The<i>Herschel</i>Virgo Cluster Survey

Smith, M.; Vlahakis, C.; Baes, M.; Bendo, G. J.; Bianchi, S.; Bomans, D. J.; Boselli, A.; Clemens, M.; Corbelli, E.; Cortese, Luca; Dariush, Aliakbar; Davies, J. I.; Looze, I. De; Alighieri, S. di Serego; Fadda, D.; Fritz, J.; Garcia‐Appadoo, D. A.; Gavazzi, G.; Giovanardi, C.; Grossi, M.; Hughes, T. M.; Hunt, L. K.; Jones, A. P.; Madden, S.; Pierini, D.; Pohlen, M.; Sabatini, S.; Verstappen, J.; Xilouris, E. M.; Zibetti, S.

doi:10.1051/0004-6361/201014584

Cited by 45 publications

(22 citation statements)

References 23 publications

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“…If the 70-µm point is higher than our fit using 160, 250, 350 and 500 µm, this suggests a warmer component (i.e. Bendo et al 2010a;Smith et al 2010). We find that the SED fit overpredicts the 70-µm value over much of the galaxy.…”

Section: Temperature and Emissivitymentioning

confidence: 51%

“…The dust temperature is highest ahead of the dust mass surface density arms if we assume a trailing spiral structure rotating in the clockwise direction. Dust temperature and mass maps for NGC 4501 and NGC 4567/8 in the Herschel Virgo Cluster Survey have also shown that the peaks in dust temperature were not coincident with those in mass (Smith et al 2010). Fig.…”

Section: Distribution Of Dust Temperature and Massmentioning

confidence: 99%

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The dust and gas properties of M83

Foyle

Wilson

Mentuch

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We examine the dust and gas properties of the nearby, barred galaxy M83, which is part of the Very Nearby Galaxy Survey. Using images from the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging REceiver (SPIRE) instruments of Herschel, we examine the dust temperature and dust mass surface density distribution. We find that the nuclear, bar and spiral arm regions exhibit higher dust temperatures and masses compared to interarm regions. However, the distributions of dust temperature and mass are not spatially coincident. Assuming a trailing spiral structure, the dust temperature peaks in the spiral arms lie ahead of the dust surface density peaks. The dust mass surface density correlates well with the distribution of molecular gas as traced by CO (J= 3?2) images (James Clerk Maxwell Telescope) and the star formation rate as traced by Ha with a correction for obscured star formation using 24-mu m emission. Using H i images from The H i Nearby Galaxy Survey (THINGS) to trace the atomic gas component, we make total gas mass surface density maps and calculate the gas-to-dust ratio. We find a mean gas-to-dust ratio of 84 +/- 4 with higher values in the inner region assuming a constant CO-to-H2 conversion factor. We also examine the gas-to-dust ratio using CO-to-H2 conversion factor that varies with metallicity

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Section: Temperature and Emissivitymentioning

confidence: 51%

Section: Distribution Of Dust Temperature and Massmentioning

confidence: 99%

The dust and gas properties of M83

Foyle

Wilson

Mentuch

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…excluding the 24 µm data point) using a single modified blackbody. This can be explained because there is a non-negligible contribution from the warm dust component to the Herschel PACS 70 µm flux density, as found for the integrated emission of other nearby galaxies (see, e.g., Bendo et al 2010;Smith et al 2010). However, the temperature of the warm component is not tightly constrained since varying the warm dust temperature by as much as ±4 K produces statistically similar good fits (χ 2 ≤ 2 χ 2 min ).…”

Section: Dust Propertiesmentioning

confidence: 80%

Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

Alonso‐Herrero

Sánchez‐Portal

Almeida³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present new far‐infrared (70–500 μm) Herschel Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) imaging observations as well as new mid‐IR Gemini/Thermal‐Region Camera Spectrograph imaging (8.7 and 18.3 μm) and spectroscopy of the inner Lindblad resonance (ILR) region (R < 2.5 kpc) of the spiral galaxy NGC 1365. We complemented these observations with archival Spitzer imaging and spectral mapping observations. The ILR region of NGC 1365 contains a Seyfert 1.5 nucleus and a ring of star formation with an approximate diameter of 2 kpc. The strong star formation activity in the ring is resolved by the Herschel/PACS imaging data, as well as by the Spitzer 24 μm continuum emission, [Ne ii] 12.81 μm line emission, and 6.2 and 11.3 μm PAH emission. The active galactic nucleus (AGN) is the brightest source in the central regions up to λ ∼ 24 μm, but it becomes increasingly fainter in the far‐infrared when compared to the emission originating in the infrared clusters (or groups of them) located in the ring. We modelled the AGN unresolved infrared emission with the clumpy torus models and estimated that the AGN contributes only to a small fraction (∼5 per cent) of the infrared emission produced in the inner ∼5 kpc. We fitted the non‐AGN 24–500 μm spectral energy distribution of the ILR region and found that the dust temperatures and mass are similar to those of other nuclear and circumnuclear starburst regions. Finally we showed that within the ILR region of NGC 1365, most of the ongoing star formation activity is taking place in dusty regions as probed by the 24 μm emission.

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“…3, and fitting the resulting totals. Note that we tested the effect of removing the 70-µm data point from our SED fit to ensure that it was not forcing the curve to peak at shorter wavelengths and that it was not from a separate thermal component of the dust (Bendo et al 2010a(Bendo et al , 2012Smith et al 2010). We found that the 70-µm flux falls on the best-fitting curves within uncertainties for these tests, and thus we use all five wavelengths in our fitting routine.…”

Section: Sed Fittingmentioning

confidence: 99%

The gas-to-dust mass ratio of Centaurus A as seen by Herschel★

Parkin¹,

Wilson²,

Foyle³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present photometry of the nearby galaxy NGC 5128 (Centaurus A) observed with the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on board the Herschel Space Observatory, at 70, 160, 250, 350 and 500 μm, as well as new CO J= 3–2 observations taken with the HARP‐B instrument on the James Clerk Maxwell Telescope (JCMT). Using a single‐component modified blackbody, we model the dust spectral energy distribution within the disc of the galaxy using all five Herschel wavebands and find dust temperatures of ∼30 K towards the centre of the disc and a smoothly decreasing trend to ∼20 K with increasing radius. We find a total dust mass of (1.59 ± 0.05) × 107 M⊙ and a total gas mass of (2.7 ± 0.2) × 109 M⊙. The average gas‐to‐dust mass ratio is 103 ± 8, but we find an interesting increase in this ratio to approximately 275 towards the centre of Cen A. We discuss several possible physical processes that may be causing this effect, including dust sputtering, jet entrainment and systematic variables such as the XCO factor. Dust sputtering by X‐rays originating in the active galactic nucleus or the removal of dust by the jets is our most favoured explanation.

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TheHerschelVirgo Cluster Survey

Cited by 45 publications

References 23 publications

The dust and gas properties of M83

The dust and gas properties of M83

Probing the nuclear and circumnuclear activity of NGC 1365 in the infrared

The gas-to-dust mass ratio of Centaurus A as seen by Herschel★

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