TY - JOUR
T1 - Mergers, starbursts, and quenching in the SIMBA simulation
AU - Montero, Francisco Rodriguez
AU - Dave, Romeel
AU - Wild, Vivienne
AU - Angles-Alcazar, Daniel
AU - Narayanan, Desika
PY - 2019/12/1
Y1 - 2019/12/1
N2 - We use the SIMBAcosmological galaxy formation simulation to investigate the relationship between major mergers (≲4:1), starbursts, and galaxy quenching. Mergers are identified via sudden jumps in stellar mass M∗ well above that expected from in situ star formation, while quenching is defined as going from specific star formation rate (sSFR) > tH−1 to < 0.2tH−1, where tH is the Hubble time. At z ≈ 0-3, mergers show ∼2-3× higher SFR than a mass-matched sample of star-forming galaxies, but globally represent ≲ 1 per cent of the cosmic SF budget. At low masses, the increase in SFR in mergers is mostly attributed to an increase in the H2 content, but for M∗ ≳ 1010.5 M☉ mergers also show an elevated star formation efficiency suggesting denser gas within merging galaxies. The merger rate for star-forming galaxies shows a rapid increase with redshift, ∝(1 + z)3.5, but the quenching rate evolves much more slowly, ∝(1 + z)0.9; there are insufficient mergers to explain the quenching rate at z ≲ 1.5. SIMBA first quenches galaxies at z ≳ 3, with a number density in good agreement with observations. The quenching time-scales τq are strongly bimodal, with 'slow' quenchings (τq ∼ 0.1tH) dominating overall, but 'fast' quenchings (τq ∼ 0.01tH) dominating in M∗ ∼ 1010-1010.5 M☉ galaxies, likely induced by SIMBA's jet-mode black hole feedback. The delay time distribution between mergers and quenching events suggests no physical connection to either fast or slow quenching. Hence, SIMBA predicts that major mergers induce starbursts, but are unrelated to quenching in either fast or slow mode.
AB - We use the SIMBAcosmological galaxy formation simulation to investigate the relationship between major mergers (≲4:1), starbursts, and galaxy quenching. Mergers are identified via sudden jumps in stellar mass M∗ well above that expected from in situ star formation, while quenching is defined as going from specific star formation rate (sSFR) > tH−1 to < 0.2tH−1, where tH is the Hubble time. At z ≈ 0-3, mergers show ∼2-3× higher SFR than a mass-matched sample of star-forming galaxies, but globally represent ≲ 1 per cent of the cosmic SF budget. At low masses, the increase in SFR in mergers is mostly attributed to an increase in the H2 content, but for M∗ ≳ 1010.5 M☉ mergers also show an elevated star formation efficiency suggesting denser gas within merging galaxies. The merger rate for star-forming galaxies shows a rapid increase with redshift, ∝(1 + z)3.5, but the quenching rate evolves much more slowly, ∝(1 + z)0.9; there are insufficient mergers to explain the quenching rate at z ≲ 1.5. SIMBA first quenches galaxies at z ≳ 3, with a number density in good agreement with observations. The quenching time-scales τq are strongly bimodal, with 'slow' quenchings (τq ∼ 0.1tH) dominating overall, but 'fast' quenchings (τq ∼ 0.01tH) dominating in M∗ ∼ 1010-1010.5 M☉ galaxies, likely induced by SIMBA's jet-mode black hole feedback. The delay time distribution between mergers and quenching events suggests no physical connection to either fast or slow quenching. Hence, SIMBA predicts that major mergers induce starbursts, but are unrelated to quenching in either fast or slow mode.
KW - galaxies: evolution
KW - galaxies: formation
U2 - 10.1093/mnras/stz2580
DO - 10.1093/mnras/stz2580
M3 - Journal article
SN - 0035-8711
VL - 490
SP - 2139
EP - 2154
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
IS - 2
ER -