# ALMA Mapping of Rapid Gas and Dust Variations in Comet C/2012 S1 (ISON): New Insights into the Origin of Cometary HNC

M. Cordiner, J. Boissier, S. Charnley, J. Remijan, M. Mumma, G. Villanueva, D. Lis, S. Milam, L. Paganini, J. Crovisier, et al.

► To cite this version:

M. Cordiner, J. Boissier, S. Charnley, J. Remijan, M. Mumma, et al., ALMA Mapping of Rapid Gas and Dust Variations in Comet C/2012 S1 (ISON): New Insights into the Origin of Cometary HNC. The Astrophysical Journal, 2017, 838 (2), pp.147. 10.3847/1538-4357/aa6590. hal-02186841

HAL Id: hal-02186841

https://hal.science/hal-02186841v1

Submitted on 28 Aug 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_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
<figure><img src="image_2.png" /></figure>

# ALMA Mapping of Rapid Gas and Dust Variations in Comet C/2012 S1 (ISON): New Insights into the Origin of Cometary HNC

M. A. Cordiner<fnref n="1" />,<fnref n="2" />, J. Boissier<fnref n="3" />, S. B. Charnley<fnref n="1" />, A. J. Remijan<fnref n="4" />, M. J. Mumma<fnref n="1" />, G. Villanueva<fnref n="1" />,<fnref n="2" />, D. C. Lis<fnref n="5" />, S. N. Milam<fnref n="1" />, L. Paganini<fnref n="1" />,<fnref n="2" />, J. Crovisier<fnref n="6" />, D. Bockelee-Morvan<fnref n="6" />, Y.-J. Kuan<fnref n="7" />,<fnref n="8" />, N. Biver<fnref n="6" />, and I. M. Coulson<fnref n="9" />

Received 2016 December 8; revised 2017 January 30; accepted 2017 February 8; published 2017 April 4

## Abstract

Observations of the sungrazing comet C/2012 S1 (ISON) were carried out using the Atacama Large Millimeter/ submillimeter Array at a heliocentric distance of 0.58–0.54 au (pre-perihelion) on 2013 November 16–17. Temporally resolved measurements of the coma distributions of HNC, CH₃OH, H₂CO, and dust were obtained over the course of about an hour on each day. During the period UT 10:10–11:00 on November 16, the comet displayed a remarkable drop in activity, manifested as a >42% decline in the molecular line and continuum fluxes. The H₂CO observations are consistent with an abrupt, ≈50% reduction in the cometary gas production rate soon after the start of our observations. On November 17, the total observed fluxes remained relatively constant during a similar period, but strong variations in the morphology of the HNC distribution were detected as a function of time, indicative of a clumpy, intermittent outflow for this species. Our observations suggest that at least part of the detected HNC originated from degradation of nitrogen-rich organic refractory material, released intermittently from confined regions of the nucleus. By contrast, the distributions of CH₃OH and H₂CO during the November 17 observations were relatively uniform, consistent with isotropic outflow and stable activity levels for these species. These results highlight a large degree of variability in the production of gas and dust from comet ISON during its pre-perihelion outburst, consistent with repeated disruption of the nucleus interspersed with periods of relative quiescence.

**Key words:** comets: individual (C/2012 S1 (ISON) – molecular processes – techniques: imaging spectroscopy – techniques: interferometric

## 1. Introduction

Sungrazing comet C/2012 S1 (hereafter referred to as comet ISON) made its first (and final) passage through the inner Solar System in 2013. It originated in the Oort Cloud at a distance ≳20,000 au, and its orbit passed within 0.013 au of the Sun at perihelion on 2013 November 28. By the time comet ISON reached perihelion, its (~300 m diameter) nucleus had disintegrated (Knight & Battams 2014; Lamy et al. 2014; Keane et al. 2016), leaving a trail of dust and debris in its wake.

Between 2013 November 12–18, comet ISON’s activity increased dramatically (see for example, Crovisier et al. 2013) as it traversed a heliocentric distance $r_H = 0.8–0.5$ au. During this period of outburst, the comet’s visual brightness and water production rate increased by over an order of magnitude, and strong brightness fluctuations (on the order of a factor of two) began to occur over timescales of less than a day (Combi et al. 2014; Sekanina & Kracht 2014). This event has been associated with fragmentation of the cometary nucleus and consequent increase in active surface area. The observation of coma wing features in the optical on November 14, 16, and 18 by Boehnhardt et al. (2013) may be taken as further evidence for the release of nucleus fragments. Agúndez et al. (2014) observed a dramatic increase in HCN production on November 14, followed by a remarkable daily variability using the IRAM

30 m telescope during the period November 13–16, immediately preceding our observations with the Atacama Large Millimeter/Submillimeter Array (ALMA)

Measurements of the spatial distributions of HCN, HNC, and H₂CO gas as well as thermal dust emission from the inner coma of comet ISON were presented by Cordiner et al. (2014), based on observations using ALMA on 2013 November 17, when the comet’s active area reached a peak (Combi et al. 2014). The HCN and H₂CO distributions were found to be quite symmetric, consistent with predominantly isotropic release of these molecules from within a few hundred kilometers of the nucleus. The HNC distribution, on the other hand, showed surprising collimated/clumpy features, suggesting release of this molecule within jets, streams, or clumps. Distributed/extended coma sources for HNC and H₂CO were definitively identified, but the detailed production mechanisms for these molecules are still not well understood (see also Cottin & Fray 2008).

In this article, we use temporally resolved ALMA observations to examine the detailed spatial distribution and time variability of emission from dust and molecules in comet ISON on 2013 November 16–17. The fine (≈17 minutes) time cadence of our molecular mapping provides powerful new insights into the short timescale variability of this comet during outburst, and helps elucidate the nature and origin of the anisotropic HNC features identified by Cordiner et al. (2014).

<footnote n="1">¹NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA; martin.cordiner@nasa.gov</footnote>

<footnote n="2">²Department of Physics, Catholic University of America, Washington, DC 20064, USA</footnote>

<footnote n="3">³IRAM, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France</footnote>

<footnote n="4">⁴National Radio Astronomy Observatory, Charlottesville, VA 22903, USA</footnote>

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

<footnote n="6">⁶LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, 5 place Jules Janssen, F-92195 Meudon, France</footnote>

<footnote n="7">⁷National Taiwan Normal University, Taipei 116, Taiwan, ROC</footnote>

<footnote n="8">⁸Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 106, Taiwan, ROC</footnote>

<footnote n="9">⁹East Asian Observatory, Hilo, HI 96720, USA</footnote>
<table><caption>**Table 1**
Summary of Observations</caption><thead><tr><th>Date</th><th>UT Time</th><th>Object</th><th>Scan</th></tr></thead><tbody><tr><td rowspan="15">2013 Nov 16</td><td>10:03:47–10:04:49</td><td>3C 279</td><td>1</td></tr><tr><td>10:05:44–10:08:21</td><td>Pallas</td><td>2</td></tr><tr><td>10:08:44–10:09:46</td><td>3C 279</td><td>3</td></tr><tr><td>10:10:27–10:17:19</td><td>ISON</td><td>4</td></tr><tr><td>10:17:30–10:18:32</td><td>3C 279</td><td>5</td></tr><tr><td>10:19:02–10:25:53</td><td>ISON</td><td>6</td></tr><tr><td>10:26:04–10:27:05</td><td>3C 279</td><td>7</td></tr><tr><td>10:27:36–10:34:28</td><td>ISON</td><td>8</td></tr><tr><td>10:34:45–10:35:47</td><td>3C 279</td><td>9</td></tr><tr><td>10:36:17–10:43:09</td><td>ISON</td><td>10</td></tr><tr><td>10:43:19–10:44:21</td><td>3C 279</td><td>11</td></tr><tr><td>10:45:02–10:51:53</td><td>ISON</td><td>12</td></tr><tr><td>10:52:03–10:53:06</td><td>3C 279</td><td>13</td></tr><tr><td>10:53:36–11:00:27</td><td>ISON</td><td>14</td></tr><tr><td>11:00:37–11:01:39</td><td>3C 279</td><td>15</td></tr><tr><td rowspan="20">2013 Nov 17</td><td>12:23:25–12:24:27</td><td>3C 279</td><td>1</td></tr><tr><td>12:25:16–12:27:53</td><td>Titan</td><td>2</td></tr><tr><td>12:28:08–12:29:10</td><td>3C 279</td><td>3</td></tr><tr><td>12:29:54–12:36:46</td><td>ISON</td><td>4</td></tr><tr><td>12:36:57–12:37:59</td><td>3C 279</td><td>5</td></tr><tr><td>12:38:30–12:45:21</td><td>ISON</td><td>6</td></tr><tr><td>12:45:33–12:46:35</td><td>3C 279</td><td>7</td></tr><tr><td>12:47:06–12:53:58</td><td>ISON</td><td>8</td></tr><tr><td>12:54:17–12:55:19</td><td>3C 279</td><td>9</td></tr><tr><td>12:55:50–13:02:42</td><td>ISON</td><td>10</td></tr><tr><td>13:02:53–13:03:55</td><td>3C 279</td><td>11</td></tr><tr><td>13:04:41–13:11:32</td><td>ISON</td><td>12</td></tr><tr><td>13:11:43–13:12:45</td><td>3C 279</td><td>13</td></tr><tr><td>13:13:16–13:20:08</td><td>ISON</td><td>14</td></tr><tr><td>13:20:19–13:21:21</td><td>3C 279</td><td>15</td></tr></tbody></table>

## 2. Observations

Observations were made in Cycle 1 Early Science mode using the (dual sideband) ALMA band 7 receiver, covering frequencies 350.3–352.3 GHz (lower sideband) and 362.2–364.1 GHz (upper sideband). Comet ISON was observed pre-perihelion on UT 2013 November 16 at 10:10–11:00 (at a heliocentric distance $r_H = 0.58$ au and geocentric distance $\Delta = 0.89$ au), and again on UT 2013 November 17 at 12:30–13:20 ($r_H = 0.54$ au, $\Delta = 0.88$ au). The illumination (Sun–comet–observer) phase angle was 82°–85°. The comet’s position was tracked using JPL Horizons ephemeris solution #45 and the coordinates of the ALMA phase center were updated in real time to account for the comet’s rapid non-sidereal motion. A summary of these observations, which constitute a subset of the data acquired during our full ALMA/ISON observing campaign, is given in Table 1.

The ALMA correlator was configured with four spectral windows to simultaneously observe all the lines of interest plus continuum on each day (see Table 2). Observations of the bright quasar 3C 279 were used to calibrate the instrumental bandpass, phase, and gain. For calibration of the flux scale, observations of the Solar System bodies Pallas and Titan were used, resulting in absolute fluxes accurate to within about 15%. Using 28 × 12 m antennae (with baseline lengths in the range 17.3–1284 m), the angular resolution was $0''28 \times 0''44$. The correlator channel spacing of 244 kHz resulted in a spectral resolution of 488 kHz (about $0.4 \text{ km s}^{-1}$) after Hanning

smoothing in the time domain. Weather conditions were excellent for all observations, with precipitable water vapor column at zenith of less than 0.57 mm. The rms of the phase variation was measured for all visits to the phase calibrator and for all baseline pairs, with median rms values of $15^{\circ}8$ on November 16 and $6^{\circ}4$ on November 17. These phase variations were tracked and corrected accordingly for each antenna.

The data were flagged, calibrated, and imaged using standard routines in CASA version 4.1.0 (McMullin et al. 2007). No significant flux was detected for baselines $\ge 400$ m, so the most distant antennae (DV07, DV19, and DV25; $>500$ m from the array center) were excluded during imaging to provide a more uniform Fourier sampling pattern (in the uv plane), resulting in a corresponding improvement in image quality at the expense of a small degradation in angular resolution (to $0''40 \times 0''54$). Deconvolution of the point-spread function was performed using the Högbom algorithm, with natural visibility weighting and a flux threshold of twice the expected rms noise per channel in each image. Initially, each science scan (see Table 1) was cleaned and imaged individually. However, to improve the signal-to-noise ratio for the purpose of the present study, the scans taken on each day were combined into pairs, by averaging scans 4 & 6, scans 8 & 10, and scans 12 & 14 into three discrete observation periods (hereafter referred to as periods 1, 2, and 3). Each period had a total on-source integration time of 13.7 minutes and the time interval between the start of successive periods was approximately 17–18 minutes.

Comet ISON’s 0.8 mm continuum was imaged by averaging the observed data over all line-free channels. The continuum peak was found to be offset by $5''7$ from the predicted ephemeris position at the start of observations on November 16, and by $6''6$ on November 17. The direction of offset was the same on both days: $75^{\circ}$ clockwise from celestial north, compared with the $71^{\circ}$ position angle of the Sun–comet vector. A similar offset was measured by optical observers, explainable as a result of non-gravitational acceleration of the comet due to preferential outgassing in the sunward-facing hemisphere (Sekanina & Kracht 2014). To maintain accurate flux measurements across our field of view, the interferometric images were corrected for the Gaussian spatial response of the ALMA primary beam (half-power beam-width = $16''$ at 363 GHz). Finally, the images were transformed from celestial coordinates to cometocentric (sky-projected) spatial distances, the origin of which was determined as the mean location of the continuum flux peak on each day. The coordinate axes are aligned with the equatorial system (celestial north is up).

## 3. Results

The molecular line data cubes were spectrally integrated over the full extent of detectable emission (between $-2$ and $+2 \text{ km s}^{-1}$ of line center), to produce maps for each molecule in each time period on November 16 (Figures 1 and 2) and November 17 (Figures 3 and 4). For consistency, common integration ranges and contour levels were applied across all time periods for a given species. For CH$_3$OH, several emission lines were detected (the $J_K = 1_1 - 0_0, 4_0 - 3_{-1}, 7_2 - 6_1$ and $16_1 - 16_0$ transitions), and these data were summed together to produce a single image for each period, with improved signal-to-noise ratio.

For each species (plus continuum), the total flux was obtained by integrating over the emission maps within a circle of radius $2''5$ (1600 km) centered on the origin. These fluxes
<table><caption>**Table 2**
Integrated Spectral Line and Continuum Fluxes as a Function of Time</caption><thead><tr><th rowspan="2">Species</th><th rowspan="2">Period<sup>a</sup></th><th rowspan="2">Transition</th><th rowspan="2">Frequency<br>(GHz)</th><th rowspan="2">E<sub>u</sub><br>(K)</th><th colspan="2">Flux<sup>b</sup></th></tr><tr><th>Nov 16</th><th>Nov 17</th></tr></thead><tbody><tr><td>HNC</td><td>1</td><td>4–3</td><td>362.630</td><td>43.5</td><td>1.03 ± 20</td><td>2.23 ± 20</td></tr><tr><td>HNC</td><td>2</td><td>4–3</td><td>362.630</td><td>43.5</td><td>0.21 ± 20</td><td>1.79 ± 20</td></tr><tr><td>HNC</td><td>3</td><td>4–3</td><td>362.630</td><td>43.5</td><td>0.17 ± 20</td><td>1.97 ± 20</td></tr><tr><td>CH<sub>3</sub>OH</td><td>1</td><td>multi<sup>c</sup></td><td>350–364</td><td>17–333</td><td>1.02 ± 44</td><td>2.08 ± 60</td></tr><tr><td>CH<sub>3</sub>OH</td><td>2</td><td>multi<sup>c</sup></td><td>350–364</td><td>17–333</td><td>0.21 ± 44</td><td>2.42 ± 60</td></tr><tr><td>CH<sub>3</sub>OH</td><td>3</td><td>multi<sup>c</sup></td><td>350–364</td><td>17–333</td><td>-0.32 ± 44</td><td>2.03 ± 60</td></tr><tr><td>H<sub>2</sub>CO</td><td>1</td><td>5<sub>1,5</sub> – 4<sub>1,4</sub></td><td>351.769</td><td>62.5</td><td>1.96 ± 17</td><td>3.83 ± 18</td></tr><tr><td>H<sub>2</sub>CO</td><td>2</td><td>5<sub>1,5</sub> – 4<sub>1,4</sub></td><td>351.769</td><td>62.5</td><td>1.13 ± 17</td><td>3.59 ± 18</td></tr><tr><td>H<sub>2</sub>CO</td><td>3</td><td>5<sub>1,5</sub> – 4<sub>1,4</sub></td><td>351.769</td><td>62.5</td><td>0.77 ± 17</td><td>3.73 ± 18</td></tr><tr><td>Continuum</td><td>1</td><td>...</td><td>357</td><td>...</td><td>8.2 ± 1.9</td><td>14.9 ± 2.3</td></tr><tr><td>Continuum</td><td>2</td><td>...</td><td>357</td><td>...</td><td>4.9 ± 1.9</td><td>10.2 ± 2.3</td></tr><tr><td>Continuum</td><td>3</td><td>...</td><td>357</td><td>...</td><td>1.8 ± 1.9</td><td>17.1 ± 2.3</td></tr></tbody></table>

**Notes.**

<sup>a</sup> Time period—see Section 2.

<sup>b</sup> Integrated line flux within a 2"5-radius circular aperture centered on the comet; 1σ errors on trailing digits given in parentheses. Units are Jy km s⁻¹ for the molecular lines and mJy for continuum.

<sup>c</sup> The CH<sub>3</sub>OH maps are a sum over four transitions: 4<sub>0</sub> – 3<sub>−1</sub> (350687.7 MHz), 1<sub>1</sub> – 0<sub>0</sub> (350905.1 MHz), 16<sub>1</sub> – 16<sub>0</sub> (363440.4 MHz) and 7<sub>2</sub> – 6<sub>1</sub> (363739.9 MHz).

are given in Table 2. Uncertainties (in parentheses) are statistical 1σ errors, calculated from the rms of emission-free regions of the observed images. The maximum recoverable angular scale for our observations was about 6".

### 3.1. 2013 November 16

Between the start and finish of our observations on November 16, a dramatic drop in total integrated flux was observed in comet ISON for all spectral lines and the continuum. A calibration error or problem with the telescope array can be ruled out as the source of this variation because our images of the phase calibrator 3C 279 (less than 10° away on the sky) showed a uniform intensity point-source throughout the observations. As stated in Section 2, the antenna phase fluctuations were small enough to be easily tracked and corrected between visits to the phase calibrator; resulting in a stable flux response as a function of time.

The HNC map for period 1, observed on November 16 (starting at UT 2013 November 16 10:10; see Figure 1) shows a peak near the nominal nucleus position (indicated with a white cross), and a second, elongated structure extending away toward the north, which appears to be partially separated from the main peak. This northerly elongated clump is reminiscent of the HNC streams/jets identified by Cordiner et al. (2014) on November 17, indicating that these peculiar structures were not a temporally isolated phenomenon unique to those observations. The HNC flux on November 16 fell from 0.7 ± 0.2 Jy km s⁻¹ to 0.1 ± 0.2 Jy km s⁻¹ during the 35 minutes between periods 1 and 3. The corresponding reduction in signal-to-noise ratio precludes the possibility of tracking the time-evolution of the HNC clumpy structure on this date.

A significant reduction in flux as a function of time was also observed for CH<sub>3</sub>OH, but again, these maps suffer from low signal-to-noise. The H<sub>2</sub>CO maps contain more flux, showing a clear central peak and relatively symmetric spatial distribution consistent with isotropic outgassing. The H<sub>2</sub>CO distribution remained centrally peaked while the flux fell in an approximately linear fashion by 52%–72% between periods 1 and 3.

In the 0.8 mm continuum maps (shown in the lower panels of Figure 2), the emission contours show a clear elongation toward the upper right of the figure, consistent with the approximate direction of the comet’s orbital trail and the anti-sunward vector. Similar to the molecular species, the integrated continuum flux also exhibited an apparently linear decrease with time, falling by at least 42% during our observations, and shows that the rapid decline in comet ISON’s activity was not limited to only the gaseous component of the coma. Figure 5 (upper panel) shows a plot of the gas and continuum flux measurements as a function of time (including 1σ error bars), where the declining flux trends are clearly apparent.

### 3.2. 2013 November 17

By the start of our ALMA observations on November 17 (approximately 26 hr later), the observed line and continuum fluxes had risen by about a factor of two relative to the start of observations on November 16, and remained at a relatively constant level throughout the subsequent hour of ALMA observing. The total fluxes are shown as a function of time in the lower panel of Figure 5 and there is little evidence of any significant variation outside of the observational uncertainties.

The relative stability of the comet’s activity is also apparent from the coma maps in Figures 3 and 4. Apart from the (random) noise features, the CH<sub>3</sub>OH, H<sub>2</sub>CO, and continuum morphologies all show good consistency between the three time periods. The HNC maps, on the other hand, reveal a striking time variability that is most evident when comparing observation periods 1 and 3. In period 1, the HNC peak (detected at >6σ level, where σ is the rms noise), appears at a position coincident with the continuum and other molecules, but in period 2, the HNC peak is shifted about 400 km toward the upper right of the map. Period 3 shows a weaker central emission peak and isolated, compact clump of strong (6σ) HNC emission (marked with an asterisk), at a position 870 ± 25 km north-west of the nominal nucleus position, at an angle 47° clockwise from celestial north.
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Contour maps of the spectrally integrated HNC (top row) and CH₃OH (bottom row) line flux maps observed in comet S1/ISON on 2013 November 16. Three time intervals are shown, each separated by about 18 minutes. Contour intervals are 1.5σ for HNC and 2σ for CH₃OH, where σ(HNC) = 26 mJy km s⁻¹ and σ(CH₃OH) = 58 mJy km s⁻¹. Integrated flux within a circular aperture of radius 1600 km centered on the comet is given at the top left of each map, with 1σ uncertainty in parentheses. Central crosses mark the same reference position relative to the comet in each map. The hatched ellipse indicates the spatial resolution. Axes are aligned with the equatorial system (celestial north is up).</figcaption></figure>

To highlight the significance of this temporal HNC variation, Figure 6 shows one-dimensional slices through the HNC maps for each period, taken along the black dashed line shown in Figure 3, and passing through the center of the isolated clump. The shaded area in these plots represents the 1σ error envelope. Note that in this analysis the signal-to-noise of our spectral profiles was insufficient to derive any useful radial velocity information for the gases, so we are necessarily limited to the discussion of sky-projected distances in two dimensions, which is implicitly assumed from here on.

In the first observation period, the 1D HNC profile (Figure 6) is strongly centrally peaked. In period 2, the distribution is significantly broader and flatter, with a weakened central peak. In the third period the profile is broader and flatter still (with the central peak weakened to less than or about half its initial value), combined with the appearance of a spatially isolated HNC peak/clump far out into the coma. About 20% of the total HNC flux is concentrated inside the 3σ contour surrounding this clump.

We followed the same methodology as Cordiner et al. (2014) to fit the visibility (Fourier) amplitude components of the observed HNC data using a Haser daughter model. The real parts of the visibility amplitudes (visibilities) were first rebinned to a uniform antenna separation (baseline) grid and are plotted as a function of baseline in Figure 7 for the three time periods. For each period, the visibilities show a relative excess of flux at large angular scales (short baselines) that

cannot be explained if the observed HNC is a parent molecule, thus confirming the conclusions of Lis et al. (2008) and Cordiner et al. (2014) that HNC is a daughter/product species, with a distributed source in the coma. For the first two time periods, the best-fitting HNC parent scale length ($L_p$) was found to be 450 km (with possible values in the range $L_p$ = 250–1200 km due to statistical uncertainties). For the third period, it was only possible to derive a lower limit from our data of $L_p$ > 750 km; this is due to an excess of extended flux that cannot be accounted for by our model. Our inability to fully constrain the scale of HNC production at that epoch suggests that the observed HNC distribution was even broader than can be explained using a standard Haser model, and further highlights the importance of coma production for this species. For a more detailed interpretation of these data, a three-dimensional (anisotropic), time-variable radiative transfer model is required, which is beyond the scope of the present study, but is currently in development.

# 4. Discussion

## 4.1. *Temporal Variability of ISON's Coma*

Cometary activity is often observed to vary smoothly with heliocentric distance. Nevertheless, short timescale variations (on periods of hours to days) are not uncommon (e.g., Mumma et al. 1986; Sekanina et al. 2002; Li et al. 2011; Drahus et al. 2012), and localized outbursts have recently been observed
<figure><img src="image_4.png" /><figcaption>**Figure 2.** As Figure 1, but for H₂CO and continuum emission. Contour intervals are 4σ for H₂CO and 1σ for continuum, where σ(H₂CO) = 22 mJy km s⁻¹ and σ (continuum) = 0.25 mJy km s⁻¹. The comet's illumination phase and sky-projected vectors in the direction of the Sun and dust trail are shown bottom-right in the upper middle panel.</figcaption></figure>

in detail by Rosetta in comet 67P/Churyumov–Gerasimenko (Grün et al. 2016). Our ALMA observations of C/2012 S1 (ISON), however, constitute the first detections of strong variability in HNC, H₂CO and sub-millimeter continuum over timescales of less than an hour. The drop in line and continuum fluxes by over 42% in such a short timescale is remarkable as it implies an extremely abrupt, spontaneous change in the comet’s activity.

The observed rapid drop in line and continuum fluxes during our November 16 observations can plausibly be explained by an abrupt decrease in the comet’s gas and dust production near to the start of our ALMA observations. Following this drop in activity, we hypothesize that the three main processes responsible for the loss of detected emission as a function of time are (1) molecular photodissociation, (2) sublimation of icy grains, and (3) transport of the coma material out of the ALMA field of view. The latter is expected due to the outflow/ expansion of the coma (for gas and dust), with the additional possibility of differential sublimation pressure that may result in the acceleration of solid particles.

To explore the possible impact on the observed fluxes of coma expansion following a reduction in comet activity, a simple, spherically symmetric, constant-velocity outflow model was generated. Assuming the nucleus instantaneously stopped producing material at the start of our observations on November 16 (at around UT 2013 November 16 10:10), and the coma was allowed to continue expanding outwards at the same velocity, the fraction of material remaining within the 2.′′5-radius integration aperture was calculated as a function

of time and plotted with a dotted curve (for an outflow velocity $v_{\text{out}} = 1.0 \text{ km s}^{-1}$) and a dotted-dashed curve (for $v_{\text{out}} = 0.5 \text{ km s}^{-1}$) in the upper panel of Figure 5. These curves bracket the range of gradients in the observed line and continuum fluxes.

Given the reappearance of intense molecular and dust emission from the comet 26 hr later on November 17, combined with the general trend for increasing $\text{Ly}\alpha$ and optical flux on the days around our ALMA observations (see Combi et al. 2014; Sekanina & Kracht 2014), it seems unlikely that cometary activity ceased completely during our November 16 observations. The decay in the ALMA fluxes was probably offset by at least some new gas and dust production. A more realistic scenario to explain our observations was obtained by constructing a time-dependent Haser daughter model for H₂CO, with fixed parent scale length of 280 km, H₂CO mixing ratio of 0.8%, fixed temperature of T = 90 K, $v_{\text{out}} = 1.0 \text{ km s}^{-1}$ (see Cordiner et al. 2014) and a photodissociation rate of $6.7 \times 10^{-4} \text{ s}^{-1}$ (appropriate for $r_{\text{H}} = 0.58$ au; Huebner et al. 1992). Synthetic images were generated using the CASA simulator, with the same observational and imaging characteristics as for our ALMA observations. Although our observations could be reproduced by many different time-variability scenarios, given our limited number of data points we adopt the simplest possible model to fit the data, in which the cometary H₂O production rate has an initial value $Q_i$, which falls (instantaneously) to a final value $Q_f$ after a time t. The best fit to our measured H₂CO fluxes is for $Q_i = 1.05 \times 10^{29} \text{ s}^{-1}$, $Q_f/Q_i = 0.49$ and t = 3.5 minutes, which results in the decay
<figure><img src="image_5.png" /><figcaption>**Figure 3.** As Figure 1, but for the following day (2013 November 17). The asterisk in the upper right panel indicates the position of an HNC clump and the dashed line is its putative outflow axis. Contour intervals are 1.5σ for HNC and 2σ for CH₃OH, where the rms noise levels are σ(HNC) = 30 mJy km s⁻¹ and σ(CH₃OH) = 68 mJy km s⁻¹.</figcaption></figure>

curve shown with a dashed black line in Figure 5. Such a sharp ≈50% reduction in the cometary production rate could be due, for example, to (1) the switching off of a powerful jet or large active region as a result of rotation-induced changes in the nucleus illumination, or (2) sudden depletion/exhaustion of volatiles from a component of the cometary material, which may be a consequence of the rapid evolution of a nucleus undergoing a series of disruptive outbursts.

Photodissociation can be ruled out as a loss process for the large dust grains thought to be responsible for the 0.8 mm continuum emission. However, if these grains contain a significant amount of ice, sublimation may be an important mechanism. For icy sub-millimeter grains at $r_H \approx 0.5$ au, Beer et al. (2006) calculated a lifetime (for complete sublimation) on the order of a few thousand seconds. The observed drop in continuum flux is therefore likely due to a reduction in dust grain production, followed by sublimation and the continued motion of the dust out of the ALMA field of view. Without sublimation, and assuming a constant size and temperature for the grains, a radial outflow velocity of >0.5 km s⁻¹ is required to explain the more than a factor of two drop in continuum flux on November 16 (Figure 5, upper panel). Due to its small size, the thermal continuum emitted by the comet's nucleus is assumed to be negligible.

Due to a lack of previous mapping observations at mm/sub-mm wavelengths, the velocity distribution of large grains in cometary comae is not well established. Sekanina & Chodas (2012) determined a velocity of 30 m s⁻¹ for the submillimeter-sized dust released from sungrazing comet C/2013 W3 (Lovejoy) during its disruption. Boissier et al. (2012) found grain outflow velocities up

to 100 m s⁻¹ in the coma of 17P/Holmes, and during the Deep Impact event, $v_{\text{out}} \sim 200$ m s⁻¹ was observed for the dust in 9P/Tempel 1 (Keller et al. 2007). Thus, the drop in continuum flux can probably not be explained by outflow alone confirming the likely role of icy grain sublimation. Our simplistic calculation does not account for the observed asymmetry (and implied anisotropic outflow) in the continuum maps. The properties of the large grains in comet ISON, including their density distribution, velocity field, and sublimation rates may thus be better constrained through detailed (3D) modeling of our ALMA continuum data in a future study.

Sublimation pressure of vaporizing material in comet ISON (including water as well as more refractory species) has been invoked to explain the anomalous non-gravitational motions experienced by the comet in its run up to perihelion (Sekanina & Kracht 2014), and such forces may also have played a role in the breakup of the nucleus (Steckloff et al. 2015). Single-dish observations of ISON's sub-millimeter continuum emission by Keane et al. (2016) were found to be consistent with the non-gravitational model of Sekanina & Kracht (2014), thus confirming the impact of intense sublimation pressure on the trajectory of the cometary material. The presence of a (time-variable) sub-millimeter emission tail in the anti-sunward direction (see Figures 2 and 4) is consistent with this scenario. We therefore conclude that the large grains responsible for the sub-millimeter continuum emission observed by ALMA underwent enhanced heating on the sunward side, giving rise to a sublimation pressure that accelerated them away from the nucleus in the anti-sunward direction. This acceleration was
<figure><img src="image_6.png" /><figcaption>**Figure 4.** As Figure 2, but for the following day (2013 November 17). Contour intervals are $4\sigma$ for H$_2$CO and $1\sigma$ for continuum, where $\sigma(\text{H}_2\text{CO}) = 18$ mJy km s$^{-1}$ and $\sigma(\text{continuum}) = 0.26$ mJy km s$^{-1}$.</figcaption></figure>

probably responsible for some of the drop in continuum flux observed on November 16.

## 4.2. Elucidating the Nature of Cometary HNC Release

The time-evolution of the HNC distribution on November 17 (Figures 3 and 6) seems to be most naturally interpreted as due to the release of an isolated clump of material from the nucleus that traveled radially outward through the coma at an average velocity of $0.41 \text{ km s}^{-1}$ (in the plane of the sky), to reach a distance of 870 km in period 3. Given the HNC line FWHM of $2.0 \text{ km s}^{-1}$, the inferred clump outflow rate is reasonable (especially considering the possibility of an additional velocity component perpendicular to the plane of the sky), and is well within the $1 \text{ km s}^{-1}$ outflow velocity for HCN and other species deduced by Agúndez et al. (2014) and Cordiner et al. (2014). The derived outflow velocity is also consistent with the approximate limit of $0.5 \text{ km s}^{-1}$ on the outflow rate of millimeter-sized dust. Such a transient, spatially isolated, directional outburst of material bears qualitative similarities to the collimated dust jets (Lin et al. 2015) and decimeter-sized aggregates (Agarwal et al. 2016), emitted from confined regions on the surface of comet 67P/Churyumov–Gerasimenko, as observed by the Rosetta spacecraft.

The production rate of HNC in the clump can be derived by modeling the flux map in period 3 of November 17 using a two-component isotropic outflow model. A source of HNC was placed at the nominal nucleus position (white cross) and at the HNC peak (asterisk), both with $v_{\text{out}} = 1 \text{ km s}^{-1}$ and $T = 90$ K. Optimizing the HNC production rates of the two sources using

a nonlinear least-squares procedure, an excellent fit to the observed image was obtained with $Q(\text{HNC}) = 2.9 \times 10^{25} \text{ s}^{-1}$ for the nucleus and $Q(\text{HNC}) = 3.2 \times 10^{25} \text{ s}^{-1}$ for the clump. A spectrally integrated image of the best-fitting two-component HNC model is shown in the middle panel of Figure 8, and the observation-minus-model image is shown in the right panel, for which the noise-like residuals indicate the quality of fit.

Given the expected $1/r^2$ falloff in the density of a parcel of expanding gas released from the nucleus, and the fact that the amplitude of the main HNC peak in Figure 6 remains approximately constant despite traversing over a factor of two in distance between periods 2 and 3, it seems unlikely that such a well-defined clump could be released as gaseous HNC directly from the nucleus unless it was as an extremely narrow, well-confined HNC jet. Based on our interpretation of the HNC time series, a more likely explanation is that the observed HNC peak originates from an ice or organic dust-rich clump, aggregate or chunk of material emitted from the nucleus that underwent degradation/sublimation as it traveled out through the coma. If this material was mostly ice, then unless it was extremely HNC rich, a clump would also be expected to be apparent at the same positions in the H$_2$CO and CH$_3$OH maps. From the fact that the clump is not observed in H$_2$CO or CH$_3$OH but appears in the same general direction from the nucleus as the dust continuum tail, it follows that the clump likely originates from a macromolecular or polymeric (refractive) precursor more closely associated with the cometary dust than the ice. The increase in HNC flux on large scales in the third epoch, as highlighted by the observed visibility
<figure><img src="image_7.png" /><figcaption>**Figure 5.** Total line flux (left ordinate) and continuum flux (right ordinate) as a function of time after the start of observations on November 16 (top panel) and November 17 (bottom panel). The result of a simulated H₂CO outflow model (with gas production rate falling to Qf = 0.49Qi after 3.5 minutes) is shown with a black dashed line. Calculated flux decay curves due to coma expansion following an instantaneous halt to cometary production are also shown for outflow velocities of 1 km s⁻¹ and 0.5 km s⁻¹.</figcaption></figure>

amplitudes (Figure 7), is also consistent with a spontaneous increase in the production of HNC in the coma as this clumpy material moved outward.

Our results are consistent with the hypothesis that cometary HNC originates from the degradation of macromolecules or polymeric material contained within the nucleus. Previously, Rodgers & Charnley (2001) and Lis et al. (2008) discussed possible macromolecular sources of cometary HNC, including hexamethylenetetramine (HMT; C₆H₁₂N₄), HCN polymer or other large organic molecules that undergo photolytic or thermal degradation in the coma. Refractory organic particles are known to exist in comets (Cottin et al. 2004), and are believed to have originated in the interstellar medium or protosolar disk. Polyoxymethylene (POM), in particular, has been studied in detail as a candidate to explain the distributed H₂CO sources in comets 1P/Halley and C/1995 O1 (Hale-Bopp) (Cottin et al. 2004; Fray et al. 2006). Recent in situ work on comet 67P using the Rosetta COSIMA instrument revealed the presence of very large macromolecular compounds in the cometary dust, analogous to the insoluble organic matter found in carbonaceous meteorites (Fray et al. 2016). Possible

evidence for a radiation-induced, POM-like polymer was also found on the surface of 67P by the Ptolemy instrument (Wright et al. 2015), but a conclusive identification of specific macromolecules (including HMT, POM and HNC polymer), remains elusive (C. Altwegg 2016, private communication). Now that detailed mapping of cometary molecular distributions has become routine (thanks to ALMA), additional comparisons between laboratory data and astronomical observations on the breakdown of large molecules will be possible, to further constrain the nature of macromolecular cometary organic material.

Based on the differences between the HNC and H₂CO coma morphologies, we conclude that the organic dust source for HNC is not related to that responsible for the distributed source of cometary H₂CO. This implies the presence of at least two kinds of macromolecular parent material in comets: nitrogen-rich and oxygen-rich, the identification of which remains a challenge for laboratory astrophysics.

## 5. Conclusion

Spatially and temporally resolved observations of molecular and dust emission from C/2012 S1 (ISON) were obtained as the comet passed between 0.58 and 0.54 au of the Sun on its approach to perihelion in November 2013. The observed maps reveal a complex and dynamic coma, with molecular line and continuum features evolving rapidly over periods of tens of minutes. The anisotropic HNC outflow features detected by Cordiner et al. (2014) are found to be due to the presence of time-variable HNC clumps or well-confined jets moving outward through the coma, and may be explained as the result of the breakdown of HNC-rich icy particles, or refractory materials including organic dust grains, polymers or other macromolecules. The exact nature of the HNC parent has been debated in the literature for some time (Irvine et al. 1998; Rodgers & Charnley 2005; Lis et al. 2008; Cordiner et al. 2014), but our observations strongly suggest an origin for cometary HNC in organic refractory material, released intermittently from confined regions on the nucleus.

A rapid decay in the observed gas emission on November 16 (over a period of 50 minutes) is probably the result of a substantial reduction in the activity of the comet during our observations, followed by partial dissipation of the coma through photodissociation and outflow processes. Using a Haser daughter model the H₂CO observations on November 16 can be explained as being due to a ≈50% drop in the cometary production rate near the beginning of our observations. The surprisingly rapid decay in millimeter continuum flux implies rapid dust outflow, probably combined with the partial sublimation of large, icy grains. Following this lull, coma activity had returned strongly by UT 12:30 on November 17, about a factor of two higher than at the start of our observations on November 16.

Combined with previous radio and optical observations, these data reveal an extremely erratic behavior in the outgassing of volatiles from comet ISON as it approached the Sun, with periods of strong outburst interspersed with quiescent intervals, resulting in sporadic production of gas and dust. Future studies of cometary outgassing and volatile depletion during nucleus disruption will be required to help explain the origin of this behavior. The surprising coma variability detected with ALMA demonstrates the importance of temporally and spatially resolved observations on the
<figure><img src="image_8.png" /><figcaption>**Figure 6.** Spatial cuts through the HNC maps at the top of Figure 3, showing the flux as a function of distance along the dashed black line (passing through the continuum peak and HNC clump marked "*"). Vertical dashed lines show the peak flux position for each period.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Figure 7.** Real part of the observed HNC (4–3) visibility amplitude (Re) vs. baseline length, for each of the three time periods on November 17. For the first two epochs, the best-fitting Haser daughter model (with $L_p = 450$ km) is shown with a red curve. For the third epoch, only a lower limit for the HNC parent scale length ($L_p > 750$ km) could be obtained. Purple dotted curves show the simulated visibility amplitudes for a parent distribution, which do not provide a good fit to the data.</figcaption></figure>

<figure><img src="image_10.png" /><figcaption>**Figure 8.** Left: integrated flux map for HNC on November 17, period 3. Middle: best-fitting two-component (composite) HNC production model. Right: residuals (model minus observed image); contour intervals are $1\sigma$.</figcaption></figure>

smallest scales in order to properly understand the structure and composition of cometary comae. Detailed maps of the distributions of coma product species such as HNC and H₂CO, combined with laboratory experiments on the breakdown of candidate parent materials will be required to obtain a full understanding of the origins and complex behaviors of these intriguing cometary molecules.

This study was supported by the National Science Foundation under grant no. AST-1616306, by NASA's Planetary Atmospheres and Planetary Astronomy Programs and by the NASA Astrobiology Institute through the Goddard Center for

Astrobiology. It makes use of ALMA data set #2012.A.00033. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. D.C.L. is supported by NASA through JPL/Caltech. D.M. is supported by Basal CATA PFB-06 and the ICM MAS. Y.J.K. is supported by NSC grants 99-2112-M-003-003-MY3 and 100-2119-M-003-001-MY3.
References

Agarwal, J., A'Hearn, J., & Vincent, J.-B. 2016, MNRAS, 462, S78

Agúndez, M., Biver, N., Santos-Sanz, P., Bockelée-Morvan, D., & Moreno, R. 2014, A&A, 564, L2

Beer, E. H., Podolak, M., & Prialnik, D. 2006, Icar, 180, 473

Boehnhardt, H., Tubiana, C., Oklay, N., et al. 2013, CBET, 3715, 1

Boissier, J., Bockelée-Morvan, D., Biver, N., et al. 2012, A&A, 542, A73

Combi, M. R., Fougere, N., Mäkinen, J. T. T., et al. 2014, ApJL, 788, L7

Cordiner, M. A., Remijan, A. J., Boissier, J., et al. 2014, ApJL, 792, L2

Cottin, H., Bénilan, Y., Gazeau, M.-C., & Raulin, F. 2004, Icar, 167, 397

Cottin, H., & Fray, N. 2008, SSRv, 138, 179

Crovisier, J., Colom, P., Bockelée-Morvan, D., et al. 2013, CBET, 3711, 1

Drahus, M., Jewitt, D., Guilbert-Lepoutre, A., Waniak, W., & Sievers, A. 2012, ApJ, 756, 80

Fray, N., Bardyn, A., Cottin, H., et al. 2016, Natur, 538, 72

Fray, N., Bénilan, Y., Biver, N., et al. 2006, Icar, 184, 239

Grün, E., Agarwal, J., Altobelli, N., et al. 2016, MNRAS, 462, S220

Huebner, W. F., Keady, J. J., & Lyon, S. P. 1992, Ap&SS, 195, 1

Irvine, W. M., Bergin, E. A., Dickens, J. E., et al. 1998, Natur, 393, 547

Keane, J. V., Milam, S. N., Coulson, I. M., et al. 2016, ApJ, 831, 207

Keller, H. U., Küppers, M., & Fornasier, S. 2007, Icar, 191, 241

Knight, M. M., & Battams, K. 2014, ApJL, 782, L37

Lamy, P., Toth, I., Li, J., & Weaver, H. 2014, in Asteroids, Comets, Meteors—Book of Abstracts, ed. K. Muinonen et al. (Finland: Univ. Helsinki), 304

Li, J., Jewitt, D., Clover, J. M., & Jackson, B. V. 2011, ApJ, 728, 31

Lin, Z.-Y., Ip, W.-H., & Lai, I.-L 2015, A&A, 583, A11

Lis, D. C., Bockeleé-Morvan, D., Boissier, J., et al. 2008, ApJ, 675, 931

McMullin, J. P., Waters, B., Schiebel, D., Young, W., & Golap, K. 2007, in ASP Conf. Ser. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw, F. Hill, & D. J. Bell (San Francisco, CA: ASP), 127

Mumma, M. J., Weaver, H. A., Larson, H. P., Williams, M., & Davis, D. S. 1986, Sci, 232, 1523

Rodgers, S. D., & Charnley, S. B. 2001, MNRAS, 323, 84

Rodgers, S. D., & Charnley, S. B. 2005, MNRAS, 356, 1542

Sekanina, Z., & Chodas, P. W. 2012, ApJ, 757, 127

Sekanina, Z., Jehin, E., Boehnhardt, H., et al. 2002, ApJ, 572, 679

Sekanina, Z., & Kracht, R. 2014, arXiv:1404.5968

Steckloff, J. K., Johnson, B. C., & Bowling, T. 2015, Icar, 258, 430

Wright, I., Sheridan, S., Barber, S., et al. 2015, Sci, 349, aab0673