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

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 (Δmin ∼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 CH3OH, C2H6, and H2O. 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.


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 nearinfrared 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 2 H 6 ), methanol (CH 3 OH), hydrogen cyanide (HCN), ammonia (NH 3 )) relative to water (H 2 O), the dominant volatile in the comae of most measured comets, and reveal how volatiles (ices) are associated or segregated in the nucleus by searching 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 −1 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 2 O (or its proxy, OH * prompt emission; Bonev et al. 2006), C 2 H 6 , and CH 3 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.

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 min = 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(Rayner et al. , 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(Martin et al. , 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 4 . 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. 2006DiSanti et al. , 2014Villanueva 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. 2016DiSanti et al. , 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 4 ) 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 NC ) were determined using a well-documented formalism (Dello Russo et al. 1998;DiSanti et al. 2001;Bonev 2005;); see Section 3.2.2 of DiSanti et al. (2016) for further details. The Q NC were multiplied by an appropriate growth factor (GF), determined using the Q-curve Note. r H , Δ, and dΔ/dt are the heliocentric distance, geocentric distance, and geocentric velocity, respectively, of Wirtanen at the time of observations. T int 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.
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/m 2 /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 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 Dopplershifted 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 H 2 O , C 2 H 6 (Villanueva et al. 2011b), and CH 3 OH 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).

Determination of Rotational Temperature
Rotational temperatures (T rot ) were determined using correlation and excitation analyses as described in Bonev (2005), Bonev et al. (2008, 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 H 2 O, C 2 H 6 , and CH 3 OH.
We found consistent and well-constrained rotational temperatures for H 2 O and C 2 H 6 . The T rot for H 2 O (94 ± 5 K) was in formal agreement with that for C 2 H 6 (90 ± 3 K). Although the T rot for CH 3 OH (88 -+ 15 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).

Results
We securely detected molecular emission from H 2 O, C 2 H 6 , CH 3 OH, 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.

Spatial Profiles
We were able to extract spatial profiles for H 2 O (measured directly or through its proxy, OH * ; see Bonev et al. 2006), C 2 H 6 , and CH 3 OH in Wirtanen ( Figure 3). The high brightness and small geocentric distance of Wirtanen enabled us to map the inner coma (within ∼200 km to either side of the nucleus) in exceptional detail. The small phase angle (f ∼ 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 3 OH were both broader than C 2 H 6 , 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 2 O was broader than the continuum, and again showed enhancement in the projected anti-sunward direction. The antisunward enhancement for H 2 O could be indicative of coma production of H 2 O, in which icy grains are driven by radiation pressure into the anti-sunward tail before releasing their H 2 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 2 H 6 and CH 3 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 2 O. Bearing this in mind, the broader H 2 O distribution (Figure 3(A)) when compared with co-measured C 2 H 6 is highly consistent with higher signal-to-noise measurements (especially for H 2 O) from NIRSPEC-2 , and independently suggest an additional source of H 2 O, perhaps from icy grains.

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 2 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 2 H 6 , CH 3 OH, C 2 H 2 , and NH 3 and examined potential short-term variability in H 2 O and HCN production , with emphasis on UT December 21. McKay et al. (2021) reported detections of H 2 O, C 2 H 6 , and CH 3 OH, as well as upper limits on CO and CH 4 , on UT 2019 January 11-13. Our H 2 O production rate, (8.25 ± 0.60) × 10 27 s −1 , is considerably higher than that reported by Saki et al. (2020) and Khan et al. (2021) (both papers report ∼ 6 × 10 27 s −1 ). This suggests that H 2 O production in Wirtanen may have been variable on timescales of days. Combi et al. (2020) found Q(H 2 O) ∼1.6 × 10 28 s −1 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 2 O emission from icy grain production.
In terms of the trace species C 2 H 6 and CH 3 OH, our C 2 H 6 mixing ratio is in agreement with that from Khan et al. (2021) (0.71 ± 0.09% relative to H 2 O), yet our CH 3 OH mixing ratio is lower than the Khan et al. value (4.26 ± 0.34%). In contrast, our CH 3 OH mixing ratio is in formal agreement with those reported by McKay et al. (2021) (∼3%), while our C 2 H 6 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 2 O) as well as mixing ratios of C 2 H 6 and CH 3 OH as measured by iSHELL and NIRSPEC-2 (Section 4; Bonev et al. 2021). Future work will comprehensively address potential variability in H 2 O production and trace species mixing ratios in Wirtanen as measured with iSHELL.

Comparison with Comets Measured at Near-infrared Wavelengths
Our results indicate that Wirtanen was enriched in both C 2 H 6 and CH 3 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-Pajdusáková (points #12 and 13 in Figure 5), which displayed similarly enriched C 2 H 6 and CH 3 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 2 H 6 mixing ratio, yet considerably lower CH 3 OH. In making these comparisons, it is important to note that although C 2 H 6 , CH 3 OH, and H 2 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,

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 H 2 O were taken nearly simultaneously with NIR-SPEC-2, whereas our L3-Custom observations sampling C 2 H 6 and CH 3 OH 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. 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 C 2 H 6 as an alternative compositional baseline when measuring mixing ratios.

Molecular Composition of the Coma
The T rot measured for H 2 O and C 2 H 6 are in formal agreement, and the measured iSHELL CH 3 OH T rot is consistent with all of these within 1σ uncertainty (the NIRSPEC-2 CH 3 OH T rot was assumed). The production rates and mixing ratios for C 2 H 6 agree within 1σ uncertainty for both instruments, and the H 2 O and CH 3 OH 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.

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(H 2 O) for its small size (∼1 km) attributed to significant release of H 2 O 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 H 2 O 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 H 2 O production in Wirtanen (up to 40%), and potentially an icy grain contribution to CH 3 OH 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-sunwardfacing 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 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 NC ) 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 H 2 O production as did the 24″ long NIRSPEC-2 slit.
To address this issue, we carefully examined the spatial profiles for H 2 O 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 H 2 O, C 2 H 6 , and CH 3 OH extracted from each instrument overlain on one another for comparison, and Figure 7 shows a comparison of spatial profiles for H 2 O emission as measured with iSHELL and NIRSPEC-2 along with their corresponding Q-curves. Figure 6(A) shows that the H 2 O 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 H 2 O spatial profile is at least as extended as (if not moreso 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 H 2 O production that was sampled by NIRSPEC-2, and that the differences in slit lengths between the two instruments did not significantly affect Q(H 2 O) 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 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 slitwidth 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(H 2 O) 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.

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, CH 4 , and C 2 H 6 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.

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 H 2 O as well as to C 2 H 6 . 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 C 2 H 4 and HC 3 N, as well as deuterated species (e.g., H 2 O and HDO, CH 4 and CH 3 D, C 2 H 6 and C 2 H 5 D). It also provides high signal-to-noise, spatially  . Bottom: relative abundances (% relative to H 2 O) for C 2 H 6 and CH 3 OH, with references for each date as cited above. 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.

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, H 2 O, and OCS. Recently published iSHELL studies have significantly increased the number of comets for which Figure 5. Mixing ratios of CH 3 OH and C 2 H 6 relative to H 2 O in comets characterized to date at near-infrared wavelengths (Dello Russo et al. 2016a;DiSanti et al. 2017;Faggi et al. 2018Faggi et al. , 2019Roth et al. 2018;Dello Russo et al. 2020). Comets are numbered and color coded, with triangles for JFCs and X's for OCCs. 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, nearinfrared 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 These iSHELL studies can reveal how coma abundances and spatial associations vary (or remain consistent) "seasonally" across a perihelion passage.

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 spatialspectral 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 2 O, H 2 CO, C 2 H 6 , CH 4 , HCN, NH 3 , C 2 H 2 ) in a single instrument setting, while iSHELL simultaneously samples M-band molecules (H 2 O, 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 2 O, C 2 H 6 , and CH 3 OH with high signal-to-noise far along the slit in only ten minutes onsource on December 18, and additionally detected HCN, C 2 H 2 , and NH 3 with only 19 minutes on-source during the previous night . 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 2 H 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, Δ = 0.1 au, Q(H 2 O)=10 28 s −1 ), C 2 H 6 and CH 3 OH could be detected (5σ 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 2 O. 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 2 H 6 and CH 3 OH in this study.

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 2 O, C 2 H 6 , and CH 3 OH in the inner coma of Wirtanen. Spatial profiles extracted for these molecules revealed that H 2 O emission was extended in the projected anti-sunward hemisphere, perhaps due to sublimation from icy grains in the coma, whereas C 2 H 6 emission was narrower. These results were highly consistent with those from coordinated NIRSPEC-2 observations , 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.