Abstract
The designation ``ultracompact H II region'' first appeared in the astronomical literature over 30 years ago. Since that time, of order 103 actual or candidate ultracompact (UC) H II regions have been identified, and no fewer than seven theoretical models have been proposed to describe them. Recent observational evidence suggests that the conventional ``UC H II'' classification may not be adequate to describe all of the small, dense nebulae surrounding young, massive stars. In particular, it appears that some UC H II regions may be small, high density regions that are integral parts of much larger structures; these we call ``UC H II regions with extended emission''. Other H II regions appear to be an order of magnitude smaller and two orders of magnitude denser than traditional UC H II regions, and hence are deserving of a new classification. We designate these as ``super-ultracompact H II regions'', (though we suspect that ``hypercompact'' will prevail). We provide brief scientific and historical perspectives, present the new observational data and arguments for the new classifications, and briefly discuss possible implications for theoretical models of UC H II regions.