High Excitation ISM and Gas

Peeters, E.; Martín-Hernández, Nieves Leticia; Rodriguez‐fernandez, Nemesio; Tielens, Xander

doi:10.1007/s11214-005-8070-1

Cited by 8 publications

(8 citation statements)

References 85 publications

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“…Scaling factors applied to each source are the following: Orion Pk2 band 4 -0.52; Orion Pk1 band 3D -1.56, band 4 -0.99; Orion IRc2 band 3D -0.53, band 4 -0.42; Orion Bar band 3D -0.40; S106 band 3D -1.27, band 4 -0.58; IRAS02575 band 3D -4.82, band 4 -3.86; IRAS10589 band 3D -2.46, band 4 -1.77. who claim them to be artefacts. See also Peeters et al (2005) who cites a paper in preparation by Kemper et al, but which has not so far been published to our knowledge.…”

Section: Crystalline Silicate and Other Features At 30-45 µMmentioning

confidence: 99%

Absorption at 11 μm in the interstellar medium and embedded sources: evidence for crystalline silicates

Wright

Duy

Lawson

2016

Mon. Not. R. Astron. Soc.

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An absorption feature is occasionally reported around 11 µm in astronomical spectra, including those of forming stars. Candidate carriers include water ice, polycyclic aromatic hydrocarbons (PAHs), silicon carbide, crystalline silicates or even carbonates. All are known constituents of cosmic dust in one or more types of environments, though not necessarily together. In this paper we present new ground-based 8-13 µm spectra of one evolved star, several embedded young stellar objects (YSOs) and a background source lying behind a large column of the interstellar medium (ISM) toward the Galactic Centre. Our observations, obtained at a spectral resolution of ∼ 100, are compared with previous lower resolution data, as well as data obtained with the Infrared Space Observatory (ISO) on these and other targets. By presenting a subset of a larger sample our aim is to establish the reality of the feature and subsequently speculate on its carrier. All evidence points toward crystalline silicate. For instance, the 11 µm band profile is well matched with the emissivity of crystalline olivine. Furthermore, the apparent association of the absorption feature with a sharp polarisation signature in the spectrum of two previously reported cases suggests a carrier with a relatively high band strength compared to amorphous silicates. If true, this would either set back the evolutionary stage in which silicates are crystallised, either to the embedded phase or even before within the ISM, or else the silicates ejected from the outflows of evolved stars retain some of their crystalline identity during their long residence in the ISM.

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Section: Crystalline Silicate and Other Features At 30-45 µMmentioning

confidence: 99%

Absorption at 11 μm in the interstellar medium and embedded sources: evidence for crystalline silicates

Wright

Duy

Lawson

2016

Mon. Not. R. Astron. Soc.

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“…Peeters et al (2005) review the ISO spectroscopic observations of compact and evolved H ii regions and the PDRs surrounding them. They find gas temperatures in the PDRs between 100 K ( NGC 2024) and 200-500 K (S106IR) and densities between 10 4 cm À3 (W75N ) and 10 6 cm À3 (NGC 2024).…”

Section: Introductionmentioning

confidence: 99%

Infrared Dust Bubbles: Probing the Detailed Structure and Young Massive Stellar Populations of Galactic HiiRegions

Watson

Povich

Churchwell

et al. 2008

ApJ

183

293

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We present an analysis of wind-blown, parsec-sized, mid-infrared bubbles and associated star formation using the GLIMPSE IRAC, MIPSGAL MIPS, and MAGPIS VLA surveys. Three bubbles from the Churchwell et al. catalog were selected. The relative distribution of the ionized gas (based on 20 cm emission), PAH emission (based on 8 m, 5.8 m, and lack of 4.5 m emission), and hot dust (24 m emission) is compared. At the center of each bubble there is a region containing ionized gas and hot dust surrounded by PAHs. We identify the likely source(s) of the stellar wind and ionizing flux producing each bubble based on SED fitting to numerical hot stellar photosphere models. Candidate YSOs are also identified using SED fitting, including several sites of possible triggered star formation.

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“…FIR forbidden lines are less sensitive to the electron temperature than optical forbidden lines in H II regions, and observations with balloon-borne and airborne telescopes have been used to determine physical properties such as the electron density and elemental abundance (Rubin et al 1988;Simpson et al 1995Simpson et al , 2004. The long-wavelength spectrometer (LWS; Clegg et al 1996) onboard the Infrared Space Observatory (ISO; Kessler et al 1996) provided continuous spectra of the wavelength range 43−197 μm, enabling us to investigate the physical conditions of the gas in the ionized and/or photodissociation regions (PDRs) by measuring several emission lines and the continuum emission (Martín-Hernández et al 2002;see Abergel et al 2005;and Peeters et al 2005, for reviews). Since the LWS was a single-beam instrument, raster-scan observations were needed to investigate the spatial distribution of emission spectra and physical properties (e.g.…”

Section: Introductionmentioning

confidence: 99%

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Okada

Kawada

Murakami

et al. 2010

A&A

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Aims. We investigate the structure of the interstellar medium (ISM) and identify the location of possible embedded excitation sources from far-infrared (FIR) line and mid-infrared continuum emission maps. Methods. We carried out imaging spectroscopic observations of four giant Galactic star-forming regions with the Fourier transform spectrometer (FTS) onboard AKARI. We obtained [O III] 88 μm and [C II] 158 μm line intensity maps of all the regions: G3.270-0.101, G333.6-0.2, NGC 3603, and M 17. Results. For G3.270-0.101, we obtained high-spatial-resolution [O III] 88 μm line-emission maps and a FIR continuum map for the first time, which imply that [O III] 88 μm emission identifies the excitation sources more clearly than the radio continuum emission. In G333.6-0.2, we found a local [O III] 88 μm emission peak, which is indicative of an excitation source. This is supported by the 18 μm continuum emission, which is considered to trace the hot dust distribution. For all regions, the [C II] 158 μm emission is distributed widely as suggested by previous observations of star-forming regions. Conclusions. We conclude that [O III] 88 μm emission traces the excitation sources more accurately than the radio continuum emission, especially where there is a high density and/or column density gradient. The FIR spectroscopy provides a promising means of understanding the nature of star-forming regions.

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High Excitation ISM and Gas

Cited by 8 publications

References 85 publications

Absorption at 11 μm in the interstellar medium and embedded sources: evidence for crystalline silicates

Absorption at 11 μm in the interstellar medium and embedded sources: evidence for crystalline silicates

Infrared Dust Bubbles: Probing the Detailed Structure and Young Massive Stellar Populations of Galactic HiiRegions

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

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