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  MUFASA: Time-scales for H ı consumption and SFR depletion of satellite galaxies in groups

Rafieferantsoa, M., Davé, R., & Naab, T. (2019). MUFASA: Time-scales for H ı consumption and SFR depletion of satellite galaxies in groups. Monthly Notices of the Royal Astronomical Society, 486(4), 5184-5196. doi:10.1093/mnras/stz1199.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0004-7421-4 Version Permalink: http://hdl.handle.net/21.11116/0000-0004-7422-3
Genre: Journal Article

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Rafieferantsoa, Mika1, Author              
Davé, Romeel, Author
Naab, Thorsten1, Author              
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1Computational Structure Formation, MPI for Astrophysics, Max Planck Society, ou_2205642              

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 Abstract: We investigate the connection between the H i content, star formation rate (SFR), and environment of galaxies using a hydrodynamic simulation that incorporates scaling relations for galactic wind and a heuristic halo mass based quenching prescription. We run two zoom-in simulations of galaxy groups with Mhalo>1013M at z = 0, selected to have quiet merger histories. We track galaxies as they become satellites, and compute the delay time τd during which the satellites are similar to central galaxies at a given stellar mass, and a fading time τf during which satellites go from gas-rich and star-forming to gas-poor and quiescent. We find 0.7 ≲ τd ≲ 3 Gyr at z = 0, and depends inversely on the satellite halo mass at infall. At z ∼ 1 we find ∼0.3 ≲ τd ≲ 2 Gyr, broadly consistent with a positive correlation with the Hubble time. For low halo mass at infall, lower stellar mass galaxies at infall time have higher τd. We generally find τf ≪ τd, ranging between ∼150 Myr at z ∼ 0 and ∼80 Myr at z ∼ 1 based on linear interpolation, with some uncertainty because they are smaller than our simulation output frequency (200−300 Myr). τf has no obvious dependence on infall halo mass. Both time-scales show little difference between H i depletion and SF quenching, indicating that using up the gas reservoir by star formation without refilling is the main mechanism to transform satellite galaxies at these halo masses. At a given physical distance from the centre of the main halo of interest, higher redshift galaxies have on average higher cold gas content, but the ratio of gas (H  ı or H2) to SFR is similar, indicating that star formation is consistently fed through reservoirs of H  ı then H2. For a given amount of H  ı, galaxies have shorter consumption times in more massive halo structures at infall. Our results suggest that group-scale simulations naturally yield a delayed-then-rapid satellite quenching scenario as inferred from observations both today and at earlier epochs, though we highlight some quantitative discrepancies.

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 Dates: 2019-05-02
 Publication Status: Published online
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 Rev. Method: Peer
 Identifiers: DOI: 10.1093/mnras/stz1199
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Title: Monthly Notices of the Royal Astronomical Society
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Source Genre: Journal
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Publ. Info: OXFORD : OXFORD UNIV PRESS
Pages: - Volume / Issue: 486 (4) Sequence Number: - Start / End Page: 5184 - 5196 Identifier: ISSN: 0035-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000021470