Dust outflows from quiescent spiral disks

Alton, P. B.; Rand, Richard J.; Xilouris, E. M.; Bevan, S.; Ferguson, Annette M. N.; Davies, Jonathan Ivor; Bianchi, S.

doi:10.1051/aas:2000103

Cited by 41 publications

(61 citation statements)

References 61 publications

(87 reference statements)

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“…• 01 (Bianchi 2007), the galaxy is displaying a dust lane, visible along the entire disc and with an extensive vertical dust distribution (Howk & Savage 1999;Thompson et al 2004), although we note that Alton et al (2000a) consider this galaxy to be too highly inclined to make any unambiguous claims about extraplanar dust. A global fit of extinction by the dust distribution to optical images was carried out in Bianchi (2007), giving a dust scalelength of 70 or 6.7 kpc, which is 75% larger than the stellar disc scalelength.…”

Section: Ngc 4217mentioning

confidence: 88%

“…The dust lane extends from the centre out to the edges along the major axis, and although Howk & Savage (1999) state that the galaxy has no detectable vertically extended dust or ionised gas, Alton et al (2000a) claim this galaxy to be insufficiently edge-on to make any definite statements about extraplanar dust. The dust distribution has been previously modelled using global fits to the dust lane extinction in optical images (Xilouris et al 1999), leading to a dust scalelength of 100 or 7.8 kpc, which is about 10% larger than the corresponding stellar disc scalelength.…”

Section: Ngc 5907mentioning

confidence: 96%

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HERschelObservations of Edge-on Spirals (HEROES)

Verstappen

Fritz

Baes

et al. 2013

A&A

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Context. Edge-on spiral galaxies with prominent dust lanes provide us with an excellent opportunity to study the distribution and properties of the dust within them. The HEROES project was set up to observe a sample of seven large edge-on galaxies across various wavelengths for this investigation. Aims. Within this first paper, we present the Herschel observations and perform a qualitative and quantitative analysis on them, and we derive some global properties of the far infrared and submillimetre emission. Methods. We determine horizontal and vertical profiles from the Herschel observations of the galaxies in the sample and describe the morphology. Modified black-body fits to the global fluxes, measured using aperture photometry, result in dust temperatures and dust masses. The latter values are compared to those that are derived from radiative transfer models taken from the literature. Results. On the whole, our Herschel flux measurements agree well with archival values. We find that the exponential horizontal dust distribution model often used in the literature generally provides a good description of the observed horizontal profiles. Three out of the seven galaxies show signatures of extended vertical emission at 100 and 160 μm at the 5σ level, but in two of these it is probably due to deviations from an exactly edge-on orientation. Only for NGC 4013, a galaxy in which vertically extended dust has already been detected in optical images, we can detect vertically extended dust, and the derived scaleheight agrees with the value estimated through radiative transfer modelling. Our analysis hints at a correlation between the dust scaleheight and its degree of clumpiness, which we infer from the difference between the dust masses as calculated from modelling of optical data and from fitting the spectral energy distribution of Herschel datapoints.

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Section: Ngc 4217mentioning

confidence: 88%

Section: Ngc 5907mentioning

confidence: 96%

HERschelObservations of Edge-on Spirals (HEROES)

Verstappen

Fritz

Baes

et al. 2013

A&A

Self Cite

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“…To evaluate the latter uncertainty we fitted a modified black body from 100 to 200 µm assuming an β = 1.5. Grain emissivities larger than 2 or smaller than 1.5 have not been observed at these wavelengths in average interstellar medium conditions of normal galaxies (see Alton et al 2000 and references therein). The temperatures obtained are ∼ 15% smaller than the values given in Table 5.…”

Section: The Spectral Energy Distributionsmentioning

confidence: 99%

“…Using SCUBA sub-millimeter observations of the nearby normal galaxy NGC 891 Israel et al (1999) found a cold dust component at a temperature ∼ 21 K. For the same galaxy Alton et al (2000) found that, though the bulk of the sub-millimeter emission is associated with the molecular gas, it extends beyond the optical radius, where it follows the distribution of the neutral HI gas. This dust component could be easily removed during the ram pressure stripping process occurring on cluster galaxies.…”

Section: Introductionmentioning

confidence: 98%

Mid and Far IR properties of late-type galaxies in the Coma and A1367 clusters: ISOCAM and ISOPHOT observations

Contursi

Boselli

Gavazzi

et al. 2001

A&A

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Abstract. We present Mid (MIR) and Far (FIR) Infrared observations of 18 spiral/irregular galaxies belonging to the Coma and A1367 clusters, carried out with the CAM and PHOT instruments on board the ISO satellite. Complementary photometry from the UV to the Near Infrared (NIR) together with Hα imaging, HI and 12 CO line measurements allow us to study the relationships between the IR emission and the star formation properties of these galaxies. Most of the resolved galaxies show extended MIR emission throughout their disks even where no Hα emission is present. This suggests that the Aromatic carriers can be excited by the general interstellar radiation field (ISRF), i.e. by visible photons. Only close to HII regions the UV photons are the principal sources of Aromatic carrier excitation. However, when the UV radiation field becomes intense enough these carriers can be destroyed. The average integrated 15/6.75 µm ratio of the observed galaxies is ∼ 1, i.e. the typical value for the photodissociation regions (PDRs). This suggests that, despite the high star formation rate (SFR) and the very luminous HII regions of these galaxies, their integrated MIR emission is dominated by PDR-like regions rather than HII-like regions. A cold dust component with average temperature ∼ 22 K exists in most of the target galaxies, probably arising from big dust grains (BGs) in thermal equilibrium with the ISRF. The contribution to the BGs heating from the ionizing stars decreases with increasing wavelength. A warmer dust component whose emission dominates the spectrum between 20 and 100 µm is likely to exist. This is probably due to both Very Small Grains (VSGs) and warm BGs emission. The dust to gas ratio of the target galaxies is comparable to that of the solar neighborhood. There is a weak trend between the dust total mass and both the atomic and molecular gas content. The MIR and FIR properties of the analyzed galaxies do not seem to be affected by the environment despite the fact that most of the targets are interacting with the Intra-Cluster-Medium.

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“…These galaxies are closer to edge-on, meaning that some of the dust in the line of sight may be far from the nucleus. As the scale heights of dust in spiral galaxies tend to be small (Alton et al 2000), though, these spectra are likely to still contain a substantial contribution from nuclear dust. This suggests that the hydrocarbons in the dust in these galaxies are robust enough to survive unchanged in quite harsh conditions.…”

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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Dust outflows from quiescent spiral disks

Cited by 41 publications

References 61 publications

HERschelObservations of Edge-on Spirals (HEROES)

HERschelObservations of Edge-on Spirals (HEROES)

Mid and Far IR properties of late-type galaxies in the Coma and A1367 clusters: ISOCAM and ISOPHOT observations

Hydrocarbon Dust Absorption in Seyfert Galaxies and Ultraluminous Infrared Galaxies

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