Optical spectrum of the planetary nebula M 2-24

Zhang, Yong; Xw, Liu

doi:10.1051/0004-6361:20030466

Cited by 30 publications

(39 citation statements)

References 53 publications

(60 reference statements)

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“…Clearly emission of these diagnostic lines is dominated by the surrounding diffuse nebula. A similar result has been found in the peculiar bulge PN M 2-24 (Zhang & Liu 2003). Thus the possibility of a dense symbiotic nebula embedded in the low-N e ionized region of Me 1-1 cannot be completely ruled out.…”

Section: Discussionsupporting

confidence: 80%

Me 1-1: A PN containing a cool star

Shen¹,

Liu²,

Danziger

2004

A&A

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Abstract.We report the detection of a cool stellar component at the center of the planetary nebula (PN) Me 1-1 and present optical spectra of the system. From measurements of nebular emission lines, we have derived electron temperature, density and chemical composition. Heavy elemental abundances deduced from collisionally excited lines (CELs) are compared with those derived from optical recombination lines (ORLs). The electron temperature and density deduced from the nebular analysis were used to calculate the nebular continuum emission, which was then subtracted from the observed spectrum in order to obtain the spectrum of the cool stellar component apparent in the observed spectrum. We calculate B and V magnitudes of the cool companion and obtain a color index of B − V = 1.20. By comparing the spectrum of the cool star with standard spectra in Pickles's 1998 Stellar Flux Library, we find that the cool component has the spectral type of a K3-4 bright giant. Our analysis suggests that Me 1-1 is probably a yellow symbiotic system.

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Section: Discussionsupporting

confidence: 80%

Me 1-1: A PN containing a cool star

Shen¹,

Liu²,

Danziger

2004

A&A

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“…The large uncertainty of ADF(N 2+ ) is due to the large uncertainty in the CEL N 2+ abundance. ADF(O 2+ ) in M1-11 is comparable to that of high-density PN M2-24 (namely, 17;Zhang & Liu 2003). The density structure for M1-11 is similar to that of M2-24, showing a large density contrast of n e = 10 3−6 cm −3 .…”

Section: Rl Ionic Abundancesmentioning

confidence: 61%

“…Effective recombination coefficients for the lines' parent multiplet are the same as those used by Otsuka et al (2010). The RL ionic abundances are insensitive to the electron density under 10 8 cm −3 (Zhang & Liu 2003). For the ionic abundance calculations, we therefore adopted the effective recombination coefficients in case of n e = 10 4 cm −3 for C 2+ and N 2+ .…”

Section: Rl Ionic Abundancesmentioning

confidence: 99%

The Detection of C60 in the Well-Characterized Planetary Nebula M1-11

Otsuka

Kemper

Hyung

et al. 2013

ApJ

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We performed multiwavelength observations of the young planetary nebula (PN) M1-11 and obtained its elemental abundances, dust mass, and the evolutionary status of the central star. The AKARI/IRC, VLT/VISIR, and Spitzer/IRS spectra show features due to carbon-rich dust, such as the 3.3, 8.6, and 11.3 μm features due to polycyclic aromatic hydrocarbons (PAHs), a smooth continuum attributable to amorphous carbon, and the broad 11.5 and 30 μm features often ascribed to SiC and MgS, respectively. We also report the presence of an unidentified broad feature at 16-22 μm, similar to the feature found in Magellanic Cloud PNe with either C-rich or O-rich gas-phase compositions. We identify for the first time in M1-11 spectral lines at 8.5 (blended with PAH), 17.3, and 18.9 μm that we attribute to the C 60 fullerene. This identification is strengthened by the fact that other Galactic PNe in which fullerenes are detected have similar central stars, similar gas-phase abundances, and a similar dust composition to M1-11. The weak radiation field due to the relatively cool central stars in these PNe may provide favorable conditions for fullerenes to survive in the circumstellar medium. Using the photoionization code Cloudy, combined with a modified blackbody, we have fitted the ∼0.1-90 μm spectral energy distribution (SED) and determined the dust mass in the nebula to be ∼3.5 × 10 −4 M . Our chemical abundance analysis and SED model suggest that M1-11 is perhaps a C-rich PN with C/O ratio in the gas phase of +0.19 dex, and that it evolved from a 1-1.5 M star.

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“…This extremely low total helium abundance can be explained by the fact that a significant amount of He 0 is expected to be present in a low‐excitation nebula like NGC 40, and He 0 was not considered in the He/H given above. To circumvent this kind of problem, Zhang & Liu (2003) suggested that an ICF based on the S + and S ++ abundances can be used to account for the He 0 abundance of low‐ excitation PNe. Using our own data we were not able to calculate a S ++ abundance map, nevertheless, if we consider the S ++ abundances found by Pottasch et al (2003) and Liu et al (2004b) (Table 8), and the mean value of the S + /H + map that we calculated (8.88 × 10 −7 , in Table 8), we can determine a more reliable value for the He total abundance of NGC 40.…”

Section: Mapping Resultsmentioning

confidence: 99%

Physico-chemical spectroscopic mapping of the planetary nebula NGC 40 and the 2d_neb, a new 2D algorithm to study ionized nebulae

Leal-Ferreira

Gonçalves

Monteiro³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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In this paper we present an analysis of the physical and chemical conditions of the planetary nebula NGC 40 through spatially resolved spectroscopic maps. We also introduce a new algorithm –2d_neb– based on the well‐established iraf nebular package, which was developed to enable the use of the spectroscopic maps to easily estimate the astrophysical quantities of ionized nebulae. The 2d_neb was benchmarked, and we clearly show that it works properly, since it compares nicely with the iraf nebular software. Using this software, we derive the maps of several physical parameters of NGC 40. From these maps, we conclude that Te[N ii] shows only a slight temperature variation from region to region, with its values constrained between ∼8000 and 9500 K. Electron densities, on the other hand, have a much more prominent spatial variation, as Ne[S ii] values vary from ∼1000 to 3000 cm−3. Maps of the chemical abundances also show significant variations. From the big picture of our work, we strongly suggest that analysis with spatial resolution be mandatory for more complete study of the physical and chemical properties of planetary nebulae.

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Optical spectrum of the planetary nebula M 2-24

Cited by 30 publications

References 53 publications

Me 1-1: A PN containing a cool star

Me 1-1: A PN containing a cool star

The Detection of C60 in the Well-Characterized Planetary Nebula M1-11

Physico-chemical spectroscopic mapping of the planetary nebula NGC 40 and the 2d_neb, a new 2D algorithm to study ionized nebulae

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