First results from the IllustrisTNG simulations: matter and galaxy clustering. Springel, V., Pakmor, R., Pillepich, A., Weinberger, R., Nelson, D., Hernquist, L., Vogelsberger, M., Genel, S., Torrey, P., Marinacci, F., & Naiman, J. ArXiv e-prints, 1707:arXiv:1707.03397, July, 2017. ![First results from the IllustrisTNG simulations: matter and galaxy clustering [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k \textasciitilde 10 h/Mpc by 20%. The non-linear two-point correlation function of the stellar mass is close to a power-law over a wide range of scales and approximately invariant in time from very high redshift to the present. The two-point correlation function of the simulated galaxies agrees well with SDSS at its mean redshift z \textasciitilde 0.1, both as a function of stellar mass and when split according to galaxy colour, apart from a mild excess in the clustering of red galaxies in the stellar mass range 10\textasciicircum9-10\textasciicircum10 Msun/h\textasciicircum2. Given this agreement, the TNG simulations can make valuable theoretical predictions for the clustering bias of different galaxy samples. We find that the clustering length of the galaxy auto-correlation function depends strongly on stellar mass and redshift. Its power-law slope gamma is nearly invariant with stellar mass, but declines from gamma \textasciitilde 1.8 at redshift z=0 to gamma \textasciitilde 1.6 at redshift z \textasciitilde 1, beyond which the slope steepens again. We detect significant scale-dependencies in the bias of different observational tracers of large-scale structure, extending well into the range of the baryonic acoustic oscillations and causing nominal (yet fortunately correctable) shifts of the acoustic peaks of around \textasciitilde5%.
@article{springel_first_2017,
title = {First results from the {IllustrisTNG} simulations: matter and galaxy clustering},
volume = {1707},
shorttitle = {First results from the {IllustrisTNG} simulations},
url = {http://adsabs.harvard.edu/abs/2017arXiv170703397S},
abstract = {Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an
exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k {\textasciitilde} 10 h/Mpc by 20\%. The non-linear two-point correlation function of the stellar mass is close to a power-law over a wide range of scales and approximately invariant in time from very high redshift to the present. The two-point
correlation function of the simulated galaxies agrees well with SDSS at its mean redshift z {\textasciitilde} 0.1, both as a function of stellar mass and when split according to galaxy colour, apart from a mild excess in the clustering of red galaxies in the stellar mass range 10{\textasciicircum}9-10{\textasciicircum}10
Msun/h{\textasciicircum}2. Given this agreement, the TNG simulations can make valuable theoretical predictions for the clustering bias of different galaxy samples. We find that the clustering length of the galaxy
auto-correlation function depends strongly on stellar mass and redshift. Its power-law slope gamma is nearly invariant with stellar mass, but declines from gamma {\textasciitilde} 1.8 at redshift z=0 to gamma {\textasciitilde} 1.6 at redshift z {\textasciitilde} 1, beyond which the slope steepens again. We detect significant
scale-dependencies in the bias of different observational tracers of large-scale structure, extending well into the range of the baryonic acoustic oscillations and causing nominal (yet fortunately correctable) shifts of the acoustic peaks of around {\textasciitilde}5\%.},
journal = {ArXiv e-prints},
author = {Springel, Volker and Pakmor, Rüdiger and Pillepich, Annalisa and Weinberger, Rainer and Nelson, Dylan and Hernquist, Lars and Vogelsberger, Mark and Genel, Shy and Torrey, Paul and Marinacci, Federico and Naiman, Jill},
month = jul,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:1707.03397},
}
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Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an exceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k \\textasciitilde 10 h/Mpc by 20%. The non-linear two-point correlation function of the stellar mass is close to a power-law over a wide range of scales and approximately invariant in time from very high redshift to the present. The two-point correlation function of the simulated galaxies agrees well with SDSS at its mean redshift z \\textasciitilde 0.1, both as a function of stellar mass and when split according to galaxy colour, apart from a mild excess in the clustering of red galaxies in the stellar mass range 10\\textasciicircum9-10\\textasciicircum10 Msun/h\\textasciicircum2. Given this agreement, the TNG simulations can make valuable theoretical predictions for the clustering bias of different galaxy samples. We find that the clustering length of the galaxy auto-correlation function depends strongly on stellar mass and redshift. Its power-law slope gamma is nearly invariant with stellar mass, but declines from gamma \\textasciitilde 1.8 at redshift z=0 to gamma \\textasciitilde 1.6 at redshift z \\textasciitilde 1, beyond which the slope steepens again. We detect significant scale-dependencies in the bias of different observational tracers of large-scale structure, extending well into the range of the baryonic acoustic oscillations and causing nominal (yet fortunately correctable) shifts of the acoustic peaks of around \\textasciitilde5%.","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Springel"],"firstnames":["Volker"],"suffixes":[]},{"propositions":[],"lastnames":["Pakmor"],"firstnames":["Rüdiger"],"suffixes":[]},{"propositions":[],"lastnames":["Pillepich"],"firstnames":["Annalisa"],"suffixes":[]},{"propositions":[],"lastnames":["Weinberger"],"firstnames":["Rainer"],"suffixes":[]},{"propositions":[],"lastnames":["Nelson"],"firstnames":["Dylan"],"suffixes":[]},{"propositions":[],"lastnames":["Hernquist"],"firstnames":["Lars"],"suffixes":[]},{"propositions":[],"lastnames":["Vogelsberger"],"firstnames":["Mark"],"suffixes":[]},{"propositions":[],"lastnames":["Genel"],"firstnames":["Shy"],"suffixes":[]},{"propositions":[],"lastnames":["Torrey"],"firstnames":["Paul"],"suffixes":[]},{"propositions":[],"lastnames":["Marinacci"],"firstnames":["Federico"],"suffixes":[]},{"propositions":[],"lastnames":["Naiman"],"firstnames":["Jill"],"suffixes":[]}],"month":"July","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","pages":"arXiv:1707.03397","bibtex":"@article{springel_first_2017,\n\ttitle = {First results from the {IllustrisTNG} simulations: matter and galaxy clustering},\n\tvolume = {1707},\n\tshorttitle = {First results from the {IllustrisTNG} simulations},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv170703397S},\n\tabstract = {Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG simulations to study the non-linear correlation functions and power spectra of baryons, dark matter, galaxies and haloes over an\nexceptionally large range of scales. We find that baryonic effects increase the clustering of dark matter on small scales and damp the total matter power spectrum on scales up to k {\\textasciitilde} 10 h/Mpc by 20\\%. The non-linear two-point correlation function of the stellar mass is close to a power-law over a wide range of scales and approximately invariant in time from very high redshift to the present. The two-point\ncorrelation function of the simulated galaxies agrees well with SDSS at its mean redshift z {\\textasciitilde} 0.1, both as a function of stellar mass and when split according to galaxy colour, apart from a mild excess in the clustering of red galaxies in the stellar mass range 10{\\textasciicircum}9-10{\\textasciicircum}10\nMsun/h{\\textasciicircum}2. Given this agreement, the TNG simulations can make valuable theoretical predictions for the clustering bias of different galaxy samples. We find that the clustering length of the galaxy\nauto-correlation function depends strongly on stellar mass and redshift. Its power-law slope gamma is nearly invariant with stellar mass, but declines from gamma {\\textasciitilde} 1.8 at redshift z=0 to gamma {\\textasciitilde} 1.6 at redshift z {\\textasciitilde} 1, beyond which the slope steepens again. 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