========================================================================== J/A+A/538/A54 Spectroscopy of 12 [WC] planetary nebulae (Garcia-Rojas+, 2012) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat hbeta.dat table3.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/538/A54 ==========================================================================
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Beginning of ReadMe : J/A+A/538/A54 Spectroscopy of 12 [WC] planetary nebulae (Garcia-Rojas+, 2012) ================================================================================ Analysis of chemical abundances in planetary nebulae with [WC] central stars. I. Line intensities and physical conditions. Garcia-Rojas J., Pena M., Morisset C., Mesa-Delgado A., Ruiz M.T. <Astron. Astrophys., 538, A54 (2012)> =2012A&A...538A..54G ================================================================================ ADC_Keywords: Planetary nebulae ; Spectroscopy Keywords: stars: AGB and post-AGB - ISM: abundances - planetary nebulae: general - line: identification Abstract: Planetary nebulae (PNe) around Wolf-Rayet [WR] central stars ([WR]PNe) constitute a particular photoionized nebula class that represents about 10% of the PNe with classified central stars. We analyse deep high-resolution spectrophotometric data of 12 [WR] PNe. This sample of [WR]PNe represents the most extensive analysed so far, at such high spectral resolution. We aim to select the optimal physical conditions in the nebulae to be used in ionic abundance calculations that will be presented in a forthcoming paper. Description: We acquired spectra at Las Campanas Observatory with the 6.5-m telescope and the Magellan Inamori Kyocera (MIKE) spectrograph, covering a wavelength range from 3350AA to 9400AA on September 2009 and June 2010. The spectra were exposed deep enough to detect, with signal-to-noise ratio higher than three, the weak optical recombination lines (ORLs) of OII, CII, and other species. We detect and identify about 2980 emission lines, which, to date, is the most complete set of spectrophotometric data published for this type of objects. From our deep data, numerous diagnostic line ratios for Te and ne are determined from collisionally excited lines (CELs), ORLs, and continuum measurements (HI Paschen continuum in particular).