Far-infrared emission from the galaxy in extra-galactic windows

Boulanger, F.; Abergel, A.; Bernard, J. P.; Désert, F.‐X.; Lagache, G.; Puget, J.‐L.; Burton, W. B.; Hartmann, D.

doi:10.1063/1.49215

Cited by 239 publications

(392 citation statements)

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“…Our data analysis makes use of, and explores, the dust/gas correlation by spatially correlating Planck and IRAS data with H i observations. More specifically our study extends previous work on the diffuse ISM SED carried out with 7 • resolution Far InfraRed Absolute Spectrophotometer (FIRAS) data (Boulanger et al 1996) or with 5 resolution 100 μm IRAS data (Reach et al 1998). …”

Section: Introductionsupporting

confidence: 66%

“…In particular Boulanger et al (1996) studied this relation over the whole high Galactic latitude sky. They reported a tight dust-H i correlation for W HI < 250 K km s −1 , corresponding to N HI < 4.6 × 10 20 cm −2 .…”

Section: Modelmentioning

confidence: 99%

“…Many studies, mostly using the IRAS and COBE data compared with various 21-cm surveys (Boulanger & Pérault 1988;Joncas et al 1992;Jones et al 1995;Boulanger et al 1996;Arendt et al 1998;Reach et al 1998;Lockman & Condon 2005;MivilleDeschênes et al 2005), have revealed the strong correlation between far-infrared/submm dust emission and 21-cm integrated emission W HI 3 at high Galactic latitudes. In particular Boulanger et al (1996) studied this relation over the whole high Galactic latitude sky.…”

Section: Modelmentioning

confidence: 99%

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Planckearly results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo

Abergel

Ade

Aghanim

et al. 2011

A&A

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183

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This paper presents the first results from a comparison of Planck dust maps at 353, 545 and 857 GHz, along with IRAS data at 3000 (100 μm) and 5000 GHz (60 μm), with Green Bank Telescope 21-cm observations of H i in 14 fields covering more than 800 deg 2 at high Galactic latitude. The main goal of this study is to estimate the far-infrared to sub-millimeter (submm) emissivity of dust in the diffuse local interstellar medium (ISM) and in the intermediate-velocity (IVC) and high-velocity clouds (HVC) of the Galactic halo. Galactic dust emission for fields with average H i column density lower than 2 × 10 20 cm −2 is well correlated with 21-cm emission because in such diffuse areas the hydrogen is predominantly in the neutral atomic phase. The residual emission in these fields, once the H i-correlated emission is removed, is consistent with the expected statistical properties of the cosmic infrared background fluctuations. The brighter fields in our sample, with an average H i column density greater than 2 × 10 20 cm −2 , show significant excess dust emission compared to the H i column density. Regions of excess lie in organized structures that suggest the presence of hydrogen in molecular form, though they are not always correlated with CO emission. In the higher H i column density fields the excess emission at 857 GHz is about 40% of that coming from the H i, but over all the high latitude fields surveyed the molecular mass faction is about 10%. Dust emission from IVCs is detected with high significance by this correlation analysis. Its spectral properties are consistent with, compared to the local ISM values, significantly hotter dust (T ∼ 20 K), lower submm dust opacity normalized per H-atom, and a relative abundance of very small grains to large grains about four times higher. These results are compatible with expectations for clouds that are part of the Galactic fountain in which there is dust shattering and fragmentation. Correlated dust emission in HVCs is not detected; the average of the 99.9% confidence upper limits to the emissivity is 0.15 times the local ISM value at 857 and 3000 GHz, in accordance with gas phase evidence for lower metallicity and depletion in these clouds. Unexpected anti-correlated variations of the dust temperature and emission cross-section per H atom are identified in the local ISM and IVCs, a trend that continues into molecular environments. This suggests that dust growth through aggregation, seen in molecular clouds, is active much earlier in the cloud condensation and star formation processes.

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Section: Introductionsupporting

confidence: 66%

Section: Modelmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

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Planckearly results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo

Abergel

Ade

Aghanim

et al. 2011

A&A

Self Cite

183

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“…DIRBE and FIRAS on board COBE produced all-sky maps of resolutions 40 and 7 • , respectively. The dust temperature is found to be on average ∼17.5 K (with β = 2) in the diffuse atomic medium (Boulanger et al 1996) and to be lower in molecular clouds with no embedded bright stars (Lagache et al 1998). Small patches of bright molecular clouds have been observed in more detail from the ground by the JCMT (Johnstone et al 2006), and from the balloon borne experiments PRONAOS (Ristorcelli et al 2006) and Archeops (Désert et al 2008).…”

Section: Interstellar Dustmentioning

confidence: 99%

Evolution of interstellar dust withHerschel. First results in the photodissociation regions of NGC 7023

Abergel¹,

Arab²,

Compiègne

et al. 2010

A&A

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Context. In photodissociation regions (PDRs), the physical conditions and the excitation evolve on short spatial scales as a function of depth within the cloud, providing a unique opportunity to study how the dust and gas populations evolve with the excitation and physical conditions. The mapping of the PDRs in NGC 7023 performed during the science demonstration phase of Herschel is part of the "Evolution of interstellar dust" key program. The goal of this project is to build a coherent database on interstellar dust emission from diffuse clouds to the sites of star formation. Aims. We study the far-infrared/submillimeter emission of the PDRs and their fainter surrounding regions. We combine the Herschel and Spitzer maps to derive at each position the full emission spectrum of all dust components, which we compare to dust and radiative transfer models in order to learn about the spatial variations in both the excitation conditions and the dust properties. Methods. We adjust the emission spectra derived from PACS and SPIRE maps using modified black bodies to derive the temperature and the emissivity index β of the dust in thermal equilibrium with the radiation field. We present a first modeling of the NGC 7023-E PDR with standard dust properties and abundances. Results. At the peak positions, a value of β equal to 2 is compatible with the data. The detected spectra and the spatial structures are strongly influenced by radiative transfer effects. We are able to reproduce the spectra at the peak positions deduced from Herschel maps and emitted by dust particles at thermal equilibrium, and also the evolution of the spatial structures observed from the near infrared to the submillimeter. On the other hand, the emission of the stochastically heated smaller particles is overestimated by a factor ∼2.

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“…As can be seen in Table 3 the estimated temperatures for the H ii region G68.14+0.92 and the candidate CHII (see Section 5) are typical for H ii regions and higher than the ones found for the shell structure and its interior. On the other hand, the interior region is the coldest, with a temperature around 20 K, which is characteristic of the more diffuse interstellar medium (Boulanger et al 1996) and consistent with the lack of bubble material in this region. As for the ISRF factor, it can be noted that it is also larger in regions 4 and 7, as expected for regions near a strong radiation field, as is the case for these regions, since they host new stars (see Section 5).…”

Section: Infrared Emission and Dust Propertiesmentioning

confidence: 88%

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

Cichowolski

Suad

Pineault

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a study of the molecular CO gas and mid/far infrared radiation arising from the environment surrounding the Wolf-Rayet (W-R) star 130. We use the multi-wavelength data to analyze the properties of the dense gas and dust, and its possible spatial correlation with that of Young Stellar Objects (YSOs). We use CO J=1-0 data from the FCRAO survey as tracer of the molecular gas, and mid/far infrared data from the recent WISE and Herschel space surveys to study the dust continuum radiation and to identify a population of associated candidate YSOs. The spatial distribution of the molecular gas shows a ring-like structure very similar to that observed in the H i gas, and over the same velocity interval. The relative spatial distribution of the H i and CO components is consistent with a photo-dissociation region. We have identified and characterized four main and distinct molecular clouds that create this structure. Cold dust is coincident with the dense gas shown in the CO measurements. We have found several cYSOs that lie along the regions with the highest gas column density, and suggest that they are spatially correlated with the shell. These are indicative of regions of star formation induced by the strong wind and ionization of the WR star.

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Far-infrared emission from the galaxy in extra-galactic windows

Cited by 239 publications

References 0 publications

Planckearly results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo

Planckearly results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo

Evolution of interstellar dust withHerschel. First results in the photodissociation regions of NGC 7023

The infrared and molecular environment surrounding the Wolf-Rayet star WR 130

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