Spectroscopy Lab Report

The purpose of this experiment is to determine the maximum absorbance of fast green, and the chlorophylls, also in the case of fast green create a concentration curve to determine an unknown substance. Each test will use the spectrophotometer.

We can determine an object’s temperature from its thermal (or “blackbody”) spectrum by finding the wavelength at which it emits the most electromagnetic radiation.

2- It is impossible to identify all element with the naked eye because they don’t release enough energy, therefore the color is not as visible. Besides, not all elements give a light that it is in the visible part of the spectrum, so we need to use a prism.

Once a light beam shines through the flame, the atoms absorb some of the light. It is then detected, recorded and compared to a series of standard solutions. In the absorption spectrum, the absorbed light show up as black gaps. These distinctive gaps indicate the difference in energy levels for a particular element. If this can be compared to the concentration of its standard solution, then it can form a calibration curve.

The purpose of this experiment was to test and observe the physical and chemical properties of gases, and to use these properties to identify these gases when they are encountered.

In the effect of light wavelength experiment, the action spectrum is used to demonstrate the effectiveness of various wavelengths of light on photosynthesis. To observe these effects of the wavelengths the wavelength pigments red, blue, green, white light, and no light are used. In the experiment, spinach leave disks were aspirated in a sodium bicarbonate solution in order to remove all internal gases and make the disks sink to the bottom of a beaker. Each beaker full of 10 spinach disks was placed into a different box with a different colored light source.

Ozone Monitoring Instrument, or OMI, is a mission formed in coalition with the Netherland’s Agency for Agency for Aerospace Programs, or NIVR, and Finnish Meteorological Institute, FMI to help with the EOS Aura mission. It will aid in recording total ozone measurements and other fields related to this topic. The instruments employed on OMI consist of hyperspectral imaging in a push-broom mode to observe the solar backscatter radiation. This hyperspectral component greatly strengthens the accuracy and precision of the ozone data collected. It also allows for pinpoint radiometric and wavelength auto-calibration over the mission timeline. The Earth, as a whole, will be viewed using 740 wavelength bands with a swath that is large enough to gain full coverage in 14 orbits, or one day (Dunbar, 2005).

163 absorption between 700 and 750 nm from each spectrum [40]. The exponential decay of the absorption

Scientist measure the wavelengths and frequencies, from weakest to strongest radio waves have the longest wavelength and frequency and gamma rays have the shortest wavelengths and frequency, and so on for the types of light in between

The data from this experiment has the relationship , and by using the slope, the wavelength of the laser’s light can be calculated. The wavelength of the red laser pointer should be between 620nm and 670nm, and if the experimental value is within this range then the data can be assumed to be accurate.

The Lyman Alpha Photometer consist of an ultra violet detector which has a pure molecular gas filled hydrogen and deuterium cells weighing about 1.5kgs. The LAP would be normally operated in the range of 3000 km before and after Mars perimeter. It measures the proportion of deuterium and hydrogen from Lyman-alpha emissions. Its main function is study the Mars

Fig. 4. (a) The phase parameter (Δ) and (b) shift parameters given by variable angle spectroscopic ellipsometer and the corresponding fitted model are shown. An example of the refractive index and extinction coefficient are illustrated in (c).

The field synthesis is only completed by sampling the synthesized transients. For that we have opted “Attosecond streaking” technique3,4 for sampling the synthesized transients, which gives an access to the field of the synthesized waveform. For this sampling technique, the generation of isolated EUV attosecond pulse is essential. The sampling takes place at the focus of these transients where the planned experiment takes place in order to attain high intensities. The isolated EUV attosecond pulse is generated by focusing (f~ -35 cm) the light transients generated at the exit of the synthesizer apparatus into a quasi-static gas cell, a thin nickel tube (~2mm inner diameter), filled with neon gas and kept at a

The data obtained from PTF and PESSTO is a combination of flux and wavelength values, with wavelength range typically between 3000 and 9000Å. The flux values had to be de-reddened to account for absorption and scattering of the electromagnetic radiation from the SNe, due to dust and gas present in the interstellar medium and the Earth’s atmosphere. To do this a reddening

13.5984 2 4.0026 Helium He -272 -269 0.18 1895 18 1s2 24.5874 3 6.941 Lithium Li 180 1347 0.53 1817 1 [He] 2s1 5.3917 4 9.0122