# Deuterated methanol on Solar System scale around the HH212 protostar

E. Bianchi, C. Codella, C. Ceccarelli, V. Taquet, S. Cabrit, F. Bacciotti, R.

Bachiller, E. Chapillon, F. Gueth, A. Gusdorf, et al.

► To cite this version:

E. Bianchi, C. Codella, C. Ceccarelli, V. Taquet, S. Cabrit, et al. Deuterated methanol on Solar System scale around the HH212 protostar. Astronomy & Astrophysics - A&A, 2017, 606, pp.id.L7. 10.1051/0004-6361/201731404. hal-01589748

HAL Id: hal-01589748

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

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LETTER TO THE EDITOR

# Deuterated methanol on a solar system scale around the HH212 protostar

E. Bianchi<fnref n="1" />,<fnref n="2" />, C. Codella<fnref n="1" />, C. Ceccarelli<fnref n="3" />,<fnref n="4" />,<fnref n="1" />, V. Taquet<fnref n="1" />, S. Cabrit<fnref n="5" />, F. Bacciotti<fnref n="1" />, R. Bachiller<fnref n="6" />, E. Chapillon<fnref n="7" />,<fnref n="8" />,
F. Gueth<fnref n="8" />, A. Gusdorf<fnref n="9" />, B. Lefloch<fnref n="3" />,<fnref n="4" />, S. Leurini<fnref n="10" />, L. Podio<fnref n="1" />, K. L. J. Rygl<fnref n="11" />, B. Tabone<fnref n="5" />, and M. Tafalla<fnref n="6" />

Received 19 June 2017 / Accepted 14 September 2017

ABSTRACT

*Context.* Deuterium fractionation is a valuable tool for understanding the chemical evolution during the process that leads to the formation of a Sun-like planetary system.

*Aims.* Methanol is thought to be mainly formed during the prestellar phase, and its deuterated form keeps a memory of the conditions at that epoch. The unique combination of high angular resolution and sensitivity provided by ALMA enables us to measure methanol deuteration in the planet formation region around a Class 0 protostar and to understand its origin.

*Methods.* We mapped both the ¹³CH₃OH and CH₂DOH distribution in the inner regions (~100 au) of the HH212 system in Orion B. To this end, we used ALMA Cycle 1 and Cycle 4 observations in Band 7 with angular resolution down to ~0.′15.

*Results.* We detected 6 lines of ¹³CH₃OH and 13 lines of CH₂DOH with upper level energies of up to 438 K in temperature units. We derived a rotational temperature of (171 ± 52) K and column densities of 7 × 10¹<fnref n="6" /> cm⁻<fnref n="2" /> (¹³CH₃OH) and 1 × 10¹<fnref n="7" /> cm⁻<fnref n="2" /> (CH₂DOH), respectively. This yields a D/H ratio of (2.4 ± 0.4) × 10⁻<fnref n="2" />, which is lower by an order of magnitude than previously measured values using single-dish telescopes toward protostars located in Perseus. Our findings are consistent with the higher dust temperatures in Orion B with respect to the temperature derived for the Perseus cloud. The emission traces a rotating structure extending up to 45 au from the jet axis, which is elongated by 90 au along the jet axis. So far, the origin of the observed emission appears to be related with the accretion disc. Only higher spatial resolution measurements will be able to distinguish between different possible scenarios, however: disc wind, disc atmosphere, or accretion shocks.

**Key words.** stars: formation – ISM: molecules – ISM: individual objects: HH212 – ISM: abundances

**1. Introduction**

Molecular deuteration is a powerful diagnostic tool for studying the past history of the gas associated with the formation of a proto-Sun and its protoplanetary system (see e.g. Ceccarelli et al. 2014, and references therein). In the prestellar core phase, the low temperatures and the resulting CO freeze-out enhance the abundance of the deuterated molecules. These molecules are stored in the icy grain mantles and are then released into the gas phase in the protostellar stage (Ceccarelli et al. 2007; Caselli et al. 2008). This is the case of methanol (CH₃OH), which is formed on the grain surfaces (e.g. Tielens 1983; Rimola et al. 2014) and is then released into the gas phase because dust mantles are thermally evaporated in the inner warm regions around

low-mass protostars (e.g. Ceccarelli et al. 2000, 2007; Parise et al. 2002, 2004, 2006) and/or sputtered by shocks (Codella et al. 2012; Fontani et al. 2014).

Deuterated methanol has been analysed towards Class 0 protostars (Parise et al. 2006): the measured D/H of 0.4–0.6 indicates that CH₂DOH can be almost as abundant as CH₃OH. In the only other more evolved source studied so far, the same ratio appears to be lower (D/H ~ 1–7 × 10⁻<fnref n="3" />), suggesting a decrease in deuterated species that is due to evolutionary effects (Bianchi et al. 2017). However, all the existing observations have been performed with single-dish telescopes (angular resolution ≥10′′), which do not distinguish the different components associated with a protostellar system (jet, high-velocity shocks, slower accretion shocks, and inner envelope). Sub-arcsecond resolution

<footnote n="1">¹ INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
e-mail: ebianchi@arcetri.astro.it</footnote>

<footnote n="2">² Università degli Studi di Firenze, Dipartimento di Fisica e Astronomia, via G. Sansone 1, 50019 Sesto Fiorentino, Italy</footnote>

<footnote n="3">³ Univ. Grenoble Alpes, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38401 Grenoble, France</footnote>

<footnote n="4">⁴ CNRS, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38401 Grenoble, France</footnote>

<footnote n="5">⁵ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06,
École Normale Supérieure, 75014 Paris, France</footnote>

<footnote n="6">⁶ IGN, Observatorio Astronómico Nacional, Alfonso XII 3, 28014 Madrid, Spain</footnote>

<footnote n="7">⁷ Laboratoire d'astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France</footnote>

<footnote n="8">⁸ IRAM, 300 rue de la Piscine, 38406 Saint-Martin-d'Hères, France</footnote>

<footnote n="9">⁹ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, École Normale Supérieure, 75005 Paris, France</footnote>

<footnote n="10">¹⁰ INAF-Osservatorio Astronomico di Cagliari, via della Scienza 5, 09047 Selargius (CA), Italy</footnote>

<footnote n="11">¹¹ INAF-Istituto di Radioastronomia & Italian ALMA Regional Centre, via P. Gobetti 101, 40129 Bologna, Italy</footnote>
observations are then crucial to measure the D/H ratio within
50–100 au from the protostar, that is, in the region hosting the
protoplanetary discs. Dust grains and ices may also be affected
by the accretion shock near the centrifugal barrier, therefore we
do not know the deuterium fractionation at small scales.

The HH212 star-forming region in Orion (d = 450 pc) is an ideal laboratory for studying the jet-disc system. The HH212-mm Class 0 protostar is driving a bright, extended, and bipo-lar molecular jet extensively observed using IRAM-NOEMA, SMA, and ALMA (e.g. Lee et al. 2006, 2007, 2008, 2015, 2016, 2017a,b; Codella et al. 2007; Cabrit et al. 2007, 2012). A molec- ular disc was revealed in HCO+, C$^{17}$O, and SO emission, using the first ALMA cycles with angular resolutions of ~0′.6. Veloc- ity gradients have been detected along the equatorial plane con- sistent with a rotating disc around a 0.2–0.3 M$_{\odot}$ protostar (Lee et al. 2014; Codella et al. 2014; Podio et al. 2015). A disc with a radius of 60 au has indeed been imaged by Lee et al. (2017a), who observed the dust continuum emission at 850 µm. Finally, Codella et al. (2016) and Leurini et al. (2016) suggested that HDO and CH$_3$OH emission is likely associated with outflowing gas, and possibly with a disc wind. To conclude, the HH212 re- gion is the unique Class 0 protostellar region where a bright jet, a compact rotating disc, and signatures of a disc wind have been revealed. In this Letter, we exploit ALMA Band 7 observations with an angular resolution down to 0′.15 to obtain the first mea- surement of methanol deuteration in the disc formation region.

## 2. Observations

HH212 was observed in Band 7 with ALMA using 34 12 m an-
tennas between 15 June and 19 July 2014 during the Cycle 1
phase. Further observations of HH212 were performed in Band 7
with ALMA using 44 12 m antennas between 6 October and
26 November 2016 during the Cycle 4 phase. The maximum
baselines for Cycle 1 and 4 were 650 m and 3 km, respectively.

In Cycle 1 the spectral windows between 337.1–338.9 GHz and 348.4–350.7 GHz were observed using spectral channels of 488 kHz (0.42–0.43 km s⁻<fnref n="1" />), subsequently smoothed to 1.0 km s⁻<fnref n="1" />. Calibration was carried out following standard procedures, using quasars J0607-0834, J0541-0541, J0423-013, and Ganymede. The continuum-subtracted images have clean-beam FWHMs from 0′.41 × 0′.33 to 0′.52 × 0′.34 (PA = −63°), and an rms noise level of 5–6 mJy beam⁻<fnref n="1" /> in the 1.0 km s⁻<fnref n="1" /> channels. For Cycle 4 spectral units of 977 kHz (0.87 km s⁻<fnref n="1" />) were used to observe the spectral windows between 334.1–336.0 GHz. Calibration was carried out following standard procedures, using quasars J0510+1800, J0552+0313, J0541-0211, and J0552-3627. The continuum-subtracted images have a typical clean-beam FWHM of 0′.15 × 0′.12 (PA = −88°) and an rms noise level of 1 mJy beam⁻<fnref n="1" /> in the 0.87 km s⁻<fnref n="1" /> channels. Spectral line imaging was achieved with the CASA package, while the data analysis was performed using the GILDAS<fnref n="1" /> package. Positions are given with respect to the MM1 protostar continuum peak located at α(J2000) = 05h 43m 51s41, δ(J2000) = −01° 02′ 53″17 (Lee et al. 2014). Lines were identified using spectroscopic parameters extracted from the Jet Propulsor Laboratory (JPL<fnref n="2" />, Pickett et al. 1998) and the Cologne Database for Molecular Spectroscopy (CDMS<fnref n="3" />; Müller et al. 2001, 2005).

<figure><img src="image_2.png" /></figure>

**Fig. 1.** Left panel: HH212 protostellar system as observed by ALMA-Band 7 (Codella et al. 2014). Blue and red contours plot the blue- and redshifted SiO(8–7) jet overlaid on the continuum at 0.9 mm (black contours). Positions are with respect to the coordinates reported in Sect. 2. The filled ellipse shows the synthesised beam (HPBW): 0′.61 × 0′.45. Central panels: zoom-in of the central region as observed by ALMA-Band 7 Cycle 1: ¹³CH₃OH(13₀.₁₃–12₁.₁₂)E and CH₂DOH(9₀.₉–8₁.₈)e0 integrated over ±4 km s⁻<fnref n="1" /> with respect to the vsys = +1.7 km s⁻<fnref n="1" />, (black contours and grey scale). First contours and steps are 5σ for ¹³CH₃OH (15 mJy beam⁻<fnref n="1" /> km s⁻<fnref n="1" />) and CH₂DOH (35 mJy beam⁻<fnref n="1" /> km s⁻<fnref n="1" />). The HPBWs are 0′.52 × 0′.34 (PA = −64°) for ¹³CH₃OH and 0′.54 × 0′.35 (PA = −65°) for CH₂DOH. Right panel: zoom-in of the central region, as observed by ALMA-Band 7 Cycle 4, showing the ¹³CH₃OH(12₁.₁₁–12₀.₁₂)A emission integrated over 10 km s⁻<fnref n="1" /> around vsys (black contours and grey scale). First contours and steps are 5σ (20 mJy beam⁻<fnref n="1" /> km s⁻<fnref n="1" />) and 3σ, respectively. The HPBW is 0′.15 × 0′.12 (PA = −88°).

## 3. Results and discussion

### 3.1. *Line spectra and maps*

In Cycle 1 data, we detected 5 lines of ¹³CH₃OH and 12 lines of CH₂DOH covering excitation energies, E_up, from 17 to 438 K (see Table A.1). In addition, in the Cycle 4 dataset we revealed one transition of ¹³CH₃OH (E_up = 193 K) and one of CH₂DOH (E_up = 327 K). Examples of the detected line profiles are shown in Fig. A.1: the emission peaks at velocities between ≈+1 km s⁻<fnref n="1" /> and +3 km s⁻<fnref n="1" />, consistent with the systemic velocity of +1.7 km s⁻<fnref n="1" /> (Lee et al. 2014), when the spectral resolution of 1 km s⁻<fnref n="1" /> is considered. The profiles, fit using the GILDAS package, are Gaussian with typical full width at half-maximum (FWHM) ~5 km s⁻<fnref n="1" />. The spectral parameters of the detected lines are presented in Table A.1. Figure 1 introduces the HH212 system: the 0.9 mm continuum traces the envelope hosting the protostar. The bipolar blue- and red-shifted lobes are traced by SiO (Codella et al. 2007; Lee et al. 2014). The central panels, covering a zoom-in of the central protostellar region (≤0′.5, i.e. 225 au), show the Cycle 1 data, specifically, examples of the emission maps of ¹³CH₃OH and CH₂DOH. The emission is spatially unresolved with a size smaller than the Cycle 1 beam (0′.5 × 0′.3), corresponding to a size of 225 × 135 au. However, the definitely higher angular resolution provided by the Cycle 4 dataset (0′.15×0′.12 corresponding to a radius of 34 × 27 au) provides spatially resolved images of the ¹³CH₃OH and CH₂DOH <fnref n="4" /> emission lines. We used the ¹³CH₃OH emission as revealed in the Cycle 4 image to show in the right panel of Fig. 1 a further zoom-in, sampling the inner 100 au.

<footnote n="1">¹ http://www.iram.fr/IRAMFR/GILDAS</footnote>

<footnote n="2">² https://spec.jpl.nasa.gov/</footnote>

<footnote n="3">³ http://www.astro.uni-koeln.de/cdms/</footnote>

<footnote n="4">⁴ The CH₂DOH line is blended with the SO₂(8₂.₆–7₁.₇) line (Table A.1).</footnote>
## 3.2. Methanol deuteration

We used the ¹³CH₃OH lines detected in Cycle 1 to perform a rotation diagram analysis, assuming local thermal equilibrium (LTE) conditions and optically thin lines. In order to exclude opacity effects, we used the ¹³CH₃OH lines to derive the CH₃OH column density because the main isotopologue lines observed by Leurini et al. (2016) are moderately optically thick ($\tau < 0.4$). We also verified that the CH₂DOH transitions are indeed optically thin using a population diagram analysis (Goldsmith & Langer 1999) in which opacities are self-consistently computed. We used ¹³CH₃OH and CH₂DOH lines extracted from the same ALMA dataset in order to have the same u–v coverage and to minimise calibration effects. Moreover, the Cycle 0 (beam ≈0′6) observations of CH₃OH (Leurini et al. 2016) trace a much warmer component dominated by lines with $E_{up}$ up to 747 K with respect to the emission lines analysed in this paper. A source size of 0′19 ± 0′02 has been derived from the ¹³CH₃OH Cycle 4 map integrated over the whole emission range and then used to correct the Cycle 1 observed values. This value is in good agreement with ~0′2, as derived from CH₃OH (Leurini et al. 2016). Figure A.2 shows the derived rotational temperature and column density, which are $T_{\text{tot}} = (171 \pm 52)$ K and $N_{\text{tot}} = (6.5 \pm 2.1) \times 10^{16}$ cm⁻², respectively. Conservatively, we used only Cycle 1 data to perform the fit; however, the ¹³CH₃OH Cycle 4 line is in good agreement with Cycle 1 observations. In the lower panel of Fig. A.2 we derive the column density of CH₂DOH, assuming the same rotational temperature and size derived for ¹³CH₃OH. We excluded from the fitting the two CH₂DOH transitions with $E_{up} > 300$ K to exclude any possible contamination from non-thermal excitation processes or the occurrence of a component with a different higher excitation condition. However, the fitting obtained with the low-energy transitions (continuous line) is in agreement with the two excluded transitions, as well as with the Cycle 4 transition, as shown by the dotted line. The derived column density for CH₂DOH is then $N_{\text{tot}} = (1.1 \pm 0.2) \times 10^{17}$ cm⁻². We note that an LVG analysis (see Ceccarelli et al. 2003, for further details) of the ¹³CH₃OH emission indicates a source size of 0′1–0′2, $T_{\text{kin}}$ larger than 100 K and densities higher than $10^6$ cm⁻³, in agreement with the HDO results reported by Codella et al. (2016).

The column densities derived from the rotation diagrams were used to derive the methanol D/H for the first time in the inner 100 au around a low-mass protostar. When we assume a ¹²C/¹³C ratio of 70 (Milam et al. 2005) at the galactocentric distance of HH212 (~8.3 kpc), the D/H is (2.4 ± 0.4) × 10⁻². This value is in agreement with the upper limit of 0.27 derived by Lee et al. (2017b) using CH₂DOH and three lines of CH₃OH. In addition, our measurement is lower than previous values of CH₂DOH in other Class 0 objects performed with the IRAM 30 m single dish, which indicate D/H ≈ 40–60% (Parise et al. 2006). Taking into account that as reported by Belloche et al. (2016), the column densities of CH₂DOH derived in Parise et al. (2006) were overestimated by a factor ~2 because of a problem in the spectroscopic parameters, the HH212 deuteration is still one order of magnitude lower. What are the reasons of this difference? To start with, the single-dish measurements by Parise et al. (2006) are sampling regions ≥2000 au: the D/H is calculated assuming that the main isotopologue and the deuterated species come from the same emitting source, but this cannot be verified with low angular resolutions. This issue is overcome with high angular resolution observations, like those presented here, which allow us to directly image the emitting region. Interestingly, Jørgensen et al. (2016) reported a level of deuteration

for glycolaldehyde of ~5% in IRAS 16293 in Ophiuchus on a scale of 50 au. That said, a possible explanation for the lower methanol deuteration measured for HH212 mm could be related to different physical conditions during the formation of methanol on dust mantles during the prestellar phase. A higher gas temperature reduces the atomic gas D/H ratio landing on the grain surfaces and in turn reduces the deuteration of methanol. All the sources observed by Parise et al. (2006) are located in the Perseus star-forming region, which could have had experienced different conditions with respect to the Orion B region where HH212 lies. Specifically, while in Perseus the dust temperature is about ~12 K (Zari et al. 2016), HH212 is located about one degree north of the high-mass star-forming region NGC 2024, and the dust temperature here is ≥16 K (Lombardi et al. 2014). As shown by Taquet et al. (2012, 2014), for instance, after the volume density is fixed, deuteration (including that of methanol) decreases as temperature increases. The models indicate that D/H can decrease by up to one order of magnitude by increasing the temperature from 10 K to 20 K. Interestingly, we note that according to Fuente et al. (2014), the methanol deuteration in the hot core in the intermediate-mass star-forming region NGC 7129, FIRS 2 is ~2%. However, in hot cores associated with massive star-forming regions in Orion (Peng et al. 2012), the methanol D/H is between 0.8 × 10⁻³ and 1.3 × 10⁻³, which is lower by one order of magnitude than the values reported here.

## 3.3. Emitting region of deuterated methanol

Figure 2 shows the channel maps of the two transitions observed during ALMA Cycle 4, that is, at the highest spatial resolution presented here: ¹³CH₃OH (12<sub>1,11</sub>–12<sub>0,12</sub>)A and CH₂DOH (16<sub>2,15</sub>–16<sub>1,15</sub>)b1 (see Table A.1). For both lines the rightmost panels show the spatial distributions of the emission close to the systemic velocity. The remaining panels are for the blue- and redshifted velocities, imaged up to ±4 km s⁻¹. We note that for CH₂DOH the redshifted emission is partially contaminated by the SO₂(8<sub>2,6</sub>–7<sub>1,7</sub>) emission (see Table A.1 and Fig. A.1).

The spatial distribution of the methanol isotopologues at the systemic velocity is elongated along the jet axis (PA = 22°). A fit in the image plane gives for ¹³CH₃OH a beam-deconvolved FWHM size of 0′18(0′02) × 0′12(0′02) at PA = 33°. For CH₂DOH we derived 0′20(0′02) × 0′10(0′02) and PA = 19°. These values correspond to FWHM sizes of 81 × 54 au (¹³CH₃OH) and 90 × 45 au (CH₂DOH). Closer to the blue- and redshifted emission, we resolve a clear velocity gradient parallel to the equatorial plane (see also Fig. A.3) with shifts of ±0′1 = 45 au, in the same sense as the HH212 disc rotation. The typical (beam-deconvolved) size of the blue- and redshifted emission at ±2 km s⁻¹ from systemic is 0′22(0′04) × 0′14(0′04) and 0′18(0′02) × 0′10(0′03), respectively, similar to the size at $V_{\text{sys}}$. Rotation has previously been noted in CH₃OH by Leurini et al. (2016) from unresolved maps at lower resolution (≈0′6). The authors further noted that emission centroids (fitted in u–v plane) moved away from the source, and eventually away from the mid plane, at higher velocity, speculating that the methanol emission is not dominated by a Keplerian disc or the rotating-infalling cavity, and possibly associated with a disc wind. With the present images we reach higher angular resolution, which allows us to refine the picture: the systemic velocity appears to arise mainly from two peaks at ±0′05 = 20 au above and below the disc plane (of which the centroids in Leurini et al. 2016 only traced the barycentre). In addition, channel maps at ±1 km s⁻¹ suggest redshifted emission peaking in the north and blueshifted emission peaking in the south, which is not the sense
<figure><img src="image_3.png" /></figure>

**Fig. 2.** Channel maps of the <sup>13</sup>CH<sub>3</sub>OH(12<sub>1,11</sub>–12<sub>0,12</sub>)A (upper panels) and CH<sub>2</sub>DOH(16<sub>2,15</sub>–16<sub>1,15</sub>)o1 (lower panels) blue- and redshifted (continuum subtracted) emissions observed during ALMA-Cycle 4 towards the HH212 mm protostar. Each panel shows the emission integrated over a velocity interval of 1 km s<sup>-1</sup> shifted with respect to the systemic velocity (see the magenta channel, sampling the velocity between +1.5 km s<sup>-1</sup> and +2.5 km s<sup>-1</sup>) by the value given in the upper-right corner. The black cross (inclined in order to point the SiO jet direction and consequently the equatorial plane, see Fig. 1) indicates the position of the protostar. The ellipse in the top left panel shows the ALMA synthesised beam (HPBW): 0.′15 × 0.′12 (PA = −88°). First contours and steps correspond to 3σ (2.7 mJy beam<sup>-1</sup> km s<sup>-1</sup>). Note that for CH<sub>2</sub>DOH at velocities higher than +1.0 km s<sup>-1</sup> a further emission appears along the jet axes to the north and to the south with respect to the CH<sub>2</sub>DOH emission. This is due to the SO<sub>2</sub>(8<sub>2,6</sub>–7<sub>1,7</sub>) emission line (see Table 1 and Fig. 2), which has been confirmed to be a good tracer of outflowing material (Podio et al. 2015). Given that the velocity scale has been derived by first fixing the CH<sub>2</sub>DOH frequency, the SO<sub>2</sub> emission looks artificially red, but it is clearly blueshifted (see Fig. A.1).

we would naively expect for a wind from HH212 mm. Since the jet axis is so close to the plane of the sky<sup>5</sup>, this might perhaps still be explained by non-axisymmetric structure in a disc wind, but synthetic predictions would be needed to test this. Alternatively, our data suggest that the emission could arise from accretion shocks occurring at the centrifugal barrier associated with the accretion disc, and heating the gas at temperatures around 100 K (Sakai et al. 2014; Oya et al. 2016). The radial extent ~50 au of the observed red- and blueshifted emission is indeed consistent with the dust disc radius ~60 au, recently resolved by Lee et al. (2017a) at 850 µm with ALMA. In this case, we would observe a thicker accretion shock near the centrifugal barrier in HH212, as recently seen in C<sub>2</sub>H in L1527 (Sakai et al. 2017). We may also have a contribution from a warm disc atmosphere, emitting in the northern/southern portions of the accretion disc, thicker than the dust atmosphere.

## 4. Conclusions

The ALMA Cycle 1 and 4 observations allow us to measure methanol deuteration in the inner 50 au of the jet-disc system associated with the Class 0 protostar HH212, in Orion B. The deuteration is ≈2 × 10<sup>-2</sup>, a value lower than has previously been measured using single-dish telescopes towards Class 0 protostars in Perseus. Although we cannot exclude that single-dish observations are mixing different gas components with different D/H values, our findings are consistent with a higher dust temperature in Orion B than in the Perseus cloud. This confirms the diagnostic value of molecular deuteration for recovering the physical conditions during the pre-collapse phase. The emission is confined in a rotating structure that extends at ±45 au from the equatorial plane and is elongated along the jet axis. Disc wind, disc atmosphere, and accretion shocks could explain the observed images. Higher spatial resolution maps are necessary to distinguish between these possibilities.

*Acknowledgements.* We thank C.-F. Lee for instructive comments and suggestions. We also thank the anonymous referee for having improved the manuscript. This paper makes use of the ADS/JAO.ALMA#2012.1.00997.S and ADS/JAO.ALMA#2016.1.01475.S data (PI: C. Codella). 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 work was supported (i) by the Italian Ministero dell'Istruzione, Università e Ricerca (MIUR) through the grant Progetti Premiali 2012 - iALMA (CUP C52113000140001); and (ii) by the program PRIN-MIUR 2015 STARS in the CAOS (Simulation Tools for Astrochemical Reactivity and Spectroscopy in the Cyberinfrastructure for Astrochemical Organic Species, 2015F59J3R, MIUR e della Scuola Normale Superiore). M.T. acknowledges partial support from the project AYA2016-79006-P.

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## Appendix A: Additional material

Table A.1 lists all the methanol isotopologue lines observed towards HH212 mm during ALMA Cycle 1 and Cycle 4 operations. Figure A.1 shows examples of line profiles in $T_B$ scale, while Fig. A.2 shows the rotation diagrams for $^{13}$CH$_3$OH and CH$_2$DOH. Figure A.3 shows the $^{13}$CH$_3$OH(12$_{1,11}$–12$_{0,12}$)A spectrum extracted at ± 0.0′06 from the protostar, in the equatorial plane direction.

<table><caption>**Table A.1.** Emission lines detected in ALMA Cycle 1 and 4 measurements towards HH212 mm.</caption><thead><tr><th>Transition</th><th>ν<sup>a</sup><br>(GHz)</th><th>E<sub>up</sub><sup>a</sup><br>(K)</th><th>Sμ<sup>2a</sup><br>(D<sup>2</sup>)</th><th>rms<br>(K)</th><th>F<sub>int</sub><sup>b</sup><br>(K km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td colspan="6"><strong><sup>13</sup>CH<sub>3</sub>OH Cycle 1</strong></td></tr><tr><td>13<sub>0,13</sub>–12<sub>1,12</sub>A</td><td>338.75995</td><td>206</td><td>13</td><td>0.29</td><td>9.6(1.1)</td></tr><tr><td>13<sub>4,9</sub>–14<sub>3,11</sub>E</td><td>347.78840</td><td>303</td><td>4</td><td>0.36</td><td>4.0(1.4)</td></tr><tr><td>11<sub>0,11</sub>–10<sub>1,9</sub>E</td><td>348.10019</td><td>162</td><td>5</td><td>0.84</td><td>7.5(3.0)</td></tr><tr><td>1<sub>1,1</sub>–0<sub>0,0</sub>A</td><td>350.10312</td><td>17</td><td>2</td><td>1.16</td><td>7.4(3.0)</td></tr><tr><td>8<sub>1,7</sub>–7<sub>2,5</sub>E</td><td>350.42158</td><td>103</td><td>2</td><td>0.93</td><td>8.7(2.6)</td></tr><tr><td colspan="6"><strong>CH<sub>2</sub>DOH Cycle 1</strong></td></tr><tr><td>9<sub>0,9</sub>–8<sub>1,8</sub>e0</td><td>337.34866</td><td>96</td><td>6</td><td>0.15</td><td>15.3(0.5)</td></tr><tr><td>9<sub>1,8</sub>–8<sub>2,6</sub>o1<sup>c</sup></td><td>338.46254</td><td>120</td><td>2</td><td>0.26</td><td>10.7(2.1)<sup>c</sup></td></tr><tr><td>13<sub>1,12</sub>–12<sub>0,12</sub>e0</td><td>338.86898</td><td>202</td><td>2</td><td>0.13</td><td>9.7(0.4)</td></tr><tr><td>6<sub>1,6</sub>–5<sub>0,5</sub>e0</td><td>338.95711</td><td>48</td><td>5</td><td>0.29</td><td>16.7(0.9)</td></tr><tr><td>18<sub>4,15</sub>–18<sub>3,15</sub>e1</td><td>347.76728</td><td>438</td><td>10</td><td>0.09</td><td>6.6(0.3)</td></tr><tr><td>18<sub>4,14</sub>–18<sub>3,16</sub>e1</td><td>347.95281</td><td>438</td><td>10</td><td>0.18</td><td>6.4(0.6)</td></tr><tr><td>4<sub>1,3</sub>–4<sub>0,4</sub>e1</td><td>348.16076</td><td>38</td><td>4</td><td>0.15</td><td>18.1(0.5)</td></tr><tr><td>7<sub>4,4</sub>–7<sub>3,4</sub>e1</td><td>349.95168</td><td>132</td><td>3</td><td>0.16</td><td>25.3(0.5)</td></tr><tr><td>7<sub>4,3</sub>–7<sub>3,5</sub>e1</td><td>349.95272</td><td>132</td><td>3</td><td></td><td></td></tr><tr><td>6<sub>4,3</sub>–6<sub>3,3</sub>e1</td><td>350.02735</td><td>117</td><td>2</td><td>0.23</td><td>19.5(0.7)</td></tr><tr><td>6<sub>4,2</sub>–6<sub>3,4</sub>e1</td><td>350.02777</td><td>117</td><td>2</td><td></td><td></td></tr><tr><td>5<sub>4,2</sub>–5<sub>3,2</sub>e1</td><td>350.09024</td><td>104</td><td>2</td><td>0.63</td><td>20.0(2.2)</td></tr><tr><td>5<sub>4,1</sub>–5<sub>3,3</sub>e1</td><td>350.09038</td><td>104</td><td>2</td><td></td><td></td></tr><tr><td>6<sub>2,5</sub>–5<sub>1,5</sub>e1<sup>c</sup></td><td>350.45387</td><td>72</td><td>4</td><td>0.63</td><td>17.0(3.9)<sup>c</sup></td></tr><tr><td>5<sub>1,4</sub>–5<sub>0,5</sub>e1</td><td>350.63207</td><td>49</td><td>5</td><td>0.60</td><td>21.0(2.0)</td></tr><tr><td colspan="6"><strong><sup>13</sup>CH<sub>3</sub>OH Cycle 4</strong></td></tr><tr><td>12<sub>1,11</sub>–12<sub>0,12</sub>A</td><td>335.56021</td><td>193</td><td>23</td><td>0.81</td><td>61.7(2.7)</td></tr><tr><td colspan="6"><strong>CH<sub>2</sub>DOH Cycle 4</strong></td></tr><tr><td>16<sub>2,15</sub>–16<sub>1,15</sub>o1<sup>d</sup></td><td>334.68395</td><td>327</td><td>8</td><td>0.67</td><td>51.1(2.9)<sup>d</sup></td></tr></tbody></table>

**Notes.** (a) Frequencies and spectroscopic parameters are extracted from the Jet Propulsion Laboratory molecular database (JPL, Pickett et al. 1998) and from the Cologne Database for Molecular Spectroscopy (CDMS, Müller et al. 2001). Upper level energies refer to the ground state of each symmetry. (b) Gaussian fit. (c) The line transition (9$_{1,8}$–8$_{2,6}$)o1 is partially blended with the (7$_{-5,2}$–6$_{-5,1}$)E1 CH$_3$OH transition. The line (6$_{2,5}$–5$_{1,5}$)e1 is partially blended with the (18$_{1,17}$–17$_{1,16}$)E CH$_3$CHO transition. (d) The CH$_2$DOH (16$_{2,15}$–16$_{1,15}$) o1 line ($E_u$ = 327 K, $S_{ij}μ^2$ = 8 D$^2$) is partially blended with the SO$_2$ (8–7) transition.

<figure><img src="image_4.png" /><figcaption>**Fig. A.1.** Examples of line profiles in $T_B$ scale (not corrected for the beam dilution): species and transitions are reported. The vertical dashed line stands for the systemic $V_{LSR}$ velocity (+1.7 km s$^{-1}$, Lee et al. 2014). Red and blue curves are for the Gaussian fit. In the spectrum of the Cycle 1 (1$_{1,1}$–0$_{0,0}$)A $^{13}$CH$_3$OH transition, a CH$_2$DOH doublet containing the (5$_{4,2}$–5$_{3,2}$)e1 and the (5$_{4,1}$–5$_{3,3}$)e1 transitions is also shown (see Table A.1). In Cycle 4 spectra the (7$_{1,7}$–6$_{1,6}$)A CH$_3$OH and the (8$_{2,6}$–7$_{1,7}$) SO$_2$ transitions are also shown.</figcaption></figure>

<figure><img src="image_5.png" /><figcaption>**Fig. A.2.** Rotation diagrams for $^{13}$CH$_3$OH (upper panel) and CH$_2$DOH (lower panel). An emitting region size of 0.0′19 is assumed (see text). The parameters $N_u$, $g_u$, and $E_{up}$ are the column density, the degeneracy, and the energy of the upper level, respectively. The derived value of the rotational temperature is reported for $^{13}$CH$_3$OH. For CH$_2$DOH the $T_{rot}$ derived from the $^{13}$C-isotopologues is assumed to derive the column density. The two CH$_2$DOH transitions with excitation energies higher than 400 K as well as the Cycle 4 point are excluded from the fit, although they are in good agreement with it.</figcaption></figure>
<figure><img src="image_6.png" /></figure>

**Fig. A.3.** Comparison in flux density and in $T_B$ scales ($T_B/F_ν = 482.609$ K Jy$^{-1}$) between the $^{13}$CH$_3$OH(12$_{1,11}$–12$_{0,12}$)A spectrum extracted at ±0.06 from the protostar (see Fig. 2: blue- and redshifted emission towards north-west and south-east, respectively) in the direction along the equatorial plane (i.e. disc plane; Lee et al. 2017). The vertical dashed line stands for the systemic $V_{LSR}$ velocity (+1.7 km s$^{-1}$, Lee et al. 2014).