| discov_num |
notes |
refcode |
| B 719 |
VY CMa. This multiple "star" is involved in nebulosity, shaped like |
|
|
the tail of a comet. All companions may be knots in the nebulosity, |
|
|
and all may seem variable. |
|
|
Adaptive optics imaging by Shenoy et al. (2013) in Ks, L', and M bands |
|
|
suggest the brightness of the "Southwest Clump" (~1.5" from central |
|
|
star) is almost entirely due to scattering from silicate dust grains. |
|
|
Lower mass limit for this feature is 5 x 10^-3 to 2.5 x 10^-2 Msun, |
|
|
depending on assumed gas-to-dust ratio. Presence of clump with no |
|
|
apparent counterpart on other side of star suggests ejection event. |
SDP2013 |
| refcode |
metd |
author |
reference |
| SDP2013 |
A - |
Shenoy, D.P., Jones, T.J., Humphreys, R.M., Marengo, M., Leisenring, J.M., |
2013AJ....146...90S |
| SDP2013 |
|
Nelson, M.J., Wilson, J.C., Skrutskie, M.F., Hinz, P.M., Hoffmann, W.F., |
|
| SDP2013 |
|
Bailey, V., Skemer, A., et al. |
|
| SDP2013 |
|
AJ 146, 90, 2013 |
|
