Series Wave-Lenght Int. Attribution Int. Wave-Lenght 3328.34 3 1 3328.487 3336.33 5 Cr 2 3336.477 3324.06 3 3324.19 3339.80 10 Co, Cr 3 3339.932 3347.83 6 Cr 3 3347.970 3342.58 10 Cr 3 3342.717 3358.50 10 Ti, Cr 4 3358.649 3368.04 20 Cr, - ? 3368.193 3132.04 20 -, Cr 4 3132.169 3124.97 20 Cr 4 3125.109 3147.22 5 Cr 3 3147.350 3120.36 15 Cr, - 3 3120.481 3136.69 5 Cr, Co 3 3136.822 3159.10 1 0 3159.225 3118.65 10 Cr, - 2 3118.764 3128.68 5 Cr, - 2 3128.819 3145.07 2 2 3145.251 [Pg 78] MANGANESE (25) The lines of manganese are conspicuous in stellar spectra, and all the classified lines[312] within the range of Rowland’s table are found in the solar spectrum, namely the multiplets , , , , , , , , , . The ultimate lines are at 4030, and constitute a conspicuous group in the solar spectrum. They are well seen in the cooler stars, and are progressively strengthened with advancing type.[313] They first appear at . The multiplet, at 4018, 4041, 4055, 4084, etc., has a maximum, according to Menzel,[314] at . IONIZED MANGANESE Meggers, Kiess, and Walters[315] give one multiplet of ionized manganese, and this is within the range of Rowland’s table. The multiplet was previously picked out by Catalan[316] as being analogous to the arc multiplet . All the lines can be satisfactorily identified with lines in the solar spectrum, as in the following table. TABLE XIV Series Wave-Lenght Int. Cl. Attribution Int. Wave-Lenght 3441.999 9 V Mn 6 3442.118 3474.050 7 V Mn 2 3474.197 3460.332 8 V Mn, - ? 3460.460 3496.815 4 V Co, Mn 3 3496.952 3482.918 7 V Mn, - 3483.047 3474.13 6 V Mn 2 3474.287 3497.540 6 V Mn 3 3497.668 3488.618 8 V Mn 4 3488.817 3495.810 8 V Mn 2 3495.974 [Pg 79] IRON (26) The extensive occurrence of the arc lines of iron in the stellar spectrum is well known. The following multiplets[317] have been traced in the solar spectrum, and the corresponding lines are also to be traced in the spectra of the cooler stars: , , , , , , , , , , , , , , , . The iron lines have, in general,[318] a maximum at , but the only ultimate lines which are well shown in stellar spectra, the lines near 4480, increase with advancing type to the end of the sequence.[319] The following lines are used as criteria of absolute magnitude by Harper and Young:[320] 4202, 4250, 4272 (), 4072 (), 4482 (). IONIZED IRON [Pg 80] The lines of ionized iron are strong in F stars of high luminosity, and are especially conspicuous in the stars which have the c-character. Menzel[321] places the maximum at , and the writer[322] finds it at . The following multiplets, as classified by Russell,[323] occur in the solar spectrum: , , , , , , , , , , , , , , , , , , , , . Doubtfully present are: , , . The ionized iron lines are strengthened, as are other enhanced lines, over sunspots, and many of the fainter components of multiplets are observed only in the spot spectrum. COBALT (27)