L. Matrà 1,2 , B. Merín 1 , C. Alves de Oliveira 1 , N. Huélamo 3 , Á. Kóspál 4 , N. L.J. Cox 5 , Á. Ribas 1,3 , E. Puga 1 , R. Vavrek 1 , P. Royer 5 , T. Prusti 4 , G. L. Pilbratt 4 , and P. André 6 1 ESA – ESAC Herschel Science Centre, 2 TCD - School of Physics, 3 Centro de Astrobiología, 4 ESA - ESTEC, 5 K.U. Leuven, 6 Saclay Introduction Introduction Transitional disks (TDs) are circumstellar disks that present inner clearings or gaps induced by different physical processes, which cause a wide range of spectral energy distribution (SED) properties to be observed. This makes TDs not easy to disentangle from sources of different nature, such as systems with nebulosity in their surroundings. Herschel, with its high spatial resolution, can greatly serve the purpose of detecting contamination at far-IR and sub-mm wavelengths. The young T54 binary system, in the Chamaeleon I star-forming region, was classified as a transitional/circumbinary disk, but new Herschel images revealed something unexpected. Acknowledgements This work was partially made possible thanks to the ESA Trainee and Research Fellowship programs at ESAC (Spain). Support was also provided by the Enterprise Ireland Space Education Program, and by the Belgian Federal Science Policy Office via the PRODEX Programme of ESA. IC 348 Perseus Rho Ophiuchi Serpens Core NGC 1333 Perseus Figure 1: The T54 (northern cross) system at different wavelengths. North is up, east is left. Herschel images show extended emission offset from it, resolved at 70 μm (arrows) and causing most of the emission at longer wavelengths (dashed ellipse). This is not observed at shorter wavelengths. The southern cross represents the unrelated object 2MASS J11124076-7722378. The diameter of the circles in the bottom left of each image represents the FWHM of the different PSFs. Figure 2 : SED of T54, with the blue solid triangles representing Herschel fluxes not attributed to T54 but to off-source extended emission. The dashed line is a NEXTGEN stellar model for spectral type G8. The red line is the Spitzer IRS spectrum. The green solid line represents a T = 94 K blackbody curve fit to the mid-IR fluxes. We obtain a stellar luminosity of ~3.66 L that with a temperature of 5520 K from Kim et al. (2009) leads to a mass of approximately 1.5 M and an age between 3 and 10 Myr. The blackbody fit (green line in Fig. 2) to remaining excess yields a dust temperature of ~94 K and a fractional luminosity value of 0.005. Get the full paper! Matrà et al. (2012), A&A, in press. http://arxiv.org/abs/1210.7679 Luca Matrà: [email protected] However, if a disk is to be present, it would fall under the definition of debris disk from Wyatt (2008). In such picture, the calculated disk radius would make T54 an interesting case of an evolved disk around a single binary component. Regarding the remaining excess, T54 shows no silicate feature at 10 μm and PAH emission at 11.3 μm, setting it among other examples of dubious disks. One such example (see Fig. 3) is the strikingly similar system DoAr 21. Figure 3 : High-resolution images of DoAr 21 from Jensen et al. 2009. Analogous extended emission at these scales could explain the remaining unresolved excess in T54. Figure 4 : Possible configuration if an evolved disk was to be present in the T54 binary system (not to scale)
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L. Matrà1,2, B. Merín1, C. Alves de Oliveira1, N. Huélamo3, Á. Kóspál4, N. L.J. Cox5, Á. Ribas1,3, E. Puga1, R. Vavrek1, P. Royer5, T. Prusti4, G. L. Pilbratt4, and P. André6
1 ESA – ESAC Herschel Science Centre, 2 TCD - School of Physics, 3 Centro de Astrobiología, 4 ESA - ESTEC, 5 K.U. Leuven, 6 Saclay
IntroductionIntroduction
Transitional disks (TDs) are circumstellar disks that present inner clearings or gaps induced by different physical processes, which cause a wide range of spectral energy distribution (SED) properties to be observed. This makes TDs not easy to disentangle from sources of different nature, such as systems with nebulosity in their surroundings. Herschel, with its high spatial resolution, can greatly serve the purpose of detecting contamination at far-IR and sub-mm wavelengths. The young T54 binary system, in the Chamaeleon I star-forming region, was classified as a transitional/circumbinary disk, but new Herschel images revealed something unexpected.
Acknowledgements
This work was partially made possible thanks to the ESA Trainee and Research Fellowship programs at ESAC (Spain).
Support was also provided by the Enterprise Ireland Space Education Program, and by the Belgian Federal Science Policy
Office via the PRODEX Programme of ESA.
IC 348 Perseus Rho Ophiuchi
Serpens CoreNGC 1333 Perseus
Figure 1: The T54 (northern cross) system at different wavelengths. North is up, east is left. Herschel images show extended emission offset from it, resolved at 70 μm (arrows) and causing most of the emission at longer wavelengths (dashed ellipse). This is not observed at shorter wavelengths. The southern cross represents the unrelated object 2MASS J11124076-7722378. The diameter of the circles in the bottom left of each image represents the FWHM of the different PSFs.
Figure 2: SED of T54, with the blue solid triangles representing Herschel fluxes not attributed to T54 but to off-source extended emission. The dashed line is a NEXTGEN stellar model for spectral type G8. The red line is the Spitzer IRS spectrum. The green solid line represents a T = 94 K blackbody curve fit to the mid-IR fluxes.
We obtain a stellar luminosity of ~3.66 L that with a temperature of 5520 K from Kim et al. (2009) leads to a mass of approximately 1.5 M and an age between 3 and 10 Myr. The blackbody fit (green line in Fig. 2) to remaining excess yields a dust temperature of ~94 K and a fractional luminosity value of 0.005.
Get the full paper! Matrà et al. (2012), A&A, in press.http://arxiv.org/abs/1210.7679
Luca Matrà: [email protected]
However, if a disk is to be present, it would fall under the definition of debris disk from Wyatt (2008). In such picture, the calculated disk radius would make T54 an interesting case of an evolved disk around a single binary component.
Regarding the remaining excess, T54 shows no silicate feature at 10 μm and PAH emission at 11.3 μm, setting it among other examples of dubious disks. One such example (see Fig. 3) is the strikingly similar system DoAr 21.
Figure 3: High-resolution images of DoAr 21 from Jensen et al. 2009. Analogous extended emission at these scales could explain the remaining unresolved excess in T54.
Figure 4: Possible configuration if an evolved disk was to be present in the T54 binary system (not to scale)
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