The abundance, distribution, and physical nature of highly ionized oxygen OVI, OVII, and OVIII in IllustrisTNG. Nelson, D., Kauffmann, G., Pillepich, A., Genel, S., Springel, V., Pakmor, R., Hernquist, L., Weinberger, R., Torrey, P., Vogelsberger, M., & Marinacci, F. ArXiv e-prints, 1712:arXiv:1712.00016, November, 2017. ![The abundance, distribution, and physical nature of highly ionized oxygen OVI, OVII, and OVIII in IllustrisTNG [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We explore the abundance, spatial distribution, and physical properties of the OVI, OVII, and OVIII ions of oxygen in circumgalactic and intergalactic media (the CGM, IGM, and WHIM). We use the TNG100 and TNG300 large volume cosmological magneto-hydrodynamical simulations. Modeling the ionization states of simulated oxygen, we find good agreement with observations of the low-redshift OVI column density distribution function (CDDF), and present its evolution for all three ions from z=0 to z=4. Producing mock quasar absorption line spectral surveys, we show that the IllustrisTNG simulations are fully consistent with constraints on the OVI content of the CGM from COS-Halos and other low redshift observations, producing columns as high as observed. We measure the total amount of mass and average column densities of each ion using hundreds of thousands of simulated galaxies spanning 10\textasciicircum11 \textless Mhalo/Msun \textless 10\textasciicircum15 corresponding to 10\textasciicircum9 \textless M*/Msun \textless 10\textasciicircum12 in stellar mass. The stacked radial profiles of OVI around halos of different masses are computed in 3D number density as well as 2D projected column, decomposing into the 1-halo and 2-halo terms, the latter of which begins to dominate for Milky Way mass halos in the WHIM just beyond the virial radius. Relating halo OVI to properties of the central galaxy, we find a correlation between the (g-r) color of a galaxy and the total amount of OVI in its CGM. In comparison to the COS-Halos finding, this leads to a dichotomy of columns around star-forming versus passive galaxies at fixed stellar (or halo) mass. We demonstrate that this correlation is a direct result of blackhole feedback associated with quenching, which also produces additional trends with other galaxy properties, and represents a causal consequence of galactic-scale baryonic feedback impacting the physical state of the circumgalactic medium.
@article{nelson_abundance_2017,
title = {The abundance, distribution, and physical nature of highly ionized oxygen {OVI}, {OVII}, and {OVIII} in {IllustrisTNG}},
volume = {1712},
url = {http://adsabs.harvard.edu/abs/2017arXiv171200016N},
abstract = {We explore the abundance, spatial distribution, and physical properties
of the OVI, OVII, and OVIII ions of oxygen in circumgalactic and
intergalactic media (the CGM, IGM, and WHIM). We use the TNG100 and
TNG300 large volume cosmological magneto-hydrodynamical simulations.
Modeling the ionization states of simulated oxygen, we find good
agreement with observations of the low-redshift OVI column density
distribution function (CDDF), and present its evolution for all three
ions from z=0 to z=4. Producing mock quasar absorption line spectral
surveys, we show that the IllustrisTNG simulations are fully consistent
with constraints on the OVI content of the CGM from COS-Halos and other
low redshift observations, producing columns as high as observed. We
measure the total amount of mass and average column densities of each
ion using hundreds of thousands of simulated galaxies spanning 10{\textasciicircum}11
{\textless} Mhalo/Msun {\textless} 10{\textasciicircum}15 corresponding to 10{\textasciicircum}9 {\textless} M*/Msun {\textless} 10{\textasciicircum}12
in stellar mass. The stacked radial profiles of OVI around halos of
different masses are computed in 3D number density as well as 2D
projected column, decomposing into the 1-halo and 2-halo terms, the
latter of which begins to dominate for Milky Way mass halos in the WHIM
just beyond the virial radius. Relating halo OVI to properties of the
central galaxy, we find a correlation between the (g-r) color of a
galaxy and the total amount of OVI in its CGM. In comparison to the
COS-Halos finding, this leads to a dichotomy of columns around
star-forming versus passive galaxies at fixed stellar (or halo) mass. We
demonstrate that this correlation is a direct result of blackhole
feedback associated with quenching, which also produces additional
trends with other galaxy properties, and represents a causal consequence
of galactic-scale baryonic feedback impacting the physical state of the
circumgalactic medium.},
urldate = {2017-12-11},
journal = {ArXiv e-prints},
author = {Nelson, Dylan and Kauffmann, Guinevere and Pillepich, Annalisa and Genel, Shy and Springel, Volker and Pakmor, Ruediger and Hernquist, Lars and Weinberger, Rainer and Torrey, Paul and Vogelsberger, Mark and Marinacci, Federico},
month = nov,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:1712.00016},
}
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Modeling the ionization states of simulated oxygen, we find good agreement with observations of the low-redshift OVI column density distribution function (CDDF), and present its evolution for all three ions from z=0 to z=4. Producing mock quasar absorption line spectral surveys, we show that the IllustrisTNG simulations are fully consistent with constraints on the OVI content of the CGM from COS-Halos and other low redshift observations, producing columns as high as observed. We measure the total amount of mass and average column densities of each ion using hundreds of thousands of simulated galaxies spanning 10\\textasciicircum11 \\textless Mhalo/Msun \\textless 10\\textasciicircum15 corresponding to 10\\textasciicircum9 \\textless M*/Msun \\textless 10\\textasciicircum12 in stellar mass. The stacked radial profiles of OVI around halos of different masses are computed in 3D number density as well as 2D projected column, decomposing into the 1-halo and 2-halo terms, the latter of which begins to dominate for Milky Way mass halos in the WHIM just beyond the virial radius. Relating halo OVI to properties of the central galaxy, we find a correlation between the (g-r) color of a galaxy and the total amount of OVI in its CGM. In comparison to the COS-Halos finding, this leads to a dichotomy of columns around star-forming versus passive galaxies at fixed stellar (or halo) mass. We demonstrate that this correlation is a direct result of blackhole feedback associated with quenching, which also produces additional trends with other galaxy properties, and represents a causal consequence of galactic-scale baryonic feedback impacting the physical state of the circumgalactic medium.","urldate":"2017-12-11","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Nelson"],"firstnames":["Dylan"],"suffixes":[]},{"propositions":[],"lastnames":["Kauffmann"],"firstnames":["Guinevere"],"suffixes":[]},{"propositions":[],"lastnames":["Pillepich"],"firstnames":["Annalisa"],"suffixes":[]},{"propositions":[],"lastnames":["Genel"],"firstnames":["Shy"],"suffixes":[]},{"propositions":[],"lastnames":["Springel"],"firstnames":["Volker"],"suffixes":[]},{"propositions":[],"lastnames":["Pakmor"],"firstnames":["Ruediger"],"suffixes":[]},{"propositions":[],"lastnames":["Hernquist"],"firstnames":["Lars"],"suffixes":[]},{"propositions":[],"lastnames":["Weinberger"],"firstnames":["Rainer"],"suffixes":[]},{"propositions":[],"lastnames":["Torrey"],"firstnames":["Paul"],"suffixes":[]},{"propositions":[],"lastnames":["Vogelsberger"],"firstnames":["Mark"],"suffixes":[]},{"propositions":[],"lastnames":["Marinacci"],"firstnames":["Federico"],"suffixes":[]}],"month":"November","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","pages":"arXiv:1712.00016","bibtex":"@article{nelson_abundance_2017,\n\ttitle = {The abundance, distribution, and physical nature of highly ionized oxygen {OVI}, {OVII}, and {OVIII} in {IllustrisTNG}},\n\tvolume = {1712},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171200016N},\n\tabstract = {We explore the abundance, spatial distribution, and physical properties \nof the OVI, OVII, and OVIII ions of oxygen in circumgalactic and\nintergalactic media (the CGM, IGM, and WHIM). We use the TNG100 and\nTNG300 large volume cosmological magneto-hydrodynamical simulations.\nModeling the ionization states of simulated oxygen, we find good\nagreement with observations of the low-redshift OVI column density\ndistribution function (CDDF), and present its evolution for all three\nions from z=0 to z=4. Producing mock quasar absorption line spectral\nsurveys, we show that the IllustrisTNG simulations are fully consistent\nwith constraints on the OVI content of the CGM from COS-Halos and other\nlow redshift observations, producing columns as high as observed. We\nmeasure the total amount of mass and average column densities of each\nion using hundreds of thousands of simulated galaxies spanning 10{\\textasciicircum}11\n{\\textless} Mhalo/Msun {\\textless} 10{\\textasciicircum}15 corresponding to 10{\\textasciicircum}9 {\\textless} M*/Msun {\\textless} 10{\\textasciicircum}12\nin stellar mass. The stacked radial profiles of OVI around halos of\ndifferent masses are computed in 3D number density as well as 2D\nprojected column, decomposing into the 1-halo and 2-halo terms, the\nlatter of which begins to dominate for Milky Way mass halos in the WHIM\njust beyond the virial radius. Relating halo OVI to properties of the\ncentral galaxy, we find a correlation between the (g-r) color of a\ngalaxy and the total amount of OVI in its CGM. In comparison to the\nCOS-Halos finding, this leads to a dichotomy of columns around\nstar-forming versus passive galaxies at fixed stellar (or halo) mass. 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