the hunter, is one of the most famous constellations. Its declination
is such that it is visible from most of the civilized world. In addition,
most of the stars of Orion are very bright and interesting. Originally
this Project was called the Betelgeuse Campaign. Because Campaigns usually
have a defined end and this is an on going Project and also now includes
three more stars of Orion, the name was changed to the Orion Project.
This is a developing Project and comments and suggestions are welcome.
We all have something to learn and contribute.
To provide a focal point for discussions a Orion Project
Forum was created. To join the Forum please use the following email address
is not a Citizen Science type project. Observers must be willing to
use the proper equipment and develop the necessary skills to produce
quality data. This Project presents an opportunity to both learn photometry
and/or spectroscopy or sharpen your skills while contributing valuable
data. This is Discovery Science and an on going Project.
(alpha Orionis) is one of the brightest stars in Orion and the
eighth brightest star in the sky and sometimes even brighter than Rigel
(beta Orionis), the lower right star of Orion). Betelgeuse is
the big bright reddish orange star in the upper left of the constellation.
Betelgeuse and Rigel as well as the right most star in Orion's belt
Mintaka (delta Orionis) along with the middle star in
Orion's belt, Alnilam (epsilon Orionis) and the left most
star Alnitak (zeta Orionis) have been designated as stars
of interest for photometry and spectroscopy. Observers are encouraged
to take photometric and/or spectroscopic data on one or more of these
stars and report the results to the Project.
are two main objectives.
first objective is to help the observer produce quality photometric and
spectroscopic data. Since these stars are bright and easy to find, many
will think they are easy to observe. For photometry they present a large
challenge because they are bright. Doing photometry on these stars will
require special techniques and care. For spectroscopy, these are actually
easier stars to work with because they are bright. Short exposures will
allow easy experimentation to develop good techniques and obtain good
spectra. This project is an excellent means to learn more about photometry
second objective is to produce archival quality photometric and spectroscopic
data as indicated below.
SSP-3 BVRI(Primarily BV)
CCD BVRI (Primarily BV)
Photon Counting UBV
the SSP-3 and CCD the BV filters should be sufficient as the RI can be
a problem with the transformation.
DSLR can be used, it is not recommended as the dynamic range is low
and only the V band can be used. An inexpensive monochrome camera
lens coupled with a 50 mm camera lines and BV filters is ideal.
Mid and Low-Resolution Spectroscopy
Lhires III (2400 l/mm grating)
of these stars produce emission lines that randomly pop up. Low-resolution
spectroscopy may find those and alert others to investigate with high-resolution
spectroscopy. Low-resolution work is encouraged and can prove valuable.
seems every so often professionals start a Campaign on one or more of
these stars. Many times small observatories only hear of the Campaign
when it is over or just starting giving little time if any to prepare.
Because of this, the basic purpose of this Project is to continue photometric
and spectroscopic observations of these stars. This will provide continuous
observational data for the stars.
To help beginners do photometry and spectroscopy and get to the
point where good data is submitted that can be scientifically useful.
The means transformed and extinction corrected photometric data
that is consistent and close to what others are producing for the
same time. For spectroscopy beginners will be mentored to the point
of being able to submit high-quality wavelength calibrated line
2. Data will be archived and available to anyone. For spectroscopy.
A showcase of wavelength calibrated spectral line profiles in .Jpg format
will be shown. Corresponding line profile .Dat files will be archived.
Photometric data will be archived and periodically submitted to the
and continuous observations producing high-quality photometric and spectroscopy
data of the program stars.
web site will be developed and devoted to the project. The Hopkins
Phoenix Observatory will maintain the site.
data will be listed on the web site as well as archived with the AAVSO.
Wavelength-calibrated spectroscopic line profiles will be showcased
on the site and .Dat files of the profiles and raw image fits files
will be archived on the web site.
and suggestions are most welcome.
To join the
Project and for more information, comments or questions, please
send an email to Jeff Hopkins at
the Photometry Pages for magnitude plots
in the September issue of Sky & Telescope in the Letters
section on page 8.