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

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

doi:10.1051/0004-6361/201014653

Cited by 48 publications

(59 citation statements)

References 45 publications

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“…Melisse & Israel 1994) or of cold FIR SEDs (as revealed by ISO and Herschel measurements extending longwards of 100 μm -e.g. Popescu et al 2002;Grossi et al 2010). Such variety may not be too surprising given that the SF in dwarf galaxies is likely to be fundamentally bursty in nature.…”

Section: Introductionmentioning

confidence: 99%

The dust SED of dwarf galaxies

Hermelo

Lisenfeld

Relaño

et al. 2012

A&A

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Context. High-resolution data from Spitzer, Herschel, and Planck allow us to probe the entire spectral energy distribution (SED) of morphologically separated components of the dust emission from nearby galaxies and allow a more detailed comparison between data and models. Aims. We wish to establish the physical origin of dust heating and emission based on radiation transfer models, that self-consistently connect the emission components from diffuse dust and the dust in massive star forming regions. Methods. NGC 4214 is a nearby dwarf galaxy with a large set of ancillary data, ranging from the ultraviolet (UV) to radio, including maps from Spitzer and Herschel and detections from Planck. We mapped this galaxy with MAMBO at 1.2 mm at the IRAM 30 m telescope. We extracted separate dust emission components for the HII regions (plus their associated PDRs on pc scales) and for the diffuse dust (on kpc scales). We analysed the full UV to FIR/submm SED of the galaxy using a radiation transfer model that self-consistently treats the dust emission from diffuse and star forming (SF) complexes components, considering the illumination of diffuse dust both by the distributed stellar populations and by escaping light from the HII regions. While maintaining consistency within the framework of this model, we additionally used a model that provides a detailed description of the dust emission from the HII regions and their surrounding PDRs on pc scales. Thanks to the large amount of available data and many previous studies for NGC 4214, very few free parameters remained in the model fitting process. Results. We achieve a satisfactory fit for the emission from HII + PDR regions on pc scales, with the exception of the emission at 8 μm, which is underpredicted by the model. For the diffuse emission we achieve a good fit if we assume that about 40-65% of the emission escaping the HII + PDR regions is able to leave the galaxy without passing through a diffuse ISM, which is not an unlikely scenario for a dwarf galaxy that has recently undergone a nuclear starburst. We determine a dust-to-gas mass ratio of 350-470, which is close to the expected value based on the metallicity.

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Section: Introductionmentioning

confidence: 99%

The dust SED of dwarf galaxies

Hermelo

Lisenfeld

Relaño

et al. 2012

A&A

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“…These have mapped the temperature gradient in the dusty interstellar medium (ISM; Bendo et al 2010;Smith et al 2010;Engelbracht et al 2010;Pohlen et al 2010;Foyle et al 2012), notably in the spiral arms (Bendo et al 2010) and bulge (Engelbracht et al 2010) and the power spectrum of the ISM, gas and dust (Combes et al 2012). In the case of dwarf galaxies, Spitzer and results are restricted to a few individual galaxies (e.g., Hinz et al 2006Hinz et al , 2012Hermelo et al 2013), the Herschel Virgo Cluster Survey (Grossi et al 2010), or results of stacked observations (Popescu et al 2002;de Looze et al 2010;Bourne et al 2012). However, the smallest scales can still only be probed in some of the most nearby galaxies, e.g., Andromeda, the Magellanic Clouds or the Milky Way itself.…”

Section: Introductionmentioning

confidence: 99%

The occulting galaxy pair UGC 3995

Holwerda

Keel

2013

A&A

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UGC 3995 is an interacting and occulting galaxy pair. UGC 3995B is a foreground face-on spiral and UGC 3995A a bright background spiral with an AGN. We present analysis of the dust in the disc of UGC 3995B based on archival Hubble Space Telescope (HST) WFPC2 and PPAK IFU data from the CALIFA survey's first data release. From the HST F606W image, we construct an extinction map by modeling the isophotes of the background galaxy UGC 3995A and the resulting transmission through UGC 3995B. This extinction map of UGC 3995B shows several distinct spiral extinction features. The radial distribution of A V values declines slowly with peaks corresponding to the spiral structures. The distribution of A V values in the HST extinction map peaks near A V = 0.3-0.4. Beyond this point, the distribution of A V values drops like an exponential:The 0.5 value is higher than typical for a spiral galaxy. The outer arms may be tidally distended; the extinction in the corresponding interarm regions is small to an unusually small radius. To analyze the PPAK IFU data, we take the ratio of a fibre spectrum in the overlap region and the corresponding background fiber spectrum to construct an extinction curve. We fit the Cardelli, Clayton and Mathis (CCM) curve to the extinction curve of each fiber element in the overlap region. A map of the extinction constructed from PPEX IFU data-cubes shows the same spiral structure of the HST extinction map but the some differences in the distribution of the normalization of the CCM fits (A V ). The inferred extinction slopes (R V ) maps do not display any structure and a range of values partly due to the sampling effects of the disc by fibers, sometimes due to bad fits, and possibly partly due to some reprocessing of dust grains in the interacting disc. We compare these findings to our other analysis of an occulting pair with HST and IFU data. In both cases the canonical R V = 3.1 is not recovered even though there is enough signal in the extinction curve. We attribute this to mixing opaque and more transparent sections of the disc in each resolution element (∼3 or 0.9 kpc). To illustrate the difficulty of imposing a R V = 3.1 law over a section of a spiral disc, we average all spectra and show how a fully gray extinction curve is recovered.

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“…Being so nearby, the Virgo cluster has previously been studied in detail at many wavelengths and so there is a wealth of data available, to which we are now able to add the FIR. This is the first of a series of seven papers, based on HeViCS SDP data, in which we discuss: how the cluster environment truncates the dust discs of spiral galaxies (Paper II, Cortese et al 2010), the dust life-time in early-type galaxies (Paper III, Clemens et al 2010), the spiral galaxy dust surface density and temperature distribution (Paper IV, Smith et al 2010), the properties of metal-poor star-forming dwarf galaxies (Paper V, Grossi et al 2010), the lack of thermal emission from the elliptical galaxy M 87 (Paper VI, Baes et al 2010) and the far-infrared (FIR) detection of dwarf elliptical galaxies (Paper VII, De Looze et al 2010). A further paper discusses the spectral energy distributions of HeViCS galaxies together with others observed as part of the Herschel Reference Survey (Boselli et al 2010).…”

Section: Introductionmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Davies

Baes²,

Bendo

et al. 2010

A&A

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130

136

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We describe the Herschel Virgo Cluster Survey (HeViCS) and the first data obtained as part of the science demonstration phase (SDP). The data cover a central 4 × 4 sq deg region of the cluster. We use SPIRE and PACS photometry data to produce 100, 160, 250, 350 and 500 μm luminosity functions (LFs) for optically bright galaxies that are selected at 500 μm and detected in all bands. We compare these LFs with those previously derived using IRAS, BLAST and Herschel-ATLAS data. The Virgo cluster LFs do not have the large numbers of faint galaxies or examples of very luminous galaxies seen previously in surveys covering less dense environments.

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TheHerschelVirgo Cluster Survey

Cited by 48 publications

References 45 publications

The dust SED of dwarf galaxies

The dust SED of dwarf galaxies

The occulting galaxy pair UGC 3995

TheHerschelVirgo Cluster Survey

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