The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics. Donnari, M., Pillepich, A., Nelson, D., Vogelsberger, M., Genel, S., Weinberger, R., Marinacci, F., Springel, V., & Hernquist, L. Monthly Notices of the Royal Astronomical Society, 485:4817–4840, June, 2019. ![The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We select galaxies from the IllustrisTNG hydrodynamical simulations (M_stars\textgreater 10\textasciicircum9 M_⊙ at 0 ≤ z ≤ 2) and characterize the shapes and evolutions of their UVJ and star formation rate-stellar mass (SFR-Mstars) diagrams. We quantify the systematic uncertainties related to different criteria to classify star-forming versus quiescent galaxies, different SFR estimates, and by accounting for the star formation measured within different physical apertures. The TNG model returns the observed features of the UVJ diagram at z ≤ 2, with a clear separation between two classes of galaxies. It also returns a tight star-forming main sequence (MS) for M_stars\textless 10\textasciicircum\10.5\ (M_⊙) with a ˜0.3 dex scatter at z ˜ 0 in our fiducial choices. If a UVJ-based cut is adopted, the TNG MS exhibits a downwardly bending at stellar masses of about 1010.5-10.7 M⊙. Moreover, the model predicts that \˜ \80 (50) per cent of 1010.5-11 M⊙ galaxies at z = 0 (z = 2) are quiescent and the numbers of quenched galaxies at intermediate redshifts and high masses are in better agreement with observational estimates than previous models. However, shorter SFR-averaging time-scales imply higher normalizations and scatter of the MS, while smaller apertures lead to underestimating the galaxy SFRs: overall we estimate the inspected systematic uncertainties to sum up to about 0.2-0.3 dex in the locus of the MS and to about 15 percentage points in the fraction of quenched galaxies. While TNG colour distributions are clearly bimodal, this is not the case for the SFR logarithmic distributions in bins of stellar mass (SFR ≳ 10-3 M⊙yr-1). Finally, the slope and z = 0 normalization of the TNG MS are consistent with observational findings; however, the locus of the TNG MS remains lower by about 0.2-0.5 dex at 0.75 ≤ z \textless 2 than the available observational estimates taken at face value.
@article{donnari_star_2019,
title = {The star formation activity of {IllustrisTNG} galaxies: main sequence, {UVJ} diagram, quenched fractions, and systematics},
volume = {485},
issn = {0035-8711},
shorttitle = {The star formation activity of {IllustrisTNG} galaxies},
url = {http://adsabs.harvard.edu/abs/2019MNRAS.485.4817D},
doi = {10.1093/mnras/stz712},
abstract = {We select galaxies from the IllustrisTNG hydrodynamical simulations
(M\_stars{\textgreater} 10{\textasciicircum}9 M\_⊙ at 0 ≤ z ≤ 2) and characterize the
shapes and evolutions of their UVJ and star formation rate-stellar mass
(SFR-Mstars) diagrams. We quantify the systematic
uncertainties related to different criteria to classify star-forming
versus quiescent galaxies, different SFR estimates, and by accounting
for the star formation measured within different physical apertures. The
TNG model returns the observed features of the UVJ diagram at z ≤ 2,
with a clear separation between two classes of galaxies. It also returns
a tight star-forming main sequence (MS) for M\_stars{\textless} 10{\textasciicircum}\{10.5\}
(M\_⊙) with a ˜0.3 dex scatter at z ˜ 0 in our fiducial
choices. If a UVJ-based cut is adopted, the TNG MS exhibits a downwardly
bending at stellar masses of about 1010.5-10.7
M⊙. Moreover, the model predicts that \{˜ \}80 (50)
per cent of 1010.5-11 M⊙ galaxies at z = 0 (z
= 2) are quiescent and the numbers of quenched galaxies at intermediate
redshifts and high masses are in better agreement with observational
estimates than previous models. However, shorter SFR-averaging
time-scales imply higher normalizations and scatter of the MS, while
smaller apertures lead to underestimating the galaxy SFRs: overall we
estimate the inspected systematic uncertainties to sum up to about
0.2-0.3 dex in the locus of the MS and to about 15 percentage points in
the fraction of quenched galaxies. While TNG colour distributions are
clearly bimodal, this is not the case for the SFR logarithmic
distributions in bins of stellar mass (SFR ≳ 10-3
M⊙yr-1). Finally, the slope and z = 0
normalization of the TNG MS are consistent with observational findings;
however, the locus of the TNG MS remains lower by about 0.2-0.5 dex at
0.75 ≤ z {\textless} 2 than the available observational estimates taken at
face value.},
urldate = {2019-04-15},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Donnari, Martina and Pillepich, Annalisa and Nelson, Dylan and Vogelsberger, Mark and Genel, Shy and Weinberger, Rainer and Marinacci, Federico and Springel, Volker and Hernquist, Lars},
month = jun,
year = {2019},
keywords = {cosmology: theory, galaxies: evolution, galaxies: formation, galaxies: star formation, methods: numerical},
pages = {4817--4840},
}
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We quantify the systematic uncertainties related to different criteria to classify star-forming versus quiescent galaxies, different SFR estimates, and by accounting for the star formation measured within different physical apertures. The TNG model returns the observed features of the UVJ diagram at z ≤ 2, with a clear separation between two classes of galaxies. It also returns a tight star-forming main sequence (MS) for M_stars\\textless 10\\textasciicircum\\10.5\\ (M_⊙) with a ˜0.3 dex scatter at z ˜ 0 in our fiducial choices. If a UVJ-based cut is adopted, the TNG MS exhibits a downwardly bending at stellar masses of about 1010.5-10.7 M⊙. Moreover, the model predicts that \\˜ \\80 (50) per cent of 1010.5-11 M⊙ galaxies at z = 0 (z = 2) are quiescent and the numbers of quenched galaxies at intermediate redshifts and high masses are in better agreement with observational estimates than previous models. However, shorter SFR-averaging time-scales imply higher normalizations and scatter of the MS, while smaller apertures lead to underestimating the galaxy SFRs: overall we estimate the inspected systematic uncertainties to sum up to about 0.2-0.3 dex in the locus of the MS and to about 15 percentage points in the fraction of quenched galaxies. While TNG colour distributions are clearly bimodal, this is not the case for the SFR logarithmic distributions in bins of stellar mass (SFR ≳ 10-3 M⊙yr-1). Finally, the slope and z = 0 normalization of the TNG MS are consistent with observational findings; however, the locus of the TNG MS remains lower by about 0.2-0.5 dex at 0.75 ≤ z \\textless 2 than the available observational estimates taken at face value.","urldate":"2019-04-15","journal":"Monthly Notices of the Royal Astronomical Society","author":[{"propositions":[],"lastnames":["Donnari"],"firstnames":["Martina"],"suffixes":[]},{"propositions":[],"lastnames":["Pillepich"],"firstnames":["Annalisa"],"suffixes":[]},{"propositions":[],"lastnames":["Nelson"],"firstnames":["Dylan"],"suffixes":[]},{"propositions":[],"lastnames":["Vogelsberger"],"firstnames":["Mark"],"suffixes":[]},{"propositions":[],"lastnames":["Genel"],"firstnames":["Shy"],"suffixes":[]},{"propositions":[],"lastnames":["Weinberger"],"firstnames":["Rainer"],"suffixes":[]},{"propositions":[],"lastnames":["Marinacci"],"firstnames":["Federico"],"suffixes":[]},{"propositions":[],"lastnames":["Springel"],"firstnames":["Volker"],"suffixes":[]},{"propositions":[],"lastnames":["Hernquist"],"firstnames":["Lars"],"suffixes":[]}],"month":"June","year":"2019","keywords":"cosmology: theory, galaxies: evolution, galaxies: formation, galaxies: star formation, methods: numerical","pages":"4817–4840","bibtex":"@article{donnari_star_2019,\n\ttitle = {The star formation activity of {IllustrisTNG} galaxies: main sequence, {UVJ} diagram, quenched fractions, and systematics},\n\tvolume = {485},\n\tissn = {0035-8711},\n\tshorttitle = {The star formation activity of {IllustrisTNG} galaxies},\n\turl = {http://adsabs.harvard.edu/abs/2019MNRAS.485.4817D},\n\tdoi = {10.1093/mnras/stz712},\n\tabstract = {We select galaxies from the IllustrisTNG hydrodynamical simulations \n(M\\_stars{\\textgreater} 10{\\textasciicircum}9 M\\_⊙ at 0 ≤ z ≤ 2) and characterize the\nshapes and evolutions of their UVJ and star formation rate-stellar mass\n(SFR-Mstars) diagrams. We quantify the systematic\nuncertainties related to different criteria to classify star-forming\nversus quiescent galaxies, different SFR estimates, and by accounting\nfor the star formation measured within different physical apertures. The\nTNG model returns the observed features of the UVJ diagram at z ≤ 2,\nwith a clear separation between two classes of galaxies. It also returns\na tight star-forming main sequence (MS) for M\\_stars{\\textless} 10{\\textasciicircum}\\{10.5\\}\n(M\\_⊙) with a ˜0.3 dex scatter at z ˜ 0 in our fiducial\nchoices. If a UVJ-based cut is adopted, the TNG MS exhibits a downwardly\nbending at stellar masses of about 1010.5-10.7\nM⊙. Moreover, the model predicts that \\{˜ \\}80 (50)\nper cent of 1010.5-11 M⊙ galaxies at z = 0 (z\n= 2) are quiescent and the numbers of quenched galaxies at intermediate\nredshifts and high masses are in better agreement with observational\nestimates than previous models. However, shorter SFR-averaging\ntime-scales imply higher normalizations and scatter of the MS, while\nsmaller apertures lead to underestimating the galaxy SFRs: overall we\nestimate the inspected systematic uncertainties to sum up to about\n0.2-0.3 dex in the locus of the MS and to about 15 percentage points in\nthe fraction of quenched galaxies. While TNG colour distributions are\nclearly bimodal, this is not the case for the SFR logarithmic\ndistributions in bins of stellar mass (SFR ≳ 10-3\nM⊙yr-1). 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