ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O B-Formula O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Formula O B-Formula I-Formula I-Formula O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O B-Wavelength O O O O O O O O B-Wavelength O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: stellar mass growth that for individual massive galaxies. At a fixed space density threshold of density of , the most massive blue galaxies are ∼0.3 dex lower in stellar mass than the most massive red galaxies (i.e., half the mass). While we expect the most massive red galaxies to remain on the red sequence and increase in mass via mergers, it is likely that the most massive blue galaxies have star formation quenched and then move onto the red sequence. The rate at which massive red galaxies increase in stellar mass through mergers with smaller galaxies appears to slow somewhat from ∼0.4 dex per unit redshift for z = 1.1 to z = 0.7 to ∼0.2 dex per unit redshift for z = 0.7 to z = 0.3. We know that massive early-type galaxies must have grown in stellar mass because observations clearly show them experiencing mergers sufficient in frequency and mass ratio to give rise to a significant increase in stellar mass. In fact, merger studies have produced a range of estimates of stellar mass growth. For example, van Dokkum ( 2005 ) found a stellar mass increase due to mergers in massive red galaxies of per Gyr, which implies a stellar mass increase over the 4.7 Gyr from z = 1.1 to z = 0.3 of ×∼1.4. Similarly, López-Sanjuan et al. ( 2012 ) found stellar mass growth in massive early-type galaxies due to mergers of ×∼1.3 from z = 1 to the present. On the other hand, Masjedi et al. ( 2008 ) found that luminous red galaxies were growing due to merger activity at a much slower rate: at least per Gyr on average at redshift ∼0.25, implying at least 8% growth from z = 1.3 to z = 0.3. The lack of evolution (in comoving coordinates) of the spatial correlation function of massive red galaxies also clearly indicates that the most massive red galaxies must be undergoing mergers. White et al. ( 2007 ) used observations of the clustering of luminous red galaxies to show that about one-third of the most luminous satellite galaxies appear to have undergone merging or disruption with massive halos between z = 0.9 and z = 0.5, while Brown et al. ( 2008 ) found that massive red galaxies grew by ×1.3 from z = 1.0 to z = 0. As with SMD evolution, our stellar mass growth measurements for massive red galaxies based on SMF evolution (×1.7) are comparable with the those implied by comparison of the K -band LF with passive evolution (×1.4). 10.4. Stellar Mass Evolution—Errors In addition to the sources of error inherent in measuring K -band luminosity evolution (Section 9.4 ), we have one very significant additional source of error in measuring stellar mass evolution—namely, uncertainty in stellar mass-to-light ratios M / L K —and we include this in Table 5 for red galaxies. M / L K uncertainties arise from the evolving M / L K –rest-frame ( B − V ) relationships in Equations ( 3 ) and ( 5 ). We take the intrinsic random variation in between galaxies to be 0.1 dex (Section 5 ). Systematic uncertainties arise from the fact that Equations ( 3 ) and ( 5 ) are derived from SPS