Observational constraints on the progenitor metallicities of core-collapse supernovae

We present constraints on the progenitor metallicities of core-collapse supernovae. To date, nearly all metallicity constraints have been inferred from indirect methods such as metallicity gradients in host galaxies, luminosities of host galaxies, or derived global galaxy metallicities. Here, progenitor metallicities are derived from optical spectra taken at the sites of nearby supernovae, from the ratio of strong emission lines found in their host HII regions.We present results from the spectra of 74 host HII regions and discuss the implications that these have on the nature of core-collapse supernova progenitors. Overall, while we find that the mean metallicity of type Ibc environments is higher than that of type II events, this difference is smaller than observed in previous studies. There is only a 0.06 dex difference in the mean metallicity values, at a statistical significance of ~1.5 sigma, while using a KS-test we find that the two metallicity distributions are marginally consistent with being drawn from the same parent population (probability >10%). This argues that progenitor metallicity is not a dominant parameter in deciding supernovae type, with progenitor mass and/or binarity playing a much more significant role.Comment: ACCEPTED for publication in MNRA

Comparisons of the radial distributions of core-collapse supernovae with those of young and old stellar populations

We present observational constraints on the nature of core-collapse supernovae through an investigation into their radial distributions with respect to those of young and old stellar populations within their host galaxies, as traced by H-alpha emission and R-band light respectively. We discuss results and the implications they have on the nature of supernova progenitors, for a sample of 177 core-collapse supernovae. We find that the radial positions of the overall core-collapse population closely follow the radial distribution of H-alpha emission, implying that both are excellent tracers of star formation within galaxies. Within this overall distribution we find that there is a central deficit of SNII which is offset by a central excess of SNIb/c. This implies a strong metallicity dependence on the relative production of the two types, with SNIb/c arising from higher metallicity progenitors than SNII. Separating the SNIb/c into individual classes we find that a trend emerges in terms of progenitor metallicity going from SNII through SNIb to SNIc, with the latter arising from the highest metallicity progenitors.Comment: Accepted for publication in MNRA

A Central Excess of Stripped-Envelope Supernovae within Disturbed Galaxies

This paper presents an analysis of core-collapse supernova distributions in isolated and interacting host galaxies, paying close attention to the selection effects involved in conducting host galaxy supernova studies. When taking into account all of the selection effects within our host galaxy sample, we draw the following conclusions: i) Within interacting, or 'disturbed', systems there is a real, and statistically significant, increase in the fraction of stripped-envelope supernovae in the central regions. A discussion into what may cause this increased fraction, compared to the more common type IIP supernovae, and type II supernovae without sub-classifications, is presented. Selection effects are shown not to drive this result, and so we propose that this study provides direct evidence for a high-mass weighted initial mass function within the central regions of disturbed galaxies. ii) Within 'undisturbed' spiral galaxies the radial distribution of type Ib and type Ic supernovae is statistically very different, with the latter showing a more centrally concentrated distribution. This could be driven by metallicity gradients in these undisturbed galaxies, or radial variations in other properties (binarity or stellar rotation) driving envelope loss in progenitor stars. This result is not found in 'disturbed' systems, where the distributions of type Ib and Ic supernovae are consistent.Comment: Accepted for publication in MNRA

Network anatomy in logopenic variant of primary progressive aphasia

The logopenic variant of primary progressive aphasia (lvPPA) is a neurodegenerative syndrome characterized linguistically by gradual loss of repetition and naming skills resulting from left posterior temporal and inferior parietal atrophy. Here, we sought to identify which specific cortical loci are initially targeted by the disease (epicenters) and investigate whether atrophy spreads through predetermined networks. First, we used cross-sectional structural MRI data from individuals with lvPPA to define putative disease epicenters using a surface-based approach paired with an anatomically fine-grained parcellation of the cortical surface (i.e., HCP-MMP1.0 atlas). Second, we combined cross-sectional functional MRI data from healthy controls and longitudinal structural MRI data from individuals with lvPPA to derive the epicenter-seeded resting-state networks most relevant to lvPPA symptomatology and ascertain whether functional connectivity in these networks predicts longitudinal atrophy spread in lvPPA. Our results show that two partially distinct brain networks anchored to the left anterior angular and posterior superior temporal gyri epicenters were preferentially associated with sentence repetition and naming skills in lvPPA. Critically, the strength of connectivity within these two networks in the neurologically-intact brain significantly predicted longitudinal atrophy progression in lvPPA. Taken together, our findings indicate that atrophy progression in lvPPA, starting from inferior parietal and temporoparietal junction regions, predominantly follows at least two partially nonoverlapping pathways, which may influence the heterogeneity in clinical presentation and prognosis

Benchmarking the reproducibility of all-solid-state battery cell performance

The interlaboratory comparability and reproducibility of all-solid-state battery cell cycling performance are poorly understood due to the lack of standardized set-ups and assembly parameters. This study quantifies the extent of this variability by providing commercially sourced battery materials—LiNi0.6Mn0.2Co0.2O2 for the positive electrode, Li6PS5Cl as the solid electrolyte and indium for the negative electrode—to 21 research groups. Each group was asked to use their own cell assembly protocol but follow a specific electrochemical protocol. The results show large variability in assembly and electrochemical performance, including differences in processing pressures, pressing durations and In-to-Li ratios. Despite this, an initial open circuit voltage of 2.5 and 2.7 V vs Li+/Li is a good predictor of successful cycling for cells using these electroactive materials. We suggest a set of parameters for reporting all-solid-state battery cycling results and advocate for reporting data in triplicate

Progenitor mass constraints for core-collapse supernovae from correlations with host galaxy star formation

Using H-alpha emission as a tracer of on-going (<16 Myr old) and near-UV emission as a tracer of recent (16-100 Myr old) star formation (SF), we present constraints on core-collapse (CC) supernova (SN) progenitors through their association with SF regions. We present statistics of a large sample of SNe; 163.5 type II (58 IIP, 13 IIL, 13.5 IIb, 19 IIn and 12 'impostors') and 96.5 type Ib/c (39.5 Ib and 52 Ic). Using pixel statistics our main findings and conclusions are: 1) An increasing progenitor mass sequence is observed, implied from an increasing association of SNe to host galaxy H-alpha emission. This commences with the type Ia (SNIa) showing the weakest association, followed by the SNII, then the SNIb, with the SNIc showing the strongest correlation to SF regions. Thus our progenitor mass sequence runs Ia-II-Ib-Ic. 2) Overall SNIbc are found to occur nearer to bright HII regions than SNII. This implies that the former have shorter stellar lifetimes thus arising from more massive progenitor stars. 3) While SNIIP do not closely follow the on-going SF, they accurately trace the recent formation. This implies that their progenitors arise from stars at the low end of the CC SN mass sequence, consistent with direct detections of progenitors in pre-explosion imaging. 4) Similarly SNIIn trace recent but not the on-going SF. This implies that, contrary to the general consensus, the majority of these SNe do not arise from the most massive stars. Results and constraints are also presented for the less numerous SNIIL, IIb, and 'impostors'. Finally we present analysis of possible biases in the data, the results of which argue strongly against any selection effects that could explain the relative excess of SNIbc within bright HII regions. Thus intrinsic progenitor differences in the sense of the mass sequence we propose remain the most plausible explanation of our findings.Comment: 22 pages, 13 figures. Accepted for publication in MNRAS. The abstract has been edited to fit within arXiv.org submission requirement

Vollbremsung: Die Folgen von Corona für den Straßenverkehr

Die Corona-Krise geht mit massiven wirtschaftlichen Einbußen ebenso einher wie mit Einschränkungen und Veränderungen im Privat- und Arbeitsleben. Die Effekte zeigen sich auch in den Verkehrsdaten, die offenbaren, dass im Zuge der Corona-Krise der LKW-Verkehr um etwa ein Viertel und der PKW-Verkehr sogar um über die Hälfte zurückgegangen ist