Computer Science
Scientific paper
Jul 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8687k&link_type=abstract
HST Proposal ID #8687
Computer Science
Hst Proposal Id #8687 Galaxies
Scientific paper
def s defmbhM_o We propose STIS spectroscopy of the galaxies NGC 3706 {E3} and NGC 4486A {E2} to search for supermassive black holes {BHs}. NGC 3706 contains a bright, edge-on nuclear disk of stars. Therefore we can measure the BH mass mbh as easily as in a galaxy with a gas disk but without uncertainty about whether the motions are affected by non-gravitational forces. NGC 4486A, like NGC 4486B, is a dwarf elliptical companion of NGC 4486 {M s87} with signs of an unusually massive BH. Keck spectroscopy shows that its velocity dispersion Sigma eq 160 km s^-1 is abnormally high for a dwarf galaxy of absolute magnitude M_B eq -17.5. We want to know whether it is an exception to the correlation of mbh with bulge luminosity. We propose low-resolution Mg I b spectroscopy of the above galaxies and NGC 5845 to compare the stellar populations in their nuclear disks with those of their bulge components. Many ellipticals contain dust disks or stellar disks. NGC 4486A and NGC 5845 are ``Rosetta stone'' objects that contain both. They can provide direct evidence that gas disks grow stellar disks near the centers of early- type galaxies and thereby secularly increase the cuspiness of the mass distribution. The timescale of this process is unknown. Our spectra would tell us the relative ages of the stellar disks and bulges in two ellipticals that are caught in the act and in one with a remarkably prominent and fully formed stellar disk.
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