<i>Herschel</i>-SPIRE observations of the Polaris flare: Structure of the diffuse interstellar medium at the sub-parsec scale

Miville-Deschênes, M.-A.; Martín, P. G.; Abergel, A.; Bernard, J.-P.; Boulanger, F.; Lagache, G.; Anderson, L. D.; André, Ph.; Arab, H.; Baluteau, J. P.; Blagrave, K.; Bontemps, Sylvain; Cohen, Martin; Compiègne, M.; Cox, P.; Dartois, E.; Davis, G. R.; Emery, R. J.; Fulton, T.; Gry, C.; Habart, E.; Huang, M.; Joblin, C.; Jones, Scott C.; Kirk, J. M.; Lim, T.; Madden, S.; Makiwa, G.; Men’shchikov, A.; Molinari, S.; Moseley, H.; Motte, F.; Naylor, David; Okumura, K.; Gonçalves, D. Pinheiro; Polehampton, E. T.; Rodón, J. A.; Russeil, D.; Saraceno, P.; Schneider, N.; Sidher, S.; Spencer, L. D.; Swinyard, Bruce; Ward-Thompson, Derek; White, G. J.; Zavagno, A.

doi:10.1051/0004-6361/201014678

Cited by 150 publications

(89 citation statements)

References 10 publications

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“…(A color version of this figure is available in the online journal.) recently, studies of various fields using BLAST and SPIRE data have found a much wider range of the index, e.g., α c ∼ −2.4 (Bracco et al 2011), −2.6 , −2.8 Miville-Deschênes et al 2010), −2.9 , and even ranging from −2.5 to −3.6, depending on the field (Miville-Deschênes et al 2007). Thus, rather than assume a power law with α = −3 (e.g., Viero et al 2009), we proceed by treating each field independently.…”

Section: Galactic Cirrusmentioning

confidence: 99%

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Viero

Wang

Zemcov

et al. 2013

ApJ

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155

208

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We present measurements of the auto-and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 μm (1200, 860, and 600 GHz) from observations totaling ∼70 deg 2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy δI /I = 14% ± 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2-to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k θ ∼ 0.10-0.12 arcmin −1 ( ∼ 2160-2380), from 250 to 500 μm. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources-suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z ∼ 1-3, is log(M peak /M ) ∼ 12.1 ± 0.5, and that the minimum halo mass to host infrared galaxies is log(M min /M ) ∼ 10.1 ± 0.6.

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Section: Galactic Cirrusmentioning

confidence: 99%

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Viero

Wang

Zemcov

et al. 2013

ApJ

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155

208

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“…This characteristic can be examined by calculating the spatial power spectra of the cirrus distribution taken from the AKARI diffuse all sky survey, as the cirrus power spectra can be well represented by power-law spectra (see e.g., Miville-Deschênes et al, 2010;Martin et al, 2010).…”

Section: Spatial Power Spectramentioning

confidence: 99%

Akari Far-Infrared All-Sky Survey Maps

Doi¹,

Komugi²,

Kawada³

et al. 2012

Publications of The Korean Astronomical Society

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Far-infrared observations provide crucial data for the investigation and characterisation of the properties of dusty material in the Interstellar Medium (ISM), since most of its energy is emitted between ∼ 100 and 200 µm. We present the first all-sky image from a sensitive all-sky survey using the Japanese AKARI satellite, in the wavelength range 50 -180 µm. Covering > 99% of the sky in four photometric bands with four filters centred at 65 µm, 90 µm, 140 µm, and 160 µm wavelengths, this achieved spatial resolutions from 1 to 2 arcmin and a detection limit of < 10 MJy sr −1 , with absolute and relative photometric accuracies of < 20%. All-sky images of the Galactic dust continuum emission enable astronomers to map the large-scale distribution of the diffuse ISM cirrus, to study its thermal dust temperature, emissivity and column density, and to measure the interaction of the Galactic radiation field and embedded objects with the surrounding ISM. In addition to the point source population of stars, protostars, star-forming regions, and galaxies, the high Galactic latitude sky is shown to be covered with a diffuse filamentary-web of dusty emission that traces the potential sites of high latitude star formation. We show that the temperature of dust particles in thermal equilibrium with the ambient interstellar radiation field can be estimated by using 90 µm, 140 µm, and 160 µm data. The FIR AKARI full-sky maps provide a rich new data set within which astronomers can investigate the distribution of interstellar matter throughout our Galaxy, and beyond.

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“…The uncertainty in submm colour G is estimated by taking the rms of the ratio involving S(λ)/I(100) once the offset S 0 is removed from each of the maps, while the uncertainty in S 0 comes from the rms of the difference involving S(λ) − G × I(100), with the best-fitting values for submm colour used in the computation. As described in Miville-Deschênes et al (2010), these rms values reflect the overall uncertainties more accurately than if one were to simply use the statistics associated with the linear fit to the relation between S(λ) and I(100). Those have uncertainties that are at least a factor of 10 smaller than the errors quoted above.…”

Section: Zero-level In Spire Mapsmentioning

confidence: 99%

“…Some of these clouds may be on the verge of gravitational collapse leading to the formation of a new star (Olmi et al 2010;Sadavoy, Di Francesco & Johnstone 2010;Ward-Thompson et al 2010). At large angular scales, dust is a key tracer of the large-scale physical processes occurring in the diffuse ISM (Miville-Deschênes et al 2010). Dust emission is also related to the density structure of diffuse clouds and could potentially provide a way to study the projected density distribution within the Galactic cirrus.…”

Section: Introductionmentioning

confidence: 99%

Herschel-ATLAS: statistical properties of Galactic cirrus in the GAMA-9 Hour Science Demonstration Phase Field

Bracco

Cooray

Veneziani

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We study the spectral energy distribution (SED) and the power spectrum of Galactic cirrus emission observed in the 14 deg2 Science Demonstration Phase field of the Herschel‐ATLAS using Herschel and IRAS data from 100 to 500 μm. We compare the Spectral and Photometric Imaging Receiver (SPIRE) 250, 350 and 500 μm maps with IRAS 100‐μm emission, binned in 6‐arcmin pixels. We assume a modified blackbody SED with dust emissivity parameter β (F∝λ−β) and a single dust temperature Td, and find that the dust temperature and emissivity index varies over the science demonstration field as and 1 < β < 4. The latter values are somewhat higher than the range of β often quoted in the literature (1 < β < 2). We estimate the mean values of these parameters to be Td= 19.0 ± 2.4 K and β= 1.4 ± 0.4. In regions of bright cirrus emission, we find that the dust has similar temperatures with , and similar values of β, ranging from 1.4 ± 0.5 to 1.9 ± 0.5. We show that Td and β associated with diffuse cirrus emission are anti‐correlated and can be described by the relationship: β(Td) =NTαd with [N= 116 ± 38, α=−1.4 ± 0.1]. The strong correlation found in this analysis is not just limited to high‐density clumps of cirrus emission as seen in previous studies, but is also seen in diffuse cirrus in low‐density regions. To provide an independent measure of Td and β, we obtain the angular power spectrum of the cirrus emission in the IRAS and SPIRE maps, which is consistent with a power spectrum of the form P(k) =P0(k/k0)γ, where γ= 2.6 ± 0.2 for scales of 50–200 arcmin in the SPIRE maps. The cirrus rms fluctuation amplitude at angular scales of 100 arcmin is consistent with a modified blackbody SED with and β= 1.3 ± 0.2, in agreement with the values obtained above.

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Herschel-SPIRE observations of the Polaris flare: Structure of the diffuse interstellar medium at the sub-parsec scale

Cited by 150 publications

References 10 publications

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Akari Far-Infrared All-Sky Survey Maps

Herschel-ATLAS: statistical properties of Galactic cirrus in the GAMA-9 Hour Science Demonstration Phase Field

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