The Kuiper belt luminosity function from m_R=21 to 26

详细信息    查看全文

• 作者：Wesley C. Fraser ; J.J. Kavelaars ; M.J. Holman ; C.J. Pritchet ; B.J. Gladman ; T. Grav ; R.L. Jones ; J. MacWilliams ; J.-M. Petit
• 关键词：Collisional physics ; Kuiper belt
• 刊名：Icarus
• 出版年：2008
• 出版时间：June 2008
• 年：2008
• 卷：195
• 期：2
• 页码：827-843
• 全文大小：634 K

文摘

We have performed an ecliptic imaging survey of the Kuiper belt with our deepest and widest field achieving a limiting flux of m(g^′)_{50 %} 26.4, with a sky coverage of 3.0 square-degrees. This is the largest coverage of any other Kuiper belt survey to this depth. We detect 72 objects, two of which have been previously observed. We have improved the Bayesian maximum likelihood fitting technique presented in Gladman et al. [Gladman, B., Kavelaars, J.J., Nicholson, P.D., Loredo, T.J., Burns, J.A., 1998. Astron. J. 116, 2042–2054] to account for calibration and sky density variations and have used this to determine the luminosity function of the Kuiper belt. Combining our detections with previous surveys, we find the luminosity function is well represented by a single power-law with slope =0.65±0.05 and an on ecliptic sky density of 1 object per square-degree brighter than m_R=23.42±0.13. Assuming constant albedos, this slope suggests a differential size-distribution slope of 4.25±0.25, which is steeper than the Dohnanyi slope of 3.5 expected if the belt is in a state of collisional equilibrium. We find no evidence for a roll-over or knee in the luminosity function and reject such models brightward of 1022883bc7"" title=""Click to view the MathML source"" alt=""Click to view the MathML source"">m(R)24.6.