Crystalline silicon nanoparticles as carriers for the Extended Red Emission

Ledoux, Gilles; Guillois, O.; Huisken, F.; Kohn, Bernhard; Porterat, D.; Reynaud, C.

doi:10.1051/0004-6361:20011136

Cited by 56 publications

(58 citation statements)

References 60 publications

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“…In particular, it should be emphasized that the spectrum of forsterite peaks at about 645-655 nm and at 590 nm is very similar to the ERE of the Red Rectangle. (Witt & Boroson 1990) It should be noted that possible size effects of crystalline silicon nanoparticles have been proposed to explain the gross structure of ERE spectra (Ledoux et al 2001). However, this model can explain only the gross structure of the spectra of ERE sources, and seems unable to explain the characteristic features observed at 590 nm.…”

Section: Discussionmentioning

confidence: 99%

Thermoluminescence of simulated interstellar matter after gamma-ray irradiation

Koike¹,

Nakagawa²,

Koike

et al. 2002

A&A

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Abstract. Interstellar matter is known to be strongly irradiated by cosmic radiation and several types of cosmic ray particles. Simulated interstellar matter, such as synthesized forsterite (Mg 2 SiO 4 ), enstatite (MgSiO 3 ) and magnesite (MgCO 3 ), has been irradiated with 60 Co gamma-rays in liquid nitrogen, and also irradiated with fast neutrons at 10 K and 70 K by making use of the low-temperature irradiation facility of the Kyoto University Reactor (KUR-LTL. Maximum fast neutron dose is 10 17 n f /cm 2 ). After irradiation, samples are stored in liquid nitrogen for several months to allow the decay of induced radioactivity. We measured the luminescence spectra of the gamma ray irradiated samples during warming to 370 K using a spectrophotometer. For the forsterite and magnesite, the spectra exhibit a rather intense peak at about 645-655 nm and 660 nm respectively, whereas luminescence scarcely appeared in the natural olivine sample. The spectra of forsterite is very similar to the ERE of the Red Rectangle.

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Section: Discussionmentioning

confidence: 99%

Thermoluminescence of simulated interstellar matter after gamma-ray irradiation

Koike¹,

Nakagawa²,

Koike

et al. 2002

A&A

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“…Many candidates have been proposed over the past decades: polycyclic aromatic hydrocarbon (PAH) molecules, ions or clusters (D'Hendecourt et al 1986;Vijh et al 2005;Rhee et al 2007;Berné et al 2008), hydrogenated amorphous carbons (HAC or a-C:H) (Duley 1985;Duley & Williams 1988;Witt & Schild 1988;Witt & Boroson 1990;Furton & Witt 1993;Duley et al 1997;Seahra & Duley 1999), quenched carbonaceous composites (QCC) (Sakata et al 1992;Wada et al 2009), nanodiamonds (Duley 1988;Chang et al 2006), C 60 (Webster 1993), and also non carbon-based materials such as crystalline silicon nanoparticules (SNP) (Ledoux et al 1998;Witt et al 1998;Ledoux et al 2001;Smith & Witt 2002).…”

Section: ) H II Regionsmentioning

confidence: 99%

“…Rusli et al 1996) and only for a few excitation wavelengths. The few results for absolute a-C:H PL efficiencies (Furton & Witt 1993;Furton et al 1999;Ledoux et al 2001) vary over four orders of magnitude. In addition, optical effects modifying the apparent efficiency as compared to the intrinsic efficiency are not properly taken into account.…”

Section: ) H II Regionsmentioning

confidence: 99%

“…The a-C:H PL data are those presented in Fig. 10 of this paper, together with data from Lin & Feldman (1982), Lin & Feldman (1983), Watanabe et al (1982), Wagner & Lautenschlager (1986), Chernyshov et al (1991), Xu et al (1993), Rusli et al (1996), Ledoux et al (2001), and Dartois et al (2005). The ERE observations data are taken from Fig.…”

Section: Photoluminescence Spectramentioning

confidence: 99%

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Photoluminescence of hydrogenated amorphous carbons

Godard

Dartois

2010

A&A

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Context. Hydrogenated amorphous carbons (a-C:H or HAC) have proved to be excellent analogs of interstellar dust observed in galaxies diffuse interstellar medium (DISM) through infrared vibrational absorption bands (3.4 μm, 6.8 μm, and 7.2 μm bands). They exhibit photoluminescence (PL) after excitation by UV-visible photons, and are possible carriers for the extended red emission (ERE), a broad red emission band observed in various interstellar environments. Aims. As many candidate materials/molecules can photoluminesce in the visible, along with the carrier abundance, the PL efficiency represents one of the strongest constraints set by such ERE observations. We wish to precisely characterize the PL behavior of a-C:H as a family of materials. Methods. The a-C:H samples are produced in the form of films deposited on substrates by plasma-enhanced chemical vapor deposition. The produced films were analyzed in transmission by UV-visible and IR spectroscopy, and the wavelength dependent PL spectra were recorded. The intrinsic absolute quantum yield η was then rigorously calculated taking self-absorption of the PL by the film and interfaces effects into account. Results. A wide range of different laboratory synthesized a-C:H were analyzed. Their PL properties are dependent on the optical gap E 04 : when E 04 decreases from 4.3 eV to 2.8 eV, the a-C:H vary from highly (η ∼ 1%) yellow photoluminescent soft materials to hard materials that emit a wider PL band in the red spectral range, with a lower efficiency (η ∼ 0.01−0.1%). For any given a-C:H, the PL characteristics (central wavelength, band width and efficiency) are found to be essentially constant over the explored excitation range (λ exc > ∼ 250 nm). We compared the characteristics of the produced interstellar dust analog to the constraints imposed by the ERE observations. Conclusions. As for ERE observations, PL efficiencies and band widths of a-C:H are both correlated to the PL central wavelengths. The excitation responsible for the a-C:H emission is efficient over a wide spectral range that matches the ERE excitation. The present a-C:H encounter difficulties for the diffuse ISM ERE observations (η ≥ 10%) in simultaneously satisfying the high quantum yield criteria and PL spectral characteristics. We still need to investigate the role of a small number of residual oxygen atoms in the laboratory-produced a-C:H network in quenching the PL yield, as well as to consider the interstellar temperature effect for our analogs.

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“…spectra at longer wavelengths (∼20-45 μm) have been associated with crystalline silicates, specifically olivines (Mg x Fe 1−x ) 2 SiO 4 and pyroxenes (Mg x Fe 1−x SiO 3 ) (Waters et al 1998). In the optical regime the spectrum is dominated by extended red emission (ERE), a strong and broad emission feature that stretches over about 250 nm in the optical (Schmidt et al 1980) and by broad blue luminescence in the UV (Vijh et al , 2005(Vijh et al , 2006) that may originate from silicate nano particles or carbonaceous grains (see Duley 1985;Witt & Boroson 1990;Witt et al 1998;Ledoux et al 1998Ledoux et al , 2001Van Winckel et al 2002;. Superimposed on the ERE a chaotic pattern of narrow emission features has been found.…”

Section: Introductionmentioning

confidence: 99%

The offset dependent behavior of narrow optical emission features in the Red Rectangle proto-planetary nebula

Wehres

Linnartz

Winckel

et al. 2011

A&A

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Context. The Red Rectangle proto-planetary nebula provides a unique laboratory to study the physical conditions and chemical processes in stellar outflows. Snapshots of the ongoing chemical evolution are obtained by monitoring spectra as function of the offset from the central star. Aims. The focus in this study is on the characterization of narrow optical emission features, that are superimposed on top of extended red emission (ERE). The primary aim is to provide a two-dimensional catalogue of these features for offsets varying from 3 to 20 from the central star. Methods. Medium resolution emission spectra for this catalogue have been obtained through optical long-slit measurements using the New Technology Telescope (EMMI-NTT) in La Silla, Chile. Results. The recorded spectra cover the range between 5550 and 6800 Å. A complete overview of the central band positions and bandwidths (FWHMs) is provided for both stronger (previously reported) and weaker narrow features. Only some bands are omnipresent in the nebula outflows and other bands only appear further away from the central star.Conclusions. The optical emission bands show intensity variations over the nebula. We suggest that these variations reflect a spatially resolved photochemistry where larger species are photolysed, producing daughter molecules which may be the carriers of the optical emission bands.

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Crystalline silicon nanoparticles as carriers for the Extended Red Emission

Cited by 56 publications

References 60 publications

Thermoluminescence of simulated interstellar matter after gamma-ray irradiation

Thermoluminescence of simulated interstellar matter after gamma-ray irradiation

Photoluminescence of hydrogenated amorphous carbons

The offset dependent behavior of narrow optical emission features in the Red Rectangle proto-planetary nebula

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