C2D Spitzer-IRS spectra of disks around T Tauri stars

II. PAH emission features

¹ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands e-mail: vcgeers@strw.leidenuniv.nl
² Laboratoire d'Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
³ Division of GPS, Mail Code 150-21, California Institute of Technology, Pasadena, CA 91125, USA
⁴ Max-Plank-Institut für Astronomie, Koenigstuhl 17, 69117 Heidelberg, Germany
⁵ Department of Astronomy, University of Texas, 1 University Station C1400, Austin, TX 78712-0259, USA
⁶ Division of PMA, Mail Code 105-24, California Institute of Technology, Pasadena, CA 91125, USA
⁷ SRON, PO Box 800, 9700 AV Groningen, The Netherlands

Received: 9 January 2006
Accepted: 22 August 2006

Abstract

Aims.We search for Polycyclic Aromatic Hydrocarbon (PAH) features towards young low-mass (T Tauri) stars and compare them with surveys of intermediate mass (Herbig Ae/Be) stars. The presence and strength of the PAH features are interpreted with disk radiative transfer models exploring the PAH feature dependence on the incident UV radiation, PAH abundance and disk parameters.

Methods.Spitzer Space Telescope 5–35 μm spectra of 54 pre-main sequence stars with disks were obtained, consisting of 38 T Tauri, 7 Herbig Ae/Be and 9 stars with unknown spectral type.

Results.Compact PAH emission is detected towards at least 8 sources of which 5 are Herbig Ae/Be stars. The 11.2 μm PAH feature is detected in all of these sources, as is the 6.2 μm PAH feature for the 4 sources for which short wavelength data are available. However, the 7.7 and 8.6 μm features appear strongly in only 1 of these 4 sources. Based on the 11.2 μm feature, PAH emission is observed towards at least 3 T Tauri stars, with 14 tentative detections, resulting in a lower limit to the PAH detection rate of 8%. The lowest mass source with PAH emission in our sample is T Cha with a spectral type G8. All 4 sources in our sample with evidence for dust holes in their inner disk show PAH emission, increasing the feature/continuum ratio. Typical 11.2 μm line intensities are an order of magnitude lower than those observed for the more massive Herbig Ae/Be stars. Measured line fluxes indicate PAH abundances that are factors of 10–100 lower than standard interstellar values. Conversely, PAH features from disks exposed to stars with K without enhanced UV are predicted to be below the current detection limit, even for high PAH abundances. Disk modeling shows that the 6.2 and 11.2 μm features are the best PAH tracers for T Tauri stars, whereas the 7.7 and 8.6 μm bands have low feature over continuum ratios due to the strongly rising silicate emission.