SNe) from a single star cluster on the surrounding medium, we test three commonly used feedback recipes: delayed cooling (e.g., used in the GASOLINE-2 code), momentum-energy injection (a resolution-dependent transition between momentum-dominated feedback and energy-dominated feedback used, e.g., in the FIRE-2 code), and simultaneous energy injection (e.g., used in the EAGLE simulations). Our work provides an intermediary test for these recipes: we analyse a setting that is more complex than the simplified scenarios for which many were designed, but one more controlled than a full galactic simulation. In particular, we test how well these models reproduce the enhanced momentum efficiency seen for an 11 SN cluster simulated at high resolution (0.6 pc; a factor of 12 enhancement relative to the isolated SN case) when these subgrid recipes are implemented in low resolution (20 pc) runs. We find that: 1) the delayed cooling model performs well -resulting in 9 times the momentum efficiency of the fiducial isolated SN value -when SNe are clustered and 10 51 erg are injected per SN, while clearly over-predicting the momentum efficiency in the single SN test case; 2) the momentum-energy model always achieves good results, with a factor of 5 boost in momentum efficiency; and 3) injecting the energy from all SNe simultaneously does little to prevent over-cooling and greatly under-produces the momentum deposited by clustered SNe, resulting in a factor of 3 decrease in momentum efficiency on the average.

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Section: Methodsmentioning

confidence: 99%

Momentum injection by clustered supernovae: testing subgrid feedback prescriptions

Gentry

Madau

Krumholz

2019

Monthly Notices of the Royal Astronomical Society

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“…Assuming typical initial conditions for molecular clouds, with temperatures of theorder of 10 K, gas is expected to fragment into sub-solar-mass cores, preventing gaseous material from accreting onto single high-mass stars (Krumholz et al 2015). Even after high-mass stars successfully form, further fragmentation could halt the growth of these stars and limit their final mass (Peters et al 2010b;Girichidis et al 2012).…”

Section: Fragmentation: Jeans Analysismentioning

confidence: 99%

Thermal Feedback in the High-mass Star- and Cluster-forming Region W51

Ginsburg

Goddi

Kruijssen

et al. 2017

ApJ

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Thermal Feedback in the High-mass Star-and Cluster-forming Region W51http://researchonline.ljmu.ac.uk/7346/ Article LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain.The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. LJMU Research OnlineThermal Feedback in the High-mass Star-and Cluster-forming Region W51 Abstract High-mass stars have generally been assumed to accrete most of their mass while already contracted onto the main sequence, but this hypothesis has not been observationally tested. We present ALMA observations of a3 1.5 pc area in the W51 high-mass star-forming complex. We identify dust continuum sources and measure the gas and dust temperature through both rotational diagram modeling of CHO H 3 and brightness-temperature-based limits. The observed region contains three high-mass YSOs that appear to be at the earliest stages of their formation, with no signs of ionizing radiation from their central sources. The data reveal high gas and dust temperatures ( > T 100 K) extending out to about 5000 au from each of these sources. There are no clear signs of disks or rotating structures down to our 1000 au resolution. The extended warm gas provides evidence that, during the process of forming, these high-mass stars heat a large volume and correspondingly large mass of gas in their surroundings, inhibiting fragmentation and therefore keeping a large reservoir available to feed from. By contrast, the more mature massive stars that illuminate compact H II regions have little effect on their surrounding dense gas, suggesting that these main-sequence stars have completed most or all of their accretion. The high luminosity of the massive protostars ( > L 10 4  L ), combined with a lack of centimeter continuum emission from these sources, implies that they are not on the main sequence while they accrete the majority of their mass; instead, they may be bloated and cool.

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“…When these stars disappear, the curve drops to a floor value produced by the less massive stars with M < 30 M (see e.g. da Silva et al 2014;Krumholz et al 2015, for a detailed analysis of the effect of stochastic stellar populations on estimated SFRs).…”

Section: Energy Inputmentioning

confidence: 99%

The SILCC project – IV. Impact of dissociating and ionizing radiation on the interstellar medium and Hα emission as a tracer of the star formation rate

Peters

Naab

Walch

et al. 2016

Mon. Not. R. Astron. Soc.

108

117

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We present three-dimensional radiation-hydrodynamical simulations of the impact of stellar winds, photoelectric heating, photodissociating and photoionising radiation, and supernovae on the chemical composition and star formation in a stratified disc model. This is followed with a sink-based model for star clusters with populations of individual massive stars. Stellar winds and ionising radiation regulate the star formation rate at a factor of ∼ 10 below the simulation with only supernova feedback due to their immediate impact on the ambient interstellar medium after star formation. Ionising radiation (with winds and supernovae) significantly reduces the ambient densities for most supernova explosions to ρ < 10 −25 g cm −3 , compared to 10 −23 g cmfor the model with only winds and supernovae. Radiation from massive stars reduces the amount of molecular hydrogen and increases the neutral hydrogen mass and volume filling fraction. Only this model results in a molecular gas depletion time scale of 2 Gyr and shows the best agreement with observations. In the radiative models, the Hα emission is dominated by radiative recombination as opposed to collisional excitation (the dominant emission in non-radiative models), which only contributes ∼ 1-10 % to the total Hα emission. Individual massive stars (M 30 M ) with short lifetimes are responsible for significant fluctuations in the Hα luminosities. The corresponding inferred star formation rates can underestimate the true instantaneous star formation rate by factors of ∼ 10.

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SLUG – stochastically lighting up galaxies – III. A suite of tools for simulated photometry, spectroscopy, and Bayesian inference with stochastic stellar populations

Cited by 142 publications

References 90 publications

Momentum injection by clustered supernovae: testing subgrid feedback prescriptions

Momentum injection by clustered supernovae: testing subgrid feedback prescriptions

Thermal Feedback in the High-mass Star- and Cluster-forming Region W51

The SILCC project – IV. Impact of dissociating and ionizing radiation on the interstellar medium and Hα emission as a tracer of the star formation rate

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