The Collimated Jet Source in IRAS 16547-4247

The Collimated Jet Source in IRAS 16547-4247: Time Variation, Possible Precession, and Upper Limits to the Proper Motions Along the Jet Axis

Luis F. Rodríguez Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72, Morelia, Michoacán, 58089 México    James M. Moran and Ramiro Franco-Hernández111Centro de Radioastronomía y Astrofísica, UNAM, Morelia 58089, México Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA jmoran,    Guido Garay Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile    Kate J. Brooks Australia Telescope National Facility, P.O. Box 76, Epping NSW 1710 Australia    Diego Mardones Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile

The triple radio source detected in association with the luminous infrared source IRAS 16547-4247 has previously been studied with high angular resolution and high sensitivity with the Very Large Array (VLA) at 3.6-cm wavelength. In this paper, we present new 3.6 cm observations taken 2.68 years after the first epoch that allow a search for variability and proper motions, as well as the detection of additional faint sources in the region. We do not detect proper motions along the axis of the outflow in the outer lobes of this source at a 4- upper limit of 160 km s. This suggests that these lobes are probably working surfaces where the jet is interacting with a denser medium. However, the brightest components of the lobes show evidence of precession, at a rate of yr clockwise in the plane of the sky. It may be possible to understand the distribution of almost all the identified sources as the result of ejecta from a precessing jet. The core of the thermal jet shows significant variations in flux density and morphology. We compare this source with other jets in low and high mass young stars and suggest that the former can be understood as a scaled-up version of the latter.

To appear in The Astronomical Journal

1 Introduction

A successful model of low-mass star formation, based on accretion via a circumstellar disk and a collimated outflow in the form of jets (Shu, Adams, & Lizano 1987), has been developed and found to be consistent with the observations. An important question related to star formation is whether or not this model can be scaled up for the case of high-mass protostars or if other physical processes (i.e., stellar merging; Bonnell, Bate, & Zinnecker 1998; Stahler, Palla, & Ho 2000; Bally & Zinnecker 2005) are important. A small number of B-type young stars have been found to be associated with collimated outflows and possibly even circumstellar disks (see Garay & Lizano 1999; Arce et al. 2007; Cesaroni et al. 2007). The source IRAS 16547-4247 is the best example of a highly-collimated outflow associated with an O-type protostar studied so far, and its study may reveal important information about the way high mass stars form.

The systemic LSR velocity of the ambient molecular cloud where IRAS 16547-4247 is embedded is 30.6 km s (Garay et al. 2007). Adopting the galactic rotation model of Brand & Blitz (1993) and assuming that the one-dimensional rms velocity dispersion among molecular clouds is 7.8 km s (Stark & Brand 1989), we estimate a distance of 2.90.6 kpc for the source. IRAS 16547-4247 has a bolometric luminosity of 6.210 , equivalent to that of a single O8 zero-age main-sequence star, although it is probably a cluster for which the most massive star would have slightly lower luminosity. Garay et al. (2003) detected an embedded triple radio continuum source associated with the IRAS 16547-4247. The three radio components are aligned in a northwest-southeast direction, with the outer lobes symmetrically separated from the central source by an angular distance of , equivalent to a physical separation in the plane of the sky of 0.14 pc. The positive spectral index of the central source is consistent with that expected for a radio thermal (free-free) jet (e.g., Anglada 1996; Rodríguez 1997), while the spectral index of the lobes suggests a mix of thermal and nonthermal emission. Forster & Caswell (1989) detected both mainline OH and HO masers at a position close to the central continuum source. The triple system is centered on the position of the IRAS source and is also coincident within measurement error with a 1.2 mm dust continuum and molecular line emission core whose mass is on the order of 10 (Garay et al. 2003). Brooks et al. (2003) reported a chain of 2.12 m emission knots that trace a collimated flow extending over 1.5 pc that emanates from close to the central component of the triple radio source and has a position angle very similar to that defined by the outer lobes of the triple radio source. Most likely this extended component traces gas ejected in the past by the central component of the triple source. The molecular observations of Garay et al. (2007) revealed the presence of a collimated bipolar outflow with lobes 0.7 pc in extent and aligned with the thermal jet located at the center of the core.

In a high angular resolution study made with the VLA and ATCA, Rodríguez et al. (2005) confirmed that the central object is a thermal radio jet, while the two outer lobes are most probably heavily obscured HH objects. The thermal radio jet was resolved angularly for the first time by these authors and found to align closely with the outer lobes. Several fainter sources detected in the region away from the main outflow axis were interpreted as most probably associated with other stars in a young cluster. Brooks et al. (2007) used ATCA observations to substantiate the jet nature of the central source and to detect emission at 88 GHz that most probably arises from dust associated with this source.

In this paper, we present new sensitive high angular-resolution Very Large Array observations that provide new information on the characteristics of the radio triple source in IRAS 16547-4247 as well as other sources in the field.

2 Observations

The new 3.6-cm wavelength observations were made using the Very Large Array (VLA) of the National Radio Astronomy Observatory (NRAO)222NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.. These VLA radio continuum observations were carried out in 2006 May 31 and June 08 at the frequency of 8.46 GHz. The array was in the BnA configuration and an effective bandwidth of 100 MHz was used. The absolute amplitude calibrator was 1331+305 (with an adopted flux density of 5.21 Jy), and a source model provided by NRAO was used for its calibration. The phase calibrator was 1626298, with bootstrapped flux densities of 1.6840.003 and 1.8230.004 Jy for the first and second epochs, respectively. The phase center of the array was and (J2000.0). The data were edited and calibrated using the software package Astronomical Image Processing System (AIPS) of NRAO. To correct for amplitude and phase errors caused by the low elevation of the source, the data were self-calibrated in phase and amplitude. No significant variations were found between the two epochs of observations (separated by only eight days) and the final analysis was made from the result of concatenating all data. The average epoch for the two data sets is 2006.42, which we use in subsequent analysis. Clean maps were obtained using the task IMAGR of AIPS with the ROBUST parameter set to 0. The synthesized (FWHM) beam was . The noise level achieved in the final image was 23 Jy beam.

The 3.6-cm wavelength archive data was taken on 2003 September 25 and 30 (epoch 2003.74) in very similar conditions to those of the new observations and the resulting beam was . This old data set is described in Rodríguez et al. (2005). These data were cross-calibrated in phase and amplitude using the 2006.42 epoch as the model, which serves to globally minimize the differences in positions and flux densities of the sources. The absolute flux density error is estimated to be 10%.

3 Results and Discussion

To allow a more reliable comparison between the two epochs, both images were convolved to the same angular resolution (). To improve the relative gain calibration between the two epochs we examined the relative strengths of the 13 sources we identified in the images. It is clear that the ratios of the flux densities of all the sources except S-1 and N-1 had the same constant value of 0.910.02. Hence, we adjusted the flux scale of the first epoch by this relative gain factor. Figure 1 shows the corrected ratio of the flux densities of all the sources. The reduced of the estimate of the gain constant is 0.76, which suggests that the flux density errors may be slightly overestimated by about 15 percent. Since the is close to unity we conclude that there is no evidence for variability among the 11 sources, whereas the changes in flux densities of S-1 and the jet are highly significant. Figure 2 shows contour images of the emission observed at 8.46 GHz in the two epochs, as well as the difference image (2006.42 - 2003.74). The positions, flux densities, and deconvolved angular sizes of the sources identified in Fig. 2 are given in Table 1. The observed parameters for each component were determined from a linearized least-squares fit to a Gaussian ellipsoid function using the task JMFIT of AIPS. In Table 2 we summarize the parameters of the proper motions of all sources in the field, derived from differences of the positions in the two epochs. Note that the position of the jet changes slightly between the epochs by about 6 mas in each coordinate (). We do not attach any significance to this shift. If we aligned the jet positions, the proper motions listed in Table 2 would change by about 2 mas yr. This amount is insignificant and does not change any of our conclusions.

We note that the faint features that appear marginally detected at the 4- level in the images of the individual epochs (for example, some faint structures to the west of the central source in the 2006.42 image), do not appear in the difference image, since this is about noisier than the individual images.

As already discussed by Rodríguez et al. (2005), the lobes first observed by Garay et al. (2003) break into several components. A more careful examination of the 2003 map in conjunction with the 2006 map shows that there are two other components present in the northern lobe (components N-4 and N-5; see Table 1 and Figure 2), as well as two additional field sources (sources D and E, see Table 1).

In this section we will discuss the sources individually when new information was found, and in the following section we focus on the search for variability and proper motions. Most of the interpretation is in the context of a jet and bipolar outflow. The position angle of the jet is , whereas the PA of the CO lobes is about and the PA of the line joining N-1 and S-1 is . We adopt a nominal angle for the jet outflow of .

3.1 The central jet source

An important difference with respect to the analysis of Rodríguez et al. (2005) is that we recognize the presence of a compact source (source D) very close to the jet source (see Fig. 2), about to its NW. To obtain the parameters of the jet and of source D separately we fitted simultaneously two Gaussian ellipsoids to this region of the image. The jet parameters for the two epochs discussed are given in Table 1. We note that the consideration of source D in the fitting procedure results in somewhat smaller deconvolved dimensions for the minor axis of the jet than obtained in Rodríguez et al. (2005). We assume that the opening angle of the thermal jet is the angle subtended by the deconvolved minor axis at a distance of one-half the deconvolved major axis (Eislöffel et al. 2000). Using the average of the deconvolved angular dimensions given in Table 1, we then estimate the opening angle of the thermal jet to be 15 (as opposed to the value of 25 derived by Rodríguez et al.), indicating significant collimation in this massive protostar. This result suggests that jets from high mass young stars can be as collimated as those found in lower mass objects, where HST studies indicate opening angles in the range of tens of degrees in scales of tens of AU from the star (Ray et al. 2007). On larger physical scales the optical jets from low mass young stars are known to show recollimation, resulting in opening angles of a few degrees (Ray et al. 2007). This recollimation is not evident in the thermal radio jets, which are usually detected only close to the star.

3.2 The northern lobe

As noted before, we identify two additional components (N-4 and N-5) in this lobe, indicating an almost continuous sequence of knots between the central jet and the outermost N-1 component (see Fig. 2). The sequence of five knots, N-1 to N-5, shows a gentle monotonic curvature that may be indicative of precession (see Section 5). Four of the five knots are resolved angularly, and it is interesting to note that all four have position angles consistent with . This result suggests that they are part of the northern outflow. This orientation does not seem to be valid for component S-1, as discussed in the next subsection. The N-1 and N-2 continuum components are the only ones in the whole region that appear to be associated with class I methanol masers (Voronkov et al. 2006).

3.3 The southern lobe

Only the component S-1 is clearly resolved, but in contrast to the components of the northern lobe that have intrinsic position angles consistent with , the southern lobe’s intrinsic position angle is . The misalignment between the intrinsic position angle of S-1 and the outflow axis, suggests that more than part of the main jet body, S-1 could be its working surface (e.g., Chakrabarti 1988) to the south. As we will see below, the time variability of this component could support this interpretation. On the other hand, the presence of an additional component (S-2) downstream suggests that our interpretation of S-1 as a working surface may be incorrect, or that S-2 is an independent source associated with a star. The fact that S-2 is unresolved is consistent with this interpretation.

3.4 Source A

This source is clearly resolved. It appears to be part of a diffuse region of emission that connects with the brighter component of the northern lobe. Source A could actually be part of the outflow, either if the outflow is less collimated and the ionized gas preferentially highlights regions where the flow is interacting with dense ambient material or if source A is part of the northern flow being deflected to the east by interaction with a dense clump of gas. The second possibility is interesting and it may be related to the fact that components N1 and N2 are the only ones in the region showing methanol maser emission. It is possible that the methanol maser emission is being stimulated by the deflection of the jet, as it interacts with N1 and N2. Finally, the position of source A could be understood if the outflow has precession (see discussion in Section 5). High angular resolution observations of a tracer of dense molecular gas are needed to advance our understanding of this source.

3.5 Source D

Source D is the faint source located to the NW of the jet, and first identified as an independent source here. It is unresolved angularly and may probably trace an independent star. In the 2006.42 image, it shows a faint extension to the west.

3.6 Source E

Source E is a barely detected source located about to the east of the core of IRAS 16547-4247. It is located outside of the region shown in Figure 2, and is unresolved in angular size. A contour image of this source is shown in Figure 3. The a priori probability of finding a 3.6 cm background source with a flux density of 0.14 mJy (the average flux density of the two epochs) in a solid angle of is only 0.003 (Windhorst et al. 1993). We conclude that this radio source most probably traces a young star embedded in this region.

4 Search for variation and proper motions

Analysis of Figure 2 and Table 1 indicates that significant flux density or morphological variations are observed only in three sources: the jet source, N-1, and S-1. This is not unexpected, since these are the three brightest sources in the field and small variations in position or flux density are not evident in weaker sources where the signal-to-noise ratio is much smaller. In the case of N-1 the variation is only in position since the flux density remained constant and the flux density variations are evident only for the jet source and S-1. We will discuss our interpretation of the observed variabilities and proper motions in the following subsections.

4.1 The central jet source and source S-1

The jet source seems to have increased its flux density by about 10% between the two epochs (see Table 1 and Figure 1). This difference is consistent with the fact that both thermal jets (Rodríguez et al. 2001; Galván-Madrid, Avila, & Rodríguez 2004) and HH knots (Rodríguez et al. 2000) can show small but statistically significant flux density variations on scales of years or even months. The difference image (Figure 4) suggests that the increase in emission comes from two discrete positions. One increase (of about 0.8 mJy) is unresolved and associated with the central source and we attribute it to an increase in mass loss at the core of the jet. The second increase (of about 0.4 mJy) comes from an unresolved component clearly displaced to the SE, and located at , at from the center of the jet. The OH maser emission detected by Caswell (1998) is close to the unresolved component associated with this second increase. We can think of three interpretations for this localized flux density increase. One is that we are observing a time-variable source powered by an independent star. There are two arguments against this interpretation: the first is that the sources in this region in general show little variation (see Table 1) and the second is that the source lies exactly in the path of the outflow, suggesting a relation with the jet. This latter fact suggests a second interpretation: we are seeing a discrete, new ejecta from the jet. This interpretation, on its turn, has several difficulties. The first is that, while a similar phenomenon was observed and monitored in the jet associated with HH 80-81 (Martí, Rodríguez, & Reipurth 1995; 1998), in this source the ejection was clearly bipolar, while in IRAS 16547-4247 we would have to consider a monopolar ejection. The second problem is related to the large velocity required for the ejection to move over in 2.68 years or less, that at a distance of 2.9 kpc implies the unlikely velocity of  km s or more. Finally, a third possibility is that we are observing the brightening of the jet flow as it interacts with dense gas in its path. Observations of higher angular resolution are required to disentangle the nature of the variations seen in the jet source. Unfortunately, the present observations are the best that it can be done now and possibly for decades (until completion of the Square Kilometer Array). The source can be observed, but with lower angular resolution, with ATCA (as already done) but it cannot be observed from the latitude of the future e-MERLIN. Finally, the emission is thermal and not easily detectable with VLBI arrays.

The source S-1 is the one with the largest flux density variation, with an increase of 40% (see Figure 1 and Table 1) between the two epochs. We believe that this large increase is related to our suggestion that S-1 may be a working surface of the jet, where kinetic energy is rapidly being dissipated and changes are expected.

4.2 Lack of Proper Motions Along the Jet Axis

The proper motions of the prominent components N-1 and S-1 along the nominal jet axis of are and mas yr, respectively. These motions correspond to inward motions of 28 and 42 km s, respectively, and are not statistically significant. The weighted average radial motion of all the components is mas yr, corresponding to km s. We adopt a conservative 4- upper limit on the proper motion of 160 km s. This upper limit is not very stringent, but certainly indicates that the IRAS 16547-4247 lobes are not moving as fast as the knots observed in the jets associated with the massive young stars HH 80-81 and Cep A HW2, where velocities in the plane of the sky of 500 km s have been reported (Martí, Rodríguez, & Reipurth 1998; Curiel et al. 2006).

4.3 Proper Motions in the Direction Transverse to the Jet Axis

The only components that show transverse motions to the nominal jet direction of degrees above the 4- level are N-1 and S-1 (see Table 2). These motions are and  mas yr, corresponding to clockwise transverse motions of and km s, respectively. The discovery of transverse (clockwise) motion, with no radial motion, was unexpected.

The total flux density of component N-1 hardly changed, and the difference images shown in Figures 2 and 5 clearly show the negative-positive residuals characteristic of a moving source with constant flux density. In contrast, the negative-positive signature of proper motion is not present in the case of S-1 (see Figures 2 and 6) because during the same period there was the strong brightening previously discussed that dominated the difference image.

5 A Precession Model for IRAS 16547-4247

We believe that it may be possible to understand the distribution of almost all the identified sources as well as the clockwise precession as the result of ejecta from a precessing jet of stellar origin. The gently curved and antisymmetric distribution of the radio components strongly suggests such a model. The basic idea is that the jet itself is not observed directly (because of the lack of radial motion in the outflow). Rather the observed sources are the result of the jet interacting with the ambient medium. We describe this model in simple empirical terms. We assume that the axis of symmetry is along the N-S direction and that the position angle (measured East of North) of the precession axis is given by

where is the amplitude of precession, is the precession rate and is the position angle at . We assume that the time scale of the observable outflow phenomenon is much shorter than the precession period. Hence, over a short period the precession position angle changes linearly,

The coordinates in the plane of the sky at the time of our observations, , for the location of gas ejected from the star at time will be

where is the precession angle at the time of emission, and is the radial position of the ejecta, . We assume that the ejection velocity, , is constant. Since we obtain

The prediction of this simple model is that is linearly related to , that is

Figure 7 shows the position angle of each component plotted versus its radial offset from the center of the jet component, which we identify as the origin. Source C deviates from the straight line fit to the data by about 19. We assume that it is not part of the jet, but a separate entity from the jet, perhaps evidence of another nearby star. The straight-line fit of equation 7 to the remaining 9 sources gives parameters, (the current PA of the jet), and degrees/arcsecond. For a distance of 2.9 kpc the value of in the source frame is 9.2 radians/cm or 2.9 radians/pc. Since the jet seems to be precessing linearly with time, we assume that the precession period is much greater than the time scale of the flow. Note that we cannot solve separately for the precession rate and the ejection velocity. The shape of the jet at the current epoch, as determined by equations 5 and 6, is shown in Figure 8.

As noted before only two sources have significant proper motions, N-1 and S-1. Their motions are both in the transverse direction to the direction of the jet, whereas their motions along the jet are insignificant (see Table 2). Hence, we assume that the sources are caused by the interaction of the jet and clumps of ambient material as the jet sweeps across the clumps. In this model, the clumps will have apparent transverse velocities given by

which, with the observed value of , becomes

The proper motion measurements of all the sources are listed in Table 2. We believe that the apparent motions of source C could be due to the presence of an additional, time-variable component to the NW of the main component of source C (see Fig. 2). Source N-4 shows proper motions that are slightly below 4- (see Table 2). However, these marginal proper motions are against the expected flow of the jet and, if real, are probably due to a “Christmas tree” effect more that to a real motion.

The velocity vectors of S-1 and N-1 are nearly transverse to the jet direction, and agree in direction with the sense of precession of the jet (see Fig. 8). These velocities are 180 and 220 km s, respectively. Since N-1 and S-1 both have about the same radial distance, we cannot confirm the expected linear trend in transverse velocity with radius predicted by eqn. 8. However, with these two data points we estimate from eqn. 9 that the ejection velocity is  km s. If we assume that we are indeed dealing with a working surface, the lack of proper motions (160 km s) allow us to estimate the ratio between the density of the medium and the density of the jet. Using the formulation of Raga, Rodríguez, & Cantó (1997), the ratio of ambient medium density, , to jet density, , is

where and are the jet and working surface velocities, respectively. For a jet velocity of 490 km s and an upper limit of 160 km s for the velocity of the working surface, we obtain 4.

The precession rate of the jet is . Hence with degree/arcsecond, and v =  km s, degrees/year. Note that the measurements of and v are both 6- results, but the measurement of is a 4- result. The precession period of the jet is , which for a precession opening angle of 30, would be about 5500 years. Since the range in PA among the components is about 25 (see Fig. 7), the jet travel time to outer components is about 300 years.

We might expect that the sources excited by the passing jet would persist after the jet moves on. However, there is no evidence (see Fig. 8) of structure in the transverse direction in any of the sources. This absence of “trails” suggests that the decay times for emission must be less than years, which would produce an extension of 1.5 at the radius of sources N-1 and S-1. The recombination time for an H II region with electron density is estimated as

The spectral index of N-1 indicates it is probably a thermal optically thin HII region (Rodriguez et al. 2005). Using the values for the flux density and size in Table 1 we estimate a emission measure of cm pc and the electron density as cm. Using this value for the electron density in eqn. (10) we find a recombination time for the N-1 component to be about 11 years. This time is an order of magnitude smaller than that required for the jet to leave an observable transverse trail.

For the S-1 source the emission may have a nonthermal component (Rodriguez et al 2005). The density of relativistic electrons, , and magnetic field, , can be estimated using eqns. (2) and (3) from Garay et al. (1996)

where and are the maximum and minimum energies of the relativistic electrons that we assume are and eV respectively. For the distance kpc and arcsec, we get mG and a density of relativistic electrons of cm. The decay time is given by Krolick (1999) as sec with in Hz and in G, or for our frequency. Using the value derived above for we get yr, which is much too long. A magnetic field of 30 mG would be required to achieve a synchrotron decay time of 100 years.

Franco-Hernández et al. (2008, in preparation) have discovered two linear structures traced by water vapor masers on the mas scale. Their g2 group of maser has a PA of about , which is 13 away from the current PA of the proposed precessing source (). Another group of masers (g1) has a position angle of about 50. If these masers were in a disk, their pole PA would be , close to the current precession angle. Hence these masers may be associated with the precessing excitation source.

The larger scale CO lobes are offset from the jet by about 15” along a PA of about . The line of sight velocity with respect to the ambient cloud is about 30 km s. These lobes could also be associated with the precessing source. The expected PA for emission at 15” from eqn. (7) would be about , close to the observed value. If the molecular flow picks up the full jet velocity of 490 km s, then the inclination would be about 90 – arctan (30/490), or about 86, very close to the value inferred from the analysis of the velocity structure of the CO lobes (Garay et al 2007). More realistically, the molecular flow velocity will be smaller, implying a smaller inclination angle.

The precession model nicely accounts for the fact that the line from N-1 to S-1 does not intercept the known jet. However, if the angle of the driving precessing source is currently , it is significantly discrepant with the PA of of the known radio jet. A possible explanation for this discrepancy might be that the central source is really a binary stellar system. Source I would be a non-precessing source associated with the known jet, which is related to the large scale CO outflow with about the same PA. Source II would be a precessing source which drives the continuum thermal sources and may be associated with the water masers and also the large scale CO outflow.

6 Putting the IRAS 16547-4247 Jet in Context

How does the IRAS 16547-4247 jet compare with other jets found in regions of star formation? Anglada et al. (1992) have compared the centimeter radio luminosity (taken to be proportional to the flux density times the distance squared, ) of thermal jets associated with low mass young stars with the momentum rate () in the associated molecular outflow. For 16 sources studied, they conclude that these low mass objects can be fitted with a power law of the form , where is in yr km s, is in mJy and is in kpc. In Figure 9, we plot the data used by Anglada et al. (1992). They interpret the fit to be in agreement with a simple model in which the observed ionization is produced by shocks (Curiel, Cantó, & Rodríguez 1987; Curiel et al. 1989), where about 10% of the energy in the jet is thermalized. We have plotted in the same figure, the three best studied cases of thermal jets associated with massive young stars: IRAS 16547-4247, HH 80-81, and Cep A HW2, using the data listed in Table 3. Remarkably, these three data points fall reasonably well on the Anglada et al. correlation. We believe that this agreement suggests that the jets associated with massive young stars may be a scaled-up version of the phenomenon seen in low mass young stars, although a firmer conclusion requires the study of a larger sample of objects than now available. Note that the intrinsic radio luminosity of the IRAS 16547-4247 jet is about larger than the typical radio luminosity of jets associated with low mass stars, and that it is the most luminous case known.

7 Conclusions

Our main conclusions follow:

1) We present new, sensitive 3.6-cm wavelength VLA observations of the multiple radio source associated with the luminous infrared source IRAS 16547-4247, the most massive example known of a thermal jet found in association with a forming star. The main purposes of these new observations were to search for variability and proper motions as well as to detect additional faint sources in the region. We detected four new components (N-4, N-5, D, and E) in the region;

2) We do not detect proper motions along the axis of the flow in the outer lobes of this source at a 4- upper limit of 160 km s, suggesting that if these lobes are the working surfaces of the jets and the jet velocity is 490km s, the ambient medium is at least four times as dense as the jet;

3) The brightest components of the lobes, sources N-1 and S-1, show evidence of clockwise precession, at a rate of yr in the plane of the sky;

4) A precessing model can account for the antisymmetric distribution of most of the sources in the field, as well as for the evidence of precession in sources N-1 and S-1;

5) The thermal jet at the core of the region shows significant variations in flux density and morphology but our angular resolution is insufficient to reach a clear conclusion on what produces these changes; and

6) The correlation found by Anglada et al. (1992) for outflows and jets in low mass stars extends to the handful of massive forming stars known. This result suggests that the jets associated with massive young stars are a scaled-up version of the phenomenon seen in low mass young stars, although a firmer conclusion requires the study of a larger sample of jets that now available.

We thank an anonymous referee for valuable comments. LFR acknowledges support from grant CB0702172_3 of COECyT, Michoacán, México. DM and GG acknowledge support from the Chilean Centro de Astrofísica FONDAP 15010003.



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Figure 1: Ratio of 2006 to 2003 flux densities versus the logarithm of the 2003 flux density, given in mJy. Only the jet and source S-1 show clear evidence of variability between the two epochs.
Figure 2: VLA contour images at 8.46 GHz towards IRAS 16547-4247 for epochs 2003.74 (left) and 2006.42 (center), as well as the difference image (2006.42 - 2003.74). Contours are -25, -20, -15, -10, -8, -6, -5, -4, 4, 5, 6, 8, 10, 15, 20, 25, 30, 40, 60, 100, 140, 160, and 200 times 27 Jy beam for the 2003.74 and 2006.42 images (the average value of the rms noises of the two images) and 38 Jy beam for the difference image (the rms noise of this last image). The half power contour of the synthesized beams (; PA = ) is shown in the bottom left corner of each panel. The individual sources are identified in the 2003.74 image.
Figure 3: VLA contour images at 8.46 GHz of the source E, made from the average of both epochs (2003.74 and 2006.42). Contours are -4, 4, 5, and 6 times 18 Jy beam, the rms noise of the image. The half power contour of the synthesized beam is as in Fig. 2.
Figure 4: VLA contour images at 8.46 GHz towards the jet in IRAS 16547-4247 for epochs 2003.74 (left) and 2006.42 (center), as well as the difference image (2006.42 - 2003.74). Contours are -25, -20, -15, -10, -8, -6, -5, -4, 4, 5, 6, 8, 10, 15, 20, 25, 30, 40, 60, 100, 140, 160, and 200 times 27 Jy beam for the 2003.74 and 2006.42 images and 38 Jy beam for the difference image. The half power contour of the synthesized beams (; PA = ) is shown in the bottom right corner. The cross marks the peak position of the jet as determined from the average of the two positions given in Table 1. Individual sources are identified in the 2003.74 image.
Figure 5: VLA contour images at 8.46 GHz towards the component N-1 in IRAS 16547-4247 for epochs 2003.74 (left) and 2006.42 (center), as well as the difference image (2006.42 - 2003.74). Contours are -25, -20, -15, -10, -8, -6, -5, -4, 4, 5, 6, 8, 10, 15, 20, 25, 30, 40, 60, 100, 140, 160, and 200 times 27 Jy beam for the 2003.74 and 2006.42 images and 38 Jy beam for the difference image. The half power contour of the synthesized beams (; PA = ) is shown in the bottom right corner. Individual sources are identified in the 2003.74 image.
Figure 6: VLA contour images at 8.46 GHz towards the component S-1 in IRAS 16547-4247 for epochs 2003.74 (left) and 2006.42 (center), as well as the difference image (2006.42 - 2003.74). Contours are -25, -20, -15, -10, -8, -6, -5, -4, 4, 5, 6, 8, 10, 15, 20, 25, 30, 40, 60, 100, 140, 160, and 200 times 27 Jy beam for the 2003.74 and 2006.42 images and 38 Jy beam for the difference image. The half power contour of the synthesized beams (; PA = ) is shown in the bottom right corner. Individual sources are identified in the 2003.74 image.
Figure 7: Position angle of the jet components as a function of radial offset from the jet center. The components south of the jet have been folded by 180 in this figure. The dashed line is the linear least squares fit to the components, with the exception of source C, that is taken to be an independent star.
Figure 8: VLA contour image at 8.46 GHz towards IRAS 16547-4247 for epoch 2003.74. Contours and beam are as in Figure 2. The solid line indicates the position of the spiral model discussed in the text. The arrows indicate the proper motions of components N-1 and S-1 for a period of 300 years.
Figure 9: Momentum rate in the molecular outflow, , versus the radio flux density times distance squared, . The solid dots are the 16 low mass young stars from the study of Anglada et al. (1992). We have included three high mass young stars (solid triangles, see also labels in figure) from this paper as well as from the references given in Table 3. The dashed line is the fit of Anglada et al. (1992) to the low mass young stars. The high mass young stars fall reasonably well on the correlation, suggesting a common nature for thermal jets associated with low and high mass young stars.
Component (2000) (2000) S
(Epoch) () () (mJy) Deconvolved Size
A(2003) 1705970.0077 51 550390240 1.580.23 4.”20.”61.”20.”2; 94
A(2006) 1706410.0072 51 552120205 1.600.20 4.”10.”51.”50.”2; 45
N-1(2003) 1681650.0005 51 570480011 1.”060.”040.”310.”05; 1633
N-1(2006) 1681360.0004 51 570600009 1.”150.”030.”230.”08; 1562
N-2(2003) 1687060.0015 51 583390028 1.”650.”090.”800.”08; 1625
N-2(2006) 1686690.0011 51 582490019 1.”470.”070.”760.”07; 1515
N-3(2003) 1691420.0021 52 007760061 2.”520.”170.”620.”10; 1683
N-3(2006) 1691140.0022 52 009210052 2.”520.”140.”780.”09; 1623
E(2003) 1823480.0080 52 021830115 0.160.05
E(2006) 1821280.0044 52 023190106 0.120.04
N-4(2003) 1696450.0061 52 026500164 2.”660.”430.”880.”27; 1719
N-4(2006) 1698510.0033 52 032860092 2.”400.”250.”710.”16; 1705
N-5(2003) 1707640.0053 52 048810079
N-5(2006) 1707150.0024 52 047370046
D(2003) 1712650.0016 52 068400031 0.500.03
D(2006) 1712110.0012 52 068330023 0.480.02
Jet(2003) 1720970.0001 52 071420003 10.40.1 1.”210.”010.”150.”03; 1651
Jet(2006) 1720930.0001 52 071500002 11.30.1 1.”200.”010.”140.”02; 1631
B(2003) 1739460.0013 52 096750019 0.810.06
B(2006) 1739040.0009 52 097320015 0.850.04
C(2003) 1765490.0010 52 121500018 1.100.06
C(2006) 1766030.0007 52 122210012 0.970.04
S-1(2003) 1745190.0004 52 163010006 0.”590.”040.”400.”05; 519
S-1(2006) 1745560.0002 52 162840003 0.”660.”020.”380.”02; 354
S-2(2003) 1754810.0013 52 181130031 0.630.06
S-2(2006) 1754730.0011 52 182100026 0.690.05

Peak position. Right ascension () given in hours, minutes, and seconds, and declination (), given in degrees, arcmins, and arcsecs. The errors given are formal statistical errors. The absolute positional error of the images are estimated to be 02 in right ascension and 05 in declination. The sources are listed in order of decreasing declination.

Total flux density. The errors given are formal statistical errors. The absolute flux density error is estimated to be on the order of 10%.

Deconvolved dimensions of the source: FWHM major axis FWHM minor axis; position angle of major axis.


Table 1: Observed 3.6 cm parameters of sources in the field
Source (”) () () (mas yr) (mas yr) (mas yr) () (mas yr) (mas yr)
A 12.215 -7.76 -15 1843 -65118 67114 16497 -67114 053
N-1 10.981 -23.19 -18 -123 -45 133 -11114 -15 -133
N-2 9.560 -22.96 -21 -158 3413 3712 -2419 3612 -58
N-3 7.147 -27.04 -27 -1112 -5430 5529 -16830 -4929 -2615
E 12.316 66.26 -15 -9037 -5158 10443 -11924 -2457 -10139
N-4 5.239 -30.98 -31 8528 -23770 25267 16015 -25168 1634
N-5 2.695 -32.96 -37 -2024 5434 5733 -2133 5733 -525
D 0.964 -71.73 -41 -228 314 228 -8321 914 -219
Jet 0.000 0.00 -43 -21 -31 31 -15120 -21 -21
B 3.248 141.24 144 -176 -219 278 -14117 179 227
C 7.004 135.65 153 225 -268 357 14012 318 -165
S-1 9.538 163.79 159 152 63 162 677 -32 -162
S-2 11.585 161.26 164 -37 -3615 3615 -17524 3515 118

Displacement with respect to the jet in arcsec.

Observed position angle with respect to the jet in degrees.

Predicted position angle in the precession model.

Right Ascension proper motion in milliarcsec per year. (1 mas yr = 14 km s at a distance of 2.9 Kpc)

Declination proper motion in milliarcsec per year.

Total proper motion in milliarcsec per year.

Position angle of the total proper motion in degrees.

Radial proper motion with respect to an axis with PA = , in milliarcsec per year. A negative sign corresponds to motions approaching the jet.

Transversal proper motion with respect to an axis with PA = , in milliarcsec per year. A positive sign corresponds to counterclockwise motion.

Note that if the maps were aligned to make the position of the jet fixed, the proper motions of the other components would change by 2 and 3 mas yr in Right Ascension and Declination, respectively.

Table 2: Proper Motions of Sources
  • Distance (3.6 cm)
    Source (kpc) (mJy) ( yr km s) References
    IRAS 16547-4247 2.9 8.7 1,2,3,4
    HH 80-81 1.7 3.0 5,6
    Cep A HW2 0.725 6.9 7,8
  • 1) Garay et al. (2007); 2) Garay et al. (2003); 3) Rodríguez et al. (2005); 4) this paper; 5) Martí et al. (1993); 6) Yamashita et al. (1989); 7) Curiel et al. (2006); 8) Narayanan & Walker (1996).

Table 3: Jet and Molecular Outflow Parameters of Three Massive Young Stars.
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