The Uppsala-DLR Trojan Survey of the Preceding Lagrangian Cloud

Lagerkvist, C. I.; Mottola, S.; Carsenty, U.; Hahn, Gerhard; Doppler, A.; Gnädig, A.

doi:10.1007/10651968_27

Cited by 4 publications

(5 citation statements)

References 6 publications

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“…For Trojans, this is less than 10 day −1 (Lagerkvist et al 2000) close to opposition. All integrated data is given at midnight UT, so the position mismatch between integrations of an observation should be at most on the order of 5 day −1 due to the time resolution.…”

Section: Discussionmentioning

confidence: 94%

“…Palomar (code 675) is the site of the PLS, three follow-up surveys T-1, T-2, and T-3 (Marsden 1991(Marsden , 1989(Marsden , 1987, and additional observations (Shoemaker et al 1989;Shoemaker & Shoemaker 1990). The second site is La Silla (code 809), where ESO is located and the Uppsala-DLR Trojan survey was conducted in 1996, 1997, and 1998(Lagerkvist et al 2000, 2002.…”

Section: Introductionmentioning

confidence: 99%

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On the observational bias of the Trojan swarms

Karlsson¹

2010

A&A

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Aims. I investigate whether the Trojan swarms are observationally biased and place a completion limit on their absolute magnitude. Methods. Observations including Trojans from a number of observation sites are cross-checked with orbital integration of known Trojans and a set of fictitious Trojan orbits. Results. The completion limit for the Trojans swarms can be set to be H = 11.5 mag. The L 5 swarm is 71% of the L 4 size down to this limit. It is not likely that any existing set of orbital elements can have escaped detections. However, parts of the orbital element space, especially in the inclination, are biased for Trojans fainter than the completion limit. In the absolute magnitude interval 11.5−13 mag, 65% of new objects should have inclinations 15−40 • , while this inclination interval currently contains 49% of Trojans in the complete interval 9.5−11.5 mag. Trojans fainter than an absolute magnitude of 13 mag are also clearly biased in the ascending node at values coinciding with the Milky Way.

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Section: Discussionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

On the observational bias of the Trojan swarms

Karlsson¹

2010

A&A

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“…Recent attempts have been made to explain the absolute magnitude distributions of Trojans and their breaks in slope (Jewitt et al, 2000;Lagerkvist et al, 2002;Yoshida and Nakamura, 2005). Assuming a shared visual albedo (of 0.04), the magnitude distribution may be converted to a size distribution, as detailed by Jewitt et al (2000).…”

Section: Population Studiesmentioning

confidence: 99%

“…In a survey of the L4 Trojan cloud Lagerkvist et al (2002) observed 399 moving objects classified as Trojans. Using just numbered and multiopposition asteroids as of 2002, they note the average librational amplitude in the L and L 5 clouds as 15.45 0 and 14.45 0 , respectively.…”

Section: Observational Datamentioning

confidence: 99%

A centenary survey of orbits of co-orbitals of Jupiter

Stacey

Connors

2008

Planetary and Space Science

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Jupiter's Trojan asteroids fulfill the prediction of Lagrange that orbits can be stable when a small body orbits in specific locations relative to its 'parent' planet and the Sun. The first such Trojan asteroid was discovered slightly over one hundred years ago, in 1906, and subsequently similar asteroids have been discovered associated with Mars and with Neptune. To date no Trojans have been discovered associated with Earth, but several horseshoe asteroids, co-orbital asteroids moving along a large range of the Earth's orbit, have been found. Other planets also are not known to have Trojan-type asteroids associated with them. Since the number of detected Jupiter Trojans has increased dramatically in the last few years, we have conducted a numerical survey of their orbital motions to see whether any in fact move in horseshoe orbits. We find that none do, but we use the enlarged database of information about Trojans to summarize their properties as now known, and compare these to results of theory.

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“…In 1985, 1988Shoemaker et al (1989 searched both L 4 and L 5 . The Uppsala-DLR Trojan Survey (Lagerkvist et al 2000(Lagerkvist et al , 2002 of L 4 were made in 1996 (600 square degrees), 1997 (600 square degrees) and 1998 (1000 square degrees). Since about 1997 several large surveys for Near Earth Objects (NEO) have been running, and cover most of the northern sky each year.…”

Section: Introductionmentioning

confidence: 99%

Transitional and temporary objects in the Jupiter Trojan area

Karlsson¹

2004

A&A

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Abstract. I have integrated 1233 objects with semimajor axes between 4.6 and 5.8 AU 1000 years back and forward in time. A search for Jupiter horseshoe Trojans in transition from tadpole orbits to non-Trojan orbits and objects in temporary horseshoe orbits was made. A total of 13 objects (5 comets, 3 asteroids and 5 Trojans) were found. In a second group, among 337 new Trojans discovered after the primary investigation, 7 transitional candidates were found. Two objects, 2000 HR 24 and 2002 GP 31 , are falsely identified as Trojans. No likely transitional objects were found in the first object set, but all of them have at least temporary captures in orbit types associated with Jupiter's 1:1 mean motion resonance. Trojans in the first set have short observational arcs which can explain the low probability for a Trojan past. Trojans in the second set have longer arcs and 5 of them are good candidates for being in transition from the Trojan area.

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The Uppsala-DLR Trojan Survey of the Preceding Lagrangian Cloud

Cited by 4 publications

References 6 publications

On the observational bias of the Trojan swarms

On the observational bias of the Trojan swarms

A centenary survey of orbits of co-orbitals of Jupiter

Transitional and temporary objects in the Jupiter Trojan area

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