{"extern":"1","publication_status":"published","date_published":"2019-03-01T00:00:00Z","issue":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"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."}],"type":"journal_article","day":"01","article_processing_charge":"No","month":"03","date_updated":"2022-08-19T06:42:43Z","quality_controlled":"1","title":"The origin of scatter in the star formation rate–stellar mass relation","status":"public","oa":1,"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-08T07:48:31Z","publisher":"Oxford University Press","scopus_import":"1","article_type":"original","citation":{"short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","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>","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>.","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.","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.","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>."},"language":[{"iso":"eng"}],"_id":"11540","doi":"10.1093/mnras/stz030","page":"915-932","publication":"Monthly Notices of the Royal Astronomical Society","author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"}],"external_id":{"arxiv":["1805.05956"]},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"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).","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"intvolume":"       484","volume":484,"year":"2019"}