# Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies

R. Rolffs, P. Schilke, C. Comito, E. A. Bergin, F. F. S. van Der Tak, D. C.

Lis, S. -L. Qin, K. M. Menten, R. Güsten, T. A. Bell, et al.

► To cite this version:

R. Rolffs, P. Schilke, C. Comito, E. A. Bergin, F. F. S. van Der Tak, et al. Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies. Astronomy and Astrophysics - A&A, 2010, 521, pp.L46. 10.1051/0004-6361/201015106. insu-03625633

HAL Id: insu-03625633

https://insu.hal.science/insu-03625633

Submitted on 31 Mar 2022

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
LETTER TO THE EDITOR

# Reversal of infall in SgrB2(M) revealed by Herschel\*/HIFI observations of HCN lines at THz frequencies

R. Rolffs¹,², P. Schilke¹,², C. Comito¹, E. A. Bergin³, F. F. S. van der Tak⁴, D. C. Lis⁵, S.-L. Qin², K. M. Menten¹,

R. Güsten¹, T. A. Bell⁵, G. A. Blake⁶, E. Caux⁷,⁸, C. Ceccarelli⁹, J. Cernicharo¹⁰, N. R. Crockett³, F. Daniel¹⁰,¹¹, M.-L. Dubernet¹²,¹³, M. Emprechtinger⁵, P. Encrenaz¹¹, M. Gerin¹¹, T. F. Giesen², J. R. Goicoechea¹⁰,

P. F. Goldsmith¹⁴, H. Gupta¹⁴, E. Herbst¹⁵, C. Joblin⁷,⁸, D. Johnstone¹⁶, W. D. Langer¹⁴, W. D. Latter¹⁷, S. D. Lord¹⁷, S. Maret⁹, P. G. Martin¹⁸, G. J. Melnick¹⁹, P. Morris¹⁷, H. S. P. Müller², J. A. Murphy²⁰, V. Ossenkopf²,⁴,

J. C. Pearson¹⁴, M. Pérault¹¹, T. G. Phillips⁵, R. Plume²¹, S. Schlemmer², J. Stutzki², N. Trappe²⁰, C. Vastel⁷,⁸,

S. Wang³, H. W. Yorke¹⁴, S. Yu¹⁴, J. Zmuidzinas⁵, M. C. Diez-Gonzalez²², R. Bachiller²², J. Martin-Pintado²³, W. Baechtold²⁴, M. Olberg²⁵,⁴, L. H. Nordh²⁶, J. J. Gill¹⁴, and G. Chattopadhyay¹⁴

*(Affiliations are available on page 5 of the online edition)*

Received 31 May 2010 / Accepted 7 July 2010

## ABSTRACT

**Aims.** To investigate the accretion and feedback processes in massive star formation, we analyze the shapes of emission lines from hot molecular cores, whose asymmetries trace infall and expansion motions.

**Methods.** The high-mass star forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in various lines of HCN and its isotopologues, complemented by APEX data. The observations are compared to spherically symmetric, centrally heated models with density power-law gradient and different velocity fields (infall or infall+expansion), using the radiative transfer code RATRAN.

**Results.** The HCN line profiles are asymmetric, with the emission peak shifting from blue to red with increasing J and decreasing line opacity (HCN to H¹³CN). This is most evident in the HCN 12–11 line at 1062 GHz. These line shapes are reproduced by a model whose velocity field changes from infall in the outer part to expansion in the inner part.

**Conclusions.** The qualitative reproduction of the HCN lines suggests that infall dominates in the colder, outer regions, but expansion dominates in the warmer, inner regions. We are thus witnessing the onset of feedback in massive star formation, starting to reverse the infall and finally disrupting the whole molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI were critically important.

**Key words.** stars: formation – ISM: kinematics and dynamics – ISM: structure – ISM: molecules – ISM: individual objects: SgrB2(M) – submillimeter: ISM

## 1. Introduction

Massive stars form deep inside molecular clouds. While this obscures the process at infrared or shorter wavelengths, it offers the possibility of investigating high-mass star formation using dust emission and molecular lines from the radio to the far-infrared. The shapes of molecular lines are a particularly powerful tool, since they trace the density and temperature gradients as well as the velocity field. Even when the cores are not spatially resolved, radiative transfer modeling of a variety of lines can constrain their structure. The unique spectral coverage of HIFI opens up the full potential of this technique, since both the excitation of rotational transitions and the dust opacity increase with frequency. While the former allows us to study higher temperatures and densities, the latter leads to stronger continuum radiation, thereby facilitating the production of absorption features.

A particularly important stage of high-mass star formation is the hot core phase. When massive stars begin burning hydrogen, they are still accreting and surrounded by dense molecular gas,

which is heated and emits a rich spectrum of molecular lines. Various feedback mechanisms (radiation pressure, pressure increase due to ionization, stellar winds, bipolar outflows) push the gas outwards. Finally, this dominates over gravitational accretion, and the molecular cloud is disrupted.

The giant molecular cloud Sagittarius B2 is the most massive and active star-forming region in our Galaxy. It is located close to the Galactic center at a distance of 7.8 kpc (Reid et al. 2009). SgrB2(Main) is a tight cluster of ultracompact HII regions (Gaume & Claussen 1990), associated with a massive hot molecular core. Its luminosity is estimated to be 6.3 × 10⁶ L⊙ (Goldsmith et al. 1992), the most luminous hot core of the Galaxy. Both infall and a decelerating outflow were seen by Qin et al. (2008).

In this paper, we present new results for the velocity field of SgrB2(M), based on Herschel/HIFI observations of HCN and complemented by APEX data.

## 2. Observations

Herschel is a new space observatory with a 3.5 m antenna operating at submm to far-infrared wavelengths (Pilbratt et al. 2010).

<footnote>* Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Herschel/HIFI observations of HCN in SgrB2(M). The green model has a constant infall, the red model has infall in the outer part and expansion in the inner region. Note the different asymmetries in the lines, which are reproduced by the red model. Upper state energies are stated above the plot.</figcaption></figure>

Its spectral line receiver is HIFI (Heterodyne Instrument for the Far Infrared, de Graauw et al. 2010). The guaranteed time key project HEXOS (Herschel/HIFI Observations of EXtraOrdinary Sources, Bergin et al. 2010) includes a full line survey of SgrB2(M) ($\alpha_{J2000} = 17^h47^m20.35^s$ and $\delta_{J2000} = -28^\circ23'03.0''$). In March 2010, this was started with HIFI bands 1a, 1b, 2a, and 4b, providing coverage of the frequency ranges 479–726 GHz and 1051–1121 GHz. Each band contains one rotational transition from HCN, $H^{13}CN$, and $HC^{15}N$ (Fig. 1), and two rotational transitions within their first vibrational state, which lies around 1000 K higher in energy (Fig. 2). Transition frequencies of HCN (Thorwirth et al. 2003; Fuchs et al. 2004) are taken from CDMS (Müller et al. 2001, 2005). HIFI spectral scans are carried out in dual beam switch (DBS) mode, where the DBS reference beams lie approximately 6' apart. The wide band spectrometer (WBS) is used as a back-end, providing a spectral resolution of 1.1 MHz over a 4-GHz-wide intermediate frequency (IF) band. To allow separation of the two sidebands, bands 1a, 1b, 2a, and 4b were scanned with a redundancy of 4, 8, 8, and 4, respectively (Comito & Schilke 2002). The data were calibrated using the standard pipeline released with version 2.9 of HIPE (Ott 2010), and subsequently exported to CLASS<fnref n="1" /> using the HiClass task within HIPE. Deconvolution of the DSB data into single-sideband (SSB) format was performed using CLASS. All the HIFI data presented here, spectral features and continuum emission, are deconvolved SSB spectra. The horizontal and vertical polarizations differ by around 10%, and were averaged. The intensity scale is main-beam temperature, and results from applying a beam efficiency correction of about 0.68.

<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Herschel/HIFI observations of vibrationally excited HCN in SgrB2(M), overlaid with the pure-infall (green) and the expansion+infall model (red). The kinematics are not well constrained in this hot, innermost region.</figcaption></figure>

APEX (Atacama Pathfinder EXperiment) is a 12-m telescope located at 5100 m altitude in the Atacama Desert, Chile, one of the optimal sites for submm observations on Earth (Güsten et al. 2006). The lines presented here (Fig. 3) are from a study of the structure of 12 hot cores (Rolffs et al. 2010, in prep.). Since the baseline levels in the ground-based data are not determined reliably enough to extract the continuum, the 850 µm continuum is taken from ATLASGAL (Schuller et al. 2009).

<footnote n="1">¹ Continuum and Line Analysis Single-dish Software, distributed with the GILDAS software, see http://www.iram.fr/IRAMFR/GILDAS</footnote>
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** APEX observations of HCN in SgrB2(M), overlaid with the pure-infall (green) and the expansion+infall model (red). Although less clear than in the HIFI data, the same asymmetry change can be seen.</figcaption></figure>

<table><caption>**Table 1.** Continuum fluxes of SgrB2(M) and the model.</caption><thead><tr><th>Frequency [GHz]</th><th>Beam size ["]</th><th>SgrB2(M) [K]</th><th>Model [K]</th></tr></thead><tbody><tr><td>345</td><td>18.2</td><td>3.8</td><td>3.5</td></tr><tr><td>500</td><td>43.1</td><td>2.4</td><td>2.4</td></tr><tr><td>600</td><td>35.9</td><td>3.8</td><td>3.8</td></tr><tr><td>700</td><td>30.8</td><td>5.7</td><td>5.7</td></tr><tr><td>1100</td><td>19.6</td><td>14.6</td><td>14.2</td></tr></tbody></table>

**Notes.** The first row is the 850 µm flux from LABOCA on APEX, which contains also lines. The next rows are the baseline levels at the given frequencies in HIFI bands 1a, 1b, 2a and 4b. The baseline level of HIFI is a reliable continuum measurement, since it is as strong as saturated absorption lines and compares well with ground-based continuum data.

### 3. Modeling

The spherical Monte Carlo radiative transfer code RATRAN (Hogerheijde & van der Tak 2000) was employed to compute the molecular lines and the dust continuum. Using an iterative by-eye comparison, the fit to the data was obtained in two steps. First, the physical structure (density and temperature) was adapted to match the continuum. Second, the HCN abundance and the velocity were optimized for the lines.

The model we present here is centrally heated, its density following a radial power law with index 1.5. The dust opacity was taken from Ossenkopf & Henning (1994), without either ice mantles or coagulation. At the inner radius, 1340 AU, the density is $1.8 \times 10^8$ cm$^{-3}$ and the temperature is 1500 K. The temperature was computed in an approximate way from central heating, using the diffusion equation in the inner part and balance between heating and cooling in the outer part, assuming an effective temperature for the dust photosphere of 58 K. The temperature has a steeper gradient in the inner part, and falls off to 20 K at the outer radius of 5.6 pc, where the density is $7 \times 10^3$ cm$^{-3}$. The model reproduces the continuum very well (Table 1). Its central dust optical depth is 0.4 at 345 GHz, 0.8 at 500 GHz, 1.5 at 700 GHz, and 3.7 at 1.1 THz.

To compute the lines, we used a turbulent 1/e half width of 7 km s$^{-1}$ (12 km s$^{-1}$ FWHM). The lines were additionally broadened by their high optical depth. We found no evidence of significant variations in the turbulent width with radius. The HCN abundance increases with temperature from $10^{-8}$ at temperatures

<figure><img src="image_5.png" /><figcaption>**Fig. 4.** Sketch of the scenario described in the text. In the outer parts of the cloud, infall dominates. In the inner part, feedback has set in, in this example envisioned as multiple outflows, and gas is expelled from it. At the same time, infall continues along certain paths.</figcaption></figure>

<figure><img src="image_6.png" /><figcaption>**Fig. 5.** Physical structure of the model. Density is plotted as dashed green, temperature as dotted blue. The velocity field of the infall+expansion model is shown as the solid red curve (the infall model has a constant velocity of -2 km s$^{-1}$). At the transition between infall and expansion, the temperature is 65 K and the density is $6 \times 10^5$ cm$^{-3}$.</figcaption></figure>

below 100 K, to $3 \times 10^{-8}$ between 100 and 300 K, to $3 \times 10^{-7}$ at temperatures above 300 K. The first jump is mainly needed to reproduce the intensities of the isotopologues and of vibrationally excited HCN, the second jump serves to fit vibrationally excited H$^{13}$CN. These jumps could be due to evaporation of ice mantles and/or increased chemical production. We used a $^{12}$C/$^{13}$C ratio of 20 and $^{14}$N/$^{15}$N of 600 (Wilson & Rood 1994). The green model has a constant infall velocity of 2 km s$^{-1}$, and the red model has the same velocity in its outer parts, but an expansion in its inner parts. Figure 5 shows the velocity field. We note that the exact shape of this, particularly the transition from infall to outflow, is not constrained by the observations, hence modeling the true velocity field by adopting this spherical approximation is an oversimplification (see Fig. 4).

A comparison with the observations (Figs. 1–3) shows that the red model reproduces more closely the observed features. In particular, to reproduce the changes in the asymmetry that occur both from lower to higher J and from higher to lower optical depth (from HCN 6–5 to H$^{13}$CN 6–5), a change in the velocity field is required, from infall in the colder, outer parts to expansion in the warmer, inner parts.

### 4. Discussion

We now discuss the velocity field and how it is physically determined.
In a gravitationally contracting sphere with density power-law index $p$, a first guess and upper limit to the infall speed would correspond to free fall, i.e., $v_{ff}(R) = \sqrt{\frac{2GM(R)}{R}}$, where the mass inside the radius $R$ is $M(R) \propto R^{3-p}$ (for $p < 3$), such that $v_{ff} \propto R^{\frac{2-p}{2}}$. In our model, this free-fall speed is roughly (at a radius of 1 pc) 10 times higher than the 2 km s⁻¹ of the model. Such high infall velocities can be excluded because they would produce lines that are far more asymmetric than observed.

The mass accretion rate $\dot{M} = v_{acc}(R) \frac{dM(R)}{dR}$, so $v_{acc} \propto R^{p-2}$ for a constant mass accretion rate. Hence, infall accelerates in a spherical steady-state model with $p = 1.5$. However, an accelerating infall, at least in the inner part, is inconsistent with the data. For simplicity, we chose a constant infall velocity, corresponding to accretion rates onto the cluster of $3 \times 10^{-1} M_{\odot}/\text{yr}$ at the outer boundary and $10^{-1} M_{\odot}/\text{yr}$ at a radius of $10^5 \text{ AU}$. The excretion rate reaches $8 \times 10^{-2} M_{\odot}/\text{yr}$ at $2 \times 10^4 \text{ AU}$.

The real velocity field must be non-spherical, and infall could well continue in the inner part (see Fig. 4 and also Qin et al. 2008). The peak on top of the HCN 12–11 absorption (Fig. 1) could be a hint of that infall. Since the $H^{13}\text{CN}$ transitions are less asymmetric than modeled points in that direction, one may suspect that a linear combination of the pure infall and expanding models would produce the line spectra very well. For the HCN lines, because of their high optical depths, such a linear combination of intensities does not naturally reproduce the observed spectra; more sophisticated modeling, in which we abandon the spherical approximation, would be required. For overlying model and data (Figs. 1–3), we assumed a source velocity of 64 km s⁻¹, although 60 km s⁻¹ would reproduce more closely the high-$J$ lines. This blue shift of absorption towards higher $J$ is consistent with our picture of a velocity field changing from infall to expansion, and is indicative of a deviation from spherical symmetry.

While gravity is clearly responsible for the infall, there must also be feedback mechanisms from newly formed stars working against gravity, thus regulating star formation. The velocity of the infalling envelope must be lower than that of pure gravitational collapse by around 90%. Apart from magnetic braking, turbulence induced by bipolar outflows may be such a long-range feedback mechanism providing the necessary pressure (Wang et al. 2010). The massive stars in the center dominate the luminosity, and drive the expansion by means of stellar winds, radiation pressure (including reprocessed light), and heating and ionization of the gas, in particular thermal pressure of their HII regions (Krumholz & Matzner 2009). Since in our model only 1% of the total mass of $7 \times 10^5 M_{\odot}$ is expanding, the outward momentum remains much lower than the inward momentum, indicating that feedback is not yet able to disrupt the cloud.

## 5. Conclusions

The changing asymmetry of the HCN lines clearly indicates a reversal of infall. Expansion motions dominate in the inner, warmer parts, and infall dominates in the outer, colder parts of the core. This can be naturally explained by the onset of feedback from massive stars. Our radiative transfer modeling demonstrates the power of constraining the source structure by fitting line shapes. A model that successfully reproduces all the features cannot have spherical symmetry, and the exact geometry probably has to be constrained by interferometric observations, to determine the free parameters. Although the Herschel/HIFI

data do not have the desired spatial resolution, they place strong constraints on any such model, since they have to be reproduced.

We propose a scenario in which the cloud gravitationally contracts at significantly below the free-fall speed. A star cluster forms by fragmentation and accretion. The stars, especially the massive stars that dominate the luminosity, provide various feedback mechanisms to counteract the contraction. The additional pressure, be it thermal, radiative, or turbulent, decelerates the contraction, then dominates first in the inner part, before finally disrupting the whole cloud. SgrB2(M) is just beginning to drive out the gas, while large-scale global infall and probably also infall among very localized pathways in the interior remains ongoing.

This study illustrates the importance of high-frequency lines in constraining the source structure, and demonstrates the great potential of HIFI, which delivers velocity-resolved spectra at these frequencies. Ground-based telescopes may not be able to reach high enough frequencies. In our case, detecting the HCN 12–11 line was necessary in order to unambiguously trace the reversal of infall, so this result is unique to HIFI. We expect that a systematic study of high-$J$ HCN transitions, even higher than the 12–11 line seen here, with a high signal-to-noise ratio, and toward a sample of hot core sources, would be highly rewarding in finding more sources in this particular stage of evolution.

**Acknowledgements.** HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS, Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronòmico Nacional (IGN), Centro de Astrobiología (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882.

## References

Bergin, E. A., Phillips, T. G., Comito, C., et al. 2010, A&A, 521, L20

Comito, C., & Schilke, P. 2002, A&A, 395, 357

de Graauw, Th., Helmich, F. P., Phillips, T. G., et al. 2010, A&A, 518, L6

Fuchs, U., Bruenken, S., Fuchs, G. W., et al. 2004, Z. Naturforsch. A, 59, 861

Gaume, R. A., & Claussen, M. J. 1990, ApJ, 351, 538

Goldsmith, P. F., Lis, D. C., Lester, D. F., & Harvey, P. M. 1992, ApJ, 389, 338

Güsten, R., Nyman, L. Å., Schilke, P., et al. 2006, A&A, 454, L13

Hogerheijde, M. R., & van der Tak, F. F. S. 2000, A&A, 362, 697

Krumholz, M. R., & Matzner, C. D. 2009, ApJ, 703, 1352

Müller, H. S. P., Schlöder, F., Stutzki, J., & Winnewisser, G. 2005, J. Mol. Struct., 742, 215

Müller, H. S. P., Thorwirth, S., Roth, D. A., & Winnewisser, G. 2001, A&A, 370, L49

Ossenkopf, V., & Henning, T. 1994, A&A, 291, 943

Ott, S. 2010, Astronomical Data Analysis Software and Systems XIX, ed. Y. Mizumoto, K.-I. Morita, & M. Ohishi, ASP Conf. Ser., in press

Pilbratt, G. L., Riedinger, J., Passvogel, T., et al. 2010, A&A, 518, L1

Qin, S., Zhao, J., Moran, J. M., et al. 2008, ApJ, 677, 353

Reid, M. J., Menten, K. M., Zheng, X. W., Brunthaler, A., & Xu, Y. 2009, ApJ, 705, 1548

Schuller, F., Menten, K. M., Contreras, Y., et al. 2009, A&A, 504, 415

Thorwirth, S., Müller, H. S. P., Lewen, F., et al. 2003, ApJ, 585, L163

Wang, P., Li, Z., Abel, T., & Nakamura, F. 2010, ApJ, 709, 27

Wilson, T. L., & Rood, R. 1994, ARA&A, 32, 191
1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: rrolffs@mpifr.de

2 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany

3 Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA

4 SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV, Groningen, The Netherlands

5 California Institute of Technology, Cahill Center for Astronomy and Astrophysics 301-17, Pasadena, CA 91125, USA

6 California Institute of Technology, Division of Geological and Planetary Sciences, MS 150-21, Pasadena, CA 91125, USA

7 Centre d'Étude Spatiale des Rayonnements, Université de Toulouse [UPS], 31062 Toulouse Cedex 9, France

8 CNRS/INSU, UMR 5187, 9 avenue du Colonel Roche, 31028 Toulouse Cedex 4, France

9 Laboratoire d'Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France

10 Centro de Astrobiología (CSIC/INTA), Laboratorio de Astrofísica Molecular, Ctra. de Torrejón a Ajalvir km 4, 28850 Madrid, Spain

11 LERMA, CNRS UMR8112, Observatoire de Paris and École Normale Supérieure, 24 Rue Lhomond, 75231 Paris Cedex 05, France

12 LPMAA, UMR7092, Université Pierre et Marie Curie, Paris, France

13 LUTH, UMR8102, Observatoire de Paris, Meudon, France

14 Jet Propulsion Laboratory, Caltech, Pasadena, CA 91109, USA

15 Departments of Physics, Astronomy and Chemistry, Ohio State University, Columbus, OH 43210, USA

16 National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada

17 Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USA

18 Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St George St, Toronto, ON M5S 3H8, Canada

19 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA

20 National University of Ireland Maynooth, Ireland

21 Department of Physics and Astronomy, University of Calgary, 2500 University Drive NW, Calgary, AB T2N 1N4, Canada

22 Observatorio Astronómico Nacional (IGN), Centro Astronómico de Yebes, Apartado 148, 19080 Guadalajara, Spain

23 Departamento de Astrofísica Molecular e Infrarroja, Instituto de Estructura de la Materia, CSIC, Calle Serrano 121, 28006 Madrid, Spain

24 Microwave Laboratory, ETH Zurich, 8092 Zurich, Switzerland

25 Chalmers University of Technology, 412 96 Göteborg, Sweden, Sweden

26 Department of Astronomy, Stockholm University, 106 91 Stockholm, Sweden