HIGH-DISPERSION SPECTRUM OF THE HALO PLANETARY NEBULA DdDm 1

Otsuka, Masaaki; Hyung, Siek; Lee, Seongjae; Izumiura, Hideyuki; Tajitsu, Akito

doi:10.1088/0004-637x/705/1/509

Cited by 25 publications

(20 citation statements)

References 60 publications

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“…This anomalously low abundance is entirely the result of low spatial resolution ground-based observations averaging over the strong spatial variation of [O III] λ4363/λ5007 (TP97; Miszalski et al 2009). TP97 measured an O abundance of 8.5 dex from HST spectroscopy of the inner nebula and yet it is still incorrectly referred to as a halo PN in the literature (Otsuka et al 2009;Lutz et al 2010;Stasińska et al 2010;Schönberner et al 2010). To settle the issue we have recalculated the chemical abundances of M 2-29 from our spectrum of the outer nebula.…”

Section: Chemical Abundancesmentioning

confidence: 99%

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

Miszalski¹,

Mikołajewska²,

Köppen³

et al. 2011

A&A

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The central star of the planetary nebula (CSPN) M 2-29 shows an extraordinary R Coronae Borealis-like fading event in its optical lightcurve. The only other CSPN to show these events are CPD-56 • 8032 (Hen 3-1333) and V651 Mon (NGC 2346). Dust cloud formation in the line of sight appears responsible but the exact triggering mechanism is not well understood. Understanding how planetary nebulae (PNe) trigger dust obscuration events may help understand the same process in a wide range of objects including Population-I WC9 stars, symbiotic stars and perhaps asymptotic giant branch (AGB) stars with long secondary periods (LSPs). A binary scenario involving an eccentric, wide companion that triggers dust formation via interaction at periastron is a potential explanation that has been suggested for LSP variables. Model fits to the lightcurves of CPD-56 • 8032 and M 2-29 show the dust forms in excess of 70 AU at the inner edge of a dust disk. In the case of CPD-56 • 8032 this radius is far too large to coincide with a binary companion trigger, although a binary may have been responsible for the formation of the dust disk. We find no direct evidence to support previous claims of binarity in M 2-29 either from the OGLE lightcurve or deep medium-resolution VLT FLAMES spectroscopy of the CSPN. We classify the CSPN as Of(H) with T eff = 50 ± 10 kK and log g = 4.0 ± 0.3. We find a mean distance of 7.4 ± 1.8 kpc to M 2-29 at which the M V = −0.9 mag CSPN could potentially hide a subgiant luminosity or fainter companion. A companion would help explain the multiple similarities with D -type symbiotic stars whose outer nebulae are thought to be bona-fide PNe. The 7.4 kpc distance, oxygen abundance of 8.3 dex and Galactic coordinates ( = 4.0, b = −3.0) prove that M 2-29 is a Galactic Bulge PN and not a Halo PN as commonly misconceived.

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Section: Chemical Abundancesmentioning

confidence: 99%

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

Miszalski¹,

Mikołajewska²,

Köppen³

et al. 2011

A&A

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“…Simultaneously, the angular extent of the nebula measured using the estimated distance and radii should match the angular extent of the nebula as observed in the 2D image. The readers may find a similar argument in Otsuka et al (2009).…”

Section: Ionization Characteristics: Photoionization Modelingmentioning

confidence: 66%

Morphology and ionization characteristics of planetary nebulae PB 1 and PC 19

Bandyopadhyay,

Das,

Mondal

et al. 2020

Preprint

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We present results of our study of two planetary nebulae (PNe), PB1 and PC 19. We use the optical spectra of these two PNe observed at 2 m Himalayan Chandra Telescope and also archival and literature data for the study. We use the morphokinematic code SHAPE to construct 3D morphologies of the PNe and the photoionization code CLOUDY to model the observed spectra. The 3D model of PB 1 consists of an elongated shell surrounded by a bipolar halo and that of PC 19 consists of an open lobed bipolar structure and a spiral filamentary pair. We analyze the ionization structure of the PNe by deriving several plasma parameters and by photoionization modelling. We estimate the elemental abundances of the the elements, He, C, N, O, Ne, S, Ar, and Cl, from our analysis. We find He, C and N abundances to be significantly higher in case of PB 1. We estimate different physical parameters of the central stars, namely effective temperature, luminosity and gravity, and of the nebula, namely hydrogen density profiles, radii, etc., from photoionization modelling. We estimate distances to the PNe as ∼4.3 kpc for PB 1 and as ∼5.6 kpc for PC 19 by fitting the photoionization models to absolute observed fluxes. Progenitor masses are estimated from theoretical evolutionary trajectories and are found to be ∼1.67 and ∼2.38 M for PB 1 and PC 19, respectively.

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“…With the atomic constant as given in Aller (1984) and Osterbrock (1989), the ratios of some diagnostically useful lines would allow us to derive the electron temperatures and densities of the gas. The recent up-to-date data can be found in Otsuka et al (2009). Table 4 gives the nebular physical conditions, T e and log N e , derived based on the combined line intensities, I(HES), i.e., Col. 6 of Table 2, while Fig.…”

Section: Nebular Physical Conditionsmentioning

confidence: 99%

High-resolution spectra of the planetary nebula NGC 6803

Lee

Hyung

2012

A&A

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We present the high-dispersion spectra of the elliptical ring shaped planetary nebula NGC 6803, secured with the Hamilton Echelle Spectrograph attached to the 3-m Shane telescope of Lick Observatory. Numerous lines from neutral to quadruply ionized ions are presented in the wavelength region from 3650 to 9900 Å. We also use the low dispersion UV spectral data obtained with the 60-cm interstellar ultraviolet explorer. In spite of its simplistic symmetrical bilateral shape, the diagnostics imply that the physical condition of the nebular shell is very complex with a huge density range of 1300−80 000 cm −3. A comparison of the 1995 and 2001 [Ar iv] data suggests that the density increase occurred near the inner shell boundary. In spite of a huge ionization potential range, the average electron temperature indicated by primary diagnostic lines is relatively low, i.e., T e ≤ 9500 K, except for [Cl iv], from which we derive a temperature that is around 11 500 K. We derived the chemical abundances of He, C, N, O, Ne, S, Ar, Cl, and K, based on the physical condition suggested by diagnostics and photo-ionization analysis. The chemical abundances of NGC 6803 are mostly enhanced when compared with the average Galactic planetary nebula. The effective temperature of its central star appears to be about 90 000 K and its luminosity about 2400 L , assuming a distance of 3000 pc. The evolutionary track implies that NGC 6803 might have been evolved from a companion star of about 1.0 M in a binary system, or from a single progenitor of about 1.5 M , born in a metal-rich zone near the Galactic plane.

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HIGH-DISPERSION SPECTRUM OF THE HALO PLANETARY NEBULA DdDm 1

Cited by 25 publications

References 60 publications

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

Morphology and ionization characteristics of planetary nebulae PB 1 and PC 19

High-resolution spectra of the planetary nebula NGC 6803

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