1509 Esclangona , provisional designation 1938 YG , is a rare-type Hungaria
asteroid and
binary system from the inner regions of the
asteroid belt , approximately 8 kilometers in diameter. It is named after French astronomer
Ernest Esclangon .
Discoveries
Esclangona was discovered on 21 December 1938, by French astronomer
André Patry at
Nice Observatory . The body's
observation arc begins with its official discovery observation as no
precoveries were taken, and no prior identifications were made.
[3] On 13 February 2003, a
minor-planet moon in orbit of Esclangona was discovered by astronomers at ESO's
Very Large Telescope (UT4) on
Cerro Paranal in Chile.
[2]
[3]
Orbit and classification
Esclangona is a member of the
Hungaria family , which form the innermost concentration of asteroids in the
Solar System . It orbits the Sun in the
inner main-belt at a distance of 1.8–1.9
AU once every 2 years and 7 months (931 days). Its orbit has an
eccentricity of 0.03 and an
inclination of 22
° with respect to the
ecliptic .
[1]
Binary system
Esclangona has a small
moon , provisionally named S/2003 (1509) 1 , which measures 4 kilometers in diameter, and orbits 140 kilometers from its parent. This wide separation relative to the pair's size is rather unusual and it is believed that both Esclangona and its moon are
ejecta from an asteroidal collision in the past that left the scene as a co-orbiting pair; a similar pairing is
3749 Balam and its moon.
[6]
Physical characteristics
In the
Tholen taxonomy, Esclangona is a common stony
S-type asteroid . It has since been characterized as a rare
K-type asteroid by polarimetric observations.
[19]
Rotation period
In December 2004,
photometric measurements of Esclangona made by American astronomer
Brian Warner at his Palmer Divide Observatory, California, showed a
lightcurve with a
rotation period of 3.247± 0.002 hours and a brightness variation of 0.17± 0.02 in
magnitude .
[13]
[a]
Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite
IRAS , the Japanese
Akari satellite, and NASA's
Wide-field Infrared Survey Explorer with its subsequent
NEOWISE mission, Esclangona measures between 6.83 and 9.87 kilometers in diameter and its surface has an
albedo between 0.107 and 0.41.
[7]
[8]
[9]
[11] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2041 and a diameter of 8.18 kilometers with an
absolute magnitude of 12.858.
[4]
Naming
This
minor planet was named after French astronomer
Ernest Esclangon (1876–1954), was a director of the
Paris Observatory and president of the
International Astronomical Union . Naming citation was first mentioned in
The Names of the Minor Planets by
Paul Herget in 1955 (
H 134 ).
[2]
Notes
References
^
a
b
c
d
e
f
g
h
"JPL Small-Body Database Browser: 1509 Esclangona (1938 YG)" (2016-08-27 last obs.).
Jet Propulsion Laboratory . Retrieved 30 June 2017 .
^
a
b
c Schmadel, Lutz D. (2007). "(1509) Esclangona". Dictionary of Minor Planet Names – (1509) Esclangona .
Springer Berlin Heidelberg . p. 120.
doi :
10.1007/978-3-540-29925-7_1510 .
ISBN
978-3-540-00238-3 .
^
a
b
c
"1509 Esclangona (1938 YG)" . Minor Planet Center . Retrieved 8 April 2017 .
^
a
b
c
d
e
f
"LCDB Data for (1509) Esclangona" . Asteroid Lightcurve Database (LCDB). Retrieved 8 April 2017 .
^ Spratt, Christopher E. (April 1990).
"The Hungaria group of minor planets" . Journal of the Royal Astronomical Society of Canada . 84 : 123–131.
Bibcode :
1990JRASC..84..123S .
ISSN
0035-872X . Retrieved 8 April 2017 .
^
a
b Merline, W. J.; Close, L. M.; Dumas, C.; Chapman, C. R.; Menard, F.; Tamblyn, P. M.; et al. (May 2003).
"Discovery of new asteroid binaries (121) Hermione and (1509) Esclangona" . American Astronomical Society . 35 : 972.
Bibcode :
2003DPS....35.3106M . Retrieved 8 April 2017 .
^
a
b
c
d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015).
"NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos" . The Astrophysical Journal . 814 (2): 13.
arXiv :
1509.02522 .
Bibcode :
2015ApJ...814..117N .
doi :
10.1088/0004-637X/814/2/117 .
S2CID
9341381 . Retrieved 8 April 2017 .
^
a
b
c
d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016).
"NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos" . The Astronomical Journal . 152 (3): 12.
arXiv :
1606.08923 .
Bibcode :
2016AJ....152...63N .
doi :
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^
a
b
c
d Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004).
"IRAS Minor Planet Survey V6.0" . NASA Planetary Data System . 12 : IRAS-A-FPA-3-RDR-IMPS-V6.0.
Bibcode :
2004PDSS...12.....T . Retrieved 22 October 2019 .
^
a
b
c
d Marchis, F.; Enriquez, J. E.; Emery, J. P.; Mueller, M.; Baek, M.; Pollock, J.; et al. (November 2012).
"Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations" . Icarus . 221 (2): 1130–1161.
arXiv :
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Bibcode :
2012Icar..221.1130M .
doi :
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hdl :
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^
a
b
c
d Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan . 63 (5): 1117–1138.
Bibcode :
2011PASJ...63.1117U .
doi :
10.1093/pasj/63.5.1117 . (
online ,
AcuA catalog p. 153 )
^ Behrend, Raoul.
"Asteroids and comets rotation curves – (1509) Esclangona" .
Geneva Observatory . Retrieved 8 April 2017 .
^
a
b Warner, Brian D. (September 2005).
"Asteroid lightcurve analysis at the Palmer Divide Observatory - winter 2004-2005" . The Minor Planet Bulletin . 32 (3): 54–58.
Bibcode :
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ISSN
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^ Warner, Brian D. (July 2013).
"Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2013 January - March" . The Minor Planet Bulletin . 40 (3): 137–145.
Bibcode :
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ISSN
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^ Polishook, D.; Brosch, N.; Prialnik, D.; Kaspi, S. (January 2009).
"Simultaneous spectroscopic and photometric observations of binary asteroids" . Meteoritics and Planetary Science . 44 (12): 1955–1966.
arXiv :
0909.0512 .
Bibcode :
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doi :
10.1111/j.1945-5100.2009.tb02005.x .
S2CID
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^ Polishook, D.; Brosch, N.; Prialnik, D. (March 2011).
"Rotation periods of binary asteroids with large separations - Confronting the Escaping Ejecta Binaries model with observations" . Icarus . 212 (1): 167–174.
arXiv :
1012.4810 .
Bibcode :
2011Icar..212..167P .
doi :
10.1016/j.icarus.2010.12.020 .
S2CID
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^ Warner, Brian D.; Pravec, Petr; Kusnirak, Peter; Hornoch, K.; Harris, Alan; Stephens, Robert D.; et al. (April 2010).
"A Trio of Hungaria Binary Asteroids" . The Minor Planet Bulletin . 37 (2): 70–73.
Bibcode :
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ISSN
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^ Gil-Hutton, R.; Lazzaro, D.; Benavidez, P. (June 2007).
"Polarimetric observations of Hungaria asteroids" . Astronomy and Astrophysics . 468 (3): 1109–1114.
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doi :
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hdl :
11336/213855 .
^
a
b Belskaya, I. N.; Fornasier, S.; Tozzi, G. P.; Gil-Hutton, R.; Cellino, A.; Antonyuk, K.; et al. (March 2017).
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hdl :
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^ Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012).
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External links