SIMBAD references

We present results from a 12 year survey of the Daytime Arietid meteor shower using the Canadian Meteor Orbit Radar, a VHF backscattering orbital meteor radar, covering the interval 2002-2013. This survey recorded more than 2x10⁴ Daytime Arietid orbits having representative masses of 8x10^–8 kg and sizes of ~0.4 mm. The core activity for the Arietids is found in the range 73 _.^○5 ≤ λ_☉ ≤ 84 _.^○5 and shows a broad 4-d maximum centred near λ_☉ = 80 _.^○5 of 0.04 meteoroids/km2h-1 producing meteors of equivalent radio magnitude of +6.5 from a mean radiant at αg = 44 _.^○9±1 _.^○1, δg = 25 _.^○5±1 _.^○0. During the plateau of shower peak activity, the mass index of the stream reaches a minimum with s = 1.6-1.7. Contamination from another nearby shower (likely the Daytime Zeta Perseids) and/or sub-streams showing different orbits compared to the core of the stream is evident in the interval 60 _.^○5 ≤ λ_☉ ≤ 71 _.^○5. Similar contamination beyond λ_☉ = 84 _.^○5 may be due to the Helion sporadic source. We also characterized the deceleration profiles for Daytime Arietid meteor echoes using several independent speed techniques including Fresnel pre-t0, Fresnel amplitude oscillation and time-of-flight speeds which together with modelling produced a best estimate for the stream's out-of-atmosphere speed of v∞ = 40.5±0.7 km/s. The mean radar orbit from our study is noticeably smaller in semi-major axis and eccentricity than is found for larger Arietids measured with optical systems, a difference which if real indicates a particle-size sorting of the stream orbit. The broad activity maximum, long duration of activity and particle-size dependence of the orbital elements suggest the stream is too old to have been solely formed during the breakup of the parent comet of the Marsden sunskirters about a millennium ago as proposed by Sekanina & Chodas.