2006/07/31 by M. M. Dunham, Michael M. Dunham, Neal J. Evans II +21 · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Context (archaeology) #Luminosity #Luminosity function #Outflow #Protostar #Radiative transfer #Star formation #Young stellar object #astro-ph
paper · pdf · doi:10.1086/508051
published as Astrophys.J.651:945-959,2006 · Accepted for publication in the Astrophysical Journal. 39 pages, 9 figures. See http://peggysue.as.utexas.edu/SIRTF/ for high-resolution figures
arxiv created 2006/07/31 · openalex publication_date 2006/11/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We report the first detections of the Class 0 protostellar source IRAM 04191+1522 at wavelengths shortward of 60 μm with the Spitzer Space Telescope . We see extended emission in the Spitzer images that suggests the presence of an outflow cavity in the circumstellar envelope. We combine the Spitzer observations with existing data to form a complete data set ranging from 3.6 to 1300 μm and use these data to construct radiative transfer models of the source. We conclude that the internal luminosity of IRAM 04191+1522, defined to be the sum of the luminosity from the internal sources (a star and a disk), is L int = 0.08 ± 0.04 L ☉ , placing it among the lowest luminosity protostars known. Although it was discovered before the launch of the Spitzer Space Telescope , IRAM 04191+1522 falls within a new class of very low luminosity objects being discovered by Spitzer . Unlike the two other well-studied objects in this class, which are associated either with weak, compact outflows or no outflows at all, IRAM 04191+1522 has a well-defined molecular outflow with properties consistent with those expected based on relations derived from higher luminosity ( L int ≥ 1 L ☉ ) protostars. We discuss the difficulties in understanding IRAM 04191+1522 in the context of the standard model of star formation and suggest a possible explanation for the very low luminosity of this source.