Teller et al. (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019) present radiocarbon analyses and paleoenvironmental data for a stratigraphic section at Lake Hind, Manitoba, Canada. The article expands on previous ones (Firestone et al., Reference Firestone, West, Kennett, Becker, Bunch, Revay, Schultz, Belgya, Kennett and Erlandson2007; Kennett et al., Reference Kennett, Kennett, Culleton, Aura Tortosa, Bischoff, Bunch and Daniel2015) arguing that extraterrestrial impact proxies are present at Lake Hind, comprising a Younger Dryas Boundary layer (YDB), and that this layer is synchronous with similar layers at other sites. However, we note three significant problems that cast doubt on their conclusions.

First, there are inconsistencies in the reporting of radiocarbon dates purported to be associated with the YDB. Teller et al. (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019) state that middle Subunit B1 corresponds to the deposition of YDB impact proxies. They further report that this layer yielded “one calibrated radiocarbon age of 12,630 ± 78 cal yr BP (PSUAMS-88701, 10,470 ± 35 ¹⁴C yr BP)” (Teller et al., Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019, p. 68) (we believe that sample PSUAMS-88701 was intended to read UCIAMS-88701). They indicate that this sample is associated with the hypothesized event. Curiously, prior work indicates that sample UCIAMS-29317, with an age of 10,610 ± 35 ¹⁴C yr BP, was also recovered “from directly within the proxy-rich YDB sample” (Kennett et al., Reference Kennett, Kennett, Culleton, Aura Tortosa, Bischoff, Bunch and Daniel2015, p. E4349; see also p. SI23 from this reference). This is not mentioned by Teller et al. (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019), although they describe the date as originating somewhere from within middle Subunit B1. Additionally, Teller et al. (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019, p. 67) list UCIAMS-29317 as a bulk sediment sample, whereas Kennett et al. (Reference Kennett, Kennett, Culleton, Aura Tortosa, Bischoff, Bunch and Daniel2015, p. SI23) identify it as charcoal. Which sample material is correct? Did the proxy-rich YDB layer contain one or two samples?

Second, we note that the inferred age of the Lake Hind YDB layer is, in part, a result of decisions made in the construction of their age–depth model. Their inferred YDB age is reported as 13,059–12,682 cal yr BP (95% interval; Teller et al., Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019, Supplementary Table S2). Age–depth models can be fit with a variety of methods and software packages that will yield different results (Trachsel and Telford, Reference Trachsel and Telford2017; Blaauw et al., Reference Blaauw, Christen, Bennett and Reimer2018). As such, we also fit Bayesian age–depth models to the Lake Hind dates using alternative software, the Bchron (Haslett and Parnell, Reference Haslett and Parnell2008) and rbacon (Blaauw and Christen, Reference Blaauw and Christen2019) R packages. The code used to fit these models is available at https:// github.com/taphocoenose/Lake-Hind.

Because Bchron uses sampling depth thickness, we used the dates from Table 1 of Teller et al. (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019). Following their description, we treated dates from upper and lower Subunit B1 (but not those from middle Subunit B1) and date UCIAMS-29317 as outliers. We assigned an outlier probability of 0.5 to these samples and the default outlier probability of 0.01 to the remaining samples. Unlike Teller et al.’s (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019) age–depth model, this Bchron model did not find that the start boundary of middle Subunit B1 (i.e., the YDB) was deposited synchronously with YDB layers at other sites (Supplementary Fig. S1). Rather, this modeled Lake Hind YDB age is ~80–350 yr younger than the hypothesized Younger Dryas impact and ~20–570 yr younger than Teller et al.’s (Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019, Supplementary Table S2) modeled Lake Hind YDB age.

The rbacon age–depth model also infers a YDB age that is younger than the hypothesized Younger Dryas impact, in this case by ~20–150 yr (Supplementary Fig. S2). We fit this model using the software's default parameter settings. The rbacon modeled boundary is between ~40 yr older and ~370 yr younger than the OxCal-modeled boundary. Notably, the model also identified 15 dates (58%) with 95% intervals that sit outside the 95% envelope of the model, indicating severe age-reversal issues. In sum, neither alternative software produced age–depth models supporting the hypothesis that the Lake Hind YDB age is synchronous with similar layers at other sites. They both suggest a younger age for the bottom of middle Subunit B1. Choosing between alternate age–depth models requires either well-justified support for the assumptions of a specific model or, if no one model is well justified, consideration of results from multiple plausibly justifiable models.

Finally, we question whether the melted magnetic spherules presented in this paper support the impact hypothesis. Previous papers (Firestone et al., Reference Firestone, West, Kennett, Becker, Bunch, Revay, Schultz, Belgya, Kennett and Erlandson2007; Bunch et al., Reference Bunch, Hermes, Moore, Kennett, Weaver, Wittke and DeCarli2012; Israde-Alcantara et al., Reference Israde-Alcantara, Bischoff, Dominguez-Vazquez, Li, DeCarli, Bunch and Wittke2012) have argued that magnetic spherules are best explained by the high temperatures resulting from an extraterrestrial impact or airburst and are not produced by lower temperatures associated with noncatastrophic events. Other researchers have identified magnetic spherules in non-YDB contexts (Surovell, et al., Reference Surovell, Holliday, Gingerich, Ketron, Haynes, Hilman, Wagner, Johnson and Claeys2009; Pinter et al., Reference Pinter, Scott, Daulton, Podoll, Koeberl, Anderson and Ishman2011; Pigati et al., Reference Pigati, Latorre, Rech, Betancourt, Martinez and Budahn2012; Holliday et al., Reference Holliday, Surovell and Johnson2016), but Younger Dryas impact hypothesis proponents have countered that melted spherules are only found in YDB-age layers (LeCompte et al., Reference LeCompte, Goodyear, Demitroff, Batchelor, Vogel, Mooney, Rock and Seidel2012; Wittke et al., Reference Wittke, Weaver, Bunch, Kennett, Kennett, Moore and Hillman2013; Teller et al., Reference Teller, Boyd, LeCompte, Kennett, West, Telka and Diaz2019). Thus, we are surprised that in the current contribution, only 2 of 11 melted magnetic spherules were recovered from the YDB layer at −33 to −30 cm. The other nine were recovered from a sample collected at a depth of −27 to −26 cm (12,510 ± 113 and 12,287 ± 111cal yr BP, ~200–550 yr younger than the age of the YDB in their age model). As such, the melted magnetic spherules appear to challenge their own conclusions and their previous claims that these objects are rare outside impact layers.

These problems call into question the Lake Hind chronology and YDB impact proxies. Given that the Younger Dryas impact hypothesis requires YDB layer synchroneity across multiple sites and that these layers should be defined by distinct impact proxies, it is critical that Lake Hind has a reliable chronology supported by accurate radiocarbon data and clear associations between spherules and the YDB layer.