A&A 484, 773-781 (2008)
DOI: 10.1051/0004-6361:200809447
W. H. T. Vlemmings
Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
Received 24 January 2008 / Accepted 30 March 2008
Abstract
Context. The role of magnetic fields during high-mass star formation is a matter of fierce debate, yet only a few direct probes of magnetic field strengths are available.
Aims. The magnetic field is detected in a number of massive star-forming regions through polarization observations of 6.7 GHz methanol masers. Although these masers are the most abundant of the maser species occurring during high-mass star formation, most magnetic field measurements in the high-density gas currently come from OH and H2O maser observations.
Methods. The 100-m Effelsberg telescope was used to measure the Zeeman splitting of 6.7 GHz methanol masers for the first time. The observations were performed on a sample of 24 bright northern maser sources.
Results. Significant Zeeman splitting is detected in 17 of the sources with an average magnitude of 0.56 m s-1. Using the current best estimate of the 6.7 GHz methanol maser Zeeman splitting coefficient and a geometrical correction, this corresponds to an absolute magnetic field strength of 23 mG in the methanol maser region.
Conclusions. The magnetic field is dynamically important in the dense maser regions. No clear relation is found with the available OH maser magnetic field measurements. The general sense of direction of the magnetic field is consistent with other Galactic magnetic field measurements, although a few of the masers display a change of direction between different maser features. Due to the abundance of methanol masers, measuring their Zeeman splitting provides the opportunity to construct a comprehensive sample of magnetic fields in high-mass star-forming regions.
Key words: masers - polarization - stars: formation - magnetic fields
Although massive stars play an important role in the chemical and energetic evolution of their host galaxies, their formation mechanism remains elusive. This problem is the topic of extensive observational and theoretical efforts. Even though few of the current simulations include magnetic fields, the influence of magnetism on the star formation processes is extensive as it can support a molecular cloud against collapse, affect core fragmentation and change the feedback processes (e.g. Krumholz & Bonnell 2007, and references therein).
Most current high-mass star formation magnetic field information comes
from H2O and OH maser polarization observations. The observations
of the H2O maser Zeeman effect using Very Long Baseline
Interferometry (VLBI) reveal field strengths between 10 and
600 mG, while the linear polarization measurements reveal a complex
but often ordered magnetic field morphology (e.g. Vlemmings et al. 2006a).
Aside from H2O masers, tracing high-density regions (
-1011 cm-3), the magnetic field in the less
dense surrounding regions is typically probed by polarimetric OH maser
observations (e.g. Bartkiewicz et al. 2005). These observations reveal
fields of a few mG as well as ordered structure in the magnetic
field. However, the strongest and most abundant of the high-mass star
formation region masers arises from the 6.7 GHz 51-60 A+methanol transition, and for this maser hitherto only very few
polarization observations exist.
Over
of the class II 6.7 GHz masers have been found to harbor
warm dust emission, even though only some of the masers are associated
with a detectable ultra-compact (UC) HII region
(e.g. Hill et al. 2005). This seems to indicate that the masers probe a
range of early phases of massive star formation. The 6.7 GHz masers
are likely pumped by a combination of collisions and emission from
nearby, warm (T>150 K) dust, but themselves arise from gas at much
lower temperature (T<50 K) with high hydrogen number densities
(
cm-3) and a high methanol abundance
(e.g. Sobolev et al. 1997; Cragg et al. 2005). Like H2O, methanol is a
non-paramagnetic molecule, and thus both the linear and circular
polarization fractions are small. The first polarization measurements
were made with the Australia Telescope Compact Array (ATCA) on the 6.7 GHz maser toward a handful of southern massive star-forming regions
(Ellingsen 2002) and linear polarization between few and 10% was detected.
The first high angular resolution linear polarization maps were
recently made using MERLIN (Vlemmings et al. 2006b) and the Long Baseline
Array (Dodson 2008). These observations indicate a typical linear
polarization fraction of
2-3%. In addition to the first linear
polarization measurements, a marginal possible detection of circular
polarization, caused by the Zeeman effect, was made for the masers of
the ON1 starforming region (Green et al. 2007).
This paper presents the first significant detection of Zeeman splitting in the 6.7 GHz maser transition for a sample of northern massive star-forming regions. The observations, data reduction and error analysis are discussed in Sect. 2 and methanol maser Zeeman splitting in Sect. 3. The results are given in Sect. 4 and are discussed in Sect. 5.
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Figure 1: Total intensity spectra ( bottom) and magnetic field strengths ( top) for six sources of our sample. The magnetic field strength is determined from the measured Zeeman splitting using the current best value for the 6.7 GHz methanol maser splitting coefficient. The Zeeman splitting is derived using the ``running'' cross-correlation method (see text). |
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The 6668.512 MHz (51-60A+) methanol maser line of a sample of
massive star-forming regions was observed on Nov. 12th 2007 using the
5 cm primary focus receiver of the 100-m Effelsberg telescope. The data were taken in
position switch mode with a 2 min cycle time. The full width at
half-maximum (FWHM) beam of the telescope is
120
at the maser
frequency. Data were collected using the fast Fourier transform
spectrometer (FFTS) using two spectral windows, corresponding to the
right- and left-circular polarizations (RCP and LCP). The spectral
windows of 20 MHz were divided in 16384 spectral channels,
resulting in a
0.055 km s-1channel spacing and were centered on
the local standard of rest (LSR) source velocities.
The data were reduced using the Continuum and Line Analysis
Single-dish Software (CLASS) package. The amplitudes were calibrated
using scans on 3C 123, 3C 286 and 3C 84. No special efforts were
undertaken to model short time-scale gain fluctuations during the
observations, however, the small gain difference between the RCP and
LCP was corrected. Small RCP and LCP gain differences do not affect
the Zeeman splitting determination when using the cross correlation
method, as with this method the Zeeman splitting measurements are not
reliant on accurate absolute fluxes. It is found that in general the
measured peak fluxes agree well with the literature values in the
methanol maser catalogue of Pestalozzi et al. (2005). From the literature
comparison and from a comparison of the measured flux of G9.62+0.20,
which is the target of regular monitoring, with the flux obtained on
Nov. 12th with the Hartebeesthoek radio telescope (Goedhart, priv. communication), the absolute flux errors are estimated to be 10%. Still, for a few sources the measured flux density is up to
different from the published values, which is likely due to
variability and/or structural changes in the maser themselves.
The sample was taken from the 6.7 GHz methanol maser catalogue by Pestalozzi et al. (2005) and consists of some of the strongest (>50 Jy) northern maser sources observable from Effelsberg. Priority was given to sources previously observed at high resolution or with existing OH/H2O maser polarization observations. To detect the Zeeman splitting the goal was to reach a signal-to-noise of >3000 and thus the total integration time per source was variable. As the observations were limited to 13 h, source selection also depended on observability and was occasionally adjusted based on the flux detected in a first observing scan. As a result, the noise level is different for each of the sources and ranges from 20 mJy to 100 mJy for each polarization.
The circular polarization fraction arising from the small Zeeman splitting of the paramagnetic methanol molecule, is extremely low (<0.5%). Detection of such small circular polarization fraction is very sensitive to an accurate relative calibration between the RCP and LCP signals. Zeeman splitting can be detected relatively straightforward using the cross-correlation method, described by Modjaz et al. (2005). This method directly determines the Zeeman splitting from the RCP and LCP data. It has been shown to be robust against the relative RCP and LCP gain calibration errors while still reaching a comparable sensitivity as performing S-curve fitting to the circular polarization spectrum. Also, essential for single dish work, it is able to measure Zeeman splitting in the case of spectrally blended maser features in a straightforward manner without the need for fitting a number of Gaussian components to identify individual maser features. It was for instance used on Green Bank Telescope data to determine limits on the Zeeman splitting for two H2O maser megamaser galaxies (Vlemmings et al. 2007; Modjaz et al. 2005).
As many of the sources will have blended maser features, and to reduce
the effect of remaining RCP and LCP gain calibration errors, the
Zeeman splitting is thus determined using the cross-correlation
method. Applying this method to the entire maser spectrum essentially
means that the resulting Zeeman splitting is a flux weighted average
of the true Zeeman splitting. To examine changes of the magnetic field
over the maser spectrum, one can perform the cross-correlation
analysis on sub-sections of the spectrum. In the case of these
observations, rms noise considerations limit the useful spectral range
over which the analysis can be applied to >3 km s-1. Thus, to describe
the magnetic field changes over the maser spectrum, cross-correlation
was done in the interval [(Vi-1.5), (Vi+1.5)] km s-1, with Vitaken along the spectrum at steps of 3 channel widths. Examples of
such ``running'' cross-correlation are shown in Fig. 1 with
only magnetic field values plotted that had >5significance. Special care has to be taken with velocity intervals
which are dominated by the wings of a bright emission peak. In this
case, remaining gain errors between RCP and LCP could create a
spurious Zeeman detection. Although a test with varying gain factors
indicates that the ``running'' cross-correlation is robust against cases
with a uniform gain error across the spectrum, small baseline
variations can still cause errors. Thus, only Zeeman determinations in
velocity intervals that included a separate maser feature (i.e. a
local flux maximum) in the inner 80% of the interval were taken to be
significant. It should be noted that, as the ``running''
cross-correlation effectively convolves the spectra down to a
3 km s-1 spectral resolution, apparent gradual magnetic field
variations are introduced when spectral features with a different
field strength are blended together. This gradual magnetic field
change between the maser features is thus not necessarily physically
the case in the maser region.
Although the analysis was performed using the cross-correlation
method, the circular polarization pattern as expected from Zeeman
splitting was detected for several of the least complex sources. The
magnitude of the circular polarization was
0.2%. Figure 2 shows an example of two sources. The
case of Cepheus A illustrates the problem with determining magnetic
fields from the circular polarization produced by such a complex
maser. Although the structure of the Cepheus A circular polarization
is similar to the total power derivative, it is extremely
difficult to properly distinguish the individual features.
Small amplitude non-Gaussian effects on the spectral baselines can
introduce an additional uncertainty in the Zeeman splitting
determination. To estimate this effect, Monte-Carlo modeling was
performed using artificially generated maser spectra with actual
baselines taken from emission free spectral regions for each of the
sources of the sample. It was found that typically the rms from the
cross-correlation Zeeman splitting calculations need to be increased
by 15% to accommodate this effect. This additional source of
error has been included in the errors quoted below.
The effect of a slight difference in the pointing center between the RCP and LCP, as a result of both feeds being off-axis, is called beam squint (e.g. Heiles 1996). Beam squint can mimic the effect of Zeeman splitting when a velocity gradient is present across extended emission of a spectral line, as the RCP and LCP telescope beam will then be probing gas at a slightly different velocity. This severely complicates the Zeeman splitting observations of extended thermal line emission and needs significant additional effort by rotating the feeds during the observations.
However, typically, individual maser features are not very
extended. Minier et al. (2002) found that the majority of the methanol
masers consist of a compact core with a diffuse halo structure of up
to a few hundred AU, corresponding to up to 100 mas. Even for the most
extended sources, such as W3(OH), where methanol maser emission
extends over several arcseconds, the bulk of the maser flux which
dominates the Zeeman splitting determination, comes from a region
smaller than 100 mas. The pointing difference between the Effelsberg
RCP and LCP receivers are
(e.g. Fiebig 1990). The effect of beam squint will be most
severe when the velocity gradient exists in the direction of the beam
off-set. Thus, during longer observation scans, any artificial
circular polarization signature will be quenched when the feeds rotate
under the source. However, as the observation scans were occasionally
as short as a few minutes, it was determined to what level beam squint
could contribute to the observed Zeeman splitting. Assuming the worst
case, a velocity gradient across the maser in the direction of the
RCP-LCP beam off-set, a broad maser spectrum of
5 km s-1 and a
maser extension of 100 mas, the contribution of the beam squint to
the Zeeman splitting is found to be less than 0.002 m s-1,
corresponding to 0.04 mG. The beam squint circular polarization
signature and the regular maser Zeeman splitting only becomes similar
if the maser would extend over more than 5
.
However, when an
extended maser region consists of individual compact maser features
that dominate the spectrum, the beam squint effect is negligible. It
can thus be concluded that the velocity splitting between RCP and LCP
measured for the 6.7 GHz methanol maser sources is not due to beam
squint.
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Figure 2: Total intensity and circular polarization spectrum for G37.40+1.52 ( left) and G109.86+2.10 (Cepheus A; right). The thick solid line in the bottom panel is best fit fractional total power derivative to the circular polarization spectrum. |
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The methanol molecule is non-paramagnetic and as a result the Zeeman
splitting under the influence of a magnetic field is extremely
small. The split energy,
,
of an energy level under the
influence of a magnetic field, B, is described by
.
Here MJ denotes the magnetic quantum number
for the rotational transition with the rotational quantum number J,
B is the magnetic field strength in Gauss,
is the nuclear
magneton and g is the Landé g-factor, which thus determines the
magnitude of the Zeeman effect. This factor was investigated many
years ago by Jen (1951), who found empirically that it is probably an
average of the true g-factor of several interacting states and can
be described by the equation:
g = 0.078 + 1.88/[J(J+1)]. | (1) |
There are several, non-instrumental, effects other than Zeeman
splitting that might cause circular polarization of the maser
line. One possibility is a rotation of the axis of symmetry for the
molecular quantum states. This can occur when, as the maser saturates,
the rate for maser stimulated emission R becomes larger than the
Zeeman frequency shift .
While
,
the magnetic
field direction is the quantization axis. Then, when R becomes smaller
than
,
the molecules interact more strongly with the
radiation field than with the magnetic field and the quantization axis
changes towards the maser propagation direction. From the Zeeman
splitting coefficient derived above,
s-1 for the 6.7 GHz methanol maser. The rate for
stimulated emission can be estimated using:
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(2) |
Alternatively, Wiebe & Watson (1998) have shown that the propagation of
strong linear polarization can cause circular polarization when the
direction of the magnetic field changes significantly along the maser
propagation direction. For a smooth change of magnetic field direction
of 1 rad along the maser, the fractional circular polarization
caused by this effect is approximately
,
where
is the
fractional linear polarization. For the typical 6.7 GHz methanol maser
linear polarization fraction of 2-3%, this implies that the
generated circular polarization is only
0.02%, which is less
than
of the observed circular polarization. And, the fairly
constant linear polarization vectors observed at high-resolution
(e.g. Vlemmings et al. 2006b), indicate that the magnetic field
rotation along the maser path length is likely much smaller than
1 rad, making the propagation of linear polarization an unlikely
source of the methanol maser circular polarization.
Finally, a velocity gradient in intrinsic circular polarization (i.e. not caused by the magnetic field) could mimic the effect of Zeeman splitting. However, as in a maser the stimulated emission quickly dominates the intrinsic emission, any intrinsic circular polarization quickly becomes negligible. This is described in more detail in e.g. Elitzur (1998).
Table 1: Zeeman splitting results.
The results of the Zeeman splitting analysis using the RCP-LCP
cross-correlation method are presented in
Table 1. The table lists the source name, position,
central
velocity, peak and integrated flux and the
measured Zeeman splitting
.
As described in Sect. 2.3,
this value corresponds to the flux averaged Zeeman splitting of the
entire maser spectrum. In the final column it lists the strength of
the magnetic field component along the line-of-sight (B||)
determined using the current best value of the 6.7 GHz methanol maser
Zeeman splitting coefficient as discussed in Sect. 3. Throughout
the paper, the quoted magnetic field strength will correspond to this
value. Should in the future a better value of the Zeeman coefficient
be determined then all magnetic field values need to be adjusted
correspondingly.
Figure 1 shows six methanol maser spectra and corresponding magnetic fields derived using the running cross-correlation method described in Sect. 2.3. The figure shows that for a number of the sources, the magnetic field changes across the maser. For those sources, Table 1 also lists separately the magnetic field derived for sub-sections of the spectrum. Total intensity spectra and magnetic field strengths for all the sources in the sample with a significant Zeeman detection are presented in the Online material as Figs. 6 and 7. Online Fig. 8 shows the total intensity spectra for the sources without Zeeman detection.
A number of the maser sources from the sample have been observed at high angular resolution, providing information on the morphology of the methanol maser region. Additionally, several sources have been the target of magnetic field measurements using mainly OH and/or H2O maser polarization observations. Sources for which high-resolution 6.7 GHz observations and/or additional magnetic field measurements are available are discussed here in detail.
The 6.7 and 12.2 GHz methanol masers associated with the high-mass
star formation complex G09.62+0.20 undergo periodic flares with a
period of 244 days, making these the first reported incidence of
periodic variations in a high-mass star-forming region
(Goedhart et al. 2004,2003). The origin of the periodic behavior,
however, is still unclear. The 6.7 GHz methanol masers have been
mapped with the ATCA by Phillips et al. (1998), and the strongest features
are shown to be associated with the hypercompact HII region
labeled E by Garay et al. (1993). This region also hosts OH masers for
which Zeeman splitting observations indicates a magnetic field
strength of 5 mG (Fish et al. 2005). As seen in Fig. 1,
the magnetic field determined from the 6.7 GHz methanol maser Zeeman
splitting reverses direction between the second-strongest maser
feature at
km s-1 (
B||=8.6 mG) and the strongest
feature at 1.2 km s-1 (
B||=-2.96 mG), even though the ATCA image
shows that the features are located within
100 mas of each
other. The periodicity of the flaring of both maser features is the
same, with the weaker of the two features flaring with a
1 month
delay. There is an intriguing possibility that the maser flaring and
time delay is the result of a periodic change in the magnetic field
orientation due to a form of magnetic beaming
(e.g. Gray & Field 1994). However, this hypothesis needs to be tested by
magnetic field monitoring observations and improved maser modeling.
This young massive star-forming region contains methanol, H2O and
OH maser emission as well as a weak hypercompact HII region. The
6.7 GHz methanol masers have been mapped with the ATCA and consist of two
regions separated by 1.5
(Walsh et al. 1997). The strong maser feature at
km s-1, which shows the smallest Zeeman splitting
(B||=4 mG) is located closest to the sub-millimeter continuum
peak imaged by, e.g., Beuther et al. (2005) at high-resolution with the
submillimeter array (SMA). The higher velocity features, with B||=12 mG, are located in the direction of the North-South molecular outflow found in the same SMA observations. The OH masers on
the other hand, are located in the direction of extended molecular emission in the East-West direction, which shows indications of a rotation signature perpendicular to the outflow (Beuther et al. 2005; Beuther & Walsh 2008). The magnetic field measured from OH maser Zeeman splitting is B=3.93 mG (Ruiz-Velasco et al. 2006).
The Zeeman splitting for this source, and consequently the magnetic
field, shows a very strong negative magnetic field for the brightest
maser peak at
km s-1 (
B||=-30.3 mG), while the
other maser features have a positive field direction with a strength
of
mG. In Fig. 1, this results in a
dip towards an increasingly negative magnetic field across the maser,
because, as described in Sect. 2.3, the running average calculates
the Zeeman splitting over a 3 km s-1 interval. Szymczak & Gérard (2004) find
a 1667 MHz OH maser feature with a magnetic field strength of
B=-0.2 mG at
km s-1. Unfortunately, no high
resolution maps are available to check the morphology of the maser
source.
The largest Zeeman splitting was measured for the masers of the UC
HII region G31.28+006, which is part of the giant HII
region W43, and correspond to B||=42 mG. The 6.7 GHz methanol
masers were observed with the European VLBI Network (EVN) and reveal a
complex distribution over
mas (Minier et al. 2000). No
other maser polarization observations are found in the literature.
As seen in Fig. 1, the magnetic field of this source is stable over the entire velocity range with a flux averaged strength of
B||=-18 mG. The only other magnetic field measurement for 33.64-0.21 comes from a single 1720 mG OH maser feature at
km s-1, which has B=-1 mG (Szymczak & Gérard 2004).
The methanol masers of the bipolar outflow source G35.20-074N have
only recently been mapped using the Japanese VLBI Network
(Sugiyama et al. 2007), showing that the brightest features make up two
compact regions separated by more than 2
in a direction
perpendicular to the CO outflow, along a putative molecular disc
(Dent et al. 1985). The Zeeman splitting observations indicate a stable
flux averaged magnetic field strength of
B||=16.5 mG, which is
likely dominated by the strongest maser feature at
km s-1 in the southern maser cluster. The OH maser
polarization of this source has been studied with MERLIN by
Hutawarakorn & Cohen (1999), who find that the magnetic field reverses on
opposite sides of the disc. The OH maser distribution is thought to
lie along the disc, with the southern masers tracing a mean field
mG and a northern maser feature having B=-2.5 mG.
The UC HII region G 35.20-1.74, in the Galactic HII region W48,
is believed to be a site of massive star formation and has both OH and
methanol masers. EVN observations of the
6.7 GHz methanol maser region shows a ring-like structure of
mas (Minier et al. 2000). Although the spectrum is
complex, the Zeeman splitting observations do not show any large
variations and yield a flux averaged field strength of
B||=6.4 mG. The magnetic field at the periphery of the UC H
II region has been determined from carbon recombination line
observations, which give a field of B=2.9 mG at a hydrogen number
density of
cm-3 (Roshi et al. 2005).
W51 is one of the most luminous massive star formation complexes of
our Galaxy and can be divided in three regions, W51A, W51B and W51C
(Carpenter & Sanders 1998). The maser site G49.49-0.39 is associated with
W51A and particularly with W51-e1/e2 (Caswell et al. 1995). OH maser
polarization observations reveal a total of 46 Zeeman pairs near e1
and e2, with the region having predominantly a positive magnetic field
direction which reverses in the northern part of e1
(Fish & Reid 2006). W51e2 has two Zeeman pairs that imply a magnetic field
of the order of 20 mG (Argon et al. 2002), with the rest of the OH
masers indicating
mG. For the 6.7 GHz methanol masers the
Zeeman splitting indicates a flux averaged
B||=14.7 mG.
The 6.7 GHz methanol maser emission and polarization was recently
mapped with MERLIN by Green et al. (2007). Those observations indicate
a tentative first detection of 6.7 GHz methanol maser Zeeman splitting
of m s-1, corresponding to a field strength of
-18 mG. This marginal detection could not be confirmed in the
observations presented here. However, the Zeeman splitting measured by
Green et al. was found on a maser feature that, in lower resolution
observations, would be blended both positionally and spectroscopically
with the brightest maser. As a results, the flux averaged Zeeman
splitting measurement is biased toward a possibly negligible
magnetic field of the brightest feature.
The 6.7 GHz methanol masers of the very active region of massive star
formation W75N have been mapped with the EVN (Minier et al. 2000). Their
map reveals that the masers make up two distinct regions, an elongated
region of 200 mas with
km s-1 and a compact
feature
500 mas South-East at
km s-1. The
observations shown in Fig. 1 highlight the distinct
nature of these maser features as the masers in the linearly extended
structure have
B||=5.7 mG while those in the compact region have
B||=9.5 mG. W75N has been the target of numerous OH maser
polarization observations indicating another possible disc related
field reversal and typical magnetic field strengths of
-7 mG (e.g. Slysh et al. 2002; Hutawarakorn et al. 2002). Magnetic
field measurements during a OH maser flare in W75N reveal the
strongest OH maser magnetic field B=40 mG to date (Slysh & Migenes 2006).
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Figure 3:
Magnetic field strength B in the massive star
forming region Cepheus A measured from Zeeman measurements as a
function of
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The masers of the Cepheus A massive star formation region has been
studied in great detail (e.g. Vlemmings et al. 2006a, and references therein). The 6.7 GHz methanol maser distribution has been mapped with the Japanese VLBI Network (Sugiyama et al. 2007) and the EVN
(Torstensson et al., in prep.). These observations show that the
masers are found in an elongated structure of 1500 mas across
Cepheus A HW2. The measured methanol maser magnetic field is stable at
B||=8.1 mG.
Cepheus A is the source in the sample for which the most magnetic
field measurements at different hydrogen density are
available. Figure 3 presents on overview of all these
measurements. It seems clear that the magnetic field strength B in
Cepheus A has a power-law dependence on the hydrogen number density
,
with the best-fit giving
.
This
is consistent with the empirical relation
from
low-density molecular cloud Zeeman observations by
Crutcher (1999). Of course, one has to be cautious when relating
the maser observations with the other Zeeman splitting results and the
dust polarization observations at very different scales. Additionally,
the methanol and H2O maser magnetic field strengths depend on an
assumption with regard to the angle between the maser propagation
direction and the magnetic field and their number density has to
be determined using maser excitation models.
The methanol masers of NGC 7538 have been proposed to trace a disk around a high-mass protostar (Pestalozzi et al. 2004), however, this interpretation has been questioned by De Buizer & Minier (2005) who find that the maser might be related to an outflow. The observations presented here indicate a flux averaged magnetic field
B||=16.2 mG. The ``running'' cross-correlation however, reveals a more complex picture. The spectrum is made up of several strong maser features
with apparently different magnetic field strengths. The strongest
magnetic field 16 mG is measured on the maser feature at
km s-1, while
12 mG is found for the maser at
km s-1. In both cases the ``running''
cross-correlation derived magnetic field is somewhat supressed as
the masers between
and -56 km s-1 have a field of
only a few mG. Meanwhile, no significant magnetic field is detected
in the masers near
km s-1, implying a field strength
mG. The flux averaged magnetic field is
marginally larger than the field determined using the ``running''
cross-correlation for individual maser features. This is due to the
fact that, in determining the flux averaged field strength, strong
fields, which have nevertheless <
significance in the
smaller 3 km s-1 intervals used for the ``running'' cross-correlation,
still contribute. OH maser measurements indicate the region
undergoes a field reversal and has |B|=1 mG (Fish & Reid 2006).
Linear polarization of the 6.7 GHz methanol masers of W3(OH) is described in Vlemmings et al. (2006b), who also give a compilation of previous OH maser magnetic field strength measurements. The polarization observations show that the magnetic field traces the extended methanol filament but has a more complex structure in the dominating compact region described in Harvey-Smith & Cohen (2006). The Zeeman splitting presented here corresponds to a flux averaged magnetic field strength of B||=2.87 mG. However, due to the rich spectrum and large extent of W3(OH) a direct comparison with other Zeeman splitting measurements is impossible and would need high resolution observations.
Significant Zeeman splitting was detected for 17 out of 24 sources and
indicates an absolute magnetic field strength component |B|||along the maser propagation direction between 2.8 and 42 mG. There
are several effects that bias the observed field strength towards
higher or lower values. As is the case for H2O masers, low spatial
resolution observations, velocity gradients across
the maser and increased maser saturation tend to cause an
underestimate of the magnetic field strength (Vlemmings 2006; Sarma et al. 2001). As discussed above, beam squint can create a false
Zeeman splitting signature, however, for milliarcsecond-scale masers
this is unlikely to contribute more than 0.04 mG. Finally, the
Zeeman coefficient which is used to determine the magnetic field is
uncertain, as is described in Sect. 3, which leads to a
systematic bias in the magnetic field. Thus the uncertainty in the measured
absolute magnetic field strength will be substantial, with most of the
described effects biasing it towards a value that is lower than the
actual field strength. Weighing the field strength by measurement
significance, the average magnetic field
mG. This needs to be corrected for a random angle between
magnetic field and the line-of-sight, which implies for the absolute field strength
(e.g. Crutcher 1999). This
gives
mG. The error on the
absolute field strength is dominated by the estimated uncertainty in the Zeeman
coefficient. This field strength is larger than that found in
the OH maser regions, with the average OH maser determined field strength
being
4 mG (Fish & Reid 2006).
The dynamical importance of the magnetic field can be quantified by
defining a critical magnetic field strength
for which the dynamic and magnetic pressure are
equal. Here
and v are the density and velocity of the maser
medium respectively. Cragg et al. (2005) find that the current
observational limits suggest that the majority of the 6.7 GHz maser
sources occur near the high-density limit of the maser range
(
-109 cm-3), with a typical value of
cm-3. Taking this density and a typical gas
velocity of
5 km s-1 from proper motion measurements
(e.g. Xu et al. 2006),
mG. The measured
magnetic field vales are thus comparable to
and hence
dynamically important.
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Figure 4: Measured flux averaged 6.7 GHz methanol maser magnetic field strength vs. average 1.6 and 6 GHz OH maser magnetic field strengths for those sources where both are available. Most literature values were taken from the compilation of molecular cloud magnetic field measurements by Han & Zhang (2007). |
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Theoretical modeling indicates that, given sufficient abundance, both 1.6 and 6 GHz OH masers as well as the methanol masers can be pumped simultaneously (Cragg et al. 2002). However, observations have shown that, although they are closely associated, co-propagation between OH and methanol masers is rare (e.g. Etoka et al. 2005). Still, as the masers are closely related, one might expect a relation between the OH magnetic field strengths and those derived from the methanol masers. As seen in Fig. 4, no clear relation is found for those sources which have magnetic field strength measurements from both maser species. This is likely due to the fact that the flux averaged methanol maser magnetic field strengths cannot be easily related to the OH maser measurements often performed at much higher resolution.
Figure 4 does, however, show that the magnetic field directions determined from methanol and OH masers are fully consistent. As discussed for some of the individual sources, this even holds for regions where the OH masers show a magnetic field reversal. This implies that the magnetic field orientation derived from the methanol maser regions, as that from OH masers, could be indicative of the Galactic magnetic field. This is illustrated in Fig. 5, although a much larger number of measurements as well as accurate distances to the star-forming regions would be needed. Since several efforts are underway to determine accurate distances to methanol maser regions (e.g. Xu et al. 2006), methanol maser Zeeman splitting measurements will provide an important opportunity to study the Galactic magnetic field (e.g. Han & Zhang 2007).
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Figure 5: Magnetic field direction and strength along the line-of-sight derived from the methanol maser Zeeman splitting observations presented in this paper projected onto the Galactic plane. The solid dots are the observed star-forming region with kinematic distances from Pestalozzi et al. (2005). These are known to be highly uncertain. The length of the vectors is scaled with B||. The approximate location of the spiral arms is indicated as taken from Taylor & Cordes (1993). |
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Figure 3 shows the B-field measurements of both maser
and non-maser Zeeman observations as a function of hydrogen number
density. The figure seems to indicate that the B-field follows the
density scaling law discussed in
e.g. Mouschovias & Ciolek (1999) over an enormous range of densities. This makes
the maser measurements consistent with low-density molecular cloud
measurements (Crutcher 1999), implying that the magnetic field
remains partly coupled to the gas up to the highest number
densities. However, some care has to be taken in interpreting this
relation, as for instance the shock excited masers are short-lived
(H2O masers have a typical lifetime
s) compared
to the typical ambipolar diffusion time-scale at the highest densities
(
s). This suggests that in the non-masing gas of
similar densities, magnetic field strengths are likely lower due to
ambipolar diffusion. Still, the maser magnetic field measurements
strongly imply a dynamical importance of magnetic fields during the
high-mass star formation process, with the methanol maser observations
presented here filling the gap between the OH and H2O maser
observations.
This paper presents the first significant Zeeman splitting
measurements obtained on the 6.7 GHz methanol maser. As this highly
abundant maser uniquely pinpoints massive star formation, a detection
of the Zeeman splitting gives the opportunity to measure the magnetic
field in a large number of high-mass star-forming regions at densities
of
cm-3. The average line-of-sight magnetic
field in the methanol maser region
mG, although this depends on the exact Zeeman
coefficient used to calculate the field strength as discussed in
Sect. 3. A statistical correction for a randomly oriented
magnetic field gives
mG. This indicates that the
magnetic field is dynamically important. The 100-m Effelsberg
telescope observations presented here, detected significant magnetic
fields in 70% of the sources with peak fluxes down to
50 Jy. Thus, with additional observations it will be possible to
construct a catalogue of magnetic field measurements for over 100
high-mass star-forming regions giving unique insight in Galactic
magnetic fields.
Acknowledgements
W.V. thanks A. Kraus for his help setting up the Effelsberg observations, S. Goedhart for making available her most recent G09.62+0.20 monitoring results and V. Migenes and V. Slysh for providing details on the IRAS 18089-1732 OH maser observations. W.V. also thanks the referee for comments that have greatly improved the paper.
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Figure 6: Total intensity spectra ( bottom) and magnetic field strength ( top) for all the sources of our sample with significant Zeeman splitting detection. The magnetic field strength is determined from the measured Zeeman splitting using the current best value for the 6.7 GHz methanol maser splitting coefficient. The Zeeman splitting is derived using the ``running'' cross-correlation method (see Sect. 2.3). |
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Figure 7: As Fig. 6. |
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Figure 8: Total intensity spectra of the sources in our sample for which no significant Zeeman splitting was detected. |
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