1. Astrochemistry basics How we detect elements and molecular compounds in space Begin Background photograph - NASA - http://hubblesite.org/gallery/album/galaxy_collection/pr1999041a/ Background photograph - NASA - http://hubblesite.org/gallery/album/galaxy_collection/pr1999041a/http://hubblesite.org/gallery/album/galaxy_collection/pr1999041a/

2. Whoa!! I don’t understand the term Astrochemistry??? Astrochemistry is the (relatively) new branch of Astronomy that deals with how/where elements and compounds come from that are found in: Astrochemistry is the (relatively) new branch of Astronomy that deals with how/where elements and compounds come from that are found in: The Milky Way (our very own Galaxy) learn moreThe Milky Way (our very own Galaxy) learn morelearn morelearn more Nebulae (clouds of gas within our galaxy) learn moreNebulae (clouds of gas within our galaxy) learn morelearn morelearn more Other galaxies learn moreOther galaxies learn morelearn morelearn more Any other place in the universe INCLUDING our Solar SystemAny other place in the universe INCLUDING our Solar System

3. Some useful concepts Spectral lines Spectral lines Absorption / Emission lines Absorption / Emission lines Radio Telescopes Radio Telescopes Detection

4. We detect these chemicals in space by at least two methods: Atomic Spectroscopy – Useful for Visible, Infrared, and Ultraviolet Light Atomic Spectroscopy – Useful for Visible, Infrared, and Ultraviolet Light Atomic Spectroscopy Atomic Spectroscopy Molecular Spectroscopy – Useful for Radio Waves, and Microwaves (type of Radio Wave), Molecular Spectroscopy – Useful for Radio Waves, and Microwaves (type of Radio Wave), Molecular Spectroscopy Molecular Spectroscopy

5. Atomic Spectroscopy Atoms of a specific element emit a specific wavelength of light when an electron undergoes a transition between energy levels (Bohr model of the Atom) Atoms of a specific element emit a specific wavelength of light when an electron undergoes a transition between energy levels (Bohr model of the Atom)

6. Molecular Spectroscopy Molecules of a compound have rotation energy. When they change rotation energy states, they emit a photon at a specific wavelength (λ). Molecules of a compound have rotation energy. When they change rotation energy states, they emit a photon at a specific wavelength (λ). Different molecules emit photons of unique wavelengths for that rotation energy state. Different molecules emit photons of unique wavelengths for that rotation energy state. Diatomic molecule rotation Diatomic molecule rotation

7. Absorption / Emission lines Electrons making an energy transition is the key to either emission of light or radio waves. Electrons making an energy transition is the key to either emission of light or radio waves. Absorption is the process where energy is taken in by an electron to change it’s energy level to a “non-rest” state. Absorption is the process where energy is taken in by an electron to change it’s energy level to a “non-rest” state. Absorption Emission is the process where energy is given off by the electron as it returns to its “rest” state. Emission is the process where energy is given off by the electron as it returns to its “rest” state. Emission

8. Absorption Spectra Happens when waves of an electromagnetic wave (shown in visible light) passes through a cool gas. The gas “robs ” (absorbs) photons at specific wavelengths to energize its electrons. Happens when waves of an electromagnetic wave (shown in visible light) passes through a cool gas. The gas “robs ” (absorbs) photons at specific wavelengths to energize its electrons. Result – Specific wavelengths “drop out” of the otherwise continuous spectrum. Result – Specific wavelengths “drop out” of the otherwise continuous spectrum.

9. Absorption Spectra Examples: The absorption of these specific wavelengths of light prove the presence of Hydrogen gas in the outer atmosphere of the star. The absorption of these specific wavelengths of light prove the presence of Hydrogen gas in the outer atmosphere of the star.

10. Absorption Spectra Examples: Yup, another example… Psst!, This is how we identify Spectral types!!! Psst!, This is how we identify Spectral types!!!

11. Emission Spectra Happens when photons are created by an energized gas. The gas “creates ” (emits) photons at wavelengths corresponding to the energy change of its electrons. Happens when photons are created by an energized gas. The gas “creates ” (emits) photons at wavelengths corresponding to the energy change of its electrons. Result – Specific wavelengths of light are created where there was no light before. Result – Specific wavelengths of light are created where there was no light before. Emission lines of specific gasses

12. Tools of the Radio Astronomer Radio Telescopes – Similar in many ways to Optical telescopes Radio Telescopes – Similar in many ways to Optical telescopes Focus configurations: Focus configurations: A. Prime Focus – radio receiver at the prime focusA. Prime Focus – radio receiver at the prime focus B. Cassegrain – secondary convex reflector at prime focusB. Cassegrain – secondary convex reflector at prime focus How do you make a radio telescope (almost) the size of the Earth?? How do you make a radio telescope (almost) the size of the Earth?? Ans: VLBAAns: VLBA

13. Very Long Baseline Array What is a VLBA?? What is a VLBA?? Answer: a Very Long Baseline Array – Answer: a Very Long Baseline Array – A grouping of identical radio telescopes at different places on the earth that act as one large radio telescope Combining the signals from more than one telescope is called interferometry. (learn more) Combining the signals from more than one telescope is called interferometry. (learn more)learn morelearn more

14. Telescopes of the VLBA The National Science Foundation's VLBA (learn more) is a system of ten identical radio-telescopes controlled from a common headquarters in New Mexico, and working together as a single instrument. The radio signals received by each individual antenna contribute part of the information used to produce images of celestial objects with hundreds of times more detail than Hubble Space Telescope images. The National Science Foundation's VLBA (learn more) is a system of ten identical radio-telescopes controlled from a common headquarters in New Mexico, and working together as a single instrument. The radio signals received by each individual antenna contribute part of the information used to produce images of celestial objects with hundreds of times more detail than Hubble Space Telescope images.learn morelearn more

15. Telescopes of the Very Long Baseline Array (VLBA) NRAO / AUI / NSF NRAO / AUI / NSF

16. Radio Telescopes How big is the world’s largest Radio Telescope, and where is it? How big is the world’s largest Radio Telescope, and where is it?largest Radio Telescopelargest Radio Telescope NRAO / AUI / NSF How Big: > 100 m (> 300 ft.) Where: Green Bank, West Virginia

17. Beginnings In the ‘50s & ’60s, Radio telescopes first discovered the “signature” line of Hydrogen at 21 cm wavelength between stars. In the ‘50s & ’60s, Radio telescopes first discovered the “signature” line of Hydrogen at 21 cm wavelength between stars. The hydrogen gas was found (in abundance) in the “empty” space between stars.The hydrogen gas was found (in abundance) in the “empty” space between stars. Note: Domestic microwave ovens use a signal ofNote: Domestic microwave ovens use a signal of ~ 12 cm wavelength to cook food ~ 12 cm wavelength to cook food This gas was “dark” in optical wavelengths but “bright” in radio wavelengths. This gas was “dark” in optical wavelengths but “bright” in radio wavelengths.

18. Keeping score What molecules have been discovered and at which wavelengths? What molecules have been discovered and at which wavelengths? Ans: Well over 100 molecules of compounds have been found in Interstellar space. Here are just a few of them showing where they were discovered and at the corresponding “signature” frequencies and wavelengths Here are just a few of them showing where they were discovered and at the corresponding “signature” frequencies and wavelengths

19. Familiar Compounds in Space Name (Popular Name) Formula (Chemical formula) Wavelength ( λ - in cm) Frequency(MHz) Found In: Suphur Monoxide SO8.2836202Orion Methanol CH 3 OH 8.2936169Sagittarius Formaldehyde H 2 C 18 O 6.834388Sagittarius Carbon Oxide Sulfide OCS8.2236488Taurus Silicon Monoxide SiO7.0542519Sagittarius (Var. Supergiant) Silicon Tetracarbide Silicon Tetracarbide SiC 4 6.9842944 Taurus Taurus Ammonia NH 3 16.6518017 Giant Molecular Cloud

20. How can we find Molecules with a Radio Telescope Check out this website. It relates many compounds found in the universe and at which frequency they are detected. Check out this website. It relates many compounds found in the universe and at which frequency they are detected. http://physics.nist.gov/cgi-bin/micro/table5/start.pl Hints: Start the frequency range at about 1200 Hz. You can type in the upper frequency range at about 44,000 Hz.Start the frequency range at about 1200 Hz. You can type in the upper frequency range at about 44,000 Hz. Check the “Name” field at the bottom. This will add the familiar chemical formula name to the table which the web site creates for you.Check the “Name” field at the bottom. This will add the familiar chemical formula name to the table which the web site creates for you.