Table 5: This table was organized in increasing order of $T\rm _{eff}$, with the comments about the results shown in the last column of each series of 4 columns.
Star $T\rm _{eff}$(K) $\log g$ Comm.   Star $T\rm _{eff}$(K) $\log g$ Comm.   Star $T\rm _{eff}$(K) $\log g$ Comm.
HD 123396 4360 1.4(3)     HD 202109 4910 2.41     HD 13551 5870 4.0(1)  
HD 220009 4370 1.91     HD 104979 4920 2.58     HD 106191 5890 4.2(1) a, c, g
HD 210910 4570 2.7(2) a, b, f   HD 46407 4940 2.65     HD 8270 5940 4.2(1)  
HD 5424 4570 2.0(3)     HD 223938 4970 3.1(1)     HD 147609 5960 4.42(9) a, b, e
HD 749 4610 2.8(1)     HD 12392 5000 3.2(1)     HD 89948 6010 4.30(8) h
HD 210709 4630 2.4(2)     HD 139195 5010 2.89     HD 188985 6090 4.3(1) c
HD 26967 4650 2.51     HD 20894 5080 2.60 j   HD 76225 6110 3.8(1) i
HD 116869 4720 2.2(2)     HD 113226 5082 2.85     HD 222349 6130 3.9(1)  
HD 205011 4780 2.41     HD 13611 5120 2.49     HD 92545 6210 4.0(1) c
HD 9362 4780 2.43     HD 204075 5250 1.53 c, f   BD+18 5215 6300 4.2(1) d
HD 116713 4790 2.67     HD 22589 5400 3.3(1)     HD 150862 6310 4.6(1) c
HD 181053 4810 2.48     HD 87080 5460 3.7(2)     HD 107574 6400 3.6(2) c
HD 27271 4830 2.9(1)     HD 48565 5860 4.01(8) i   HR 107 6440 4.08(7) a, b
Comments: a. upper limit for Hf; b. one of the lines has only an upper limit for Ru; c. poor line profiles at $\lambda $4080; d. poor line profiles of Ru I at $\lambda $4757; e. poor line profile of Hf II at $\lambda $4093; f. very broadened spectral lines; g. S/N $\approx$ 100; h. S/N $\approx$ 250; i. $\Delta$(Ru) >0.3; j. $\Delta$(Hf) > 0.3.

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