Open AccessInfrared [Fe ii ] emission in the circumstellar nebulae of luminous blue variables
Author(s) -
Smith Nathan
Publication year - 2002
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 - 10.1046/j.1365-8711.2002.05964.x
Subject(s) - physics , astrophysics , stars , supernova , luminous blue variable , infrared , astronomy , planetary nebula , supergiant , doubly ionized oxygen , spectral line , emission spectrum
After a serendipitous discovery of bright [Fe ii ]λ16435 emission in nebulae around η Carinae and P Cygni, infrared spectra of other luminous blue variables (LBV) and LBV candidates were obtained. Bright infrared [Fe ii ] emission appears to be a common property among LBVs with prominent nebulae; this is an interesting discovery because strong [Fe ii ]λ16435 is typically seen in shock‐excited objects like supernova remnants and outflows from newly formed massive stars, as well as in active galactic nuclei (AGN), where the excitation mechanism is uncertain. This paper presents spectra in the H‐band (1.5 to 1.75 μm) for the central stars and nebulae of η Car, AG Car, P Cyg, Wra 751, HR Car, HD 168625, HD 160529, R 127 and S Doradus. Seven of nine targets show bright [Fe ii ]λ16435 in their nebulae, while it is absent in all central stars except the LBV candidate Wra 751. The two objects (S Dor and HD 160529) without prominent [Fe ii ]λ16435 are not yet known to have nebulae detected in optical images, and both lack bright thermal infrared emission from dust. The possible excitation mechanisms for this line and the implications of its discovery in LBV nebulae are discussed; there are good reasons to expect shock excitation in some objects, but other mechanisms cannot be ruled out.