A Survey of 3.3 μm PAH Emission in Planetary Nebulae

Smith, Erin C.; McLean, Ian S.

doi:10.1086/527370

Cited by 12 publications

(9 citation statements)

References 21 publications

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“…This is determined by the abundance of each element during the AGB phase. Spectroscopic observations did not reveal any 3.3 μm PAHs in the core of M2-9 (Smith & McLean 2008), but other PAH features are present in the lobes (this work, Sect. 3.1).…”

Section: Modelmentioning

confidence: 58%

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A disc inside the bipolar planetary nebula M2-9

Lykou

Chesneau

Zijlstra

et al. 2011

A&A

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Aims. Bipolarity in proto-planetary and planetary nebulae is associated with events occurring in or around their cores. Past infrared observations have revealed the presence of dusty structures around the cores, many in the form of discs. Characterising those dusty discs provides invaluable constraints on the physical processes that govern the final mass expulsion of intermediate mass stars. We focus this study on the famous M2-9 bipolar nebula, where the moving lighthouse beam pattern indicates the presence of a wide binary. The compact and dense dusty core in the centre of the nebula can be studied by means of optical interferometry. Methods. M2-9 was observed with VLTI/MIDI at 39-47 m baselines with the UT2-UT3 and UT3-UT4 baseline configurations. These observations are interpreted using a dust radiative transfer Monte Carlo code. Results. A disc-like structure is detected perpendicular to the lobes, and a good fit is found with a stratified disc model composed of amorphous silicates. The disc is compact, 25 × 35 mas at 8 μm and 37 × 46 mas at 13 μm. For the adopted distance of 1.2 kpc, the inner rim of the disc is ∼15 AU. The mass represents a few percent of the mass found in the lobes. The compactness of the disc puts strong constraints on the binary content of the system, given an estimated orbital period 90-120 yr. We derive masses of the binary components between 0.6-1.0 M for a white dwarf and 0.6-1.4 M for an evolved star. We present different scenarios on the geometric structure of the disc accounting for the interactions of the binary system, which includes an accretion disc as well.

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Section: Modelmentioning

confidence: 58%

“…Spectroscopic observations did not reveal any 3.3µm polyaromatic hydrocarbons (PAHs, i.e. signature of C-rich chemistry) in the core of M2-9 (Smith & McLean 2008), but other PAH features are present in the lobes (this work, Section 3.1). The nebula is O-rich with C/O < 0.5 (Liu et al 2001), thus the dust is expected to be O-rich.…”

Section: Modelmentioning

confidence: 69%

A disc inside the bipolar planetary nebula M2-9

Lykou

Chesneau

Zijlstra

et al. 2011

A&A

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“…We did not find any obvious difference in the morphology, the type of the central star, or the dust chemistry of the PNe with the highest and lowest depletion factors. Using the C/O values and the infrared dust features identified in the literature, we infer that 13 PNe of the sample are O-rich (C/O < 1), 8 are C-rich (C/O > 1 and/or they show PAHs or SiC in their spectra), and 7 are uncertain since C/O ∼ 1 or they do not have clear dust features (Cohen et al 1986;Rola & Stasińska 1994;Roche et al 1996;Kholtygin 1998;Kwitter & Henry 1998;Pottasch & Beintema 1999;Henry et al 2000;Liu et al 2000;Casassus et al 2001;Tsamis et al 2003;Liu et al 2004a;Pottasch et al 2004;Tsamis et al 2004;Cohen & Barlow 2005;Wesson et al 2005;Smith & McLean 2008). It is not clear yet which are the main iron compounds condensing onto dust grains, but O-rich environments are expected to have metallic iron grains, silicates, and oxides, whereas C-rich environments can have their iron in the form of metallic grains, Fe 3 C, FeSi, FeS, and FeS 2 (Whittet 2003;Ferrarotti & Gail 2006).…”

Section: Discussionmentioning

confidence: 99%

The Iron Abundance in Galactic Planetary Nebulae

Delgado-Inglada

Rodríguez

Mampaso

et al. 2009

ApJ

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We constrain the iron abundance in a sample of 33 low-ionization Galactic planetary nebulae (PNe) using [Fe III] lines and correcting for the contribution of higher ionization states with ionization correction factors that take into account uncertainties in the atomic data. We find very low iron abundances in all the objects, suggesting that more than 90% of their iron atoms are condensed onto dust grains. This number is based on the solar iron abundance and implies a lower limit on the dust-to-gas mass ratio, solely due to iron, of M dust /M gas ≥ 1.3 × 10 −3 for our sample. The depletion factors of different PNe cover about two orders of magnitude, probably reflecting differences in the formation, growth, or destruction of their dust grains. However, we do not find any systematic difference between the gaseous iron abundances calculated for C-rich and O-rich PNe, suggesting similar iron depletion efficiencies in both environments. The iron abundances of our sample PNe are similar to those derived following the same procedure for a group of 10 Galactic H II regions. These high depletion factors argue for high depletion efficiencies of refractory elements onto dust grains both in molecular clouds and asymptotic giant brach stars, and low dust destruction efficiencies both in interstellar and circumstellar ionized gas.

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“…The PAH features of PNe in the mid-infrared have been intensively investigated with Spitzer (e.g., Bernard-Salas et al 2009;Stanghellini et al 2012Stanghellini et al , 2007. Surveys of the 3.3 µm PAH feature in Galactic PNe were carried out by Roche et al (1996) and Smith & McLean (2008). Their samples were, however, biased towards carbon-rich objects.…”

Section: Pah Features Of Galactic Pne In the Near-infraredmentioning

confidence: 99%

“…The type of dust features (carbon-rich or oxygen-rich) is thought to be closely related to the abundance ratio of nebular gas. Several studies have suggested that the intensities of the PAH features increases with the carbon-to-oxygen abundance (C/O) ratio (e.g., Cohen et al 1986;Cohen & Barlow 2005;Roche et al 1996;Smith & McLean 2008). However, PAH formation both in carbon-rich and oxygen-rich environments has been suggested recently (Guzman-Ramirez et al 2014.…”

Section: Pah Features Of Galactic Pne In the Near-infraredmentioning

confidence: 99%

Akari/Irc Near-Infrared Spectral Atlas of Galactic Planetary Nebulae

Ohsawa

Onaka

Sakon

et al. 2016

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Near-infrared (2.5-5.0 µm) low-resolution (λ/∆λ∼100) spectra of 72 Galactic planetary nebulae (PNe) were obtained with the Infrared Camera (IRC) in the post-helium phase. The IRC, equipped with a 1 ×1 window for spectroscopy of a point source, was capable of obtaining nearinfrared spectra in a slit-less mode without any flux loss due to a slit. The spectra show emission features including hydrogen recombination lines and the 3.3-3.5 µm hydrocarbon features. The intensity and equivalent width of the emission features were measured by spectral fitting. We made a catalog 1 providing unique information on the investigation of the near-infrared emission of PNe. In this paper, details of the observations and characteristics of the catalog are described.Subject headings: Catalogs -planetary nebulae: general InstrumentsAlthough the AKARI /IRC has three channels (Onaka et al. 2007), only the NIR channel was available during the post-helium phase. The field of view of the NIR channel consists of four parts: the N/Nc-window, the Ns-slit, the Np-window, and the Nh-slit (see, Figure 3 in Onaka et al. 2007). The observations were performed with the Np-window, which was designed for point source, slit-less spectroscopy. Spectroscopy with the Np-window allows us to collect all of the flux from an object. The present spectroscopy was carried out with the grism, providing 2.5-5.0 µm spectra with the spectral resolution of λ/∆λ∼100, for point sources ( 3 ). The spectral resolution was degraded for extended objects.The observations were carried out with the observation template IRCZ4. This mode consists of three sequences: the first set is four spectroscopic images, the second set is a broad band image, and the final set is another sequence of four spectroscopic images. Thus, each pointing observation involves eight frames for spectroscopy and one frame for broad-band imaging. Every frame consists of short (4.58 sec) and long (44.41 sec) exposure images. Due to the short integration time, the typical signal-to-noise ratio of the short

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A Survey of 3.3 μm PAH Emission in Planetary Nebulae

Cited by 12 publications

References 21 publications

A disc inside the bipolar planetary nebula M2-9

A disc inside the bipolar planetary nebula M2-9

The Iron Abundance in Galactic Planetary Nebulae

Akari/Irc Near-Infrared Spectral Atlas of Galactic Planetary Nebulae

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