Quenching Timescales in the IllustrisTNG Simulation. Walters, D., Woo, J., & Ellison, S. L. Technical Report January, 2022. Publication Title: arXiv e-prints ADS Bibcode: 2022arXiv220200015W Type: article
Quenching Timescales in the IllustrisTNG Simulation [link]Paper  abstract   bibtex   
The timescales for galaxy quenching offer clues to its underlying physical drivers. We investigate central galaxy quenching timescales in the IllustrisTNG 100-1 simulation, their evolution over time, and the pre-quenching properties of galaxies that predict their quenching timescales. Defining quenching duration \${\textbackslash}tau_q\$ as the time between crossing sSFR thresholds, we find that \${\textbackslash}sim\$40% of galaxies quench rapidly with \${\textbackslash}tau_q{\textless}\$1 Gyr, but a substantial tail of galaxies can take up to 10 Gyr to quench. Furthermore, 29% of galaxies that left the star forming main sequence (SFMS) more than 2 Gyr ago never fully quench by \$z=0\$. While the median \${\textbackslash}tau_q\$ is fairly constant with epoch, the rate of galaxies leaving the SFMS increases steadily over cosmic time, with the rate of slow quenchers being dominant around \$z{\textbackslash}sim2\$ to 0.7. Compared to fast quenchers (\${\textbackslash}tau_q{\textless}\$1 Gyr), slow-quenching galaxies (\${\textbackslash}tau_q{\textgreater}\$1 Gyr) were more massive, had more massive black holes, had larger stellar radii and accreted gas with higher specific angular momentum (AM) prior to quenching. These properties evolve little by \$z=0\$, except for the accreting gas AM for fast quenchers, which reaches the same high AM as the gas in slow quenchers. By \$z=0\$, slow quenchers also have residual star formation in extended gas rings. Using the expected relationship between stellar age gradient and \${\textbackslash}tau_q\$ for inside-out quenching we find agreement with MaNGA IFU observations. Our results suggest the accreting gas AM and potential well depth determine the quenching timescale.
@techreport{walters_quenching_2022,
	title = {Quenching {Timescales} in the {IllustrisTNG} {Simulation}},
	url = {https://ui.adsabs.harvard.edu/abs/2022arXiv220200015W},
	abstract = {The timescales for galaxy quenching offer clues to its underlying physical drivers. We investigate central galaxy quenching timescales in the IllustrisTNG 100-1 simulation, their evolution over time, and the pre-quenching properties of galaxies that predict their quenching timescales. Defining quenching duration \${\textbackslash}tau\_q\$ as the time between crossing sSFR thresholds, we find that \${\textbackslash}sim\$40\% of galaxies quench rapidly with \${\textbackslash}tau\_q{\textless}\$1 Gyr, but a substantial tail of galaxies can take up to 10 Gyr to quench. Furthermore, 29\% of galaxies that left the star forming main sequence (SFMS) more than 2 Gyr ago never fully quench by \$z=0\$. While the median \${\textbackslash}tau\_q\$ is fairly constant with epoch, the rate of galaxies leaving the SFMS increases steadily over cosmic time, with the rate of slow quenchers being dominant around \$z{\textbackslash}sim2\$ to 0.7. Compared to fast quenchers (\${\textbackslash}tau\_q{\textless}\$1 Gyr), slow-quenching galaxies (\${\textbackslash}tau\_q{\textgreater}\$1 Gyr) were more massive, had more massive black holes, had larger stellar radii and accreted gas with higher specific angular momentum (AM) prior to quenching. These properties evolve little by \$z=0\$, except for the accreting gas AM for fast quenchers, which reaches the same high AM as the gas in slow quenchers. By \$z=0\$, slow quenchers also have residual star formation in extended gas rings. Using the expected relationship between stellar age gradient and \${\textbackslash}tau\_q\$ for inside-out quenching we find agreement with MaNGA IFU observations. Our results suggest the accreting gas AM and potential well depth determine the quenching timescale.},
	urldate = {2022-02-02},
	author = {Walters, Dan and Woo, Joanna and Ellison, Sara L.},
	month = jan,
	year = {2022},
	note = {Publication Title: arXiv e-prints
ADS Bibcode: 2022arXiv220200015W
Type: article},
	keywords = {Astrophysics - Astrophysics of Galaxies},
}

Downloads: 0