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The Pan-STARRS 1 Discoveries of Five New Neptune Trojans

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The Pan-STARRS 1 Discoveries of Five New Neptune Trojans The Pan-STARRS 1 discoveries of five new neptune trojans Lin, H. W., Chen, Y-T., Holman, M. J., Ip, W-H., Payne, M. J., Lacerda, P., Fraser, W. C., Gerdes, D. W., Bieryla, A., Sie, Z. F., Chen, W. P., Burgett, W. S., Denneau, L., Jedicke, R., Kaiser, N., Magnier, E. A., Tonry, J. L., Wainscoat, R. J., & Waters, C. (2016). The Pan-STARRS 1 discoveries of five new neptune trojans. Astronomical Journal, 152(5), [147]. https://doi.org/10.3847/0004-6256/152/5/147 Published in: Astronomical Journal Document Version: Publisher's PDF, also known as Version of record Queen's University Belfast - Research Portal: Link to publication record in Queen's University Belfast Research Portal Publisher rights © 2016 The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. Please refer to any applicable terms of use of the publisher. General rights Copyright for the publications made accessible via the Queen's University Belfast Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy The Research Portal is Queen's institutional repository that provides access to Queen's research output. Every effort has been made to ensure that content in the Research Portal does not infringe any person's rights, or applicable UK laws. If you discover content in the Research Portal that you believe breaches copyright or violates any law, please contact [email protected]. Download date:27. Sep. 2021 The Astronomical Journal, 152:147 (8pp), 2016 November doi:10.3847/0004-6256/152/5/147 © 2016. The American Astronomical Society. All rights reserved. THE PAN-STARRS 1 DISCOVERIES OF FIVE NEW NEPTUNE TROJANS Hsing Wen Lin (林省文)1, Ying-Tung Chen (陳英同)2, Matthew J. Holman3,4, Wing-Huen Ip (葉永烜)1,5, M. J. Payne4, P. Lacerda6, W. C. Fraser6, D. W. Gerdes7, A. Bieryla4, Z.-F. Sie (謝宗富)1, W.-P. Chen (陳文屏)1, W. S. Burgett8, L. Denneau8, R. Jedicke8, N. Kaiser8, E. A. Magnier8, J. L. Tonry8, R. J. Wainscoat8, and C. Waters8 1 Institute of Astronomy, National Central University, 32001, Taiwan; [email protected] 2 Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 106, Taiwan 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4 Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5 Space Science Institute, Macau University of Science and Technology, Macau 6 Astrophysics Research Centre, Queen’s University Belfast, BT7 1NN, Northern Ireland, UK 7 Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA 8 Institute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USA Received 2016 June 2; revised 2016 September 14; accepted 2016 September 14; published 2016 October 31 ABSTRACT In this work, we report the detection of seven Neptune Trojans (NTs) in the Pan-STARRS 1 (PS1) survey. Five of these are new discoveries, consisting of four L4 Trojans and one L5 Trojan. Our orbital simulations show that the L5 Trojan stably librates for only several million years. This suggests that the L5 Trojan must be of recent capture origin. On the other hand, all four new L4 Trojans stably occupy the 1:1 resonance with Neptune for more than 1 Gyr. They can, therefore, be of primordial origin. Our survey simulation results show that the inclination width of the NT population should be between 7° and 27° at >95% confidence, and most likely ∼11°. In this paper, we describe the PS1 survey, the Outer Solar System pipeline, the confirming observations, and the orbital/physical properties of the new NTs. Key words: Kuiper belt: general – minor planets, asteroids: general – surveys 1. INTRODUCTION chaotic capture of small bodies at the two Lagrangian points of Jupiter during the planetary migration phase. Following a The best-known Trojans are the asteroids in a co-orbital 1:1 similar approach, Nesvorný & Vokrouhlický (2009) produced a mean motion resonance with Jupiter. Those in stable libration model calculation of the capture process of NTs. Although the around the Lagrange point 60° ahead of Jupiter are called L4 inclinations of the objects captured from the thin solar nebula Trojans, and those around the Lagrange point 60° behind are disk could be later increased by dynamical processes, the called L5 Trojans. There are more than 6000 known Jovian numerical results could not account for the 4:1 high-i to low-i Trojans with sizes 10 km. Yoshida & Nakamura (2005) NT ratio indicated by the observations of Sheppard & Trujillo estimated that the total number of 1 km sized Jovian Trojans (2006). This discrepancy might be worsened if the orbits of the could be as many as 600,000. After Jupiter, Neptune has the planetesimals before chaotic capture were excited by the second-largest population of Trojans. Prior to this study, nine gravitational scattering effect of a population of Pluto-sized L4 Neptune Trojans (or NTs) and three L5 NTs had been objects, according to these authors. discovered (Elliot et al. 2005; Sheppard & Trujillo 2006, Parker (2015) applied a statistical method to debias the 2010b; Parker et al. 2013; Alexandersen et al. 2014; Gerdes ) observed distributions of orbital inclinations, eccentricities, and et al. 2016 . libration amplitudes of NTs. His treatment confirmed the Nesvorný & Dones (2002) examined the orbital evolution existence of the thick-cloud population with σi>11°. Here σi and long-term stability of Trojans of Saturn, Uranus, and ( fi is the inclination width of the Brown distribution Brown Neptune, under the current planetary con guration. They found 2001): that unlike the cases of Saturn and Uranus, where their Trojans could be removed on relatively short timescales, the primordial ⎛ ⎞ ⎜⎟1 2 population of NTs can survive to the present time after their pi()=-sin () i exp ( isi ) di.1 ( ) ⎝ 2 ⎠ formation. Subsequently, the first NT, 2001 QR322 at L4, was found in the Deep Ecliptic Survey (Elliot et al. 2005). Based on From a numerical study of the resonant capture effect via the low inclination (∼1°.3) of 2001 QR322 with a size of ∼100 planetary orbital migration, Parker (2015) showed that low- km, Chiang & Lithwick (2005) proposed that large (∼100 km inclination objects can be captured into high-inclination NTs, sized) NTs might be primordial objects formed in situ by but the conversion efficiency is too low to account for the accretion in a thin disk. This means that NTs should generally presence of the high-inclination population. On the other hand, have i10°. Following the discovery of three more NTs, one if the original planetesimals were characterized by high- of which has a high inclination (see Table 1, with a list of the inclination orbits, their NT counterparts captured into 1:1 known NTs and those detected in this study), Sheppard & resonance with Neptune could preserve their high inclinations Trujillo (2006) suggested that a thick cloud of high-inclination and hence cause the formation of a thick NT cloud. NTs, which could be of capture origin, should exist with a 4:1 Chen et al. (2016) provided an alternative mechanism to ratio over the low-inclination population. effectively form the high-inclination NTs. They investigated In the context of the Nice model (Gomes et al. 2005; how planetary migration affects the orbital elements’ distribu- Tsiganis et al. 2005), Morbidelli et al. (2005) investigated the tion of NTs and found that if orbital eccentricities and 1 The Astronomical Journal, 152:147 (8pp), 2016 November Lin et al. Table 1 Barycentric Oscillating Orbital Elements of PS1-detected and Known NTs Peri. PS1 Name a (au) ei(deg) Ω (deg) ω (deg) Date (JD) Epoch (JD) HL Detected βa λb 2001 QR322 30.233 0.0285 1.323 151.636 158.76 2444677 2452142.8 7.9 L4 yes 21.85 −1.05 c 2004 KV18 30.353 0.189 13.573 235.593 295.733 2446125.4 2453351.5 8.9 L5 LLL 385571 Otrera 30.184 0.027 1.431 34.780 358.452 2457945.4 2454668.5 8.8 L4 LLL (2004 UP10) 385695 (2005 TO74) 30.137 0.051 5.253 169.387 304.750 2470616.8 2454522.5 8.3 L4 LLL 2005 TN53 30.171 0.064 24.988 9.278 85.892 2467102.2 2454775.5 9.0 L4 LLL 2006 RJ103 30.038 0.0300 8.163 120.867 27.26 2475056 2453626.8 7.5 L4 yes 28.12 −8.42 2007 VL305 30.004 0.062 28.125 188.611 215.518 2456036.1 2454566.5 7.9 L4 LL 2008 LC18 30.090 0.079 27.489 88.528 6.845 2427000.1 2454759.5 8.4 L5 LLL 2010 TS191 30.006 0.0457 6.563 129.600 299.5 2460637 2455476.9 7.9 L4 yes 36.07 −6.76 2010 TT191 30.094 0.0701 4.276 249.295 7.8 2429839 2454419.0 7.9 L4 yes 54.76 1.18 2011 HM102 30.119 0.081 29.389 100.993 152.287 2452480.3 2455758.5 8.1 L5 LLL 2011 SO277 30.161 0.0118 9.639 113.528 117.7 2431675 2455831.0 7.6 L4 yes 16.19 −9.87 2011 WG157 30.031 0.0278 23.299 352.165 215.3 2482896 2455885.8 7.0 L4 yes 41.95 18.06 2012 UV177 30.175 0.074 20.811 265.753 200.784 2467673.8 2456131.5 9.2 L4 LLL 2013 KY18 30.149 0.123 6.659 84.397 271.2 2471956 2456429.0 6.6 L5 yes 249.82 1.79 2014 QO441 30.104 0.105 18.824 107.110 113.897 2429010.4 2456910.5 8.3 L4 LL 2014 QP441 30.0785 0.067 19.394 96.626 2.639 2467286.1 2456979.5 9.3 L4 LL Notes.
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