18 results on '"Looze, I. De"'
Search Results
2. High-resolution, 3D radiative transfer modelling: III. The DustPedia barred galaxies
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Nersesian, A. Verstocken, S. Viaene, S. Baes, M. Xilouris, E.M. Bianchi, S. Casasola, V. Clark, C.J.R. Davies, J.I. De Looze, I. De Vis, P. Dobbels, W. Fritz, J. Galametz, M. Galliano, F. Jones, A.P. Madden, S.C. Mosenkov, A.V. Trčka, A. Ysard, N.
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Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Context. Dust in late-type galaxies in the local Universe is responsible for absorbing approximately one third of the energy emitted by stars. It is often assumed that dust heating is mainly attributable to the absorption of ultraviolet and optical photons emitted by the youngest (100 Myr) stars. Consequently, thermal re-emission by ust at far-infrared wavelengths is often linked to the star-formation activity of a galaxy. However, several studies argue that the contribution to dust heating by much older stellar populations might be more significant than previously thought. Advances in radiation transfer simulations finally allow us to actually quantify the heating mechanisms of difuse dust by the stellar radiation field. Aims. As one of the main goals in the DustPedia project, we have developed a framework to construct detailed 3D stellar and dust radiative transfer models for nearby galaxies. In this study, we analyse the contribution of the di erent stellar populations to the dust heating in four nearby face-on barred galaxies: NGC 1365, M 83, M 95, and M 100. We aim to quantify the fraction directly related to young stellar populations, both globally and on local scales, and to assess the influence of the bar on the heating fraction. Methods. From 2D images we derive the 3D distributions of stars and dust. To model the complex geometries, we used skirt, a state-of-the-art 3D Monte Carlo radiative transfer code designed to self-consistently simulate the absorption, scattering, and thermal re-emission by the dust for arbitrary 3D distributions. Results. We derive global attenuation laws for each galaxy and confirm that galaxies of high specific star-formation rate have shallower attenuation curves and weaker UV bumps. On average, 36.5% of the bolometric luminosity is absorbed by dust in our galaxy sample. We report a clear e ect of the bar structure on the radial profiles of the dust-heating fraction by the young stellar populations, and the dust temperature.We find that the young stellar populations are the main contributors to the dust heating, donating, on average 59% of their luminosity to this purpose throughout the galaxy. This dust-heating fraction drops to 53% in the bar region and 38% in the bulge region where the old stars are the dominant contributors to the dust heating.We also find a strong link between the heating fraction by the young stellar populations and the specific star-formation rate. © 2020 ESO.
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- 2020
3. High-resolution, 3D radiative transfer modelling: IV. AGN-powered dust heating in NGC 1068
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Viaene, S. Nersesian, A. Fritz, J. Verstocken, S. Baes, M. Bianchi, S. Casasola, V. Cassarà, L. Clark, C. Davies, J. De Looze, I. De Vis, P. Dobbels, W. Galametz, M. Galliano, F. Jones, A. Madden, S. Mosenkov, A. Trcka, A. Xilouris, E.M. Ysard, N.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The star formation rate and the mass of interstellar medium (ISM) have a high predictive power for the future evolution of a galaxy. Nevertheless, deriving such properties is not straightforward. Dust emission, an important diagnostic of star formation and ISM mass throughout the Universe, can be powered by sources unrelated to ongoing star formation. In the framework of the DustPedia project we set out to disentangle the radiation of the ongoing star formation from that of the older stellar populations. This is done through detailed 3D radiative transfer simulations of face-on spiral galaxies. We take special care in modelling the morphological features present for each source of radiation. In this particular study, we focus on NGC 1068, which in addition contains an active galactic nucleus (AGN). The effect of diffuse dust heating by an AGN (beyond the torus) has so far only been investigated for quasars. This additional dust heating source further contaminates the broadband fluxes that are used by classic galaxy modelling tools to derive physical properties. We aim to fit a realistic model to the observations of NGC 1068 and quantify the contribution of the several dust-heating sources. Our model is able to reproduce the global spectral energy distribution of the galaxy. It matches the resolved optical and infrared images fairly well, but deviates in the UV and the submillimetre (submm). This is partly due to beam smearing effects, but also because the input dust distribution is not sufficiently peaked in the centre. We find that AGN contamination of the broadband fluxes has a strong dependency on wavelength. It peaks in the mid-infrared, drops in the far-infrared, and then rises again at submm wavelengths. We quantify the contribution of the dust-heating sources in each 3D dust cell and find a median value of 83% for the star formation component. The AGN contribution is measurable at the percentage level in the disc, but quickly increases in the inner few hundred parsecs, peaking above 90%. This is the first time the phenomenon of an AGN heating the diffuse dust beyond its torus is quantified in a nearby star-forming galaxy. NGC 1068 only contains a weak AGN, meaning this effect could be stronger in galaxies with a more luminous AGN. This could significantly impact the derived star formation rates and ISM masses for such systems. © ESO 2020.
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- 2020
4. High-resolution, 3D radiative transfer modelling: II. The early-type spiral galaxy M 81
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Verstocken, S. Nersesian, A. Baes, M. Viaene, S. Bianchi, S. Casasola, V. Clark, C.J.R. Davies, J.I. De Looze, I. De Vis, P. Dobbels, W. Galliano, F. Jones, A.P. Madden, S.C. Mosenkov, A.V. Trčka, A. Xilouris, E.M.
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Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Context. Interstellar dust absorbs stellar light very efficiently, thus shaping the energy output of galaxies. Studying the impact of different stellar populations on the dust heating continues to be a challenge because it requires decoupling the relative geometry of stars and dust and also involves complex processes such as scattering and non-local dust heating. Aims. We aim to constrain the relative distribution of dust and stellar populations in the spiral galaxy M 81 and create a realistic model of the radiation field that adequately describes the observations. By investigating the dust-starlight interaction on local scales, we want to quantify the contribution of young and old stellar populations to the dust heating. We aim to standardise the setup and model selection of such inverse radiative transfer simulations so these can be used for comparable modelling of other nearby galaxies. Methods. We present a semi-automated radiative transfer modelling pipeline that implements necessary steps such as the geometric model construction and the normalisation of the components through an optimisation routine. We used the Monte Carlo radiative transfer code SKIRT to calculate a self-consistent, panchromatic model of the interstellar radiation field. By looking at different stellar populations independently, we were able to quantify to what extent different stellar age populations contribute to the heating of dust. Our method takes into account the effects of non-local heating. Results. We obtained a realistic 3D radiative transfer model of the face-on galaxy M 81. We find that only 50.2% of the dust heating can be attributed to young stellar populations (≲ 100 Myr). We confirm that there is a tight correlation between the specific star formation rate and the heating fraction by young stellar populations, both in sky projections and in 3D, which is also found for radiative transfer models of M 31 and M 51. Conclusions. We conclude that old stellar populations can be a major contributor to the heating of dust. In M 81, old stellar populations are the dominant heating agent in the central regions, contributing to half of the absorbed radiation. Regions of higher star formation do not correspond to the highest dust temperatures. On the contrary, it is the dominant bulge which is most efficient in heating the dust. The approach we present here can immediately be applied to other galaxies. It does contain a number of caveats, which we discuss in detail. © ESO 2020.
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- 2020
5. Reproducing the universe: A comparison between the EAGLE simulations and the nearby DustPedia galaxy sample
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Trčka, A. Baes, M. Camps, P. Meidt, S.E. Trayford, J. Bianchi, S. Casasola, V. Cassarà, L.P. de Looze, I. de Vis, P. Dobbels, W. Fritz, J. Galametz, M. Galliano, F. Katsianis, A. Madden, S.C. Mosenkov, A.V. Nersesian, A. Viaene, S. Xilouris, E.M.
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Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We compare the spectral energy distributions (SEDs) and inferred physical properties for simulated and observed galaxies at low redshift. We exploit UV-submillimetre mock fluxes of ∼7000 z = 0 galaxies from the EAGLE suite of cosmological simulations, derived using the radiative transfer code SKIRT. We compare these to ∼800 observed galaxies in the UV-submillimetre range, from the DustPedia sample of nearby galaxies. To derive global properties, we apply the SED fitting code CIGALE consistently to both data sets, using the same set of ∼80 million models. The results of this comparison reveal overall agreement between the simulations and observations, both in the SEDs and in the derived physical properties, with a number of discrepancies. The optical and far-infrared regimes, and the scaling relations based upon the global emission, diffuse dust, and stellar mass, show high levels of agreement. However, the mid-infrared fluxes of the EAGLE galaxies are overestimated while the far-UV domain is not attenuated enough, compared to the observations. We attribute these discrepancies to a combination of galaxy population differences between the samples and limitations in the subgrid treatment of star-forming regions in the EAGLE-SKIRT post-processing recipe. Our findings show the importance of detailed radiative transfer calculations and consistent comparison, and provide suggestions for improved numerical models. © 2020 The Author(s)
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- 2020
6. SOFIA/FIFI-LS Full-disk [C ii] Mapping and CO-dark Molecular Gas across the Nearby Spiral Galaxy NGC 6946
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Bigiel, F., primary, Looze, I. de, additional, Krabbe, A., additional, Cormier, D., additional, Barnes, A. T., additional, Fischer, C., additional, Bolatto, A. D., additional, Bryant, A., additional, Colditz, S., additional, Geis, N., additional, Herrera-Camus, R., additional, Iserlohe, C., additional, Klein, R., additional, Leroy, A. K., additional, Linz, H., additional, Looney, L. W., additional, Madden, S. C., additional, Poglitsch, A., additional, Stutzki, J., additional, and Vacca, W. D., additional
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- 2020
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7. Erratum: “Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample” (2020, ApJ, 889, 150)
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Aniano, G., primary, Draine, B. T., additional, Hunt, L. K., additional, Sandstrom, K., additional, Calzetti, D., additional, Kennicutt, R. C., additional, Dale, D. A., additional, Galametz, M., additional, Gordon, K. D., additional, Leroy, A. K., additional, Smith, J.-D. T., additional, Roussel, H., additional, Sauvage, M., additional, Walter, F., additional, Armus, L., additional, Bolatto, A. D., additional, Boquien, M., additional, Crocker, A., additional, Looze, I. De, additional, Meyer, J. Donovan, additional, Helou, G., additional, Hinz, J., additional, Johnson, B. D., additional, Koda, J., additional, Miller, A., additional, Montiel, E., additional, Murphy, E. J., additional, Relaño, M., additional, Rix, H.-W., additional, Schinnerer, E., additional, Skibba, R., additional, Wolfire, M. G., additional, and Engelbracht, C. W., additional
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- 2020
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8. Old and young stellar populations in DustPedia galaxies and their role in dust heating
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Nersesian, A. Xilouris, E.M. Bianchi, S. Galliano, F. Jones, A.P. Baes, M. Casasola, V. Cassarà, L.P. Clark, C.J.R. Davies, J.I. Decleir, M. Dobbels, W. De Looze, I. De Vis, P. Fritz, J. Galametz, M. Madden, S.C. Mosenkov, A.V. Trčka, A. Verstocken, S. Viaene, S. Lianou, S.
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Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Aims. Within the framework of the DustPedia project we investigate the properties of cosmic dust and its interaction with stellar radiation (originating from di erent stellar populations) for 814 galaxies in the nearby Universe, all observed by the Herschel Space Observatory. Methods. We take advantage of the widely used fitting code CIGALE, properly adapted to include the state-of-the-art dust model THEMIS. For comparison purposes, an estimation of the dust properties is provided by approximating the emission at far-infrared and sub-millimeter wavelengths with a modified blackbody. Using the DustPedia photometry we determine the physical properties of the galaxies, such as the dust and stellar mass, the star-formation rate, the bolometric luminosity, the unattenuated and the absorbed by dust stellar light, for both the old (>200 Myr) and young (≤200 Myr) stellar populations. Results. We show how the mass of stars, dust, and atomic gas, as well as the star-formation rate and the dust temperature vary between galaxies of di erent morphologies and provide recipes to estimate these parameters given their Hubble stage (T). We find a mild correlation between the mass fraction of the small a-C(:H) grains with the specific star-formation rate. On average, young stars are very ecient in heating the dust, with absorption fractions reaching as high as ~77% of the total unattenuated luminosity of this population. On the other hand, the maximum absorption fraction of old stars is ~24%. Dust heating in early-type galaxies is mainly due to old stars, up to a level of ~90%. Young stars progressively contribute more for 'typical' spiral galaxies and they become the dominant source of dust heating for Sm-type and irregular galaxies, with ~60% of their luminosity contributing to that purpose. Finally, we find a strong correlation of the dust heating fraction by young stars with morphology and the specific star-formation rate. © ESO 2019.
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- 2019
9. Dust emissivity and absorption cross section in DustPedia late-type galaxies
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Bianchi, S. Casasola, V. Baes, M. Clark, C.J.R. Corbelli, E. Davies, J.I. De Looze, I. De Vis, P. Dobbels, W. Galametz, M. Galliano, F. Jones, A.P. Madden, S.C. Magrini, L. Mosenkov, A. Nersesian, A. Viaene, S. Xilouris, E.M. Ysard, N.
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Aims. We compare the far-infrared to sub-millimetre dust emission properties measured in high Galactic latitude cirrus with those determined in a sample of 204 late-type DustPedia galaxies. The aim is to verify if it is appropriate to use Milky Way dust properties to derive dust masses in external galaxies. Methods. We used Herschel observations and atomic and molecular gas masses to estimate ϵ (250 μm), the disc-averaged dust emissivity at 250 μm, and from this, the absorption cross section per H atom σ(250 μm) and per dust mass κ(250 μm). The emissivity ϵ (250 μm) requires one assumption, which is the CO-to-H2 conversion factor, and the dust temperature is additionally required for σ(250 μm); yet another constraint on the dust-to-hydrogen ratio D/H, depending on metallicity, is required for κ(250 μm). Results. We find ϵ (250 μm) = 0.82 ± 0.07 MJy sr-1 (1020 H cm-2)-1 for galaxies with 4 < F(250 μm)/F(500 μm) < 5. This depends only weakly on the adopted CO-to-H2 conversion factor. The value is almost the same as that for the Milky Way at the same colour ratio. Instead, for F(250 μm)/F(500 μm) > 6, ϵ (250 μm) is lower than predicted by its dependence on the heating conditions. The reduction suggests a variation in dust emission properties for spirals of earlier type, higher metallicity, and with a higher fraction of molecular gas. When the standard emission properties of Galactic cirrus are used for these galaxies, their dust masses might be underestimated by up to a factor of two. Values for σ(250 μm) and κ(250 μm) at the Milky Way metallicity are also close to those of the cirrus. Mild trends of the absorption cross sections with metallicity are found, although the results depend on the assumptions made. © ESO 2019.
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- 2019
10. Dust emission profiles of DustPedia galaxies
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Mosenkov, A.V. Baes, M. Bianchi, S. Casasola, V. Cassarà, L.P. Clark, C.J.R. Davies, J. De Looze, I. De Vis, P. Fritz, J. Galametz, M. Galliano, F. Jones, A.P. Lianou, S. Madden, S.C. Nersesian, A. Smith, M.W.L. Trčka, A. Verstocken, S. Viaene, S. Vika, M. Xilouris, E.
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Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Most radiative transfer models assume that dust in spiral galaxies is distributed exponentially. In this paper our goal is to verify this assumption by analysing the two-dimensional large-scale distribution of dust in galaxies from the DustPedia sample. For this purpose, we have made use of Herschel imaging in five bands, from 100 to 500 μm, in which the cold dust constituent is primarily traced and makes up the bulk of the dust mass in spiral galaxies. For a subsample of 320 disc galaxies, we successfully performed a simultaneous fitting with a single Srsic model of the Herschel images in all five bands using the multi-band modelling code galfitm. We report that the Srsic index n, which characterises the shape of the Srsic profile, lies systematically below 1 in all Herschel bands and is almost constant with wavelength. The average value at 250 μm is 0:67 ± 0:37 (187 galaxies are fitted with n 250 = 0:75, 87 galaxies have 0:75 < n 250 = 1:25, and 46 with n 250 > 1:25). Most observed profiles exhibit a depletion in the inner region (at r < 0:3-0:4 of the optical radius r 25 ) and are more or less exponential in the outer part. We also find breaks in the dust emission profiles at longer distances (0:5-0:6) r25 which are associated with the breaks in the optical and near-infrared. We assumed that the observed deficit of dust emission in the inner galaxy region is related to the depression in the radial profile of the Hi surface density in the same region because the atomic gas reaches high enough surface densities there to be transformed into molecular gas. If a galaxy has a triggered star formation in the inner region (for example, because of a strong bar instability, which transfers the gas inwards to the centre, or a pseudobulge formation), no depletion or even an excess of dust emission in the centre is observed. © 2019 ESO.
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- 2019
11. The Origin of [C ii] 157μm Emission in a Five-component Interstellar Medium: The Case of NGC 3184 and NGC 628
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Abdullah, A., primary, Brandl, B. R., additional, Groves, B., additional, Wolfire, M., additional, Calzetti, D., additional, Croxall, K., additional, Looze, I. de, additional, Kennicutt, R. C., additional, Sandstrom, K. M., additional, Armus, L., additional, Dale, D. A., additional, Galametz, M., additional, Herrera-Camus, R., additional, Hunt, L. K., additional, Smith, J. D., additional, and Tielens, A. G. G. M., additional
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- 2017
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12. DustPedia: A Definitive Study of Cosmic Dust in the Local Universe
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Davies, J. I., primary, Baes, M., additional, Bianchi, S., additional, Jones, A., additional, Madden, S., additional, Xilouris, M., additional, Bocchio, M., additional, Casasola, V., additional, Cassara, L., additional, Clark, C., additional, Looze, I. De, additional, Evans, R., additional, Fritz, J., additional, Galametz, M., additional, Galliano, F., additional, Lianou, S., additional, Mosenkov, A. V., additional, Smith, M., additional, Verstocken, S., additional, Viaene, S., additional, Vika, M., additional, Wagle, G., additional, and Ysard, N., additional
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- 2017
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13. Updated 34-band Photometry for the SINGS/KINGFISH Samples of Nearby Galaxies
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Dale, D. A., primary, Cook, D. O., additional, Roussel, H., additional, Turner, J. A., additional, Armus, L., additional, Bolatto, A. D., additional, Boquien, M., additional, Brown, M. J. I., additional, Calzetti, D., additional, Looze, I. De, additional, Galametz, M., additional, Gordon, K. D., additional, Groves, B. A., additional, Jarrett, T. H., additional, Helou, G., additional, Herrera-Camus, R., additional, Hinz, J. L., additional, Hunt, L. K., additional, Kennicutt, R. C., additional, Murphy, E. J., additional, Rest, A., additional, Sandstrom, K. M., additional, Smith, J.-D. T., additional, Tabatabaei, F. S., additional, and Wilson, C. D., additional
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- 2017
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14. The Radio Spectral Energy Distribution and Star-formation Rate Calibration in Galaxies
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Tabatabaei, F. S., primary, Schinnerer, E., additional, Krause, M., additional, Dumas, G., additional, Meidt, S., additional, Damas-Segovia, A., additional, Beck, R., additional, Murphy, E. J., additional, Mulcahy, D. D., additional, Groves, B., additional, Bolatto, A., additional, Dale, D., additional, Galametz, M., additional, Sandstrom, K., additional, Boquien, M., additional, Calzetti, D., additional, Kennicutt, R. C., additional, Hunt, L. K., additional, Looze, I. De, additional, and Pellegrini, E. W., additional
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- 2017
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15. THE IONIZED GAS IN NEARBY GALAXIES AS TRACED BY THE [NII] 122 AND 205 μm TRANSITIONS
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Herrera-Camus, R., primary, Bolatto, A., additional, Smith, J. D., additional, Draine, B., additional, Pellegrini, E., additional, Wolfire, M., additional, Croxall, K., additional, Looze, I. de, additional, Calzetti, D., additional, Kennicutt, R., additional, Crocker, A., additional, Armus, L., additional, van der Werf, P., additional, Sandstrom, K., additional, Galametz, M., additional, Brandl, B., additional, Groves, B., additional, Rigopoulou, D., additional, Walter, F., additional, Leroy, A., additional, Boquien, M., additional, Tabatabaei, F. S., additional, and Beirao, P., additional
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- 2016
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16. REGIONAL VARIATIONS IN THE DENSE GAS HEATING AND COOLING IN M51 FROM HERSCHEL Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. FAR-INFRARED SPECTROSCOPY
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Parkin, T. J., Wilson, C. D., Schirm, M. R. P., Baes, M., Boquien, M., Boselli, A., Cooray, A., Cormier, D., Foyle, K., Karczewski, O. Ł., Lebouteiller, V., Looze, I. de, Madden, S. C., Roussel, H., Sauvage, M., and Spinoglio, L.
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PHOTONS ,GALAXIES ,MOLECULAR clouds ,INTERSTELLAR molecules ,ULTRAVIOLET radiation - Abstract
We present Herschel PACS and SPIRE spectroscopy of the most important far-infrared cooling lines in M51, [C II](158 μm), [N II](122 and 205 μm), [O I](63 and 145 μm), and [O III](88 μm). We compare the observed flux of these lines with the predicted flux from a photon-dominated region model to determine characteristics of the cold gas such as density, temperature, and the far-ultraviolet (FUV) radiation field, G
0 , resolving details on physical scales of roughly 600 pc. We find an average [C II]/FTIR of 4 × 10–3 , in agreement with previous studies of other galaxies. A pixel-by-pixel analysis of four distinct regions of M51 shows a radially decreasing trend in both the FUV radiation field, G0 , and the hydrogen density, n, peaking in the nucleus of the galaxy, and then falling off out to the arm and interarm regions. We see for the first time that the FUV flux and gas density are similar in the differing environments of the arm and interarm regions, suggesting that the inherent physical properties of the molecular clouds in both regions are essentially the same. [ABSTRACT FROM AUTHOR]- Published
- 2013
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17. THE PHYSICAL CHARACTERISTICS OF THE GAS IN THE DISK OF CENTAURUS A USING THE HERSCHEL SPACE OBSERVATORY.
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Parkin, T. J., Wilson, C. D., Schirm, M. R. P., Baes, M., Boquien, M., Boselli, A., Cormier, D., Galametz, M., Karczewski, O. Ł., Lebouteiller, V., Looze, I. De, Madden, S. C., Roussel, H., Smith, M. W. L., and Spinoglio, L.
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CENTAURUS (Constellation) ,DISKS (Astrophysics) ,INTERSTELLAR medium ,ASTROPHYSICS research - Abstract
We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. In particular, we observe the [C II](158 μm), [N II](122 and 205 μm), [O I](63 and 145 μm), and [O III](88 μm) lines, which all play an important role in cooling the gas in photo-ionized and photodissociation regions (PDRs). We determine that the ([C II]+[O I]
63 )/FTIR line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10%-20% of the observed [C II] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, G0 , varies between 101.75 and 102.75 and the hydrogen nucleus density varies between 102.75 and 103.75 cm–3 , with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies. [ABSTRACT FROM AUTHOR]- Published
- 2014
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18. COLD DUST BUT WARM GAS IN THE UNUSUAL ELLIPTICAL GALAXY NGC 4125.
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Wilson, C. D., Cridland, A., Foyle, K., Parkin, T. J., Cooper, E. Mentuch, Roussel, H., Sauvage, M., Smith, M. W. L., Baes, M., Bendo, G., Boquien, M., Boselli, A., Ciesla, L., Clements, D. L., Cooray, A., Looze, I. De, Galametz, M., Gear, W., Lebouteiller, V., and Madden, S.
- Published
- 2013
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