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New Binary Asteroid 809 Lundia I

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New Binary Asteroid 809 Lundia I A&A 501, 769–776 (2009) Astronomy DOI: 10.1051/0004-6361/200809877 & c ESO 2009 Astrophysics New binary asteroid 809 Lundia I. Photometry and modelling A. Kryszczynska´ 1,F.Colas2, P. Descamps2, P. Bartczak1,M.Polinska´ 1, T. Kwiatkowski1, J. Lecacheux3, R. Hirsch1, M. Fagas1,K.Kaminski´ 1,T.Michałowski1, and A. Marciniak1 1 Astronomical Observatory, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznan,´ Poland e-mail: [email protected] 2 Institut de Mécanique Céleste et Calcul des Ephemerides, Observatoire de Paris, UMR8028 CNRS, 77 Av. Denfert Rochereau, 75014 Paris, France 3 Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon, France Received 31 March 2008 / Accepted 23 February 2009 ABSTRACT CCD photometry of 809 Lundia obtained between September 2005 and January 2006 at Borowiec and Pic du Midi Observatories demonstrates that this object is a synchronous binary system with an orbital period of 15.418 ± 0.001 h. In this paper, we present the results of photometric observations of Lundia from two oppositions in 2005/2006 and 2007, as well as the first modelling of the system. For simplicity we assumed a fluid-like nature for each component with a modified Roche model and a triaxial ellipsoid shape in kinematic models. Our models provided similar results. Poles of the orbit in ecliptic coordinates are λ = 119 ± 2◦, β = 28 ± 4◦ (modified Roche) or λ = 120 ± 5◦, β = 18 ± 12◦ (kinematic). Triaxial ellipsoid shape solutions and a separation between components of 15.8 km are given after taking an equivalent diameter of 9.1 km from H = 11.8 mag and assuming an albedo of 0.4. The orbital period of the Lundia system obtained from modelling is the same as from the lightcurve analysis i.e., 15.418 ± 0.001 h. The bulk density of both components is 1.64 or 1.71 ± 0.01 g/cm3. The double system of Lundia probably originates from the fission process of a single body that could have been spun up by the YORP effect. The predicted lightcurves for future oppositions are also presented. Key words. planets and satellites: formation – minor planets, asteroids – techniques: photometric 1. Introduction binaries, showing that thermal radiation can affect orbits of syn- chronous asteroidal satelites. Vokrouhlicky et al. (2005) studied 809 Lundia was discovered by Wolf at Heidelberg in the possibility of detection of the-long term Yarkovsky perturba- August 1915 and named after the city and Observatory of Lund tion in the relative motion of two components of binary system (Sweden). The parameters of the orbit of Lundia allow us to clas- and concluded that it is detectable for the well-studied systems. sify this object using hierarchical clustering method (HCM) to However, their studies also concentrated on binary NEAs. the Flora dynamical family, although it is not a member of the In this paper, we present CCD photometry of 809 Lundia Flora/Ariadne family according to the wavelet analysis method and a description of observing techniques and data reduction. (WAM) (Zappala et al. 1995). The modelling of the system using two different methods is also The old Flora family was detected by Mothe-Diniz et al. presented. In the second paper, we present the results of spectro- (2005) as the nominal Baptistina family plus a lot of small scopic observations of the Lundia system. clumps and background asteroids that eventually merge together at a different cutoff. However, they also merge with the Vesta family. In this classification, Lundia belongs to the background 2. Photometric observations of the Baptistina and Vesta families. 809 Lundia was observed within an ongoing program of obser- Its spectra at visible wavelengths observed on 26 and vations of the Flora region. In this paper, we present lightcurves 27 May 2001 allows us to identify Lundia as a V-type ob- from 22 nights from two oppositions in 2005/2006 and 2007 at ject outside the Vesta dynamical family (Florczak et al. 2002). Borowiec and Pic du Midi observatories. The aspect data for Carruba et al. (2005) investigated the possibility of the migration Lundia are listed in Table 1, the individual columns of which of 809 Lundia and 956 Elisa from the Vesta family to their cur- provide dates of observations with respect to the middle of rent positions by the interplay of the Yarkovsky effect and non- the lightcurve, the asteroid’s distances to the Sun (r)andthe linear secular resonances. However, they assumed single bodies. Earth (Δ) in AU, phase angle (α), ecliptic longitude (λ) and lati- We now know that Lundia is a binary system, but we do not tude (β) for J2000.0, and the observatory, i.e., Bor for Borowiec, know how Yarkovsky/YORP effects or resonances influence bi- and Pic for Pic du Midi. naries in the main belt. The effect called BYORP (Binary YORP) First photometric data were obtained on Sept. 18. 2005, al- was studied by Cuk´ & Burns (2005) for NEAs synchronous most two months before opposition on November 5.8, showing Article published by EDP Sciences 770 A. Kryszczynska´ et al.: New binary asteroid 809 Lundia – photometry and modelling 18 - 26 September 2005, Borowiec Table 1. Aspect data. 1 r Δ Phase λβObservatory P = 15.418 h Date (UT) angle (J2000) ◦ ◦ ◦ (AU) (AU) ( )()() 1,5 2005 Sep. 18.04 1.894 1.133 25.9 50.1 –9.1 Bor 2005 Sep. 19.04 1.985 1.126 25.6 50.2 –9.2 Bor 2005 Sep. 24.04 1.901 1.095 23.9 50.4 –9.8 Bor 2005 Sep. 25.02 1.903 1.089 23.5 50.4 –9.9 Bor 2 2005 Sep. 26.10 1.904 1.083 23.1 50.4 –10.1 Bor 2005 Oct. 11.03 1.925 1.012 16.6 49.3 –11.7 Bor Relative Magnitude 2005 Oct. 12.04 1.927 1.008 16.1 49.2 –11.8 Bor 2,5 2005 Oct. 13.07 1.929 1.005 15.6 49.0 –11.9 Bor 18 Sep, C filter 19 Sep, C filter 2005 Oct. 16.04 1.933 0.997 14.2 48.5 –12.2 Bor 24 Sep, C filter 25 Sep, C filter 2005 Oct. 27.88 1.952 0.981 8.7 45.9 –13.0 Bor 26 Sep, C filter 2005 Oct. 31.10 1.958 0.982 7.6 45.0 –13.2 Bor Zero Phase at 2005 Sep 18.8490 UT 3 2005 Nov. 01.05 1.960 0.983 7.3 44.8 –13.2 Bor 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 2005 Nov. 21.00 1.998 1.054 11.5 39.7 –13.2 Pic Orbital Phase 2005 Nov. 22.94 2.000 1.059 11.9 39.6 –13.1 Pic Fig. 1. Composite lightcurve of 809 Lundia from September 2005 data, 2005 Dec. 15.89 2.045 1.247 20.8 37.6 –11.7 Pic zero phase corrected for light-time. 2005 Dec. 18.94 2.052 1.279 21.7 37.7 –11.5 Pic 2005 Dec. 19.88 2.054 1.289 21.9 37.8 –11.4 Pic 2006 Jan. 23.85 2.129 1.720 27.1 44.1 –8.8 Pic October, November 2005, Borowiec 2006 Jan. 24.85 2.131 1.734 27.1 44.4 –8.7 Pic -0,5 2006 Dec. 21.17 2.691 2.422 21.4 174.2 –0.3 Pic P = 15.418 h 2007 Jan. 19.15 2.708 2.053 17.9 176.6 0.6 Pic 2007 Jan. 20.15 2.708 2.042 17.7 176.6 0.7 Pic 0 Observatory code: Bor – Borowiec, Pic – Pic du Midi. a deep minimum in the lightcurve and suggesting that this object 0,5 could be a binary system. We continued observations of Lundia on 9 consecutive nights using our 0.4 m telescope equipped Relative Magnitude with KAF 400 CCD and clear filter, finally obtaining a typical 1 11 Oct, C filter 12 Oct, C filter lightcurve of a synchronous binary asteroid (Kryszczynska´ et al. 13 Oct, C filter 16 Oct, C filter 2005), similar to 90 Antiope (Hansen et al. 1997; Michałowski 27 Oct, C filter 31 Oct, C filter et al. 2002, Micha04b; Descamps et al. 2007a), 854 Frostia, Zero Phase at 2005 Oct 11.9821 UT 1 Nov, C filter 1,5 1089 Tama, 1313 Berna, 4492 Debussy (Behrend et al. 2006), 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 and Trojan asteroid 617 Patroclus (Marchis et al. 2006). All Orbital Phase CCD frames from Borowiec were reduced with the CCLR Fig. 2. Composite lightcurve of 809 Lundia from October 2005 data, STARLINK package. Corrections for bias, dark current, and flat- zero phase corrected for light-time. fielding were applied and aperture photometry was used to mea- sure the instrumental brightness of the asteroid, and the compari- son and check star. Details concerning instrument and reduction procedure were described by Michałowski et al. (2004a). The composite lightcurve of Lundia from September 2005 is pre- 2 nights in November 2005 is presented in Fig. 3 and shows sented in Fig. 1. The vertical shift in each lightcurve was com- a total amplitude of 1.0 mag, 0.65 mag for the eclipsing and pleted by minimizing the dispersion in the data points. The 0.35 mag for the rotational components. This lightcurve has lightcurve of total amplitude 1.1 mag consists of two compo- a feature visible close to the maximum of brightness (around nents.
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