The M96 group of galaxies
This conspicuous group of galaxies
contains 3 Messier objects
and M105), plus a larger number of fainter
galaxies (including NGCs 3299, 3377, 3384, 3412 and 3489 as well as
UGC 5889, which is also called NGC 3377A in the Sky Catalogue 2000.0).
The Sc galaxy NGC 3389, which is in the same field and close to M105,
is probably a background galaxy, as its redshift corresponds to a receding
velocity of 1138 km/sec, whereas the members of the Leo I group have
radial velocities of only 449..766 km/sec.
In our image on the right hand side, M95 is in the lower right corner,
while M96 is in the lower middle, and M105 is the bright elliptical galaxy
above and left of the picture’s center, together with its fainter neighbors
NGC 3384 and faint NGC 3889.
Nial R. Tanvir of the
Cambridge Astronomy group has investigated this
group of galaxies with the Hubble Space Telescope. He and his coworkers
found 8 Delta Cephei variable stars in the brightest galaxy of the group,
M96, and were able to derive its distance
from the Cepheid period-luminosity relation: M96 is 231+/-13 times more
remote from us than the Large Magellanic Cloud, thus 12.7+/-0.8 Mpc
(41+/-2 million light years).
An improvement of this value is hoped to be obtained from ongoing HST
observations of Cepheid variables in the group galaxies
M95 and UGC 5889 (both spirals).
A first result was obtained for M95 in 1996-97 by the HST H0 Key Project
J.A. Graham et.al., The Extragalactic Distance Scale Key Project VII.
The Discovery of Cepheids in the Leo I Group Galaxy NGC 3351.
They obtained a distance of 10.05+-0.88 Mpc (32.8+-2.9 million light years),
which after correction for the new Cepheid distance scale becomes
10.90+-0.95 Mpc (35.5+-3.1 million light years).
As a mean value of the two distances obtained in the work of Tanvir and the
H0 key project team, we will use a distance of 38 million light years here.
From the distance derived here, it is possible to gauge a
diameter-velocity dispersion-relation for elliptical galaxies, namely by
using the galaxies M105 and NGC 3377.
By the relation obtained for this, the distance of the
Virgo and Coma clusters of galaxies could be
estimated; one obtains a distance of 18.3+/-2.0 Mpc (60+/-6 million
light years) for the Virgo cluster, and of 105+/-11 Mpc (~340 million
light years) for the Coma cluster of galaxies. (The Virgo cluster distance
may be estimated from that of the M96 group also by other methods,
yielding about the same value).
The Coma distance then allows to estimate the value of the current Hubble
constant (H0, “Hnaught”) to be
H0 = 69+/-8 km/(s*Mpc)
which is again (after the M100 result) intermediate between the
rivaling values of H0=50 and H0=100
(the values given here are corrected for the new Hipparcos results of
February, 1997).
The M96 group may be physically related to the
M66 group which is roughly at the same distance
and situated rather nearby in the sky.
The following table lists some data of the M96 or Leo I group members
listed above (most data from the Sky Catalogue 2000.0):
Name | RA(h:m) | Dec(d:m) | type | m_v | dim | RV |
---|---|---|---|---|---|---|
NGC 3299 | 10:36.4 | +12:42 | SABdm | 13.29p | 2.1×1.7 | 465 |
M95 | 10:44.0 | +11:42 | SBb | 9.71 | 7.4×5.1 | 649 |
M96 | 10:46.8 | +11:49 | Sbp | 9.24 | 7.1×5.1 | 766 |
UGC 5889 | 10:47.4 | +14:04 | SABm | 14.15p | 2.0×1.9 | 449 |
NGC 3377 | 10:47.7 | +13:59 | E5 | 10.21 | 4.4×2.7 | 595 |
M105 | 10:47.8 | +12:35 | E1 | 9.26 | 4.5×4.0 | 752 |
NGC 3384 | 10:48.3 | +12:38 | E7 | 9.96 | 5.9×2.6 | 641 |
NGC 3412 | 10:50.9 | +13:25 | E5 | 10.55 | 3.6×2.0 | 737 |
NGC 3489 | 11:00.3 | +13:54 | E6 | 10.33 | 3.7×2.1 | 576 |
Key:
Name: M/NGC/UGC number,
RA/Dec: Right Ascension and Declination for 2000.0,
type: Hubble type,
m_v: Visual magnitude,
dim: Angular diameter in arc minutes,
RV: Radial velocity wrt Galactic center in km/sec
(from R. Brent Tully’s Nearby Galaxy’s Catalog).
Last Modification: 6 Apr 1998, 21:50 MEST