Near-Infrared Imaging Polarimetry of Embedded Young Stars in the Taurus-Auriga Molecular Cloud

Details Near-Infrared Imaging Polarimetry of Embedded Young Stars in the Taurus-Auriga Molecular Cloud Near-Infrared Imaging Polarimetry of Embedded Young Stars in the Taurus-Auriga Molecular Cloud

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...485..703w&link_type=abstract

Astrophysical Journal v.485, p.703

Astronomy and Astrophysics

Astronomy

97

Infrared: Stars, Stars: Formation, Stars: Pre-Main-Sequence, Ism: Reflection Nebulae, Polarization

Scientific paper

We describe near-infrared (JHK) imaging polarimetry of 21 embedded protostars in the Taurus-Auriga molecular cloud. These objects display extended, highly polarized reflection nebulae with V-shaped, unipolar, and bipolar morphologies. Most sources have PK ~ 5%-20% in an 8" aperture; a few objects have PK <~ 5%. The polarization increases toward shorter wavelengths and is generally aligned perpendicular to the long axis of the reflection nebula. We develop an analytic scattering model for the near-IR colors and polarizations of embedded protostars. Our Taurus data require visual extinctions, AV ~ 25-60 mag, comparable to those predicted for models of collapsing clouds. The ratio of scattered flux to intrinsic source flux ranges from Fs/F0 ~ 0.001 at 1.25 mu m to Fs/F0 ~ 0.015 at 3.5 mu m. These results indicate that the observed ratio of scattered light to direct (extincted) light increases from Fs/Fd ~ 0.1 at 3.5 mu m to Fs/Fd ~ 25 at 1.25 mu m. Our data further require intrinsic colors of 0.6 <~ J-H <~ 0.9, 0.3 <~ H-K <~ 0.6, and 0.4 <~ K-L <~ 1.2 for the central sources of Taurus protostars. We adopt the Terebey, Shu, & Cassen solution for an infalling, rotating protostellar cloud and use a two dimensional Monte Carlo radiative transfer code to model the near-IR polarization data for this sample. Our results indicate envelope parameters in agreement with previous estimates from broadband spectral energy distributions and near-IR images. We estimate infall rates, M dot ~(2-5)x10^{-6} M&sun; yr-1; centrifugal radii, Rc ~ 10-50 AU; and opening angles of the bipolar cavity, theta h ~ 10 deg-20 deg, for a typical object. Standard grain parameters can explain the near-IR colors and polarizations of Taurus protostars. The polarization maps show that Taurus grains have a high maximum polarization at K, Pmax,K >~ 80%. The large image sizes of this sample further imply a high K-band albedo, omega K ~ 0.3-0.4. Model polarization maps indicate that the size of the "polarization disk" increases with the size of the instrumental point-spread function. Relating the morphology of polarization vectors to disk or envelope properties thus requires some care and a good understanding of the characteristics of the instrument.

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