2005/11/16 by Dana S. Balser, W. M. Goss, T. M. Bania +1
Physics and Astronomy · #Abundance (ecology) #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #CMB cold spot #Galactic Center #Interstellar medium #Nebula #Planetary nebula #Spectral line #Stars #Stellar evolution #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/499937
published as Astrophys.J.640:360-368,2006 · 27 pages, 10 figures (accepted for publication in the ApJ)
arxiv created 2005/11/16 · openalex publication_date 2006/03/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We used the VLA to search for 3 He + emission from two Galactic planetary nebulae (PNe): NGC 6572 and J320. Standard stellar models predict that the 3 He/H abundance ratios for PNe should be 1-2 orders of magnitude higher than the primordial value ( 3 He/H ~ 10 -5 by number) determined from Galactic H II region abundances and confirmed by WMAP cosmic microwave background results. Chemical evolution models suggest that fewer than 5% of all PNe enrich the interstellar medium (ISM) with 3 He at the level of standard stellar models. Our target PNe are therefore anomalous in that they were selected from a sample deliberately biased to contain objects with properties that maximized the likelihood of a 3 He detection by the VLA. We have detected the 8.665 GHz hyperfine 3 He + transition in J320 at the 4 σ level. The 3 He/H abundance ratio is 1.9 × 10 -3 with roughly a factor of 2 uncertainty. For NGC 6572 we find an upper limit of 3 He/H ≲ 10 -3 . This detection of 3 He in J320 makes it the second PN known to have an anomalously high 3 He abundance, confirming that at least some low-mass stars produce significant amounts of 3 He that survives to the PN stage and enriches the ISM.