Reviews

Rowan-Robinson, Jeremy

doi:10.1093/jel/9.2.409

Cited by 30 publications

(46 citation statements)

References 0 publications

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“…Our first results on exploration of the full FIR SED are given by Elbaz et al (), Rowan‐Robinson et al (), Hwang et al () and Chapman et al (). Elbaz et al () combined photometry from PACS (from the PEP programme) and SPIRE (from HerMES).…”

Section: Early and Anticipated Sciencementioning

confidence: 88%

TheHerschelMulti-tiered Extragalactic Survey: HerMES

Oliver

Bock

Altiéri

et al. 2012

Monthly Notices of the Royal Astronomical Society

741

615

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The Herschel Multi‐tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ∼380 deg2. Fields range in size from 0.01 to ∼20 deg2, using the Herschel‐Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500 μm) and the Herschel‐Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160 μm), with an additional wider component of 270 deg2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100 000 galaxies at 5σ in some of the best‐studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X‐ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

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Section: Early and Anticipated Sciencementioning

confidence: 88%

TheHerschelMulti-tiered Extragalactic Survey: HerMES

Oliver

Bock

Altiéri

et al. 2012

Monthly Notices of the Royal Astronomical Society

741

615

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“…The Planck satellite, launched by the same rocket, performs an all‐sky survey at nine wavelengths between 350 μm and 1 cm, complementing Herschel coverage, at a lower resolution. Ade et al () studies have suggested that some nearby galaxies are both luminous and cool (presence of dust with T < 20 K), with properties comparable to those of galaxies observed with Herschel at higher redshifts (Rowan‐Robinson et al ; Magnelli et al ). Using Herschel observations, Engelbracht et al () compute separate SEDs for the centre and discs of nearby galaxies and find that the cool dust is on average 15 per cent hotter in the centre than in the disc and correlate this effect with morphological type and bar strength.…”

Section: Introductionmentioning

confidence: 87%

Mapping the cold dust temperatures and masses of nearby KINGFISH galaxies withHerschel

Galametz

Kennicutt

Albrecht³

et al. 2012

Monthly Notices of the Royal Astronomical Society

145

155

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Taking advantage of the unprecedented combination of sensitivity and angular resolution afforded by the Herschel Space Observatory at far‐infrared and submillimetre wavelengths, we aim to characterize the physical properties of cold dust within nearby galaxies, as well as the associated uncertainties, namely the robustness of the parameters we derive using different modified blackbody models. For a pilot subsample of the KINGFISH (Key Insights on Nearby Galaxies: A Far‐Infrared Survey with Herschel) key programme, we perform two‐temperature fits of the Spitzer and Herschel photometric data (from 24 to 500 μm), with a warm and a cold component, both globally and in each resolution element. We compare the results obtained from different analysis strategies. At global scale, we observe a range of values of the modified blackbody fit parameters βc (0.8–2.5) and Tc (19.1–25.1 K). We compute maps of our modelling parameters with βc fixed or treated as a free parameter to test the robustness of the temperature and dust surface density maps we deduce. When the emissivity is fixed, we observe steeper temperature gradients as a function of radius than when it is allowed to vary. When the emissivity is fitted as a free parameter, barred galaxies tend to have uniform fitted emissivities. Gathering the parameters obtained in each resolution element in a Tc–βc diagram underlines an anticorrelation between the two parameters. It remains difficult to assess whether the dominant effect is the physics of dust grains, noise, or mixing along the line of sight and in the beam. We finally observe in both cases that the dust column density peaks in central regions of galaxies and bar‐ends (coinciding with molecular gas density enhancements usually found in these locations). We also quantify how the total dust mass varies with our assumptions about the emissivity index as well as the influence of the wavelength coverage used in the fits. We show that modified blackbody fits using a shallow emissivity (β < 2.0) lead to significantly lower dust masses compared to the β < 2.0 case, with dust masses lower by up to 50 per cent if βc = 1.5, for instance. The working resolution affects our total dust mass estimates: masses increase from global fits to spatially resolved fits.

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“…ψ = 1 corresponds to the interstellar radiation field in the vicinity of the Sun ('cool' dust). Rowan-Robinson et al (2010 found that some Herschel galaxies need a much lower intensity radiation field than this, with ψ = 0.1 ('cold' dust). A similar result was found for some Planck galaxies by Ade et al (2011).…”

Section: Predicted Submillimetre Diametersmentioning

confidence: 99%

“…A similar result was found for some Planck galaxies by Ade et al (2011). The corresponding grain temperatures in the dust model of RR92 are given in Table 1 of Rowan-Robinson et al (2010). For the three values of ψ = 5, 1, 0.1, the ranges of dust grain temperatures for the different grain types are 20-24 K, 14.5-19.7 K and 9.8-13.4 K respectively.…”

Section: Predicted Submillimetre Diametersmentioning

confidence: 99%