A Spectral Atlas of the Pre‐WN Candidate HD 326823

Abstract

HD 326823 is a peculiar emission line object. In the literature it was considered as a pre-WN candidate. Based mainly on high resolution data, obtained with the FEROS spectrograph, we made an atlas covering 3800-9200 Å region. This atlas confirms the presence of several strong He i lines and numerous N lines. There is also a deficiency of H, indicating that this object is indeed in an evolved stage. In addition, with low resolution spectra, we obtained intensities of several lines.

The Oxygen Abundance in the Inner HiiRegions of M101: Implications for the Calibration of Strong‐Line Metallicity Indicators

“…The high detection fraction of W-R features, often including the signatures of WC stars, in high-metallicity H ii regions has been noted in earlier works Hadfield et al 2005), and is expected from the increase in the stellar mass loss with metallicity (Meynet & Maeder 2005). Given the scope of this paper, I will not further discuss the W-R content of the H ii regions under consideration, and will simply note that the stellar envelope of stars with Fe ii lines in emission can also be responsible for emission in auroral lines such as [ N ii] k5755 and [O ii] k7325 ( Hillier et al 1998;Borges Fernandes et al 2001). Therefore, these lines will not be used to measure nebular electron temperatures in H507.…”

HR Carinae: New spectroscopic data and physical parameters

“…The line identification was carried out using the line lists provided by Moore (1945), Garcia-Lario et al (1998), Landaberry et al (2001) and Fernandes et al (2001). We also looked up two sites on the web: NIST Atomic Spectra Database Lines Form (URL physics.nist.gov/cgi/AtData/lines) and The Atomic Line List v2.04 (URL www.pa.uky.edu/peter/atomic/).…”

Rotation of B[e] Supergiants, Luminous Blue Variables and Wolf-Rayet Stars

“…Smith & Davidson (2001) found shocked gas in the polar lobes of TJ Car and interpreted it as an indication of the presence of a fast polar wind. HD 326823 is another interesting star, as it is believed to be in transition between the LBVs and WR phases (Borges Fernandes et al 2001). Its HeI spectrum displays double-peak profiles reminiscent of a disk structure.…”