Open AccessDeep echelle spectrophotometry of S 311, a Galactic H ii region located outside the solar circle
Author(s) -
GarcíaRojas J.,
Esteban C.,
Peimbert A.,
Peimbert M.,
Rodríguez M.,
Ruiz M. T.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09302.x
Subject(s) - physics , balmer series , astrophysics , excited state , spectrograph , planetary nebula , emission spectrum , spectral line , deuterium , doubly ionized oxygen , ultraviolet , spectrophotometry , line (geometry) , ion , astronomy , atomic physics , optics , stars , geometry , mathematics , quantum mechanics
We present echelle spectrophotometry of the Galactic H ii region S 311. The data have been taken with the Very Large Telescope Ultraviolet‐Visual Echelle Spectrograph in the 3100–10 400 Å range. We have measured the intensities of 263 emission lines; 178 are permitted lines of H 0 , D 0 (deuterium), He 0 , C 0 , C + , N 0 , N + , O 0 , O + , S + , Si 0 , Si + , Ar 0 and Fe 0 ; some of them are produced by recombination and others mainly by fluorescence. Physical conditions have been derived using different continuum‐ and line‐intensity ratios. We have derived He + , C ++ and O ++ ionic abundances from pure recombination lines as well as abundances from collisionally excited lines for a large number of ions of different elements. We have obtained consistent estimations of t 2 applying different methods. We have found that the temperature fluctuations paradigm is consistent with the T e (He i ) versus T e (H i ) relation for H ii regions, in contrast with what has been found for planetary nebulae. We report the detection of deuterium Balmer lines up to Dδ in the blue wings of the hydrogen lines, whose excitation mechanism seems to be continuum fluorescence.