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A&A
Volume 603, July 2017
Article Number L2
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201731170
Published online 11 July 2017

© ESO, 2017

1. Introduction

The circumstellar envelopes (CSEs) of asymptotic giant branch (AGB) and post-AGB objects have turned out to be rich in different molecular species; more than 100 are now detected. This is the effect of a number of different processes, such as stellar atmosphere equilibrium chemistry, extended atmosphere non-equilibrium chemistry, and photo-induced circumstellar chemistry (e.g., Millar 2016). The post-AGB objects have a special niche in terms of chemistry because of the increased internal UV light and the presence of shocks where fast winds interact with slower-moving material. The result being that they often show molecular species that are not detected (or tend to be much weaker) in AGB CSEs; for example, a number of ions (Sánchez Contreras et al. 2015). One species, methanol (CH3OH), has escaped every attempt at detection in an AGB-related object (e.g., Charnley & Latter 1997; Gómez et al. 2014), despite detectable predicted abundances (Willacy & Millar 1997). It is therefore taken as a clear signpost for a young stellar object (YSO) (Breen et al. 2013). However, in the course of a chemical study of an interesting post-AGB object HD 101584 using ALMA, we have detected methanol for the first time in an AGB-related object, and in this Letter we discuss its origin together with detections of CO, SiO, SO, CS, and H2CO.

HD 101584 is a bright star (V ≈ 7m) of spectral type A6Ia (Sivarani et al. 1999). It was shown to have a large far infrared excess and an evolutionary status at, or shortly after, the end of the AGB was proposed by Parthasarathy & Pottasch (1986) and further corroborated by Bakker et al. (1996b). It has also been shown to be a binary system (Bakker et al. 1996a; Díaz et al. 2007). The distance is estimated to be 0.7 kpc, but recent Gaia data suggests a somewhat larger distance, 0.9−1.8 kpc. The HST images show only a diffuse circumstellar medium in dust-scattered light (Sahai et al. 2007), but its circumstellar gas characteristics are remarkable.

Olofsson et al. (2015) used ALMA 12CO(J = 2–1) data to identify a narrow, ≈10′′ long, high-velocity molecular outflow directed at PA ≈ 90°. Its velocity range covers almost 300 km s-1 and has a Hubble-like gradient. The outflow is seen almost along its axis. The kinematical age is estimated to be ≲500 yr. There is an hour-glass structure surrounding the outflow, and a complex structure within 1′′ (in radius) of HD 101584, most likely a torus-like component centered on a circumbinary disc. Here we provide further evidence, based on circumstellar isotopolog ratios, for the post-AGB nature of HD 101584.

2. Observations

The ALMA data were obtained during Cycles 1 and 3 with 35 to 43 antennas of the 12 m main array in two frequency settings in Band 6, one for the 12CO(J = 2–1) line and one for the 13CO(J = 2–1) line (only Cycle 1). In both cases, the data set contains four 1.875 GHz spectral windows with 3840 channels each. The baselines range from 13 to 12934 m. Olofsson et al. (2015) concluded that very little flux is lost even in the 12CO(2–1) ALMA data, in particular at the extreme velocities and close to the systemic velocity. Bandpass calibration was performed on J1107-4449, and gain calibration on J1131-5818 (Cycle 1) and J1132-5606 (Cycle 3). Flux calibration was done using Ceres and Titan. Based on the calibrator fluxes, we estimate the absolute flux calibration to be accurate to within 5%.

The data were reduced using CASA 4.5.2. After corrections for the time and frequency dependence of the system temperatures, and rapid atmospheric variations at each antenna using water vapour radiometer data, bandpass and gain calibration were done. For the 12CO(J = 2–1) setting, data obtained in three different configurations were combined. Subsequently, for each individual tuning, self-calibration was performed on the strong continuum. Imaging was done using the CASA clean algorithm after a continuum subtraction was performed on the emission line data. The final line images were created using natural weighting.

Complementary 12CO J = 3–2 and 4–3, and C17O and C18O J = 2–1 line data were obtained using APEX. The Swedish heterodyne facility instruments APEX-1,2 (Vassilev et al. 2008) and APEX-3 were used together with the facility FFT spectrometer covering about 4 GHz. The observations were made from August to October 2015 in dual-beamswitch mode with a beam throw of 2′. Regular pointing checks were made on strong CO line emitters and continuum sources. Typically, the pointing was found to be consistent with the pointing model within 3″. The antenna temperature, , is corrected for atmospheric attenuation. A Jy/K conversion of 40 and 48 was adopted for APEX-1, 2 and APEX-3, respectively. The uncertainty in the absolute intensity scale is estimated to be about ± 20%.

Finally, in our analysis we make use of the 12CO and 13CO J = 1–0 data published by Olofsson & Nyman (1999).

thumbnail Fig. 1

APEX C18O (upper) and C17O (middle), and ALMA 13C17O (lower) J = 2–1 line profiles towards HD101584. The vertical dashed line marks the estimated systemic velocity. A Local Standard of Rest velocity scale is used.

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thumbnail Fig. 2

SiO(5–4) (left, 0.̋08 beam in the lower left corner), H2CO(303–202) (middle, 0.̋6 beam), and CH3OH(8-1–70) (right, 0.̋15 beam) images towards HD 101584 produced by selecting the peak intensity (in absolute terms along the velocity axis) in each pixel. This highlights the morphology of the high-velocity outflow. In particular, the methanol line emission marks the positions of the 4′′ W and 4′′ E EVSs.

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3. Discussion

3.1. The evolutionary nature of HD 101584

The most likely interpretation of the A6Ia spectral classification and the circumstellar characteristics is that HD 101584 is a post-AGB object, but an evolved massive supergiant or possibly a star of young age remain alternatives. However, HD 101584, being a high-latitude source, is not associated with any star-forming region or molecular cloud. Nevertheless, since here we claim the first detection of methanol in an AGB-related object, we provide some further evidence that supports the post-AGB nature of HD 101584.

The circumstellar chemistry (detections of e.g., SO, SO2, and OCS, Olofsson et al., in prep.), the strong 1667 MHz OH maser (te Lintel Hekkert et al. 1992), and the presence of a silicate feature (Bakker et al. 1996b) all strongly favor the idea that the circumstellar medium of HD 101584 is O-rich (C/O < 1).

A stellar 12C/13C ratio that is not consistent with that in the local interstellar medium, 45–70 (e.g., Lucas & Liszt 1998), nor with that of the Sun, 87 (Scott et al. 2006), would be a strong argument for an AGB-related object. We provide such an estimate where opacity and chemistry are expected to have little effect by using the APEX and ALMA detections of the 12C17O and 13C17O J = 2–1 lines, respectively (Fig. 1). We have determined the intensities of the emission coming from the very central region, within 0.̋5 of HD 101584 in the ALMA data and using the narrow feature in a Gaussian line decomposition of the single-dish data (Table A.1). The integrated line intensity ratio is 13±6, suggesting a low 12C/13C ratio in line with matter that has been processed in the CNO-cycle and brought to the surface in an AGB star; Ramstedt & Olofsson (2014), for example, find circumstellar 12CO/13CO ratios in the range 6−30 for M-type AGB stars, an effect believed to be due to evolution on the Red Giant Branch.

The 17O/18O ratio is a measure of the initial mass of an AGB star provided that it is not affected by hot-bottom-burning (HBB), that is, Mi ≲ 4 M⊙ (Hinkle et al. 2016; De Nutte et al. 2017). During HBB the 17O/18O ratio rapidly becomes very high (Justtanont et al. 2015). The intensity ratio of the APEX C17O and C18O J = 2–1 lines (Fig. 1), 0.20 ± 0.08, is expected to be a good measure of the 17O/18O ratio. This shows that HD 101584 has not gone through HBB, and the low ratio suggests an initial mass of ≈1 M⊙ (De Nutte et al. 2017). This low mass is also consistent with the fact that HD 101584 has not evolved into a carbon star, and with the present-day mass estimate of Bakker et al. (1996b) provided that only the core mass remains.

Thus, the inferred isotope ratios provide strong evidence that HD 101584 was a low-mass, M-type AGB star.

3.2. The extreme velocity spots

The high-velocity outflow is marked with a number of emission spots along its extent, particularly prominent in the SiO(5–4) data (Fig. 2). The end-points at about 4′′ W and 4′′ E of the central star are visible as distinct features at the extreme velocities υLSR ≈ –100 and 185 km s-1, respectively, in many of the detected molecular lines (we refer to Olofsson & Nyman 1999). Notably, the H2CO (303–202, 322–221, and 321–220) line emissions emanate most strongly from these extreme-velocity spots (EVSs) (Fig. 2). This suggests special conditions, either in chemical or excitation terms, and the presence of shocked gas is likely. With an inclination angle of 10°, the physical distances between the star and the EVSs are ≈3×1017 cm, that is, ≈0.1 pc or 20 000 au.

3.3. The detection of methanol

We detect two CH3OH lines, the JK = 42–31 line at 218.440 GHz and the 8-1–70 line at 229.759 GHz (Fig. 3). In the frequency range covered by our ALMA data, these are also the strongest lines in, for example, star-forming regions (Nummelin et al. 1998), where the 8-1–70 line has a tendency to show maser emission (Kalenskii et al. 2002), but there is no indication of this in our data. At the sensitivity obtained, the CH3OH line emission comes exclusively from the EVSs (Fig. 2), further supporting the idea that the conditions are special in these regions. To our knowledge, this is the first detection ever of methanol in an AGB-related object. We note that IRAS 19312+1950 has been detected in methanol, but it has been convincingly shown to be a young object rather than an AGB star (Cordiner et al. 2016). Likewise, methanol was detected towards IRC+10420, but this is an evolved massive star (Quintana-Lacaci et al. 2016).

thumbnail Fig. 3

Methanol lines detected towards the 4′′ W (blue) and 4′′ E (red) EVSs; 42–31 (bottom), 8-1–70 (top). The lines are integrated over 1′′× 1′′ areas centered on the spots. The feature at ≈130 km s-1 is due to the H2CO(322–221) line. The vertical dashed line marks the estimated systemic velocity. A Local Standard of Rest velocity scale is used.

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3.4. Molecular abundances

We need a physical model for an EVS to derive the molecular abundances through a radiative transfer analysis. The observational data provide limited information here except that the emission is largely confined to a region of size ≲1′′, and the emission from the rarer species seems to come from a region at least two times smaller than this. The geometry is also uncertain. In order to get at least order-of-magnitude estimates we assume a spherical clump with an inner higher-density, higher-temperature region (015 in diameter) surrounded by an outer lower-density, lower-temperature envelope (1′′ in diameter; required to mainly reproduce the CO line intensities); we refer to Table 1. Radiative excitation due to central star light (too distant) and dust emission inside the clump (too low optical depth) can be safely ignored.

Based on this physical model we solve the radiative transfer using an Accelerated-Lambda-Iteration code, taking into account excitation through collisions with H2. Collisional coefficients for CH3OH were taken from Pottage et al. (2004). We have not included the torsionally excited states of methanol, which may lead to an underestimate of its abundance by up to a factor of two. We use as input the line intensities for the 4′′ E EVS where the emission is slightly stronger (Table A.2). The size of the higher-density region is constrained by requiring that the 28SiO/29SiO abundance ratio equals 20 (the solar value) since an AGB star is not expected to alter this ratio. Its size fits well the observed sizes of the most intense molecular line emissions of, for example, H2CO and CH3OH. The densities and kinetic temperatures are reasonably constrained by the observed CO, H2CO, and CH3OH line intensities (Table 1).

The resulting fractional abundances with regards to H2 are listed in Table 1. The 12CO abundance (5 × 10-4) is at the level expected in an O-rich circumstellar gas (full association of CO and solar values for O and C results in a fractional CO abundance of 5 × 10-4). Furthermore, the 12CO/13CO ratio is ≈15, that is, in very good agreement with the value derived in Sect. 3.1. Importantly, this means that the EVS material is dominated by circumstellar gas (possibly swept-up from the previous AGB wind), not by swept-up interstellar material. This is strengthened by the H2CO/H213CO line intensity ratio, 12. The C16O/C18O ratio of 210 (the solar value is 480, Scott et al. 2006) is somewhat low since AGB stars are expected to destroy rather than produce 18O, but considering our simple model we draw no conclusions based on this result.

The estimated gas mass of the 4′′ E EVS is 4 × 10-3 M⊙. A crude estimate shows that such a clump would produce a 1.3 mm continuum flux density that is lower than the noise limit in our ALMA data.

Table 1

Radiative transfer results.

3.5. Chemistry

We focus here on the results for the inner region of the 4′′ E EVS. The SO (1 × 10-6), SiO (5 × 10-6), and CS (1 × 10-6; after correcting the 13CS abundance by the estimated 12C/13C ≈ 10) abundances all lie in the range reported for AGB CSEs (Danilovich et al. 2016; Schöier et al. 2013; Velilla Prieto et al. 2017), while the H2CO abundance (2 × 10-6; assuming an ortho-to-para ratio of 3) is about an order of magnitude higher than in IK Tau (Velilla Prieto et al. 2017). CH3OH has an estimated abundance of 3 × 10-6 (assuming an E-to-A ratio of 1), almost two orders of magnitude higher than towards the supergiant IRC+10420 (Quintana-Lacaci et al. 2016). However, the large distance between HD 101584 and the EVS (3 × 1017 cm) combined with a reasonable expansion velocity of the AGB wind (15 km s-1) indicate a time scale of ≈6500 yr. This strongly suggests that due to photodissociation all detected species, except CO which is self-shielding, have their origin in the EVS.

A comparison with the results for OH231.8+4.2, a post-AGB object with a rich molecular setup (incl. SO, SiO, CS, and H2CO) and a number of characteristics similar to those of HD 101584 (Velilla Prieto et al. 2015), shows that also here some of the species are particularly abundant in regions where shocks are likely present, although these are not associated with the outer extremes of its high-velocity outflow. Another interesting comparison can be made with the results for the high-velocity outflows of young stellar objects (YSOs), where in particular the features at the extreme velocities resemble the EVS emission features of HD 101584 (Bachiller et al. 1991a,b). Interestingly, the detected abundant molecules, including CH3OH, are largely to be the same (Tafalla et al. 2010); as are the masses and temperatures of the clumps.

It is therefore tempting to compare with the work on the chemistry of such outflows, for example, that of L1157-B1 (Codella et al. 2010; Benedettini et al. 2013). In this case a chemical model where gas-grain interaction, including freeze-out and chemical processing over ≈105 yr, and subsequent release of the formed species by a C-shock, works reasonably well to explain the observed abundances (e.g., Viti et al. 2011). However, there are notable differences with HD 101584. In the latter, the shock works on pre-existing circumstellar grains, not interstellar grains coated in a proto-stellar environment. Further, in HD 101584 the observed CH3OH/H2CO abundance ratio is ≈1 as opposed to a value of ≈20 for L1157-B1 (Benedettini et al. 2013). Finally, H2S is detected in L1157-B1 (Holdship et al. 2016), while this is not the case for the EVSs of HD 101584 despite the fact that the H2S(220–211) line, emanating from the central region of HD 101584, is almost as strong as the 12CO(2–1) line (about 30% of its strength) (Olofsson et al., in prep.). An alternative explanation could be evaporation of pre-existing planetary system objects, but also here the observed CH3OH/H2CO abundance ratio is very different, for example, ≈10 in comets (de Val-Borro et al. 2013). Lacking an obvious explanation, but building on the similarity with the YSO high-velocity outflows, we propose that the circumstellar grains around HD 101584 have had time to develop some surface chemistry, the result of which is liberated when the high-velocity gas hits the circumstellar medium.

4. Conclusions

We have, for the first time, detected CH3OH towards an AGB-related object, HD 101584. Among other things, this is interesting since the detection of methanol is normally taken as being characteristic of star-forming activity. The detections of CS, SO, SiO, H2CO, and CH3OH in the EVSs of HD 101584 follow a very similar pattern of molecular detections in the extreme velocity flows of YSOs. However, there are significant differences both in the environmental conditions and in the observed (relative) abundances. Nevertheless, based on the similarity, we propose that the detected molecular species in the EVSs have their origin in a post-shock chemistry where circumstellar grains play a role; the details of this situation, however, remain to be elucidated. It would be interesting to perform searches for CH3OH in other post-AGB objects where shocks are likely to be present, for example, the water fountain sources (e.g., Tafoya et al. 2014). Finally, we have added evidence that HD 101584 is a post-AGB object, the remnant of a solar-mass M-type AGB star.

Acknowledgments

H.O. and W.V. acknowledge support from the Swedish Research Council. W.V. acknowledges support from the ERC through consolidator grant 614264. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00248.S and #2015.1.00078.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This paper makes use of the following APEX data: O-093.F-9307 and O-096.F-9303. The Atacama Pathfinder EXperiment (APEX) is a collaboration between the Max-Planck-Institut für Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory.

References

  1. Bachiller, R., Martin-Pintado, J., & Fuente, A. 1991a, A&A, 243, L21 [NASA ADS] [Google Scholar]
  2. Bachiller, R., Martin-Pintado, J., & Planesas, P. 1991b, A&A, 251, 639 [NASA ADS] [Google Scholar]
  3. Bakker, E. J., Lamers, H. J. G. L. M., Waters, L. B. F. M., & Waelkens, C. 1996a, A&A, 310, 861 [NASA ADS] [Google Scholar]
  4. Bakker, E. J., Lamers, H. J. G. L. M., Waters, L. B. F. M., et al. 1996b, A&A, 307, 869 [NASA ADS] [Google Scholar]
  5. Benedettini, M., Viti, S., Codella, C., et al. 2013, MNRAS, 436, 179 [NASA ADS] [CrossRef] [Google Scholar]
  6. Breen, S. L., Ellingsen, S. P., Contreras, Y., et al. 2013, MNRAS, 435, 524 [NASA ADS] [CrossRef] [Google Scholar]
  7. Charnley, S. B., & Latter, W. B. 1997, MNRAS, 287, 538 [NASA ADS] [CrossRef] [Google Scholar]
  8. Codella, C., Lefloch, B., Ceccarelli, C., et al. 2010, A&A, 518, L112 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  9. Cordiner, M. A., Boogert, A. C. A., Charnley, S. B., et al. 2016, ApJ, 828, 51 [NASA ADS] [CrossRef] [Google Scholar]
  10. Danilovich, T., De Beck, E., Black, J. H., Olofsson, H., & Justtanont, K. 2016, A&A, 588, A119 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  11. De Nutte, R., Decin, L., Olofsson, H., et al. 2017, A&A, 600, A71 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  12. de Val-Borro, M., Küppers, M., Hartogh, P., et al. 2013, A&A, 559, A48 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  13. Díaz, F., Hearnshaw, J., Rosenzweig, P., et al. 2007, in IAU Symp. 240, ed. W. I. Hartkopf, P. Harmanec, & E. F. Guinan, 127 [Google Scholar]
  14. Gómez, J. F., Uscanga, L., Suárez, O., Rizzo, J. R., & de Gregorio-Monsalvo, I. 2014, Rev. Mexicana Astron. Astrofis., 50, 137 [NASA ADS] [Google Scholar]
  15. Hinkle, K. H., Lebzelter, T., & Straniero, O. 2016, ApJ, 825, 38 [NASA ADS] [CrossRef] [Google Scholar]
  16. Holdship, J., Viti, S., Jimenez-Serra, I., et al. 2016, MNRAS, 463, 802 [NASA ADS] [CrossRef] [Google Scholar]
  17. Justtanont, K., Barlow, M. J., Blommaert, J., et al. 2015, A&A, 578, A115 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  18. Kalenskii, S. V., Slysh, V. I., & Val’tts, I. E. 2002, Astron. Rep., 46, 96 [NASA ADS] [CrossRef] [Google Scholar]
  19. Lucas, R., & Liszt, H. 1998, A&A, 337, 246 [NASA ADS] [Google Scholar]
  20. Millar, T. J. 2016, J. Phys. Conf. Ser., 728, 052001 [CrossRef] [Google Scholar]
  21. Nummelin, A., Bergman, P., Hjalmarson, Å., et al. 1998, ApJS, 117, 427 [NASA ADS] [CrossRef] [Google Scholar]
  22. Olofsson, H., & Nyman, L.-Å. 1999, A&A, 347, 194 [NASA ADS] [Google Scholar]
  23. Olofsson, H., Vlemmings, W. H. T., Maercker, M., et al. 2015, A&A, 576, L15 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  24. Parthasarathy, M., & Pottasch, S. R. 1986, A&A, 154, L16 [NASA ADS] [Google Scholar]
  25. Pottage, J. T., Flower, D. R., & Davis, S. L. 2004, MNRAS, 352, 39 [NASA ADS] [CrossRef] [Google Scholar]
  26. Quintana-Lacaci, G., Agúndez, M., Cernicharo, J., et al. 2016, A&A, 592, A51 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  27. Ramstedt, S., & Olofsson, H. 2014, A&A, 566, A145 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  28. Sahai, R., Morris, M., Sánchez Contreras, C., & Claussen, M. 2007, AJ, 134, 2200 [NASA ADS] [CrossRef] [Google Scholar]
  29. Sánchez Contreras, C., Velil la Prieto, L., Agúndez, M., et al. 2015, A&A, 577, A52 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  30. Schöier, F. L., Ramstedt, S., Olofsson, H., et al. 2013, A&A, 550, A78 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  31. Scott, P. C., Asplund, M., Grevesse, N., & Sauval, A. J. 2006, A&A, 456, 675 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  32. Sivarani, T., Parthasarathy, M., García-Lario, P., Manchado, A., & Pottasch, S. R. 1999, A&AS, 137, 505 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  33. Tafalla, M., Santiago-García, J., Hacar, A., & Bachiller, R. 2010, A&A, 522, A91 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  34. Tafoya, D., Franco-Hernández, R., Vlemmings, W. H. T., Pérez-Sánchez, A. F., & Garay, G. 2014, A&A, 562, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  35. te Lintel Hekkert, P. T. L., Chapman, J. M., & Zijlstra, A. A. 1992, ApJ, 390, L23 [NASA ADS] [CrossRef] [Google Scholar]
  36. Vassilev, V., Meledin, D., Lapkin, I., et al. 2008, A&A, 490, 1157 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  37. Velilla Prieto, L., Sánchez Contreras, C., Cernicharo, J., et al. 2015, A&A, 575, A84 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  38. Velilla Prieto, L., Sánchez Contreras, C., Cernicharo, J., et al. 2017, A&A, 597, A25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  39. Viti, S., Jimenez-Serra, I., Yates, J. A., et al. 2011, ApJ, 740, L3 [NASA ADS] [CrossRef] [Google Scholar]
  40. Willacy, K., & Millar, T. J. 1997, A&A, 324, 237 [NASA ADS] [Google Scholar]

Appendix A: Observational results

Table A.1

Observational results towards the center of HD 101584.

Table A.2

Observational results at the 4′′ E EVS.

All Tables

Table 1

Radiative transfer results.

In the text
Table A.1

Observational results towards the center of HD 101584.

In the text
Table A.2

Observational results at the 4′′ E EVS.

In the text

All Figures

thumbnail Fig. 1

APEX C18O (upper) and C17O (middle), and ALMA 13C17O (lower) J = 2–1 line profiles towards HD101584. The vertical dashed line marks the estimated systemic velocity. A Local Standard of Rest velocity scale is used.

Open with DEXTER
In the text
thumbnail Fig. 2

SiO(5–4) (left, 0.̋08 beam in the lower left corner), H2CO(303–202) (middle, 0.̋6 beam), and CH3OH(8-1–70) (right, 0.̋15 beam) images towards HD 101584 produced by selecting the peak intensity (in absolute terms along the velocity axis) in each pixel. This highlights the morphology of the high-velocity outflow. In particular, the methanol line emission marks the positions of the 4′′ W and 4′′ E EVSs.

Open with DEXTER
In the text
thumbnail Fig. 3

Methanol lines detected towards the 4′′ W (blue) and 4′′ E (red) EVSs; 42–31 (bottom), 8-1–70 (top). The lines are integrated over 1′′× 1′′ areas centered on the spots. The feature at ≈130 km s-1 is due to the H2CO(322–221) line. The vertical dashed line marks the estimated systemic velocity. A Local Standard of Rest velocity scale is used.

Open with DEXTER
In the text

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