BGGs/BCGs group multiplicity >5 0.09 < z < 0.27 ! Previous work: Lin & Mohr (2004): z < 0.09, ~0.26 Brough et al. (2008): z < 0.1, ~0.24 Hansen et al. (2009): 0.1 < z < 0.3, ~0.3 Lidman et al. (2012): 0.63+/-0.07 0.05 < z < 1.6 14! Oliva)Altamirano!et.!al.!(2014)!
the halos of similar mass at z = 0 18! Halo!Mass! BGG/BCG!Stellar!Mass! Halo!Mass! <M* >!=!1011.18Mo ! <M* >!=!1011.14Mo ! <M* >!=!1011.29Mo ! <M* >!=!1011.34Mo !
! Nevertheless!major!mergers!are!not! impossible!to!occur!at!low!redshi_s! (Brough!et.!al.,!2011). The importance of major and minor mergers in BCGs 29!
(2007) ATLAS3D ellipticity parameter Cappellari et al. (2011) BCG are predicted to be slow rotators... 31! The!SAURON!sample!contains!only!9!galaxies!with!M*! >!1011.3Msun ,! and!only!1!of!them!is!a!BCG!
plotted with thick orange and green lines. The SAURON sample is plotted in grey. We choose not to plot the full ATLAS3D sample of 260 galaxies in order to keep the plot legible. Fast rotators are plotted as solid lines and slow rotators are plotted as dashed lines. Fast rotators have a convex profile, and slow rotators have a concave profile. Fig. 6.— Lambda at the e↵ective radius as a function of ellip- ticity, also measured at the e↵ective radius. SAURON galaxies are plotted as triangles, ATLAS3D galaxies are plotted as crosses, BCGs from this study are plotted as squares, and Companion galaxies from this study are plotted as plus symbols. The blue line indicates the division between fast rotating and slow rotating galaxies. We find that three BCGs (1048, 1153, 1261) and four companions (1027, 1066, 1048) are classified as fast rotators. as fast rotators. We find that 3 BCGs and all 4 com- Jimmy et. al. (2013) ~30% of BCGs are fast rotators 34! AMR simulations of Martizzi et. al. (2014) ε! Figure 6. Stellar mass vs. star formation rate for the “star- forming”BCGs. The simulations are compared to the observa- tional data by Liu et al. (2012) (green squares). The BCGs with reported SFR< 10−1 M /yr are represented by upper limits (the measured SFR is 0 M /yr). The blue solid line represents a power-law extrapolation of the sequence for star forming galaxies measured by Brinchmann et al. (2004). 0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 λr Jimmy+ 2013 - BCGs z = 0 - AGN-ON z = 0 - AGN-OFF Figure 7. Ellipticity (edge-on view) vs. angular momentum probe parameter λr. This plot is used to separate fast rotators and slow rotators: here the separation is represented by the black solid line λr = 0.33 ∗ √ . Data from Jimmy et al. (2013) is also compared to our results (blue circles). λ!
radius. BCGs are plotted as squares, and companions are plotted as crosses. Plot symbols are scaled according to galaxy mass, with a larger symbol indicating a higher dynamical mass. Plot symbols are also color coded, with orange indicating a fast rotating galaxy, and green indicating a slow rotating galaxy. Galaxies plotted on the negative side of the x-axis are classified as not merging by the G M20 criteria, galaxies on the positive side of the x-axis are classified as merging. There appears to be no correlation between just the core that is similarly slowl extended discs se could help confirm in which they fo angular momentu 4.1.4. BCGs 1027, 10 currently undergo the G M20 criter have a more than adding evidence t the future. Altho S/N over 10 to de galaxy to BCG 20 rotating BCGs w 1027 (FR) exhibit a slight velocity extreme rotation to BCG 1066 (S appears under vis two cores, much l 4. Irregularities in the galaxy’s light distribution are morphological signatures of merging In!the!last!0.2Gyr! (Lotz!et.!al.,!2008)! Is the angular momentum a good indicator of ongoing mergers? 35! Jimmy et. al. (2013)
the result of major dissipationless mergers. Met gradient < -0.3 Met! R! R! Met! Steep gradients could be due to a core collapsed formation or major mergers Involving high fractions of gas. Met gradient > -0.4 Kobayashi et. al. 2004, Hopkins et. al. 2009, Hirschmann in prep.
Agrees!with!early)type!galaxy!simulaAons:! Naab!et.!al.!2013,!Hirschmann!et.!al.!2013,! Peeple!et.!al.!2014.! ! They!experience!passive!accreAon!histories! (No!star!formaAon!since!z!=!2).! Brightest$cluster$galaxies:$ Intermediate!age)metal!rich!central!stellar!! PopulaAons.! Shallow!stellar!populaAon!gradients.!! ! Disagrees!with!SAM!De!Lucia!et.!al.!2007!! Agrees!with!Tonini!et.!al.!2012.! ! They!experience!ac?ve!accreAon!histories! (Star!formaAon!up!to!z!=!1).! Figure 4. Star formation activity of the model BCGs from z = 0.02 to z formation rate (SFR). Right column: distribution of the instantaneous spe fraction of BCGs in a given bin of star formation rate/specific star formatio
them to experience many mergers in time. These ongoing accretion events will trigger star formation at z > 1 resulting in intermediate central ages, and will disrupt the metallicity gradients at z < 1.
Group Galaxies from the GAMA. • Kinematics • Central stellar populations • Stellar population gradients • Other properties of the group: dominance, masses, emission lines. 48! Anglo!Australian!Telescope!(AAT)!
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