T. D. Kinman's scientific contributions

Citations

... The mean period of the RRLs pulsating in the first overtone (RRc) displays a similar dichotomic distribution, with á ñP 0.31 c and~0.36days in the OoI and OoII globular cluster, respectively. Subsequent spectroscopic investigations enriched the empirical scenario demonstrating that OoI globular clusters are more metal-rich and cover a broad range in metal abundances, while OoII globular clusters are more metal-poor stellar systems (Arp 1955;Kinman 1959). Later on, it was also recognized that the population ratio, i.e., the ratio between RRc and the total number of RRLs, is smaller in OoI (N c /N tot ≈ 0.29) than in OoII (N c /N tot ≈ 0.44) globular clusters (Stobie 1971;Bono et al. 2016;Braga et al. 2016). ...
... An interesting feature of GC populations is their use as beacons in the darkness to infer the structure of galaxies (e.g. Shapley, 1918a;Kinman, 1959a;Harris and Petrie, 1978;Frenk and White, 1980;van Dokkum et al., 2018). The avalanche of data from the Gaia mission (Gaia Collaboration et al., 2018;Baumgardt et al., 2019;Vasiliev, 2019), combined with recent developments in the modelling of stellar clusters, has enabled to link GC populations to the formation and assembly history of their host galaxies in a quantitative manner Kruijssen et al., 2019a,b;Forbes, 2020;Horta et al., 2020b;Kruijssen et al., 2020). ...