[{"date_created":"2022-07-08T07:48:31Z","publisher":"Oxford University Press","scopus_import":"1","language":[{"iso":"eng"}],"month":"03","date_published":"2019-03-01T00:00:00Z","article_type":"original","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"915-932","intvolume":"       484","status":"public","day":"01","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1805.05956","open_access":"1"}],"external_id":{"arxiv":["1805.05956"]},"title":"The origin of scatter in the star formation rate–stellar mass relation","doi":"10.1093/mnras/stz030","year":"2019","_id":"11540","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Preprint","arxiv":1,"oa":1,"volume":484,"date_updated":"2022-08-19T06:42:43Z","article_processing_charge":"No","abstract":[{"lang":"eng","text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr."}],"author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"publication_status":"published","citation":{"ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","apa":"Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>.","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932. doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932."}},{"doi":"10.1093/mnras/stw2884","year":"2017","external_id":{"arxiv":["1608.08218"]},"title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1608.08218"}],"citation":{"apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>.","ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396."},"publication_status":"published","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"last_name":"Crain","full_name":"Crain, Robert A.","first_name":"Robert A."},{"first_name":"Matthieu","last_name":"Schaller","full_name":"Schaller, Matthieu"},{"first_name":"Richard","last_name":"Bower","full_name":"Bower, Richard"},{"full_name":"Theuns, Tom","last_name":"Theuns","first_name":"Tom"}],"abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"article_processing_charge":"No","volume":465,"date_updated":"2022-08-19T07:56:07Z","oa":1,"arxiv":1,"oa_version":"Preprint","quality_controlled":"1","acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","_id":"11565","article_type":"original","date_published":"2017-02-01T00:00:00Z","month":"02","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"Oxford University Press","date_created":"2022-07-12T12:25:08Z","type":"journal_article","day":"01","status":"public","intvolume":"       465","page":"2381-2396","publication":"Monthly Notices of the Royal Astronomical Society","issue":"2"}]