摘要：Long-period comets observed in our solar system are believed to originate from the Oort cloud, which is estimated to extend from roughly a few thousand to 10 5 au from the Sun. Despite many theoretical arguments for the existence of the Oort cloud, no direct observations of outer Oort cloud objects have been reported. Here, we explore the possibility of measuring Oort clouds around other stars through their emission at submillimeter wavelengths. Observations with the 545 and 857 GHz bands of the Planck satellite are well matched to the expected temperatures of Oort cloud bodies (on the order of 10 K). By correlating the Planck maps with catalogs of stars observed by the Gaia mission, we are able to constrain interesting regions of the exo-Oort cloud (EXOC) parameter space, placing limits on the total mass and the minimum size of grains in the cloud. We compare our measurements with known debris disk systems—in the case of Vega and Fomalhaut, we find a significant excess that is in agreement with measurements from Herschel. We use the measurements around Fomalhaut to constrain a possible EXOC of that system. We explore an observed excess around the brightest and nearest stars in our sample as arising from possible EXOCs or other extended sources of thermal emission. We argue that future CMB surveys and targeted observations with far-infrared and millimeter wavelength telescopes have the potential to detect EXOCs or other extended sources of thermal emission beyond ∼1000au from the parent stars.
关键词：cosmic background radiation;Oort Cloud;submillimeter: planetary systems
