bHROS high spectral resolution observations of PN forbidden and recombination line profiles

Barlow, M. J.; Hales, As S.; Storey, P. J.; Liu, Xw-W.; Tsamis, Y. G.; Aderin, Me E.

doi:10.1017/s1743921306003279

Cited by 8 publications

(5 citation statements)

References 5 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…So far, such components are directly or indirectly observed in the some PNe, for example, Abell 30 (Wesson et al 2003), NGC 6153 and NGC 7009 (Barlow et al 2006). In highvelocity components of Abell 30, Wesson et al (2003) found that the electron temperature derived from O II lines is 500-2500 K and the ORL oxygen abundance is ∼100 times larger than from CELs.…”

Section: High Density Componentsmentioning

confidence: 99%

“…case of Abell 30, the ORL oxygen abundance might indicate the amount of O synthesized in the He-rich intershell. Barlow et al (2006) To verify whether the large O (and O 2+ ) discrepancy in BoBn 1 is due to difference physical properties between O II and [O III] lines or not, following Barlow et al (2006), we compare the expansion and the radial velocities of O II and those of [O III] lines. The resultant values are summarized in Table 18.…”

Section: High Density Componentsmentioning

confidence: 99%

See 1 more Smart Citation

THE ORIGIN AND EVOLUTION OF THE HALO PN BoBn 1: FROM A VIEWPOINT OF CHEMICAL ABUNDANCES BASED ON MULTIWAVELENGTH SPECTRA

Otsuka

Tajitsu

Hyung

et al. 2010

ApJ

View full text Add to dashboard Cite

We have performed a comprehensive chemical abundance analysis of the extremely metal-poor ([Ar/H]<-2) halo planetary nebula (PN) BoBn 1 based on IUE archive data, Subaru/HDS spectra, VLT/UVES archive data, and Spitzer/IRS spectra. We have detected over 600 lines in total and calculated ionic and elemental abundances of 13 elements using detected optical recombination lines (ORLs) and collisionally excited lines (CELs). The estimations of C, N, O, and Ne abundances from the ORLs and Kr, Xe, and Ba from the CELs are done the first for this nebula, empirically and theoretically. The C, N, O, and Ne abundances from ORLs are systematically larger than those from CELs. The abundance discrepancies apart from O could be explained by a temperature fluctuation model, and that of O might be by a hydrogen deficient cold component model. We have detected 5 fluorine and several slow neutron capture elements (the s-process). The amounts of [F/H], [Kr/H], and [Xe/H] suggest that BoBn 1 is the most F-rich among F detected PNe and is a heavy s-process element rich PN. We have confirmed dust in the nebula that is composed of amorphous carbon and PAHs with a total mass of 5.8×10 −6 M ⊙ . The photo-ionization models built with non-LTE theoretical stellar atmospheres indicate that the progenitor was a 1-1.5 M ⊙ star that would evolve into a white dwarf with an ∼0.62 M ⊙ core mass and ∼0.09 M ⊙ ionized nebula. We have measured a heliocentric radial velocity of +191.6 ±1.3 km s −1 and expansion velocity 2V exp of 40.5 ± 3.3 km s −1 from an average over 300 lines. The derived elemental abundances have been reviewed from the standpoint of theoretical nucleosynthesis models. It is likely that the elemental abundances except N could be explained either by a 1.5 M ⊙ single star model or by a binary model composed of 0.75 M ⊙ + 1.5 M ⊙ stars. Careful examination implies that BoBn 1 has evolved from a 0.75 M ⊙ + 1.5 M ⊙ binary and experienced coalescence during the evolution to become a visible PN, similar to the other extremely metal-poor halo PN, K 648 in M 15.

show abstract

Section: High Density Componentsmentioning

confidence: 99%

Section: High Density Componentsmentioning

confidence: 99%

THE ORIGIN AND EVOLUTION OF THE HALO PN BoBn 1: FROM A VIEWPOINT OF CHEMICAL ABUNDANCES BASED ON MULTIWAVELENGTH SPECTRA

Otsuka

Tajitsu

Hyung

et al. 2010

ApJ

View full text Add to dashboard Cite

show abstract

“…The zone responsible for HeII emission is perhaps the same as that of the OII emission. Barlow et al (2006) found the expansion velocities of the OII lines were smaller than those of the [OIII] lines in two PNe, NGC 7009 and NGC 6153. If so, the OII lines are emitted from the inner shell.…”

Section: Collisional and Recombination Lines From The Same Ions?mentioning

confidence: 84%

Expansion Velocity Investigation of the Elliptical Planetary Nebula NGC 6803

Choi¹,

Lee²,

Hyung³

2008

Journal of The Korean Astronomical Society

View full text Add to dashboard Cite

“…From the theoretical side, it is important to model the signature of each process on the temperature and density distributions. While, from the observational side, the combination of 3D kinematical models with high spectral resolution data, like those presented by Barlow et al (2006), might permit to derive temperature and density distributions and consequently to single out the main mechanism responsible for the temperature variations in a given object.…”

Section: Discussionmentioning

confidence: 99%

Temperature Variations and Chemical Abundances in Planetary Nebulae

Peimbert¹,

Peimbert²

2006

IAU

View full text Add to dashboard Cite

In this review we present a brief discussion on the observational evidence in favor of the presence of temperature variations, and conclude that many planetary nebulae show spatial temperature variations that are larger than those predicted by 1D static chemically homogeneous photoionization models. To determine accurate chemical abundances it is necessary to know the cause of these temperature variations and several possibilities are discussed. The importance of this problem is paramount to test the models of stellar evolution of low and intermediate mass stars and of the chemical evolution of galaxies. We conclude that the proper abundances for chemically homogeneous PNe are those derived from recombination lines, while for the two-abundance nebular model the proper heavy element abundances relative to hydrogen are those derived from visual and UV collisionally excited lines adopting the t2 values derived from Te([OIII]) and Te(Balmer)Comment: 8 pages, invited review to appear in Proc. IAU Symp. 234, Planetary Nebulae in Our Galaxy and Beyond (3-7 Apr 2006), eds. M.J. Barlow & R.H. Mendez (Cambridge Univ. Press

show abstract

bHROS high spectral resolution observations of PN forbidden and recombination line profiles

Cited by 8 publications

References 5 publications

THE ORIGIN AND EVOLUTION OF THE HALO PN BoBn 1: FROM A VIEWPOINT OF CHEMICAL ABUNDANCES BASED ON MULTIWAVELENGTH SPECTRA

THE ORIGIN AND EVOLUTION OF THE HALO PN BoBn 1: FROM A VIEWPOINT OF CHEMICAL ABUNDANCES BASED ON MULTIWAVELENGTH SPECTRA

Expansion Velocity Investigation of the Elliptical Planetary Nebula NGC 6803

Temperature Variations and Chemical Abundances in Planetary Nebulae

Contact Info

Product

Resources

About