# The Volatile Composition of the Inner Coma of Comet 46P/Wirtanen: Coordinated Observations Using iSHELL at the NASA-IRTF and Keck/NIRSPEC-2

Nathan Roth, Boncho Bonev, Michael Disanti, Neil Dello Russo, Adam Mckay, Erika Gibb, Mohammad Saki, Younas Khan, Ronald Vervack, Hideyo Kawakita, et al.

► To cite this version:

Nathan Roth, Boncho Bonev, Michael Disanti, Neil Dello Russo, Adam Mckay, et al. The Volatile Composition of the Inner Coma of Comet 46P/Wirtanen: Coordinated Observations Using iSHELL at the NASA-IRTF and Keck/NIRSPEC-2. The Planetary Science Journal, 2021, 2 (2), pp.54. 10.3847/PSJ/abd706/54. hal-03447139

HAL Id: hal-03447139

https://hal.science/hal-03447139

Submitted on 10 Dec 2021

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>

# The Volatile Composition of the Inner Coma of Comet 46P/Wirtanen: Coordinated Observations Using iSHELL at the NASA-IRTF and Keck/NIRSPEC-2

Nathan X. Roth<sup>1,2,12</sup> ID, Boncho P. Bonev<sup>3,12</sup> ID, Michael A. DiSanti<sup>4,12</sup> ID, Neil Dello Russo<sup>5,12</sup> ID, Adam J. McKay<sup>3,4,12</sup> ID, Erika L. Gibb<sup>6,12</sup> ID, Mohammad Saki<sup>6,12</sup> ID, Younas Khan<sup>6,12</sup> ID, Ronald J. Vervack, Jr.<sup>5,12</sup> ID, Hideyo Kawakita<sup>7,12</sup> ID, Anita L. Cochran<sup>8</sup> ID, Nicolas Biver<sup>9</sup> ID, Martin A. Cordiner<sup>1,10</sup> ID, Jacques Crovisier<sup>9</sup>, Emmanuel Jehin<sup>11</sup> ID, and Harold Weaver<sup>5</sup> ID

## Abstract

The 2018 perihelion passage of comet 46P/Wirtanen afforded an opportunity to measure the abundances and spatial distributions of coma volatiles in a Jupiter-family comet with exceptional spatial resolution for several weeks surrounding its closest approach to Earth ($\Delta_{min} \sim 0.078$ au on UT December 16). We conducted near-infrared spectroscopic observations of 46P/Wirtanen using iSHELL at the NASA Infrared Telescope Facility on UT 2018 December 18 in direct coordination with observations using the newly upgraded NIRSPEC-2 instrument at the W. M. Keck Observatory, and securely detected fluorescent emission from $CH_3OH$, $C_2H_6$, and $H_2O$. This coordinated campaign utilizing the two premier near-infrared facilities in the northern hemisphere enabled us to sample distinct projections of the coma into the plane of the sky simultaneously, and provided an unprecedented view into the inner coma of 46P/Wirtanen near closest approach. We report rotational temperatures, production rates, and abundance ratios (i.e., mixing ratios) for all sampled species and compare our iSHELL results to simultaneous (or near-simultaneous) measurements taken with NIRSPEC-2. We demonstrate the extraordinary synergy of coordinated measurements using iSHELL and NIRSPEC-2, and advocate for future cometary studies that jointly leverage the capabilities of these two facilities.

*Unified Astronomy Thesaurus concepts: Molecular spectroscopy (2095); High resolution spectroscopy (2096); Near infrared astronomy (1093); Comae (271); Comets (280)*

## 1. Introduction

The study of comets affords a unique window into the birth, infancy, and subsequent evolution of the solar system. Soon after their accretion from the solar nebula at the time of planet formation, comets were gravitationally scattered across the solar system, with many emplaced in their present-day dynamical reservoirs, the Oort cloud or the Kuiper disk. Here they have remained in the cold outer solar system for the last ~4.5 Gyr, suffering minimal thermal and radiative processing. Systematically characterizing the compositions of their nuclei should therefore provide insights into the composition and thermochemical processes in the solar nebula where (and when) they formed (Bockelée-Morvan et al. 2004; Mumma &

Charnley 2011; Dello Russo et al. 2016a; Bockelée-Morvan & Biver 2017).

The composition of the nucleus is predominantly inferred through remote sensing observations, with each wavelength from the millimeter to the UV probing a distinct chemical and physical domain of the coma. Long-slit, high-resolution near-infrared spectroscopy samples the chemistry of the coma within a few thousand kilometers of the nucleus, providing information in two dimensions, spectral and spatial. With their wide spectral grasp, modern state-of-the-art near-infrared echelle spectrometers, such as iSHELL at the NASA Infrared Telescope Facility (IRTF) and NIRSPEC-2 at the W. M. Keck Observatory, provide not only compositional information by sampling multiple strong transitions of targeted coma molecules, but also spatial information via measurement of molecular column densities along their slits (of length 15" for iSHELL and 24" for NIRSPEC-2). These measurements provide abundances of trace species (e.g., ethane ($C_2H_6$), methanol ($CH_3OH$), hydrogen cyanide (HCN), ammonia ($NH_3$)) relative to water ($H_2O$), the dominant volatile in the comae of most measured comets, and reveal how volatiles (ices) are associated or segregated in the nucleus by searching

<figure><img src="image_3.png" /></figure>

<footnote n="1">¹ Solar System Exploration Division, Astrochemistry Laboratory Code 691, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA
nathaniel.x.roth@nasa.gov</footnote>

<footnote n="2">² Universities Space Research Association, Columbia, MD 21046, USA</footnote>

<footnote n="3">³ Department of Physics, American University, 4400 Massachusetts Avenue NW, Washington, DC 20016, USA</footnote>

<footnote n="4">⁴ Solar System Exploration Division, Planetary Systems Laboratory Code 693, NASA-GSFC, Greenbelt, MD 20771, USA</footnote>

<footnote n="5">⁵ Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA</footnote>

<footnote n="6">⁶ Department of Physics & Astronomy 1 University Boulevard, University of Missouri-St. Louis, St. Louis, MO 63121, USA</footnote>

<footnote n="7">⁷ Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, 603-8555, Japan</footnote>

<footnote n="8">⁸ University of Texas at Austin/McDonald Observatory, 2512 Speedway, Stop C1402, Austin, TX 78712, USA</footnote>

<footnote n="9">⁹ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, F-92195 Meudon, France</footnote>

<footnote n="10">¹⁰ Department of Physics, Catholic University of America, Washington DC, USA</footnote>

<footnote n="11">¹¹ Space sciences, Technologies & Astrophysics Research (STAR) Institute, University of Liège, Belgium</footnote>

<footnote>Received 2020 September 30; revised 2020 December 16; accepted 2020 December 17; published 2021 March 15</footnote>

<footnote n="12">¹² Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration.</footnote>

<footnote>Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.</footnote>
<table><caption>**Table 1**
Observing Log</caption><thead><tr><th>UT Time</th><th>Setting</th><th>Target</th><th>T<sub>int</sub><br>(minute)</th><th>r<sub>H</sub><br>(au)</th><th>Δ<br>(au)</th><th>dΔ/dt<br>(km s<sup>-1</sup>)</th><th>Molecules<br>Sampled</th><th>Slit PA<br>(°)</th></tr></thead><tbody><tr><td colspan="9" style="text-align: center; font-weight: bold;">Keck II/NIRSPEC-2</td></tr><tr><td>08:33–08:40</td><td>KL1</td><td>BS-718</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>09:50–10:11</td><td>KL1</td><td>Wirtanen</td><td>10</td><td>1.058</td><td>0.0778</td><td>1.6</td><td>H<sub>2</sub>O, C<sub>2</sub>H<sub>6</sub>, CH<sub>3</sub>OH</td><td>131–110</td></tr><tr><td colspan="9" style="text-align: center; font-weight: bold;">IRTF/iSHELL</td></tr><tr><td>09:42–10:04</td><td>L-Custom</td><td>Wirtanen</td><td>18</td><td>1.058</td><td>0.0778</td><td>1.6</td><td>H<sub>2</sub>O</td><td>101</td></tr><tr><td>10:09–11:53</td><td>L3-Custom</td><td>Wirtanen</td><td>96</td><td>1.058</td><td>0.0778</td><td>1.7</td><td>C<sub>2</sub>H<sub>6</sub>, CH<sub>3</sub>OH, OH<sup>*</sup></td><td>101</td></tr><tr><td>12:13–12:19</td><td>L3-Custom</td><td>BS-2421</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>12:23–12:29</td><td>L-Custom</td><td>BS-2421</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>

**Note.** r<sub>H</sub>, Δ, and dΔ/dt are the heliocentric distance, geocentric distance, and geocentric velocity, respectively, of Wirtanen at the time of observations. T<sub>int</sub> is the integrated time on-source. L-Custom and L3-Custom are custom iSHELL settings spanning 2.81–3.09 µm and 3.12–3.41 µm, respectively.

for common or distinct outgassing sources (e.g., Dello Russo et al. 2016b).

The 2018 close approach to Earth of Jupiter-family comet (JFC) 46P/Wirtanen (hereafter Wirtanen) presented an opportunity to perform ground-based measurements of coma composition and spatial distributions of the various species with exceptional sensitivity and spatial resolution, making it one of the most favorable JFC apparitions of the decade. Taken near Wirtanen's closest approach to Earth, our observations with the iSHELL spectrograph at the NASA-IRTF on Maunakea, HI sampled the volatile composition of the innermost 200 km of the coma (as projected onto the sky plane) with a seeing-limited spatial resolution at a scale of ~9 km pixel<sup>-1</sup> at the geocentric distance of the comet. Coordinated observations of common species with NIRSPEC-2 at the W. M. Keck Observatory were highly complementary, enabling us to measure volatile production and spatial associations in a distinctly different projection of the coma into the plane of the sky from that sampled by iSHELL. Here we report detections and spatial profiles of emissions for the three species targeted by both instruments on December 18: H<sub>2</sub>O (or its proxy, OH<sup>*</sup> prompt emission; Bonev et al. 2006), C<sub>2</sub>H<sub>6</sub>, and CH<sub>3</sub>OH. In Section 2, we discuss our observations and data analysis. In Section 3, we present our results. In Section 4, we discuss our results and compare them to coordinated observations with NIRSPEC-2. In Section 5, we advocate for future studies leveraging the capabilities of iSHELL and NIRSPEC-2 in concert.

## 2. Observations and Data Reduction

Wirtanen is a JFC with a period P = 5.4 yr, and was the original target of the Rosetta (ESA) mission. During its 2018 apparition, Wirtanen reached perihelion (q = 1.05 au) on UT 2018 December 12, and passed closest to the Earth (Δ<sub>min</sub> = 0.0774 au, approximately 30 lunar distances) on UT 2018 December 16. As part of a coordinated observing campaign, on UT 2018 December 18 we targeted Wirtanen with the high-resolution, near-infrared facility spectograph iSHELL (Rayner et al. 2012, 2016) at the 3 m NASA-IRTF to characterize its volatile composition. The observing log is shown in Table 1. We utilized two custom iSHELL settings (referred to as L-Custom and L3-Custom, see Table 1) so as to fully sample a suite of molecular abundances. We oriented the slit along the Sun-comet line. Coordinated observations were

carried out with NIRSPEC-2 (Martin et al. 2016, 2018) at the 10 m W. M. Keck Observatory (Table 1). A detailed analysis of these observations is reported in Bonev et al. (2021).

The iSHELL observations were performed with a 6 pixel (0.′′75) wide slit with resolving power (λ/Δλ) ~ 4.5 × 10<sup>4</sup>. We used a standard ABBA nod pattern in which the telescope is nodded along the slit between successive exposures, thereby placing the comet at two distinct positions along the slit (“A” and “B”) to facilitate sky subtraction. The A and B beams were symmetrically placed about the midpoint along the 15′′ long slit and separated by half its length. Wirtanen was bright and easily acquired with iSHELL’s near-infrared active guiding system. Combining spectra of the nodded beams as A–B–B + A canceled emissions from thermal background, instrumental biases, and sky emission (lines and continuum) to second order in air mass. Flux calibration was performed using an appropriately placed bright infrared flux standard star using a wide (4′′0) slit.

We employed data reduction procedures that have been rigorously tested and are described extensively in the refereed literature (Bonev 2005; DiSanti et al. 2006, 2014; Villanueva et al. 2009; Radeva et al. 2010), including their application to unique aspects of iSHELL spectra (DiSanti et al. 2017; Roth et al. 2020). Each echelle order within an iSHELL setting was processed individually as previously described, such that each row corresponded to a unique position along the slit, and each column to a unique wavelength. Spectra were extracted from the processed frames by summing the signal over 15 rows (approximately 2′′5), seven rows to each side of the nucleus, defined as the peak of dust emission in a given spectral order.

We determined contributions from continuum and gaseous emissions in comet spectra as previously described (e.g., DiSanti et al. 2016, 2017) and illustrate the procedure in Figure 1. We convolved the fully resolved transmittance function to the resolving power of the data (~4.5 × 10<sup>4</sup>) and scaled it to the level of the comet continuum. We then subtracted the modeled continuum to isolate cometary emission lines and compared synthetic models of fluorescent emission for each targeted species to the observed line intensities.

Nucleocentric (or nucleus-centered) production rates (Q<sub>NC</sub>) were determined using a well-documented formalism (Dello Russo et al. 1998; DiSanti et al. 2001; Bonev 2005; Villanueva et al. 2011b); see Section 3.2.2 of DiSanti et al. (2016) for further details. The Q<sub>NC</sub> were multiplied by an appropriate growth factor (GF), determined using the Q-curve
<figure><img src="image_4.png" /><figcaption>**Figure 1.** (A) Extracted iSHELL spectrum showing detections of C₂H₆, CH₃OH, and OH⁺ in Wirtanen on UT 2018 December 18. The gold trace overplotted on the uppermost cometary spectrum is the telluric absorption model (convolved to the instrumental resolution and scaled to the observed continuum level). (B) Residual emission spectrum (after subtracting the telluric absorption model) with individual fluorescence models overlaid (color coded and styled by species) and the 1σ uncertainty envelope shaded in bronze. Arrows indicate positions of OH⁺ lines.</figcaption></figure>

methodology (e.g., Dello Russo et al. 1998; DiSanti et al. 2001; Bonev 2005; Gibb et al. 2012) to establish total (or global) production rates (Q). The Q-curve formalism corrects for atmospheric seeing, which suppresses signal along lines of sight passing close to the nucleus owing to the use of a narrow slit, as well as for potential perpendicular drift of the comet during an exposure sequence. We estimate the uncertainty in Q due to flux calibration to be 3% for the L-Custom setting and

2% for the L3-Custom setting based on the standard deviation of flux calibration factors (Γ, W/m²/cm⁻¹/(counts/s)) within each echelle order taken from eight exposures. We incorporated this additional uncertainty into our production rates. Global production rates for all detected molecules are listed in Table 2. GFs were determined for H₂O, C₂H₆, and CH₃OH.

## 2.1. Mixing Ratios of Volatile Species

### 2.1.1. Molecular Fluorescence Analysis

Synthetic models of fluorescent emission for each targeted species were compared with observed line intensities, after correcting each modeled g-factor (line intensity) for the monochromatic atmospheric transmittance at its Doppler-shifted wavelength (according to the geocentric velocity of the comet at the time of the observations). The g-factors used in synthetic fluorescent emission models in this study were generated with quantum mechanical models developed for H₂O (Villanueva et al. 2012a), C₂H₆ (Villanueva et al. 2011b), and CH₃OH (Villanueva et al. 2012a; DiSanti et al. 2013). A Levenburg-Marquardt nonlinear minimization technique (Villanueva et al. 2008) was used to fit fluorescent emission from all species simultaneously in each echelle order, allowing for high precision results, even in spectrally crowded regions containing many spectral lines within a single instrumental resolution element. Production rates for each sampled species were determined from the appropriate fluorescence model at the rotational temperature of each molecule (Section 2.1.2).

### 2.1.2. Determination of Rotational Temperature

Rotational temperatures ($T_{\text{rot}}$) were determined using correlation and excitation analyses as described in Bonev (2005), Bonev et al. (2008), DiSanti et al. (2006), Villanueva et al. (2008). In general, well-constrained rotational temperatures can be determined for individual species having intrinsically bright lines and for which a sufficiently broad range of excitation energies is sampled. Utilizing the large spectral grasp of iSHELL, these conditions were satisfied for H₂O, C₂H₆, and CH₃OH.

We found consistent and well-constrained rotational temperatures for H₂O and C₂H₆. The $T_{\text{rot}}$ for H₂O (94 ± 5 K) was in formal agreement with that for C₂H₆ (90 ± 3 K). Although the $T_{\text{rot}}$ for CH₃OH (88±¹⁸) was consistent with both of these, it was less well-constrained. This is consistent with previous work demonstrating that rotational temperatures for primary species sampled at near-infrared wavelengths are generally in agreement (see for example Gibb et al. 2012; DiSanti et al. 2016, and references therein).

# 3. Results

We securely detected molecular emission from H₂O, C₂H₆, CH₃OH, and OH⁺ (prompt emission) in the coma of Wirtanen. Figures 1 and 2 show clear detections of multiple transitions of each detected species superimposed on the cometary continuum.

## 3.1. Spatial Profiles

We were able to extract spatial profiles for H₂O (measured directly or through its proxy, OH⁺; see Bonev et al. 2006), C₂H₆, and CH₃OH in Wirtanen (Figure 3). The high brightness and small geocentric distance of Wirtanen enabled us to map
<table><caption>**Table 2**
Molecular Composition of 46P/Wirtanen as Measured by iSHELL</caption><thead><tr><th rowspan="2">Setting</th><th rowspan="2">Species</th><th rowspan="2">T<sub>rot</sub><sup>a</sup><br>(K)</th><th rowspan="2">GF<sup>b</sup></th><th rowspan="2">Q<sup>c</sup><br>(10<sup>25</sup> s<sup>-1</sup>)</th><th colspan="2">Relative Abundance</th></tr><tr><th>Q<sub>x</sub>/Q<sub>H2O</sub><sup>d</sup></th><th>Q<sub>x</sub>/Q<sub>C2H6</sub><sup>e</sup></th></tr></thead><tbody><tr><td colspan="7">UT 2018 December 18, r<sub>H</sub> = 1.07 au, Δ = 0.078 au</td></tr><tr><td>L-Custom</td><td>H<sub>2</sub>O</td><td>94 ± 5</td><td>2.4 ± 0.2</td><td>825 ± 60</td><td>100</td><td>131 ± 14</td></tr><tr><td rowspan="2">L3-Custom</td><td>C<sub>2</sub>H<sub>6</sub></td><td>90 ± 3</td><td>2.05 ± 0.04</td><td>6.3 ± 0.2</td><td>0.75 ± 0.08</td><td>1</td></tr><tr><td>CH<sub>3</sub>OH</td><td>88<sup>+18</sup><sub>-15</sub></td><td>2.3 ± 0.1</td><td>22 ± 2</td><td>2.8 ± 0.3</td><td>3.5 ± 0.2</td></tr></tbody></table>

**Notes.**

<sup>a</sup> Rotational temperature.

<sup>b</sup> Growth factor. This represents the ratio of global Q to Q<sub>NC</sub> based on the central 0''75 × 0''83 aperture having peak emission flux.

<sup>c</sup> Production rate.

<sup>d</sup> Mixing ratio with respect to H<sub>2</sub>O (H<sub>2</sub>O = 100). L3-Custom mixing ratios were calculated using Q(H<sub>2</sub>O) as measured with L-Custom. An additional 10% uncertainty was incorporated into the L3-Custom H<sub>2</sub>O mixing ratios to account for the non-simultaneous observations of H<sub>2</sub>O.

<sup>e</sup> Mixing ratio with respect to C<sub>2</sub>H<sub>6</sub> (C<sub>2</sub>H<sub>6</sub> = 1).

the inner coma (within ~200 km to either side of the nucleus) in exceptional detail. The small phase angle (φ ~ 18°) during our observations must be considered when interpreting spatial profiles, as the anti-sunward hemisphere was nearly along the line-of-sight toward the comet. Nevertheless, Figure 3(A) shows that the spatial profiles for OH* and CH<sub>3</sub>OH were both broader than C<sub>2</sub>H<sub>6</sub>, and all three gases were broader than the dust continuum and enhanced in the projected anti-sunward direction. Similarly, Figure 3(B) shows that the spatial profile for H<sub>2</sub>O was broader than the continuum, and again showed enhancement in the projected anti-sunward direction. The anti-sunward enhancement for H<sub>2</sub>O could be indicative of coma production of H<sub>2</sub>O, in which icy grains are driven by radiation pressure into the anti-sunward tail before releasing their H<sub>2</sub>O ice into the coma (e.g., Kawakita et al. 2013; Knight & Schleicher 2013).

It is important to note that Figures 3(A) and (B) do not correspond to simultaneous measurements. The C<sub>2</sub>H<sub>6</sub> and CH<sub>3</sub>OH measurements are based on almost two hours of clock time (i.e., ~20% of the nucleus rotational period of 9 hr; Farnham et al. 2018; Jehin et al. 2018; Handzlik et al. 2019). The illumination of active regions on the nucleus could have changed significantly during this time compared with the source region for H<sub>2</sub>O. Bearing this in mind, the broader H<sub>2</sub>O distribution (Figure 3(A)) when compared with co-measured C<sub>2</sub>H<sub>6</sub> is highly consistent with higher signal-to-noise measurements (especially for H<sub>2</sub>O) from NIRSPEC-2 (Bonev et al. 2021), and independently suggest an additional source of H<sub>2</sub>O, perhaps from icy grains.

## 3.2. Comparison with Other iSHELL Observations During the 2018–2019 Perihelion Passage

The observations reported here represent one component of a multi-date iSHELL observing campaign toward Wirtanen during its 2018–2019 perihelion passage (Dello Russo et al. 2019). Saki et al. (2020) reported H<sub>2</sub>O production rates and a stringent upper limit on OCS (carbonyl sulfide) on UT 2018 December 14 and 19, and Khan et al. (2021) reported detections of C<sub>2</sub>H<sub>6</sub>, CH<sub>3</sub>OH, C<sub>2</sub>H<sub>2</sub>, and NH<sub>3</sub> and examined potential short-term variability in H<sub>2</sub>O and HCN production, with emphasis on UT December 21. McKay et al. (2021) reported detections of H<sub>2</sub>O, C<sub>2</sub>H<sub>6</sub>, and CH<sub>3</sub>OH, as well as upper limits on CO and CH<sub>4</sub>, on UT 2019 January 11–13. Our H<sub>2</sub>O production rate, (8.25 ± 0.60) × 10<sup>27</sup> s<sup>-1</sup>, is considerably

higher than that reported by Saki et al. (2020) and Khan et al. (2021) (both papers report ~6 × 10<sup>27</sup> s<sup>-1</sup>). This suggests that H<sub>2</sub>O production in Wirtanen may have been variable on timescales of days. Combi et al. (2020) found Q(H<sub>2</sub>O) ~1.6 × 10<sup>28</sup> s<sup>-1</sup> on UT 2018 December 22 based on SOHO/SWAN observations of Lyα, although these measurements span a considerably larger portion of the coma than those from iSHELL and may sample more of the extended H<sub>2</sub>O emission from icy grain production.

In terms of the trace species C<sub>2</sub>H<sub>6</sub> and CH<sub>3</sub>OH, our C<sub>2</sub>H<sub>6</sub> mixing ratio is in agreement with that from Khan et al. (2021) (0.71 ± 0.09% relative to H<sub>2</sub>O), yet our CH<sub>3</sub>OH mixing ratio is lower than the Khan et al. value (4.26 ± 0.34%). In contrast, our CH<sub>3</sub>OH mixing ratio is in formal agreement with those reported by McKay et al. (2021) (~3%), while our C<sub>2</sub>H<sub>6</sub> mixing ratio is marginally lower than their value of 1%. Collectively, these results emphasize the complex nature of Wirtanen's volatile outgassing throughout the 2018–2019 perihelion passage. Figure 4 shows the evolution of Q(H<sub>2</sub>O) as well as mixing ratios of C<sub>2</sub>H<sub>6</sub> and CH<sub>3</sub>OH as measured by iSHELL and NIRSPEC-2 (Section 4; Bonev et al. 2021). Future work will comprehensively address potential variability in H<sub>2</sub>O production and trace species mixing ratios in Wirtanen as measured with iSHELL.

## 3.3. Comparison with Comets Measured at Near-infrared Wavelengths

Our results indicate that Wirtanen was enriched in both C<sub>2</sub>H<sub>6</sub> and CH<sub>3</sub>OH compared with their respective mean abundances in JFCs characterized to date at near-IR wavelengths (Dello Russo et al. 2016a). Figure 5 reinforces that the abundances of these two molecules in Wirtanen were more similar to those measured in OCCs. Of JFCs characterized to date, perhaps the most similar to our results is 45P/Honda–Mrkos–Pajdušáková (points #12 and 13 in Figure 5), which displayed similarly enriched C<sub>2</sub>H<sub>6</sub> and CH<sub>3</sub>OH (DiSanti et al. 2017; Dello Russo et al. 2020). It is also interesting to compare with the hyperactive comet 103P/Hartley 2 (point #10), which had a similarly high C<sub>2</sub>H<sub>6</sub> mixing ratio, yet considerably lower CH<sub>3</sub>OH. In making these comparisons, it is important to note that although C<sub>2</sub>H<sub>6</sub>, CH<sub>3</sub>OH, and H<sub>2</sub>O were measured very close in time in Wirtanen, this was not necessarily the case for other comets. For a comparison of additional molecules sampled in Wirtanen at near-infrared wavelengths (e.g., HCN,
<figure><img src="image_5.png" /><figcaption>**Figure 2.** (A)–(B) Extracted iSHELL spectra showing detections of H₂O in Wirtanen on UT 2018 December 18, with traces and labels as described in Figure 1.</figcaption></figure>

C₂H₂, CO) during the 2018–2019 perihelion passage in the context of the comet population, see Khan et al. (2021), McKay et al. (2021), and Bonev et al. (2021).

# 4. Coordinated Observations with iSHELL and NIRSPEC-2

Wirtanen’s long on-sky availability from the summit of Maunakea, HI, near the closest approach to Earth enabled us to leverage the capabilities of the two premier near-infrared facilities in the northern hemisphere: iSHELL at the NASA-IRTF and the newly upgraded NIRSPEC-2 at the W. M. Keck Observatory. This allowed a direct comparison of our iSHELL

results with measurements from a 10 m telescope and a somewhat longer (24′′) slit, invaluable for spatial-spectral studies of the innermost coma. We coordinated these observations to sample distinct projections of the coma into the plane of the sky, and chose instrument settings so as to target emissions from the same coma volatiles.

Table 1 shows that our L-Custom iSHELL observations sampling H₂O were taken nearly simultaneously with NIR-SPEC-2, whereas our L3-Custom observations sampling C₂H₆ and CH₃OH were taken after the conclusion of the NIRSPEC-2 observations. This short temporal spread reduces the effects of potential short-term variability on the measurements between the two instruments. We discuss the results of measurements from both instruments and advocate for their joint application to future cometary observations.

## 4.1. Molecular Composition of the Coma

Table 3 shows a comparison of the rotational temperatures, production rates, and mixing ratios for each molecule in Wirtanen as derived from iSHELL and NIRSPEC-2 observations. As described in Bonev et al. (2021 and references therein), we utilized C₂H₆ as an alternative compositional baseline when measuring mixing ratios.

The T<sub>rot</sub> measured for H₂O and C₂H₆ are in formal agreement, and the measured iSHELL CH₃OH T<sub>rot</sub> is consistent with all of these within 1σ uncertainty (the NIRSPEC-2 CH₃OH T<sub>rot</sub> was assumed). The production rates and mixing ratios for C₂H₆ agree within 1σ uncertainty for both instruments, and the H₂O and CH₃OH production rates agree within 2σ. Taking into account the different projections of the coma sampled by each measurement, these measurements suggest compositional uniformity of the coma within several hundred km of the nucleus.

## 4.2. Potential Extended Sources in Wirtanen.

Wirtanen is considered a hyperactive comet (e.g., Lis et al. 2019 and references therein), with its unusually high Q(H₂O) for its small size (~1 km) attributed to significant release of H₂O from icy grains in its coma. One of the more well-known hyperactive comets is 103P/Hartley 2, visited by the EPOXI spacecraft, in which both direct nucleus release and icy grain production of H₂O were unambiguously observed (A’Hearn et al. 2011). The long-slit iSHELL and NIRSPEC-2 measurements enabled us to search for these putative icy grain contributions to Wirtanen’s coma through analysis of spatial profiles for each volatile. As detailed in Bonev et al. (2021), the NIRSPEC-2 measurements indicate a significant icy grain contribution to H₂O production in Wirtanen (up to 40%), and potentially an icy grain contribution to CH₃OH production as well.

Similar to the compositional results, our iSHELL measurements of spatial associations in Wirtanen are in excellent agreement with those obtained with NIRSPEC-2. We oriented the iSHELL slit along the Sun-comet line (PA 101°) to sample material released into projected sunward- and anti-sunward-facing hemispheres. This provided the most direct measure of the projected sunward versus anti-sunward outflow, although the small solar phase angle (18°) meant that the true Sun-comet direction was oriented nearly along the line-of-sight. The simultaneous/contemporaneous spectra with NIRSPEC-2 were taken in rotator stationary mode, meaning the slit PA changed
<figure><img src="image_6.png" /><figcaption>**Figure 3.** (A) Spatial profiles of emissions for co-measured C₂H₆ (black, solid), CH₃OH (blue, dashed), OH* (pink, dotted), dust continuum (red, dashed-dotted), and the stellar PSF (green, dashed-dotted-dotted) in Wirtanen on UT 2018 December 18 measured with iSHELL. Color-coded 1σ uncertainties are shown for the profile of each species. The slit was oriented along the projected Sun-comet line (position angle 101°), with the Sun-facing direction to the left as indicated. Also shown is the Sun-comet-Earth angle (phase angle, β) of 18°. (B) Spatial profiles of emissions for H₂O (black, solid), dust continuum (red, dashed-dotted), and the stellar PSF (green, dashed-dotted-dotted) in Wirtanen on UT 2018 December 18 measured with iSHELL.</figcaption></figure>

continuously yet remained close to the projected Sun-comet direction over the course of those observations (for details see Bonev et al. 2021). For comparison with our December 18 observations, iSHELL measurements on December 21 reported in Khan et al. (2021) provided spatial information along the slit at two independent orientations (along the Sun-comet PA, and orthogonal to this direction).

In comparing our results on December 18 with iSHELL and NIRSPEC-2, it is important to consider differences in their fields of view. Our iSHELL observations used a 0.75 wide by 15" long slit, with a spatial scale of approximately 0.167 pixel⁻¹. The NIRSPEC-2 observations used a 0.43 wide by 24" long slit, with a scale of 0.129 pixel⁻¹. As detailed in Section 2, we extracted spatial profiles—maps of emission intensity along the slit—and used these to establish a GF through the *Q*-curve methodology, which relates nucleocentric production rate (*Q*<sub>NC</sub>) to global production rate (*Q*). Given the apparent hyperactivity of Wirtanen, coupled with its small Δ during our observations, it is important to address whether the 15" long iSHELL slit captured as large a contribution from icy grains to H₂O production as did the 24" long NIRSPEC-2 slit.

To address this issue, we carefully examined the spatial profiles for H₂O as measured by iSHELL and NIRSPEC-2, as well as the *Q*-curve calculation used in determining GF for measurements with each instrument. Figure 6 shows the spatial profiles for H₂O, C₂H₆, and CH₃OH extracted from each instrument overlain on one another for comparison, and Figure 7 shows a comparison of spatial profiles for H₂O emission as measured with iSHELL and NIRSPEC-2 along with their corresponding *Q*-curves. Figure 6(A) shows that the H₂O profiles from each instrument are both clearly extended in

the projected anti-sunward direction, indicative of the icy grains in Wirtanen's coma. Importantly, the iSHELL H₂O spatial profile is at least as extended as (if not more so than) that from NIRSPEC-2. This is not surprising, as the iSHELL measurements taken along the Sun-comet line would be expected to provide the most direct picture of the projected sunward/anti-sunward hemispheres. Comparing the spatial extent of the iSHELL and NIRSPEC-2 profiles, Figure 6(A) suggests that iSHELL captured the vast majority of the icy grain contribution to H₂O production that was sampled by NIRSPEC-2, and that the differences in slit lengths between the two instruments did not significantly affect *Q*(H₂O) as measured by each.

We now detail the *Q*-curve calculation for each instrument. This *Q*-curve methodology averages the emission intensity on either side of and equidistant from the nucleus. Averages were stepped in successive intervals along the slit (0.38 for NIRSPEC-2; 0.83 for iSHELL), resulting in a “symmetric” *Q*-curve. These symmetric *Q*-values increase with nucleocentric distance owing primarily to atmospheric seeing, until reaching a terminal value—the global production rate, *Q*. The GF is calculated as the ratio of the weighted mean of the terminal pixel *Q*-values (slit-width pixels 4–8 for NIRSPEC; slit-width pixels 1–3 for iSHELL) to the nucleocentric *Q*-value. Figures 7(A) and (B) demonstrate this *Q*-curve methodology graphically for iSHELL and NIRSPEC-2, respectively.

Examination of the *Q*-curves with the spatial scales for both instruments overlain demonstrates that the spatial profiles (and associated *Q*-curves) are quite consistent, and that the same range of nucleocentric distances can be used to derive the GF's for both instruments; however, it is important to remember that
<figure><img src="image_7.png" /><figcaption>**Figure 4.** Top: water production rates in Wirtanen measured with iSHELL on December 14 and 19 (Saki et al. 2020), December 18 (this work), December 21 (Khan et al. 2021), and January 11–13 (McKay et al. 2021), and with NIRSPEC-2 on December 17–18 (Bonev et al. 2021). Bottom: relative abundances (% relative to H₂O) for C₂H₆ and CH₃OH, with references for each date as cited above.</figcaption></figure>

each instrument was sampling a different projection of the coma into the sky plane because of the differing slit PA values. It is important to note the higher angular resolution and longer slit (and thus, the larger number of *Q*-values) afforded by NIRSPEC-2. The NIRSPEC-2 *Q*-curve shows that a terminal value had been reached (i.e., a nucleocentric distance at which the signal is no longer dominated by atmospheric seeing) by the third successive *Q*-value (NIRSPEC-2 slit-width pixel #3). The iSHELL *Q*-curve shows that a terminal value had been reached by the first successive *Q*-value (iSHELL slit-width pixel #1) because of the lower angular resolution and shorter slit, and that this first pixel would have included the still-rising *Q*-values indicated at the first and second NIRSPEC-2 slit-width pixels. The inclusion of these coma regions that were still being suppressed by atmospheric seeing into the first terminal iSHELL *Q*-value (and therefore the iSHELL GF) could have lowered its value. Nevertheless, the agreement between the *Q*(H₂O) and spatial profiles as measured by each instrument is excellent, and differences in field of view between the two instruments did not significantly affect the results.

## 5. Applications to Future Cometary Observations

In total, iSHELL observations of Wirtanen were taken on multiple dates spanning 2018 December–2019 February, including six dates near closest approach to Earth. A

comprehensive analysis of the full suite of iSHELL observations is the subject of a future study. Analysis of iSHELL observations on December 21 are reported in Khan et al. (2021), with observations characterizing the hypervolatiles CO, CH₄, and C₂H₆ in January reported by McKay et al. (2021). The coordinated iSHELL and NIRSPEC-2 observations on December 18 and their consistency point toward their application to these broader iSHELL observations of Wirtanen, and in turn to future cometary studies leveraging the capabilities of both instruments, as we now discuss.

### 5.1. The Unique Strengths of NIRSPEC-2

NIRSPEC-2 occupies a unique niche in cometary composition studies. With its cross-dispersed capability, it can sample nearly the entire parent volatile chemistry in a single setting, enabling simultaneous measures of mixing ratios relative to H₂O as well as to C₂H₆. It offers the longest slit available at near-infrared wavelengths. This affords the most sensitive test of coma spatial associations possible, and the sensitivity of the Keck II 10 m primary provides time-resolved measures of targeted species with relatively short on-source integration times. With its high sensitivity, it is well-suited for measuring challenging weaker species such as C₂H₄ and HC₃N, as well as deuterated species (e.g., H₂O and HDO, CH₄ and CH₃D, C₂H₆ and C₂H₅D). It also provides high signal-to-noise, spatially
<figure><img src="image_8.png" /><figcaption>**Figure 5.** Mixing ratios of CH₃OH and C₂H₆ relative to H₂O in comets characterized to date at near-infrared wavelengths (Dello Russo et al. 2016a; DiSanti et al. 2017; Faggi et al. 2018, 2019; Roth et al. 2018; Dello Russo et al. 2020). Comets are numbered and color coded, with triangles for JFCs and X's for OCCs.</figcaption></figure>

<table><caption>**Table 3**
Comparison of iSHELL and NIRSPEC-2 Results</caption><thead><tr><th rowspan="3">Species</th><th colspan="2">T<sub>rot</sub><sup>a</sup> (K)</th><th colspan="2">Q<sup>b</sup> (10<sup>25</sup> s<sup>-1</sup>)</th><th colspan="4">Relative Abundance</th></tr><tr><th rowspan="2">iSHELL</th><th rowspan="2">NIRSPEC</th><th rowspan="2">iSHELL</th><th rowspan="2">NIRSPEC</th><th colspan="2">iSHELL</th><th colspan="2">NIRSPEC</th></tr><tr><th>Q<sub>x</sub>/Q<sub>H2O</sub><sup>c</sup></th><th>Q<sub>x</sub>/Q<sub>C2H6</sub><sup>d</sup></th><th>Q<sub>x</sub>/Q<sub>H2O</sub><sup>c</sup></th><th>Q<sub>x</sub>/Q<sub>C2H6</sub><sup>d</sup></th></tr></thead><tbody><tr><td>H<sub>2</sub>O</td><td>94 ± 5</td><td>87 ± 1</td><td>825 ± 60</td><td>903 ± 30</td><td>100</td><td>131 ± 14</td><td>100</td><td>151 ± 7</td></tr><tr><td>C<sub>2</sub>H<sub>6</sub></td><td>90 ± 3</td><td>84<sup>+5</sup><sub>-4</sub></td><td>6.3 ± 0.2</td><td>5.98 ± 0.19</td><td>0.75 ± 0.08</td><td>1</td><td>0.66 ± 0.03</td><td>1</td></tr><tr><td>CH<sub>3</sub>OH</td><td>88<sup>+18</sup><sub>-15</sub></td><td>(87)</td><td>22 ± 2</td><td>27.32 ± 1.91</td><td>2.8 ± 0.3</td><td>3.5 ± 0.2</td><td>3.03 ± 0.23</td><td>4.57 ± 0.35</td></tr></tbody></table>

**Notes.**

<sup>a</sup> Rotational temperature. Values in parentheses are assumed.

<sup>b</sup> Production rate.

<sup>c</sup> Mixing ratio with respect to H<sub>2</sub>O (H<sub>2</sub>O = 100).

<sup>d</sup> Mixing ratio with respect to C<sub>2</sub>H<sub>6</sub> (C<sub>2</sub>H<sub>6</sub> = 1). NIRSPEC-2 measurements taken from (Bonev et al. 2021).

resolved measures of emission intensities along the slit. Therefore, NIRSPEC-2 can provide the most sensitive temporally and spatially resolved measurements of coma volatile composition.

## 5.2. The Unique Strengths of iSHELL

Since its commissioning in 2016, iSHELL has quickly become an indispensable instrument for studies of parent volatiles in comets. With its daytime observing capability

(unique among ground-based IR facilities) and its high fraction of observing time dedicated to planetary science, the IRTF permits conducting cometary science on timescales ranging from days to months, as demonstrated by serial campaigns on comet Wirtanen (Dello Russo et al. 2019), aspects of which are included in companion papers (Khan et al. 2021; McKay et al. 2021). Its capabilities at M-band are unmatched, enabling high observing efficiency while sampling multiple strong transitions of CO, H₂O, and OCS. Recently published iSHELL studies have significantly increased the number of comets for which
<figure><img src="image_9.png" /><figcaption>**Figure 6.** (A) Spatial profiles of emissions for H₂O in Wirtanen on UT 2018 December 18 as measured by iSHELL (red, dashed), NIRSPEC-2 (black, solid) and continuum (blue, dashed-dotted). Color-coded 1σ uncertainties are shown for the profile of each species. The iSHELL slit was oriented along the projected Sun-comet line (position angle 101°), with the Sun-facing direction to the left. The NIRSPEC-2 observations were conducted in rotator stationary mode, with the slit PA decreasing from 131° to 110° over the course of the night. (B) Spatial profiles of emissions for C₂H₆ in Wirtanen as measured by iSHELL (red, dashed), NIRSPEC-2 (black, solid), and continuum (blue, dashed-dotted). C. Spatial profiles of emissions for CH₃OH in Wirtanen as measured by iSHELL (red, dashed), NIRSPEC-2 (black, solid), and continuum (blue, dashed-dotted). NIRSPEC-2 profiles taken from Bonev et al. (2021).</figcaption></figure>

OCS has been securely measured (Saki et al. 2020), a highly underrepresented species owing to the smaller spectral grasp and/or lower sensitivity of previously available instruments. Its near-infrared guiding capabilities enable active guiding independent of the wavelength of the spectrograph setting, including for challenging daytime targets (e.g., 2P/Encke; Roth et al. 2018).

Furthermore, prior to the commissioning of iSHELL, near-infrared cometary studies at the IRTF were typically limited to a few measurements of a given comet taken over a limited

range of heliocentric distances, and often on a limited number of dates. Such measurements frequently suffered from a “snapshot” bias, and so could not test for many of the variable behaviors reported in comets. However, understanding these phenomena and their occurrence across the broader comet population is crucial to placing the results of cometary compositional studies in the context of solar system formation. iSHELL has ameliorated such “snapshot” biases. It is routinely used to sample coma composition on multiple dates and at a variety of heliocentric distances
<figure><img src="image_10.png" /><figcaption>**Figure 7.** (A) Left: spatial profile of emissions for H₂O and dust continuum in Wirtanen as measured by iSHELL, with sunward and anti-sunward hemispheres labeled. Right: *Q*-curve for H₂O with iSHELL, with the NIRSPEC-2 spatial scale overlain for comparison. (B) Left: spatial profile of emissions for H₂O and dust continuum in Wirtanen as measured by NIRSPEC-2. Right. *Q*-curve for H₂O with NIRSPEC-2.</figcaption></figure>

(e.g., DiSanti et al. 2017; Roth et al. 2018), including pre-and post-perihelion (e.g., Faggi et al. 2019; Roth et al. 2020). These iSHELL studies can reveal how coma abundances and spatial associations vary (or remain consistent) “seasonally” across a perihelion passage.

### 5.3. Synergy between iSHELL and NIRSPEC-2 for Cometary Science

Clearly, iSHELL and NIRSPEC-2 are highly complementary for studies of parent volatiles in comets, with each instrument offering unique strengths and powerful capabilities. When
conducted simultaneously, observations with iSHELL and NIRSPEC-2 can bridge these realms of specialized measurements over various timescales, and Wirtanen provided an excellent opportunity for demonstrating such synergies. With NIRSPEC-2 now fully commissioned, this work demonstrates that even more complex measurements of future comets utilizing the two facilities in a coordinated fashion will be possible. These include programs simultaneously placing the iSHELL and NIRSPEC-2 slits at mutually orthogonal orientations on the sky, thereby enabling comprehensive spatial-spectral studies (e.g., Bonev et al. 2013). In a similar fashion, complementary instrument settings could be chosen so as to sample different (yet partially overlapping) species with each facility/instrument. For example, NIRSPEC-2 may be used to target L-band molecules ($H_2O, H_2CO, C_2H_6, CH_4, HCN, NH_3, C_2H_2$) in a single instrument setting, while iSHELL simultaneously samples M-band molecules ($H_2O, CO, OCS$); together, these observations sample essentially the entire parent volatile inventory at once, which is only possible with these two instruments working in concert. Clearly, the possibilities for paradigm-challenging science from coordinated observations such as those described here abound.

It must be recognized that despite these synergies, each instrument plays a role in comprehensive parent volatile studies that cannot be replicated by the other. Atop the 10 m Keck II primary, NIRSPEC-2 detected $H_2O, C_2H_6$, and $CH_3OH$ with high signal-to-noise far along the slit in only ten minutes on-source on December 18, and additionally detected HCN, $C_2H_2$, and $NH_3$ with only 19 minutes on-source during the previous night (Bonev et al. 2021). iSHELL cannot perform these narrow time-domain measurements on any but the brightest comets and the species with the strongest transitions—securely detecting $NH_3$ and $C_2H_2$ in Wirtanen with iSHELL required hours of on-source integration time (Khan et al. 2021). In terms of strong species in a bright comet, for a comet similar to Wirtanen ($r_H = 1$ au, $\Delta = 0.1$ au, $Q(H_2O)=10^{28} s^{-1}$), $C_2H_6$ and $CH_3OH$ could be detected ($5\sigma$ in a single line) down to (depleted) abundances of 0.03% and 0.3%, respectively, in one hour on-source integration with iSHELL. On the other hand, the high fraction of dedicated planetary science time on iSHELL that enables studies of coma volatile composition and spatial distributions on long timescales (days, months, seasonally) is simply not available with NIRSPEC-2.

Furthermore, we emphasize that it is as remarkable that we found the observed consistency between the iSHELL and NIRSPEC-2 production rates as it would have been had we found significant differences. In the context of the variable nature of comets (with an ever increasing number of examples in the literature, well beyond those cited here), the only production rates for which we should truly expect agreement are those taken truly simultaneously—in this case, $H_2O$. In future comets, coordinated iSHELL and NIRSPEC-2 measurements may well reveal short-term variability in production for molecules observed in cadence, as was the case for $C_2H_6$ and $CH_3OH$ in this study.

## 6. Conclusion

The 2018 perihelion passage of Wirtanen presented an extraordinary opportunity to characterize the relative abundances, spatial associations, and production mechanisms of its volatiles with resolution rarely available to ground-based measurements. Coordinated observations of Wirtanen with

the iSHELL and NIRSPEC-2 spectrographs revealed a coma with asymmetries along the projected Sun-comet vector. These iSHELL measurements detected emission from $H_2O, C_2H_6$, and $CH_3OH$ in the inner coma of Wirtanen. Spatial profiles extracted for these molecules revealed that $H_2O$ emission was extended in the projected anti-sunward hemisphere, perhaps due to sublimation from icy grains in the coma, whereas $C_2H_6$ emission was narrower. These results were highly consistent with those from coordinated NIRSPEC-2 observations (Bonev et al. 2021), with excellent agreement among measured rotational temperatures, molecular production rates, and spatial profiles between the two instruments. This campaign emphasized the highly complementary nature of simultaneous (or contemporaneous) observations of comets with these two facilities, and highlighted the outstanding opportunities that will be afforded by future cometary studies leveraging these instruments.

Data for this study were obtained at the NASA Infrared Telescope Facility (IRTF), operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration, as well as from the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. We are most fortunate to have the opportunity to conduct observations from Maunakea, and recognize the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous community. N.X.R. acknowledges support by the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Universities Space Research Association under contract with NASA, and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program (grant NNX16AP49H). A.J.M. acknowledges support from the NASA Solar System Observations and Solar System Workings Programs. BPB acknowledges support from the NSF Astronomy and Astrophysics grants 1616306 and 200939 and from the NASA Solar System Workings Programs (NNX17AC86G). B.P.B., N.D.R., and R.J.V. acknowledge support from the NASA Solar System Observations program through grant 80NSSC17K0705, and M.A.D. and A.J.M. acknowledge support through grant 18-SSO18_2-0040. E.J. is a F.R.S-FNRS Belgian Senior Research Associate.

## ORCID iDs

Nathan X. Roth https://orcid.org/0000-0002-6006-9574
Boncho P. Bonev https://orcid.org/0000-0002-6391-4817
Michael A. DiSanti https://orcid.org/0000-0001-8843-7511
Neil Dello Russo https://orcid.org/0000-0002-8379-7304
Adam J. McKay https://orcid.org/0000-0002-0622-2400
Erika L. Gibb https://orcid.org/0000-0003-0142-5265
Mohammad Saki https://orcid.org/0000-0003-2277-6232
Younas Khan https://orcid.org/0000-0003-4773-2674
Ronald J. Vervack, Jr. https://orcid.org/0000-0002-8227-9564
Hideyo Kawakita https://orcid.org/0000-0003-2011-9159
Anita L. Cochran https://orcid.org/0000-0003-4828-7787
Nicolas Biver https://orcid.org/0000-0003-2414-5370
Martin A. Cordiner https://orcid.org/0000-0001-8233-2436
Emmanuël Jehin https://orcid.org/0000-0001-8923-488X
Harold Weaver https://orcid.org/0000-0003-0951-7762
References

A'Hearn, M. F., Belton, M. J. S., Delamere, W. A., et al. 2011, *Sci*, **332**, 1396

Bockelée-Morvan, D., & Biver, N. 2017, *PTRSA*, **375**, 20160252

Bockelée-Morvan, D., Crovisier, J., Mumma, M. J., & Weaver, H. A. 2004, in
Comets II, ed. H. U. Keller & H. A. Weaver (Tucson, AZ: Univ. Arizona
Press), 391

Bonev, B. P. 2005, PhD thesis, Univ. Toledo

Bonev, B. P., Dello Russo, N., DiSanti, M. A., et al. 2021, PSJ, **2**, 45

Bonev, B. P., Mumma, M. J., DiSanti, M. A., et al. 2006, AJ, **653**, 774

Bonev, B. P., Mumma, M. J., Radeva, Y. L., et al. 2008, ApJL, **680**, L61

Bonev, B. P., Villanueva, G. L., Paganini, L., et al. 2013, *Icar*, **222**, 740

Combi, M. R., Mäkinen, T. T., Bertaux, J. L., et al. 2020, PSJ, **1**, 72

Dello Russo, N., DiSanti, M. A., Mumma, M. J., Magee-Sauer, K., & Rettig, T. W. 1998, *Icar*, **135**, 377

Dello Russo, N., Kawakita, H., Bonev, B. P., et al. 2020, *Icar*, **355**, 113411

Dello Russo, N., Kawakita, H., Vervack, R. J., Jr., & Weaver, H. A. 2016a,
*Icar*, **278**, 301

Dello Russo, N., McKay, A. J., Saki, M., et al. 2019, EPSC-DPS Joint Meeting
2019, **13**, 742

Dello Russo, N., Vervack, R. J. J., Kawakita, H., et al. 2016b, *Icar*, **266**, 152

DiSanti, M. A., Bonev, B. P., Dello Russo, N., et al. 2017, *AJ*, **154**, 246

DiSanti, M. A., Bonev, B. P., Gibb, E. L., et al. 2016, ApJ, **820**, 20

DiSanti, M. A., Bonev, B. P., Magee-Sauer, K., et al. 2006, ApJ, **650**, 470

DiSanti, M. A., Bonev, B. P., Villanueva, G. L., & Mumma, M. J. 2013, ApJ,
763, 19

DiSanti, M. A., Mumma, M. J., Dello Russo, N., & Magee-Sauer, K. 2001,
*Icar*, **153**, 361

DiSanti, M. A., Villanueva, G. L., Paganini, L., et al. 2014, *Icar*, **228**, 167

Faggi, S., Mumma, M. J., Villanueva, G. L., Paganini, L., & Lippi, M. 2019,
AJ, **158**, 254

Faggi, S., Villanueva, G. L., Mumma, M. J., & Paganini, L. 2018, *AJ*, **156**, 68

Farnham, T. L., Knight, M. M., & Schleicher, D. G. 2018, CBET, **4571**, 1

Gibb, E. L., Bonev, B. P., Villanueva, G., et al. 2012, ApJ, **750**, 102

Handzlik, B., Drahus, M., & Kurowski, S. 2019, EPSC-DPS Joint Meeting
2019, **13**, 1775

Jehin, E., Moulane, Y., Manfroid, J., & Pozuelos, F. 2018, CBET, 4585, 1

Kawakita, H., Kobayashi, H., Dello Russo, N., et al. 2013, *Icar*, **222**, 723

Khan, Y., Gibb, E. L., Bonev, B. P., et al. 2021, PSJ, **2**, 20

Knight, M. M., & Schleicher, D. G. 2013, *Icar*, **222**, 691

Lis, D. C., Bockelée-Morvan, D., Güsten, R., et al. 2019, A&A, **625**, L5

Martin, E. C., Fitzgerald, M. P., McLean, I. S., et al. 2018, Proc. SPIE, **10702**,
**107020A**

Martin, E. C., Fitzgerald, M. P., McLean, I. S., Kress, E., & Wang, E. 2016,
Proc. SPIE, **9908**, 99082R

McKay, A. J., DiSanti, M. A., Cochran, A. L., et al. 2021, PSJ, **2**, 21

Mumma, M. J., & Charnley, S. B. 2011, ARA&A, **49**, 471

Radeva, Y. L., Mumma, M. J., Bonev, B. P., et al. 2010, *Icar*, **206**, 764

Rayner, J., Bond, T., Bonnet, M., et al. 2012, Proc. SPIE, **8446**, 84462C

Rayner, J., Tokunaga, A., Jaffe, D., et al. 2016, Proc. SPIE, **9908**, 990884

Roth, N. X., Gibb, E. L., Bonev, B. P., et al. 2018, *AJ*, **156**, 251

Roth, N. X., Gibb, E. L., Bonev, B. P., et al. 2020, *AJ*, **159**, 42

Saki, M., Gibb, E. L., B., P. B., et al. 2020, *AJ*, **160**, 184

Villanueva, G. L., DiSanti, M. A., Mumma, M. J., & Xu, L.-H. 2012a, ApJ,
747, 3

Villanueva, G. L., Mumma, M. J., Bonev, B. P., et al. 2009, ApJL, **690**, L5

Villanueva, G. L., Mumma, M. J., Bonev, B. P., et al. 2012a, JQSRT, **113**, 202

Villanueva, G. L., Mumma, M. J., DiSanti, M. A., et al. 2011b, *Icar*, **216**, 227

Villanueva, G. L., Mumma, M. J., & Magee-Sauer, K. 2011b, JGR, **116**,
E08012

Villanueva, G. L., Mumma, M. J., Novak, R. E., & Hewagama, T. 2008, *Icar*,
**195**, 34