![]() ![]() Your instructor will assign you a quasar and show you how to open the data in LoggerPro. In this lab, where useful, note that 1 pc / Myr = 1 km / s, where 1 Myr = 1 million years. The quasar data can be opened in LoggerPro, and is found under LabImage → Spectra → SDSS. (Spring 2021, the questions on your worksheet are different)Įach lab group will be responsible for a quasar. An Angstrom is 10 -10 m, one ten-billionth of a meter or one tenth of a nanometer. Use this spectrum to help you identify the emission lines of the spectra of the quasars in your lab questions. Remember that the ordering and relative spacing of of these lines will not change for example, Hα will always be at a longer wavelength than Hβ, and Hγ will be at a longer wavelength than both Hδ and Hε.ĭetermining the Age of the Universe from Spectra of Quasars The redshift of Mrk 1460 is of the order z = 10 -4.) The x-axis of the plot is in Angstroms astronomers sometimes prefer to use this unit for wavelength rather than nanometers. (Mrk 1460 is very close to the Milky Way and therefore does not have a detectable redshift the shift is so small that it can be ignored. A second pair of strong lines (OII, singly ionized) can be found at 372.7 nm and 373.0 nm. Examples of these galaxy features can be seen labeled in the spectrum of the galaxy Mrk 1460 shown below. In the spectra of quasars, a pair of strong lines caused by oxygen molecules that have been doubly ionized (OIII) can be found at 500.7 nm and 495.9 nm. The spectra of most galaxies (including quasars) are dominated in the optical by two types of emission lines: hydrogen lines (the Balmer series) and oxygen lines. Image Analysis with Solar System Objects.Image Analysis II - Animation and Stacking.Image Analysis I - Image Processing and the Ring Nebula.Exploring the Sky II - Star Charts and Stellarium.Hertzsprung-Russell Diagram and Star Clusters.ASTR:1771 - Intro Astronomy I: Basic Astrophysics.ASTR:1080 - Exploration of the Solar System.ASTR:1070 - Stars, Galaxies, and the Universe. ![]()
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