PHOTOMETRY OF SYNCHRONOUS BINARY ASTEROID (8474) RETTIG PHOTOMETRY OF SYNCHRONOUS BINARY ASTEROID (8474) RETTIG IN 2015 V. G. Chiorny 1, Yu. N. Krugly 1, V. Benishek 2, P. Pravec 3, P. Kusnirak 3, A. Galad 3, J. Oye 4, R. Groom 4 V. Reddy 5, D. Pray 6, W. Cooney 7, J. Gross 7, R. Inasaridze 8, V. Aivazyan 8, V. Zhuzhunadze 8, D. Terrell 9, R. Montaigut 10, A. Leroy 10, I. Molotov 11 1 Institute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine 2 Belgrade Astronomical Observatory, Volgina 7, Belgrade 38, Serbia 3 Astronomical Institute, Academy of Sciences of the Czech Republic, Fricova 1, CZ Ondrejov, Czech Republic 4 Blue Mountains Observatory, Leura, NSW, Australia 5 Planetary Science Institute, Tucson, AZ 85719, USA 6 Sugarloaf Mountain Observatory, South Deerfield, MA 01373, USA 7 Sonoita Research Observatory, 77 Paint Trail, Sonoita, AZ 85637, USA 8 Kharadze Abastumani Astrophysical Observatory, Ilia State University, G. Tsereteli str. 3, Tbilisi 0162, Georgia 9 Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA 10 OPERA Observatory, Saint Palais, France 11 Keldysh Institute of Applied Mathematics, Russian Academy of Sciences, Miusskaya sq. 4, Moscow , Russia The 4th Workshop on Binaries in the Solar System Prague, Czech Republic 2016 June 21-23

Synchronous binary asteroids D 2 / D 1 = 0.8  1.0 Both components are approximately equal size  D 2 / D 1 = 0.8  1.0 P 1 = P 2 = P orb synchronous rotation  P 1 = P 2 = P orb Currently knows 14 similar objects : The biggest : (90) Antiope (MBA) D 1 ~ D 2 ~ 80 km (Merline W.J. et al., 2000) (617) Patroclus (Trojan) D 1 ~ D 2 = 120 km (Merline W.J. et al., 2001) The smallest: (69230) Hermes (NEA) D 1 ~ D 2 ~ 0.6 km (Margot J.-L. et al., 2003; Pravec P. et al.,2003) < The small main-belt asteroids (MBA) with D 1, D 2 < 13 km - 11 syncronous pairs (809) Lundia (Kryszczynska A. et al., 2005) ; (1139) Atami (Manzini F. et al., 2006); (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy (Behrend R. et al, 2006); (3905) Doppler (Franco L. et al., 2013) The Photometric Survey of Asynchronous Binary Asteroids : The Photometric Survey of Asynchronous Binary Asteroids (Pravec P., 2005) : (4951) Iwamoto (Reddy V. et al., 2007); (2478) Tokai (Higgins D. et al, 2007); (7369) Gavrilin (Higgins D. et al, 2008); (8474) Rettig (Chiorny V. et al., 2015)

Photometry of (8474) Rettig in 2015 Main-belt asteroid (8474) Rettig Orbital elements: Observational circumstances : a = AU 2015, May 18.8 – July 23.9 i = deg Phase angles – 29.0 deg e = Visual magnitude m – 16.6 m

Kharkiv Observatory (Ukraine) (founded in 1883) Pixels – 3326 x 2404 Pixel size – 5.4  m Sensor size – 17.9 x 13.5 mm Sensor Quantum Efficiency ~ 55 % The field of view – 21.5' x 16.2 ' 0.7 –meter reflector telescope CCD camera ML 8300 (FLI) Location : 36.94° E ; 49.62° N: Observatory code Newtonian fokus (f/4) Filter wheel CFW-1 (FLI) - VR (BI) – filters of the standard Jonson-Cousins photometric system

Photometry of (8474) Rettig in 2015 (Kryszczynska A. et al., 2009 ) Synchronous rotations of the components with the orbital period P orb = hours Amplitude of the combined primery and secondary rotational lihtcurve A 1 + A 2 = 0.34 mag at solar phases from 7 to 15 degrees Deep mutual eclipse/occultation events  m = 0.60 – 0.93 mag  m = 2.5 log (1 + k 2 ) k = D 2 / D 1 The ratio of mean diameters D 2 /D 1 ≥ 0.86 (809) Lundia in 2005

Photometry of (8474) Rettig in 2015 Standardization of photometric observations in the V and R-filters The measured color index V – R = 0.52 ± 0.02 The estimated mean absolute magnitude H R = ± 0.06 H V = ± 0.07 Log D(km) = – 0.2H V – 0.5 *Log(p V ) p V = 0.20 for S-type (Warner et al., 2009) D = D 1 (1 + k 2 ) 1/2 k = D 2 / D 1 The estimated mean diameters of components D 1 = 3.5 ± 0.9 km D 2 = 3.0 ± 0.8 km

The parameters of the small main-belt synchronous binary asteroids Asteroid D 1 (km) D 2 /D 1 D 2 (km) P orb (hr) A 1 + A 2 (mag) (8474) Rettig (7369) Gavrilin (4951) Iwamoto (4492) Debussi <0.48 (3905) Doppler (2478) Tokai 7, (1313) Berna (1139) Atami < 0.40 (1089) Tama <0.41 (854) Frostia (809) Lundia < 0.35 (Kryszczynska A. et al., 2005) (Behrend R. et al, 2006) (Manzini F. et al., 2006) (Reddy V. et al., 2007) (Higgins D. et al, 2007) (Higgins D. et al, 2008) (Franco L. et al., 2013) (Chiorny V. et al., 2015) D 1 and D 2 from (Warner B. et al., 2009), updated 2016

Summary Photometry of small main-belt asteroid (8474) Rettig – synchronous bynary system: 2015, May UT – July UT more than 2 months of observations 35 lightcurves Collaboration of 10 observatory, located in Europe, Australia and North America Physical parameters – Absolute magnitude H = mag Color index V – R = 0.52 mag The ratio of mean diameters D 2 / D 2 ≥ 0.86 Rotation period P 1 = P 2 = P orb = hours Amplitude A 1 + A 2 = 0.34 mag Diameters D 1 = 3.5 km ; D 2 = 3.0 km ; _

Discussion Abundance of synchronous binary asteroids : BinAst program - 4 synchronous 500) ( Joint program of Geneva Observatory - 4 synchronous < 1 % (N ~ 450) (Behrend R. et al., 2006) “ These binaries formed via rotational fission and so share a common parent body. If binaries are trapped in a long-term stable equilibrium, then binary creation could be infrequent. ” (Jacobson S.A. & Scheeres D.J., 2011) These objects are unique …??? … !!! “ Because these systems are doubly synchronous, there are strong biases against discovery; only mutual events reveal the presence of the satellite. Thus they are possibly significantly under-represented amongst known asteroid binaries. ” (Walsh K.J. & Jacobson S.A., 2016) (Jacobson S.A., 2014)

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