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PYTHON FOR ASTRONOMY | HOW TO READ ASTRONOMICAL SPECTRA FITS FILE| SDSS| #python #sdss
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Astronomical spectra are representations of the electromagnetic radiation emitted, absorbed, or scattered by celestial objects. They provide valuable information about those objects' composition, temperature, density, motion, and physical properties. There are several types of astronomical spectra:
Chapter TimeStamps
00:00:00 Introduction To Astronomical Spectra
00:01:20 Import Libraries
00:02:24 Read FITS Spectra File, File Information & Header
00:06:00 Extracr Data: Flux, Wavelength, Redshift
00:07:40 Plot & Visual FITS Spectra In Moving Frame
00:13:00 Interactive Spectrum
00:15:10 Spectra in REST Frame
Continuous Spectra: These spectra show a continuous range of wavelengths without any breaks or gaps. They are produced by hot, dense objects like stars, which emit radiation across a broad range of wavelengths.
Emission Spectra: Emission spectra are produced when atoms or molecules in a hot, low-density gas emit radiation at specific wavelengths characteristic of the elements or compounds present. These spectra appear as bright lines against a dark background and are often observed in nebulae and the outer atmospheres of stars.
Absorption Spectra: Absorption spectra are formed when a continuous spectrum passes through a cooler, low-density gas. Atoms or molecules in the gas absorb specific wavelengths of light, creating dark lines or bands in the spectrum. These lines correspond to the wavelengths of light absorbed by the atoms or molecules in the gas. Absorption spectra are useful for identifying the chemical composition of stars and interstellar matter.
Atomic Absorption Spectra: Atomic absorption spectra result from transitions of electrons within atoms. They typically appear as sharp lines corresponding to specific energy transitions within the atom.
Molecular Absorption Spectra: Molecular absorption spectra arise from transitions of energy levels within molecules. They can be more complex than atomic spectra, with multiple lines and bands corresponding to different molecular transitions.
Stellar Spectra: Stellar spectra are a combination of absorption and emission spectra, providing information about the composition and temperature of stars. They are typically classified into spectral types based on the presence and intensity of absorption lines, with the OBAFGKM sequence being the most commonly used classification scheme.
Astronomers use spectroscopy to study objects ranging from individual stars and galaxies to the universe's large-scale structure. By analyzing the spectra of celestial objects, scientists can uncover fundamental properties such as chemical composition, temperature, density, velocity, and even the presence of magnetic fields. Spectroscopy is thus a powerful tool in modern astronomy, enabling researchers to unlock the mysteries of the cosmos.
Astronomical spectra are representations of the electromagnetic radiation emitted, absorbed, or scattered by celestial objects. They provide valuable information about those objects' composition, temperature, density, motion, and physical properties. There are several types of astronomical spectra:
Chapter TimeStamps
00:00:00 Introduction To Astronomical Spectra
00:01:20 Import Libraries
00:02:24 Read FITS Spectra File, File Information & Header
00:06:00 Extracr Data: Flux, Wavelength, Redshift
00:07:40 Plot & Visual FITS Spectra In Moving Frame
00:13:00 Interactive Spectrum
00:15:10 Spectra in REST Frame
Continuous Spectra: These spectra show a continuous range of wavelengths without any breaks or gaps. They are produced by hot, dense objects like stars, which emit radiation across a broad range of wavelengths.
Emission Spectra: Emission spectra are produced when atoms or molecules in a hot, low-density gas emit radiation at specific wavelengths characteristic of the elements or compounds present. These spectra appear as bright lines against a dark background and are often observed in nebulae and the outer atmospheres of stars.
Absorption Spectra: Absorption spectra are formed when a continuous spectrum passes through a cooler, low-density gas. Atoms or molecules in the gas absorb specific wavelengths of light, creating dark lines or bands in the spectrum. These lines correspond to the wavelengths of light absorbed by the atoms or molecules in the gas. Absorption spectra are useful for identifying the chemical composition of stars and interstellar matter.
Atomic Absorption Spectra: Atomic absorption spectra result from transitions of electrons within atoms. They typically appear as sharp lines corresponding to specific energy transitions within the atom.
Molecular Absorption Spectra: Molecular absorption spectra arise from transitions of energy levels within molecules. They can be more complex than atomic spectra, with multiple lines and bands corresponding to different molecular transitions.
Stellar Spectra: Stellar spectra are a combination of absorption and emission spectra, providing information about the composition and temperature of stars. They are typically classified into spectral types based on the presence and intensity of absorption lines, with the OBAFGKM sequence being the most commonly used classification scheme.
Astronomers use spectroscopy to study objects ranging from individual stars and galaxies to the universe's large-scale structure. By analyzing the spectra of celestial objects, scientists can uncover fundamental properties such as chemical composition, temperature, density, velocity, and even the presence of magnetic fields. Spectroscopy is thus a powerful tool in modern astronomy, enabling researchers to unlock the mysteries of the cosmos.
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