1188 Gothlandia

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1188 Gothlandia
Lightcurve-based 3D-model of Gothlandia
Discovery[1]
Discovered byJ. Comas Solà
Discovery siteFabra Obs.
Discovery date30 September 1930
Designations
(1188) Gothlandia
Pronunciation/ɡɒθˈlændiə/
Named after
Catalonia[2]
(Spanish autonomous community)
1930 SB · 2016 FU5
A917 SK
main-belt · (inner)
Flora[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc86.62 yr (31,639 days)
Aphelion2.5856 AU
Perihelion1.7948 AU
2.1902 AU
Eccentricity0.1805
3.24 yr (1,184 days)
294.72°
0° 18m 14.76s / day
Inclination4.8169°
5.4502°
7.1662°
Physical characteristics
Dimensions11.19±2.21 km[5]
12.11±0.76 km[6]
12.40±0.6 km[7]
12.42±0.6 km[8]
12.46 km (derived)[3]
12.670±0.136 km[9]
14.255±0.040 km[10]
3.49138±0.00006 h[8]
3.4915±0.0001 h[11]
3.49153±0.00002 h[12]
3.4916 h[3]
3.4917±0.0005 h[13]
3.491820±0.00005 h[14]
3.491820 h[15]
3.49198±0.00014 h[12]
3.4921±0.0001 h[12]
3.493 h[16]
0.2065±0.0170[10]
0.2401±0.025[7]
0.2476±0.0242[8]
0.252±0.034[6]
0.2631 (derived)[3]
0.273±0.031[9]
0.41±0.18[5]
SMASS = S[1][3][17]
11.34±0.27[18] · 11.50[5] · 11.59[3][10][16] · 11.6[1] · 11.662±0.014[8] · 11.70[6][7]

1188 Gothlandia, provisional designation 1930 SB, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 12 kilometers in diameter. Discovered by astronomer Josep Comas i Solà at the Fabra Observatory in 1930, the asteroid was later named after the ancient name of the Spanish autonomous community of Catalonia.

Discovery[edit]

Gothlandia was discovered on 30 September 1930, by Catalan astronomer Josep Comas i Solà at the Fabra Observatory in Barcelona, Spain.[19] It was independently discovered by Soviet Grigory Neujmin at Simeiz Observatory on 17 October 1930, and by K. Nakamura at Kyoto Observatory, Japan, on 18 October 1930.[2] The Minor Planet Center, however, only credits the first discoverer. The asteroid was first identified as A917 SK at Simeiz in September 1917.[19]

Orbit and classification[edit]

Gothlandia is a member of the Flora family (402),[4] a giant asteroid family and the largest family of stony asteroids in the main-belt.[20]: 23  It orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,184 days). Its orbit has an eccentricity of 0.18 and an inclination of 5° with respect to the ecliptic.[1] The body's observation arc begins with its official discovery observation at Barcelona in 1930.[19]

Physical characteristics[edit]

In the SMASS classification, Gothlandia is a stony S-type asteroid,[1][17] which corresponds to the overall spectral type for Florian asteroids.[20]: 23 

Rotation period and poles[edit]

Several rotational lightcurves of Gothlandia have been obtained from photometric observations since the 1990s.[8][11][12][13][16] Lightcurve analysis gave a consolidated rotation period of 3.4916 hours with a brightness variation of 0.81 magnitude (U=3).[3] A high brightness amplitude typically indicates a non-spherical shape.

Modeled lightcurves using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a concurring period 3.491820 hours.[14][15] In 2013, another modeled lightcurve obtained form photometric data collected by the Catalina Sky Survey also determined a spin axis of (334.0°, −84.0°) in ecliptic coordinates (λ, β).[21]

Diameter and albedo[edit]

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Gothlandia measures between 11.19 and 14.255 kilometers in diameter and its surface has an albedo between 0.2065 and 0.41.[5][6][7][8][9][10]

The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2631 and a diameter of 12.46 kilometers based on an absolute magnitude of 11.59.[3]

Naming[edit]

This minor planet was named after the Spanish autonomous community of Catalonia, by its ancient, per-medieval name Gothlandia ("Land of the Goths"). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 110).[2]

References[edit]

  1. ^ a b c d e f "JPL Small-Body Database Browser: 1188 Gothlandia (1930 SB)" (2017-06-02 last obs.). Jet Propulsion Laboratory. Retrieved 11 October 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1188) Gothlandia". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 100. doi:10.1007/978-3-540-29925-7_1189. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g h "LCDB Data for (1188) Gothlandia". Asteroid Lightcurve Database (LCDB). Retrieved 11 October 2017.
  4. ^ a b "Asteroid 1188 Gothlandia – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ 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. Retrieved 11 October 2017.
  6. ^ 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. Retrieved 17 October 2019. (online, AcuA catalog p. 153)
  7. ^ 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.
  8. ^ a b c d e f Baker, Ronald E.; Pilcher, Frederick; Klinglesmith, Daniel A. III (April 2012). "Rotation Period and H-G Parameters Determination for 1188 Gothlandia". The Minor Planet Bulletin. 39 (2): 60–63. Bibcode:2012MPBu...39...60B. ISSN 1052-8091. Retrieved 11 October 2017.
  9. ^ a b c Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 11 October 2017.
  10. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
  11. ^ a b Hamanowa, Hiromi; Hamanowa, Hiroko (July 2009). "Lightcurves of 494 Virtus, 556 Phyllis, 624 Hektor 657 Gunlod, 111 Reinmuthia, 1188 Gothlandia, and 1376 Michelle". The Minor Planet Bulletin. 36 (3): 87–88. Bibcode:2009MPBu...36...87H. ISSN 1052-8091. Retrieved 11 October 2017.
  12. ^ a b c d Behrend, Raoul. "Asteroids and comets rotation curves – (1188) Gothlandia". Geneva Observatory. Retrieved 11 October 2017.
  13. ^ a b Kryszczynska, A.; Colas, F.; Polinska, M.; Hirsch, R.; Ivanova, V.; Apostolovska, G.; et al. (October 2012). "Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region". Astronomy and Astrophysics. 546: 51. Bibcode:2012A&A...546A..72K. doi:10.1051/0004-6361/201219199.
  14. ^ a b Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 11 October 2017.
  15. ^ a b Durech, J.; Kaasalainen, M.; Warner, B. D.; Fauerbach, M.; Marks, S. A.; Fauvaud, S.; et al. (January 2009). "Asteroid models from combined sparse and dense photometric data" (PDF). Astronomy and Astrophysics. 493 (1): 291–297. Bibcode:2009A&A...493..291D. doi:10.1051/0004-6361:200810393. Retrieved 24 August 2017.
  16. ^ a b c di Martino, Mario; Dotto, E.; Barucci, M. A.; Fulchignoni, M.; Rotundi, A. (May 1994). "Photoelectric photometry of ten small and fast spinning asteroids". Icarus. 109 (1): 210–218. Bibcode:1994Icar..109..210D. doi:10.1006/icar.1994.1087. ISSN 0019-1035. Archived from the original on 2 February 2017. Retrieved 11 October 2017.
  17. ^ a b Bus, S.; Binzel, R. P. (October 2004). "1188 Gothlandia CCD Spectrum". NASA Planetary Data System. Bibcode:2004PDSS....1.....B. Retrieved 11 October 2017.
  18. ^ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 11 October 2017.
  19. ^ a b c "1188 Gothlandia (1930 SB)". Minor Planet Center. Retrieved 11 October 2017.
  20. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 978-0-8165-3213-1.
  21. ^ Hanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: 16. arXiv:1301.6943. Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701.

External links[edit]

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