SMA Observations of the Herbig Ae star AB Aur. Nagayoshi Ohashi (ASIAA). Main Collaborators: S.-Y. Lin 1 , J. Lim 2 , P. Ho 3 , M. Momose 4 , M. Fukagawa 5 (1. NTHU, 2. ASIAA, 3. SAO, 4. Ibaraki Univ., 5. Uinv. Of Tokyo) This study is a part of the master thesis of S.-Y. Lin.
Nagayoshi Ohashi (ASIAA)
Main Collaborators: S.-Y. Lin1, J. Lim2, P. Ho3, M. Momose4, M. Fukagawa5 (1. NTHU, 2. ASIAA, 3. SAO, 4. Ibaraki Univ., 5. Uinv. Of Tokyo)
This study is a part of the master thesis of S.-Y. Lin.
12CO 2-1 integrated
12CO 2-1 mean velocityObservations of Herbig Ae stars using mm-interferometers
Manning, Koerner, & Sargent 1997, Nature
Interferometers can help us to understand basic
characteristics of circumstellar disks.
angular resolution (~5”).
outer armAB Aur: 1.6 mm Coronagraphic Image
What is the actual disk structure?
12CO (3-2) and 345 GHz dust continuum were simultaneously observed using the Submillimeter Array (SMA) in 2003 and 2004.
12CO (3-2) traces warmer, denser gas, while stronger dust
emission at 345 GHz may show more details of the disk structure.
Compact and extended configurations; three tracks
Velocity resolution ~0.2 km/s
Total bandwidth: 2 GHz for each side band
Angular resolution (natural weight): 1.0” x 0.7” (~140 AU x 90 AUSMA Observations of AB Aur
AB Aur was also independently observed using the OVRO
mm-array (Corder et al. 2004), the PdBI (Pietu et al.2005), and the NMA (Ohashi, Momose et al.) at mm-wavelengths.
The structure of the dust disk seems to be very different
from those of CDs around other Herbig Ae/T Tauri stars.
SMA 850 m
PdBI 1.4 mm
PdBI 2.8 mm
2.1"1.6"Comparison of Dust Maps at Different Frequencies
SWSED of AB Aur Dust Emission
Structures of the gaseous disk seems to be very different
from those around other Herbig Ae/T Tauri stars.
Several channel maps trace the spiral arms seen
in the Subaru image.
The velocity structures strongly deviate from
simple Kepler rotation.
The upper limit of the Rdust disk ~ 250 AU.
The gas disk was resolved
Rdisk ~ 390 AU, P.A. ~ 79°, inclination ~ 76°
Clear velocity gradient along the major axis.
rotation consistent with Kepler motion.
(Mannings & Sargent 1997)
2.7 mm continuumAB Aur: 2.7 mm Continuum and 13CO (1-0) maps