C/2005 L3 McNaught
more info
C/2005 L3 was discovered by Robert LH. McNaught with the 0.5-m Uppsala Schmidt in the course of the Siding Spring Survey on 3 June 2005 [IAUC 8536, 2005 June 7]. Later, prediscovery detections by Siding Spring Survey were found (16 July and 16 August 2004, see figure).
This comet made two closest approaches to the Earth on 24 June 2007 (4.852 au, almost seven months before perihelion) and 12 May 2008 (4.857 au, four months after perihelion).
Solution given here is based on data spanning over 8.7 yr (10 oppositions) in a range of heliocentric distances: 10.3 au – 5.593 au (perihelion) – 13.4 au. Currently, two more positions are available at the MPC (from 9 January 2014).
This Oort spike comet suffers rather small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.

solution description
number of observations 5337
data interval 2004 07 16 – 2013 03 05
data type perihelion within the observation arc (FULL)
data arc selection entire data set (STD)
range of heliocentric distances 10.3 au – 5.59 au (perihelion) – 13.4 au
detectability of NG effects in the comet's motion NG effects not determinable
type of model of motion GR - gravitational orbit
data weighting YES
number of residuals 10503
RMS [arcseconds] 0.49
orbit quality class 1a+
previous orbit elements (barycentric ecliptic J2000)
no. of returning VCs in the swarm 5001 *
no. of escaping VCs in the swarm 0
no. of hyperbolas among escaping VCs in the swarm 0
previous recip semi-major axis [10-6 au-1] 62.21 ± 0.12
previous perihelion distance [au] 53.339 ± 0.096
previous aphelion distance [103 au] 32.1 ± 0.1
time interval to previous perihelion [Myr] 2.017 ± 0.006
percentage of VCs with q > 20100
dynamical status definitely dynamically new (DN+)
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On stellar perturbations
Time distribution of positional observations with corresponding heliocentric (red curve) and geocentric (green curve) distance at which they were taken. The horizontal dotted line shows the perihelion distance for a given comet whereas vertical dotted line — the moment of perihelion passage.