The black hole versus bulge mass relationship in spiral galaxies

Details The black hole versus bulge mass relationship in spiral galaxies The black hole versus bulge mass relationship in spiral galaxies

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8228a&link_type=abstract

HST Proposal ID #8228

Computer Science

Hst Proposal Id #8228 Galaxy Structure And Dynamics

Scientific paper

We will obtain long-slit spectroscopic observations with STIS of the ionized disk gas in a volume limited sample of 54 nearby spirals, for which we already have ground based emission line rotation curves, CCD surface photometry and radio maps. For each galaxy we will use the G750M grating to measure the H_alpha+[NII] rotation curve in three different locations {a central 0.1" wide slit and two parallel 0.2" wide slits offset by 0.2"}. We will use these observations to determine if the gas motions and line-profiles match those of a thin disk in Keplerian motion. Our strategy of securing data along three parallel slits yields kinematic constraints on the center of mass, inclination angle and line-of-nodes that are independent of photometric constraints. This greatly improves the robustness of our estimates compared to single slit measurements. Our observations will enable us to measure the mass within a radius of 7-14 pc. Detailed simulations show that any black hole or mass concentration in excess of 10^7 solar masses will be confidently detected. Even for the most distant and most massive bulges we should either detect a black hole or derive a meaningful upper-bound. In combination with our acquisition images of the central 5x5 arcsec, our results will for the first time establish the black hole mass distribution and its relationship to bulge mass/luminosity and cusp-slope in a significant number of local spiral galaxies.

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