Direct Observations of the Ionizing Star in the UC HII Region G29.96-0.02: A Strong Constraint on the Stellar Birth Line for Massive Stars

Simple item page
dc.creatorWatson, Alan M.
dc.creatorCoil, Alison L.
dc.creatorShepherd, Debra S.
dc.creatorHofner, Peter
dc.creatorChurchwell, Ed
dc.date1997-05-01
dc.date.accessioned2026-07-07T12:41:40Z
dc.date.available2026-07-07T12:41:40Z
dc.descriptionWe have observed the ultracompact HII region G29.96-0.02 in the near infrared J, H, and K bands and in the Br-gamma line. By comparison with radio observations, we determine that the extinction to the nebula is AK = 2.14 with a 3 sigma uncertainty of 0.25. We identify the ionizing star and determine its intrinsic K magnitude. The star does not have an infrared excess and so appears to be no longer accreting. The K magnitude and the bolometric luminosity allow us to place limits on the location of the ionizing star in the HR diagram. The 3 sigma upper limit on the effective temperature of the ionizing star is 42500 K. We favor a luminosity appropriate for star with a mass in excess of about 60 solar masses. The limit on the temperature and luminosity exclude stars on the ZAMS and stars within 10^6 yr of the ZAMS. Since the age of the UC HII region is estimated to be only about 10^5 yr, we suggest that this is direct evidence that the stellar birth line for massive stars at twice solar metallicity must be significantly redder than the ZAMS.
dc.description42 pages; LaTex; 11 Postscript figures; accepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/9705007
dc.identifierhttp://arxiv.org/abs/astro-ph/9705007
dc.identifierAstrophys.J.487:818-833,1997
dc.identifierdoi:10.1086/304650
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/219853
dc.subjectAstrophysics
dc.titleDirect Observations of the Ionizing Star in the UC HII Region G29.96-0.02: A Strong Constraint on the Stellar Birth Line for Massive Stars
dc.typetext

Files

Collections

arXiv