Table 2
Analyzed sample of large-perihelion LPCs with long data arcs; three samples are listed in order of increasing q.
| Comet | q | First obs. | T | Last obs. | Data arc | Range of rh | Data arc | |||
|---|---|---|---|---|---|---|---|---|---|---|
| (au) | [yyyymmdd] | (yr) | PRE (au) | POST (au) | PRE (yr)/no. of obs. | POST | qori-number | |||
| Sample LAn | ||||||||||
| C/2000 CT54 | 3.16 | 19990321 | 20010619 | 20040117 | 4.83 | 7.716 – | 8.519 | 2.25/69 | 2.58/152 | 1 |
| C/2016 N4 | 3.20 | 20150911 | 20170916 | 20200326 | 4.54 | 7.136 – | 6.376 | 2.01/1036 | 2.52/1049 | 3 |
| C/2017 M4(*) | 3.25 | 20170616 | 20190118 | 20211130 | 4.46 | 6.088 – | 9.191 | 1.41/2854 | 2.83/430 | 4 |
| C/1980 E1 | 3.36 | 19800211 | 19820312 | 19861230 | 6.88 | 7.469 – | 13.91 | 2.02/97 | 4.78/101 | 2 |
| C/1997 BA6 | 3.44 | 19970111 | 19991127 | 20040915 | 7.68 | 9.152 – | 13.39 | 2.84/278 | 4.54/258 | 5 |
| C/2012 F3 | 3.46 | 20120119 | 20150406 | 20171017 | 5.74 | 9.928 – | 8.359 | 3.20/1034 | 2.52/729 | 6 |
| C/1999 H3 | 3.50 | 19990422 | 19990818 | 20020320 | 2.91 | 3.664 – | 8.483 | 0.31/317 | 2.59/563 | 7 |
| C/2000 SV74 | 3.54 | 20000905 | 20020430 | 20050512 | 4.68 | 6.264 – | 9.507 | 1.58/757 | 3.03/1450 | 8 |
| C/2015 O1 | 3.73 | 20150615 | 20180219 | 20200320 | 4.76 | 8.652 – | 7.276 | 2.68/1904 | 2.08/2260 | 9 |
| C/2013 G3 | 3.85 | 20130410 | 20141115 | 20161223 | 3.70 | 6.201 – | 7.337 | 1.58/850 | 2.08/62 | 10 |
| C/2005 EL173 | 3.89 | 20050303 | 20070305 | 20081117 | 3.71 | 7.120 – | 6.450 | 1.99/231 | 1.69/85 | 11 |
| Sample LBn | ||||||||||
| C/2008 FK75 | 4.51 | 20080331 | 20100929 | 20131106 | 5.60 | 8.239 – | 9.507 | 2.50/2388 | 3.10/1322 | 12 |
| C/1999 U4 | 4.92 | 19990918 | 20011028 | 20040411 | 4.56 | 7.552 – | 8.222 | 2.10/296 | 2.44/615 | 14 |
| C/2015 H2(*) | 4.97 | 20140519 | 20160913 | 20191022 | 5.43 | 7.964 – | 9.519 | 2.31/91 | 2.97/115 | 15 |
| C/2006 S3 | 5.13 | 19991013 | 20120416 | 20201124 | 21.1 | 26.1 – | 19.76 | 12.50/3183 | 8.60/3386 | 16 |
| 20060829 | 20180116 | 11.3 | 14.40 – | 14.64 | 5.63/3180 | 5.75/3370 | ||||
| C/2013 V4(*) | 5.19 | 20131023 | 20151007 | 20180806 | 4.79 | 7.352 – | 8.991 | 1.96/1370 | 2.82/1084 | 17 |
| C/2009 F4(*) | 5.45 | 20090319 | 20111231 | 20150820 | 6.41 | 8.956 – | 10.55 | 2.78/618 | 3.63/595 | 19 |
| 20150220 | 5.92 | 9.612 | 3.14/593 | |||||||
| C/2005 L3(*) | 5.59 | 20040716 | 20080116 | 20140109 | 9.48 | 10.30 – | 14.93 | 3.49/1559 | 5.96/3780 | 21 |
| C/2010 U3(*) | 8.44 | 20051105 | 20190226 | 20210318 | 15.36 | 25.75 – | 9.520 | 13.30/1882 | 2.05/599 | 32 |
| Sample LBg | ||||||||||
| C/2007 VO53 | 4.84 | 20071020 | 20100426 | 20120720 | 4.75 | 8.314 – | 7.759 | 2.44/296 | 2.20/417 | 13 |
| C/2016 A1 | 5.33 | 20160101 | 20171123 | 20200215 | 4.12 | 7.305 – | 7.896 | 1.89/974 | 2.22/1195 | 18 |
| C/1999 N4 | 5.50 | 19980827 | 20000523 | 20020506 | 3.69 | 7.143 – | 7.490 | 1.73/170 | 1.94/175 | 20 |
| C/2010 R1 | 5.62 | 20100904 | 20120518 | 20140330 | 3.57 | 7.154 – | 7.401 | 1.70/793 | 1.87/826 | 22 |
| C/2002 J5 | 5.73 | 20010806 | 20030919 | 20060305 | 4.58 | 7.869 – | 8.439 | 2.12/334 | 2.46/273 | 23 |
| C/1999 F1 | 5.79 | 19990313 | 20020213 | 20050828 | 6.46 | 9.281 – | 10.38 | 1.85/112 | 2.92/56 | 24 |
| C/2010 S1 | 5.90 | 20100921 | 20130520 | 20150719 | 4.82 | 8.850 – | 8.025 | 2.66/5260 | 2.16/3344 | 25 |
| C/2017 E3 | 5.92 | 20131214 | 20170631 | 20200620 | 6.52 | 10.28 – | 9.53 | 3.45/152 | 3.04/480 | 26 |
| C/2012 K8 | 6.46 | 20120530 | 20140819 | 20160608 | 4.02 | 8.396 – | 7.811 | 2.22/668 | 1.80/319 | 27 |
| C/2012 LP26 | 6.54 | 20120523 | 20150816 | 20181005 | 6.37 | 10.02 – | 9.865 | 3.23/196 | 3.14/246 | 28 |
| C/2015 XY1 | 7.93 | 20151204 | 20180502 | 20201020 | 4.88 | 9.525 – | 9.617 | 2.35/415 | 2.02/323 | 29 |
| C/2008 S3 | 8.01 | 20061227 | 20110603 | 20150717 | 8.55 | 12.36 – | 11.87 | 4.16/928 | 4.06/1025 | 30 |
| C/2015 D3 | 8.15 | 20130408 | 20160430 | 20200221 | 6.87 | 10.46 – | 11.92 | 3.06/163 | 3.78/151 | 31 |
Notes. We denote heliocentric distance as rh. The final column gives qori-number, the rank of the original perihelion distance, which we use in Figs. 7, 8 and 9. This order is not identical to the order in osculating perihelion distance because q changes for some comets during their passages through the planetary region. For instance, C/1980 E1 had an original perihelion distance of 3.17 au. Samples LAn and LBn include comets with determinable NG effects using astrometric data, where LAn includes comets with 3.1 au < q < 3.9 au and LBn those with q > 4.5 au. The third sample, LBg, includes comets with q > 4.5 au where NG effects are not determinable with sufficient accuracy. “PRE” means pre-perihelion data arc, while “POST” means post-perihelion data arc. The six comets marked with asterisks in samples LAn and LBn have NG effects determined for the first time by us. The two lines with different data arcs for C/2006 S3 and C/2009 F4 are described in the text.
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