A Relationship Between Supermassive Black Hole Mass And Spiral Arm Morphology In Disk Galaxies

Details A Relationship Between Supermassive Black Hole Mass And Spiral Arm Morphology In Disk Galaxies A Relationship Between Supermassive Black Hole Mass And Spiral Arm Morphology In Disk Galaxies

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.5203s&link_type=abstract

American Astronomical Society, AAS Meeting #212, #52.03; Bulletin of the American Astronomical Society, Vol. 40, p.248

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Scientific paper

We present a newly discovered relationship between supermassive black hole (SMBH) mass (M) and spiral arm pitch angle (P) in disk galaxies. A possible explanation for this M-P relationship is as follows. The recent discovery of AGN in disk galaxies with little or no bulge, suggests that the bulge mass or bulge dynamical mass (while obviously strongly related to SMBH mass) may not be the main determinant of masses of central compact objects in galaxy centers. Instead, a possible suggestion is that dark matter halo concentration (c) is the main determinant of SMBH mass, although other affects may play a role as well. Indeed, there is evidence that suggests that spiral arm pitch angle may also be determined by the concentration of dark matter, so it is no surprise that a relationship exists between M and P. This relation may be very important, since regular spiral structure can be seen in galaxies out to z𕙙.3. At these redshifts it is almost impossible to determine SMBH masses using current methods. However, the existence of the M-P relation gives us a new diagnostic tool to determine SMBH mass evolution in disk galaxies as a function of look-back time, assuming the M-P relation does not evolve .
This research is supported by the Arkansas NASA EPSCoR program.

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