@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},
}

{"_id":"e5xNJMfexuZGuApFB","bibbaseid":"walters-woo-ellison-quenchingtimescalesintheillustristngsimulation-2022","author_short":["Walters, D.","Woo, J.","Ellison, S. L."],"bibdata":{"bibtype":"techreport","type":"techreport","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":[{"propositions":[],"lastnames":["Walters"],"firstnames":["Dan"],"suffixes":[]},{"propositions":[],"lastnames":["Woo"],"firstnames":["Joanna"],"suffixes":[]},{"propositions":[],"lastnames":["Ellison"],"firstnames":["Sara","L."],"suffixes":[]}],"month":"January","year":"2022","note":"Publication Title: arXiv e-prints ADS Bibcode: 2022arXiv220200015W Type: article","keywords":"Astrophysics - Astrophysics of Galaxies","bibtex":"@techreport{walters_quenching_2022,\n\ttitle = {Quenching {Timescales} in the {IllustrisTNG} {Simulation}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022arXiv220200015W},\n\tabstract = {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.},\n\turldate = {2022-02-02},\n\tauthor = {Walters, Dan and Woo, Joanna and Ellison, Sara L.},\n\tmonth = jan,\n\tyear = {2022},\n\tnote = {Publication Title: arXiv e-prints\nADS Bibcode: 2022arXiv220200015W\nType: article},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n","author_short":["Walters, D.","Woo, J.","Ellison, S. L."],"key":"walters_quenching_2022","id":"walters_quenching_2022","bibbaseid":"walters-woo-ellison-quenchingtimescalesintheillustristngsimulation-2022","role":"author","urls":{"Paper":"https://ui.adsabs.harvard.edu/abs/2022arXiv220200015W"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"techreport","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["quenching","timescales","illustristng","simulation","walters","woo","ellison"],"title":"Quenching Timescales in the IllustrisTNG Simulation","year":2022}