The Pipe Nebula is not uniform in density; it contains a large population of dense, low-mass cores, about 134 distinct objects. In other molecular clouds these cores evolve into young stars, but in the Pipe they remain quiescent. Astronomers have been using radio astronomy techniques to study the density and temperatures of particular molecular species in these cold cores, for example species of carbon monoxide and ammonia, whose relative line strengths can quantify these parameters.
CfA astronomers Jan Frobrich, Karin Oberg, and Charlie Lada, together with four colleagues, have now completed a study of fifty-two of the Pipe’s cores in the light from six additional molecules that are particularly useful in characterizing star formation activity, and also complemented that data with infrared images from Herschel that show the cold dust distribution. They report that the dense cores in the Pipe are very cold indeed, between 13 and 19 kelvin,with the coldest ones containing the most obscuring dust. The astronomers find that one molecule in particular, N2H+, is the only species to exclusively trace the very densest and coldest cores, making this molecule a key diagnostic for future studies to figure out why these dense cores do not form stars.