Knowledge Base

1. Need Active galactic nuclei play an enormous role in studies of the early universe (Gorjian, 2009). ABSTRACT Ground Based and Hubble Space Telescope images of the Active Galaxy NGC 4261 . Knowledge Base Active Galactic Nuclei Data Sources • AGN are the center of enormous galaxies emitting huge quantities of energy generated by material flowing into a black hole at the center, which expels the matter at its poles (O’Dowd, 2002). • AGN are the most luminous persistent sources of electromagnetic radiation in the universe. • Goldstone Apple Valley Radio Telescope (GAVRT) is a radio telescope located at the Goldstone Deep Space Communications Complex. • Radio data in 8.5 GHz (X-band), and 2.3 GHz (S-band) of AGN were downloaded from GAVRT’s DSS12 radio antenna. http://www.nasa.gov/centers/jpl/images/content/160106main_gavrt-sunrise-browse.jpg • The Spitzer Space Telescope is an infrared space observatory. • Spitzer images of AGN in 3.6 microns, 4.5 microns, 5.8 microns, 8.0 microns were used. http://www.nasa.gov/centers/jpl/images/content/160106main_gavrt-sunrise-browse.jpg http://whyfiles.org/223orbital_astro/images/spitzer.jpg Literature Review • Lacy, 2001 • It was demonstrated that the ratio of nuclear luminosity to Eddingtons luminosity was strongly inversely correlated. • j Project Goals The goal is to use both measurements of infrared and radio emissions from active galaxies as well as estimates of the black hole masses of these galaxies to determine correlations between electromagnetic emission and black hole mass.

2. Methodology Active Galactic Nuclei N:13 Spitzer IRAC data: 3.8µm, 4.5µm, 5.8µm and 8.0µm Goldstone DSS12 Radio Telescope data in 2.3 GHz (S-band) and 8.5 GHz (X-band) Average Flux was calibrated in Jansky’s (Jy) Fluxes calculated using APT (Aperture Photometry Tool) Ratio between infrared flux densities and radio flux densities determined (ie. 3.8µm/S) Pearson function was used to look for correlation Results The x-axis shows the Black holes mass while the y-axis show 3.6 µm/S-band. The correlation coefficient of this graph was -0.0195734906115743. The x-axis shows the Black holes mass while the y-axis show 4.5 µm/S-band. The correlation coefficient of this graph was -0.101398440165269. The x-axis shows the Black holes mass while the y-axis show 5.8 µm/S-band. The correlation coefficient of this graph was -0.138994116981481. The x-axis shows the Black holes mass while the y-axis show 8.0 µm/S-band. The correlation coefficient of this graph was -0.0455096260989072. The x-axis shows the Black holes mass while the y-axis show 3.6 µm/X-band. The correlation coefficient of this graph was -0.0454110336062208. The x-axis shows the Black holes mass while the y-axis show 4.5 µm/X-band. The correlation coefficient of this graph was -0.11405615836447. The x-axis shows the Black holes mass while the y-axis show 8.0 µm/X-band. The correlation coefficient of this graph was -0.0413868073231374. The x-axis shows the Black holes mass while the y-axis show 5.8 µm/X-band. The correlation coefficient of this graph was -0.142398916192913.

3. Discussion Custer Picture Spitzer Tool Picture Conclusion • PEARSON function a correlation with an R-value of -0.081091074 was found. • There is no correlation between black hole mass (kg) and it infrared/radio emissions. Future Studies • More Active Galactic nuclei will be used. • Another wavelength of in the electromagnetic spectrum will be used. http://chandra.harvard.edu/photo/2001/0157blue/0157blue_xray.jpg This Chandra image of Cen A shows a bright central source: the Active Galactic Nucleus (AGN) suspected of harboring a supermassive black hole. Bibliography Alonso-Herrero, Almudena, The Relation between Mid-Infrared Emission and Black Hole Mass in Active Galactic Nuclei: A Direct Way to Probe Black Hole Growth?, The Astrophysical Journal, Volume 571, Issue 1, pp. L1-L5, c) 2002: The American Astronomical Society, 05/2002 Fabian, A. C.; M. J. Rees (1995). "The accretion luminosity of a massive black hole in an elliptical galaxy". Monthly Notices of the Royal Astronomical Society 277 (2): L55–L58. Ho Luis, On the Relationship between Radio Emission and Black Hole Mass in Galactic Nuclei, The Astrophysical Journal, Volume 564, 01/2002, pp. 120-132 Laor, Ari, On Black Holes Masses and Radio Loudness in Active Galactic Nuclei, The Astrophysical Journal, Volume 543, Issue 2, p. L111-L114, 11/2000  LYNDEN-BELL, D. (1969). "Galactic Nuclei as Collapsed Old Quasars". Nature 223 (5207): 690–694.  Marconi, A.; L. K. Hunt (2003). "The Relation between Black Hole Mass, Bulge Mass, and Near-Infrared Luminosity". The Astrophysical Journal 589 (1): L21–L24. McLure, Ross J. et. al., The relationship between radio luminosity and black hole mass in optically selected quasars, Monthly Notices of the Royal Astronomical Society, Volume 353, Issue 4, 10/2004 L45-L49 Narayan, R.; I. Yi (1994). "Advection-Dominated Accretion: A Self-Similar Solution". Journal reference: Astrophys. J 428: L13. Nelson, Charles H., Black Hole Mass, Velocity Dispersion, and the Radio Source in Active Galactic Nuclei, The Astrophysical Journal, Volume 544, Issue 2, pp. L91-L94 12/2000  O’Dowd,Matthew et. al., The Host Galaxies of Radio-loud Active Galactic Nuclei: The Black Hole- Galaxy Connection, The Astrophysical Journal, Volume 580, Issue 1, 11/2002, pp. 96-103 Panessa, F Multi- wavelength and Black Hole Mass Properties of Low Luminosity Active Nuclei, publication- THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. AIP Conference Proceedings, Vol. 924, pp. 830-835 (2007)  Pott, Jorg- Uwe, Astrophysical phenomena related to supermassive black holes, PhD Thesis, Universitat Koln, 142 pages  Vermeulen, R. C.; P. M. Ogle, H. D. Tran, I. W. A. Browne, M. H. Cohen, A. C. S. Readhead, G. B. Taylor, R. W. Goodrich (1995). "When Is BL Lac Not a BL Lac?". The Astrophysical Journal Letters 452 Zhang , Xue-Guang et Al., On the Correlation between Radio Properties and Black Hole Mass of Quasars, Chin J. Astron. Astrophys. Vol. 3 (2003), No. 3, 212-224