AMASIS Atmospheric Measurements with Absorption,

1
AMASIS - Atmospheric Measurements with
Absorption, Scattering and Imaging
Spectroscopy E.J. Llewellyn, D.A. Degenstein,
R.L. Gattinger, N.D. Lloyd University of
Saskatchewan, Saskatoon, SK S7N 5E2 I.C. McDade,
B.H. Solheim, C.S. Haley York University,
Toronto, ON M3J 1P3 W.F.J. Evans Trent
University, Peterborough, ON K9J 7B8 W.F. Payne,
G. Barnes, K. Smith, L. Piché, B. Gordon Routes
AstroEngineering Ltd., Kanata, ON K2K 2B1 C.
McLinden MSC, Toronto, ON M3H 5T4 J.P.
Burrows University of Bremen, D-28359 Bremen,
Germany D.P. Murtagh Chalmers University of
Technology, SE-412 96 Göteborg, Sweden J.
Stegman MISU, S-106 91 Stockholm, Sweden C.
Sioris SAO, Harvard University, Cambridge, MA
02138 D.E. Flittner Langley Research Center,
Hampton, VA 23665-3001 William Ward University of
New Brunswick, Fredericton, NB E3B
2
The Idea
- to build on what we have learned with the
OSIRIS Instrument - improve the spatial
resolution - limit the spectral coverage - look
in the nadir
Note this instrument is not the OSIRIS
spectrometer outlined in the STEAM documentation
I have received
3
The Instrument
4
The Primary Goal
- to measure ozone from the ground to 100 km with
very, very high spatial resolution in the
vertical, along track and cross track
dimensions - done by adapting the tomographic
technique that is used with the OSIRIS IRI to
work with spectral information collected by
vertical imagers that measure the Hartley and
Chappuis bands - column amounts will also be
measured by looking in the nadir
5
The Secondary Goal
- to measure ozone related species with very,
very high spatial resolution in both the vertical
and along track dimensions - this will be done
with two spectrographs that will use variations
of the SCHIAMACHY and OSIRIS processing
algorithms - we intend to measure from 310 nm to
495 nm simultaneously in both the nadir and the
limb
6
The Tertiary Goal
- to measure ozone at night using stellar
occultation - this will be done with a
conceptually simple slitless spectrograph (VOLE)
that uses a prism as its dispersive element -
this is intended to be a student run project at
the University of Saskatchewan - I will not
mention this add-on again
7
The Limb Viewer
spectral measurements all made with high vertical
resolution
predominantly low spectral resolution except for
the limb imaging spectrograph
1) Hartley Band Ozone Imager 2) Chappuis Band
Ozone Imager 3) Oxygen Atmospheric Band
Imager 4) Oxygen InfraRed Atmospheric and OH
Meinel Band Imager 5) Limb Imaging Spectrograph
8
The Limb Viewer
- each imager uses a single lens and a
two-dimensional detector array - a mosaic filter
is placed directly in front of the detector -
each part of the mosaic has a different pass
band - each imager measures over the appropriate
range of tangent altitudes with 500 m resolution
9
The Limb Viewer
OSIRIS retrieval techniques will be used
1) Hartley Band Ozone Imager
measures scattered sunlight from 40 to 70 km
along lines of sight that are separated by
approximately 500 m in tangent altitude the
imager measures in five separate passbands at
260, 350, 280, 295 and 319 nm the spectral
resolution of these measurements is not high
10
The Limb Viewer
OSIRIS retrieval techniques will be used
2) Chappuis Band Ozone Imager
measures scattered sunlight from 10 to 40 km
along lines of sight that are separated by
approximately 500 m in tangent altitude the
imager measures from 450 to 730 nm with six
separate passbands the spectral resolution of
these measurements is about 10 nm
11
The Limb Viewer
Extra to OSIRIS
3) Oxygen Atmospheric Band Imager
measures the Oxygen Atmospheric Band Emission
with sub-kilometer resolution the imager measures
over three passbands with spectral resolution of
about 10 nm these measurements will be used for
temperature determination, aerosol and cloud-top
retrievals and to help retrieve ozone with the
Singlet Delta Band Imager
12
The Limb Viewer
OSIRIS retrieval techniques will be used
4) Oxygen InfraRed Atmospheric and OH Meinel
Band Imager
very close to the same measurement set as the
OSIRIS Infrared Imager except that the spatial
resolution will be much better (500 m in the
vertical) these measurements will primarily be
used for ozone retrievals in the mesosphere
13
The Limb Viewer
OSIRIS retrieval techniques will be used but the
increase in spatial resolution is invaluable
4) Limb Imaging Spectrograph
image the limb from 0 to 50 km (?) with sub
kilometer tangent altitude resolution cover the
spectral range from 310 to 495 nm with 0.7 nm
resolution design will be similar to OSIRIS
spectrograph
14
The Limb Viewer
The Data Products ozone from the ground to 100 km
with very high two-dimensional spatial
resolution aerosol optical depth
information cloud distributions NO2 profiles
from 10 to 40 km BrO profiles from 20 to 30
km OClO profiles from 15 to 25 km
15
The Instrument
16
The Nadir Viewer
all of the relevant measurements that are made in
the limb will also be made in the nadir
this will be done to measure column
concentrations of certain species and to monitor
the upwelling radiation to improve the limb
measurement retrievals
1) Nadir Imaging Spectrograph 2) 2-D Ozone Mapper
17
The Nadir Viewer
SCHIAMACHY heritage will be very useful
1) Nadir Imaging Spectrograph
cover the spectral range from 310 to 495 nm with
0.7 nm resolution design will be similar to
OSIRIS spectrograph measures the same species as
the limb looking instrument
18
The Nadir Viewer
Not well defined yet. It may included the TOMS
wavelengths and a scan mirror as well as the
Chappuis wavelengths
2) 2-D Ozone Mapper
measures column ozone densities in a similar
fashion to TOMS will give the upwelling radiation
that the limb retrievals require
19
The Nadir Viewer
The Data Products NO2 vertical column BrO
vertical column OClO vertical column HCHO
vertical column SO2 vertical column Upwelling
radiation to be used for the limb retrievals
20
The Size, Mass, Power and Memory
about 1.5 times the size and mass of OSIRIS with
the additional requirement of long baffling
additional power will be required for the extra
detectors but it is likely that no cooling will
be needed
a study must be done to determine the Mass Memory
requirements we intend to collect far less
spectral information and far more spatial
21
Conclusion
We will need to work on the AMASIS Concept to
make it fit the STEAM Mission This should be
easy as all of the components that are required
by STEAM exist in AMASIS