The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

Kim, Ji-hoon; Agertz, Oscar; Teyssier, Romain; Butler, Michael J.; Ceverino, Daniel; Choi, June-Seek; Feldmann, Robert; Keller, Ben; Lupi, Alessandro; Quinn, Thomas; Revaz, Yves; Wallace, Stephen S.; Gnedin, Nickolay Y.; Leitner, Samuel N.; Shen, Sijing; Smith, Britton D.; Thompson, Raymond H.; Turk, Matthew J.; Abel, Tom; Arraki, Kenza S.; Benincasa, Samantha M.; Chakrabarti, Sukanya; DeGraf, Colin; Dekel, Avishai; Goldbaum, Nathan J.; Hopkins, Philip F.; Hummels, Cameron B.; Klypin, Anatoly; Li, Hui; Madau, Piero; Mandelker, Nir; Mayer, Lucio; Nagamine, Kentaro; Nickerson, Sarah; O’Shea, Brian W.; Primack, Joel R.; Roca-Fàbrega, S.; Semenov, Vadim A.; Shimizu, Ikkoh; Simpson, Christine M.; Todoroki, Keita; Wadsley, James; Wise, John H.

doi:10.3847/1538-4357/833/2/202

Cited by 124 publications

(146 citation statements)

References 99 publications

Supporting

Mentioning

142

Contrasting

Order By: Relevance

“…The initial conditions are those of the isolated disc galaxy in the AGORA project (Kim et al 2014(Kim et al , 2016, set up to approximate a Milky Way-like galaxy following the methods described in Hernquist (1993) and Springel (2000). Briefly, the dark matter halo has a concentration parameter c = 10 and virial circular velocity v 200 = 150 km s −1 .…”

Section: Numerical Setupmentioning

confidence: 99%

How runaway stars boost galactic outflows

Andersson

Agertz

2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Roughly ten per cent of OB stars are kicked out of their natal clusters before ending their life as supernovae. These so called runaway stars can travel hundreds of parsecs into the low-density interstellar medium, where momentum and energy from stellar feedback is efficiently deposited. In this work we explore how this mechanism affects large scale properties of the galaxy, such as outflows. To do so we use a new model which treats OB stars and their associated feedback processes on a star-by-star basis. With this model we compare two hydrodynamical simulations of Milky Way-like galaxies, one where we include runaways, and one where we ignore them. Including runaway stars leads to twice as many supernovae explosions in regions with gas densities ranging from 10 −5 cm −3 to 10 −3 cm −3 . This results in more efficient heating of the inter-arm regions, and drives strong galactic winds with mass loading factors boosted by up to one order of magnitude. These outflows produce a more massive and extended multi-phase circumgalactic medium, as well as a population of dense clouds in the halo. Conversely, since less energy and momentum is released in the dense star forming regions, the cold phase of the interstellar medium is less disturbed by feedback effects.

show abstract

Section: Numerical Setupmentioning

confidence: 99%

How runaway stars boost galactic outflows

Andersson

Agertz

2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…We adopt the initial conditions that were used in the AGORA code comparison project (Kim et al 2016) and also in the studies of Agertz et al (2013) and Semenov et al (2016). Specifically, the isolated disk is initialized inside a dark matter halo with v c,200 = 150 km s −1 and an initial concentration of c = 10.…”

Section: Introductionmentioning

confidence: 99%

The Physical Origin of Long Gas Depletion Times in Galaxies

Semenov

Kravtsov

Gnedin

2017

ApJ

Self Cite

124

106

View full text Add to dashboard Cite

We present a model that explains why galaxies form stars on a time scale significantly longer than the time scales of processes governing the evolution of interstellar gas. We show that gas evolves from a nonstar-forming to a star-forming state on a relatively short time scale and thus the rate of this evolution does not limit the star formation rate. Instead, the star formation rate is limited because only a small fraction of star-forming gas is converted into stars before star-forming regions are dispersed by feedback and dynamical processes. Thus, gas cycles into and out of star-forming state multiple times, which results in a long time scale on which galaxies convert gas into stars. Our model does not rely on the assumption of equilibrium and can be used to interpret trends of depletion times with the properties of observed galaxies and the parameters of star formation and feedback recipes in simulations. In particular, the model explains how feedback selfregulates the star formation rate in simulations and makes it insensitive to the local star formation efficiency. We illustrate our model using the results of an isolated L * -sized galaxy simulation that reproduces the observed Kennicutt-Schmidt relation for both molecular and atomic gas. Interestingly, the relation for molecular gas is almost linear on kiloparsec scales, although a nonlinear relation is adopted in simulation cells. We discuss how a linear relation emerges from non-self-similar scaling of the gas density PDF with the average gas surface density.

show abstract

“…We set the data set filename and load the data set into YT. The data set used is the publicly available 17 initial output of an ART-II run of an isolated galaxy used in an AGORA paper (Kim et al 2016), assumed to be at redshift of 0. We define the trajectory of our LightRay sightline to cross the full domain of our simulation, and additionally define which lines, ions, or atoms we wish to include in our spectrum.…”

Section: Demonstration: How To Run Tridentmentioning

confidence: 99%

“…As a reference benchmark, we ran TRIDENT on the AGORA idealized galaxy simulations (Kim et al 2016). We ran the script provided in Section 3 (without the ProjectionPlot step) on the initial outputs for each of the simulations codes supported in the AGORA study.…”

Section: Appendix a Parallelism And Performancementioning

confidence: 99%

See 1 more Smart Citation

Trident: A Universal Tool for Generating Synthetic Absorption Spectra from Astrophysical Simulations

Hummels

Smith

Silvia

2017

ApJ

Self Cite

View full text Add to dashboard Cite

Hydrodynamical simulations are increasingly able to accurately model physical systems on stellar, galactic, and cosmological scales; however, the utility of these simulations is often limited by our ability to directly compare them with the data sets produced by observers: spectra, photometry, etc. To address this problem, we have created TRIDENT, a Python-based open-source tool for post-processing hydrodynamical simulations to produce synthetic absorption spectra and related data. TRIDENT can (i) create absorption-line spectra for any trajectory through a simulated data set mimicking both background quasar and down-the-barrel configurations; (ii) reproduce the spectral characteristics of common instruments like the Cosmic Origins Spectrograph; (iii) operate across the ultraviolet, optical, and infrared using customizable absorption-line lists; (iv) trace simulated physical structures directly to spectral features; (v) approximate the presence of ion species absent from the simulation outputs; (vi) generate column density maps for any ion; and (vii) provide support for all major astrophysical hydrodynamical codes. TRIDENT was originally developed to aid in the interpretation of observations of the circumgalactic medium and intergalactic medium, but it remains a general tool applicable in other contexts.

show abstract

The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

Cited by 124 publications

References 99 publications

How runaway stars boost galactic outflows

How runaway stars boost galactic outflows

The Physical Origin of Long Gas Depletion Times in Galaxies

Trident: A Universal Tool for Generating Synthetic Absorption Spectra from Astrophysical Simulations

Contact Info

Product

Resources

About