Epsilon Indi Ba, Bb: the closest known binary brown dwarf system.
I am currently compiling a comprehensive study of these two
brown dwarfs with VRIzJHKLM photometry and 0.6-5.1 micron spectroscopy of BOTH sources.
Combined with an ongoing astrometric monitoring campaign to determine the total system
mass AND individual dynamical masses, we are in a position where the spectra of the two
components of eps Indi B can be used to calibrate model atmospheres of T dwarfs.
In addition to the soon to be determined model-indpendent masses, we have avery accurate
distance of 3.626 pc from the HIPPARCOS mission, and we have an age range of 0.8-2.0 Gyr
from previous studies of epsilon Indi A, the ~1400AU distant primary of this tertiary
system.
VLT and Chandra study of High Mass Star Formation Regions(HMSFRs)
I am also undertaking a spectroscopic study of high-mass star formation regions within
our galaxy. The primary aim is to determine the form of the initial mass function in each
of our target clusters and to compare these different environments and ages. This will be
done by employing the Chandra data of our Penn. State collaborators to select definite cluster
members for the follow-up multi-object spectroscopy which will lead to the mass determinations.
Our first targets are NGC2244 in the Rosette Nebula and Trumpler 14 in Carina. These will
be followed with observations of NGC6357 in Sagittarius and NGC6618 in M17.
This file contains the theoretical wavelength and measured intensity of
the OH Meinel bands in the region 1.154 - 4.837 microns. These are
useful for wavelength calibration of NIR spectra as they are observed
at the same time as your object(s) of interest and give relatively
good wavelength coverage.
These data are taken from
Abrams
et al. 1994, ApJS, 93, 351, dug out by
James Graham.
