Berkeley – Scientists have uncovered a supermassive black hole at the
core of a svelte, spiral galaxy, a finding that questions a recently
devised rule of thumb in which only galaxies with bulging cores have
such black holes.

Dr. Alex Filippenko, professor of astronomy at the University of
California, Berkeley, and Dr. Luis Ho, an astronomer at the
Observatories of the Carnegie Institution of Washington, in Pasadena,
discuss these results in the May 1, 2003, issue of The Astrophysical
Journal Letters.

The scientists determined that galaxy NGC 4395, a flat “pure-disk”
galaxy with no central bulge, has a central black hole approximately
10,000 to 100,000 times the mass of our sun. This suggests that other
pure-disk galaxies, thought to be devoid of supermassive black holes,
may indeed have one lurking within – quite possibly the
featherweights of the supermassive black hole club.

“The supermassive black hole in NGC 4395 is the smallest one yet
found in the center of a galaxy,” said Filippenko. “This would be
consistent with the galaxy having a small bulge. However, the bulge
is not just small, it seems to be nonexistent.”

Supermassive black holes typically range from millions to billions of
times the mass of the Sun, dwarfing the more common stellar black
holes that are created by the runaway gravitational collapse of the
cores of massive stars.

NGC 4395 is 11 million light years away in the Northern Hemisphere
constellation of Canes Venatici (“the Hunting Dogs”). The galaxy has
long been known to emit significant amounts of light, including
visible light and X rays, from its central core region. This is a
telltale sign of the presence of a central, giant black hole actively
sucking in enough matter to create a swirling, superheated accretion
disk. Yet no supermassive black hole had been detected.

Filippenko and Ho used the Keck I 10-meter telescope on Mauna Kea in
Hawaii and the Japanese-U.S. ASCA X ray telescope to determine that
NGC 4395 indeed has a supermassive black hole, albeit an unusually
light one.

“Here is an example of a massive black hole that is low in comparison
to all previously reported supermassive ones, but it is definitely
much more massive than stellar-class black holes, and is located in a
galaxy that has no bulge,” Ho said. “Thus, having a well-developed
bulge is evidently not a necessary condition for the formation of
massive, central black holes.”

Filippenko and Ho confirmed the mass range using the velocity
dispersion technique for estimating the mass of black holes, and in
the process found that this powerful tool for inferring black hole
mass works on scales far lower than previously thought.

Velocity dispersion refers to how fast, on average, the stars in a
galactic core region are orbiting about the central black hole. It is
akin to taking an average speed of a swarm of bees circling about
their hive on paths (orbits) of differing size and orientation.
Although predicted theoretically back in the 1990s, confirmation of a
very tight correlation between velocity dispersion and supermassive
black hole mass came in 2000. But until now, that correlation was
always assumed to apply to black holes weighing in at millions or
billions of solar masses. Using this technique on the NGC 4395,
Filippenko and Ho found its mass to be 66,000 solar masses – nearly
in the middle of the range found using X-ray luminosity.

This means that the black hole mass/velocity dispersion relation may
apply even on scales of relatively small star clusters that contain a
central, relatively light, supermassive black hole, Ho said.

The scientists also suggest that NGC 4395 may represent a unique step
in the evolution of supermassive black holes, in which a bulge will
develop as the black hole grows. The velocity dispersion measurements
were based on a star cluster near the central black hole, a possible
indication that a bulge may someday form.

NOTE: Alex Filippenko can be reached at (510) 642-1813 or
alex@astro.berkeley.edu. Luis Ho is at (626) 304-0248 or lho@ociw.edu.

A copy of the ApJ-Letters article is at
http://mentor.lanl.gov/abs/astro-ph/0303429.