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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

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

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

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

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

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

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

  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 – (1188) Gothlandia. 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.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  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. Retrieved 11 October 2017.
  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...77B. 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. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. {{cite book}}: |journal= ignored (help)
  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.

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