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A&A
Volume 567, July 2014
Article Number A99
Number of page(s) 6
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201423693
Published online 21 July 2014

© ESO, 2014

1. Introduction

One of the most remarkable and not yet completely understood processes involved in the formation of stars is the appearance of collimated bipolar outflows in the earliest stages of formation. This process is present until the end of the accretion phase and has significant effects in the surroundings (e.g. Froebrich et al. 2003a,b; Bally et al. 2006; Arce et al. 2010). The structure and (a)symmetries of the outflows record orientation changes of the accretion disk and motion of the source relative to the local interstellar medium (Cunningham et al. 2009). Moreover, the outflows can be deflected by material swept up in an earlier epoch of ejection by the central source (Fich & Lada 1997) and/or by dense preexisting molecular clumps (Choi 2005; Baek et al. 2009). Thus, mapping molecular outflows is very useful for studying star formation, and in particular, for investigating the interaction between young stellar objects (YSOs) and the surrounding environments.

The red MSX source G034.5964-01.0292 (hereafter MSXG34), related to IRAS 1855+0056, is catalogued as a massive YSO located at a distance of 1.1 kpc (Lumsden et al. 2013). Ammonia was detected towards this source by Wienen et al. (2012). The (J,K) = (1,1) and (2, 2) NH3 inversion lines were detected at velocities of 13.63 and 13.84 km s-1, related to the ATLASGAL source G34.60-1.03 detected at 870 μm. This source lies at the north-eastern border of the HII region G34.5-1.1, that has a recombination line at 44.7 km s-1 (Lockman 1989; Kuchar & Clark 1997); this precludes any connection between them. Thus, taking into account that very likely a massive YSO is related to dense material traced by the ammonia emission, and that no others YSOs are catalogued around this source, which would make an outflow study confusing, we decided to observe MSXG34 in the 12CO J = 3–2 and HCO+J = 4–3 lines to search for signatures of molecular outflows.

2. Observations and data reduction

The molecular observations presented in this work were carried out on September 13, 2013 with the 10 m Atacama Submillimeter Telescope Experiment (ASTE; Ezawa et al. 2004). We used the CATS345 receiver, which is a two single-band SIS receiver remotely tunable in the LO frequency range of 324−372 GHz. We simultaneously observed 12CO J = 3−2 at 345.796 GHz and HCO+J = 4–3 at 356.734 GHz, mapping a region of 3′× 3′ centred at RA = 18h58m08.4s, Dec =+01°00′38.8′′, J2000. The mapping grid spacing was 20′′ and the integration time was 20 s in each pointing. All the observations were performed in position-switching mode.

We used the XF digital spectrometer with the bandwidth and spectral resolution set to 128 MHz and 125 kHz. The velocity resolution was 0.11 km s-1, the half-power beamwidth (HPBW) 22′′. The system temperature varied from Tsys = 150 to 300 K. The main-beam efficiency was ηmb ~ 0.65. The spectra were Hanning smoothed to improve the signal-to-noise ratio, and only linear or some second-order polynomia were used for baseline fitting. The data were reduced with NEWSTAR1 and the spectra processed using the XSpec software package2.

Additionally, we used public 13CO J = 1–0 data, with an angular and spectral resolution of 46′′ and 0.2 km s-1, obtained from the Galactic Ring Survey (GRS; Jackson et al. 2006), and near-IR UKIDSS data (Lucas et al. 2008) extracted from the WFCAM Science Archive3.

3. Results and discussion

Figure 1 displays the 12CO J = 3–2 spectra obtained towards the surveyed region. The centre, that is, the (0, 0) offset, corresponds to the position of MSXG34. The spectra present a main component with an absorption dip associated with MSXG34, and additionally less intense components at higher velocities, which appear in the whole surveyed area and represent gas detected along the line of sight not related to the analysed source. The same region was also surveyed in the HCO+J = 4–3 line, but emission was only detected at the (0, 0) offset. Figure 2 shows the 12CO and HCO+ spectra towards the centre of the region. The 12CO J = 3–2 spectrum shows a double-peak structure with a main component centred at ~14.3 km s-1 and a less intense component centred at ~10.0 km s-1. Both components are far to be Gaussian, and it is very likely that the line appears self-absorbed, as is commonly found towards star-forming regions (e.g. Johnstone et al. 2003; Buckle et al. 2010), which in this case is indicated by the absorption dip at ~13.2 km s-1. Moreover, the velocity of this absorption dip is almost coincident with those of the NH3 lines detected by Wienen et al. (2012) (vLSR = 13.63 and 13.85 km s-1 with ΔvFWHM = 0.87 and 1.13 km s-1 for (J,K) = (1,1) and (2, 2) NH3 inversion lines). The presence of ammonia, tracer of high density gas, confirms the density gradient that produces the self-absorption in the optically thick 12CO line. On the other side, the HCO+ spectrum shows a simpler behaviour and can be fitted with a Gaussian centred at vLSR ~ 14.2 km s-1 with ΔvFWHM ~ 1.6 km s-1.

It is known that HCO+ and NH3 enhance in molecular outflows as reported by Torrelles et al. (1992), Girart et al. (1998), and Rawlings et al. (2004). In effect, an enhancement in the abundance of such molecular species is expected to occur in the boundary layer between the outflow and the surrounding molecular core. As these authors point out, this enhancement is probably due to the liberation and photoprocessing by the shock of the molecular material stored in the icy mantles of the dust. This process may be occurring in MSXG34, which is supported by the observed complexity in the 12CO J = 3–2 profiles that, as shown in Figs. 1 and 2, present spectral wings as usually observed towards molecular outflows.

thumbnail Fig. 1

12CO J = 3–2 spectra obtained towards the surveyed region. The (0, 0) offset is the position of the studied source.

thumbnail Fig. 2

12CO J = 3–2 and HCO+J = 4–3 spectra obtained towards the centre of the surveyed region.

Taking into account that 12CO J = 3–2 appears to be self-absorbed, a single-Gaussian function is expected to contain the two main components that are separated by the absorption dip. The emission that appears to be beyond the Gaussian shape is considered to be associated with the molecular outflows. This is shown in Fig. 3, where we display above the central 12CO spectrum the Gaussian function and high-velocity gas intervals along which the emission was integrated. The small component at ~38 km s-1 is excluded because, as shown in Fig. 1, it appears almost in the whole surveyed region, which precludes that it is produced by MSXG34. The result of the integration is shown in Fig. 4, where we display above the Spitzer-IRAC IR emission at 8 μm the 12CO J = 3–2 integrated between 20 and 35 km s-1 (red-shifted gas), and between −10 and 7 km s-1 (blue-shifted gas). An intense red-shifted 12CO lobe clearly extends towards the north-west, while a less intense 12CO blue-shifted lobe extends towards the south-west. Both lobes appear to be highly misaligned.

thumbnail Fig. 3

12CO J = 3–2 spectrum towards the centre of the surveyed region with a Gaussian function representing the unabsorbed main component. The boxes show the high-velocity gas intervals along which the emission was integrated.

thumbnail Fig. 4

Spitzer-IRAC 8 μm emission with contours of the 12CO J = 3−2 integrated between 20 and 35 km s-1 (in red), and between −10 and 7 km s-1 (in blue). The contour levels are 13, 17, and 25 K km s-1 for the red-shifted lobe, and 6.5, 7.5, and 8 K km s-1 for the blue-shifted one. The beam of the molecular observations is included in the bottom-right corner.

To roughly estimate the outflow mass, following Bertsch et al. (1993), we calculated the H2 column density from

N(H2)=2.0×1020W(12CO)[Kkms-1](cm-2),$$ N{\rm (H_{2})} = 2.0 \times 10^{20} ~\frac{W\left(^{12}\rm CO\right)}{\rm [K~km~s^{-1}]}~ {\rm \left(cm^{-2}\right)}, $$where W(12CO) is the 12CO J = 3–2 integrated intensity along the velocity intervals shown in Fig. 2 (top). Then, the mass was derived from

M=μmH∑i[D2ΩiNi(H2)],$$ M = \mu~m_{{\rm H}} \sum_{i}{\left[ D^{2}~\Omega_{i}~N_{\it i}{\rm (H_{2}}) \right]}, $$where Ω is the solid angle subtended by the beam size, mH is the hydrogen mass, μ, the mean molecular weight, is assumed to be 2.8 by taking into account a relative helium abundance of 25%, and D is the distance. We summed over all beam positions belonging to the lobes shown in Fig. 4, which yields the mass for the red- and blue-shifted outflows: Mred ~ 7.5 M⊙ and Mblue ~ 1.3 M⊙. Then we obtain the momentum Pred ~ 114 × cos-1(φ) M⊙ km s-1 and Pblue ~ 22.5 × cos-1(φ) M⊙ km s-1, and the energies Ered ~ 3.4 × 1046 × cos-2(φ) erg and Eblue ~ 7.6 × 1045 × cos-2(φ) erg, where φ is the inclination angle of the outflow, which is uncertain.

3.1. Outflows morphology

As mentioned above and shown in Fig. 4, the red- and blue-molecular outflows are highly misaligned. A jet precession, either produced by tidal interactions in a binary system or due to anisotropic accretion events (e.g. Papaloizou & Terquem 1995; Kraus et al. 2006), can generate misaligned molecular outflows. We found a similar case as presented here towards the UCHII region G045.47+0.05 (Ortega et al. 2012). Two misaligned red- and blue-shifted molecular outflows were discovered through molecular observations obtained with ASTE. Later, from very high-angular resolution observations at near-IR obtained with Gemini-NIRI, Paron et al. (2013) reported that a jet precession occurs in a massive YSO. Another similar case in which a jet precession scenario was suggested is IRAS 20126+4104, where two misaligned CO high-velocity flows are observed (Lebrón et al. 2006). To investigate this possibility we analysed near-IR data from UKIDSS towards MSXG34.

Figure 5 shows the emission of the JHK-bands from UKIDSS in a three-colour image. The point source UGPS J185808.46+010041.8 (Lucas et al. 2008; Ukidss 2012) is connected with a cone-like nebulosity composed of two arc-like features, the closest feature more intense than the farther. Both features seem to be connected by diffuse emission. It is very likely that the near-IR emission forming this cone-like shape arises from a cavity cleared in the circumstellar material. This emission can be due to a combination of different emitting processes: continuum emission from the central protostar that is scattered at the inner walls of a cavity, emission from warm dust, and probably also emission lines from shock-excited gas. The arc-like features, with a concavity pointing to the source, suggest an spiraling shape, which can be signature of a precessing jet. This can be a similar case as we found in G045.47+0.05 (Paron et al. 2013) and others in the literature (e.g. Weigelt et al. 2006; Kraus et al. 2006). Therefore, we conclude that the misaligned CO outflows and the near-IR features related to the analysed source strongly suggest a jet-precession scenario. However, higher angular resolution observations in both submillimeter and near-IR are necessary to investigate the whole circumstellar region in more detail.

thumbnail Fig. 5

Three-colour image towards MSXG34 where the JHK-bands from UKIDSS are presented in blue, green, and red. The angular resolution is about 1 arcsec.

Additionally, analysing the molecular gas on a larger scale, we found that MSXG34 lies in a molecular clump. Thus, a complementary possible scenario for the misaligned molecular outflows is that one of its lobes is deflected by the interaction with dense material. By inspecting the 13CO J = 1–0 cube obtained from the GRS, we found that the molecular clump in which MSXG34 is likely embedded extends from 10 to 14 km s-1. Taking into account that the systemic velocity of MSXG34 is about 14 km s-1 (determined from the emission of NH3 and HCO+), the formation of this YSO would be occurring at the far border of the clump. Figure 6 shows the 13CO J = 1–0 emission integrated between 10 and 14 km s-1 with contours of the blue- and red-shifted molecular outflows. The scenario might be that the YSO is located in the background border of the molecular clump, the red-shifted lobe freely flows away, while the blue-shifted one hits the inner and densest portion of the clump which deflects its trajectory. It might be a similar case as discovered in the NGC 1333 IRAS 4A region by Choi (2005). Submillimeter observations of high-density tracers such as CS and SiO, are necessary to confirm the existence of high-density gas belonging to the clump and to study the probable collision with the blue lobe. Finally, another possibility is that the red- and blue-shifted lobes come from monopolar molecular outflows, as proposed by Fernández-López et al. (2013) in IRAS 18162-2048, where the respective counterlobes are not seen because they are passing through a cavity and/or regions of low molecular abundance.

thumbnail Fig. 6

13CO J = 1–0 obtained from the GRS integrated between 10 and 14 km s-1. The contour levels are 6.8 and 7.5 K km s-1. The contours of the blue and red lobes shown in Fig. 4 are also displayed. The ASTE and GRS beams are included in the top-left corner.

3.2. Nature of the outflow-driving source

The analysis of the UKIDSS data suggests that source UGPS J185808.46+10041.8 is a good candidate to be the driving source of the discovered molecular outflow (see Fig. 7). This near-IR source is embedded in a clump of cold dust catalogued as G034.60-1.030 in the ATLASGAL cold high-mass clumps with NH3 catalogue (Wienen et al. 2012). By considering the associated dust continuum emission at 870 μm and following Beuther et al. (2005) and Hildebrand (1983), we estimate the mass of this clump from Mgas=2.0×10-2Jν(Tdust)a0.1μmρ3gcm-3R100FνJy(dkpc)2× (ν1.2THz)−3−β,\begin{eqnarray} \tiny M_{\rm gas}&=&\frac{2.0 \times 10^{-2}}{J_{\nu}(T_{\rm dust})}\frac{a}{0.1~ \mu{\rm m}}\frac{\rho}{3~{\rm g~cm}^{-3}}\frac{R}{100}\frac{F_{\nu}}{{\rm Jy}}\nonumber\left(\frac{d}{{\rm kpc}}\right)^2\\ &&\times\,\left(\frac{\nu}{1.2~{\rm THz}}\right)^{-3-\beta}, \end{eqnarray}(1)where Jν(Tdust) = [exp(hν/kTdust)−1] -1 and a,ρ,R, and β are the grain size, grain mass density, gas-to-dust ratio, and grain emissivity index, for which we adopt the values of 0.1 μm, 3 g cm-3, 100, and 2, respectively (Hunter 1997, Hunter et al. 2000, and Molinari et al. 2000). Assuming a dust temperature of 20 K and considering the integrated flux intensity Fν = 1.8 Jy at 870 μm (Wienen et al. 2012), we obtain Mgas ~ 25 M⊙. On the other hand, considering the integrated flux density Fν = 19.2 Jy at 500 μm obtained from the level-2 PLW Herschel image using the HIPE software package (Ott 2010), and using the above equation with the same considerations, we estimate a mass for the clump of about 40 M⊙. Thus, we conclude that UGPS J185808.46+10041.8 is embedded in a high-mass clump (around 30 M⊙).

thumbnail Fig. 7

UKIDSS three-colour image (JHK-bands in blue, green and red) of the MSXG34 region. The red- and blue-shifted lobes of the molecular outflows are included. The yellow circle, 30′′ in size, corresponds to the 500 μm continuum emission from SPIRE (above 5σ of the rms noise level) as extracted from the Herschel Science Archive.

To better characterize the nature of this IR source, we fitted the spectral energy distribution (SED) using the online tool developed by Robitaille et al. (2007)4. We adopted an interstellar extinction on the line of sight, AV , between 1 and 50 mag. We assumed a 20% uncertainty for the distance to UGPS J185808.46+10041.8. In Fig. 8 we show the SED with the best-fitting model (black curve), and the subsequent well-fitting models (gray curves) with χ2−χbest2≤3\hbox{$\chi^2 - \chi_{\rm best}^2 \leq 3$} (where χbest2\hbox{$\chi_{\rm best}^2$} is the χ2 per data point of the best-fitting model for the source). To construct this SED we used fluxes extracted from the UKIDSS-DR6 Galactic Plane Survey (Lucas et al. 2008) in the J, H and K bands (source UGPS J185808.46+010041.8), the MSX Point Source Catalog at 8.2, 12.1, 14.6, and 21.3 μm (source G034.5964-01.0292), the WISE All-Sky Source Catalog5 at 3.6, 12, and 22 μm (source WISE J185808.44+010041.8), the PACS bands at 70 and 160 μm (Poglitsch et al. 2010), the SPIRE bands at 250, 350, and 500 μm (Griffin et al. 2010) from Herschel, and finally ATLASGAL at 870 μm. PACS and SPIRE fluxes were obtained from level-2 MADmaps, PLW, PMW, and PSW images, respectively, using HIPE software package. Considering that UGPS J185808.46+010041.8 is by far the brightest source within the Herschel emission boundaries (see yellow circle in Fig. 7) and no contamination from clustering of infrared objects is observed in the region, we treated the larger beam-size data of WISE at 22 μm, Herschel, and ATLASGAL as “data points” instead of upper limits to make the best use of all data in constraining the SED. 20% errors on the fluxes were assumed for all data, except for UKIDSS fluxes, where 30% error were used because of extinction uncertainties.

The SED was fitted by multiple models, each model describing a set of physical parameters. The same parameter from different models can have a wide range, spanning from several factors to orders of magnitudes. We obtained 63 well-fitting models that satisfy the χ2 criterion mentioned above. To find a representative value for the distributions of the parameters, we computed a weighted mean and a range of values for some of the physical parameters of the source (see Table 1). The weight used for the weighted means is the inverse of the χ2 of each model. It is important to mention that the trend of our fitting results are not biased by the trend inherent in the model grids. The SED analysis of UGPS J185808.46+010041.8 suggests that the central object is a young intermediate-mass protostar of about 3 M⊙. By comparing the obtained bolometric luminosity of about 200 L⊙ with the total outflow mass, about 9 M⊙, we note that it agrees well, within the dispersion, with the relation found by Wu et al. (2004). The position of our point in the figure presented by the authors displaying Mout vs. Lbol also suggests an intermediate-mass protostar.

thumbnail Fig. 8

SED of MSXG34. The circles indicate the measured fluxes of the data points. The black and grey solid curves represent the best-fitting model and the subsequent well-fitting models (with χ2−χbest2≤3\hbox{$\chi^2 - \chi_{best}^2 \leq 3$}), respectively. The dashed line shows the stellar photosphere corresponding to the central source of the best-fitting model, as it would look without circumstellar dust.

Table 1

Main physical parameters from the SED of MSXG34.

4. Summary

Using the ASTE telescope, we observed MSXG34, a catalogued massive YSO at a distance of about 1 kpc, in the 12CO J = 3–2 and HCO+J = 4–3 lines with the aim of discovering and studying molecular outflows. The 12CO spectra towards the YSO present typical signatures of star-forming regions: a self-absorption dip and spectral wings that indicate outflow activity. The HCO+ was detected only towards the MSXG34 position at vLSR ~ 14.2 km s-1, in coincidence with the 12CO absorption dip and approximately with the velocity of previous ammonia observations. The HCO+ and NH3 are known to be enhanced in molecular outflows.

By analysing the 12CO J = 3–2 emission, we discovered misaligned red- and blue-shifted molecular outflows with mass, momentum, and energy of Mred ~ 7.5 M⊙ and Mblue ~ 1.3 M⊙, Pred ~ 114 × cos-1(φ) M⊙ km s-1 and Pblue ~ 22.5 × cos-1(φ) M⊙ km s-1, and Ered ~ 3.4 × 1046 × cos-2(φ) erg and Eblue ~ 7.6 × 1045 × cos-2(φ) erg, where φ is the inclination angle of the outflow, which is uncertain.

By analysing UKIDSS near-IR data, we found that the emission shows a cone-like nebulosity composed of two arc-like features related to the YSO, which can be due to a cavity cleared in the circumstellar material by a precessing jet, explaining in this way the misalignment in the molecular outflows. Additionally, the 13CO J = 1–0 data show that MSXG34 is very likely embedded in a molecular clump that extends from 10 to 14 km s-1. Taking into account that the associated central velocity of MSXG34 is about 14 km s-1, it is probable that the YSO is located in the background of the densest part of the clump, and thus the blue-shifted outflow is probably deflected by the interaction with dense gas along the line of sight. Another possibility is that the red- and blue-shifted lobes come from monopolar molecular outflows, where the respective counterlobes are not seen because they are passing through a cavity and/or regions of low molecular abundance.

Finally, we performed an SED analysis using fluxes from near- to far-IR that suggested that the central object of MSXG34 is a young intermediate-mass protostar (about 3 M⊙). The relation between the total outflow mass, obtained from our molecular observations, and the bolometric luminosity, obtained from the SED, also suggests an intermediate-mass stellar object.

1

Reduction software based on AIPS developed at NRAO, extended to treat single dish data with a graphical user interface (GUI).

2

XSpec is a spectral-line reduction package for astronomy that has been developed by Per Bergman at Onsala Space Observatory.

5

WISE is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA.

Acknowledgments

We would like to thank the anonymous referee for her/his helpful comments. S.P. and M.O. are members of the Carrera del investigador científico of CONICET, Argentina. A.P. is a post-doctoral fellow of CONICET, Argentina. This work was partially supported by grants awarded by CONICET, ANPCYT, and UBA (UBACyT). M.R. wishes to acknowledge support from FONDECYT(CHILE) grant No1140839. A.P. is very grateful to the ASTE staff for the support received during the observations. The ASTE project is driven by Nobeyama Radio Observatory (NRO), a branch of the National Astronomical Observatory of Japan (NAOJ), in collaboration with University of Chile, and Japanese institutes including the University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University, Hokkaido University, and Joetsu University of Education.

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All Tables

Table 1

Main physical parameters from the SED of MSXG34.

In the text

All Figures

thumbnail Fig. 1

12CO J = 3–2 spectra obtained towards the surveyed region. The (0, 0) offset is the position of the studied source.

In the text
thumbnail Fig. 2

12CO J = 3–2 and HCO+J = 4–3 spectra obtained towards the centre of the surveyed region.

In the text
thumbnail Fig. 3

12CO J = 3–2 spectrum towards the centre of the surveyed region with a Gaussian function representing the unabsorbed main component. The boxes show the high-velocity gas intervals along which the emission was integrated.

In the text
thumbnail Fig. 4

Spitzer-IRAC 8 μm emission with contours of the 12CO J = 3−2 integrated between 20 and 35 km s-1 (in red), and between −10 and 7 km s-1 (in blue). The contour levels are 13, 17, and 25 K km s-1 for the red-shifted lobe, and 6.5, 7.5, and 8 K km s-1 for the blue-shifted one. The beam of the molecular observations is included in the bottom-right corner.
In the text
thumbnail Fig. 5

Three-colour image towards MSXG34 where the JHK-bands from UKIDSS are presented in blue, green, and red. The angular resolution is about 1 arcsec.
In the text
thumbnail Fig. 6

13CO J = 1–0 obtained from the GRS integrated between 10 and 14 km s-1. The contour levels are 6.8 and 7.5 K km s-1. The contours of the blue and red lobes shown in Fig. 4 are also displayed. The ASTE and GRS beams are included in the top-left corner.

In the text
thumbnail Fig. 7

UKIDSS three-colour image (JHK-bands in blue, green and red) of the MSXG34 region. The red- and blue-shifted lobes of the molecular outflows are included. The yellow circle, 30′′ in size, corresponds to the 500 μm continuum emission from SPIRE (above 5σ of the rms noise level) as extracted from the Herschel Science Archive.
In the text
thumbnail Fig. 8

SED of MSXG34. The circles indicate the measured fluxes of the data points. The black and grey solid curves represent the best-fitting model and the subsequent well-fitting models (with χ2−χbest2≤3\hbox{$\chi^2 - \chi_{best}^2 \leq 3$}), respectively. The dashed line shows the stellar photosphere corresponding to the central source of the best-fitting model, as it would look without circumstellar dust.
In the text

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