Introduction.
When
I look through the web and search for "amateur spectroscopy", I
usually find a lot of material about astronomical spectroscopy: how to
build spectrographs and couple them to telescopes, interesting results about star and
nebulae spectra but relatively few about mineralogical spectroscopy
except perhaps fluorescence spectroscopy and of course professional or
academic work. In particular I have not found anything about
amateur Raman spectroscopy but I could have missed something.
I have already shown in other web pages
of this site the possibility for amateur microscopist to come into the
field of minerals spectroscopy, in particular the transmission
spectroscopy of rock sections in the visible and NIR . Although this kind of
technique allows to make interesting studies of minerals, it has some
drawbacks to help for the identification of minerals in rock
sections. First of all, it requires the preparation of a thin or thick
section depending on the mineral to be studied or identified. The reason
is that the extinction coefficient will vary greatly from a
mineral to the next. For instance we can consider the olivine series:
the absorption spectrum in the NIR around 1200 nm of such a
material is due to the presence of iron in the crystal
structure. The Iron concentration is low in forsterite and high in
fayalite so such is the absorption spectrum: forsterite requires a
rather thick section to get a good signal to noise ratio, fayalite a
thin section to avoid the saturation of the spectrum. Another example is
gypsum: to get my
spectra in the near infrared, I needed a 1 mm thick section. For some
other minerals like high iron content orthopyroxenes, the standard 30µ
thickness is enough. A second problem is of course the impossibility to
measure a spectrum of opaque mineral although the reflection coefficient
method could be used for an identification purpose. Finally, some
minerals have no absorption at all in the wavelength range considered. With those possibilities and
limitations in mind, I decided to consider the transformation of
my microscope and the construction of a Raman instrument. The goal was
to identify small crystal particles in a section of rock. By
section, I mean a roughly polished section, one face, in order to
minimize sample preparation. I began my work with an old helium neon
laser I had recovered from an old out of work granulometer instrument so
all the work described in these pages was done with the 632.8 nm He-Ne
line which is not the most common wavelength used in Raman spectroscopy.
This project was a little bit challenging because it is well known that
the Raman effect is very weak so efforts have been made to keep the
sensitivity of the system has high as possible. Moreover, to reduce the
cost, I used parts that were already available to me even if better
choice could be made buying new ones. It is especially true for the
spectrograph. Probably in the future I'll try to improve the system by
redesigning some of the parts.
The design drawing
of the first version of my Raman microscope is the following: |
Description:
the light coming out of the laser
(1) pass through a narrow band pass
filter (2) centered on the laser
wavelength to isolate the 632.8 nm line and thus to avoid that weak
emission lines from the laser at other wavelengths can reach the
detector. Remember that the Raman effect is very weak so the acquisition
time will be sufficiently large to detect any parasitic
emission lines. The laser light pass then through a modified spatial
filter (3) made up of 2 short focal
length objectives. In professional designs there is also a pinhole in
the spatial filter because commercial equipments use confocal
microscopy. Due to mechanical difficulties and in order to get as much
light as possible, I removed the pinhole from the system. The
disadvantage of this removal is a worse spatial resolution in the image
plane of the microscope in the z direction parallel to the optic axis of
the microscope lens (5). The
distance between both objectives (3)
can be adjusted by a micrometric screw to finely change the width of
the beam. This allows to fully cover the entrance pupil of the
microscope objective (5) with the
laser beam in order to get a fine laser spot on the sample
(6). The light pass then through an
important element of the Raman microscope: the beam splitter
(7). The model used is a dichroic
beam splitter. When this device is placed at 45° in a light beam, it
reflects the light towards the microscope objective lens
(5) at the laser wavelength while the
light at higher wavelengths ( in fact a few nanometers above the laser
line ) can pass through the filter. So the majority of the laser
incident light can reach the sample while the Raman light moving upwards
after interaction with the sample (6)
can pass through the beam splitter without being deflected and
thus continue its way to the spectrograph. A polarizer
(4) can been inserted into the light
beam to reduce the intensity of the laser in order to examine safely the
laser spot in the microscope field of view to help focusing the beam and
to choose the region of interest on the sample. The helium neon laser
used here is a polarized model. Above the beam splitter, an edge filter
(8) removes the 632.8nm laser light.
Only the Raman light 3 nm above the laser wavelength and over can
pass through the filter. The absorbance at the laser wavelength is
around 6. The Raman light is reflected by a mirror
(10) and refocused (18)
onto the entrance slit of the spectrograph
(11). The flip mirror (10)
can been removed from the path of the main beam so that the neon light,
used as a reference to calibrate the wavelength range of the
spectrograph, can be fed into the entrance slit. The spectrograph is a
modified Jobin Yvon H20 monochromator equipped with a concave
holographic grating (12) and two
plane mirrors (13). The exit slit of
this monochromator has been removed and replaced by a large window in
order to give access to the whole spectrum. The image of the
spectrum is focused by a camera lens (15)
onto the CCD detector of an astronomical camera
(16). Two bellows are used (14),
one to prevent spurious light to reach the detector and the second one
to allow the movement of the objective lens and thus to change the
magnification of the spectrum image or rather, in our case, the
demagnification to increase the light intensity on the detector and
adjust the spectral range to an acceptable value.
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