Comparison of dust‐to‐gas ratios in luminous, ultraluminous, and hyperluminous infrared galaxies

Contini, M.; Contini, T.

doi:10.1002/asna.200710782

Cited by 11 publications

(18 citation statements)

References 140 publications

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“…Previous calculations of models including dust (Contini, Viegas & Prieto 2004; Contini & Contini 2007) show that the peak shifts to higher frequencies by (1) increasing V s , that is increasing the collisional heating of dust grains; (2) increasing U , that is increasing radiation heating of the grains; and (3) reducing the radius of the grains. Excluding collisional heating derived from a higher velocity which would imply very broad line profiles, the only parameters that we can alter are U and a gr .…”

Section: Spitzer Observationsmentioning

confidence: 98%

An analysis of infrared emission spectra from the regions near the Galactic Centre

Contini¹

2009

Monthly Notices of the Royal Astronomical Society

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We present consistent modelling of line and continuum infrared (IR) spectra in the region close to the Galactic Centre. The models account for the coupled effect of shocks and photoionization from an external source. The results show that the shock velocities range between ∼65 and 80 km s−1 and the pre‐shock densities between 1 cm−3 in the interstellar medium (ISM) to 200 cm−3 in the filamentary structures. The pre‐shock magnetic field increases from 5 × 10−6 G in the surrounding ISM to ∼8 × 10−5 G in the arched filaments. The stellar temperatures are ∼38 000 K in the Quintuplet cluster and ∼27 000 K in the Arches Cluster. The ionization parameter is relatively low (<0.01) with the highest values near the clusters, reaching a maximum >0.01 near the Arches Cluster. Depletion from the gaseous phase of Si is found throughout the whole observed region, indicating the presence of silicate dust. Grains including iron are concentrated throughout the arched filaments. The modelling of the continuum spectral energy distribution in the IR range indicates that a component of dust at temperatures of ∼100–200 K is present in the central region of the Galaxy. Radio emission appears to be thermal bremsstrahlung in the E2–W1 filaments crossing strip; however, a synchrotron component is not excluded. More data are necessary to resolve these questions.

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Section: Spitzer Observationsmentioning

confidence: 98%

An analysis of infrared emission spectra from the regions near the Galactic Centre

Contini¹

2009

Monthly Notices of the Royal Astronomical Society

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“…This is an interesting issue not only in the specific case of symbiotic systems but also in the understanding of IR emission from starburst galaxies and luminous IR galaxies (e.g. Contini & Contini 2007), which is generally attributed to supernovae (e.g. Dweck 1987).…”

Section: The Continuum Sedmentioning

confidence: 99%

The spectral energy distribution of D-type symbiotic stars: the role of dust shells

Angeloni¹,

Contini²,

Ciroi³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We have collected continuum data of a sample of D‐type symbiotic stars. By modelling their spectral energy distribution in a colliding‐wind theoretical scenario we have found characteristics common to all the systems: (1) at least two dust shells are clearly present, one at ∼1000 K and the other at ∼400 K; they dominate the emission in the infrared; (2) the radio data are explained by thermal self‐absorbed emission from the reverse shock between the stars; while (3) the data in the long wavelength tail come from the expanding shock outwards the system; (4) in some symbiotic stars, the contribution from the white dwarf in the UV is directly seen. Finally, (5) for some objects soft X‐ray emitted by bremsstrahlung downstream of the reverse shock between the stars is predicted. The results thus confirm the validity of the colliding‐wind model and the important role of the shocks. The comparison of the fluxes calculated at the nebula with those observed at the Earth reveals the distribution throughout the system of the different components, in particular the nebulae and the dust shells. The correlation of shell radii with the orbital period shows that larger radii are found at larger periods. Moreover, the temperatures of the dust shells regarding the sample are found at ∼1000 and ≤400 K, while in the case of late giants they spread more uniformly throughout the same range.

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“…They were recognised in local as well as in high z galaxies (e.g. Contini & Contini 2007). However, in some different ranges of the continuum, in particular in the radio and ultraviolet (UV)-X-ray, data are better explained by the bremsstrahlung emitted from the gaseous clouds within the host galaxy, which also emit the spectral lines.…”

Section: Introductionmentioning

confidence: 99%

NGC 4993 and other short gamma-ray burst host galaxies

Contini

2018

A&A

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We present the spectral detailed modelling of NGC 4993 -the host galaxy of GW 170817 -and other short gamma-ray burst (SGRB) host galaxies. In order to determine their physical conditions and the element abundances, we have gathered spectroscopic and photometric data from the literature. The observation data are sometimes missing, preventing us from fully constraining the model. However, for most of the SGRB hosts the [OIII]5007/Hβ and [NII]6548/Hα line ratios are reported. The analysis of NGC 4993 by a composite model (photoionization+shock) confirms that an active galactic nucleus (AGN), most probably a low-ionization nuclear emission-line region (LINER) or a low-luminosity AGN (LLAGN) is the gas photoionization source. Shock velocities and preshock densities are similar to those found in the narrow line region of AGN. O/H and N/H have solar values. For the other SGRB of the sample, we found that O/H ratios are nearly solar, while N/H covers a much larger range of values at redshifts close to 0.4. In NGC 4993, the relative contribution to the spectral energy distribution of an old stellar population, characterized by a blackbody temperature of T bb = 4000 K, with respect to bremsstrahlung is higher by a factor of >100 than in most of the local AGN and starburst (SB) galaxies. For the other SGRB that compose the sample, T bb ranges between 2000 K for SGRB 100206A and 8000 K for SGRB 111117A.

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Comparison of dust‐to‐gas ratios in luminous, ultraluminous, and hyperluminous infrared galaxies

Cited by 11 publications

References 140 publications

An analysis of infrared emission spectra from the regions near the Galactic Centre

An analysis of infrared emission spectra from the regions near the Galactic Centre

The spectral energy distribution of D-type symbiotic stars: the role of dust shells

NGC 4993 and other short gamma-ray burst host galaxies

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