Start of main content

Sample Inspec record

Typical Inspec record

Although the layout of an Inspec record may vary between Inspec services and publications, you should expect to find the following information in a typical journal record.

TITLE: A reappraisal of the chemical composition of the Orion nebula based on Very Large Telescope echelle spectrophotometry
AUTHOR(S): Esteban, C.; Peimbert, M.; Garcia-Rojas, J.; Ruiz, M. T.; Peimbert, A.; Rodriguez, M.
AUTHOR AFFILIATION: Inst. de Astrofisica de Canarias, La Laguna, Spain
JOURNAL: Monthly Notices of the Royal Astronomical Society vol.355, no.1, p.229-47, 89 refs.
PUBLISHER: Blackwell Science for R. Astron. Soc.
PUBLISHED IN: United Kingdom
DOI: 10.1111/j.1365-2966.2004.08313.x
ISSN: 0035-8711
SICI: 0035-8711(20041121)355:1L.229:RCCO;1-7
DOCUMENT TYPE: Journal Paper
TREATMENT: Bibliography; Experimental
ABSTRACT: We present Very Large Telescope (VLT) UVES echelle spectrophotometry of the Orion nebula in the 3100-10 400 Angstroms range. We have measured the intensity of 555 emission lines, many of them corresponding to permitted lines of different heavy-element ions. This is the largest set of spectral emission lines ever obtained for a Galactic or extragalactic H II region. We have derived He+, C2+, O+, O2+ and Ne2+ abundances from pure recombination lines. This is the first time that O+ and Ne2+ abundances have been obtained from these kinds of lines in the nebula. We have also derived abundances from collisionally excited lines for a large number of ions of different elements. In all cases, ionic abundances obtained from recombination lines are larger than those derived from collisionally excited lines. We have obtained remarkably consistent independent estimations of the temperature fluctuation parameter, t2, from different methods, which are also similar to other estimates from the literature. This result strongly suggests that moderate temperature fluctuations (t2 between 0.02 and 0.03) are present in the Orion nebula. We have compared the chemical composition of the nebula with those of the Sun and other representative objects. The heavy-element abundances in the Orion nebula are only slightly higher than the solar ones, a difference that can be explained by the chemical evolution of the solar neighbourhood.
CLASSIFICATION CODES: A9840H H II regions, emission nebulae; A9580J Photographic region astronomical observations
IPC: G01J3/00 Spectrometry; Spectrophotometry; Monochromators; Measuring colours
THESAURUS TERMS: astronomical photometry; astronomical spectra; element relative abundance; H II regions; spectrophotometry
FREE TERMS: Orion nebula chemical composition; Very Large Telescope echelle spectrophotometry; VLT UVES; emission line intensity; permitted line; heavy-element ion; Galactic region; extragalactic H II region; ion abundance; recombination line; collisionally excited line; temperature fluctuation; 3100 to 10400 Å; He; C; O; Ne
CHEMICAL INDEXING: He el; C el; O el; Ne el
NUMERICAL INDEXING: wavelength 3.1E-07 to 1.04E-06 m

© Copyright 2010, The Institution of Engineering and Technology