Diffuse infrared emission from the galaxy. I - Solar neighborhood

Boulanger, F.; Pérault, M.

doi:10.1086/166526

Cited by 296 publications

(245 citation statements)

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“…The present study extends to smaller scales, and to the IVCs and HVCs, the earlier work done with the FIRAS (Boulanger et al 1996) or IRAS (Boulanger & Pérault 1988;Reach et al 1998) data on the dust emission of the diffuse ISM. It also extends to a much larger sample a similar analysis done on a diffuse 3 • × 3 • region at high Galactic latitude using IRAS and Spitzer data (Miville- .…”

Section: Planck and Iras Emissivitiessupporting

confidence: 65%

“…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: Planck and Iras Emissivitiessupporting

confidence: 65%

Section: Modelmentioning

confidence: 99%

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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“…To model these variations, we follow a two step approach where large scale variations related to changes in the Galactic Interstellar Radiation Field are separated from smaller scale fluctuations. We used the IRAS/IRIS (Miville-Deschênes & Lagache 2005) and Leiden/Argentine/Bonn (LAB, Kalberla et al 2005) surveys of the all sky IR emissivity and Galactic N H , and corrected their dependence with galactic latitude, b, by subtracting two cosecant laws with shape 1 sin |b| , following the analytic approach of Boulanger & Perault (1988) and Eqs. (3.1) and (3.2) of Desert et al (1988).…”

Section: Absorption By Galactic Neutral Hydrogenmentioning

confidence: 99%

A2163: Merger events in the hottest Abell galaxy cluster

Bourdin

Arnaud

Mazzotta

et al. 2011

A&A

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Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) that exhibits extraordinary properties, including an exceptionally high X-ray luminosity, average temperature, and a powerful and extended radio halo. The irregular and complex morphology of its gas and galaxy structure suggests that this cluster has recently undergone major merger events that involve two or more cluster components. In this paper, we study the gas structure and dynamics by means of spectral-imaging analysis of X-ray data obtained from XMM-Newton and Chandra observations. From the evidence of a cold front, we infer the westward motion of a cool core across the E-W elongated atmosphere of the main cluster A2163-A. Located close to a galaxy over-density, this gas "bullet" appears to have been spatially separated from its galaxy (and presumably dark matter component) as a result of high-velocity accretion. From gas brightness and temperature profile analysis performed in two opposite regions of the main cluster, we show that the ICM has been adiabatically compressed behind the crossing "bullet" possibly because of shock heating, leading to a strong departure of the ICM from hydrostatic equilibrium in this region. Assuming that the mass estimated from the Y X proxy best indicates the overall mass of the system and that the western cluster sector is in approximate hydrostatic equilibrium before subcluster accretion, we infer a merger scenario between two subunits of mass ratio 1:4, leading to a present total system mass of M 500 1.9 × 10 15 M . Additional analysis of the spatially-separated northern subcluster A2163-B does not show any evidence of strong interaction with the main cluster A2163-A, leading us to infer that the physical distance separating the northern subcluster and the main component is longer than the projected separation of these components. The exceptional properties of A2163 present various similarities with those of 1E0657-56, the so-called "bullet-cluster". These similarities are likely to be related to a comparable merger scenario.

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“…(1.6 ‫ע‬ 0.1) # 10 lactic X-ray absorption (∼ cm Ϫ2 ) derived from the 22 3.6 # 10 IRAS 100 mm emission in this direction (Boulanger & Perault 1988;Wheelock et al 1994). Assuming that the absorbing gas is relatively uniformly distributed along the line of sight, the distance to G54.1ϩ0.3 should be approximately 5 kpc, about halfway to the edge of the Galaxy from the Sun.…”

mentioning

confidence: 97%

[ITAL]Chandra[/ITAL] Observation of Supernova Remnant G54.1+0.3: A Close Cousin of the Crab Nebula

Wang

Aschenbach

et al. 2002

The Astrophysical Journal

113

121

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We present a Chandra Advanced CCD Imaging Spectrometer observation of supernova remnant G54.1ϩ0.3. This supernova remnant is resolved into several distinct X-ray-emitting components: a central bright pointlike source (CXOU J193030.13ϩ185214.1), a surrounding ring, bipolar elongations, plus low surface brightness diffuse emission. The spectra of these components are all well described by power-law models; the spectral index steepens with increasing distance from the pointlike source. We find no evidence for any thermal plasma emission that would correspond to shocked interstellar medium or ejecta. The observed morphological and spectral characteristics suggest that G54.1ϩ0.3 is the closest "cousin" of the Crab Nebula-a pulsar wind nebula driven by a combination of equatorial and polar outflows from the putative pulsar represented by the pointlike X-ray source. Subject headings: ISM: individual (G54.1ϩ0.3) -ISM: jets and outflows -stars: neutronsupernova remnants -X-rays: ISM On-line material: color figure

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Diffuse infrared emission from the galaxy. I - Solar neighborhood

Cited by 296 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

A2163: Merger events in the hottest Abell galaxy cluster

[ITAL]Chandra[/ITAL] Observation of Supernova Remnant G54.1+0.3: A Close Cousin of the Crab Nebula

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