FIR colours and SEDs of nearby galaxies observed with<i>Herschel</i>

Boselli, A.; Ciesla, L.; Buat, V.; Cortese, Luca; Auld, Robbie Richard; Baes, M.; Bendo, G. J.; Bianchi, S.; Bock, J. J.; Bomans, D. J.; Bradford, M.; Castro-Rodríguez, N.; Chanial, P.; Charlot, S.; Clemens, M.; Clements, D. L.; Corbelli, E.; Cooray, Asantha; Cormier, D.; Dariush, Aliakbar; Davies, Jonathan Ivor; Looze, I. De; Alighieri, S. di Serego; Dwek, Eli; Eales, Stephen Anthony; Elbaz, D.; Fadda, D.; Fritz, J.; Galametz, M.; Galliano, F.; Garcia‐Appadoo, D. A.; Gavazzi, G.; Gear, Walter Kieran; Giovanardi, C.; Glenn, J.; Gomez, Haley; Griffin, M. J.; Grossi, M.; Hony, S.; Hughes, T. M.; Hunt, L. K.; Isaak, K. G.; Jones, A. P.; Levenson, L.; Lu, N.; Madden, S.; O’Halloran, B.; Okumura, K.; Oliver, Seb; Page, M. J.; Panuzzo, P.; Παπαγεωργίου, Ανδρέας; Parkin, T. J.; Pérez-Fournón, I.; Pierini, D.; Pohlen, M.; Rangwala, Naseem; Rigby, E. E.; Roussel, H.; Rykala, Adam John; Sabatini, S.; Sacchi, N.; Sauvage, M.; Schulz, B.; Schirm, M. R. P.; Smith, M.; Spinoglio, L.; Stevens, J. A.; Sundar, Sita; Symeonidis, M.; Trichas, M.; Vaccari, M.; Verstappen, J.; Vigroux, L.; Vlahakis, C.; Wilson, C. D.; Wozniak, H.; Wright, G. S.; Xilouris, E. M.; Zeilinger, W. W.; Zibetti, S.

doi:10.1051/0004-6361/201014534

Cited by 79 publications

(47 citation statements)

References 37 publications

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“…Note that the right-hand panel uses the brighter limit of r < 19 appropriate for the GAMA redshift survey. 2010; Bernard et al 2010;Boselli et al 2010;Kramer et al 2010;Planck Collaboration 2011b). For more accurate dust mass estimates we require the mass-weighted temperature of the dust emitting at 250 μm which requires fitting a model with multiple (at least two) temperature components.…”

Section: U S T M a S S A N D L U M I N O S I T Ymentioning

confidence: 99%

Herschel★-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years

Dunne¹,

Gomez²,

Cunha³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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235

296

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We present the first direct and unbiased measurement of the evolution of the dust mass function of galaxies over the past 5 billion years of cosmic history using data from the Science Demonstration Phase of the Herschel‐Astrophysical Terahertz Large Area Survey (Herschel‐ATLAS). The sample consists of galaxies selected at 250 m which have reliable counterparts from the Sloan Digital Sky Survey (SDSS) at z < 0.5, and contains 1867 sources. Dust masses are calculated using both a single‐temperature grey‐body model for the spectral energy distribution and also a model with multiple temperature components. The dust temperature for either model shows no trend with redshift. Splitting the sample into bins of redshift reveals a strong evolution in the dust properties of the most massive galaxies. At z= 0.4–0.5, massive galaxies had dust masses about five times larger than in the local Universe. At the same time, the dust‐to‐stellar mass ratio was about three to four times larger, and the optical depth derived from fitting the UV‐sub‐mm data with an energy balance model was also higher. This increase in the dust content of massive galaxies at high redshift is difficult to explain using standard dust evolution models and requires a rapid gas consumption time‐scale together with either a more top‐heavy initial mass function (IMF), efficient mantle growth, less dust destruction or combinations of all three. This evolution in dust mass is likely to be associated with a change in overall interstellar medium mass, and points to an enhanced supply of fuel for star formation at earlier cosmic epochs.

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Section: U S T M a S S A N D L U M I N O S I T Ymentioning

confidence: 99%

Herschel★-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years

Dunne¹,

Gomez²,

Cunha³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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235

296

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“…The SED peak emission of nearby galaxies spans a relatively narrow range of dust temperatures, from ∼15 to 40 K (Bendo et al 2003;Dale et al 2005;Stevens, Amure & Gear 2005;Boselli et al 2010;D12). In this study, we decide to use an isothermal fit to describe the cold dust component and to call our parameter T c the 'cold dust temperature'.…”

Section: Naming Conventionmentioning

confidence: 99%

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

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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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“…There are three notable exceptions to this. The early-type galaxies NGC 4486 (M87) and NGC 4374 (M84) show departures from a thermal spectrum (Boselli et al 2010), particularly at longer wavelengths. As discussed in Baes et al (2010), specifically for NGC 4486, both these galaxies require modelling of the synchrotron component and its removal before the thermal dust spectrum can be analysed.…”

Section: U S T G a S A N D S T E L L A R M A S Smentioning

confidence: 99%

“…In the other six papers (of this series) on this central field, we have discussed how the cluster environment truncates the dust discs of spiral galaxies (Paper II, Cortese et al 2010), the dust lifetime 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 M87 (Paper VI, Baes et al 2010), and the far-infrared detection of dwarf elliptical galaxies (Paper VII, De Looze et al 2010). Another paper (Boselli et al 2010) discusses the SEDs of HeViCS galaxies together with others observed as part of the Herschel Reference Survey (HRS). Binggeli et al (1987) survey which led to the VCC of some 2000 galaxies.…”

Section: Introductionmentioning

confidence: 99%

The Herschel Virgo Cluster Survey - VIII. The Bright Galaxy Sample★

Davies

Bianchi

Cortese

et al. 2011

Monthly Notices of the Royal Astronomical Society

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177

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We describe the Herschel Virgo Cluster Survey and the first data that cover the complete survey area (four 4 × 4 deg2 regions). We use these data to measure and compare the global far‐infrared properties of 78 optically bright galaxies that are selected at 500 μm and detected in all five far‐infrared bands. We show that our measurements and calibration are broadly consistent with previous data obtained by the IRAS, ISO, Spitzer and Planck. We use SPIRE and PACS photometry data to produce 100‐, 160‐, 250‐, 350‐ and 500‐μm cluster luminosity distributions. These luminosity distributions are not power laws, but ‘peaked’, with small numbers of both faint and bright galaxies. We measure a cluster 100–500 μm far‐infrared luminosity density of 1.6(7.0) ± 0.2 × 109 L⊙ Mpc−3. This compares to a cluster 0.4–2.5 μm optical luminosity density of 5.0(20.0) × 109 L⊙ Mpc−3, some 3.2(2.9) times larger than the far‐infrared. A ‘typical’ photon originates from an optical depth of 0.4 ± 0.1. Most of our sample galaxies are well fitted by a single modified blackbody (β= 2), leading to a mean dust mass of log MDust= 7.31 M⊙ and temperature of 20.0 K. We also derive both stellar and atomic hydrogen masses from which we calculate mean values for the star‐to‐gas (atomic) and gas (atomic)‐to‐dust mass ratios of 15.1 and 58.2, respectively. Using our derived dust, atomic gas and stellar masses, we estimate cluster mass densities of 8.6(27.8) × 106, 4.6(13.9) × 108 and 7.8(29.7) × 109 M⊙ Mpc−3 for dust, atomic gas and stars, respectively. These values are higher than those derived for field galaxies by factors of 39(126), 6(18) and 34(129), respectively. In the above, the luminosity/mass densities are given using the whole sample with the values in brackets using just those galaxies that lie between 17 and 23 Mpc. We provide a data table of flux densities in all the Herschel bands for all 78 bright Virgo Cluster galaxies.

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FIR colours and SEDs of nearby galaxies observed withHerschel

Cited by 79 publications

References 37 publications

Herschel★-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years

Herschel★-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years

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

The Herschel Virgo Cluster Survey - VIII. The Bright Galaxy Sample★

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