Issue |
A&A
Volume 498, Number 2, May I 2009
|
|
---|---|---|
Page(s) | 419 - 423 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361/200911737 | |
Published online | 19 March 2009 |
On the possible generation of the young massive open clusters
Stephenson 2 and BDSB 122 by
Centauri
G. M. Salerno1 - E. Bica1 - C. Bonatto1 - I. Rodrigues2
1 - Universidade Federal do Rio Grande do Sul, Departamento de Astronomia
CP 15051, RS, Porto Alegre 91501-970, Brazil
2 -
IP&D - Universidade do Vale do Paraíba - UNIVAP, Av. Shishima Hifumi, 2911 - Urbanova,
São José dos Campos 12244-000, SP, Brazil
Received 27 January 2009 / Accepted 10 February 2009
Abstract
Context. Passing through the disk of a galaxy, a massive object such as a globular cluster can trigger star formation.
Aims. We test the hypothesis that the most massive globular cluster in the Galaxy, Centauri, which crossed the disk approximately
Myr ago, may have triggered the formation of the open clusters Stephenson 2 and BDSB 122.
Methods. The orbits of Centauri, Stephenson 2, and BDSB 122 are computed for the three-component model of Johnston, Hernquist & Bolte, which considers the disk, spheroidal, and halo gravitational potentials.
Results. With the reconstructed orbit of Centauri, we show that the latest impact site is consistent, within significant uncertainties, with the birth-site of the young massive open clusters BDSB 122 and Stephenson 2. Within the uncertainties, this scenario is consistent with the timescale of their backward motion in the disk, shock propagation and delayed star formation.
Conclusions. Together with open cluster formation associated with density waves in spiral arms, the present results are consistent with massive globular clusters being additional progenitors of open clusters, the most massive ones in particular.
Key words: galaxy: globular clusters: individual: Centauri -
galaxy: open clusters and associations: individual: BDSB -Galaxy: open clusters and associations: individual: Stephenson 2
1 Introduction
Disk-stability criteria and impact assumptions suggest that the passage of a globular cluster (GC) can trigger a bubble or wave of self-propagating star formation within the disk of the Galaxy (Wallin et al. 1996). The initial mechanical perturbation produces a local enhancement in the interstellar medium (ISM) density, from which localised star formation may occur. Subsequently, clustered star formation may happen along the border of a radially expanding density wave or ionisation front (e.g., Soria et al. 2005 - hereafter SCP05; Elmegreen & Lada 1977; Whitworth et al. 1994). The expanding bubble is capable of compressing the neutral ISM above the stability criterion against gravitational collapse. Alternative star-formation triggering mechanisms are the infall of a high-velocity HI cloud (Elmegreen et al. 2000; Larsen et al. 2002), or hypernova explosions (Paczynski 1998).
Prominent, isolated star-forming bubbles have been observed in external galaxies. A
bubble of diameter
pc was detected in NGC 6946 (Larsen et al. 2002),
containing a young super star cluster and at least 12 surrounding young clusters, the latter being
comparable in luminosity to the most luminous Galactic OCs. The triggering mechanism in NGC 6946
appears to be the impact of a high-velocity HI cloud and/or hypernova explosions (Elmegreen et al. 2000).
The Galaxy may harbour similar structures, a possible example being the Cygnus superbubble,
which contains OB associations (Vlemmings et al. 2004, and references therein).
For a GC, the triggering effects are essentially gravitational. A natural assumption is that GCs, crossing the disk every 1 Myr on average, may be responsible for some star formation. A possible case relates the origin of the OC NGC 6231 to the GC NGC 6397 disk-crossing (Rees & Cudworth 2003). Another possibility is that the low-mass GC FSR 584 has triggered star formation in the W 3 complex (Bica et al. 2007).
The OCs Stephenson 2 and BDSB 122 were discovered in 1990 (Stephenson 1990) and 2003
(Bica et al. 2003), respectively.
2MASS images of both clusters are shown in Fig. 1.
The suspected richness of Stephenson 2 in red supergiants was
confirmed by Nakaya et al. (2001) and Ortolani et al. (2002), providing an age of
Myr, and a distance
from the Sun of
kpc (Ortolani et al. 2002). Both clusters are among the most massive OCs
known in the Galaxy. BDSB 122 has 14 red supergiants, is located at
kpc from the Sun,
and has an estimated mass of
,
and an age of 7-12 Myr (Figer et al. 2006). Stephenson 2
has 26 red supergiants, is located at
kpc from the Sun, has an estimated mass
of
,
and an age of 12-17 Myr (Davies et al. 2007). Their distances from the Sun are
identical, within uncertainties, and their projected separation on the sky is
pc. The designation
Stephenson 2 was originally assigned by Ortolani et al. (2002), and also adopted by Dias
et al. (2002, and updates).
Stephenson 2 and BDSB 122 are clearly in the red supergiant
(RSG) phase (Bica et al. 1990). Davies et al. (2007) referred to these clusters as RSGC 1 and RSGC 2, respectively.
![]() |
Figure 1:
|
Open with DEXTER |
![]() |
Figure 2:
The present-day positions (and uncertainties) of Stephenson 2,
BDSB 122, and |
Open with DEXTER |
The positions (and uncertainties) of both clusters, together with Centauri (NGC 5139), are shown
in Fig. 2 superimposed on a schematic view of the Milky Way (based on Momany et al. 2006; and
Drimmel & Spergel 2001). BDSB 122 and Stephenson 2 are slightly closer to the Galactic centre
than the Scutum-Crux arm. Several other young clusters from the catalogues of Bica et al. (2003) and
Dutra et al. (2003) have already been studied in detail (e.g., Soares et al. 2008; Ortolani et al. 2008; Hanson & Bubnick 2008).
We trace the orbits of both
Centauri and Stephenson 2 backwards in time (and
consequently, also that of BDSB 122) in the disk, testing an impact hypothesis for the
origin of these two massive OCs. Using as constraints the GC space velocity, orbit integrations
in the Galactic potential have been applied widely to 54 GCs (e.g., Dinescu et al. 2003;
Allen et al. 2008).
This paper is structured as follows. In Sect. 2 we study the past orbit of
Centauri. In Sect. 2.1, the past orbits of Stephenson 2 and
Centauri are compared to search for spatial and time coincidence. Our conclusions
are presented in Sect. 3.
2
Centauri as a projectile
The most massive Galactic GC, Centauri
(
- Nakaya et al. 2001), has a
metallicity spread and a flat density distribution typical of a dwarf galaxy nucleus captured by
the Galaxy (Bekki & Freeman 2003). Thus, irrespective of the existence of young massive clusters,
in some way associated with the impact site, the orbit of
Centauri in the Galactic potential
is worth consideration in searching, in particular, for the effects of the last disk passage.
Evidence of a similar disk impact and a star-forming event has been observed in the spiral galaxy
NGC 4559 with Hubble Space Telescope (HST), XMM-Newton, and ground-based (SCP05) data.
The age of the star-forming complex, which has a ring-like distribution, is
Myr. It appears to
be an expanding wave of star formation, triggered by an initial density perturbation. The most likely
triggering mechanism was a collision with a satellite dwarf galaxy crossing through the gas-rich
outer disk of NGC 4559, which may have been the dwarf galaxy visible a few arcsec to the NW of the
complex. This scenario is reminiscent of a scaled-down version of the Cartwheel galaxy
(Struck-Marcell & Higdon 1993; Struck-Marcell et al. 1996).
As another example, proper motions (PMs) and radial velocity suggest that the GC NGC 6397
crossed the Galactic disk 5 Myr ago, possibly triggering the formation of the OC NGC 6231
(Rees & Cudworth 2003), and thus lending support to the present scenario (Wallin et al. 1996).
NGC 6397 and NGC 6231 are closely projected on the sky (
,
). However, in the case of the disk-crossing of
Centauri
being the possible triggering mechanism of BDSB 122 and Stephenson 2,
the GC is now widely apart from the pair of massive OCs (
,
). Thus, PM and radial velocity are fundamental constraints
for the analysis of
Centauri, and impact solutions require a detailed integration of
its orbit across the Galactic potential.
Table 1: Present-day cluster positions.
![]() |
Figure 3:
Top-left panel: galactocentric XY-plane projection of the |
Open with DEXTER |
2.1 Orbit computation
We employ a three-component mass-distribution model of the Galaxy resembling that in
the study of a high-velocity black hole on a Galactic-halo orbit in the solar neighbourhood
(Mirabel et al. 2001, and references therein). In short, we use the three-component model
of Johnston et al. (1996) - hereafter JHB96 - in which the disk, spheroidal, and halo gravitational potentials are
described by
(Miyamoto & Nagai 1975),
(Hernquist 1990),
and
,
where
,
,
,
R and z are the cylindrical
coordinates, and the scale lengths a=6.5 kpc, b=0.26 kpc, c=0.7 kpc, and d=12.0 kpc.
Table 1 shows the Galactic and Equatorial coordinates of the three clusters.
Following Mizutani et al. (2003), the relevant parameters for computing the motion of
Centauri are the distance from the Sun
kpc, the PM
components (
)
and
,
and finally the heliocentric radial velocity
.
The models were computed with
kpc (Bica et al. 2006) as the distance of the Sun
to the Galactic centre. The Galactic velocities of
Centauri are
,
,
and
.
Alternatively, we also computed orbits with
kpc, which was the value obtained by Eisenhauer et al. (2005). By means of the statistical
parallax of central stars, it should be noted that Trippe et al. (2008) found
kpc,
while Ghez et al. (2008), with the orbit of one star close to the black hole, found
kpc
or
kpc, under different assumptions. Cluster distances are heliocentric, and
therefore do not depend on
;
on the other hand, the value of
has some effect on the potentials,
and can thus, affect the orbit computation. Since the difference between the adopted value of
and
the more recent measurements is insignificant, the value of
should not influence significantly the present
results.
Based on the rotation curves of Brand & Blitz (1993) and Russeil (2003), and an estimate with
the galaxy mass model described above (Mirabel et al. 2001), we derived the orbital
velocity of Stephenson 2 to be
.
The nearly flat Galactic rotation curve at the Stephenson 2 position
allows us to adopt this circular velocity also for the orbits corresponding to distance
uncertainties (Sect. 1). The orbit of
Centauri, computed back over 2 Gyr,
is comparable to that derived by Mizutani et al. (2003), in particular its Rosette pattern, which
is projected
on the XY plane (Fig. 3). The simulation indicates that
Centauri collided with the disk as
recently as
Myr ago. This is so short a time that fossil remains of this event may nowadays
be
detectable in the disk.
![]() |
Figure 4:
Close-up of the impact site. Left panel: orbits computed with
|
Open with DEXTER |
Figure 3 (top-left panel) shows the Galactic XY-plane projection of the orbital motion of
Centauri during the past 2 Gyr. In the remaining panels, we focus on the past 30 Myr of
the motion of
Centauri and Stephenson 2. For Stephenson 2, we consider the
different orbits resulting from the adopted distance from the Sun and their corresponding
uncertainties (Sect. 1).
It is interesting that the orbit of Stephenson 2 passes close to the impact site of
Centauri at a comparable time, within the uncertainties (see below). Since Stephenson 2 and
BDSB 122 have almost the same position (within the uncertainties), the same conclusions hold for the
latter cluster. The XZ and YZ-plane projections (bottom panels) indicate that
Centauri emerged
at
from the plane to its present position.
To probe orbital uncertainties owing to the adopted potential, we also employed the potential
model of Flynn et al. (1996) - hereafter FSC96 - and tested consequences of variations of
in the input parameters of JHB96. The results are shown in Fig. 3 (top-right panel), from
which we conclude that orbit variations due to the adopted potential are much smaller than our error
ellipsoid (Fig. 4, right panel).
Close-ups of the Centauri impact site and the back-traced positions of Stephenson 2
are shown in Fig. 4 (left panel) for a Sun's distance from the Galactic centre of both 7.2 kpc
and 7.6 kpc. It is clear that the value of 7.6 kpc does not significantly alter the orbit of the encounter.
The right panel
shows the error ellipsoid of several impact site simulations computed by varying initial conditions
according to the errors in the different relevant input quantities. The ellipsoid reflects variations
implied by velocity uncertainties in the PM, radial velocity and present position of
Centauri
along the line of sight in the (U, V, W) velocities. The impact obtained with a Galactocentric distance
kpc is also shown. The disk-orbit of Stephenson 2 crosses the
Centauri ellipsoid
error distribution. The range in impact site to proto-cluster separations contains distances smaller
than
kpc, with an average separation of
pc (intersection area in Fig. 4,
right panel). Larger separations would require prohibitive expansion velocities, despite the fact
that we are dealing with an encounter in a denser, central part of the disk, while in NGC 4559, the
event was external.
For the GC-induced formation hypothesis to be valid, the timescales associated with the
onset of star formation (after impact), duration of star formation and the cluster age, should
be compatible with the disk-crossing age. Following Vande Putte & Cropper (2009), the first timescale in not
well known, ranging from virtually instantaneous, i.e. negligible compared to the cluster age,
to 15 Myr (Lépine & Duvert 1994) and 30 Myr (Wallin et al. 1996). The star formation timescale may
be short,
yr, as suggested by McKee & Tan (2002) for stars more massive than 8
.
Given that the ages of Stephenson 2 and BDSB 122 are within the ranges of 12-17 Myr and 7-12 Myr, respectively,
Centauri, which crossed the disk
Myr ago, may have triggered their formation
only if the star formation started during a time period of less than
Myr, which is within the accepted
range. In the case of NGC 4559, these combined timescales are less than
Myr
(Soria et al. 2005).
The above clues suggest that the most recent crossing of
Centauri through the disk occurred close to the sites where two massive OCs
were formed.
Both Stephenson 2 and BDSB 122 are younger than the age of the impact, and
the differences in age of a few Myr are consistent with the shock propagation and subsequent star formation.
The overall evidence gathered in the present analysis supports
Centauri being the origin of
this localised star formation in the Galaxy, which harbours two of the more massive known OCs.
This work suggests a scenario where the disk passage of GCs can generate OCs, massive ones
in particular, as indicated by the orbit of Centauri and its impact site. As a consequence,
OC formation is not induced entirely by the spiral density wave mechanism in spiral arms.
3 Summary and conclusions
Globular clusters orbiting the bulge and halo of the Galaxy cross the disk on average
once every 1 Myr, and these events are expected to produce significant physical effects
on the disk. For instance, the impact of a GC passing through the disk can trigger
star formation either by the accumulation of gas clouds around the impact site or by the
production of an expanding mechanical wave. Time delays are
expected in both cases because of the collapse and fragmentation of molecular clouds before star
formation. This phenomenon was observed in the galaxy NGC 4559 (e.g., SCP05).
If this mechanism operates frequently in the Galaxy, the most massive
GC Centauri can be assumed to be an ideal projectile for analysing the state of its last
impact site in the disk.
Since Centauri collided with the Galactic disk
Myr ago, a major star-forming event
appears to have occurred close (
kpc) to the impact locus that generated two of the most
massive young OCs known in the Galaxy, BDSB 122 and Stephenson 2. We suggest a
connection between these events that is similar to that between the impact and shock observed in NGC 4559
(SCP05). We use a model of the Galactic potential to integrate the orbit of
Centauri.
As shown in Fig. 4, when the uncertainties in space velocity, distances, and
potential are considered, the error distributions of the
Centauri impact site and the birth-site of
Stephenson 2 overlap. This overlap suggests a scenario where the disk passage and formation of the
pair of OCs may be physically connected. Alternatively, the time coincidence may have occurred within
a separation
kpc. In such a case, the expanding bubble scenario such as that in NGC 4559
would apply. The latter case is more probable, since two clusters have
been formed.
Levy (2000) performed 2D hydrodynamic simulations to study the impact of GCs on the
Galactic disk in the presence of available gas. They found that the moving GC causes a shock
in the gas that propagates through the disk on a kpc scale, thus producing star formation.
Vande Putte & Cropper (2009) simulated in detail the effects of GC impacts on the disk,
basically confirming the results of Wallin et al. (1996) and Levy (2000), even in the absence of gas at the
impact site. They found a concentration of disk material compressed to a scale of pc,
which may subsequently attract gas leading to star formation. The compression increases with
the GC mass.
At this point, an interesting question arises. For a rate of GC impact per Myr,
a high probability is expected of one GC impact occurring within 1-2 kpc of any location
within the inner Galaxy in about 10 Myr. However, the star-formation efficiency of these
events appears to be low, according to Vande Putte & Cropper (2009), who found that of the 54 GCs with accurate proper
motions studied by them, only three appear to be associated with young OCs. It is possible
that conditions
such as GC mass and impact site properties, and the availability of molecular gas, temperature
and density, constrain the star-formation efficiency.
Evidence drawn from the present work suggests that GCs can be progenitors of massive OCs.
We have focused in particular on Centauri. Density-wave shocks may not be the only
cause of the formation of the more massive OCs, which is a possibility to be further explored,
both theoretically and observationally.
Acknowledgements
We thank the anonymous referee for suggestions. We acknowledge partial support from CNPq (Brazil).
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Footnotes
All Tables
Table 1: Present-day cluster positions.
All Figures
![]() |
Figure 1:
|
Open with DEXTER | |
In the text |
![]() |
Figure 2:
The present-day positions (and uncertainties) of Stephenson 2,
BDSB 122, and |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Top-left panel: galactocentric XY-plane projection of the |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Close-up of the impact site. Left panel: orbits computed with
|
Open with DEXTER | |
In the text |
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