Photometric mapping with ISOPHOT using the “P32” Astronomical Observation Template

Tuffs, R.; Gabriel, C.

doi:10.1051/0004-6361:20030899

Cited by 28 publications

(27 citation statements)

References 16 publications

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“…The discovery of this diffuse component was one of the highlights of the Infrared Space Observatory (ISO) (see Tuffs & Popescu 2006;Sauvage et al 2006, for reviews on the ISO science legacy on normal nearby galaxies). This result was obtained both from analysing the integrated properties of infrared emission from galaxies but also from resolved studies of nearby galaxies (Haas et al 1998;Hippelein et al 2003;Tuffs & Gabriel 2003;Popescu et al 2005) and is now being confirmed by the infrared data from Spitzer (Pérez-González et al 2006;Hinz et al 2006;Dale et al 2007;Bendo et al 2008;Kennicutt et al 2009) and AKARI (Suzuki et al 2007). Our model being empirically motivated we tried to incorporate all available observational constraints provided by the data.…”

Section: The Distribution Of Stars and Dustmentioning

confidence: 74%

Modelling the spectral energy distribution of galaxies

Popescu

Tuffs

Dopita

et al. 2011

A&A

Self Cite

207

454

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We present a self-consistent model of the spectral energy distributions (SEDs) of spiral galaxies from the ultraviolet (UV) to the mid-infrared (MIR)/far-infrared (FIR)/submillimeter (submm) based on a full radiative transfer calculation of the propagation of starlight in galaxy disks. This model predicts not only the total integrated energy absorbed in the UV/optical and re-emitted in the infrared/submm, but also the colours of the dust emission based on an explicit calculation of the strength and colour of the UV/optical radiation fields heating the dust, and incorporating a full calculation of the stochastic heating of small dust grains and PAH molecules. The geometry of the translucent components of the model is empirically constrained using the results from the radiation transfer analysis of Xilouris et al. on spirals in the middle range of the Hubble sequence, while the geometry of the optically thick components is constrained from physical considerations with a posteriori checks of the model predictions with observational data. Following the observational constraints, the model has both a distribution of diffuse dust associated with the old and young disk stellar populations as well as a clumpy component arising from dust in the parent molecular clouds in star forming regions. In accordance with the fragmented nature of dense molecular gas in typical star-forming regions, UV light from massive stars is allowed to either freely stream away into the diffuse medium in some fraction of directions or be geometrically blocked and locally absorbed in clumps. These geometrical constraints enable the dust emission to be predicted in terms of a minimum set of free parameters: the central face-on dust opacity in the B-band τ f B , a clumpiness factor F for the star-forming regions, the star-formation rate SFR, the normalised luminosity of the old stellar population old and the bulge-to-disk ratio B/D. We show that these parameters are almost orthogonal in their predicted effect on the colours of the dust/PAH emission. In most practical applications B/D will actually not be a free parameter but (together with the angular size θ gal and inclination i of the disk) act as a constraint derived from morphological decomposition of higher resolution optical images. This also extends the range of applicability of the model along the Hubble sequence. We further show that the dependence of the dust emission SED on the colour of the stellar photon field depends primarily on the ratio between the luminosities of the young and old stellar populations (as specified by the parameters SFR and old) rather than on the detailed colour of the emissions from either of these populations. The model is thereby independent of a priori assumptions of the detailed mathematical form of the dependence of SFR on time, allowing UV/optical SEDs to be dereddened without recourse to population synthesis models. Utilising these findings, we show how the predictive power of radiative transfer calculations can be combined with measurements of θ ...

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Section: The Distribution Of Stars and Dustmentioning

confidence: 74%

Modelling the spectral energy distribution of galaxies

Popescu

Tuffs

Dopita

et al. 2011

A&A

Self Cite

207

454

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“…At different single epochs 60, 100, and 200 μm high-resolution maps were performed using the Astronomical Observing Template P32. These data were processed using a dedicated P32 Tool (Tuffs & Gabriel 2003) and the calibration used the related FCS measurements. The flux values were colorcorrected by convolving the SED of EX Lup with the ISOPHOT filter profiles.…”

Section: Infrared Space Observatory (Iso)mentioning

confidence: 99%

EX Lupi in quiescence

Sipos

Ábrahám

Acosta–Pulido

et al. 2009

A&A

111

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Aims. EX Lupi is the prototype of EXors, a subclass of low-mass pre-main sequence stars whose episodic eruptions are attributed to temporarily increased accretion. In quiescence the optical and near-infrared properties of EX Lup cannot be distinguished from those of normal T Tau stars. Here we investigate whether it is the circumstellar disk structure that makes EX Lup an atypical Class II object. During outburst the disk might undergo structural changes. Our characterization of the quiescent disk is intended to serve as a reference for studying the physical changes related to one of EX Lupi's strongest known eruptions in 2008 Jan-Sep. Methods. We searched the literature for photometric and spectroscopic observations including ground-based, IRAS, ISO, and Spitzer data. After constructing the optical-infrared spectral energy distribution (SED), we compared it with the typical SEDs of other young stellar objects and modeled it using the Monte Carlo radiative transfer code RADMC. We determined the mineralogical composition of the 10 μm silicate emission feature and also gave a description of the optical and near-infrared spectra. Results. The SED is similar to that of a typical T Tauri star in most aspects, though EX Lup emits higher flux above 7 μm. The quiescent phase data suggest low-level variability in the optical-mid-infrared domain. By integrating the optical and infrared fluxes, we derived a bolometric luminosity of 0.7 L . The 10 μm silicate profile could be fitted by a mixture consisting of amorphous silicates, but no crystalline silicates were found. A modestly flaring disk model with a total mass of 0.025 M and an outer radius of 150 AU was able to reproduce the observed SED. The derived inner radius of 0.2 AU is larger than the sublimation radius, and this inner gap sets EX Lup apart from typical T Tauri stars.

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“…When we increase dust scale-heights from 0.25 to 0.35 kpc, temperatures change by no more than 1-2 degrees. In order to determine the total luminosity of M 51, we integrated the UV (OAO), visual and far-infrared (IRAS) flux densities as provided in the NASA/IPAC Extragalactic Database, the 170 µm point as given by Tuffs & Gabriel (2003) and our 850 µm point. We find a luminosity of L tot = 1.1 × 10 11 L , which corresponds to a star formation rate of a few M yr −1 , with an estimated uncertainty of about 30%.…”

Section: Stellar Parametersmentioning

confidence: 99%

A submillimeter exponential disk in M 51: Evidence for an extended cold dust disk

Meijerink¹,

Tilanus

Dullemond

et al. 2005

A&A

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Abstract.A 850 µm map of the interacting spiral galaxy M 51 shows well-defined spiral arms, closely resembling the structures seen in CO and HI emission. However, most of the 850 µm emission originates in an underlying exponential disk, a component that has not been observed before in a face-on galaxy at these wavelengths. The scale-length of this disk is 5.45 kpc, which is somewhat larger than the scale-length of the stellar disk, but somewhat smaller than that of atomic hydrogen. Its profile cannot be explained solely by a radial disk temperature gradient but requires the underlying dust to have an exponential distribution as well. This reinforces the view that the submm emission from spiral galaxy disks traces total hydrogen column density, i.e. the sum of H 2 and H . A canonical gas-to-dust ratio of 100 ± 26 is obtained for κ 850 = 1.2 g −1 cm 2 , where κ 850 is the dust opacity at 850 µm.

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Photometric mapping with ISOPHOT using the “P32” Astronomical Observation Template

Cited by 28 publications

References 16 publications

Modelling the spectral energy distribution of galaxies

Modelling the spectral energy distribution of galaxies

EX Lupi in quiescence

A submillimeter exponential disk in M 51: Evidence for an extended cold dust disk

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