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 B-Formula I-Formula I-Formula O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Formula I-Formula I-Formula O B-Citation I-Citation I-Citation I-Citation O B-Formula I-Formula I-Formula O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-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 B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-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 B-Wavelength B-Formula I-Formula I-Formula I-Formula 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 B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O B-Citation I-Citation I-Citation I-Citation O O O O B-CelestialObjectRegion I-CelestialObjectRegion B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-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 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 B-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 O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula 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 B-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 O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O B-Formula I-Formula I-Formula O O B-Formula I-Formula I-Formula O O O B-Formula I-Formula I-Formula I-Formula I-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 B-Formula I-Formula I-Formula O B-Formula I-Formula I-Formula O O
tokens: however, the fraction of dust in the clumpy component ( F ) does evolve strongly with redshift, similar to the gas-mass fraction. Fig. 8 Evolution of massive galaxy properties from their local values out to z ~ 1. The evolution of the dust-mass fraction ( M d ∕ M * ) was determined from a power-law fit to data from Santini et al. (2014) , Béthermin et al. (2015) (for z ≤ 1), and Rémy-Ruyer et al. (2014) for z = 0. The upper bound to the M d ∕ M * evolution is given by assuming M d ~ 0.5 × Z × M g , and the evolution of gas and metallicity over this redshift and stellar mass range. The evolution of specific SFR is shaded purple between the relationship in Sargent et al. (2014) and . The evolution of the molecular gas fraction (blue) is from Tacconi et al. (2018) . We find that the fraction ( F ) of dust in clumps surrounding nascent star-forming regions has increased by a factor of ~5.5, and that the overall attenuation of UV (SFR MS /SFR UV ) has increased by a factor of ~2.5 (ranging from 3.4 to 1.9 for face-on to edge-on galaxies, respectively). da Cunha et al. (2010) , Smith et al. (2012) , Sandstrom et al. (2013) , and Rowlands et al. (2014) found that, in the local Universe, M d ∕ M * is proportional to sSFR. Studies such as Sargent et al. (2012) and Tasca et al. (2015) , that look at how sSFR changes with redshift, find that the sSFR varies as sSFR out to redshifts z 2. This would give a sSFR increase by a factor of ~3.6 between z = 0.07 and z = 0.7. We note, however, that this trend also is stellar mass dependent (e.g. Schreiber et al. 2015 ), and that lower-mass galaxies have a shallower evolution in sSFR than the most massive galaxies. Recent studies of molecular gas at high redshifts indicate that the cosmic density of molecular gas, similar to the cosmic density of star formation, peaks between redshifts 2 and 3 ( Decarli et al. 2016 ). Genzel et al. (2015) , Sargent et al. (2014) , and Tacconi et al. (2018) used compilations of studies that measure gas mass via CO line luminosities and found that M g ∕ M * varies like , which corresponds to an increase by a factor of ~3.5 between z = 0.07 and z = 0.7. On the other hand, Bauermeister et al. (2013) expect which would imply an increase in the gas mass fraction by a factor of ~4.4. In any case, the gas mass is expected to increase by a factor of ~4 between our two redshift slices. In Fig. 7 , we show with two solid lines the relations SFR UV /SFR and . The parameter that most strongly controls the dust-to-gas mass is the metallicity (e.g. Leroy et al. 2011 ; Accurso et al. 2017 ). According to the parametrization of Zahid et al. (2014) , a galaxy with log ( M * ∕ M ⊙ ) = 10.2 would have a metallicity of 0.069 dex less at z = 0.7 than at z = 0.07. A galaxy at M * ~ 10 10.5 M ⊙ , on the other hand, will have a change in metallicity of 0.035 dex between the same two redshifts. For our sample, the dust to gas ratio should not change significantly between z ~ 0 and z ~ 0.7, however, we