Reconstruction of asteroid spin states from Gaia DR3 photometry

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Table 3

Spins of asteroids derived from DR3 photometry.

	Asteroid	λ₁	β₁	λ₂	β₂	P	N	Method
		(deg)	(deg)	(deg)	(deg)	(h)
5	Astraea	122	37	312	40	16.8008	36	C
26	Proserpina	83	−46	255	−56	13.1092	58	C
32	Pomona	103	39	279	41	9.4475	38	CE
33	Polyhymnia	20	−29	197	−31	18.6088	36	C
41	Daphne	207	−35	355	−39	5.98807	35	C
43	Ariadne	69	−10	252	−12	5.76182	53	C
44	Nysa	96	45	287	54	6.4214	25	CE
45	Eugenia	123	−32	299	−20	5.69918	30	C
48	Doris	107	32	291	45	11.8900	50	C
50	Virginia	103	12	281	26	14.3107	31	E
⋮
301892	1998 QL98	97	−63			3.81273	28	C
307960	2004 GS75	23	71			12.7888	30	CE
313568	2003 DW4	96	63			4.53729	25	E
329036	2011 AE35	18	−50			29.959	22	E
334190	2001 SQ199	22	−61	162	−41	7.3653	30	C
353971	2000 AE210	9	−50	275	−80	21.467	26	E
354510	2004 PV66	50	−54			6.6110	29	E
362935	2012 JB5	89	53			12.6190	68	C
380282	2002 AO148	330	81			10.6120	29	C
397797	2008 MZ2	91	76			49.936	35	CE

Notes. The table lists the first ten and the last ten asteroid models derived from Gaia DR3 data. The full table is available in electronic format at the CDS. For each asteroid we report its spin axis direction in ecliptic latitude λ₁ and longitude β₁ (the second pole solution has ecliptic coordinates λ₂ and longitude β₂), the sidereal rotation period P, the number N of photometric measurements in DR3, and the method used for computing periodograms: C – convex shape models, E – ellipsoids, CE – both methods provided the same period. The uncertainty of the rotation period P is on the order of the last decimal place.

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