1188 Gothlandia, provisional designation1930 SB, is a stony Florianasteroid from the inner regions of theasteroid belt, approximately 12 kilometers in diameter. Discovered by astronomerJosep Comas i Solà at theFabra Observatory in 1930, the asteroid was later named after the ancient name of the Spanish autonomous community ofCatalonia.
Gothlandia was discovered on 30 September 1930, by Catalan astronomerJosep Comas i Solà at theFabra Observatory in Barcelona, Spain.[19] It was independently discovered by SovietGrigory Neujmin atSimeiz Observatory on 17 October 1930, and by K. Nakamura at Kyoto Observatory, Japan, on 18 October 1930.[2] TheMinor Planet Center, however, only credits the first discoverer. The asteroid was first identified asA917 SK at Simeiz in September 1917.[19]
Gothlandia is a member of theFlora family (402),[4] a giantasteroid family and the largest family of stony asteroids in the main-belt.[20]: 23 It orbits the Sun in theinner main-belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,184 days). Its orbit has aneccentricity of 0.18 and aninclination of 5° with respect to theecliptic.[1] The body'sobservation arc begins with its official discovery observation at Barcelona in 1930.[19]
Several rotationallightcurves ofGothlandia have been obtained from photometric observations since the 1990s.[8][11][12][13][16] Lightcurve analysis gave a consolidatedrotation period of 3.4916 hours with a brightness variation of 0.81magnitude (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 theCatalina Sky Survey also determined a spin axis of (334.0°, −84.0°) inecliptic coordinates (λ, β).[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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