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Table A.2

Near-parabolic comets split when they were close to perihelion, or objects that have ceased to be observed soon after perihelion passage.

Comet qosc T Observational arc No of Data Heliocentric Data Q* New rms [arcsec] Ref Data Preffered 1∕aori 1∕afut
name dates obs. span distance span type GR NG orbital /no of and selec solution? [10−6au−1]
[au] [yr] [au] class res. Notes tion
[1] [2] [3] [4] [5] [6] [7] [8] [9] [10] [11] [12] [13] [14] [15] [16] [17]
C/1999 S4 0.765 a5 20000726 19990927–20000731 1294 0.841 4.33–0.773 pre+ 7.5 1a 0.85/2567 new STD NO 17.20± 0.86 perished (1)
LINEAR n5 6.5 1b 0.34/2562 new STD NO 25.37± 0.97
a7 19990927–20000705 1116 0.770 4.33–0.861 pre+ 7.5 1a 0.63/2223 new PRE NO −0.30± 1.34
n7 6.5 1b 0.57/2221 new PRE YE1 6.24± 1.67
19990927–20000722 1070 0.816 4.33–0.768 pre GR 0.70 MPC PRE −54.51 1512.9

Notes. Preferred models are marked in Col. [15] as “YES”/“’YOS” (orbit based on full data-arc), where preferred NG solution based on g(r)-like function describing CO sublimation is marked as “YOS”, or as “YE1”/“YE2” (for orbit based on pre-perihelion or post perihelion data arc, respectively). An asterisk in Col. [11] indicates asymmetric NG solution. The last row for each comet presents data used inthe Minor Planet Center and Nakano Notes (if existing) for orbit determination and resulting original and future 1∕a (taken from these websites in March–June 2019). The observational material taken for osculating orbit determination is described in Cols. [4]−[8] and [12], whereas Cols. [9] and [10] give Q* for GR and NG model of motion, respectively, and the resulting orbit quality assessment (orbital class) is given in Col. [11]. The second and third columns show an osculating perihelion distance and perihelion time. The data distribution relative to a perihelion passage is presented in Cols. [7] and [8], where “pre” means that all observations were taken before the perihelion passage, “pre+” means that considerably more pre-perihelion measurements were available, and additional “+” means a drastic dominance of data before perihelion. Columns [13], [16], and [17] are explained in Table A.1. (1)See Sekanina (2019). The full table is available at the CDS.

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