The connection between mass, environment and slow rotation in simulated galaxies. Lagos, C. d. P., Schaye, J., Bahe, Y., van de Sande, J., Kay, S., Barnes, D., Davis, T., & Dalla Vecchia, C. ArXiv e-prints, 1712:arXiv:1712.01398, December, 2017. ![The connection between mass, environment and slow rotation in simulated galaxies [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Recent observational results from integral field spectroscopic (IFS) surveys indicate that the fraction of galaxies that are slow rotators, \$F_\{{\textbackslash}rm SR\}\$, depends primarily on stellar mass, with no significant dependence on environment. We investigate these trends and the formation paths of slow rotators using the EAGLE and Hydrangea hydro-dynamical simulation suites. EAGLE consists of several cosmological boxes of volumes up to \$(100{\textbackslash},{\textbackslash}rm Mpc){\textasciicircum}3\$, while Hydrangea consists of \$24\$ cosmological zoom-in simulations of galaxy clusters and their large scale environment. Together they provide a statistically significant sample in the stellar mass range of interest, \$10{\textasciicircum}\{9.5\}{\textbackslash},{\textbackslash}rm M_\{{\textbackslash}odot\}-10{\textasciicircum}\{12\}{\textbackslash},{\textbackslash}rm M_\{{\textbackslash}odot\}\$, of \$16,431\$ galaxies. We construct IFS-like cubes and measure stellar spin parameters, \${\textbackslash}lambda_\{{\textbackslash}rm R\}\$, and ellipticities, allowing us to classify galaxies into slow and fast rotators as in observations. The simulated galaxies display a primary dependence of \$F_\{{\textbackslash}rm SR\}\$ on stellar mass, with a weak dependence on environment. At fixed stellar mass, satellite galaxies are more likely to be slow rotators than centrals. In addition, \$F_\{{\textbackslash}rm SR\}\$ shows a dependence on halo mass at fixed stellar mass for central galaxies, while no such trend is seen for satellites. We find that \${\textbackslash}approx 70\$% of slow rotators at \$z=0\$ have experienced at least one merger with mass ratio \${\textbackslash}ge 0.1\$, with dry major mergers being at least twice more common than minor and wet major mergers in this population. Individual dry mergers tend to decrease \${\textbackslash}lambda_\{{\textbackslash}rm R\}\$, while wet mergers mostly increase it. However, \$30\$% of slow rotators at \$z=0\$ have not experienced mergers, and those inhabit halos with median spins twice smaller than the halos hosting the rest of the slow rotators. Thus, although the formation paths of slow rotators can be varied, dry major mergers and/or halos with small spins dominate.
@article{lagos_connection_2017,
title = {The connection between mass, environment and slow rotation in simulated galaxies},
volume = {1712},
url = {http://adsabs.harvard.edu/abs/2017arXiv171201398L},
abstract = {Recent observational results from integral field spectroscopic (IFS)
surveys indicate that the fraction of galaxies that are slow rotators,
\$F\_\{{\textbackslash}rm SR\}\$, depends primarily on stellar mass, with no significant
dependence on environment. We investigate these trends and the formation
paths of slow rotators using the EAGLE and Hydrangea hydro-dynamical
simulation suites. EAGLE consists of several cosmological boxes of
volumes up to \$(100{\textbackslash},{\textbackslash}rm Mpc){\textasciicircum}3\$, while Hydrangea consists of \$24\$
cosmological zoom-in simulations of galaxy clusters and their large
scale environment. Together they provide a statistically significant
sample in the stellar mass range of interest, \$10{\textasciicircum}\{9.5\}{\textbackslash},{\textbackslash}rm
M\_\{{\textbackslash}odot\}-10{\textasciicircum}\{12\}{\textbackslash},{\textbackslash}rm M\_\{{\textbackslash}odot\}\$, of \$16,431\$ galaxies. We construct
IFS-like cubes and measure stellar spin parameters, \${\textbackslash}lambda\_\{{\textbackslash}rm R\}\$,
and ellipticities, allowing us to classify galaxies into slow and fast
rotators as in observations. The simulated galaxies display a primary
dependence of \$F\_\{{\textbackslash}rm SR\}\$ on stellar mass, with a weak dependence on
environment. At fixed stellar mass, satellite galaxies are more likely
to be slow rotators than centrals. In addition, \$F\_\{{\textbackslash}rm SR\}\$ shows a
dependence on halo mass at fixed stellar mass for central galaxies,
while no such trend is seen for satellites. We find that \${\textbackslash}approx 70\$\%
of slow rotators at \$z=0\$ have experienced at least one merger with mass
ratio \${\textbackslash}ge 0.1\$, with dry major mergers being at least twice more common
than minor and wet major mergers in this population. Individual dry
mergers tend to decrease \${\textbackslash}lambda\_\{{\textbackslash}rm R\}\$, while wet mergers mostly
increase it. However, \$30\$\% of slow rotators at \$z=0\$ have not
experienced mergers, and those inhabit halos with median spins twice
smaller than the halos hosting the rest of the slow rotators. Thus,
although the formation paths of slow rotators can be varied, dry major
mergers and/or halos with small spins dominate.},
urldate = {2017-12-11},
journal = {ArXiv e-prints},
author = {Lagos, Claudia del P. and Schaye, Joop and Bahe, Yannick and van de Sande, Jesse and Kay, Scott and Barnes, David and Davis, Timothy and Dalla Vecchia, Claudio},
month = dec,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:1712.01398},
}
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EAGLE consists of several cosmological boxes of volumes up to \\$(100{\\textbackslash},{\\textbackslash}rm Mpc){\\textasciicircum}3\\$, while Hydrangea consists of \\$24\\$ cosmological zoom-in simulations of galaxy clusters and their large scale environment. Together they provide a statistically significant sample in the stellar mass range of interest, \\$10{\\textasciicircum}\\{9.5\\}{\\textbackslash},{\\textbackslash}rm M_\\{{\\textbackslash}odot\\}-10{\\textasciicircum}\\{12\\}{\\textbackslash},{\\textbackslash}rm M_\\{{\\textbackslash}odot\\}\\$, of \\$16,431\\$ galaxies. We construct IFS-like cubes and measure stellar spin parameters, \\${\\textbackslash}lambda_\\{{\\textbackslash}rm R\\}\\$, and ellipticities, allowing us to classify galaxies into slow and fast rotators as in observations. The simulated galaxies display a primary dependence of \\$F_\\{{\\textbackslash}rm SR\\}\\$ on stellar mass, with a weak dependence on environment. At fixed stellar mass, satellite galaxies are more likely to be slow rotators than centrals. In addition, \\$F_\\{{\\textbackslash}rm SR\\}\\$ shows a dependence on halo mass at fixed stellar mass for central galaxies, while no such trend is seen for satellites. We find that \\${\\textbackslash}approx 70\\$% of slow rotators at \\$z=0\\$ have experienced at least one merger with mass ratio \\${\\textbackslash}ge 0.1\\$, with dry major mergers being at least twice more common than minor and wet major mergers in this population. Individual dry mergers tend to decrease \\${\\textbackslash}lambda_\\{{\\textbackslash}rm R\\}\\$, while wet mergers mostly increase it. However, \\$30\\$% of slow rotators at \\$z=0\\$ have not experienced mergers, and those inhabit halos with median spins twice smaller than the halos hosting the rest of the slow rotators. Thus, although the formation paths of slow rotators can be varied, dry major mergers and/or halos with small spins dominate.","urldate":"2017-12-11","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Lagos"],"firstnames":["Claudia","del","P."],"suffixes":[]},{"propositions":[],"lastnames":["Schaye"],"firstnames":["Joop"],"suffixes":[]},{"propositions":[],"lastnames":["Bahe"],"firstnames":["Yannick"],"suffixes":[]},{"propositions":["van","de"],"lastnames":["Sande"],"firstnames":["Jesse"],"suffixes":[]},{"propositions":[],"lastnames":["Kay"],"firstnames":["Scott"],"suffixes":[]},{"propositions":[],"lastnames":["Barnes"],"firstnames":["David"],"suffixes":[]},{"propositions":[],"lastnames":["Davis"],"firstnames":["Timothy"],"suffixes":[]},{"propositions":[],"lastnames":["Dalla","Vecchia"],"firstnames":["Claudio"],"suffixes":[]}],"month":"December","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1712.01398","bibtex":"@article{lagos_connection_2017,\n\ttitle = {The connection between mass, environment and slow rotation in simulated galaxies},\n\tvolume = {1712},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171201398L},\n\tabstract = {Recent observational results from integral field spectroscopic (IFS) \nsurveys indicate that the fraction of galaxies that are slow rotators,\n\\$F\\_\\{{\\textbackslash}rm SR\\}\\$, depends primarily on stellar mass, with no significant\ndependence on environment. We investigate these trends and the formation\npaths of slow rotators using the EAGLE and Hydrangea hydro-dynamical\nsimulation suites. EAGLE consists of several cosmological boxes of\nvolumes up to \\$(100{\\textbackslash},{\\textbackslash}rm Mpc){\\textasciicircum}3\\$, while Hydrangea consists of \\$24\\$\ncosmological zoom-in simulations of galaxy clusters and their large\nscale environment. Together they provide a statistically significant\nsample in the stellar mass range of interest, \\$10{\\textasciicircum}\\{9.5\\}{\\textbackslash},{\\textbackslash}rm\nM\\_\\{{\\textbackslash}odot\\}-10{\\textasciicircum}\\{12\\}{\\textbackslash},{\\textbackslash}rm M\\_\\{{\\textbackslash}odot\\}\\$, of \\$16,431\\$ galaxies. We construct\nIFS-like cubes and measure stellar spin parameters, \\${\\textbackslash}lambda\\_\\{{\\textbackslash}rm R\\}\\$,\nand ellipticities, allowing us to classify galaxies into slow and fast\nrotators as in observations. The simulated galaxies display a primary\ndependence of \\$F\\_\\{{\\textbackslash}rm SR\\}\\$ on stellar mass, with a weak dependence on\nenvironment. At fixed stellar mass, satellite galaxies are more likely\nto be slow rotators than centrals. In addition, \\$F\\_\\{{\\textbackslash}rm SR\\}\\$ shows a\ndependence on halo mass at fixed stellar mass for central galaxies,\nwhile no such trend is seen for satellites. We find that \\${\\textbackslash}approx 70\\$\\%\nof slow rotators at \\$z=0\\$ have experienced at least one merger with mass\nratio \\${\\textbackslash}ge 0.1\\$, with dry major mergers being at least twice more common\nthan minor and wet major mergers in this population. Individual dry\nmergers tend to decrease \\${\\textbackslash}lambda\\_\\{{\\textbackslash}rm R\\}\\$, while wet mergers mostly\nincrease it. However, \\$30\\$\\% of slow rotators at \\$z=0\\$ have not\nexperienced mergers, and those inhabit halos with median spins twice\nsmaller than the halos hosting the rest of the slow rotators. Thus,\nalthough the formation paths of slow rotators can be varied, dry major\nmergers and/or halos with small spins dominate.},\n\turldate = {2017-12-11},\n\tjournal = {ArXiv e-prints},\n\tauthor = {Lagos, Claudia del P. and Schaye, Joop and Bahe, Yannick and van de Sande, Jesse and Kay, Scott and Barnes, David and Davis, Timothy and Dalla Vecchia, Claudio},\n\tmonth = dec,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:1712.01398},\n}\n\n","author_short":["Lagos, C. d. 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