测试主带彗星的彗星性质。~（133）P/Elst-Pizarro和~（176）P/ LINEAR的光谱
Testing the comet nature of main belt comets. The spectra of 133P/Elst-Pizarro and 176P/LINEAR
摘要：
我们介绍了MBC 133 P/Elst-Pizarro和176 P/LINEAR以及三颗Themis家族小行星：（62）Erato，（379）Huenna和（383）Janina的可见光谱，这些光谱是在2007年使用西班牙La Palma的El Roque de los Muchachos天文台和智利Cerro Paranal的8 m Kueyen（UT 2）VLT望远镜获得的。133 P和176 P的光谱与B型小行星的光谱最相似，与Themis家族成员的光谱非常相似，与162 P/Siding-Spring彗星和大多数观测到的彗星核的光谱有显著差异。在133 P的光谱中没有检测到CN气体的发射。我们确定的CN生产率的上限Q（CN）= $= 2.8 \times 10^{21}$ mol/s，三个数量级低于Q（CN）的木星家族彗星在类似的日心距离。133 P/Elst-Pizarro和176 P/LINEAR的光谱证实，它们可能是忒弥斯家族的小行星，碎片可能保留了挥发物，不太可能起源于外海王星带或奥尔特云的彗星。
英文摘要：
We present the visible spectrum of MBCs 133P/Elst-Pizarro and 176P/LINEAR, as well as three Themis family asteroids: (62) Erato, (379), Huenna and (383) Janina, obtained in 2007 using three telescopes at "El Roque de los Muchachos"' Observatory, in La Palma, Spain, and the 8m Kueyen (UT2) VLT telescope at Cerro Paranal, Chile. The spectra of 133P and 176P resemble best those of B-type asteroid and are very similar to those of Themis family members and are significantly different from the spectrum of comet 162P/Siding-Spring and most of the observed cometary nuclei. CN gas emission is not detected in the spectrum of 133P. We determine an upper limit for the CN production rate Q(CN) = $= 2.8 \times 10^{21}$ mol/s, three orders of magnitude lower than the Q(CN) of Jupiter family comets observed at similar heliocentric distances. The spectra of 133P/Elst-Pizarro and 176P/LINEAR confirm that they are likely members of the Themis family of asteroids, fragments that probably retained volatiles, and unlikely have a cometary origin in the trans-neptunian belt or the Oort cloud.
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