The Amount of Interstellar Carbon Locked in Solid Hydrogenated Amorphous Carbon

Furton, D. G.; Laiho, John W.; Witt, A. N.

doi:10.1086/308016

Cited by 74 publications

(93 citation statements)

References 56 publications

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“…At first sight, our model seems to reproduce the spectrum above 6.5 µm well (see Fig. 3a) if two absorption lines at 6.8 and 7.3 µm are included (C-H stretching mode of hydrogenated amorphous carbon, HAC; Furton et al 1999). However, the lack of the 6.2 µm PAH emission feature and the overall shape of the whole MIR spectrum (see Fig.…”

Section: Iras 00182-7112mentioning

confidence: 74%

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

Ruiz¹,

Risaliti²,

Nardini³

et al. 2013

A&A

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Context. Hyperluminous infrared galaxies (HLIRG) are the most luminous persistent objects in the Universe. They exhibit extremely high star formation rates, and most of them seem to harbour an active galactic nucleus (AGN). They are unique laboratories for investigating the most extreme star formation and its connection to super-massive black hole growth. Aims. The relative AGN and starburst (SB) contributions to the total output in these objects is still debated. Our aim is to disentangle the AGN and SB emission of a sample of thirteen HLIRG. Methods. We studied the MIR low-resolution spectra of a sample of thirteen HLIRG obtained with the Infrared Spectrograph on board Spitzer. The 5−8 µm range is an optimal window for detecting AGN activity even in a heavily obscured environment. We performed an SB/AGN decomposition of the continuum using templates, which has been successfully applied for ULIRG in previous works. Results. The MIR spectra of all sources is largely dominated by AGN emission. By converting the 6 µm luminosity into IR luminosity, we found that ∼80% of the sample shows an IR output dominated by the AGN emission. However, the SB activity is significant in all sources (mean SB contribution ∼30%), showing star formation rates ∼300−3000 M yr −1 . With X-ray and MIR data we estimated the dust covering factor (CF) of these HLIRG, finding that a significant fraction presents a CF consistent with unity. Along with the high X-ray absorption shown by these sources, this suggests that large amounts of dust and gas enshroud the nucleus of these HLIRG, as also observed in ULIRG. Conclusions. Our results agree with previous studies of the IR SED of HLIRG using radiative transfer models, and we find strong evidence that all HLIRG harbour an AGN. Moreover, this work provides further support for the idea that AGN and SB are both crucial to understanding the properties of HLIRG. Our study of the CF supports the hypothesis that HLIRG can be divided into two different populations.

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Section: Iras 00182-7112mentioning

confidence: 74%

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

Ruiz¹,

Risaliti²,

Nardini³

et al. 2013

A&A

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“…Can this uniformity reveal anything about the specific production mechanism of the hydrocarbon solids, the sensitivity of this mechanism to environmental conditions, or (Sakata et al 1987); (b) a UV-irradiated ice (Allamandola et al 1988); (c) an interstellar HAC analog (Furton et al 1999). Sturm et al 2000) showing the baseline used to derive an optical depth spectrum.…”

Section: Dust Production and Surv Viv Val In Galaxiesmentioning

confidence: 99%

Hydrocarbon Dust Absorption in Seyfert Galaxies and Ultraluminous Infrared Galaxies

Mason¹,

Wright²,

Pendleton³

et al. 2004

ApJ

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We present new spectroscopic observations of the 3.4 m absorption feature in the Seyfert galaxies NGC 1068 and NGC 7674 and the ultraluminous infrared galaxy IRAS 08572+3915. A signature of CÀH bonds in aliphatic hydrocarbons, the 3.4 m feature indicates the presence of organic material in Galactic and extragalactic dust. Here we compare the 3.4 m feature in all the galaxies in which it has been detected. In several cases, the signalto-noise ratio and spectral resolution permit a detailed examination of the feature profile, something which has rarely been attempted in extragalactic lines of sight. The 3.4 m band in these galaxies closely resembles that seen in the Galactic diffuse interstellar medium (ISM) and in newly formed dust in a protoplanetary nebula. The similarity implies a common carrier for the carbonaceous component of dust, and one which is resistant to processing in the interstellar and /or circumnuclear medium. We also examine the mid-IR spectrum of NGC 1068, because absorption bands in the 5-8 m region further constrain the chemistry of the 3.4 m band carrier. While weak features like those present in the mid-IR spectrum of diffuse dust toward the Galactic center would be undetectable in NGC 1068, the strong bands found in the spectra of many proposed dust analog materials are clearly absent, eliminating certain candidates and production mechanisms for the carrier. The absence of strong absorption features at 5-8 m is also consistent with the interpretation that the similarity in the 3.4 m feature in NGC 1068 to that in Galactic lines of sight reflects real chemical similarity in the carbonaceous dust.

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“…These are supported by many laboratory astrophysics works on various analogues in the form of pure or hydrogenated carbon materials. Various production techniques are used, such as laser pyrolysis (Schnaiter et al 1999;Herlin et al 1998;Reynaud et al 2001;Galvez et al 2002;Jäger et al 2006), laser ablation (Mennella et al 1999;Jäger et al 2008), photolysis (Dartois et al 2004(Dartois et al , 2005, reactive plasmas (Lee & Wdowiak 1993;Scott & Duley 1996;Furton et al 1999;Goto et al 2000;Godard & Dartois 2010;Godard et al 2011), and others (Jäger et al 1999;Jäger et al 2009;Biennier et al 2009). At Orsay (France), our gas-phase chemical reactor is a low-pressure flame, flat and premixed.…”

Section: Introductionmentioning

confidence: 99%