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Table C.1

Values of original and future barycentric, reciprocal semi-major axes in comparison to values published in MW08, and comparison of data used (Col. (3)) and orbit-quality assessment (Cols. (2) and (11)–(12)).

Comet Marsden & Williams Catalogue (MW08) Present Catalogue – the new results
MSE Per cent of 1 /aori 1 /aosc 1 /afut 1 /aori 1 /afut rms No. of MSE New
class residuals used in units of 10-6 AU-1 i n u n i t s of 10-6AU-1 [.̋] res. class class
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)

C/1902 R1 1B 80 27 79 865 31.04 ± 1.71 870.94 ± 1.71 2.28 2501 1A 1b
C/1902 X1 1B 29 26 218 488 74.03 ± 7.25 439.81 ± 7.24 1.66 1307 1B 1b
C/1903 M1 1B 45 33 1230 1000 24.12 ± 9.55 1010.00 ± 9.55 2.03 1021 1B 2a
C/1904 Y1 2A 32 75 360 170 101. ± 117. 348. ± 117. 2.87 302 2A 2b
C/1906 B1 1B 83 75 857 343 135.59 ± 22.96 402.66 ± 22.97 3.07 450 1B 2a
117.32 ± 73.86 149.58 ± 73.87 3.05 449 1B 2a
C/1906 E1* 1B 123 28 452 519 17.35 ± 5.55 529.52 ± 5.54 1.96 812 1A 1a
C/1907 E1 1B 45 25 489 290 33.76 ± 21.56 281.04 ± 21.55 2.56 296 1B 2a
C/1911 S3 2A 54 74 483 +175 163.8 ± 36.8 80.7 ± 36.8 2.35 246 2A 2a
796. ± 205. 1041. ± 205 2.10 244 2B 2b
C/1912 R1 1B 20 45 630 363 36.77 ± 5.27 370.81 ± 5.27 2.48 1670 1B 1b
C/1913 Y1 1A 36 29 140 063 22.14 ± 1.30 56.41 ± 1.30 2.06 1874 1A 1a
52.57 ± 4.23 86.84 ± 4.23 2.00 1860 1A 1a
C/1914 F1 2A 24 126 88 1561 57.45 ± 28.41 1492.0 ± 28.4 3.33 517 2A 2a
600. ± 152. 1475.8 ± 37.7 3.12 519 2A 2b
C/1914 M1* 1A 64 27 878 1 36.6 ± 25.9 8.5 ± 25.0 2.21 122 1B 1b
C/1916 G1 1A 45 17 353 763 35.33 ± 3.20 781.41 ± 3.20 1.97 823 1A 1a
69.59 ± 9.48 783.75 ± 8.79 1.84 817 1A 1b
C/1919 Q2 2A 35 20 199 42 34.7 ± 67.3 26.9 ± 67.3 2.58 498 2A 2a
C/1921 E1 1B 32 18 354 351 120.1 ± 37.6 488.8 ± 37.4 3.27 914 1B 2a
85.9 ± 80.8 210.9 ± 96.6 3.25 914 1B 2a
C/1922 U1 1A 45 21 334 523 2.35 ± 8.52 542.13 ± 8.51 1.82 826 1A 1b
C/1925 F1* 1A 25 35 582 128 34.83 ± 8.45 127.96 ± 8.45 2.75 463 1A 1b
C/1925 G1 1A 42 40 545 533 40.03 ± 5.74 532.49 ± 5.74 2.79 964 1A 1b
C/1925 W1 1B 44 24 244 322 28.59 ± 9.62 317.76 ± 9.61 1.94 593 1B 1b
C/1932 M1 1B 30 56 365 327 24.21 ± 19.40 245.8 ± 19.4 2.60 325 1B 1b
C/1932 M2 1A 59 45 619 240 56.58 ± 3.07 229.01 ± 3.07 1.77 546 1A 1a
C/1935 Q1* 1A 86 19 506 281 13.16 ± 5.19 285.68 ± 5.19 1.49 250 1A 1a
C/1937 C1 1B 35 62 79 1400 58.40 ± 7.16 1396.88 ± 7.17 2.53 767 1B 1b
44.8 ± 14.4 1383.3 ± 11.7 2.48 766 1B 1b
C/1937 N1 2A 55 124 17 281 37.3 ± 40.5 194.2 ± 40.5 2.05 765 2A 2a
507. ± 101. 231. ± 172. 1.92 766 2A 2a
C/1940 R2 1B 56 1 1319 1570 60.0 ± 17.7 1630.6 ± 17.7 1.77 678 1B 1b
51.6 ± 17.1 1494.0 ± 35.7 1.49 670 1B 1b
C/1940 S1 2B 62 124 1374 1123 297. ± 427. 703. ± 427. 3.67 61 2A 2b
C/1941 K1 1B 79 78 278 190 53.89 ± 2.47 166.22 ± 2.47 2.22 801 1A 1b
C/1942 C1 1B 111 16 618 821 22.60 ± 3.33 813.98 ± 3.33 1.46 412 1A 1a
37.0 ± 15.6 775.68 ± 8.58 1.23 411 1A 1b
C/1942 C2* 1A 80 34 774 282 29.1 ± 13.5 278.3 ± 13.5 1.57 88 1A 1b
C/1944 K2 1A 89 18 937 522 20.8 ± 12.8 518.7 ± 12.8 1.58 56 1A 1b
C/1946 C1 1A 43 13 678 373 0.80 ± 4.60 386.97 ± 4.60 2.54 857 1A 1a
102.4 ± 12.7 346.80 ± 5.61 2.17 848 1A 1b
C/1946 P1 1A 79 44 683 16 50.86 ± 5.08 22.55 ± 5.08 0.99 257 1A 1a
C/1946 U1 1A 75 1 393 26 0.59 ± 4.54 26.22 ± 4.54 1.25 259 1A 1a
17.08 ± 6.52 43.88 ± 6.52 1.19 259 1B 1b
C/1947 S1 1A 45 24 485 366 33.34 ± 3.46 356.31 ± 3.46 2.59 546 1A 1a
53.02 ± 8.19 277.6 ± 11.7 2.42 543 1A 1b
C/1947 Y1 1B 76 28 724 53 28.89 ± 8.49 54.31 ± 8.50 1.22 204 1B 1b
C/1948 E1 1A 44 34 373 31 37.25 ± 2.74 35.21 ± 2.74 1.48 431 1A 1a
C/1948 T1* 1A 100 34 699 225 34.2 ± 10.0 225.0 ± 10.0 0.94 52 1A 1b
C/1950 K1 1A 16 37 479 270 45.1 ± 2.2 278.4 ± 2.2 1.28 466 1A 1a

Notes. Columns (4)–(6) show values of 1 /aori, 1 /aosc and 1 /afut taken from MW08, Cols. (7)–(8) give values of 1 /aori and 1 /afut and their uncertainties derived in the present investigation. NG solutions are given in the second row of these comets when these solutions were possible to determine. The rms and the number of residuals are additionally given in Cols. (9)–(10). In the last two columns the quality class assessments are presented using the standard MSE method (Col. (12)), and the new revised method proposed by Królikowska & Dybczyński (Col. (13)). Column (3) shows the per cent of residuals used in MW08 in comparison to residuals used here for each comet (compare Col. (10) with twice as many as given in Col. (9) of Table A.1). NG models are indicated by light grey shading, an asterisk in Col. (1) indicates comets with large perihelion distances. For more details see the text.

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