Polarimetry of the binary PDS 144

Abstract

Aims. Our goal is to study the circumstellar environment associated with each component of the wide intermediate-mass pre-main sequence binary system PDS 144 using broadband polarimetry. Methods. We present near-infrared (NIR) linear polarimetric observations of PDS 144 gathered with the IAGPOL imaging polarimeter along with the CamIV infrared camera at the Observatório do Pico dos Dias (OPD). In addition, we re-analyzed OPD archive optical polarization to separate the binary and estimate the interstellar polarization using foreground stars. Results. After discounting the interstellar component, we found that both stars of the binary system are intrinsically polarized. The polarization vectors at optical and NIR bands of both components are aligned with the local magnetic field and the jet axis. These findings indicate an interplay between the interstellar magnetic field and the formation of the binary system. We also found that the PDS 144N is less polarized than its southern companion in the optical. However, in the NIR PDS 144N is more polarized. Our polarization data can only be explained by high inclinations (i 80 • ) for the disks of both members. In particular, comparisons of our NIR data with young stellar objects disk models suggest predominantly small grains in the circumstellar environment of PDS 144N. In spite of the different grain types in each component, the infrared spectral indexes indicate a coeval system. We also found evidence of coplanarity between the disks.

Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars

“…type: A5V), lacks PAH emission. PDS 144N & S are found to have intrinsic polarization, which is aligned with the local magnetic field and the jet axis (Pereyra et al 2012), and the high NIR polarization of the PDS 144N disk is in favor of the presence of small grains similar to those of the diffuse ISM. Schütz et al (2009) found that the spectral profile of the 8.6 µm PAH feature is similar to that of PAHs in the ISM (i.e., PAH class A as determined by Peeters et al 2002), whereas the peak wavelength of the 11.2 µm PAH feature is red-shifted compared to those of class A and B profiles.…”