1. Looking for a Color-Luminosity Relationship for AGN July 16, 2012 prepared by Varoujan Gorjian NITARP Scientist

2. An Image of the sky is essentially 2D VG

3. How Can we tell how far things are? VG

4. There is one way to get relative distance Thanks to the Hubble law we can separate based on redshift: VG V=H o D

5. But which clusters are near and which ones are far? Thanks to the Hubble law we can separate based on redshift: VG V=H o D

6. An Image of the sky is essentially 2D VG

7. The equivalent of a volcanic island is an Active Galactic Nucleus (AGN) VG

12. Quasars which are also Active Galactic Nuclei but more Luminous

13. Our model for an Active Galactic Nucleus (AGN) VG

14. Spectrum of AGN Blue Excess (AKA Big Blue Bump) VG

16. 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: VG

17. 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) VG

18. Color Magnitude Diagram VG

19. 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? VG

20. Black Body Radiation VG 20 The hotter something is, it emits more light.

21. 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? VG

22. Color VG Transmission → Wavelength →

23. Color VG 23 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

24. Color VG 24 The hotter something is, it emits more more short wavelength light

25. Color VG 25 So what temperature are these galaxies?

26. Color Magnitude Diagram VG

27. 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. VG

28. Black Body radiation from both the gas and the dust

29. 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 VG

30. Wise-Field Infrared Survey Explorer (WISE) VG