The secular evolution of M83 central bulge

Details The secular evolution of M83 central bulge The secular evolution of M83 central bulge

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..245..297d&link_type=abstract

Formation and Evolution of Galaxy Bulges, Proceedings of the International Astronomical Union, IAU Symposium, Volume 245, p. 297

Physics

1

Galaxies: Individual (M83), Galaxies: Kinematics And Dynamics, Black Hole Physics

Scientific paper

The luminosity profile of M 83 bulge can be traced by a de Vaucouleurs' law between ≈ 200 pc and ≈ 800 pc. The inner part can be fitted by a n = -1/2 Sérsic profile. Also the IR (J - K) color shows difference between the periphery and the central part of the bulge, both properties indicating the presence of a pseudobulge. Previous Gemini-S 3-D, Paβ spectroscopy of the central ≈ 5″×13″ revealed spider like diagrams indicating disk like motion around three extended masses identified respectively with the optical nucleus (ON), with the center of the bulge isophotes, similar to the CO kinematical center (KC), and with a condensation hidden at optical wavelengths (HN), coincident with the largest lobe in 10 μm emission, most probably a cannibalized satellite. Numerical simulations show that they suffer strong evaporation and they would merge engulfing also the star forming arc in few hundred Myr, increasing the mass at the kinematical center by a factor o five or more. Upper mass limit of putative Black Holes associated to ON, KC and HN are a few ten thousand to a million solar masses. GMOS+Gemini imaging and spectroscopy of a chain of radio sources has yield no optical high redshift counterparts. This radio sources are aligned with ON, neither associated to SN nor to HII regions and might point to an older similar phenomenon, which left behind a kick-off spur.

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