# Resolving the binary components of the outbursting protostar HBC 494 with ALMA

Pedro Henrique Nogueira, Alice Zurlo, Sebastián Pérez, Camilo

González-Ruilova, Lucas A Cieza, Antonio Hales, Trisha Bhowmik, Dary A

Ruíz-Rodríguez, David A Principe, Gregory J Herczeg, et al.

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

► To cite this version:

Pedro Henrique Nogueira, Alice Zurlo, Sebastián Pérez, Camilo González-Ruilova, Lucas A Cieza, et al. Resolving the binary components of the outbursting protostar HBC 494 with ALMA. Monthly Notices of the Royal Astronomical Society, 2023, 523 (4), pp.4970-4991. 10.1093/mnras/stad1614. hal-04961179

HAL Id: hal-04961179

https://hal.science/hal-04961179v1

Submitted on 21 Feb 2025

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_2.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
# Resolving the binary components of the outbursting protostar HBC 494 with ALMA

Pedro Henrique Nogueira Ⓒ,¹,²★ Alice Zurlo Ⓒ,¹,² Sebastián Pérez Ⓒ,²,³,⁴ Camilo González-Ruilova Ⓒ,¹,²,⁵
Lucas A. Cieza Ⓒ,¹,² Antonio Hales Ⓒ,⁶,⁷ Trisha Bhowmik Ⓒ,¹,²,³ Dary A. Ruíz-Rodríguez Ⓒ,⁷
David A. Principe Ⓒ,⁸ Gregory J. Herczeg Ⓒ,⁹ Jonathan P. Williams Ⓒ,¹⁰ Jorge Cuadra Ⓒ,¹¹,¹²
Matías Montesinos Ⓒ,¹²,¹³ Nicolás Cuello Ⓒ,¹⁴ Prachi Chavan Ⓒ,¹,² Simon Casassus Ⓒ,²,¹⁵,¹⁶,¹⁷
Zhaohuan Zhu Ⓒ¹⁸,¹⁹ and Felipe G. Goicovic Ⓒ²⁰

*Affiliations are listed at the end of the paper*

Accepted 2023 May 24. Received 2023 May 19; in original form 2023 January 25

## ABSTRACT

Episodic accretion is a low-mass pre-main sequence phenomenon characterized by sudden outbursts of enhanced accretion. These objects are classified into two: protostars with elevated levels of accretion that lasts for decades or more, called FUors, and protostars with shorter and repetitive bursts, called EXors. HBC 494 is a FUor object embedded in the Orion Molecular Cloud. Earlier Atacama Large (sub-)Millimeter Array (ALMA) continuum observations showed an asymmetry in the disc at 0.′2 resolution. Here, we present follow-up observations at ~0.′03, resolving the system into two components: HBC 494 N (primary) and HBC 494 S (secondary). No circumbinary disc was detected. Both discs are resolved with a projected separation of ~0.′18 (75 au). Their projected dimensions are 84 ± 1.8 × 66.9 ± 1.5 mas for HBC 494 N and 64.6 ± 2.5 × 46.0 ± 1.9 mas for HBC 494 S. The discs are almost aligned and with similar inclinations. The observations show that the primary is ~5 times brighter/more massive and ~2 times bigger than the secondary. We notice that the northern component has a similar mass to the FUors, while the southern has to EXors. The HBC 494 discs show individual sizes that are smaller than single eruptive YSOs. In this work, we also report ¹²CO, ¹³CO, and C¹⁸O molecular line observations. At large scale, the ¹²CO emission shows bipolar outflows, while the ¹³CO and C¹⁸O maps show a rotating and infalling envelope around the system. At a smaller scale, the ¹²CO and ¹³CO moment zero maps show cavities within the continuum discs' area, which may indicate continuum over-subtraction or slow-moving jets and chemical destruction along the line of sight.

**Key words:** accretion, accretion discs – protoplanetary discs – stars: protostars – ISM: jets and outflows – radio continuum: planetary systems – radio lines: planetary systems.

## 1 INTRODUCTION

During their evolution, young stellar objects (YSOs) dissipate their envelopes while feeding their developing protostars through accretion via a disc. However, YSOs are underluminous compared to the luminosity and accretion rates expected from steady disc accretion. This discrepancy has been established as the ‘luminosity problem’ (Kenyon et al. 1990; Evans Neal J. et al. 2009). One potential solution to the luminosity problem is that young stars undergo episodes of high accretion interspersed by quiescent phases. During the episodes of enhanced accretion, large amounts of material are accreted very quickly (e.g. Dunham & Vorobyov 2012). Such phenomena have been observed in low-mass pre-main sequence stars like FU Orionis and EX Lupi, the prototypes of the two subclasses that display the episodic accretion phenomenon.

FU Orionis type stars, also known as FUors, are pre-main sequence low-mass stars that show variability in both luminosity and spectral type due to variation in the accretion mass rate, on a short time-scale

(Herbig 1966). Their optical brightness can dramatically increase due to enhanced mass accretion by more than five magnitudes over a few months. After this outburst, FUors can remain in this active state for decades. This occurrence is considered episodic and suspected to be common at the early stages of star formation. Throughout an outburst, the star can accrete ~0.01 M$_{\odot}$ of material, roughly the mass of a typical T-Tauri disc (Andrews & Williams 2005). The bolometric luminosity of the FUors during the outburst is 100–300 L$_{\odot}$ and the accretion rate is between 10$^{-6}$ and 10$^{-4}$ M$_{\odot}$ yr$^{-1}$ (Audard et al. 2014). EX Lupi type stars, also known as EXors, are a scaled-down version of the FUors, with shorter and less intense outbursts (Herbig 2007). The EXors enhanced accretion stage can last months to years, with accretion rates ranging from 10$^{-7}$ to 10$^{-6}$ M$_{\odot}$ yr$^{-1}$, which are the order up to 5 magnitudes brighter than quiescent periods. The episodic recurrence is also on the order of years (e.g. Jurdana-Šepić et al. 2018; Giannini et al. 2022).

The mechanisms producing the eruptions in systems like FUors and EXors have yet to be understood (Cieza et al. 2018). Several different triggers have been proposed to explain this phenomenon, such as disc fragmentation (Vorobyov & Basu 2005; Zhu et al. 2012; Vorobyov & Basu 2015), coupling of gravitational and magneto-

<footnote>* E-mail: nogueirapedro404@gmail.com, pedro.soares@mail.udp.cl</footnote>
rotational instability (MRI) (Armitage, Livio & Pringle 2001; Zhu et al. 2009), and tidal interaction between the disc and a companion (Bonnell & Bastien 1992; Lodato & Clarke 2004; Borchert et al. 2022b). In terms of evolution, a scenario where FUors are understood as an earlier phase followed by an EXor phase could explain some of the observed properties of these systems (Cieza et al. 2018). EXors have less prominent (or lack of) outflows, and smaller masses/luminosities than FUors since the mass loss, accretion, and outbursts will significantly remove the gas and dust material during their evolutionary stages.

If most stars undergo FUor/EXor-like episodic accretions during their evolution, imaging the circumstellar discs of FUors at sub-mm/mm wavelengths can inform or constrain the underlying outburst mechanisms. For class 0/I objects (e.g. those still accreting from their circumstellar discs and envelopes), the massive disc could be expected to be prone to be gravitationally unstable, which can, consequently, trigger the MRI and/or disc fragmentation. Additionally, close encounters of stars can shape both gas and dust disc morphology (Cuello et al. 2019). Inferring which scenario plays in each disc requests an analysis that strongly depends on how well-resolved and which features one can extract from the observations. Consequently, when eruptive discs give a hint of irregular morphology or kinematics, follow-up observations at higher resolution are needed to resolve the substructures and infer the nature of the system.

HBC 494 is a Class I protostar, located in the Orion molecular cloud at a distance of 414 ± 7 pc (Menten et al. 2007), and has been classified as a FUor<fnref n="1" /> (Audard et al. 2014). This young eruptive object (also called Reipurth 50) was discovered during an optical survey and described as a bright, conical, and large nebula reflecting light from a 250 L⊙ infrared 1.5 arcmin away. Both were located at the southern part of the L1641 cloud in Orion (Reipurth 1985; Reipurth & Bally 1986). This nebula was claimed to appear after 1955, and its first detailed study showed high variability between 1982 and 1985, a consequence of a primordial IR source variability. Posterior studies have also confirmed its variability. For example, Chiang et al. (2015) reported a dramatic brightening (thus clearing of part of the nebula) that occurred between 2006 and 2014. These events can be explained by an episode of outflow coming from HBC 494. More recently, Postel et al. (2019), using archival photometry data along with Herschel and Spitzer spectra presented the detection of several molecular lines and the spectral energy distribution (SED) of HBC 494. The SED presented strong continuum emission in the mid- and far-infrared, which is indicative of envelope emission. Such violent outflows were observed and described in Ruíz-Rodríguez et al. (2017).

ALMA Cycle-2 observations in the millimeter continuum (~0.25 angular resolution) show that the disc is elongated with an apparent asymmetry (Cieza et al. 2018), indicating the presence of an unresolved structure or a secondary disc. In this work, we present ALMA Cycle 4 observations at ~0.03 angular resolution that reveal the binary nature of the HBC 494 system. Only Cycle 4 data were used in this work. The paper is structured as follows. The ALMA observations and data reduction are described in Section 2. The results from the continuum and line analysis are described in Section 3. The discussion is presented in Section 4, while we conclude with a summary of our results in Section 5.

<table><caption>**Table 1.** List of the Cycle 4 ALMA observations of the target HBC 494, used in this work.</caption><thead><tr><th>PI</th><th>Project ID</th><th>Angular resolution (beam minor axis)</th><th>Date of observation</th><th>Integration</th></tr></thead><tbody><tr><td>Zurlo</td><td>2016.1.00630.S</td><td>0.142</td><td>2016 October 09</td><td>8.39 min</td></tr><tr><td>Zurlo</td><td>2016.1.00630.S</td><td>0.027</td><td>2017 September 26</td><td>25.55 min</td></tr></tbody></table>

## 2 OBSERVATIONS AND DATA REDUCTION

HBC 494 has been observed during the ALMA Cycle-4 in band 6 (program 2016.1.00630.S; PI: Zurlo) for two nights, one on the 2016 October 9 and the other on the 2017 September 26 (see Table 1). On the first night, the short baseline configuration was acquired, with a precipitable water vapour of 0.42 mm. The ALMA configuration of antennas was composed of 40 12-m antennas with a baseline from 19 to 3144 m. The flux calibrator and bandpass calibrator were both J0522-3627, and the phase calibrator was J0607-0834. The total integration on the target was 8.39 min. The second night, the long baseline data set, had precipitable water vapour of 1.08 mm. The ALMA configuration consisted of 40 12-m antennas with a baseline from 42 to 14 851 m. The flux calibrator was J0423-0120, the bandpass calibrator was J0510+1800, and the phase calibrator was J0541-0541. The total integration on the target was 25.55 min.

The central frequencies of each spectral window were: 230.543 (to cover the transition ¹²CO J=2-1), 233.010 (continuum), 220.403 (¹³CO J=2-1), 219.565 (C¹⁸O J=2-1), and 218.010 (continuum) GHz. The minimum spectral resolution achieved (second night) for ¹²CO was 15.259 kHz (~ 0.02 km s⁻<fnref n="1" />), while for ¹³CO and C¹⁸CO, it was 30.518 kHz (~ 0.04 km s⁻<fnref n="1" />). Both continuum bands presented 2 GHz bandwidths. The data were calibrated with the Common Astronomy Software Applications package (CASA v.5.5, McMullin et al. 2007), and the python modules from CASA API, *casatasks*, and *casatools* (CASA Team 2022). The standard calibrations include water vapour calibration, temperature correction, and phase, amplitude, and bandpass calibrations.

### 2.1 Continuum imaging

We started our analysis by fixing the visibilities' phase centre on J2000 05 h 40 m 27.448 s –07 d 27 m 29.65 s. The image synthesis of the 1.3 mm continuum emission was performed with the *tclean* task of CASA. For the high-resolution data, we used the Briggs weighting scheme with a robust parameter of 0.5, resulting in a synthesized beam size of 41.2 × 29.8 mas, and a position angle of 40.6. The pixel scale of the image was set to 1.5 mas. One iteration step of self-calibration was applied to both observations. For the first night (low-resolution image: 142 mas), it resulted in an improvement of ~6 SNR. For the second night (high-resolution image: 27 mas), it resulted in an SNR improvement of ~1.6.

Our final continuum image was produced from a concatenated measurement set combining both, the short and the long baseline visibilities, using the *concat* task of CASA. We used the same image synthesis parameters used for the second night of observation.

### 2.2 Line imaging

The visibilities were fixed at the same phase centre as was done for the continuum coordinates (see sub-Section 2.1). After producing a dirty image from the visibilities, we noticed that the emission mimicked the presence of gaseous envelopes around the discs (moment 0 maps,

<footnote n="1">¹The FU Ori classification is still controversial and has been contested by Connelley & Reipurth (2018).</footnote>
<table><caption>**Table 2.** ALMA imfit analysis results and physical parameters inferred from the HBC 494 continuum discs.</caption><thead><tr><th></th><th>HBC 494 N</th><th>HBC 494 S</th></tr></thead><tbody><tr><td>Flux density (mJy)</td><td>105.2 ± 1.9</td><td>21.1 ± 0.6</td></tr><tr><td>Peak flux (mJy beam<sup>-1</sup>)</td><td>23.0 ± 0.4</td><td>8.7 ± 0.2</td></tr><tr><td>Major axis (mas)</td><td>84.0 ± 1.8</td><td>64.6 ± 2.5</td></tr><tr><td>Minor axis (mas)</td><td>66.9 ± 1.5</td><td>46.0 ± 1.9</td></tr><tr><td>Major axis (au)</td><td>34.8 ± 0.7</td><td>26.7 ± 1.0</td></tr><tr><td>Minor axis (au)</td><td>27.8 ± 0.6</td><td>19.9 ± 0.8</td></tr><tr><td>Position angle (deg)</td><td>70.0 ± 4.5</td><td>65.4 ± 5.3</td></tr><tr><td>Beam major axis (mas)</td><td>41.2</td><td>41.2</td></tr><tr><td>Beam minor axis (mas)</td><td>29.8</td><td>29.8</td></tr><tr><td>Beam Position angle (deg)</td><td>40.6</td><td>40.6</td></tr><tr><td>Beam area (sr)</td><td>3.3e-14</td><td>3.3e-14</td></tr><tr><td>rms (µJy beam<sup>-1</sup>)</td><td>34.0</td><td>34.0</td></tr><tr><td>Dust mass (M<sub>Jup</sub>)</td><td>1.4</td><td>0.3</td></tr><tr><td>Gas mass (M<sub>Jup</sub>)</td><td>143.5</td><td>28.7</td></tr><tr><td>Inclination (deg)</td><td>37.2 ± 2.4</td><td>44.7 ± 3.3</td></tr><tr><td>FWHM Radius (au)</td><td>34.8 ± 0.7</td><td>26.7 ± 1.0</td></tr></tbody></table>

see Fig. 1, left column) but no gas dynamic signatures were revealed (moment 1 map, see Fig. 1, right column). Therefore, we proceeded to remove the visibility’s continuum contributions by using the CASA task uvcontsub.

Further, we performed the *tclean* process using Briggs weighting with a robust parameter of 0.5, Hogbom deconvolver, and pixel scale of 6 mas. The total velocity ranged between −6 and 18 km s⁻¹, although a smaller range (0 − 11 km s⁻¹) was used to create the ¹³CO and C¹⁸O moment maps. We used spectral resolution widths of 1 km s⁻¹ for ¹²CO and of 0.3 km s⁻¹ for ¹³CO and C¹⁸O. The rms values, obtained for the channel without a clear signal on the channel maps (4 km s⁻¹), were 1.9, 3.6, and 2.6 mJy beam⁻¹ for ¹²CO, ¹³CO, and C¹⁸O, respectively.

# 3 RESULTS

## 3.1 Continuum analysis

With the high-resolution data shown in Fig. 2, we could reveal the binary nature of the HBC 494 system. Each of the components in HBC 494 is surrounded by continuum emission, most likely associated with circumstellar discs.

We performed a 2D Gaussian fitting with the *imfit* tool of CASA in order to characterize the newly resolved components. The projected separation between the two sources is 0.18 (75 au). We name each component with the usual convention, ‘N’ and ‘S’, referring to the northern and the southern source, respectively. We assume the northern component to be the primary as it is five times brighter than the southern (secondary) disc. Both individual discs are resolved according to our Gaussian fit. For the primary component, we find a major axis FWHM of 84.00 ± 1.82 mas and a minor axis of 66.94 ± 1.50 mas (34.8 ± 0.7 × 27.8 ± 0.6 au), with a position angle of 70.01 ± 4.46° (values deconvolved from the beam). For the secondary, the major axis FWHM is 64.60 ± 2.49 mas and the minor axis FWHM is 45.96 ± 1.89 mas (26.7 ± 1.0 × 19.9 ± 0.8 au), and the position angle is 65.38 ± 5.32°. The integrated fluxes for ‘N’ and ‘S’ are 105.17 ± 1.89 mJy and 21.06 ± 0.63 mJy, respectively. The peak fluxes are 22.96 ± 0.35 and 8.71 ± 0.21 mJy beam⁻¹ for the primary and secondary sources, respectively. The rms is ~0.034 mJy beam⁻¹, as observed in a circular region with a radius of 225 mas without emission. The inclinations are calculated using the aspect ratios of

<figure><img src="image_3.png" /><figcaption>**Figure 1.** Small-scale moment maps for the analysed CO isotopologues, ¹²CO (top), ¹³CO (middle), and C¹⁸O (bottom), without subtraction of the continuum. The black stars mark the peak flux positions of the continuum discs. The dashed black contours correspond to 100×rms from the continuum emission (100 × 34 µJy beam⁻¹). Left: moment 0 maps for each mentioned molecular line. The rms values at the bottom of each panel are in units (mJy beam⁻¹)(km s⁻¹). The ¹²CO moment 0 map (top-left) has contour levels of 5, 7, and 9×rms showed at the bottom of the panel. ¹³CO and C¹⁸O moment 0 maps (middle and bottom-left) have contour levels of 3 and 4×rms showed at the bottom of each panel. Right: moment 1 maps for each mentioned molecular lines. The contours are the same as each left panel respectively. The maps include only pixels above three times the rms measured from the set of channels used for each molecular line (−6 − 18 km s⁻¹ for ¹²CO and 0 − 11 km s⁻¹ for ¹³CO and C¹⁸O).</figcaption></figure>

the discs. These are assumed as projected circular discs when face-on, thus elliptical when inclined:

$$i = \arccos\left(\frac{b}{a}\right),$$

where ‘b’ and ‘a’ are the semiminor and semimajor axes, respectively. It resulted in 37.16 ± 2.36° inclination for HBC 494 N and 44.65 ± 3.27 for HBC 494 S. At 30 mas resolution, no substructures were detected (see the radial profiles in Fig. 3).

A large fraction of the mm-sized grains in protoplanetary discs resides in the mid-plane. They are usually optically thin to their own radiation. Thus, assuming standard discs, we can use the observed fluxes to estimate the dust masses of HBC 494 N and S. For that, we use the following formula (as in Beckwith et al. 1990; Andrews & Williams 2005; Cieza et al. 2018):

$$M_{\text{dust}} = \frac{F_{\nu}d^2}{k_{\nu}B_{\nu}(T_{\text{dust}})}, \qquad (1)$$

where $F_ν$ is the observed flux, $d$ is the distance to the source, $B_ν$ is the Planck function, and $κ_ν$ is the dust opacity. Adopting the distance of 414 pc, isothermal dust temperature ($T_{\text{dust}}$ = 20 K) and dust opacity assuming a $M_{\text{gas}}/M_{\text{dust}}$ fraction of 100, ($κ_ν$ = 10 (ν/10¹²Hz) cm² g⁻¹; Beckwith et al. 1990) we get dust masses of 1.43 $M_{\text{Jup}}$ (HBC 494 N)
<figure><img src="image_4.png" /><figcaption>**Figure 2.** ALMA observations at 1.3 mm of the HBC 494 system. The images reveal the binary nature of HBC 494 with two components surrounded by continuum emission associated with circumstellar dust. The respective signal-to-noise ratios of each image are shown in each panel. We show the resulting images from the long baseline observation with a resolution of 0.027 arcsec (left), the short baseline data at 0.142 arcsec resolution (middle), and the combination of the two observations with 0.0298 (right). Dashed green lines in the left and middle images represent a 3σ contour associated with the lower-resolution continuum image. The combined image has a beam size of ~41 × 30 mas, shown in the lower-left corner of the image. Its contours correspond, from the yellow (more external) to the pink dashed lines, to 10, 40, 70, and 100 times the rms value, respectively. The rms is ~0.034 mJy beam⁻¹.</figcaption></figure>

<figure><img src="image_5.png" /><figcaption>**Figure 3.** Radial brightness profile of HBC 494 N and HBC 494 S. The surface brightness (dots), measured in apertures ranging from the beam’s major axis to three times the semimajor axis FWHM of each continuum disc, were normalized to the peak fluxes. The shaded regions indicate 1σ error measured in each aperture. The dashed lines correspond to the ALMA imfit FWHM of each disc.</figcaption></figure>

and 0.29 $M_{\text{Jup}}$ (HBC 494 S). Following the standard gas-to-dust mass ratio of 100, we report disc gas masses estimations of 143.46 $M_{\text{Jup}}$ for HBC 494 N, and 28.68 $M_{\text{Jup}}$ for HBC 494 S. The physical parameters based on the CASA analysis are listed in Table 2.

## 3.2 Line analysis

The further two subsections describe the large and small-scale structure analyses. The large scale, using the extent of 8000 au, shows the results of outflows and envelopes. At such a scale, there is not
enough resolution to display both discs' dynamics and their possible interactions. The small scale (150 au) fulfills this role, and thus, both gas scenarios must be taken into account.

### 3.2.1 Large-scale structures (8000 au)

The channel maps (Figs 4, C1 and C2) show southern and northern $^{12}$CO wide-angle arcs (~150°) and no clear signal of large structures from the other molecular lines. This bipolar outflow was previously described in Ruíz-Rodríguez et al. (2017). The wide-angular structure shows an outflow morphology expected for Class I discs (Arce & Sargent 2006). In our observations, the southern and northern arcs are defined by the velocity ranges of [-6 – 1 km s⁻¹] and [5 – 18 km s⁻¹], respectively. The moment 0 and 1 $^{12}$CO arcs are shown in Fig. 5. However, it is noticeable that the northern arc (redshifted emission) dominates the displayed velocities. The lack of signal in the southern arc can be explained by lower molecular density, or due to intracloud absorption. Fig. 6 shows the three molecular lines' concentration and dynamics (moment 0 and 1 maps), as well as the spectral profile measured within the dashed regions.

The $^{13}$CO emission traces the rotating, infalling, and expanding envelope surrounding the system, showing a small deviation from the $^{12}$CO outflowing arcs' rotation axis. The blue-shifted emission concentrates around 3 km s⁻¹, while the red-shifted emission is around 5 km s⁻¹. It is noticeable that the $^{13}$CO emission has a rotation axis almost perpendicular to the $^{12}$CO outflows axis, ensuring that the physical processes behind the two are different. The spectral $^{13}$CO also shows a dip around 4 km s⁻¹, but this may not trace an absorption but a lack of signal due to the analysed UV-coverage or cloud contamination.

The $^{C^{18}O}$ emission, however, is faint and hardly distinguishable from the surrounding gas in moment 0 maps. It has also the lowest abundance of the three analysed isotopologues, being a good tracer of the higher gas densities in the innermost regions of the cloud. Its velocity maps show that a faint blueshifted motion was detected around 3 km s⁻¹, very weak when compared to the redshifted emission detected principally around 5 km s⁻¹. Due to the higher concentration of gas in the northern part, it is reasonable that we observed a weak gas counterpart in the southern region. At large scale, our results are comparable with the ones presented in (Ruíz-Rodríguez et al. 2017). Furthermore, a lower limit of the envelope material of ~600 Jy km s⁻¹ towards HBC 494 could be traced using Total Power (TP), ALMA compact array (ACA), and the main array ALMA observations with $^{C^{18}O}$ data in the range of 4.3 ± 0.5 km s⁻¹ (Ruíz-Rodríguez private communication).

### 3.2.2 Small scale structures (150 au resolution)

We started by removing the continuum contribution from all molecular lines observed ($^{12}$CO, $^{13}$CO, $^{C^{18}O}$). We already expected that $^{12}$CO would trace the gas in larger scales due to its optical depth and, thus, could blend with smaller gas signatures. To avoid cloud contamination during the creation of $^{12}$CO small-scale moment maps, we removed the channels that were more affected. We considered velocities in the range of [-6 – 1 km s⁻¹] and [5 – 18 km s⁻¹], as similarly done for the different large-scale arcs described in the previous subsection.

Following CO channel maps and moment 0 and 1 maps were produced to explore potential hints of interaction between the stars and the two circumstellar discs. In particular, we looked for disc substructures and perturbed rotation patterns. The moment maps can indeed provide valuable information about the binary orbit and the

discs' geometry. However, by looking at the molecular lines in this scale (see the moment maps in Fig. 7, left and middle columns), we could not clearly detect the presence of the discs or their rotational signatures. We can only notice that the $^{12}$CO and $^{13}$CO moment 0 maps show an interesting pattern, where less gas emission is found where the continuum discs are. Additionally, the area within the continuum discs highlights regions similar to cavities or 'holes' (Fig. 7, left column, upper and middle row). Interestingly, Ruíz-Rodríguez et al. (2022) observed similar features from the same molecular lines, in addition to HCO$^+$, for another FUor system, V883 Ori. The work also showed that the origin of cavities and ring emission around discs can be interpreted in two ways, one based on gas removal and the other on optical depth effects.

If the signal traces the lack of gas surrounding the discs, the leading mechanism may be slow-moving outflows. The central regions of young continuum discs are expected to be constantly carved by the influence of magneto-hydrodynamical jets (Frank et al. 2014). In addition, it is also expected that the lower emission observed comes from the chemical destruction by high-energy radiation (more active discs will create bigger cavities). By looking at the size of the gaps, we can observe that HBC 494 S exerts a smaller influence on the gas than HBC 494 N and, thus, HBC 494 N is the more active disc in the system if this hypothesis is correct.

Another interpretation of the negatives in our gas maps is that this is a spurious result of continuum subtraction. Usually, the continuum emission is inferred from channels devoid of gas line emission. The usual procedure does not consider the line emission where these channels overlap. Suppose the emission lines are optically thick above the continuum. In that case, the foreground gas can significantly absorb the photons coming from the underlying continuum, which may lead to a continuum overestimation. Consequently, in such cases, the continuum may be over-subtracted, causing the 'hole' feature that is stronger where the line peaks (see e.g. Boehler et al. 2017; Weaver, Isella & Boehler 2018).

# 4 DISCUSSION

## 4.1 Multiplicity and triggering mechanisms

Besides HBC 494, there are ~25 known FUor objects within 1 kpc (Audard et al. 2014). As previously commented, many triggering mechanisms can cause episodic accretion events. From this sample, only HBC 494 and a few other FUor systems are known binaries (e.g. FU Orionis, L1551 IRS, RNO 1B/C, AR 6A/B; Pueyo et al. 2012 and references therein).

Given the high occurrence rate of stellar binaries harbouring discs, the lack of detection of multiple YSO systems remains a case of investigation. Additionally, young discs evolve in crowded star-forming regions, enhancing the hypothesis that the outbursts of Class 0/I discs may affect other discs, driving episodic accretion events. Also, surveys and studies using ALMA and NIR data for Class I-III discs, show that there is a lack of detection when only visual multiple systems (separations of 20–4800 au) are considered (e.g. Zurlo et al. 2020, 2021). When all the possible separations are taken into account, the multiplicity frequencies considerably increase. For Taurus, for example, it goes up to 70 per cent when spectroscopic binaries are included (Kraus et al. 2011). In the case of Orion, 30 per cent of the systems are multiple with separations between 20 and 10 000 au (Tobin et al. 2022). The latter study also noticed that the separations decrease with time (when comparing Class 0, I, and flat-spectrum discs) and that the multiplicity frequency in Class 0 is higher than in the later evolutionary stages. Therefore, multiple eruptive young
<figure><img src="image_6.png" /><figcaption>**Figure 4.** $^{12}$CO channel maps of the HBC 494 system. The star in the centre marks the position of the continuum discs. The southern arc is more evident between the velocities -6 and 1 km s$^{-1}$, while the northern is more easily seen between 7 and 18 km s$^{-1}$.</figcaption></figure>

systems must be common, and more detectable within evolutionary
time. They probably are not frequently detected due to the short time
duration of enhanced accretion events in comparison with the lifetime
of discs in class 0/I stages (see Audard et al. 2014 for a FUors review).
Still, it is not clear if discs belonging to close-separation systems are
more susceptible to eruptive events than isolated ones.

For each HBC 494 disc, no clue of trigger mechanisms was found,
since the gas and continuum data did not reveal clear spiral or clumpy
features indicating a case of infall or GI (see e.g. Zhu et al. 2012;
Kratter & Lodato 2016). Looking at the dust continuum (Fig. 2),
CO isotopologues moment maps (Fig. 7), and the scattered $^{12}$CO
emission (Fig. 12 of Ruíz-Rodríguez et al. 2017), the hypothesis of
stellar flybys is also not encouraged since no trace of perturbation
was detected (Cuello et al. 2020; Cuello, Ménard & Price 2023).
Moreover, dynamical data (small-scale moment 1 maps) also can
provide clues for the triggering mechanism (Vorobyov et al. 2021).

However, it requires clear detection of quasi-Keplerian rotation,
which was not observed.

In the case of binaries, the first component to ignite the FUor
outbursts can quickly trigger the secondary one by inducing per-
turbations and mutual gravitational interactions (Bonnell & Bastien
1992; Reipurth & Aspin 2004; Vorobyov et al. 2021; Borchert et al.
2022a). Therefore, we can assume that all the discs in FUor multiple
systems like HBC 494 might have undergone successive enhanced
eruptive stages, despite the differences in mass and radius between
each component. However, it is not clear how the outbursts in HBC
494 N and HBC 494 S affect each other since the moment maps do
not show the connection between discs. Although on larger scales,
we detected the difference in the amount of gas mass detected in
the northern regions compared to the southern. This scenario may
be described if the more massive disc (i.e. HBC 494 N) has a higher
contribution to the outbursts and winds.
<figure><img src="image_7.png" /><figcaption>**Figure 5.** Large-scale ¹²CO moment maps split in each one of the bipolar outflow structures. The left column corresponds to moment 0 maps, and the right column to moment 1 maps. The plots in the same row refer to the same structure, which is the southern arc (*upper row*), and the northern arc (*bottom row*). The position of the HBC 494 N is marked with a star. The maps include only pixels above 2 times the rms measured from the set of channels shown at the top of each panel.</figcaption></figure>

With astrometric data, the eccentricity of orbits can be determined. If both discs are still accreting gas from the environment, it is expected that quasi-circular orbits trigger enhanced accretion every few binary periods. Eccentric orbits, on the other hand, can induce eruptive events in every orbit, preferentially when the binaries reach the pericentre (see e.g. Dunhill, Cuadra & Dougados 2015; Lai & Muñoz 2022). Observational evidence of circumbinary discs in different YSO stages was found (see e.g. Dutrey, Guilloteau & Simon 1994; Mathieu et al. 1997; Tobin et al. 2016a; Maureira et al. 2020) and are seen as a common counterpart of young binaries in formation. However, no HBC 494 circumbinary gas disc was observed due to cloud contamination and optical depth effects.

## 4.2 Disc sizes and masses

FU Orionis, the precursor of the classification FUor, is also a binary system. HBC 494 system, however, has smaller discs separation compared to the 210 au between FU Orionis north and south

components (Pérez et al. 2020). FU Orionis components have similar sizes and masses between their discs, contrary to the HBC 494 components. We can argue that, due to HBC 494 being a close-packed system with substantially different masses between their components, a scenario of radius truncation can be tested. However, the FU Orionis discs are exceptional compared to other FUors, which are generally more massive and larger. Nevertheless, it is important to check if HBC 494 follows the trend which shows that FUor objects are more massive than class 0/I discs and that discs from multiple systems are smaller compared to those from non-multiple systems (Cieza et al. 2018; Hales et al. 2020; Tobin et al. 2020; Zurlo et al. 2023). First, we will describe our results regarding masses and radius. Then, we will compare HBC 494 discs to FUors and Orion YSOs in the literature.

We assumed dust masses (assuming the gas-to-dust ratio of 100) inferred by optically thin approximation (described in Section 3.1). However, it is worth mentioning that the optically thin analysis can not take into account the innermost regions of the disc (optically
<figure><img src="image_8.png" /><figcaption>**Figure 6.** Large-scale moment maps for the analysed CO isotopologues and spectral fluxes. The left column corresponds to moment 0 maps, the middle one to moment 1 maps, and the third column to spectral profiles. The rms values at the bottom of each panel in the left column are in units (mJy beam⁻¹)(km s⁻¹). The plots in the same row refer to the same molecular lines, which are ¹²CO (upper row), ¹³CO (middle row), and C¹⁸O (bottom row). The dashed black lines in the moment 1 column correspond to the regions used to produce the spectral profiles. The red shaded area in ¹²CO profile represents the channels we excluded before creating the moment maps lying in the same row (to avoid cloud contamination). The centre of stars, in the middle of each figure, marks the position of both discs. The maps include only pixels above two times the rms measured from the set of channels used for each molecular line (−6 – 18 km s⁻¹ for 12CO and 0 – 11 km s⁻¹ for 13CO and C18O).</figcaption></figure>
<figure><img src="image_9.png" /><figcaption>**Figure 7.** Small-scale moment maps for the analysed CO isotopologues, after subtraction of the continuum, and their spectral profiles. The first column corresponds to moment 0 maps, and the middle one to moment 1 maps. The rms values at the bottom of each panel in the left column are in units (mJy beam⁻¹)(km s⁻¹). The molecular lines correspond to ¹²CO (upper row), ¹³CO (middle row), and C¹⁸O (bottom row). The dashed black lines spatially correspond to the contour level equal to 100 times the continuum rms (100 × 34 µJy beam⁻¹), in the continuum combined image (Fig. 2, right). The orange stars mark the peak flux positions of the continuum discs. The right column represents the spectral profiles measured from velocity maps taken within each disc. The red shaded area in ¹²CO profile represents the channels we excluded before creating the moment maps lying in the same row (to avoid cloud contamination).</figcaption></figure>

thick). This may lead to an underestimation of the dust masses. Also, an underlying miscalculated dust grain temperature can alter the results, overestimating the masses if the dust is warmer than expected. The chosen assumptions of temperatures (fixed 20 K for dust grains) and opacities for both discs lead to 1.43 *M*<sub>Jup</sub> and 0.29 *M*<sub>Jup</sub> for HBC 494 N and HBC 494 S, respectively. Based on these results, we can say that the HBC 494 N is comparable to other FUor sources, but HBC 494 S has its dust mass comparable to EXor discs (Cieza et al. 2018). The disc sizes were calculated using the deconvolved Gaussian FWHM/2 radius obtained from 2D Gaussian fits. This methodology was also used for other ALMA data sets (e.g. Hales et al. 2020; Tobin et al. 2020). Therefore, it allows a consistent comparison with other discs. The dust mass vs radius comparison between HBC 494 N and HBC 494 S, a sample of 14 resolved FUors and EXors (extracted from Hales et al. 2020) and Class 0/I systems (Tobin et al. 2020), can be seen in Fig. 8. Here, as previously stated, we notice that HBC 494 discs (black, hexagon symbols), as other eruptive systems (hexagon, square, and triangle symbols), present higher masses than young systems, which are not in the stage of episodic accretion. However, there is no obvious distinction between the disc sizes of individual systems, eruptive or not. A clear

difference is seen when we compare the discs from multiple systems (hexagon symbols) and single systems. The latter present bigger sizes as they are not targets for tidal truncation, enhanced radial drift, and more aggressive photoevapouration – processes known to rule close-systems dynamics and evolution (see e.g. Harris et al. 2012; Kraus et al. 2012; Rosotti & Clarke 2018; Zurlo et al. 2020, 2021).

## 4.3 Binary formation and alignment

Different scenarios have been proposed to explain the formation of binary systems. The main one for close-separated systems is fragmentation, followed by dynamic interactions (for a review, see Offner et al. 2022).

The fragmentation process consists of partial gravitational collapse from self-gravitating objects. To be successful, many initial physical conditions are relevant as thermal pressure, density, turbulence, and magnetic fields. In addition, the fragmentation can be divided into two main classes: direct/turbulent (e.g. Boss & Bodenheimer 1979; Bate & Burkert 1997) and rotational (e.g. Larson 1972; Bonnell 1994; Bonnell & Bate 1994a, b; Burkert, Bate & Bodenheimer 1997).
<figure><img src="image_10.png" /><figcaption>**Figure 8.** Dust disc masses as a function of characteristic radii (FWHM/2) for FUors (blue triangles), EXors (red squares), for double FUor and EXor classification (yellow stars), and Class 0/I objects (cyan crosses), as similarly presented in Hales et al. (2020). The horizontal arrow on V852 Aur denotes the disc radius in an upper limit. The hexagons represent eruptive/multiple systems, with matching colours for discs lying in the same system. The data for HBC 494 discs was generated in this work. The blue-dashed line corresponds to the power-fit law to the FU/EXor data (Spearman correlation coefficient: 0.63), and the cyan dash-dotted line, to the Class 0/I data (Spearman correlation coefficient: 0.55). To generate this plot, we obtained data from Kóspál et al. (2017); Cieza et al. (2018); Hales et al. (2018); Cruz-Sáenz de Miera et al. (2019); Takami et al. (2019); Hales et al. (2020); Pérez et al. (2020).</figcaption></figure>

The direct/turbulent fragmentation from a collapsing core is highly dependent on the initial density distribution. It can form wide-separated multiple YSO systems with uncorrelated angular momentum. Thus, the direct/turbulent fragmentation may lead to preferentially misaligned multiple systems (Bate 2000; Offner et al. 2016; Bate 2018; Lee et al. 2019). The rotational fragmentation, instead, is caused by instabilities in rotating discs and leads to preferentially spin-aligned and coplanar systems (Offner et al. 2016; Bate 2018). Moreover, later dynamical processes such as stellar flybys (Clarke & Pringle 1993; Nealon, Cuello & Alexander 2020; Cuello et al. 2023) and misaligned accretion from the environment (Dullemond et al. 2019; Kuffmeier, Goicovic & Dullemond 2020; Kuffmeier et al. 2021) can also induce alignment or misalignment.

The HBC 494 discs have similar inclinations (Δi = 7.5 ± 4.1°) and similar PAs (ΔPA = 4.6 ± 7.0°). The relative orientations of the discs suggest that the system is coplanar. Assuming they are quasi-coplanar, with the same PA, the unprojected separation would be ~0.24 (99 au). Therefore, the HBC 494 discs may show a spin-alignment situation, more typical to observed close-separated systems (see e.g. Tobin et al. 2016b, 2020). Thus, we tentatively suggest that HBC 494 was formed by rotational disc fragmentation rather than direct collapsing. However, more precise observation of the kinematics of the surrounding gas on a small scale (Vorobyov et al. 2021), complemented with orbital information coming from astrometrical measurements, is required to evaluate this hypothesis.

In this context, IRAS 04158+2805 is of interest as Ragusa et al. (2021) reported the detection of two circumstellar discs, similar to HBC 494 in terms of small to moderate misalignment, and an external circumbinary disc. However, in contrast to IRAS 04158+2805, no circumbinary disc was detected in HBC 494. This difference could be explained either by the absorption of the circumbinary disc emission

due to cloud contamination, or because HBC 494 had enough time to sufficiently empty the circumbinary mass reservoir. Since most hydrodynamical models of star formation naturally produce young binaries with individual discs and a surrounding circumbinary disc (Bate 2018, 2019; Kuruwita, Federrath & Haugbølle 2020), it is likely that a circumbinary disc formed at some earlier evolutionary stage of HBC 494. If the circumbinary disc is actually there, but remains undetected, the supply of material could extend the disc lifetime of the circumstellar discs in HBC 494. Deeper multiwavelength observations would provide more information, enabling us to solve this binary riddle.

## 5 CONCLUSIONS

In this work, we presented high-resolution 1.3 mm observations of HBC 494 with ALMA. The unprecedented angular resolution in this source (0.027), reveals that HBC 494 is a binary that can be resolved into two discs, HBC 494 N and HBC 494 S. The discs have a projected separation of ~75 au. We derived sizes, orientations, inclinations, and dust masses for both components. Both objects appear to be in a quasi-coplanar configuration and with their sizes halted by dynamical evolution, besides preserving high masses, common to FUors and EXors than typical (not eruptive) Class 0/I discs. Comparing the two sources, we noticed that HBC 494 N is ~5 times brighter/more massive and ~2 times bigger than HBC 494 S.

The gas kinematics was analysed at two different spatial scales: 8000 and 150 au. At large scale, we have obtained similar results as those presented in Ruíz-Rodríguez et al. (2017), revealing the wide outflow arcs (traced by the $^{12}$CO) and the infalling envelopes ($^{13}$CO and $^{18}$O). At the small-scale, we detected depleted gas emission
(cavities) for both discs ($^{12}$CO and $^{13}$CO, moment 0). They were probably formed by slow outflows and jets coming from the discs along the line of sight or by optical depth effects and over-subtraction of the continuum emission. The dynamics of both discs in such scales were masked principally by cloud contamination.

Further observations with similar resolution but of optically thin-
ner molecular lines may lead to the characterization of the dynamical
interaction of the two components. For example, the identification
of rotational signatures from the discs can be used to identify the
dynamical masses of their central stars. With this information, we
could also constrain truncation radii. Additionally, observations of
small-scale gas structures, allied to astrometric measurements, can
be used to constrain the possible formation scenarios.

We conclude that the HBC 494 system constitutes a test bed for
eruptive binary-disc interactions and the connection between stellar
multiplicity and accretion/ luminosity processes (such as outbursts).
Also, it provides a statistics enhancement about the rarely observed
systems FUors and Exors.

ACKNOWLEDGEMENTS

We want to thank the referee for their comments and suggestions that significantly improved the manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is funded by ANID – Millennium Science Initiative Program – Center Code NCN2021_080. PHN acknowledges support from the Joint China–Chile Committee fund and the ANID Doctorado Nacional grant number 21221084 from the government of Chile. AZ acknowledges support from the FONDECYT Iniciación en investigación project number 11190837. SP acknowledges support from FONDECYT Regular project number 1191934. LAC acknowledges support from the FONDECYT project number 1211656. MM acknowledges financial support by Fondos de Investigación 2022 de la Universidad Viña del Mar. JC and MM acknowledge support from ANID, – Millennium Science Initiative Program – NCN19-171. SC acknowledges support from Agencia Nacional de Investigación y Desarrollo de Chile (ANID) given by FONDECYT Regular grant number 1211496, and ANID project Data Observatory Foundation DO210001. TB acknowledges financial support from the Joint Committee ESO–Government of Chile fund and the FONDECYT postdoctorado project number 3230470. This project has received funding from the European Union (ERC, Stellar-MADE, project number 101042275).

6 DATA AVAILABILITY

This paper makes use of the following ALMA data: ADS/JAO.ALMA 2016.1.00630.S. The data are downloadable from the official ALMA archive and public. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.

REFERENCES

Andrews S. M., Williams J. P., 2005, ApJ, 631, L1134
Arce H. G., Sargent A. I., 2006, ApJ, 646, L1070
Armitage P. J., Livio M., Pringle J. E., 2001, MNRAS, 324, 705

Audard M. et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds., Protostars and Planets VI, Univ. of Arizona, Tucson, p. 387

Bate M. R., 2000, MNRAS, 314, 33

Bate M. R., 2018, MNRAS, 475, 5618

Bate M. R., 2019, MNRAS, 484, 2341

Bate M. R., Burkert A., 1997, MNRAS, 288, 1060

Beckwith S. V. W., Sargent A. I., Chini R. S., Guesten R., 1990, AJ, 99, 924

Boehler Y., Weaver E., Isella A., Ricci L., Grady C., Carpenter J., Perez L., 2017, ApJ, 840, L60

Bonnell I. A., 1994, MNRAS, 269, 837

Bonnell I. A., Bate M. R., 1994a, MNRAS, 269, 45

Bonnell I. A., Bate M. R., 1994b, MNRAS, 271, 999

Bonnell I., Bastien P., 1992, ApJ, 401, L31

Borchert E. M. A., Price D. J., Pinte C.,uello N., 2022a, MNRAS, 510, 37

Borchert E. M. A., Price D. J., Pinte C.,uello N., 2022b, MNRAS, 517, 4436

Boss A. P., Bodenheimer P., 1979, ApJ, 234, L289

Burkert A., Bate M. R., Bodenheimer P., 1997, MNRAS, 289, 497

CASA Team, 2022, PASP, 134, 114501

Chiang H.-F., Reipurth B., Walawender J., Connelley M. S., Pessev P., Geballe
T. R., Best W. M. J., Paegert M., 2015, ApJ, 805, L54

Cieza L. A. et al., 2018, MNRAS, 474, 4347

Clarke C. J., Pringle J. E., 1993, MNRAS, 261, 190

Connelley M. S., Reipurth Bo, 2018, ApJ, 861, 145

Cruz-Sáenz de Miera F., Kóspál Á., Ábrahám P., Liu H. B., Takami M., 2019, ApJ, 882, L4

Cuello N. et al., 2019, MNRAS, 483, 4114

Cuello N. et al., 2020, MNRAS, 491, 504

Cuello N., Ménard F., Price D. J., 2023, European Physical Journal Plus, 138, 11

Dullemond C. P., Küffmeier M., Goicovic F., Fukagawa M., Oehl V., Kramer M., 2019, A&A, 628, 20

Dunham M. M., Vorobyov E. I., 2012, ApJ, 747, L52

Dunhill A. C., Cuadra J., Dougados C., 2015, MNRAS, 448, 3545

Dutrey A., Guilloteau S., Simon M., 1994, A&A, 286, 149

Evans Neal J. I. et al., 2009, ApJS, 181, 321

Frank A. et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds. Protostars and Planets VI. Univ. of Arizona, Tucson, p. 451

Giannini T. et al., 2022, ApJ, 929, L129

Hales A. S. et al., 2018, ApJ, 859, L111

Hales A. S. et al., 2020, ApJ, 900, L7

Harris R. J., Andrews S. M., Wilner D. J., Kraus A. L., 2012, ApJ, 751, L115

Herbig G. H., 1966, Vistas in Astronomy, 8, 109

Herbig G. H., 2007, AJ, 133, 2679

Jurdana-Šepić R., Munari U., Antoniucci S., Giannini T., Lorenzetti D., 2018, A&A, 614, 9

Kenyon S. J., Hartmann L. W., Strom K. M., Strom S. E., 1990, AJ, 99, 869

Kóspál Á. et al., 2017, ApJ, 843, L45

Kratter K., Lodato G., 2016, ARA&A, 54, 271

Kraus A. L., Ireland M. J., Martinache F., Hillenbrand L. A., 2011, ApJ, 731, L8

Kraus A. L., Ireland M. J., Hillenbrand L. A., Martinache F., 2012, ApJ, 745, L19

Kuffmeier M., Goicovic F. G., Dullemond C. P., 2020, A&A, 633, 3

Kuffmeier M., Dullemond C. P., Reissl S., Goicovic F. G., 2021, A&A, 656, 161

Kuruwita R. L., Federrath C., Haugbølle T., 2020, A&A, 641, 59

Lai D., Muñoz D. J., 2022, preprint (arXiv:2211.00028)

Larson R. B., 1972, MNRAS, 156, 437

Lee A. T., Offner S. S. R., Kratter K. M., Smullen R. A., Li P. S., 2019, ApJ, 887, L232

Lodato G., Clarke C. J., 2004, MNRAS, 353, 841

Mathieu R. D., Stassun K., Basri G., Jensen E. L. N., Johns-Krull C. M., Valenti J. A., Hartmann L. W., 1997, AJ, 113, 1841
Maureira M. J., Pineda J. E., Segura-Cox D. M., Caselli P., Testi L., Lodato G., Loinard L., Hernández-Gómez A., 2020, ApJ, 897, L59

McMullin J. P., Waters B., Schiebel D., Young W., Golap K., 2007, in Shaw R. A., Hill F., Bell D. J. eds, Astronomical Society of the Pacific Conference Series Vol. 376, Astronomical Data Analysis Software and Systems XVI, p. 127

Menten K. M., Reid M. J., Forbrich J., Brunthaler A., 2007, A&A, 474, 515

Nealon R., Cuello N., Alexander R., 2020, MNRAS, 491, 4108

Offner S. S. R., Dunham M. M., Lee K. I., Arce H. G., Fielding D. B., 2016, ApJ, 827, L11

Offner S. S. R., Moe M., Kratter K. M., Sadavoy S. I., Jensen E. L. N., Tobin J. J., 2022, preprint (arXiv:2203.10066)

Pérez S. et al., 2020, ApJ, 889, L59

Postel A., Audard M., Vorobyov E., Dionatos O., Rab C., Güdel M., 2019, A&A, 631, 30

Pueyo L. et al., 2012, ApJ, 757, L57

Ragusa E. et al., 2021, MNRAS, 507, 1157

Reipurth B., 1985, A&AS, 61, 319

Reipurth B., Aspin C., 2004, ApJ, 608, L65

Reipurth B., Bally J., 1986, Nature, 320, 336

Rosotti G. P., Clarke C. J., 2018, MNRAS, 473, 5630

Ruíz-Rodríguez D. et al., 2017, MNRAS, 466, 3519

Ruíz-Rodríguez D. A., Williams J. P., Kastner J. H., Cieza L., Leemker M., Principe D. A., 2022, MNRAS, 515, 2646

Takami M. et al., 2019, ApJ, 884, L146

Tobin J. J. et al., 2016a, Nature, 538, 483

Tobin J. J. et al., 2016b, ApJ, 818, L73

Tobin J. J. et al., 2020, ApJ, 890, L130

Tobin J. J. et al., 2022, ApJ, 925, L39

Vorobyov E. I., Basu S., 2005, ApJ, 633, L137

Vorobyov E. I., Basu S., 2015, ApJ, 805, L115

Vorobyov E. I., Elbakyan V. G., Liu H. B., Takami M., 2021, A&A, 647, 44

Weaver E., Isella A., Boehler Y., 2018, ApJ, 853, L113

Zhu Z., Hartmann L., Gammie C., McKinney J. C., 2009, ApJ, 701, L620

Zhu Z., Hartmann L., Nelson R. P., Gammie C. F., 2012, ApJ, 746, L110

Zurlo A. et al., 2020, MNRAS, 496, 5089

Zurlo A. et al., 2021, MNRAS, 501, 2305

Zurlo A., Gratton R., Pérez S., Cieza L., 2023, The European Phys. J. Plus, 138, 411

## APPENDIX A: EFFECTS OF CONTINUUM OVER-SUBTRACTION

To evaluate the effects of continuum oversubtraction, we generated spatial profiles for each disc using ¹²CO moment 0 maps at small scales before and after continuum subtraction. We created cuts that crossed the semimajor axis of each disc (see red lines in Fig. A1, top panels) for this purpose. Fig. A1, top-left panel displays moment 0 maps before continuum removal, while the top-right panel shows the same maps after this process. The comparison between these effects is better visualized in the bottom panels, where continuum emission (magenta diamonds/lines) has a similar shape as ¹²CO before continuum subtraction (orange crosses/lines), but shifted in flux, for both discs. The spatial profile subtractions are displayed by black lines. However, they display higher fluxes when compared to the spatial profiles produced after continuum subtraction (blue-filled circles/lines). Additionally, the continuum was overestimated by foreground optical depth molecular lines that absorbed continuum emission and then propagated to the uvcontsub CASA task. The ‘holes’ or cavities seen in the top-right panel could potentially be diminished by manually adding back some of the lost line signal, but this would only create a fake signal at the level of noise. Thus, optically thinner lines must be used to obtain the real signal of discs in moment 0 and 1 maps.
<figure><img src="image_11.png" /><figcaption>**Figure A1.** The top panels show the ¹²CO moment 0 maps before (left) and after (right) continuum removal, along with their spatial profiles. The moment 0 contours represent values of 50, 75, 100, 150, and 200 times the rms (~0.06 mJy beam⁻¹ km s⁻¹). The red lines trace the axis used to create spatial profiles, which can be seen in the bottom panels. The bottom left panel shows the spatial profile of the HBC 494 N disc, while the bottom right panel shows that of the HBC 494 S disc. The vertical black-dashed lines indicate the centre of the discs. The orange crosses/lines represent spatial profiles before the continuum subtraction, created using the red line axis in the top panel, left. The magenta diamonds/lines represent the continuum spatial profile. The black lines represent the subtraction between the ¹²CO+continuum and the continuum spatial profiles for each disc. The dark blue filled circles/lines represent spatial profiles after the continuum subtraction, created using the red line axis in the top panel, right.</figcaption></figure>

## APPENDIX B: ¹²CO, ¹³CO, AND C¹⁸O CHANNEL MAPS WITH CONTOURS AND THE EFFECT OF CLOUD CONTAMINATION

This appendix presents the ¹²CO, ¹³CO, and C¹⁸O channel maps with contour plots (see Figs B1 and B2). To visualize the signals and corresponding flux values using a colour bar, we also provide versions of the same channel maps without contours (see Figs 4 and C1).

Fig. B1 shows the 3-rms significant southern arcs (velocity channels from -6 to 1 km s⁻¹) and northern arcs (velocity channels from 5 to 18 km s⁻¹). However, cloud contamination affects channels between 2 and 6 km s⁻¹. These channels were not used in the creation of large-scale moment maps. Channel 6 km s⁻¹ shows the most evidence of cloud contamination, with contour plots showing innermost flux values near the discs (marked by the central orange star). It also shows some significant contours on both horizontal extremes, which can be tracers of the filtered
<figure><img src="image_12.png" /><figcaption>**Figure B1.** $^{12}$CO channel maps of HBC 494 system with contours. The contours were displayed in black and they are equivalent to three times the rms of every channel. The rms values were calculated using all data in each channel, through the CASA task *imstat*. The peak flux values have reached up to 19 times the rms values. The star in the centre marks the position of the continuum disc around HBC 494 N.</figcaption></figure>

signals using only the main array data. The data partially trace features that, due to their large extension, require a combination of the ALMA main and single dish arrays to recover extended flux emission.

In Fig. B2, the $^{13}$CO channel maps are heavily marked by 3-rms black contours, which show the significant gas signal on each channel. Specifically, channels from 2.20 to 6.10 km s$^{-1}$ indicate gas in-falling clumps near where the discs are located, but also

show random/scattered signals far from the discs due to cloud contamination.

The C$^{18}$O channel maps represented in Fig. B3 are also heavily marked by 3-rms black contours. Channels from 2.80 to 4.60 km s$^{-1}$ indicate gas in-falling clumps near where the discs are located, but also show random/scattered signals far from the discs due to cloud contamination. Other channels are affected by cloud contamination or lack a significant signal.
<figure><img src="image_13.png" /><figcaption>**Figure B2.** $^{13}$CO channel maps of HBC 494 system with contours. The contours were displayed in black and they are equivalent to three times the rms of every channel. The rms values were calculated using all data in each channel, through the CASA task *imstat*. The peak flux values have reached up to 11 times the rms values. The star in the centre marks the position of the continuum disc around HBC 494 N.</figcaption></figure>
<figure><img src="image_14.png" /><figcaption>**Figure B3.** C$^{18}$O channel maps of HBC 494 system with contours. The contours were displayed in black and they are equivalent to three times the rms of every channel. The rms values were calculated using all data in each channel, through the CASA task *imstat*. The peak flux values have reached up to 13 times the rms values. The star in the centre marks the position of the continuum disc around HBC 494 N.</figcaption></figure>
APPENDIX C: EXTRA CHANNEL MAPS

The ¹³CO (large scale), C¹⁸O (large scale), ¹²CO (small scale and with continuum subtracted), ¹³CO (small scale and with continuum subtracted), and C¹⁸O (small scale and with continuum subtracted) channel maps are displayed in Figs C1, C2, C3, C4, and C5, respectively.

<figure><img src="image_15.png" /><figcaption>Figure C1. ¹³CO channel maps of HBC 494 system. The star in the centre marks the position of the continuum disc around HBC 494 N.</figcaption></figure>
<figure><img src="image_16.png" /><figcaption>Figure C2. C$^{18}$O channel maps of HBC 494 system.</figcaption></figure>
<figure><img src="image_17.png" /><figcaption>**Figure C3.** <sup>12</sup>CO channel maps of HBC 494 system, small-scale, after removing the continuum contribution.</figcaption></figure>
<figure><img src="image_18.png" /><figcaption>**Figure C4.** $^{13}$CO channel maps of HBC 494 system, small-scale, after removing the continuum contribution.</figcaption></figure>
<figure><img src="image_19.png" /><figcaption>**Figure C5.** C<sup>18</sup>O channel maps of HBC 494 system, small-scale, after removing the continuum contribution.</figcaption></figure>
<footnote n="1">¹Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Avenida Ejército Libertador 441, Santiago, Chile</footnote>

<footnote n="2">²Millennium Nucleus on Young Exoplanets and their Moons (YEMS), Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile</footnote>

<footnote n="3">³Departamento de Física, Universidad de Santiago de Chile, Avenida Victor Jara 3659, Santiago, Chile</footnote>

<footnote n="4">⁴Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile, Santiago, 9170022, Chile</footnote>

<footnote n="5">⁵European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago, Chile</footnote>

<footnote n="6">⁶Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura 7630355, Santiago, Chile</footnote>

<footnote n="7">⁷National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA</footnote>

<footnote n="8">⁸Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02138, USA</footnote>

<footnote n="9">⁹Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Lu 5, Haidian Qu, 100871 Beijing, People's Republic of China</footnote>

<footnote n="10">¹⁰Institute for Astronomy, University of Hawaii at Manoa, Woodlawn Drive, Honolulu, HI, 96822, USA</footnote>

<footnote n="11">¹¹Departamento de Ciencias, Facultad de Artes Liberales, Universidad Adolfo Ibáñez, Avenida Padre Hurtado 750, Viña del Mar, Chile</footnote>

<footnote n="12">¹²Núcleo Milenio de Formación Planetaria – NPF, Universidad de Valparaíso, Avenida Gran Bretaña 1111, Valparaíso, Chile</footnote>

<footnote n="13">¹³Escuela de Ciencias, Universidad Viña del Mar, Viña del Mar, 2572007, Chile</footnote>

<footnote n="14">¹⁴Université Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France</footnote>

<footnote n="15">¹⁵Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile</footnote>

<footnote n="16">¹⁶Facultad de Ingeniería y Ciencias, Universidad Adolfo Ibáñez, Avenida Diagonal las Torres 2640, Peñalolén, Santiago, Chile</footnote>

<footnote n="17">¹⁷Data Observatory Foundation, Chile</footnote>

<footnote n="18">¹⁸University of Nevada, Las Vegas, 4505 S. Maryland Parkway, Las Vegas, NV 89154, USA</footnote>

<footnote n="19">¹⁹Nevada Center for Astrophysics, University of Nevada, Las Vegas, 4505 South Maryland Parkway, Las Vegas, NV 89154, USA</footnote>

<footnote n="20">²⁰Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany</footnote>

<footnote>This paper has been typeset from a TeX/LA TeX file prepared by the author.</footnote>