1. NEAR-EARTH ASTEROID PHOTOMETRY IN FRAME OF ISON PROJECT: DETECTION OF BINARIES
Yu. Krugly1, I. Molotov2, R. Inasaridze3, V. Aivazyan3, O. Kvaratskhelia3, V. Zhuzhunadze3, I. Belskaya1, V. Chiorny1, T. Hromakina1, A. Sergeyev1, V. Shevchenko1, I. Slyusarev1, V. Rumyantsev4, Sh. Ehgamberdiev5, O. Burkhonov5, L. Elenin2, V. Voropaev2, V. Kouprianov6, M. Krugov7, A. Kusakin7, I. Reva7, N. Gaftonyuk4, A. Baransky8, Z. Donchev9, G. Borisov9, T. Irsmambetova10, A. Matkin11, D. Erofeev11, S. Schmalz12, T. Namkhai13, A. Wolf14, V. Kashuba15, V. Troianskyi15
The 4th Workshop on Binaries in the Solar System
Prague, Czech Republic
2016 June 21-23

2. ISON OBSERVATORIES Chuguev Observatory, Kharkiv, Ukraine
Keldysh Institute of Applied Mathematics, Moscow, Russia
Kharadze Abastumani Observatory, Tbilisi, Georgia
Crimean Astrophysical Observatory, Nauchny, Crimea
Maidanak Observatory, Tashkent, Uzbekistan
Pulkovo Observatory, St.-Petersburg, Russia
Tien-Shan Observatory, Almaty, Kazakhstan
Lisnyky Observatory, Kyiv, Ukraine
Rozhen Observatory, Sofia, Bolgaria
Sternberg Astronomical Institute, Moscow, Russia
ISON-Ussuriysk Observatory, Russia
Leibniz Institute for Astrophysics, Potsdam, Germany
Huraltogoot Observatory, Ulan-Bator, Mongolia
Altai State Pedagogical University, Barnaul, Russia
Mayaki Observatory, Odessa, Ukraine

3. INTERNATIONAL SCIENTIFIC OPTICAL NETWORK (ISON)
Started in 2004, currently the project involves more than 30 observatories and scientific institutions in 15 countries: Russia, Ukraine, Moldova, Georgia, Uzbekistan, Tajikistan, Kazakhstan, Italy, USA, Bolivia, Armenia, Switzerland, Spain, Mongolia, Mexico.
There are more than 70 telescopes in the network.
The work is a part of long-term agreements on a scientific and technical cooperation between the Keldysh Institute of Applied Mathematics (KIAM, Moscow) and scientific or educational organizations, using both their own instruments (telescopes) in the possession of the organization, as well as instruments provided by the ISON project.

4. WORLD OF ISON

5. THE NETWORK AIMS
Monitoring of space debris by means of carrying out astrometric and photometric observations of Earth-orbiting objects
Tracking of near-Earth asteroids (NEAs):
to discover and refine orbital parameters;
to study physical properties of NEAs
The ISON facilities:
18 telescopes of m
3 telescopes of 1 m
1.5 m and 2.6 m telescopes

6. ASTEROID PHOTOMETRY
The telescopes with diameters from 40 cm up to 2.6 m have been modernized and used in the network for carrying out photometry of asteroids. Most of these telescopes have been equipped with modern CCD cameras, mainly manufactured by the firm Finger Lakes Instrument (USA).

7. GOALS OF ASTEROID PHOTOMETRY
Physical characteristics of Near-Earth Asteroids
Observations of Potentially Hazardous Asteroids (PHAs), especially newly discovered NEAs
Search for binary asteroids and determination of parameters of binary systems
Investigation of the YORP effect: detection of the influence on asteroid’s rotation
Support of radar observations of NEAs by optical observations

8. Binary Asteroids Observed in 2013-…
Orbit
Type H
mag
Diameter Km
Albido
Rot. Period
hrs Q
Ampl
4034 Vishnu (r)
Аполлон O
18.4
0.42
0.52
~15.46
2,N
> 0.3
UCB (r)
U;S
15.1
2.72
0.18
± ;
P2 ~ 51.2 h ± 0.2
3!, B-N
0.09;
0.2
WC2 (r) -
16.5
5.063 ± 0.001
0.43
PM8 (r)
Амур
14.6
6.805h ± 0.003
CV26B(r) Sq
16.4
0.26 ±
P2~16..25h(19.7;25.)
0.17; min=0.04
CF9 (r)
18.0
0.9
~ 7
~0.55
YK5
Атон
X;RQ
16.60
1.5
3.468h ±0.008
0.12
GTB (r) S
18.5
3.764 ± 0.002
0.36
AU4
19.30
> 6
> 1.1
QE2B (r) Ch
16.98
2.75
0.06 ±
0.19
OA22 (r)
19.4
2.6211h ±
0.20
AO4
15.5 ±
0.32

9. RESULTS OF PHOTOMETRY
About 190 NEAs were observed in , among them 18 were binaries,
about 30 NEAs had been suspected to be binary, signs of possible binarity for 7 of them were actually found

10. (8373) STEPHENGOULD 2010 OPPOSITION
Mars-crosser from Hecuba group: Kirkwood gap at the 2:1 mean motion resonance with Jupiter;
unstable asteroids with lifetime <10 Myr
2010 OPPOSITION
i = 40.77°
e = 0.55
a = 3.28 AU
q = 1.47 AU
Q = 5.10 AU
Porb = 5.95 yr
H = 14.64
D = 3-6 km
ASTEROID
TAX.
CLASS D1
(km) P1
(hrs) A1
(mag)
D1/D2
R/D1
(ρ=1/2) P2
YEAR
8373 Stephengould
(EMP)
3.86
4.435
>0.27
2/3
34.1
2010

11. (8373) STEPHENGOULD
On Jan.17-18, 2010 two binary evens have been registered and orbital period was estimated as results of observations at Chuguev Observatory (Ukraine)

12. (8373) STEPHENGOULD
BinAstSurvey observations
Evens on Jan.17-27, 2010

13. (8373) STEPHENGOULD
March-June 2010: NO EVENTS FOUND

14. (8373) STEPHENGOULD in 2014
Previously the asteroid was observed in Jan by Brian Warner
In 2010 new analysis of the data showed one event on Jan. 09, 2004

15. (8373) STEPHENGOULD in 2015-2016 Jan. - Feb. 2016 Nov. - Dec. 2015
Apr. 2016
May 2016

16. (2001 WL15)
H = 18.8; Sk-type (Binzel et al. 2004); D = 530 m
Radar target at Arecibo in Dec 2015-Jan 2016
Asteroid was observed at Abastumani Observatory in March 2016
Short-period lightcurve
Long-period component

17. 337866 (2001 WL15) Observed by Hicks (2016): published in
The Astronomer’s Telegram
Long period could be connected
with binary nature
Warner informed about
the rotation period hrs

18. 163246 (2002 GT) Chesley et al. (2013) informed about
indication that it might be a binary system
from its photometry in April 2013.

19. 2002 GT campaign in frame of Gaia-FUN-SSO June - July 2013
NEA 2002 GT is a target of the Deep Impact spacecraft (flyby on Jan. 2020).
585 Lisnyky: Jun 10, 24-25
095 Nauchny: Jun 10-11
094 Simeiz: Jun 12-13, 20; Jul 12
119 Abstumani: Jun 19-20, 30
121Chuguev: Jun 19
190 Gissar: Jul 04
188 Maidanak: Jul 5

20. 2013 TV135 October-December 2013
119 Abastumani: Oct 21-22, 24-25; Dec 4
121 Chuguev: Oct 23;
H15 ISON-NM: Oct 17, 19, 22, 24, 27

21. SUMMARY We made many follow-up observations of known NEA binaries.
We should continue the observations trying to improve them by using more telescopes, especially more telescopes of larger apertures, located in different observatories.
Search of a binary among NEAs is very time-consuming, and requires better cooperation between observatories around the world.

22. ACCURACY OF PHOTOMETRY
The lightcurves example: NEA (3554) Amun observed in the network
V=16 mag, RMS = 0.03 mag
V=16 mag, RMS = 0.02 mag
V= 14 mag, RMS = mag
V= 15 mag, RMS = 0.01 mag
The typical accuracy is mag and no worse than mag.