Quenching of Star Formation in Galaxies and Its Environmental Effects
Explore the mechanisms behind galaxies becoming quiescent, such as mass quenching, feedback effects, and environmental influences. Discover the environmental bi-modality in galaxy properties and how it evolves with redshift, shedding light on the complex interplay between galaxies and their surroundings.
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Seong-Kook Lee Center for the Exploration of the Origin of the Universe (CEOU), Seoul National University (SNU) (Myungshin Im, Jae-Woo Kim, Minhee Hyun, Bomi Park, Jennifer Lotz, Conor McPartland, Michael Peth, Anton Koekemoer) STAR-FORMATION PROPERTIES AND LARGE SCALE STRUCTURES OF HIGH-REDSHIFT GALAXIES
Q : How and when did galaxies become quiescent?
Quenching of SF in galaxies What makes galaxies stop forming stars? 1. Mass quenching : virial shocks slowing down the cooling rate (Birnboim+07) 2. Feedbacks : AGN/stellar (Croton+06; Somerville+08; Hopkins+14) 3. Morphological quenching : (Gavazzi+15; Zolotov+15; Tacchella+16)
Quenching of SF in galaxies 4. Environmental quenching : (Peng+10; Woo+13) Strangulation (Larson+80; Balogh+00, Peng+15) Ram pressure stripping (Gunn&Gott 72; Abadi+99) Credit: Peng+15 Galaxy harassment (Moore+96,98) Credit: Univ. of Zurich Credit: A.Chung
Effects of Environment Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) In clusters, galaxies are In field, galaxies are red color , early-type morphology, old stellar population, no star-formation (quiescent) blue color , late-type morphology, young stellar population, star-forming
Effects of Environment Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) This environmental dependence weakens with increasing redshift
Effects of Environment Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) This environmental dependence weakens with increasing redshift Still, its detailed evolution is not conclusive :
Effects of Environment z~1 Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) This environmental dependence weakens with increasing redshift Still, its detailed evolution is not conclusive : e.g. SF-densityrelation: reversal (Elbaz+07, Cooper+08) or not (Patel+09, Muzzin+12, Quadri+12) at z~1? field
Effects of Environment Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) This environmental dependence weakens with increasing redshift Still, its detailed evolution is not conclusive : e.g. SF-densityrelation: reversal (Elbaz+07, Cooper+08) or not (Patel+09, Muzzin+12, Quadri+12) at z~1? investigation at higher redshift well beyond z~1 needed ( need deep (NIR) data)
Effects of Environment Clear environment-dependent bi-modality in galaxy properties at local (Lewis et al. 2002; Kauffmann et al. 2004; Blanton et al. 2005) This environmental dependence weakens with increasing redshift Still, its detailed evolution is not conclusive : e.g. SF-densityrelation: reversal (Elbaz+07, Cooper+08) or not (Patel+09, Muzzin+12, Quadri+12) at z~1? (NIR), Spitzer/IRAC channel 1,2,3,4 (MIR) investigation at higher redshift well beyond z~1 needed ( need deep (NIR) data) UKIDSS/UDS : ~0.8 sq. deg. Subaru B,V,R,i,z (optical), UKIRT J,H,Ks
Method: cluster finding z-range : 0.028(1+z) step size : z = 0.02
Method: cluster finding z-range : 0.028(1+z) step size : z = 0.02 4 Figures from Kang & Im 15
Quiescent galaxy fraction Q.G.F. = Nquiescent/ Ntotal : cluster : field 1. Q.G.F depends more strongly on stellar mass than environment Lee,S.-K., Im, M. et al. 2015, ApJ, 810,90
Quiescent galaxy fraction Q.G.F. = Nquiescent/ Ntotal : cluster : field 1. Q.G.F depends more strongly on stellar mass than environment 2. Environmental dependence becomes significant at z < 1.2-1.3 (for low-mass galaxies)
Quiescent galaxy fraction Variation among clusters at similar epoch
Quiescent galaxy fraction Variation among clusters at similar epoch cluster 3 cluster 2 cluster 1
Summary Quiescent galaxy fraction (Q.G.F) shows stong stellar-mass dependence within the redshift range (0.5 < z < 2.0) Environmental dependence of Q.G.F. becomes significant at z < 1.3 & for low-mass galaxies There exists large variation among individual clusters (at similar epoch) in their Q.G.F. The Q.G.F. seems to be related with the LSS to which the galaxy clusters belong
