| Author | dc.contributor.author | Wilson, Thomas L. | |
| Author | dc.contributor.author | Casassus Montero, Simón | es_CL |
| Author | dc.contributor.author | Keating, Katie M. | es_CL |
| Admission date | dc.date.accessioned | 2012-08-01T15:43:23Z | |
| Available date | dc.date.available | 2012-08-01T15:43:23Z | |
| Publication date | dc.date.issued | 2012-01-10 | |
| Cita de ítem | dc.identifier.citation | The Astrophysical Journal, 744:161 (6pp), 2012 January 10 | es_CL |
| Identifier | dc.identifier.other | doi:10.1088/0004-637X/744/2/161 | |
| Identifier | dc.identifier.uri | https://repositorio.uchile.cl/handle/2250/125677 | |
| General note | dc.description | Artículo de publicación ISI | es_CL |
| Abstract | dc.description.abstract | High angular resolution radio continuum images of NGC 1976 (M42, Orion A) at ν = 330 MHz (λ = 91 cm),
1.5 GHz (20 cm), and 10.6 GHz (2.8 cm) have been aligned, placed on a common grid, smoothed to common
resolutions of 80 (=0.16 pc at 420 pc) and 90 (=0.18 pc) and compared on a position-by-position basis. The
results are not consistent with a single value of Te. The best fit to the continuum data is a multi-layer model based
on radio recombination line data with a monotonic variation, from Te = 8500 K in the higher intensity, more
compact region at the rear of NGC 1976 to Te = 6000 K in the low-intensity, extended region in the foreground.
An estimate of temperature fluctuations toward the peak from this model yields t2 = 0.003. This is a factor of 10
lower than fluctuation values from optical collisionally excited line data. | es_CL |
| Lenguage | dc.language.iso | en | es_CL |
| Keywords | dc.subject | Hii regions | es_CL |
| Título | dc.title | THE STRUCTURE OF NGC 1976 IN THE RADIO RANGE | es_CL |
| Document type | dc.type | Artículo de revista | |
