Looking for a Color-Luminosity Relationship for AGN July 16, 2012 prepared by Varoujan Gorjian...
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![Page 1: Looking for a Color-Luminosity Relationship for AGN July 16, 2012 prepared by Varoujan Gorjian NITARP Scientist.](https://reader036.fdocuments.us/reader036/viewer/2022062806/5697c02d1a28abf838cd9a3f/html5/thumbnails/1.jpg)
Looking for a Color-Luminosity Relationship for AGN
July 16, 2012prepared by
Varoujan GorjianNITARP Scientist
![Page 2: Looking for a Color-Luminosity Relationship for AGN July 16, 2012 prepared by Varoujan Gorjian NITARP Scientist.](https://reader036.fdocuments.us/reader036/viewer/2022062806/5697c02d1a28abf838cd9a3f/html5/thumbnails/2.jpg)
An Image of the sky is essentially 2D
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How Can we tell how far things are?
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There is one way to get relative distance
• Thanks to the Hubble law we can separate based on redshift:
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V=HoD
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But which clusters are near andwhich ones are far?
• Thanks to the Hubble law we can separate based on redshift:
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V=HoD
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An Image of the sky is essentially 2D
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![Page 7: Looking for a Color-Luminosity Relationship for AGN July 16, 2012 prepared by Varoujan Gorjian NITARP Scientist.](https://reader036.fdocuments.us/reader036/viewer/2022062806/5697c02d1a28abf838cd9a3f/html5/thumbnails/7.jpg)
The equivalent of a volcanic islandis an Active Galactic Nucleus (AGN)
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Quasars which are also Active Galactic Nuclei but more Luminous
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Our model foran Active Galactic Nucleus (AGN)
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Spectrum of AGNBlue Excess (AKA Big Blue Bump)
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• But how do we figure out how far away quasar is?
• One way is to figure out its inherent luminosity and then compare it to its apparent luminosity because light follows the inverse square law:
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BRIGHTNESS =LUMINOSITY
24×π ×DISTANCE
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• This has been a very successful way of determining the distances to stars
• How do we figure out the luminosity of a star?
• This is the results of the Hertzsprung-Russell Diagram which relates the color of a star to it’s luminosity (also known as absolute magnitude)
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Color Magnitude Diagram
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• Why does this work?
• It’s based on simple physics of hot gasses:– Fusion creates energy at the core of a star
– The energy then heats the outer gas layers of the star
– What does heat have to do with luminosity?
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Black Body Radiation
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The hotter something is, it emits more light.
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• Why does this work?
• It’s based on simple physics of hot gasses:– Fusion creates energy at the core of a star
– The energy then heats the outer layers of the star
– What does heat have to do with luminosity?
– SO THE MORE MASSIVE A STAR IS, IT HAS MORE FUSION AND GENERATES MORE ENERGY AND HEATS UP THE OUTER LAYERS OF A STAR MORE AND SO CREATES A MORE LUMINOUS STAR BECAUSE OF BLACK BODY RADIATION
Now how does that relate to the color of a star?
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Color
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Tra
nsm
issi
on →
Wavelength →
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Color
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This is KPNO R band.Note that it’s not a “Top hat” function, but it’s trying.Note also that none of it is perfectly transparent!
Filter Transmission
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Color
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The hotter something is, it emits more more short wavelength light
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Color
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So what temperature are these galaxies?
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Color Magnitude Diagram
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• So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity– But AGN have no fusion, why would we expect a color-magnitude relation?
– The gas that accretes onto the black hole is still hot and so must follow the Blackbody Radiation law.
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Black Body radiation from both the gas and the dust
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• So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity
– But AGN have no fusion, why would we expect a color-magnitude relation?– The gas that accretes onto the black hole is still hot and so must follow the Blackbody
Radiation law.
• If this is so obvious, why hasn’t it been done before?
• Well it has but to no success
• So why are we trying again?– Possibly not a large enough sample, not enough wavelengths to avoid emission lines,
and AGN are variable
• We have new data covering a much wider wavelength range. Also we will be including longer wavelength infrared than has been used before which should be less sensitive to variability
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Wise-Field Infrared SurveyExplorer (WISE)
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