A&A 383, 56-64 (2002)
DOI: 10.1051/0004-6361:20011723
A. Greve1 - K. A. Wills2 - N. Neininger3 - A. Pedlar4,5
1 - Institut de Radio Astronomie Millimétrique,
300 rue de la Piscine, 38406 St. Martin d'Hères, France
2 - Department of Physics and Astronomy, University of Sheffield, Hounsfield
Road, Sheffield S37RH, UK
3 - Astronomisches Institut der Universität Bonn, Auf dem Hügel 71,
53121 Bonn, Germany
4 - University of Manchester, Jodrell Bank Observatory, Macclesfield,
Cheshire SK119DL, UK
5 - Onsala Space Observatory, 43992 Onsala, Sweden
Received 28 September 2001 / Accepted 26 November 2001
Abstract
The fueling of the starburst in M82 may be related to a stellar
bar which pushes gas towards the center where it forms stars. The
observation by McKeith et al. (1993) of the near-IR CaII
photospheric absorption line allows a direct velocity measurement of
the stars in M82, and provides by this a confirmation of the predicted
x1 and x2-orbits of the bar in M82. From this and other
observations we find that the mass of the x2-orbit stars is
15
of the mass of the bar, and that the mass of the bar of
is 20-40% of M82's mass. This mass
concentration of
1kpc extent at the center of M82 underlines the
dynamic importance of the bar.
Key words: galaxies: individual: M82 - galaxies: structure - galaxies: stellar content
The starburst in M82, of approximately 10-50 Myr age, can possibly be explained by the presence of a stellar bar which pushes gas towards the center of the galaxy where it accumulates, is compressed, shocks, and forms stars. This stellar bar may have formed during the encounter of M81 and M82, several 100 Myr ago. Tidal arms visible in 21cm-H I still connect M81, M82, and NGC3077.
In a bar, the stars move on elliptical orbits along the major axis of
the bar, the x1-orbits, and at the center of the galaxy on
perpendicular orbits along the minor axis of the bar, the
x2-orbits. The consequence for the gas distribution is
motion of gas from the far ends of the bar towards the center, shocks
at the intersection of the x1 and x2-orbits, accumulation of
gas near and inside the x2-orbits, and the formation of dust
lanes along the leading x1-orbits (Contopoulos & Mertzanides
1977; Binney et al. 1991; Athanassoula 1992). Morphological evidence
for the bar in M82 comes from the box-shaped distribution of stellar
light, in particular measured in the 2.2 m K-band which
emphasizes late-type stars (Telesco et al. 1991; Larkin et al. 1994), and the indication of dust lanes from IR extinction
measurements of x1-orbit stars (Larkin et al. 1994). Kinematic
evidence of the x1-orbits comes from position-velocity
(p-v) measurements of neutral and ionized gas (CO, H
I, H
,
etc.; Shen & Lo 1995; Seaquist et al. 1996;
Neininger et al. 1998; Wills et al. 2000; McKeith et al. 1993).
Kinematic evidence of the x2-orbits can be seen in the CO and
H I data, however it is most clearly present in the p-v diagrams
obtained from the 12.8
m [NeII] emission line (Achtermann & Lacy
1995). In fact the ionized gas traced out by the [NeII] emission appears
to be largely confined to the x2-orbits only. There are no direct
velocity measurements of the stars of the bar which may be different from
the velocity of the gas, in particular in regions of shocks, dust lanes, and
bubbles. Direct information on the stars is important since they contain the
dominant mass of the bar and define the gravitational potential in which the
material moves.
Here we show that the earlier single long-slit spectroscopic
observation by McKeith et al. (1993) of the near-IR CaII
photospheric absorption lines (at 8662, 8542, 8498 Å), which are
strong in late type stars (Jaschek & Jaschek 1995), provides direct
kinematic evidence of the stellar x1-orbits and
x2-orbits of M82. The observations of near-IR
emission lines of H II regions, like [SIII] at 9069 Å and
Paschen-10 [Pa(10)] at 9014 Å, however do not immediately
reveal the x2-orbits, at least at the selected slit position
discussed here. Evidently, the stellar absorption lines can only be observed
where the stellar continuum is strong, which is along the major axis
of the bar and along the more extended major axis of the galactic
disk. We derive from the p-v diagrams the extent and the
mass of the bar.
![]() |
Figure 1:
Major axis (PA = 65
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Position | Stellar Velocities | Gas Velocities | |
CaII IR line | [SIII] | Pa(10) | |
('') | (kms-1) | (kms-1) | (kms-1) |
![]() ![]() |
|||
-34.0 | 82 | ||
-31.0 | 102 | ||
-28.0 | 82 | 100 | |
-25.0 | 92 | ||
-22.0 | 82 | 102 | |
-19.8 | 72 | 105 | |
-18.3 | 92 | 123 | |
-16.8 | 82 | 125 | 104 |
-15.3 | 62 | 114 | |
-13.8 | 61 | 95 | |
-12.3 | 72 | ||
-11.1 | 82 | 88 | 94 |
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|||
-10.2 | 111 | 102 | |
-9.3 | ![]() |
109 | |
-8.4 | ![]() |
109 | 102 |
-7.5 | ![]() |
101 | 105 |
-6.6 | 102 | 90 | 96 |
-5.7 | 92 | 83 | 92 |
-4.8 | 62 | 79 | 91 |
-3.9 | 52 | 70 | 55 |
-3.0 | 62 | 53 | 11 |
-2.1 | 52 | 36 | 3 |
-1.2 | 32 | 25 | -13 |
-0.3 | 22 | 6 | -18 |
0.6 | -17 | -15 | -36 |
1.5 | -17 | -42 | -46 |
2.4 | -77 | -69 | -73 |
3.3 | ![]() |
-87 | -80 |
3.6 | ![]() |
||
4.2 | ![]() |
-93 | -81 |
4.5 | ![]() |
||
5.1 | -116 | -98 | -90 |
6.0 | -132 | -101 | -89 |
6.3 | -142 | -106 | -90 |
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|||
6.9 | -107 | ||
7.8 | -106 | -115 | -100 |
8.7 | -106 | -122 | -100 |
10.2 | -97 | -118 | |
11.7 | -57 | -84 | -87 |
13.2 | -47 | -77 | -69 |
14.7 | -77 | -74 | |
16.2 | -76 | -83 | |
17.7 | -57 | ||
19.2 | -47 | -90 | -45 |
20.7 | -97 | ||
22.2 | -87 | ||
23.7 | -77 | -80 | |
25.9 | -57 | ||
28.9 | -57 | ||
31.9 | -27 | ||
34.9 | -67 | -96 |
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Figure 2:
Schematic explanation of ``spraying'' in M82 (not drawn to scale):
some gas is pulled off the trailing x1-orbits and is pushed towards the
leading x1-orbits, forming dust lanes (DL). Ma is the major axis, Mi the
minor axis of the bar. The region of the x1 and x2-orbit stars is
indicated. The extent of the bar (x1-orbits) is ![]() ![]() ![]() |
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The observation used in this publication was described earlier
(McKeith et al. 1993) and was made to investigate the rotation of gas
and stars in M82, which were previously claimed to be different
(Saito et al. 1984). The single long-slit spectroscopic observation,
made with the 4.2m WHT (La Palma, Spain) along the major axis of
M82 (
), covered the wavelengths from [OII] 3729Å to [SIII] 9069Å with a velocity resolution of
30kms-1. The seeing was good and of the order of
0.7''. The velocity information of the stellar CaII photospheric
absorption line at 8542Å (strongest triplet line) and of the
ionized gas emission lines [SIII] and Pa(10), taken from the
observation by McKeith et al. (1993), is summarized in Table 1. The
extreme velocities (indicated by the dots in Table 1), which
reveal the x2-orbit stars, are confined to narrow regions
2.5'' (
45pc) in extent, at approximately 5'' distance
on either side of the dynamical center. These extreme velocities are only
detectable under good (sub-arcsec) seeing conditions.
The investigation by McKeith et al. (1993) revealed that at the same
location in M82 the rotation of the gas and stars is globally the
same, and that the apparent rotation curve becomes steeper at longer
wavelengths and in smaller regions at the center. McKeith et al. explained these features as an effect of extinction which hides at
blue wavelengths the rapidly rotating core. They also found that the
velocity measured in the direction of the center from near-IR
ionized gas emission lines and near-IR stellar absorption lines
is close to the velocity of the 12.8m [NeII] emission line
(Beck et al. 1978), which is unaffected by extinction and probes the
center of M82. They concluded therefore that - despite an average
visual extinction of
-8mag towards the
center region
(Telesco et al. 1991; Larkin et al. 1994) - the near-IR
lines, and in particular the near-IR CaII stellar absorption lines,
probe also the center of the galaxy or regions very close to it. Today
we are able to interpret this earlier observation of the near-IR
CaII line in the light of the proposed stellar bar.
The major axis p-v diagram of M82, based on the observation
by McKeith et al. (1993; including Table 1), of the region extending
to 100'' (
1700pc) on either side of the
galactic center and containing the bar is shown in Fig. 1. This
figure is mainly constructed from the stellar CaII line and thus
shows in essence the motion of stars. The velocities display the
rotation of M82.
The equivalent widths of the CaII triplet lines (see McKeith
et al. 1993, their Fig. 1) are
Å,
Å, and
Å, indicating
primarily G-KIII-V type stars (Jaschek & Jaschek 1995)
in agreement with the fact that the bar consists of late-type stars
which were spatially reshuffled in the encounter with M81. Similar
stellar types are derived by Förster Schreiber et al. (2001).
Distances along M82's major axis are originally measured in angular
scale (). For a distance of 3.6Mpc (Freedman et al. 1994;
Sakai & Madore 1999), 1'' is equivalent to 17.5pc linear
scale (r).
Detailed knowledge of the orientation of the bar, as required to understand the measured p-v diagrams, is not easily available from a single long-slit spectrogram. We use, and summarize, the results obtained by Telesco et al. (1991) and Wills et al. (2000).
The position angle of M82's major axis is
;
the western side moves towards the observer, the eastern side away
from the observer. In the following we refer to the axis at
as the ``galactic plane''. The inclination of M82 is
,
with the southern side being more distant as for instance
suggested by the higher reddening and polarization (Visvanathan &
Sandage 1972; Notni & Bronkalla 1983; Chesterman & Pallister
1980), the motion of ionized gas (Götz et al. 1990), and the
geometry of the minor axis outflow (McKeith et al. 1995; Shopbell
& Bland-Hawthorn 1998). However, from an observed increase
towards the north of free-free absorption due to ionized gas, Wills et al. (2000) discuss the possibility of the opposite orientation. Following
Telesco et al. (1991, their Fig. 11), the bar is inclined by
4
with respect to M82's galactic plane, with the western
side of the bar lying above the galactic plane. As schematically shown in
Fig. 2, the major axis of the bar is
turned out of the plane of the sky by
22
(
), with the
eastern side being more distant. We are looking at the major axis of
the bar at an angle of
68
so that the major axis
p-v diagram resembles that shown by Binney et al. (1991, their Fig. 1, left and middle panel; though referring to our
Galaxy) and Achtermann & Lacy (1994, their Fig. 15) for M82. The
orientation of the bar is inverted when using the orientation of M82
suggested by Wills et al.
The x2-orbits are perpendicular to the x1-orbits and their
major axis is rotated to the line-of-sight by
(Fig. 2). If the southern side of M82
is more
distant, the x2-orbits extend at the eastern side out of the plane of
the sky towards the observer. Following Figs. 1 and 3, the
x2-orbit stars on the north-eastern side move away from the
observer (red-shifted), at the south-western side towards the observer
(blue-shifted).
The following figures and parameters refer to the geometry and velocities of the bar as seen projected onto the plane of the sky.
For the interpretation of optical and radio observations of bar galaxies it is important to consider the effect of spraying as predicted from N-body calculations (Athanassoula 1992) and used, for instance, to explain the observations of NGC1530 (Downes et al. 1996). Altough the bars of bar galaxies are massive and several kpc in extent, the 1kpc-size bar of M82 (see below) may produce the same effect of spraying. The effect is schematically shown in Fig. 2. When passing the gravitational potential of the x2-orbit stars, some gas (and perhaps also some stars) is pulled off the trailing x1-orbits and is pushed towards the leading x1-orbits. The spraying gas may shock with the gas on the leading x1-orbits, and eventually form dust lanes and stars.
Figure 3 shows an overlay
of the observation of the near-IR stellar CaII line, the [SIII] and
Pa(10) lines (Table 1), and the x1-orbits, cusped orbits, and
x2-orbits of the bar predicted by Wills et al. (2000). Their
model of the bar is based on observations of neutral and ionized gas
motions (CO, H I, [NeII]).
![]() |
Figure 3:
Major axis (PA = 73
![]() ![]() ![]() ![]() ![]() |
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As evident from Figs. 1 and 3, the near-IR CaII stellar
absorption line clearly traces the x2-orbits which extend to
5'' (
90pc) from the galactic center
where the turn-around velocity is
150kms-1. The observation of the [SIII] and
Pa(10) gas emission lines does not show the extreme turn-around
velocity of the stellar x2-orbits. The gas apparently enters the
region of the x2-orbits at a velocity of
100kms-1 and follows the rotation of the stellar bar
only at the inner
3''(
50pc).
The original kinematic evidence for the x2-orbits comes from
Achtermann & Lacy's (1995) 12.8m [NeII] emission line
observation, which covers a radial distance of
20''(
350pc).
![]() |
Figure 4:
The contour lines show the velocity of the 12.8![]() ![]() |
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The 21cm-H I observation published by Wills et al. (2000,
their Fig. 9) does not clearly show the positive velocities of the
x2-orbits, and the negative velocities mainly on the
southern side of the galactic plane. The CO observation by Shen & Lo
(1995) (shown by Wills et al., their Fig. 9) shows mainly the
negative velocities of the x2-orbits on the southern side and in
the galactic plane, and marginally the positive velocities in and on
the northern side of the galactic plane. 12CO gas on the western
side x2-orbits is clearly seen in the observation by Weiß et al. (2001). However, they interpret this velocity feature as the
eastern part of a super-bubble (see below). 12CO gas on the
eastern side x2-orbits is marginally seen in Weiß' et al. observation. The recent determination by Weiß et al. of the H2distribution in M82 shows a weak central concentration
(
cm-2 column density) of similar
extent as the x2-orbit region.
The observation by Larkin et al. (1994) shows on the major axis
enhanced Br
emission at a radial distance of
4-5'' on either side of the galactic center, i.e. at
the edge of the x2-region, but mainly on the southern side
(0'' to -3'') of the galactic plane. The bulk velocity
of this material at 4-5'' radial distance is
(50-100)kms-1 (Larkin et al., their
Figs. 5 and 6) while the x2-orbit stars at this position have
a velocity of
150kms-1. The discrepancy of the
Br
material velocity, as compared to the stellar velocity
discussed here, may be explained, partially, by the low velocity
resolution (90kms-1) of Larkin's et al. observation. On
the other hand, the Br
radiating gas is approximately
located at the edge of the x2-orbits where the gaseous material
may ``spray'', shock, and form stars (Fig. 2), so that some of the gas is at
a velocity different from that of the x2-orbit stars. The
difference of
50-100kms-1 between the stellar velocity
and the ionized gas velocity is of the order of the expected shock velocity.
This dynamical feature may explain, at least partially, the fact that the
ionized gas observed in [SIII] and Pa(10) does not follow the stellar
turn-around velocity at the edge of the x2-orbit region but a
velocity modified by a superimposed shock (Fig. 3). Telesco et al. (1991)
find 10.8,19.2 and30
m continuum emission from gas and dust (of a
few arcsec extent) concentrated at the far ends of the x2-orbits.
The Br
emitting material and the emission features E1 and
W1 measured by Larkin et al. (1994) coincide with the continuum emission
observed by Telesco et al. and most likely is the same gas. This gas
concentration is seen along the tangential line-of-sight of the x2-orbits
and is assumed to form a ring (Achtermann & Lacy 1994; Larkin et al. 1994).
The light of the x2-orbit stars confined to the radial
distance of 5'' is not separately seen in the
2.2
m major axis profile measured by Telesco et al. (1991,
their Fig. 10), but is clearly seen as a central peak in the profile
measured by Larkin et al. (1994, their Fig. 2; effective radius
,
pc, see footnote c in Table 3).
In summary there exists convincing evidence from stellar continuum,
stellar absorption line, and gas emission line observations that M82
has a family of stellar x2-orbits which extends to
5'' (
90pc) projected radial
distance. The turn-around velocity, which is
approximately the line-of-sight velocity of the x2-orbits, is
150kms-1; the projected velocity gradient is
150kms-1/5
kms-1(arcsec)
-1 = 1.7kms-1pc-1.
However, in the cusped orbit region the gas (and perhaps also some
stars) ``spray'' from the trailing x1-orbits onto the leading
x1-orbits, usually producing shocks and dust lanes, as seen in
other bar galaxies. The cusped orbit region of M82
coincides approximately with the dust lanes proposed by Larkin et al. (1994) and Achtermann & Lacy (1995), and predicted in simulations
of gas flow in stellar bars (Athanassoula 1992). Following Larkin et
al., and Fig. 2, the western dust lane of M82 lies mainly in front of
the stars of the bar which explains the visual stellar extinction of
mag measured in this direction;
the eastern
dust lane lies mainly behind the stars of the bar which explains the
measured lower visual stellar extinction of
mag. However, the observed apparent asymmetry in the p-v pattern of the cusped orbit region is only partially due to
extinction in the dust lanes. The reason that in the observation of
Fig. 3 mainly a western negative-velocity branch and an eastern
positive-velocity branch is seen, is probably due to significant
spraying of gas (and some stars) which results in a similar p-v
pattern as the incomplete cusped orbits. To clarify the situation, a
raster of long-slit observations parallel to the major axis is
required.
From the observations published by Wills et al. (2000, their Fig.9) we notice that the cusped orbit region contains CO on the western side of the galactic center and primarily on the southern side of the galactic plane. H I and [NeII] is marginally seen on cusped orbits on the western side of the galactic center and on the northern side of the galactic plane. It is important to note that in the cusped orbit region the velocity of H I absorption features (seen against continuum sources) however follows the straight branch of the cusped orits and the x1-orbits (Wills et al. 2000, their Fig.10).
The prominent (CO) molecular gas lobes are located between 5
(90pc
pc) radial
distance and thus occupy to a large extent the region of the cusped
orbit stars. The effect of spraying may explain the strong
accumulation of the molecular gas in this region. The CO gas follows
the motion of the ``outer'' x1-orbit stars (Neininger et al. 1998).
The [NeII] observation by Achtermann & Lacy (1995; Fig. 4) shows a -70 to -185kms-1 velocity component (called W2) between approximately -7''(-120pc west) and -13''(-230pc west) radial distance. The W2-component is also seen in CO and H I (Wills et al. 2000, their Fig.9) at the western side of the unusual ``hole''-feature, in the galactic plane and on the southern side. Wills et al. suggest that the eastern side of this ``hole''-feature is gas moving along the x2-orbits and that the western side, which corresponds to W2, is produced by gas moving along the cusped orbits. Since an equivalent component has not convincingly been identified on the eastern side of the galaxy, Wills et al. suggest that the bar in M82 is asymmetric. As an alternative explanation for the asymmetric orbits of the gas, Weiß et al. (1999, 2001) interpret the ``hole''-feature including the W2-component as an expanding super-bubble, containing near its center the SNR 41.9+58, and with molecular gas flowing out into the halo. In the observation of the stellar CaII line we find no evidence of the W2-component and of the western ``hole''-feature, suggesting that these components are features of the gas only.
In the 2.2m major axis profile published by Larkin et al. (1994, their Fig. 2) the cusped orbit region corresponds to the well
defined and symmetric ``inner plateau'' (effective radius
,
pc) and the sharp transition
(30pc wide) to the ``outer
plateau''. The light distribution and the major axis velocity
distribution do not indicate an asymmetric bar.
As evident from Fig. 3, outside the cusped orbit
region (
,
i.e.
r) the stars
and gas move on x1-orbits which extend to a radial
distance of
30'' (
500pc). The turn-around velocity
of the x1-orbit stars at
30'' (
pc) radial distance is
125-150 kms-1; the projected velocity
gradient of the x1-orbits is 125kms
kms-1(arcsec)
-1 = 0.35kms-1pc-1.
In the 2.2m major axis profile measured by Larkin et al. (1994, their Fig. 2) the region of the ``outer'' x1-orbits
corresponds to the well defined and symmetric ``outer plateau''
(effective radius
,
pc).
As evident from Fig. 1 and Wills' et al. (2000) observations,
projected onto the center region of M82, but in particular outside
the bar, gas and stars are observed which belong to the galactic
disk. Projected onto the center region, this material is seen in
21cm-H I (absorption) with a projected velocity gradient of
3kms-1(arcsec)
kms-1pc-1 (Wills et al. 2000, their
Figs. 9 and 11). This foreground disk material is also seen with
the same velocity gradient in blue wavelength emission lines and the
blue stellar CaIIK line at 3933Å (McKeith et al. 1993, their
Fig. 3). At blue wavelengths the average extinction towards the center
is so high that
only the slowly moving material of the outer galactic disk is
seen. Outside the bar (
r), the CaII absorption line
of the disk stars indicates a projected velocity gradient of
1kms-1(arcsec)
-1 = 0.1kms-1pc-1(Fig. 1).
In the derivation of masses
[with G the gravitation constant] we assume that the turn-around
velocity v(rx2) of the x2-orbit material
determines the mass M(x2) of the x2-orbit stars (inside
,
i.e.
pc), and that the turn-around velocity v(rx1) of
the ``outer'' x1-orbit material determines the mass M(x1) of
the stars and gas concentrated along the bar (inside
,
i.e.
pc). The corresponding masses are given in Table 2.
Region | Radius | Velocity v at r | Velocity Gradient | Mass | Ref. |
![]() |
(kms-1) | (kms-1/'') | (![]() |
||
Stellar Bar Components | |||||
x2-region | 5''-90pc | 150 | 30 |
![]() |
|
x1-region![]() |
30''-500pc | 125 | 6 |
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|
Total (
![]() |
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||||
Mass Model (Götz et al.) | 30''-500pc |
![]() |
1 | ||
Mass Model (Förster-S. et al.). | 30''-500pc |
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2 | ||
Molecular Gas & Dust | |||||
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3 | |||
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4 | |||
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3, 4 | |||
Young starburst stars | ![]() |
![]() |
5 | ||
Galaxy Mass | |||||
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![]() |
6 | |||
![]() |
![]() |
1 |
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Figure 5:
H![]() ![]() ![]() ![]() ![]() |
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We find that the mass of the x2-orbit stars is 15%
of the mass of the x1-orbit stars (including the cusped orbit
stars), and that the mass of the bar is
.
When adopting
for the mass of M82 inside the radius of
2kpc the value
determined by Sofue et al. (1992), we find that the mass concentrated
in the bar is
20% of the galaxy mass. However, if we use
the mass distribution of M82 derived by Götz et al. (1990; see
also Förster Schreiber 2001), the mass inside the radius of
kpc is
and thus only half of the mass given by
Sofue. When using the mass of M82 determined by Götz et al., the
bar contains
40% of the galaxy mass. The mass of the gas
and dust
in the region of the bar is
40% of the stellar mass of the bar.
We get similar mass ratios from an analysis of the 2.2m major
axis profile measured by Larkin et al. (1994). If the
2.2
m radiation is primarily due to (late-type) stars, and if
the observed brightness of the radiation is proportional to the number
of stars, hence the mass along the line-of-sight, the proportionality
of the individual stellar mass components is
Stellar Component | 2.2![]() ![]() |
Radius![]() |
Brightness![]() |
10
![]() |
![]() |
Ii[mag('')-2] | |||
Background (o) | - | 14.5 | 1 | |
x1 stars (1) | Outer Plateau | 30''-500pc | 13.5 | 2.5 |
Cusped orbit stars (c) | Inner Plateau | 10''-175pc | 12.1 | 8.7 |
x2 stars (2) | [Peak] | 2''-35pc![]() |
11.7 | 12.6 |
From Larkin et al. (1994), their Fig. 2.
See Sect.4. The full extent of the component is
.
Weighted by the exponential spatial light distribution.
We assume in these estimates that the dominant amount of stellar
mass is concentrated in the late-type stars of the bar, and not in
young massive stars produced in the starburst. When following McLeod
et al. (1993), the mass of the stars formed in the starburst is
,
which is
approximately 1/10 of the mass of the bar. The newly formed stars are
primarily located near the molecular ring so that the x2-orbit
region contains only a negligible percentage of young massive
stars. The mass M(x2) (Table 2) is therefore primarily due to the
late-type stars of the bar.
This paper shows the stellar rotation curve of M82 up to
1700pc radial distance, fully traced from the near-IR
CaII photospheric absorption line of late-type stars. The
position-velocity analysis of this line gives direct evidence of the
stellar bar in M82, in particular since the observation shows
the x2-orbit stars at the center of the galaxy, hidden behind
substantial visual extinction but visible at (near-)IR
wavelengths. The observed x1 and x2-orbit structure
agrees with the stellar light distribution (at 2.2
m) of the bar
and with gas moving on the stellar orbits, although local disturbances
of the gas motion do occur. The x2-orbits extend to
pc; the x1-orbits extend to
pc; the
cusped orbits are located between
r
pc. The cusped orbits are not clearly visible in our observation
probably because in this region there exists significant spraying of
gas, and probably also of some stars. The orbital revolution time of
the x2-orbit stars is
2Myr (
pc,
kms-1) and of the x1-orbit stars
10-15Myr (
pc,
kms-1).
The mass of the bar is
.
The
x2-orbit stars contain
15% of the mass of the bar.
Dependent of the adopted mass model, i.e. the one determined by Sofue
et al. (1992) or Götz et al. (1990), the stellar bar contains
approximately 20-40% of M82's mass. This mass has a
dominating influence on the kinematics of the stars and the gas, at
least in the
1kpc center region. The stellar bar (at
2.2
m) defines the kinematic center of M82 rather than the
center region gas, which constitutes only
40% of the
stellar mass.
Figure 5 shows, in an idealized way, the location of the stellar bar
superimposed on an HST H
image. The bar (long side of the
box) is roughly aligned to the galactic plane of M82; the stars move
roughly in this plane. The thickness of the bar, in this image, is
taken to extent
10'' (
150pc) above the
galactic plane. This value is taken from the K-image published by
Telesco et al. (1991); the image shows late-type stars which are the
major constituents of the bar. Figure 5 shows the region of the
x2-orbit stars (
), the region
to which the cusped orbit stars extent (x1(co): 5
), and the full extent of the
x1-orbit stars (
). Because of
the large visual extinction, the H
image shows mainly the
pheripheral parts of M82 and the outflow along the minor axis,
especially on the SE side (Shopbell & Bland-Hawthorn 1998). The
image shows heavy extinction on the NE side in the region of the
x1-orbits. This is foreground extinction and not the dust lane
assumed to be produced by sprays (see Fig. 2); at this side of the
center (NE) the dust lane lies on the far side of the galaxy. The minor
axis outflow, which breaks out of the galactic disk at a height of
150pc (McKeith et al. 1995), is confined to the inner
region of the bar, i.e. approximately the region of the cusped orbits
where the molecular ring is located. This is the main area of the
starburst.
Acknowledgements
We appreciated the discussions with D. Downes (IRAM) on this subject. We thank the referee D. Elmegreen for her comments. Figure 5 is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. The STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.