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1. ZTF SN Ia DR2: An environmental study of Type Ia supernovae using host galaxy image decomposition

Author: Senzel, R., Maguire, K., Burgaz, U., Dimitriadis, G., Rigault, M., Goobar, A., Johansson, J., Smith, M., Deckers, M., Galbany, L., Ginolin, M., Harvey, L., Kim, Y. -L., Muller-Bravo, T. E., Nugent, P., Rosnet, P., Sollerman, J., Terwel, J. H., Laher, R. R., Reiley, D., and Rusholme, B.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The second data release of Type Ia supernovae (SNe Ia) observed by the Zwicky Transient Facility has provided a homogeneous sample of 3628 SNe Ia with photometric and spectral information. This unprecedented sample size enables us to better explore our currently tentative understanding of the dependence of host environment on SN Ia properties. In this paper, we make use of two-dimensional image decomposition to model the host galaxies of SNe Ia. We model elliptical galaxies as well as disk/spiral galaxies with or without central bulges and bars. This allows for the categorisation of SN Ia based on their morphological host environment, as well as the extraction of intrinsic galaxy properties corrected for both cosmological and atmospheric effects. We find that although this image decomposition technique leads to a significant bias towards elliptical galaxies in our final sample of galaxies, the overall results are robust. By successfully modelling 728 host galaxies, we find that the photometric properties of SNe Ia found in disks and in elliptical galaxies, correlate fundamentally differently with their host environment. We identified strong linear relations between light-curve stretch and our model-derived galaxy colour for both the elliptical (16.8$\sigma$) and disk (5.1$\sigma$) subpopulations of SNe Ia. Lower stretch SNe Ia are found in redder environments, which we identify as an age/metallicity effect. Within the subpopulation of SNe Ia found in disk containing galaxies, we find a significant linear trend (6.1$\sigma$) between light-curve stretch and model-derived local $r$-band surface brightness, which we link to the age/metallicity gradients found in disk galaxies. SN Ia colour shows little correlation with host environment as seen in the literature. We identify a possible dust effect in our model-derived surface brightness (3.3$\sigma$), for SNe Ia in disk galaxies., Comment: ZTF SN Ia DR2 release paper. Submitted to A&A (ZTF DR2 Special Issue)
Published: 2024

2. ZTF SN Ia DR2: Simulations and volume limited sample

Author: Amenouche, M., Smith, M., Rosnet, P., Rigault, M., Aubert, M., Barjou-Delayre, C., Burgaz, U., Carreres, B., Dimitriadis, G., Feinstein, F., Galbany, L., Ginolin, M., Goobar, A., Harvey, L., Kim, Y. -L., Maguire, K., Müller-Bravo, T. E., Nordin, J., Nugent, P., Racine, B., Rosselli, D., Regnault, N., Sollerman, J., Terwel, J. H., Townsend, A., Groom, S. L., Kulkarni, S. R., Kasliwal, M., Laher, R. R., and Purdum, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Type Ia supernovae (SNe Ia) constitute an historical probe to derive cosmological parameters through the fit of the Hubble-Lema\^itre diagram, i.e. SN Ia distance modulus versus their redshift. In the era of precision cosmology, realistic simulation of SNe Ia for any survey entering in an Hubble-Lema\^itre diagram is a key tool to address observational systematics, like Malmquist bias. As the distance modulus of SNe Ia is derived from the fit of their light-curves, a robust simulation framework is required. In this paper, we present the performances of the simulation framework skysurvey to reproduce the the Zwicky Transient Facility (ZTF) SN Ia DR2 covering the first phase of ZTF running from April 2018 up to December 2020. The ZTF SN Ia DR2 sample correspond to almost 3000 classified SNe Ia of cosmological quality. First, a targeted simulation of the ZTF SN Ia DR2 was carried on to check the validity of the framework after some fine tuning of the observing conditions and instrument performance. Then, a realistic simulation has been run using observing ZTF logs and ZTF SN Ia DR2 selection criteria on simulated light-curves to demonstrate the ability of the simulation framework to match the ZTF SN Ia DR2 sample. Furthermore a redshift dependency of SALT2 light-curve parameters (stretch and colour) was conducted to deduce a volume limited sample, i.e. an unbiased SNe Ia sample, characterized with $z_{lim} \leq 0.06$. This volume limited sample of about 1000 SNe Ia is unique to carry on new analysis on standardization procedure with a precision never reached (those analysis are presented in companion papers)., Comment: 10 pages, 10 figures. Submitted to A & A
Published: 2024

3. ZTF SN Ia DR2: The diversity and relative rates of the thermonuclear SN population

Author: Dimitriadis, G., Burgaz, U., Deckers, M., Maguire, K., Johansson, J., Smith, M., Rigault, M., Frohmaier, C., Sollerman, J., Galbany, L., Kim, Y. -L., Liu, C., Miller, A. A., Nugent, P. E., Alburai, A., Chen, P., Dhawan, S., Ginolin, M., Goobar, A., Groom, S. L., Harvey, L., Kenworthy, W. D., Kulkarni, S. R., Popovic, B., Riddle, R. L., Rusholme, B., Muller-Bravo, T. E., Nordin, J., Terwel, J. H., and Townsend, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Zwicky Transient Facility SN Ia Data Release 2 (ZTF SN Ia DR2) contains more than 3,000 Type Ia supernovae (SNe Ia), providing the largest homogeneous low-redshift sample of SNe Ia. Having at least one spectrum per event, this data collection is ideal for large-scale statistical studies of the photometric, spectroscopic and host-galaxy properties of SNe Ia, particularly of the more rare "peculiar" subclasses. In this paper, we first present the method we developed to spectroscopically classify the SNe in the sample, and the techniques we used to model their multi-band light curves and explore their photometric properties. We then show a method to distinguish between the "peculiar" subtypes and the normal SNe Ia. We also explore the properties of their host galaxies and estimate their relative rates, focusing on the "peculiar" subtypes and their connection to the cosmologically useful SNe Ia. Finally, we discuss the implications of our study with respect to the progenitor systems of the "peculiar" SN Ia events., Comment: 19 pages, 13 figures, submitted to Astronomy and Astrophysics
Published: 2024

4. ZTF SN Ia DR2: The spectral diversity of Type Ia supernovae in a volume-limited sample

Author: Burgaz, U., Maguire, K., Dimitriadis, G., Harvey, L., Senzel, R., Sollerman, J., Nordin, J., Galbany, L., Rigault, M., Smith, M., Goobar, A., Johansson, J., Rosnet, P., Amenouche, M., Deckers, M., Dhawan, S., Ginolin, M., Kim, Y. -L., Miller, A. A., Muller-Bravo, T. E., Nugent, P. E., Terwel, J. H., Dekany, R., Drake, A., Graham, M. J., Groom, S. L., Kasliwal, M. M., Kulkarni, S. R., Nolan, K., Nir, G., Riddle, R. L., Rusholme, B., and Sharma, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: More than 3000 spectroscopically confirmed Type Ia supernovae (SNe Ia) are presented in the Zwicky Transient Facility SN Ia Data Release 2 (ZTF DR2). In this paper, we detail the spectral properties of 482 SNe Ia near maximum light, up to a redshift limit of $z$ $\leq$ 0.06. We measure the velocities and pseudo-equivalent widths (pEW) of key spectral features (Si II $\lambda$5972 and Si II $\lambda$6355) and investigate the relation between the properties of the spectral features and the photometric properties from the SALT2 light-curve parameters as a function of spectroscopic sub-class. We discuss the non-negligible impact of host galaxy contamination on SN Ia spectral classifications, as well as investigate the accuracy of spectral template matching of the ZTF DR2 sample. We define a new subclass of underluminous SNe Ia (`04gs-like') that lie spectroscopically between normal SNe Ia and transitional 86G-like SNe Ia (stronger Si II $\lambda$5972 than normal SNe Ia but significantly weaker Ti II features than `86G-like' SNe). We model these `04gs-like' SN Ia spectra using the radiative-transfer spectral synthesis code tardis and show that cooler temperatures alone are unable to explain their spectra; some changes in elemental abundances are also required. However, the broad continuity in spectral properties seen from bright (`91T-like') to faint normal SN Ia, including the transitional and 91bg-like SNe Ia, suggests that variations within a single explosion model may be able to explain their behaviour.
Published: 2024

5. ZTF SN Ia DR2: The secondary maximum in Type Ia supernovae

Author: Deckers, M., Maguire, K., Shingles, L., Dimitriadis, G., Rigault, M., Smith, M., Goobar, A., Nordin, J., Johansson, J., Amenouche, M., Burgaz, U., Dhawan, S., Ginolin, M., Harvey, L., Kenworthy, W. D., Kim, Y. -L., Laher, R. R., Luo, N., Kulkarni, S. R., Masci, F. J., Müller-Bravo, T. E., Nugent, P. E., Pletskova, N., Purdum, J., Racine, B., Sollerman, J., and Terwel, J. H.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Type Ia supernova (SN Ia) light curves have a secondary maximum that exists in the $r$, $i$, and near-infrared filters. The secondary maximum is relatively weak in the $r$ band, but holds the advantage that it is accessible, even at high redshift. We used Gaussian Process fitting to parameterise the light curves of 893 SNe Ia from the Zwicky Transient Facility's (ZTF) second data release (DR2), and we were able to extract information about the timing and strength of the secondary maximum. We found $>5\sigma$ correlations between the light curve decline rate ($\Delta m_{15}(g)$) and the timing and strength of the secondary maximum in the $r$ band. Whilst the timing of the secondary maximum in the $i$ band also correlates with $\Delta m_{15}(g)$, the strength of the secondary maximum in the $i$ band shows significant scatter as a function of $\Delta m_{15}(g)$. We found that the transparency timescales of 97 per cent of our sample are consistent with double detonation models, and that SNe Ia with small transparency timescales ($<$ 32 d) reside predominantly in locally red environments. We measured the total ejected mass for the normal SNe Ia in our sample using two methods, and both were consistent with medians of $1.3\ \pm \ 0.3$ and $1.2\ \pm\ 0.2$ solar masses. We find that the strength of the secondary maximum is a better standardisation parameter than the SALT light curve stretch ($x_1$). Finally, we identified a spectral feature in the $r$ band as Fe II, which strengthens during the onset of the secondary maximum. The same feature begins to strengthen at $<$ 3 d post maximum light in 91bg-like SNe. Finally, the correlation between $x_1$ and the strength of the secondary maximum was best fit with a broken line, with a split at $x_1^0\ =\ -0.5\ \pm\ 0.2$, suggestive of the existence of two populations of SNe Ia., Comment: 18 pages, 14 figures
Published: 2024

6. ZTF SN Ia DR2: Study of Type Ia Supernova lightcurve fits

Author: Rigault, M., Smith, M., Regnault, N., Kenworthy, D. W., Maguire, K., Goobar, A., Dimitriadis, G., Amenouche, M., Aubert, M., Barjou-Delayre, C., Bellm, C. E., Burgaz, U., Carreres, B., Copin, Y., Deckers, M., de Jaeger, T., Dhawan, S., Feinstein, F., Fouchez, D., Galbany, L., Ginolin, M., Graham, J. M., Kim, Y. -L., Kowalski, M., Kuhn, D., Kulkarni, R. S., Muller-Bravo, E. T., Nordin, K., Popovic, M., Purdum, J., Rosnet, P., Rosselli, D., Racine, B., Ruppin, F., Sollerman, J., Terwel, H. J., and Townsend, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Type Ia supernova (SN Ia) cosmology relies on the estimation of lightcurve parameters to derive precision distances that leads to the estimation of cosmological parameters. The empirical SALT2 lightcurve modeling that relies on only two parameters, a stretch x1, and a color c, has been used by the community for almost two decades. In this paper we study the ability of the SALT2 model to fit the nearly 3000 cosmology-grade SN Ia lightcurves from the second release of the Zwicky Transient Facility (ZTF) cosmology science working group. While the ZTF data was not used to train SALT2, the algorithm is modeling the ZTF SN Ia optical lightcurves remarkably well, except for lightcurve points prior to -10 d from maximum, where the training critically lacks statistics. We find that the lightcurve fitting is robust against the considered choice of phase-range, but we show the [-10; +40] d range to be optimal in terms of statistics and accuracy. We do not detect any significant features in the lightcurve fit residuals that could be connected to the host environment. Potential systematic population differences related to the SN Ia host properties might thus not be accountable for by the addition of extra lightcurve parameters. However, a small but significant inconsistency between residuals of blue- and red-SN Ia strongly suggests the existence of a phase-dependent color term, with potential implications for the use of SNe Ia in precision cosmology. We thus encourage modellers to explore this avenue and we emphasize the importance that SN Ia cosmology must include a SALT2 retraining to accurately model the lightcurves and avoid biasing the derivation of cosmological parameters., Comment: 10 pages, 9 figures. Submitted to Astronomy and Astrophysics
Published: 2024

7. ZTF SN Ia DR2: Colour standardisation of Type Ia Supernovae and its dependence on environment

Author: Ginolin, M., Rigault, M., Copin, Y., Popovic, B., Dimitriadis, G., Goobar, A., Johansson, J., Maguire, K., Nordin, J., Smith, M., Aubert, M., Barjou-Delayre, C., Burgaz, U., Carreres, B., Dhawan, S., Deckers, M., Feinstein, F., Fouchez, D., Galbany, L., Ganot, C., de Jaeger, T., Kim, Y. -L., Kuhn, D., Lacroix, L., Müller-Bravo, T. E., Nugent, P., Racine, B., Rosnet, P., Rosselli, D., Ruppin, F., Sollerman, J., Terwel, J. H., Townsend, A., Dekany, R., Graham, M., Kasliwal, M., Groom, S. L., Purdum, J., Rusholme, B., and van der Walt, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: As Type Ia supernova cosmology transitions from a statistics dominated to a systematics dominated era, it is crucial to understand leftover unexplained uncertainties affecting their luminosity, such as the ones stemming from astrophysical biases. Indeed, SNe Ia are standardisable candles, whose absolute magnitude reach a 0.15~mag scatter once empirical correlations with their lightcurve stretch and colour and with their environment are accounted for. In this paper, we investigate how the standardisation process of SNe Ia depends on environment, to ultimately reduce their scatter in magnitude, focusing on colour standardisation. We use the volume-limited ZTF SN Ia DR2 sample, which offers unprecedented statistics for the low redshift ($z<0.06$) range. We first study the colour distribution, focusing on the effects of dust, to then select a dustless subsample of objects from low stellar mass environments and from the outskirts of their host galaxies. We then look at the colour-residuals relation and its associated parameter $\beta$. Finally, we investigate the colour dependency of the environment-dependent magnitude offsets (steps), to try to disentangle intrinsic and extrinsic colour origin. Our sample probes well the red tail of the colour distribution, up to $c=0.8$. The dustless sample exhibits a significantly lower red tail ($4.6\sigma$) in comparison to the whole sample. This suggests that reddening above $c\geq0.2$ is dominated by host interstellar dust absorption. Looking at the colour-residuals relation, we find it to be linear with lightcurve colour. We show hints of a potential evolution of $\beta$ with host stellar mass at a $2.5\sigma$ level. Finally, unlike recent claims from the literature, we see no evolution of steps as a function of lightcurve colour, suggesting that dust may not be the dominating mechanism responsible for the environmental dependency of SNe Ia magnitude., Comment: 10 pages, 7 figures, submitted to Astronomy and Astrophysics
Published: 2024

8. ZTF SN~Ia DR2: Cosmology-independent constraints on Type Ia supernova standardisation from supernova siblings

Author: Dhawan, S., Mortsell, E., Johansson, J., Goobar, A., Rigault, M., Smith, M., Maguire, K., Nordin, J., Dimitriadis, G., Nugent, P. E., Galbany, L., Sollerman, J., de Jaeger, T., Terwel, J. H., Kim, Y. -L., Burgaz, Umut, Helou, G., Purdum, J., Groom, S. L., Laher, R., and Healy, B.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Understanding Type Ia supernovae (SNe~Ia) and the empirical standardisation relations that make them excellent distance indicators is vital to improving cosmological constraints. SN~Ia ``siblings", i.e. two or more SNe~Ia in the same host or parent galaxy offer a unique way to infer the standardisation relations and their diversity across the population. We analyse a sample of 25 SN~Ia pairs, observed homogeneously by the Zwicky Transient Factory (ZTF) to infer the SNe~Ia light curve width-luminosity and colour-luminosity parameters $\alpha$ and $\beta$. Using the pairwise constraints from siblings, allowing for a diversity in the standardisation relations, we find $\alpha = 0.218 \pm 0.055 $ and $\beta = 3.084 \pm 0.312$, respectively, with a dispersion in $\alpha$ and $\beta$ of $\leq 0.195$ and $\leq 0.923$, respectively, at 95$\%$ C.L. While the median dispersion is large, the values within $\sim 1 \sigma$ are consistent with no dispersion. Hence, fitting for a single global standardisation relation, we find $\alpha = 0.228 \pm 0.029 $ and $\beta = 3.160 \pm 0.191$. We find a very small intrinsic scatter of the siblings sample $\sigma_{\rm int} \leq 0.10$ at 95\% C.L. compared to $\sigma_{\rm int} = 0.22 \pm 0.04$ when computing the scatter using the Hubble residuals without comparing them as siblings. Splitting the sample based on host galaxy stellar mass, we find that SNe~Ia in both subsamples have consistent $\alpha$ and $\beta$. The $\beta$ value is consistent with the value for the cosmological sample. However, we find a higher $\alpha$ by $\sim 2.5 - 3.5 \sigma$. The high $\alpha$ is driven by low $x_1$ pairs, potentially suggesting that the slow and fast declining SN~Ia have different slopes of the width-luminosity relation. We can confirm or refute this with increased statistics from near future time-domain surveys. (abridged), Comment: 12 pages, 7 figures, submitted to A&A
Published: 2024

9. ZTF SN Ia DR2: Impact of the galaxy cluster environment on the stretch distribution of Type Ia supernovae

Author: Ruppin, F., Rigault, M., Ginolin, M., Dimitriadis, G., Goobar, A., Johansson, J., Maguire, K., Nordin, J., Smith, M., Aubert, M., Biedermann, J., Copin, Y., Burgaz, U., Carreres, B., Feinstein, F., Fouchez, D., Muller-Bravo, T. E., Galbany, L., Groom, S. L., Kenworthy, W. D., Kim, Y. -L., Laher, R. R., Nugent, P., Popovic, B., Purdum, J., Racine, B., Rosnet, P., Rosselli, D., Smith, R., Sollerman, J., and Terwel, J. H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Understanding the impact of the astrophysical environment on Type Ia supernova (SN Ia) properties is crucial to minimize systematic uncertainties in cosmological analyses based on this probe. We investigate the dependence of the SN Ia SALT2.4 light-curve stretch on the distance from their nearest galaxy cluster to study a potential effect of the intracluster medium (ICM) environment on SN Ia intrinsic properties. We use the largest SN Ia sample to date and cross-match it with existing X-ray, Sunyaev-Zel'dovich, and optical cluster catalogs in order to study the dependence between stretch and distance to the nearest detected cluster from each SN Ia. We model the underlying stretch distribution with a Gaussian mixture with relative amplitudes that depend on redshift and cluster-centric distance. We find a significant improvement of the fit quality of the stretch distribution if we include the distance-dependant term in the model with a variation of the Akaike information criterion $\rm{\Delta AIC} = -10.2$. Because of the known correlation between galaxy age and distance from cluster center, this supports previous evidence that the age of the stellar population is the underlying driver of the bimodial shape of the SN Ia stretch distribution. We further compute the evolution of the fraction of quenched galaxies as a function of distance with respect to cluster center from our best-fit model of the SNe Ia stretch distribution and compare it to previous results obtained from $H\alpha$ line measurements, optical broadband photometry, and simulations. We find our estimate to be compatible with these results. The results of this work indicate that SNe Ia searches at high redshift targeted towards clusters to maximize detection probability should be considered with caution as the stretch distribution of the detected sample would be strongly biased towards the old sub-population of SNe Ia., Comment: Accepted in Astronomy & Astrophysics
Published: 2024

10. ZTF SN Ia DR2: Environmental dependencies of stretch and luminosity of a volume limited sample of 1,000 Type Ia Supernovae

Author: Ginolin, M., Rigault, M., Smith, M., Copin, Y., Ruppin, F., Dimitriadis, G., Goobar, A., Johansson, J., Maguire, K., Nordin, J., Amenouche, M., Aubert, M., Barjou-Delayre, C., Betoule, M., Burgaz, U., Carreres, B., Deckers, M., Dhawan, S., Feinstein, F., Fouchez, D., Galbany, L., Ganot, C., Harvey, L., de Jaeger, T., Kenworthy, W. D., Kim, Y. -L., Kowalski, M., Kuhn, D., Lacroix, L., Muller-Bravo, T. E., Nugent, P., Popovic, B., Racine, B., Rosnet, P., Rosselli, D., Sollerman, J., Terwel, J. H., Townsend, A., Brugger, J., Bellm, E. C., Kasliwal, M. M., Kulkarni, S., Laher, R. R., Masci, F. J., Riddle, R. L., and Sharma, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: To get distances, Type Ia Supernovae magnitudes are corrected for their correlation with lightcurve width and colour. Here we investigate how this standardisation is affected by the SN environment, with the aim to reduce scatter and improve standardisation. We first study the SN Ia stretch distribution, as well as its dependence on environment, as characterised by local and global (g-z) colour and stellar mass. We then look at the standardisation parameter $\alpha$, which accounts for the correlation between residuals and stretch, along with its environment dependence and linearity. We finally compute magnitude offsets between SNe in different astrophysical environments after colour and stretch standardisation, aka steps. This analysis is made possible due to the unprecedented statistics of the ZTF SN Ia DR2 volume-limited sample. The stretch distribution exhibits a bimodal behaviour, as previously found in literature. However, we find the distribution means to decrease with host stellar mass at a 9.0$\sigma$ significance. We demonstrate, at the 14.3$\sigma$ level, that the stretch-magnitude relation is non-linear, challenging the usual linear stretch-residuals relation. Fitting for a broken-$\alpha$ model, we indeed find two different slopes between stretch regimes ($x_1<-0.49\pm0.06$): $\alpha_{low}=0.28\pm0.01$ and $\alpha_{high}=0.09\pm0.01$, a $\Delta_{\alpha}=-0.19\pm0.01$ difference. As the relative proportion of SNe Ia in the high-/low-stretch modes evolves with redshift and environment, this implies that a linear $\alpha$ also evolves with redshift and environment. Concerning the environmental magnitude offset $\gamma$, we find it to be greater than 0.14 mag regardless of the considered environmental tracer used (local or global colour and stellar mass), all measured at the $\geq 6\sigma$ level, increased to $\sim0.18\pm0.01$ mag when accounting for the stretch-non linearity., Comment: 15 pages, 9 figures, submitted to Astronomy and Astrophysics
Published: 2024

11. Quantitative modelling of type Ia supernovae spectral time series: Constraining the explosion physics

Author: Magee, M. R., Siebenaler, L., Maguire, K., Ackley, K., and Killestein, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Multiple explosion mechanisms have been proposed to explain type Ia supernovae (SNe Ia). Empirical modelling tools have also been developed that allow for fast, customised modelling of individual SNe and direct comparisons between observations and explosion model predictions. Such tools have provided useful insights, but the subjective nature with which empirical modelling is performed makes it difficult to obtain robust constraints on the explosion physics or expand studies to large populations of objects. Machine learning accelerated tools have therefore begun to gain traction. In this paper, we present riddler, a framework for automated fitting of SNe Ia spectral sequences up to shortly after maximum light. We train a series of neural networks on realistic ejecta profiles predicted by the W7 and N100 explosion models to emulate full radiative transfer simulations and apply nested sampling to determine the best-fitting model parameters for multiple spectra of a given SN simultaneously. We show that riddler is able to accurately recover the parameters of input spectra and use it to fit observations of two well-studied SNe Ia. We also investigate the impact of different weighting schemes when performing quantitative spectral fitting and show that best-fitting models and parameters are highly dependent on the assumed weighting schemes and priors. As spectroscopic samples of SNe Ia continue to grow, automated spectral fitting tools such as riddler will become increasingly important to maximise the physical constraints that can be gained in a quantitative and consistent manner., Comment: 28 pages, 4 appendices, 18 figures, 4 tables. Accepted for publication in MNRAS. The riddler code is publicly available at https://github.com/MarkMageeAstro/Riddler
Published: 2024

12. The orbital period, black hole mass and distance to the X-ray transient GRS 1716-249 (=N Oph 93)

Author: Casares, J., Yanes-Rizo, I. V., Torres, M. A. P., Abbott, T. M. C., Padilla, M. Armas, Charles, P. A., Cuneo, V. A., Muñoz-Darias, T., Jonker, P. G., and Maguire, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present evidence for a 0.278(8) d (=6.7 h) orbital period in the X-ray transient GRS 1716-249 (=N Oph 93), based on a superhump modulation detected during the 1995 mini-outburst plus ellipsoidal variability in quiescence. With a quiescent magnitude of r=23.19+-0.15 N Oph 93 is too faint to warrant a full dynamical study through dedicated time-resolved spectroscopy. Instead, we apply the FWHM-K2 correlation to the disc Halpha emission line detected in Gran Telescopio Canarias spectra and obtain K2=521+-52 km/s. This leads to a mass function f(M)=4.1+-1.2 Msun, thus indicating the presence of a black hole in this historic X-ray transient. Furthermore, from the depth of the Halpha trough and the quiescent light curve we constrain the binary inclination to i=61+-15 deg, while the detection of superhumps sets an upper limit to the donor to compact star mass ratio q=M2/M1<=0.25. Our de-reddened (r-i) colour is consistent with a ~K6 main sequence star that fills its Roche lobe in a 0.278 d orbit. Using all this information we derive a compact object mass M1=6.4+3.2-2.0 Msun at 68 per cent confidence. We also constrain the distance to GRS 1716-249 to 6.9+-1.1 kpc, placing the binary ~0.8 kpc above the Galactic Plane, in support of a large natal kick., Comment: Accepted for publication in MNRAS, 12 pages, 9 figures, 2 Tables
Published: 2023

13. No plateau observed in late-time near-infrared observations of the underluminous Type Ia supernova 2021qvv

Author: Graur, O., Gonzalez, E. Padilla, Burke, J., Deckers, M., Jha, S. W., Galbany, L., Karamenhmetoglu, E., Stritzinger, M. D., Maguire, K., Howell, D. A., Fisher, R., Fullard, A. G., Handberg, R., Hiramatsu, D., Hosseinzadeh, G., Kerzendorf, W. E., McCully, C., Newsome, M., Pellegrino, C., Rest, A., Riess, A. G., Seitenzahl, I. R., Shara, M. M., Shen, K. J., Terreran, G., and Zurek, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Near-infrared (NIR) observations of normal Type Ia supernovae (SNe Ia) obtained between 150 to 500 d past maximum light reveal the existence of an extended plateau. Here, we present observations of the underluminous, 1991bg-like SN 2021qvv. Early, ground-based optical and NIR observations show that SN 2021qvv is similar to SN 2006mr, making it one of the dimmest, fastest-evolving 1991bg-like SNe to date. Late-time (170-250 d) Hubble Space Telescope observations of SN 2021qvv reveal no sign of a plateau. An extrapolation of these observations backwards to earlier-phase NIR observations of SN 2006mr suggests the complete absence of a NIR plateau, at least out to 250 d. This absence may be due to a higher ionization state of the ejecta, as predicted by certain sub-Chandrasekhar-mass detonation models, or to the lower temperatures of the ejecta of 1991bg-like SNe, relative to normal SNe Ia, which might preclude their becoming fluorescent and shifting ultraviolet light into the NIR. This suggestion can be tested by acquiring NIR imaging of a sample of 1991bg-like SNe that covers the entire range from slowly-evolving to fast-evolving events ($0.2 \lesssim s_\mathrm{BV} \lesssim 0.6$). A detection of the NIR plateau in slower-evolving, hotter 1991bg-like SNe would provide further evidence that these SNe exist along a continuum with normal SNe Ia. Theoretical progenitor and explosion scenarios would then have to match the observed properties of both SN Ia subtypes., Comment: Accepted for publication in MNRAS (14 pages, 9 figures)
Published: 2023

14. Photometric study of the late-time near-infrared plateau in Type Ia supernovae

Author: Deckers, M., Graur, O., Maguire, K., Shingles, L., Brennan, S. J., Anderson, J. P., Burke, J., Chen, T. -W., Galbany, L., Grayling, M. J. P., Gutiérrez, C. P., Harvey, L., Hiramatsu, D., Howell, D. A., Inserra, C., Killestein, T., McCully, C., Müller-Bravo, T. E., Nicholl, M., Newsome, M., Gonzalez, E. Padilla, Pellegrino, C., Terreran, G., Terwel, J. H., Toy, M., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present an in-depth study of the late-time near-infrared plateau in Type Ia supernovae (SNe Ia), which occurs between 70-500 d. We double the existing sample of SNe Ia observed during the late-time near-infrared plateau with new observations taken with the Hubble Space Telescope, Gemini, New Technology Telescope, the 3.5m Calar Alto Telescope, and the Nordic Optical Telescope. Our sample consists of 24 nearby SNe Ia at redshift < 0.025. We are able to confirm that no plateau exists in the Ks band for most normal SNe Ia. SNe Ia with broader optical light curves at peak tend to have a higher average brightness on the plateau in J and H, most likely due to a shallower decline in the preceding 100 d. SNe Ia that are more luminous at peak also show a steeper decline during the plateau phase in H. We compare our data to state-of-the-art radiative transfer models of nebular SNe Ia in the near-infrared. We find good agreement with the sub-Mch model that has reduced non-thermal ionisation rates, but no physical justification for reducing these rates has yet been proposed. An analysis of the spectral evolution during the plateau demonstrates that the ratio of [Fe II] to [Fe III] contribution in a near-infrared filter determines the light curve evolution in said filter. We find that overluminous SNe decline slower during the plateau than expected from the trend seen for normal SNe Ia, Comment: 17 pages, 8 figures, Accepted for publication in MNRAS
Published: 2023
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15. Feasibility of backfilling mines using cement kiln dust, fly ash, and cement blends

Author: Beltagui H., Sonebi M., Maguire K., and Taylor S.
Subjects: Engineering (General). Civil engineering (General), TA1-2040
Abstract: Cement kiln dust (CKD) is an industrial by-product of the cement manufacturing process, the composition of which can vary widely. Recent years of using alternative fuels have resulted in higher chloride and alkali contents within CKDs; as such, this limits the applications in which CKDs can be utilised. Using a CKD containing a high free lime content of 29.5%, it is shown that this CKD is capable of activating pulverized fuel ash (PFA) due to its high alkalinity, which can be utilised in low strength un-reinforced applications. One potential application involves the backfill of mines, reducing the need for continuous maintenance of the mine. This study focuses on the compressive strength achieved by various blends of CKD, PFA, and cement. Samples were hand mixed and compacted in 100 mm x 50 mm diameter cylinders, and unconfined compressive strength measurements taken at 28 and 56 days. The hydration products were assessed through the use of x-ray diffraction and thermogravimetric analysis. Aiming to maximise the use of CKD at a water to binder (w/b) ratio of 0.2, it was found that the maximum CKD content possible to achieve the required strength was 90% CKD blended with 10% cement.
Published: 2018
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16. The rise and fall of the iron-strong nuclear transient PS16dtm

Author: Petrushevska, T., Leloudas, G., Ilic, D., Bronikowski, M., Charalampopoulos, P., Jaisawal, G. K., Paraskeva, E., Pursiainen, M., Rakic, N., Schulze, S., Taggart, K., Wedderkopp, C. K., Anderson, J. P., de Boer, T., Chambers, K., Chen, T. W., Damljanovic, G., Fraser, M., Gao, H., Gomboc, A., Gromadzki, M., Ihanec, N., Maguire, K., Marcun, B., Muller-Bravo, T. E., Nicholl, M., Onori, F., Reynolds, T. M., Smartt, S. J., Sollerman, J., Smith, K. W., Wevers, T., and Wyrzykowski, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Thanks to the advent of large-scale optical surveys, a diverse set of flares from the nuclear regions of galaxies has recently been discovered. These include the disruption of stars by supermassive black holes at the centers of galaxies - nuclear transients known as tidal disruption events (TDEs). Active galactic nuclei (AGN) can show extreme changes in the brightness and emission line intensities, often referred to as changing-look AGN (CLAGN). Given the physical and observational similarities, the interpretation and distinction of nuclear transients as CLAGN or TDEs remains difficult. One of the obstacles of making progress in the field is the lack of well-sampled data of long-lived nuclear outbursts in AGN. Here, we study PS16dtm, a nuclear transient in a Narrow Line Seyfert 1 (NLSy1) galaxy, which has been proposed to be a TDE candidate. Our aim is to study the spectroscopic and photometric properties of PS16dtm, in order to better understand the outbursts originating in NLSy1 galaxies. Our extensive multiwavelength follow-up that spans around 2000 days includes photometry and spectroscopy in the UV/optical, as well as mid-infrared (MIR) and X-ray observations. Furthermore, we improved an existing semiempirical model in order to reproduce the spectra and study the evolution of the spectral lines. The UV/optical light curve shows a double peak at $\sim50$ and $\sim100$ days after the first detection, and it declines and flattens afterward, reaching preoutburst levels after 2000 days of monitoring. The MIR light curve rises almost simultaneously with the optical, but unlike the UV/optical which is approaching the preoutburst levels in the last epochs of our observations, the MIR emission is still rising at the time of writing. The optical spectra show broad Balmer features and the strongest broad Fe II emission ever detected in a nuclear transient. [abridged], Comment: Accepted for publication in A&A, 19 pages and 18 figures
Published: 2022
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17. The luminous type Ia supernova 2022ilv and its early excess emission

Author: Srivastav, Shubham, Smartt, S. J., Huber, M. E., Dimitriadis, G., Chambers, K. C., Fulton, Michael D., Moore, Thomas, Callan, F. P., Gillanders, James H., Maguire, K., Nicholl, M., Shingles, Luke J., Sim, S. A., Smith, K. W., Anderson, J. P., de Boer, Thomas, Chen, Ting-Wan, Gao, Hua, and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present observations and analysis of the host-less and luminous type Ia supernova 2022ilv, illustrating it is part of the 2003fg-like family, often referred to as super-Chandrasekhar (Ia-SC) explosions. The ATLAS light curve shows evidence of a short-lived, pulse-like early excess, similar to that detected in another luminous type Ia supernova (SN 2020hvf). The light curve is broad and the early spectra are remarkably similar to SN 2009dc. Adopting a redshift of $z=0.026 \pm 0.005$ for SN 2022ilv based on spectral matching, our model light curve requires a large $^{56}$Ni mass in the range $0.7-1.5$ M$_{\odot}$, and a large ejecta mass in the range $1.6-2.3$ M$_{\odot}$. The early excess can be explained by fast-moving SN ejecta interacting with a thin, dense shell of circumstellar material close to the progenitor ($\sim 10^{13}$ cm), a few hours after the explosion. This may be realised in a double-degenerate scenario, wherein a white dwarf merger is preceded by ejection of a small amount ($\sim 10^{-3}-10^{-2}$ M$_{\odot}$) of hydrogen and helium-poor tidally stripped material. A deep pre-explosion Pan-STARRS1 stack indicates no host galaxy to a limiting magnitude of $r \sim 24.5$. This implies a surprisingly faint limit for any host of $M_r \gtrsim -11$, providing further evidence that these types of explosion occur predominantly in low-metallicity environments., Comment: Accepted to ApJL after minor revision
Published: 2022
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18. Panning for gold, but finding helium: discovery of the ultra-stripped supernova SN2019wxt from gravitational-wave follow-up observations

Author: Agudo, I., Amati, L., An, T., Bauer, F. E., Benetti, S., Bernardini, M. G., Beswick, R., Bhirombhakdi, K., de Boer, T., Branchesi, M., Brennan, S. J., Caballero-García, M. D., Cappellaro, E., Rodríguez, N. Castro, Castro-Tirado, A. J., Chambers, K. C., Chassande-Mottin, E., Chaty, S., Chen, T. -W., Coleiro, A., Covino, S., D'Ammando, F., D'Avanzo, P., D'Elia, V., Fiore, A., Flörs, A., Fraser, M., Frey, S., Frohmaier, C., Galbany, L., Gall, C., Gao, H., García-Rojas, J., Ghirlanda, G., Giarratana, S., Gillanders, J. H., Giroletti, M., Gompertz, B. P., Gromadzki, M., Heintz, K. E., Hu, Y. -D., Huber, M. E., Inkenhaag, A., Izzo, L., Jin, Z. P., Jonker, P. G., Kann, D. A., Kool, E. C., Kotak, R., Leloudas, G., Levan, A. J., Lin, C. -C., Lyman, J. D., Magnier, E. A., Maguire, K., Mandel, I., Marcote, B., Sánchez, D. Mata, Mattila, S., Melandri, A., Michałowski, M. J., Moldon, J., Nicholl, M., Guelbenzu, A. Nicuesa, Oates, S. R., Onori, F., Orienti, M., Paladino, R., Paragi, Z., Perez-Torres, M., Pian, E., Pignata, G., Piranomonte, S., Quirola-Vásquez, J., Ragosta, F., Rau, A., Ronchini, S., Rossi, A., Sánchez-Ramírez, R., Salafia, O. S., Schulze, S., Smartt, S. J., Smith, K. W., Sollerman, J., Srivastav, S., Starling, R. L. C., Steeghs, D., Stevance, H. F., Testa, V., Torres, M. A. P., Vergani, S. D., Vescovi, D., Wainscost, R., Watson, D., Wiersema, K., Wyrzykowski, Ł., Yang, J., Yang, S., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the results from multi-wavelength observations of a transient discovered during the follow-up of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN2019wxt, a young transient in a galaxy whose sky position (in the 80\% GW contour) and distance ($\sim$150\,Mpc) were plausibly compatible with the localisation uncertainty of the GW event. Initially, the transient's tightly constrained age, its relatively faint peak magnitude ($M_i \sim -16.7$\,mag) and the $r-$band decline rate of $\sim 1$\,mag per 5\,days appeared suggestive of a compact binary merger. However, SN2019wxt spectroscopically resembled a type Ib supernova, and analysis of the optical-near-infrared evolution rapidly led to the conclusion that while it could not be associated with S191213g, it nevertheless represented an extreme outcome of stellar evolution. By modelling the light curve, we estimated an ejecta mass of $\sim 0.1\,M_\odot$, with $^{56}$Ni comprising $\sim 20\%$ of this. We were broadly able to reproduce its spectral evolution with a composition dominated by helium and oxygen, with trace amounts of calcium. We considered various progenitors that could give rise to the observed properties of SN2019wxt, and concluded that an ultra-stripped origin in a binary system is the most likely explanation. Disentangling electromagnetic counterparts to GW events from transients such as SN2019wxt is challenging: in a bid to characterise the level of contamination, we estimated the rate of events with properties comparable to those of SN2019wxt and found that $\sim 1$ such event per week can occur within the typical GW localisation area of O4 alerts out to a luminosity distance of 500\,Mpc, beyond which it would become fainter than the typical depth of current electromagnetic follow-up campaigns., Comment: By the ENGRAVE collaboration (engrave-eso.org). 35 pages, 20 figures, final version accepted by A&A
Published: 2022
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19. Probing for the host galaxies of the fast X-ray transients XRT 000519 and XRT 110103

Author: Eappachen, D., Jonker, P. G., Fraser, M., Torres, M. A. P., Dhillon, V. S., Marsh, T., Littlefair, S. P., Quirola-Vasquez, J., Maguire, K., Sanchez, D. Mata, Cannizzaro, G., Kostrzewa-Rutkowska, Z., Wevers, T., Onori, F., Inkenhaag, Anne, and Brennan, S. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: Over the past few years, $\sim$30 extragalactic fast X-ray transients (FXRTs) have been discovered, mainly in Chandra and XMM-Newton data. Their nature remains unclear, with proposed origins including a double neutron star merger, a tidal disruption event involving an intermediate-mass black hole and a white dwarf, or a supernova shock breakout. A decisive differentiation between these three promising mechanisms for their origin requires an understanding of the FXRT energetics, environments, and/or host properties. We present optical observations obtained with the Very Large Telescope for the FXRTs XRT 000519 and XRT 110103 and Gran Telescopio Canarias observations for XRT 000519 designed to search for host galaxies of these FXRTs. In the $g_s$, $r_s$ and $R$-band images, we detect an extended source on the North-West side of the $\sim$ $1^{\prime\prime}$ (68% confidence) error circle of the X-ray position of XRT 000519 with a Kron magnitude of $g_s=$26.29$\pm$0.09 (AB magnitude). We discuss the XRT 000519 association with the probable host candidate for various possible distances, and we conclude that if XRT 000519 is associated with the host candidate a supernova shock breakout scenario is likely excluded. No host galaxy is found near XRT 110103 down to a limiting magnitude of $R>25.8$., Comment: 11 pages, 11 figures, submitted to MNRAS
Published: 2022
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20. The detection efficiency of type Ia supernovae from the Zwicky Transient Facility: Limits on the intrinsic rate of early flux excesses

Author: Magee, M. R., Cuddy, C., Maguire, K., Deckers, M., Dhawan, S., Frohmaier, C., Miller, A. A., Nordin, J., Coughlin, M. W., Feinstein, F., and Riddle, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Samples of young type Ia supernovae have shown `early excess' emission in a few cases. Similar excesses are predicted by some explosion and progenitor scenarios and hence can provide important clues regarding the origin of thermonuclear supernovae. They are however, only predicted to last up to the first few days following explosion. It is therefore unclear whether such scenarios are intrinsically rare or if the relatively small sample size simply reflects the difficulty in obtaining sufficiently early detections. To that end, we perform toy simulations covering a range of survey depths and cadences, and investigate the efficiency with which young type Ia supernovae are recovered. As input for our simulations, we use models that broadly cover the range of predicted luminosities. Based on our simulations, we find that in a typical three day cadence survey, only $\sim$10% of type Ia supernovae would be detected early enough to rule out the presence of an excess. A two day cadence however, should see this increase to $\sim$15%. We find comparable results from more detailed simulations of the Zwicky Transient Facility surveys. Using the recovery efficiencies from these detailed simulations, we investigate the number of young type Ia supernovae expected to be discovered assuming some fraction of the population come from scenarios producing an excess at early times. Comparing the results of our simulations to observations, we find the intrinsic fraction of type Ia supernovae with early flux excesses is $\sim28^{+13}_{-11}%$%., Comment: 16 pages, 15 figures, 2 tables. Accepted for publication in MNRAS
Published: 2022
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21. Constraining Type Ia supernova explosions and early flux excesses with the Zwicky Transient Factory

Author: Deckers, M., Maguire, K., Magee, M. R., Dimitriadis, G., Smith, M., de Murieta, A. Sainz, Miller, A. A., Goobar, A., Nordin, J., Rigault, M., Bellm, E., Coughlin, M. W., Laher, R. R., Shupe, D., Graham, M. J., Kasliwal, M. M., and Walters, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In the new era of time-domain surveys Type Ia supernovae are being caught sooner after explosion, which has exposed significant variation in their early light curves. Two driving factors for early time evolution are the distribution of nickel in the ejecta and the presence of flux excesses of various causes. We perform an analysis of the largest young SN Ia sample to date. We compare 115 SN Ia light curves from the Zwicky Transient Facility to the turtls model grid containing light curves of Chandrasekhar-mass explosions with a range of nickel masses, nickel distributions and explosion energies. We find that the majority of our observed light curves are well reproduced by Chandrasekhar-mass explosion models with a preference for highly extended nickel distributions. We identify six SNe Ia with an early-time flux excess in our g- and r-band data (four `blue' and two `red' flux excesses). We find an intrinsic rate of 18+/-11 per cent of early flux excesses in SNe Ia at z < 0.07, based on three detected flux excesses out of 30 (10 per cent) observed SNe Ia with a simulated efficiency of 57 per cent. This is comparable to rates of flux excesses in the literature but also accounts for detection efficiencies. Two of these events are mostly consistent with CSM interaction, while the other four have longer lifetimes in agreement with companion interaction and nickel-clump models. We find a higher frequency of flux excesses in 91T/99aa-like events (44+/-13 per cent).
Published: 2022
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22. Close, bright and boxy: the superluminous SN 2018hti

Author: Fiore, A., Benetti, S., Nicholl, M., Reguitti, A., Cappellaro, E., Campana, S., Bose, S., Paraskeva, E., Berger, E., Bravo, T. M., Burke, J., Cai, Y. -Z., Chen, T. -W., Chen, P., Ciolfi, R., Dong, S., Gomez, S., Gromadzki, M., Gutiérrez, C. P., Hiramatsu, D., Hosseinzadeh, G., Howell, D. A., Jerkstrand, A., Kankare, E., Kozyreva, A., Maguire, K., McCully, C., Ochner, P., Pellegrino, C., Pignata, G., Post, R. S., Elias-Rosa, N., Shahbandeh, M., Schuldt, S., Thomas, B. P., Tomasella, L., Vinkó, J., Vogl, C., Wheeler, J. C., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: SN 2018hti was a very nearby (z=0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r-band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame days. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 Msun of circumstellar material or a magnetar with a magnetic field of B_p~1.3e13 G and initial period of P_spin~1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ~40 Msun progenitor star., Comment: 31 pages, 19 figures, replaced after acceptance by MNRAS (minor revisions compared to the previous version)
Published: 2021
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23. An analysis of the spectroscopic signatures of layering in the ejecta of type Iax supernovae

Author: Magee, M. R., Gillanders, J. H., Maguire, K., Sim, S. A., and Callan, F. P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Investigations of some type Iax supernovae have led to the suggestion that their ejecta must be layered to some degree. Such an ejecta structure has been argued as inconsistent with the well-mixed composition predicted by pure deflagrations. Based on explosion models, we create toy models in which the ejecta are artificially stratified and progressively mixed until a uniform composition is obtained. We find that models that are heavily mixed, containing burned and unburned material at all velocities, produce reasonably good agreement with SN 2012Z, for which a layered structure has been suggested. We also discuss how existing ejecta compositions determined for type Iax supernovae do not necessarily contradict pure deflagration models and may be consistent with a steeper density profile. We investigate previous claims that differences in line profile shapes may be due to strong blending, by presenting a series of models with different plasma states. These models indicate that blending could indeed explain differences in the observed profiles. Alternatively, stratification could also explain such differences, however all of our models indicate that this does not necessarily require stratification in abundance. Sufficient stratification in ionisation state can be achieved even for a well-mixed model. Based on our analysis, we demonstrate that there is insufficient evidence to suggest the ejecta of type Iax supernovae must be layered and therefore argue the pure deflagration scenario is not ruled out, even for the brightest type Iax supernovae. Our analysis does not indicate the ejecta cannot be layered to some degree, but observations within days of explosion are necessary to determine the extent to which the outer ejecta could be layered., Comment: 19 pages, 12 figures, 8 tables. Accepted for publication in MNRAS
Published: 2021
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24. Transitional events in the spectrophotometric regime between stripped envelope and superluminous supernovae

Author: Prentice, S. J., Inserra, C., Schulze, S., Nicholl, M., Mazzali, P. A., Vergani, S. D., Galbany, L., Anderson, J. P., Ashall, C., Chen, T. W., Deckers, M., Mancheño, M. Delgado, Díaz, R. González, González-Gaitán, S., Gromadzki, M., Gutiérrez, C. P., Harvey, L., Kozyreva, A., Magee, M. R., Maguire, K., Müller-Bravo, T. E., Torres, S. Muñoz, Pessi, P. J., Sollerman, J., Teffs, J., Terwel, J. H., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The division between stripped-envelope supernovae (SE-SNe) and superluminous supernovae (SLSNe) is not well defined in either photometric or spectroscopic space. While a sharp luminosity threshold has been suggested, there remains an increasing number of transitional objects that reach this threshold without the spectroscopic signatures common to SLSNe. In this work we present data and analysis on four SNe transitional between SE-SNe and SLSNe; the He-poor SNe 2019dwa and 2019cri, and the He-rich SNe 2019hge and 2019unb. Each object displays long-lived and variable photometric evolution with luminosities around the SLSN threshold of $M_r < -19.8$ mag. Spectroscopically however, these objects are similar to SE-SNe, with line velocities lower than either SE-SNe and SLSNe, and thus represent an interesting case of rare transitional events., Comment: Accepted for publication in MNRAS
Published: 2021
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25. SN 2018bsz: significant dust formation in a nearby superluminous supernova

Author: Chen, T. -W., Brennan, S. J., Wesson, R., Fraser, M., Schweyer, T., Inserra, C., Schulze, S., Nicholl, M., Anderson, J. P., Hsiao, E. Y., Jerkstrand, A., Kankare, E., Kool, E. C., Kravtsov, T., Kuncarayakti, H., Leloudas, G., Li, C. -J., Matsuura, M., Pursiainen, M., Roy, R., Ruiter, A. J., Schady, P., Seitenzahl, I., Sollerman, J., Tartaglia, L., Wang, L., Yates, R. M., Yang, S., Baade, D., Carini, R., Gal-Yam, A., Galbany, L., Gonzalez-Gaitan, S., Gromadzki, M., Gutierrez, C. P., Kotak, R., Maguire, K., Mazzali, P. A., Mueller-Bravo, T. E., Paraskeva, E., Pessi, P. J., Pignata, G., Rau, A., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We investigate the thermal emission and extinction from dust associated with the nearby superluminous supernova (SLSN) 2018bsz. Our dataset has daily cadence and simultaneous optical and near-infrared coverage up to ~ 100 days, together with late time (+ 1.7 yr) MIR observations. At 230 days after light curve peak the SN is not detected in the optical, but shows a surprisingly strong near-infrared excess, with r - J > 3 mag and r - Ks > 5 mag. The time evolution of the infrared light curve enables us to investigate if the mid-infrared emission is from newly formed dust inside the SN ejecta, from a pre-existing circumstellar envelope, or interstellar material heated by the radiation from the SN. We find the latter two scenarios can be ruled out, and a scenario where new dust is forming in the SN ejecta at epochs > 200 days can self-consistently reproduce the evolution of the SN flux. We can fit the spectral energy distribution well at +230 d with 5 x 10^-4 solar mass of carbon dust, increasing over the following several hundred days to 10^-2 solar mass by +535 d. SN 2018bsz is the first SLSN showing evidence for dust formation within the SN ejecta, and appears to form ten times more dust than normal core-collapse SNe at similar epochs. Together with their preference for low mass, low metallicity host galaxies, we suggest that SLSNe may be a significant contributor to dust formation in the early Universe., Comment: 14 pages and 7 figures in main text, 12 pages and 6 figures in appendix. The observational data will be updated once the paper is accepted
Published: 2021

26. Intermediate-luminosity red transients: Spectrophotometric properties and connection to electron-capture supernova explosions

Author: Cai, Y. -Z., Pastorello, A., Fraser, M., Botticella, M. T., Elias-Rosa, N., Wang, L. -Z., Kotak, R., Benetti, S., Cappellaro, E., Turatto, M., Reguitti, A., Mattila, S., Smartt, S. J., Ashall, C., Benitez, S., Chen, T. -W., Harutyunyan, A., Kankare, E., Lundqvist, P., Mazzali, P. A., Morales-Garoffolo, A., Ochner, P., Pignata, G., Prentice, S. J., Reynolds, T. M., Shu, X. -W., Stritzinger, M. D., Tartaglia, L., Terreran, G., Tomasella, L., Valenti, S., Valerin, G., Wang, G. -J., Wang, X. -F., Borsato, L., Callis, E., Cannizzaro, G., Chen, S., Congiu, E., Ergon, M., Galbany, L., Gal-Yam, A., Gao, X., Gromadzki, M., Holmbo, S., Huang, F., Inserra, C., Itagaki, K., Kostrzewa-Rutkowska, Z., Maguire, K., Margheim, S., Moran, S., Onori, F., Carracedo, A. Sagués, Smith, K. W., Sollerman, J., Somero, A., Wang, B., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the spectroscopic and photometric study of five intermediate-luminosity red transients (ILRTs), namely AT 2010dn, AT 2012jc, AT 2013la, AT 2013lb, and AT 2018aes. They share common observational properties and belong to a family of objects similar to the prototypical ILRT SN~2008S. These events have a rise time that is less than 15 days and absolute peak magnitudes of between $-11.5$ and $-14.5$ mag. Their pseudo-bolometric light curves peak in the range $0.5$ - $9.0 \times10^{40}~\mathrm{erg~s}^{-1}$ and their total radiated energies are on the order of (0.3 - 3) $\times$~10$^{47}$~erg. After maximum brightness, the light curves show a monotonic decline or a plateau, resembling those of faint supernovae IIL or IIP, respectively. At late phases, the light curves flatten, roughly following the slope of the $^{56}$Co decay. If the late-time power source is indeed radioactive decay, these transients produce $^{56}$Ni masses on the order of $10^{-4}$ to $10^{-3}$~\msun. The spectral energy distribution of our ILRT sample, extending from the optical to the mid-infrared (MIR) domain, reveals a clear IR excess soon after explosion and non-negligible MIR emission at very late phases. The spectra show prominent H lines in emission with a typical velocity of a few hundred km~s$^{-1}$, along with Ca~II features. In particular, the [Ca~II] $\lambda$7291,7324 doublet is visible at all times, which is a characteristic feature for this family of transients. The identified progenitor of SN~2008S, which is luminous in archival Spitzer MIR images, suggests an intermediate-mass precursor star embedded in a dusty cocoon. We propose the explosion of a super-asymptotic giant branch star forming an electron-capture supernova as a plausible explanation for these events., Comment: 31 pages, 17 figures; accepted for publication in Astronomy and Astrophysics
Published: 2021
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27. Core-collapse supernova subtypes in luminous infrared galaxies

Author: Kankare, E., Efstathiou, A., Kotak, R., Kool, E. C., Kangas, T., O'Neill, D., Mattila, S., Vaisanen, P., Ramphul, R., Mogotsi, M., Ryder, S. D., Parker, S., Reynolds, T., Fraser, M., Pastorello, A., Cappellaro, E., Mazzali, P. A., Ochner, P., Tomasella, L., Turatto, M., Kotilainen, J., Kuncarayakti, H., Perez-Torres, M. A., Randriamanakoto, Z., Romero-Canizales, C., Berton, M., Cartier, R., Chen, T. -W., Galbany, L., Gromadzki, M., Inserra, C., Maguire, K., Moran, S., Muller-Bravo, T. E., Nicholl, M., Reguitti, A., and Young, D. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the discovery and follow-up observations of two CCSNe that occurred in the luminous infrared galaxy (LIRG), NGC3256. The first, SN2018ec, was discovered using the ESO HAWK-I/GRAAL adaptive optics seeing enhancer, and was classified as a Type Ic with a host galaxy extinction of $A_V=2.1^{+0.3}_{-0.1}$ mag. The second, AT2018cux, was discovered during the course of follow-up observations of SN2018ec, and is consistent with a sub-luminous Type IIP classification with an $A_V=2.1 \pm 0.4$ mag of host extinction. A third CCSN, PSNJ10275082-4354034 in NGC3256, has previously been reported in 2014, and we recovered the source in late time archival HST imaging. Based on template light-curve fitting, we favour a Type IIn classification for it with modest host galaxy extinction of $A_V=0.3^{+0.4}_{-0.3}$ mag. We also extend our study with follow-up data of the recent Type IIb SN2019lqo and Type Ib SN2020fkb that occurred in the LIRG system Arp299 with host extinctions of $A_V=2.1^{+0.1}_{-0.3}$ and $A_V=0.4^{+0.1}_{-0.2}$ mag, respectively. Motivated by the above, we inspected, for the first time, a sample of 29 CCSNe located within a projected distance of 2.5 kpc from the host galaxy nuclei in a sample of 16 LIRGs. We find that, if star formation within these galaxies is modelled assuming a global starburst episode and normal IMF, there is evidence of a correlation between the starburst age and the CCSN subtype. We infer that the two subgroups of 14 H-poor (Type IIb/Ib/Ic/Ibn) and 15 H-rich (Type II/IIn) CCSNe have different underlying progenitor age distributions, with the H-poor progenitors being younger at 3$\sigma$ significance. However, we do note that the available sample sizes of CCSNe and host LIRGs are so far small, and the statistical comparisons between subgroups do not take into account possible systematic or model errors related to the estimated starburst ages. (abridged), Comment: 25 pages, 21 figures, accepted for publication in A&A
Published: 2021
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28. Progenitor, environment, and modelling of the interacting transient, AT 2016jbu (Gaia16cfr)

Author: Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., and van Soelen, B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the bolometric lightcurve, identification and analysis of the progenitor candidate, and preliminary modelling of AT2016jbu (Gaia16cfr). We find a progenitor consistent with a $\sim$22--25~$M_{\odot}$ yellow hypergiant surrounded by a dusty circumstellar shell, in agreement with what has been previously reported. We see evidence for significant photometric variability in the progenitor, as well as strong H$\alpha$ emission consistent with pre-existing circumstellar material. The age of the environment as well as the resolved stellar population surrounding AT2016jbu, support a progenitor age of $>$10 Myr, consistent with a progenitor mass of $\sim$22~$M_{\odot}$. A joint analysis of the velocity evolution of AT2016jbu, and the photospheric radius inferred from the bolometric lightcurve shows the transient is consistent with two successive outbursts/explosions. The first outburst ejected material with velocity $\sim$650$kms^{-1}$, while the second, more energetic event, ejected material at $\sim$4500$kms^{-1}$. Whether the latter is the core-collapse of the progenitor remains uncertain. We place a limit on the ejected $^{56}$Ni mass of $<$0.016$M_{\odot}$. Using the BPASS code, we explore a wide range of possible progenitor systems, and find that the majority of these are in binaries, some of which are undergoing mass transfer or common envelope evolution immediately prior to explosion. Finally, we use the SNEC code to demonstrate that the low-energy explosion within some of these binary systems, together with sufficient CSM, can reproduce the overall morphology of the lightcurve of AT2016jbu., Comment: 23 pages, 15 figures, accepted for publication in MNRAS
Published: 2021
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29. Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Author: Brennan, S. J., Fraser, M., Johansson, J., Pastorello, A., Kotak, R., Stevance, H. F., Chen, T. -W., Eldridge, J. J., Bose, S., Brown, P. J., Callis, E., Cartier, R., Dennefeld, M., Dong, Subo, Duffy, P., Elias-Rosa, N., Hosseinzadeh, G., Hsiao, E., Kuncarayakti, H., Martin-Carrillo, A., Monard, B., Nyholm, A., Pignata, G., Sand, D., Shappee, B. J., Smartt, S. J., Tucker, B. E., Wyrzykowski, L., Abbot, H., Benetti, S., Blondin, S., Chen, Ping, Bento, J., Delgado, A., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Hanlon, L., Harrison, D. L., Hiramatsu, D., Hodgkin, S. T., Holoien, T. W. -S., Howell, D. A., Inserra, C., Kankare, E., Kozlowski, S., Maguire, K., Müller-Bravo, T. E., McCully, C., Meintjes, P., Morrell, N., Nicholl, M., O'Neill, D., Pietrukowicz, P., Poleski, R., Prieto, J. L., Rau, A., Reichart, D. E., Schweyer, T., Shahbandeh, M., Skowron, J., Sollerman, J., Soszńyski, I., Stritzinger, M. D., Szymański, M., Tartaglia, L., Udalski, A., Ulaczyk, K., Young, D. R., van Leeuwen, M., and van Soelen, B.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results from a high cadence, multi-wavelength observation campaign of AT 2016jbu (aka Gaia16cfr), an interacting transient. This dataset complements the current literature by adding higher cadence as well as extended coverage of the lightcurve evolution and late-time spectroscopic evolution. Photometric coverage reveals that AT 2016jbu underwent significant photometric variability followed by two luminous events, the latter of which reached an absolute magnitude of M$_V\sim$-18.5 mag. This is similar to the transient SN 2009ip whose nature is still debated. Spectra are dominated by narrow emission lines and show a blue continuum during the peak of the second event. AT 2016jbu shows signatures of a complex, non-homogeneous circumstellar material (CSM). We see slowly evolving asymmetric hydrogen line profiles, with velocities of 500km$s^{-1}$ seen in narrow emission features from a slow moving CSM, and up to 10,000km$s^{-1}$ seen in broad absorption from some high velocity material. Late-time spectra ($\sim$+1 year) show a lack of forbidden emission lines expected from a core-collapse supernova and are dominated by strong emission from H, He i and Ca ii. Strong asymmetric emission features, a bumpy lightcurve, and continually evolving spectra suggest an inhibit nebular phase. We compare the evolution of H$\alpha$ among SN 2009ip-like transients and find possible evidence for orientation angle effects. The light-curve evolution of AT 2016jbu suggests similar, but not identical, circumstellar environments to other SN 2009ip-like transients., Comment: 27 pages, 21 figures, accepted for publication in MNRAS
Published: 2021
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30. Exploring the diversity of double detonation explosions for type Ia supernovae: Effects of the post-explosion helium shell composition

Author: Magee, M. R., Maguire, K., Kotak, R., and Sim, S. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The detonation of a helium shell on top of a carbon-oxygen white dwarf has been argued as a potential explosion mechanism for type Ia supernovae (SNe~Ia). The ash produced during helium shell burning can lead to light curves and spectra that are inconsistent with normal SNe~Ia, but may be viable for some objects showing a light curve bump within the days following explosion. We present a series of radiative transfer models designed to mimic predictions from double detonation explosion models. We consider a range of core and shell masses, and systematically explore multiple post-explosion compositions for the helium shell. We find that a variety of luminosities and timescales for early light curve bumps result from those models with shells containing $^{56}$Ni, $^{52}$Fe, or $^{48}$Cr. Comparing our models to SNe~Ia with light curve bumps, we find that these models can reproduce the shapes of almost all of the bumps observed, but only those objects with red colours around maximum light ($B-V \gtrsim 1$) are well matched throughout their evolution. Consistent with previous works, we also show that those models in which the shell does not contain iron-group elements provide good agreement with normal SNe~Ia of different luminosities from shortly after explosion up to maximum light. While our models do not amount to positive evidence in favour of the double detonation scenario, we show that provided the helium shell ash does not contain iron-group elements, it may be viable for a wide range of normal SNe~Ia., Comment: 21 pages, 25 figures, 1 table. Accepted for publication in MNRAS. Model light curves available at https://github.com/MarkMageeAstro/TURTLS-Light-curves
Published: 2021
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31. SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

Author: Prentice, S. J., Maguire, K., Boian, I., Groh, J., Anderson, J., Barbarino, C., Bostroem, K. A., Burke, J., Clark, P., Dong, Y., Fraser, M., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Howell, D. A., Hiramatsu, D., Inserra, C., James, P. A., Kankare, E., Kuncarayakti, H., Mazzali, P. A., McCully, C., Müller-Bravo, T. E., Nichol, M., Pellegrino, C., Smartt, S. J., Sollerman, J., Tartaglia, L., Valenti, S., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the data and analysis of SN 2018gjx, an unusual low-luminosity transient with three distinct spectroscopic phases. Phase I shows a hot blue spectrum with signatures of ionised circumstellar material (CSM), Phase II has the appearance of broad SN features, consistent with those seen in a Type IIb supernova at maximum light, and Phase III is that of a supernova interacting with helium-rich CSM, similar to a Type Ibn supernova. This event provides an apparently rare opportunity to view the inner workings of an interacting supernova. The observed properties can be explained by the explosion of a star in an aspherical CSM. The initial light is emitted from an extended CSM (~ 4000 Rsun), which ionises the exterior unshocked material. Some days after, the SN photosphere envelops this region, leading to the appearance of a SN IIb. Over time, the photosphere recedes in velocity space, revealing interaction between the supernova ejecta and the CSM that partially obscures the supernova nebular phase. Modelling of the initial spectrum reveals a surface composition consistent with compact H-deficient Wolf-Rayet and LBV stars. Such configurations may not be unusual, with SNe IIb being known to have signs of interaction so at least some SNe IIb and SNe Ibn may be the same phenomena viewed from different angles or, possibly with differing CSM configurations., Comment: Accepted for publication in MNRAS
Published: 2020
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32. SN 2017ivv: two years of evolution of a transitional Type II supernova

Author: Gutiérrez, C. P., Pastorello, A., Jerkstrand, A., Galbany, L., Sullivan, M., Anderson, J. P., Taubenberger, S., Kuncarayakti, H., González-Gaitán, S., Wiseman, P., Inserra, C., Fraser, M., Maguire, K., Smartt, S., Müller-Bravo, T. E., Arcavi, I., Benetti, S., Bersier, D., Bose, S., Bostroem, K. A., Burke, J., Chen, P., Chen, T. -W., Della Valle, M., Dong, Subo, Gal-Yam, A., Gromadzki, M., Hiramatsu, D., Holoien, T. W. -S., Hosseinzadeh, G., Howell, D. A., Kankare, E., Kochanek, C. S., McCully, C., Nicholl, M., Pignata, G., Prieto, J. L., Shappee, B., Taggart, K., Tomasella, L., Valenti, S., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the photometric and spectroscopic evolution of the Type II supernova (SN II) SN 2017ivv (also known as ASASSN-17qp). Located in an extremely faint galaxy (M$_r=-10.3$ mag), SN 2017ivv shows an unprecedented evolution during the two years of observations. At early times, the light curve shows a fast rise ($\sim6-8$ days) to a peak of ${\rm M}^{\rm max}_{g}= -17.84$ mag, followed by a very rapid decline of $7.94\pm0.48$ mag per 100 days in the $V-$band. The extensive photometric coverage at late phases shows that the radioactive tail has two slopes, one steeper than that expected from the decay of $^{56}$Co (between 100 and 350 days), and another slower (after 450 days), probably produced by an additional energy source. From the bolometric light curve, we estimated that the amount of ejected $^{56}$Ni is $\sim0.059\pm0.003$ M$\odot$. The nebular spectra of SN 2017ivv show a remarkable transformation that allows the evolution to be split into three phases: (1) H$\alpha$ strong phase ($<200$ days); (2) H$\alpha$ weak phase (between 200 and 350 days); and (3) H$\alpha$ broad phase ($>500$ days). We find that the nebular analysis favours a binary progenitor and an asymmetric explosion. Finally, comparing the nebular spectra of SN 2017ivv to models suggests a progenitor with a zero-age main-sequence mass of 15 -- 17 \Msun., Comment: Accepted for publication in MNRAS
Published: 2020
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33. An investigation of $^{56}$Ni shells as the source of early light curve bumps in type Ia supernovae

Author: Magee, M. R. and Maguire, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: An excess of flux (i.e. a bump) in the early light curves of type Ia supernovae has been observed in a handful of cases. Multiple scenarios have been proposed to explain this. It has been shown that for at least one object (SN~2018oh) the excess emission observed could be the result of a large amount of $^{56}$Ni in the outer ejecta ($\sim$0.03~$M_{\rm{\odot}}$). We present a series of model light curves and spectra for ejecta profiles containing $^{56}$Ni shells of varying masses (0.01, 0.02, 0.03, and 0.04~$M_{\rm{\odot}}$) and widths. We find that even for our lowest mass $^{56}$Ni shell, an increase of \textgreater2 magnitudes is produced in the bolometric light curve at one day after explosion relative to models without a $^{56}$Ni shell. We show that the colour evolution of models with a $^{56}$Ni shell differs significantly from those without and shows a colour inversion similar to some double-detonation explosions. Spectra of our $^{56}$Ni shell models show that strong suppression of flux between $\sim$3\,700 -- 4\,000~$\AA$ close to maximum light appears to be a generic feature for this class of model. Comparing our models to observations of SNe~2017cbv and 2018oh, we show that a $^{56}$Ni shell of 0.02 -- 0.04~$M_{\rm{\odot}}$ can match shapes of the early optical light curve bumps, but the colour and spectral evolution are in disagreement. This would indicate that an alternative origin for the flux excess is necessary. Based on existing explosion scenarios, producing such a $^{56}$Ni shell in the outer ejecta as required to match the light curve shape, without the presence of additional short-lived radioactive material, may prove challenging. Given that only a small amount of $^{56}$Ni in the outer ejecta is required to produce a bump in the light curve, such non-monotonically decreasing $^{56}$Ni distributions in the outer ejecta must be rare, if they were to occur at all., Comment: 14 pages, 11 figures. Updated to match version published in A&A. Model light curves available at https://github.com/MarkMageeAstro/TURTLS-Light-curves
Published: 2020
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34. Observation of inverse Compton emission from a long $\gamma$-ray burst

Author: Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinović, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Loporchio, S., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mićanović, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nozaki, S., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., Vagelli, V., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., Nava, L., Veres, P., Bhat, P. N., Briggs, M. S., Cleveland, W. H., Hamburg, R., Hui, C. M., Mailyan, B., Preece, R. D., Roberts, O., von Kienlin, A., Wilson-Hodge, C. A., Kocevski, D., Arimoto, M., Tak, D., Asano, K., Axelsson, M., Barbiellini, G., Bissaldi, E., Dirirsa, F. Fana, Gill, R., Granot, J., McEnery, J., Razzaque, S., Piron, F., Racusin, J. L., Thompson, D. J., Campana, S., Bernardini, M. G., Kuin, N. P. M., Siegel, M. H., Cenko, S. Bradley, O'Brien, P., Capalbi, M., D'Aì, A., De Pasquale, M., Gropp, J., Klingler, N., Osborne, J. P., Perri, M., Starling, R., Tagliaferri, G., Tohuvavohu, A., Ursi, A., Tavani, M., Cardillo, M., Casentini, C., Piano, G., Evangelista, Y., Verrecchia, F., Pittori, C., Lucarelli, F., Bulgarelli, A., Parmiggiani, N., Anderson, G. E., Anderson, J. P., Bernardi, G., Bolmer, J., Caballero-García, M. D., Carrasco, I. M., Castellón, A., Segura, N. Castro, Castro-Tirado, A. J., Cherukuri, S. V., Cockeram, A. M., D'Avanzo, P., Di Dato, A., Diretse, R., Fender, R. P., Fernández-García, E., Fynbo, J. P. U., Fruchter, A. S., Greiner, J., Gromadzki, M., Heintz, K. E., Heywood, I., van der Horst, A. J., Hu, Y. -D., Inserra, C., Izzo, L., Jaiswal, V., Jakobsson, P., Japelj, J., Kankare, E., Kann, D. A., Kouveliotou, C., Klose, S., Levan, A. J., Li, X. Y., Lotti, S., Maguire, K., Malesani, D. B., Manulis, I., Marongiu, M., Martin, S., Melandri, A., Michałowski, M., Miller-Jones, J. C. A., Misra, K., Moin, A., Mooley, K. P., Nasri, S., Nicholl, M., Noschese, A., Novara, G., Pandey, S. B., Peretti, E., del Pulgar, C. J. Pérez, Pérez-Torres, M. A., Perley, D. A., Piro, L., Ragosta, F., Resmi, L., Ricci, R., Rossi, A., Sánchez-Ramírez, R., Selsing, J., Schulze, S., Smartt, S. J., Smith, I. A., Sokolov, V. V., Stevens, J., Tanvir, N. R., Thóne, C. C., Tiengo, A., Tremou, E., Troja, E., Postigo, A. de Ugarte, Vergani, S. D., Wieringa, M., Woudt, P. A., Xu, D., Yaron, O., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Long-duration gamma-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterised by an initial phase of bright and highly variable radiation in the keV-MeV band that is likely produced within the jet and lasts from milliseconds to minutes, known as the prompt emission. Subsequently, the interaction of the jet with the external medium generates external shock waves, responsible for the afterglow emission, which lasts from days to months, and occurs over a broad energy range, from the radio to the GeV bands. The afterglow emission is generally well explained as synchrotron radiation by electrons accelerated at the external shock. Recently, an intense, long-lasting emission between 0.2 and 1 TeV was observed from the GRB 190114C. Here we present the results of our multi-frequency observational campaign of GRB~190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from $5\times10^{-6}$ up to $10^{12}$\,eV. We find that the broadband spectral energy distribution is double-peaked, with the TeV emission constituting a distinct spectral component that has power comparable to the synchrotron component. This component is associated with the afterglow, and is satisfactorily explained by inverse Compton upscattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed TeV component are not atypical, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
Published: 2020
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35. Search for $CP$ violation in $\Xi_c^+\rightarrow pK^-\pi^+$ decays using model-independent techniques

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Basels, J. M., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertella, C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Birnkraut, A., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Boubdir, M., Bowcock, T. J. V., Bozzi, C., Bradley, M. J., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Büchler-Germann, A., Buonaura, A., Burr, C., Bursche, A., Butkevich, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Diaz, L. Calero, Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Magalhaes, P. Camargo, Camboni, A., Campana, P., Perez, D. H. Campora, Quezada, A. F. Campoverde, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carli, I., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Celani, S., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Cholak, S., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Cowan, G. A., Craik, D. C., Crkovská, J., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dobishuk, V., Dordei, F., Dorigo, M., Reis, A. C. dos, Suárez, A. Dosil, Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ekelhof, R., Ek-In, S., Eklund, L., Ely, S., Ene, A., Epple, E., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Fan, Y., Farley, N., Farry, S., Fazzini, D., Fedin, P., Féo, M., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferrillo, M., Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Fuehring, Q., Funk, W., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Pardiñas, J. García, Plana, B. Garcia, Rosales, F. A. Garcia, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gazzoni, G., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Göbel, C., Golobardes, E., Golubkov, D., Golutvin, A., Gomes, A., Gorbounov, P., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Günther, P. A., Guo, X., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Hadavizadeh, T., Hadjivasiliou, C., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., Heß, M., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Huard, Z. C., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Karodia, S., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Khurewathanakul, C., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Korolev, M., Kostiuk, I., Kot, O., Kotriakhova, S., Kozeiha, M., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Lantwin, O., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Lefèvre, R., Leflat, A., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, L., Li, P. -R., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Ling, P., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lu, Y., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Ma, R., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meier, G., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Michielin, E., Mikhasenko, M., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mödden, A., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Müller, D., Müller, J., Müller, K., Müller, V., Murphy, C. H., Murray, D., Muzzetto, P., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Nunez, C., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., O'Hanlon, D. P., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Penso, G., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Trejo, R. I. Rabadan, Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, D. S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzhikov, A., Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Sahoo, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shchutska, L., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. Silva, Simi, G., Simone, S., Skiba, I., Skidmore, N., Skwarnicki, T., Slater, M. W., Smeaton, J. G., Smetkina, A., Smith, E., Smith, I. T., Smith, M., Snoch, A., Soares, M., Lavra, L. Soares, Sokoloff, M. D., Soler, F. J. P., De Paula, B. Souza, Spaan, B., Norella, E. Spadaro, Spradlin, P., Stagni, F., Stahl, M., Stahl, S., Stefko, P., Stefkova, S., Steinkamp, O., Stemmle, S., Stenyakin, O., Stepanova, M., Stevens, H., Stone, S., Stracka, S., Stramaglia, M. E., Straticiuc, M., Straumann, U., Strokov, S., Sun, J., Sun, L., Sun, Y., Svihra, P., Swientek, K., Szabelski, A., Szumlak, T., Szymanski, M., Taneja, S., Tang, Z., Tekampe, T., Tellarini, G., Teubert, F., Thomas, E., Thomson, K. A., Tilley, M. J., Tisserand, V., T'Jampens, S., Tobin, M., Tolk, S., Tomassetti, L., Tonelli, D., Machado, D. Torres, Tou, D. Y., Tournefier, E., Traill, M., Tran, M. T., Trifonova, E., Trippl, C., Trisovic, A., Tsaregorodtsev, A., Tuci, G., Tully, A., Tuning, N., Ukleja, A., Usachov, A., Ustyuzhanin, A., Uwer, U., Vagner, A., Vagnoni, V., Valassi, A., Valat, S., Valenti, G., van Beuzekom, M., Van Hecke, H., van Herwijnen, E., Van Hulse, C. B., van Tilburg, J., van Veghel, M., Gomez, R. Vazquez, Regueiro, P. Vazquez, Sierra, C. Vázquez, Vecchi, S., Velthuis, J. J., Veltri, M., Venkateswaran, A., Vernet, M., Veronesi, M., Vesterinen, M., Barbosa, J. V. Viana, Vieira, D., Diaz, M. Vieites, Viemann, H., Vilasis-Cardona, X., Vitkovskiy, A., Vollhardt, A., Bruch, D. Vom, Voneki, B., Vorobyev, A., Vorobyev, V., Voropaev, N., Waldi, R., Walsh, J., Wang, J., Wang, M., Wang, Y., Wang, Z., Ward, D. R., Wark, H. M., Watson, N. K., Websdale, D., Weiden, A., Weisser, C., Westhenry, B. D. C., White, D. J., Whitehead, M., Wiedner, D., Wilkinson, G., Wilkinson, M., Williams, I., Williams, M., Williams, M. R. J., Williams, T., Wilson, F. F., Winn, M., Wislicki, W., Witek, M., Witola, L., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, J., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: A first search for $CP$ violation in the Cabibbo-suppressed $\Xi_c^+\rightarrow pK^-\pi^+$ decay is performed using both a binned and an unbinned model-independent technique in the Dalitz plot. The studies are based on a sample of proton-proton collision data, corresponding to an integrated luminosity of $3.0~{\rm fb^{-1}}$, and collected by the LHCb experiment at centre-of-mass energies of $7$ and $8~\rm TeV$. The data are consistent with the hypothesis of no $CP$ violation., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-026.html (LHCb public pages)
Published: 2020
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36. The Spectacular Ultraviolet Flash From the Peculiar Type Ia Supernova 2019yvq

Author: Miller, A. A., Magee, M. R., Polin, A., Maguire, K., Zimmerman, E., Yao, Y., Sollerman, J., Schulze, S., Perley, D. A., Kromer, M., Bulla, M., Andreoni, I., Bellm, E. C., De, K., Dekany, R., Delacroix, A., Dhawan, S., Fremling, C., Gal-Yam, A., Goldstein, D. A., Golkhou, V. Z., Goobar, A., Graham, M. J., Irani, I., Kasliwal, M. M., Kaye, S., Kim, Y. -L., Laher, R. R., Mahabal, A. A., Masci, F. J., Nugent, P. E., Ofek, E., Phinney, E. S., Prentice, S. J., Riddle, R., Rigault, M., Rusholme, B., Schweyer, T., Shupe, D. L., Soumagnac, M. T., Terreran, G., Walters, R., Yan, L., Zolkower, J., and Kulkarni, S. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Early observations of Type Ia supernovae (SNe$\,$Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN$\,$2019yvq, the second observed SN$\,$Ia, after iPTF$\,$14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN$\,$2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN$\,$Ia ($M_g \approx -18.5\,$mag at peak) yet featured very high absorption velocities ($v \approx 15,000\,\mathrm{km\,s}^{-1}$ for Si II $\lambda$6355 at peak). We find that many of the observational features of SN$\,$2019yvq, aside from the flash, can be explained if the explosive yield of radioactive $^{56}\mathrm{Ni}$ is relatively low (we measure $M_{^{56}\mathrm{Ni}} = 0.31 \pm 0.05\,M_\odot$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN$\,$2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of $^{56}\mathrm{Ni}$ in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN$\,$2019yvq. In closing, we predict that the nebular spectra of SN$\,$2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger., Comment: 27 pages, 14 figures, accepted in ApJ
Published: 2020
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37. The Tidal Disruption Event AT 2018hyz I: Double-peaked emission lines and a flat Balmer decrement

Author: Short, P., Nicholl, M., Lawrence, A., Gomez, S., Arcavi, I., Wevers, T., Leloudas, G., Schulze, S., Anderson, J. P., Berger, E., Blanchard, P. K., Burke, J., Segura, N. Castro, Charalampopoulos, P., Chornock, R., Galbany, L., Gromadzki, M., Herzog, L. J., Hiramatsu, D., Horne, Keith, Hosseinzadeh, G., Howell, D. Andrew, Ihanec, N., Inserra, C., Kankare, E., Maguire, K., McCully, C., Bravo, T. E. Müller, Onori, F., Sollerman, J., and Young, D. R.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present results from spectroscopic observations of AT 2018hyz, a transient discovered by the ASAS-SN survey at an absolute magnitude of $M_V\sim -20.2$ mag, in the nucleus of a quiescent galaxy with strong Balmer absorption lines. AT 2018hyz shows a blue spectral continuum and broad emission lines, consistent with previous TDE candidates. High cadence follow-up spectra show broad Balmer lines and He I in early spectra, with He II making an appearance after $\sim70-100$ days. The Balmer lines evolve from a smooth broad profile, through a boxy, asymmetric double-peaked phase consistent with accretion disc emission, and back to smooth at late times. The Balmer lines are unlike typical AGN in that they show a flat Balmer decrement (H$\alpha$/H$\beta\sim1.5$), suggesting the lines are collisionally excited rather than being produced via photo-ionisation. The flat Balmer decrement together with the complex profiles suggest that the emission lines originate in a disc chromosphere, analogous to those seen in cataclysmic variables. The low optical depth of material due to a possible partial disruption may be what allows us to observe these double-peaked, collisionally excited lines. The late appearance of He II may be due to an expanding photosphere or outflow, or late-time shocks in debris collisions., Comment: Published in MNRAS. Accompanied by companion paper Gomez et al. (2020)
Published: 2020
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38. Measurement of the branching fraction of the decay $B_s^0\to K_S^0 K_S^0$

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Büchler-Germann, A., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Craik, D. C., Crkovská, J., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dordei, F., Dorigo, M., Reis, A. C. dos, Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dufour, L., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ekelhof, R., Ek-In, S., Eklund, L., Ely, S., Ene, A., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Farley, N., Farry, S., Fazzini, D., Féo, M., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferrillo, M., Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Fuehring, Q., Funk, W., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Pardiñas, J. García, Plana, B. Garcia, Rosales, F. A. Garcia, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Göbel, C., Golobardes, E., Golubkov, D., Golutvin, A., Gomes, A., Gorbounov, P., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Hadavizadeh, T., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hollitt, S., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Huard, Z. C., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Korolev, M., Kostiuk, I., Kot, O., Kotriakhova, S., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Lefèvre, R., Leflat, A., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lu, Y., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meier, G., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Mikhasenko, M., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mödden, A., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Müller, D., Müller, K., Müller, V., Murphy, C. H., Murray, D., Muzzetto, P., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., O'Hanlon, D. P., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Trejo, R. I. Rabadan, Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. Silva, Simi, G., Simone, S., Skiba, I., Skidmore, N., Skwarnicki, T., Slater, M. W., Smeaton, J. G., Smetkina, A., Smith, E., Smith, I. T., Smith, M., Snoch, A., Soares, M., Lavra, L. Soares, Sokoloff, M. D., Soler, F. J. P., De Paula, B. Souza, Spaan, B., Norella, E. Spadaro, Spradlin, P., Stagni, F., Stahl, M., Stahl, S., Stefko, P., Stefkova, S., Steinkamp, O., Stemmle, S., Stenyakin, O., Stepanova, M., Stevens, H., Stone, S., Stracka, S., Stramaglia, M. E., Straticiuc, M., Strokov, S., Sun, J., Sun, L., Sun, Y., Svihra, P., Swientek, K., Szabelski, A., Szumlak, T., Szymanski, M., Taneja, S., Tang, Z., Tekampe, T., Tellarini, G., Teubert, F., Thomas, E., Thomson, K. A., Tilley, M. J., Tisserand, V., T'Jampens, S., Tobin, M., Tolk, S., Tomassetti, L., Tonelli, D., Tou, D. Y., Tournefier, E., Traill, M., Tran, M. T., Trisovic, A., Tsaregorodtsev, A., Tuci, G., Tully, A., Tuning, N., Ukleja, A., Usachov, A., Ustyuzhanin, A., Uwer, U., Vagner, A., Vagnoni, V., Valassi, A., Valenti, G., van Beuzekom, M., Van Hecke, H., van Herwijnen, E., Van Hulse, C. B., van Tilburg, J., van Veghel, M., Gomez, R. Vazquez, Regueiro, P. Vazquez, Sierra, C. Vázquez, Vecchi, S., Velthuis, J. J., Veltri, M., Venkateswaran, A., Vernet, M., Veronesi, M., Vesterinen, M., Barbosa, J. V. Viana, Vieira, D., Diaz, M. Vieites, Viemann, H., Vilasis-Cardona, X., Vitkovskiy, A., Vollhardt, A., Bruch, D. Vom, Vorobyev, A., Vorobyev, V., Voropaev, N., Waldi, R., Walsh, J., Wang, J., Wang, M., Wang, Y., Wang, Z., Ward, D. R., Wark, H. M., Watson, N. K., Websdale, D., Weiden, A., Weisser, C., Westhenry, B. D. C., White, D. J., Whitehead, M., Wiedner, D., Wilkinson, G., Wilkinson, M., Williams, I., Williams, M., Williams, M. R. J., Williams, T., Wilson, F. F., Winn, M., Wislicki, W., Witek, M., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: A measurement of the branching fraction of the decay $B_s^0 \to K_S^0 K_S^0$ is performed using proton-proton collision data corresponding to an integrated luminosity of 5 $fb^{-1}$ collected by the LHCb experiment between 2011 and 2016. The branching fraction is determined to be BR($B_s^0 \to K_S^0 K_S^0$) = [8.3 $\pm$ 1.6 (stat) $\pm$ 0.9 (syst) $\pm$ 0.8 (norm) $\pm$ 0.3 ($f_s/f_d$)] $\times 10^{-6}$ , where the first uncertainty is statistical, the second is systematic, and the third and fourth are due to uncertainties on the branching fraction of the normalization mode $B^0 \to \phi K_S^0$ and the ratio of hadronization fractions $f_s/f_d$. This is the most precise measurement of this branching fraction to date. Furthermore, a measurement of the branching fraction of the decay $B^0 \to K_S^0 K_S^0$ is performed relative to that of the $B_s^0 \to K_S^0 K_S^0$ channel, and is found to be $\frac{BR(B^0 \to K_S^0 K_S^0)}{BR(B_s^0 \to K_S^0 K_S^0)}$ = [7.5 $\pm$ 3.1 (stat) $\pm$ 0.5 (syst) $\pm$ 0.3 ($f_s/f_d$)] $\times 10^{-2}$., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-030.html
Published: 2020
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39. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv

Author: Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, M., Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, T. -W., Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F. I., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., González-Fernández, C., González-Gaitán, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutiérrez, C. P., Heikkilä, T., Heintz, K. E., Hjorth, J., Hu, Y. -D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, A., Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, E. C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michałowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Guelbenzu, A. Nicuesa, Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vásquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, S., Sabha, N. B., Carracedo, A. Sagués, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, T., Smartt, S. J., Smith, K. W., Smith, M., Sollerman, J., Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, S., Yi, S. -X., and Young, D. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical/near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS and VINROUGE projects also carried out a search on this event. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN) possibly generated by this NS-BH merger, and for the strategy of future searches. Altogether, our observations allow us to exclude a KN with large ejecta mass $M\gtrsim 0.1\,\mathrm{M_\odot}$ to a high ($>90\%$) confidence, and we can exclude much smaller masses in a subsample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundreds Mpc will be detected only by large facilities with both high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event., Comment: 52 pages, revised version now accepted for publication in A&A. Abstract abridged to meet arXiv requirements
Published: 2020
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40. DES16C3cje: A low-luminosity, long-lived supernova

Author: Gutiérrez, C. P., Sullivan, M., Martinez, L., Bersten, M. C., Inserra, C., Smith, M., Anderson, J. P., Pan, Y. -C., Pastorello, A., Galbany, L., Nugent, P., Angus, C. R., Barbarino, C., Chen, T. -W., Davis, T. M., Della Valle, M., Foley, R. J., Fraser, M., Frohmaier, C., González-Gaitán, S., Lewis, G. F., Gromadzki, M., Kankare, E., Kokotanekova, R., Kollmeier, J., Magee, M. R., Maguire, K., Möller, A., Morrell, N., Nicholl, M., Pursiainen, M., Sollerman, J., Sommer, N. E., Swann, E., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morganson, E., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., and Wilkinson, R.
Subjects: High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of $\lesssim1500$ km s$^{-1}$, and the light curve shows an initial peak that fades after 50 days before slowly rebrightening over a further 100 days to reach an absolute brightness of M$_r\sim -15.5$ mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of $^{56}$Co but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either i) a low explosion energy (0.11 foe) and relatively large $^{56}$Ni production of 0.075 M$_{\odot}$ from a $\sim15$ M$_{\odot}$ red supergiant progenitor typical of other SNe II, or ii) a relatively compact $\sim40$ M$_{\odot}$ star, explosion energy of 1 foe, and 0.08 M$_{\odot}$ of $^{56}$Ni. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of $\sim0.5\times{10^{-8}}$ M$_{\odot}$ s$^{-1}$., Comment: Accepted in MNRAS. 17 pages, 6 figures
Published: 2020
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41. The Palomar Transient Factory Core-collapse Supernova Host-galaxy Sample. I. Host-galaxy Distribution Functions and Environment Dependence of Core-collapse Supernovae

Author: Schulze, S, Yaron, O, Sollerman, J, Leloudas, G, Gal, A, Wright, AH, Lunnan, R, Gal-Yam, A, Ofek, EO, Perley, DA, Filippenko, AV, Kasliwal, MM, Kulkarni, SR, Neill, JD, Nugent, PE, Quimby, RM, Sullivan, M, Strotjohann, NL, Arcavi, I, Ben-Ami, S, Bianco, F, Bloom, JS, De, K, Fraser, M, Fremling, CU, Horesh, A, Johansson, J, Kelly, PL, Knežević, N, Knežević, S, Maguire, K, Nyholm, A, Papadogiannakis, S, Petrushevska, T, Rubin, A, Yan, L, Yang, Y, Adams, SM, Bufano, F, Clubb, KI, Foley, RJ, Green, Y, Harmanen, J, Ho, AYQ, Hook, IM, Hosseinzadeh, G, Howell, DA, Kong, AKH, Kotak, R, Matheson, T, McCully, C, Milisavljevic, D, Pan, YC, Poznanski, D, Shivvers, I, Van Velzen, S, and Verbeek, KK
Subjects: Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: Several thousand core-collapse supernovae (CCSNe) of different flavors have been discovered so far. However, identifying their progenitors has remained an outstanding open question in astrophysics. Studies of SN host galaxies have proven to be powerful in providing constraints on the progenitor populations. In this paper, we present all CCSNe detected between 2009 and 2017 by the Palomar Transient Factory. This sample includes 888 SNe of 12 distinct classes out to redshift z ≈ 1. We present the photometric properties of their host galaxies from the far-ultraviolet to the mid-infrared and model the host-galaxy spectral energy distributions to derive physical properties. The galaxy mass function of Type Ic, Ib, IIb, II, and IIn SNe ranges from 105 to 1011.5 M o˙, probing the entire mass range of star-forming galaxies down to the least-massive star-forming galaxies known. Moreover, the galaxy mass distributions are consistent with models of star-formation-weighted mass functions. Regular CCSNe are hence direct tracers of star formation. Small but notable differences exist between some of the SN classes. Type Ib/c SNe prefer galaxies with slightly higher masses (i.e., higher metallicities) and star formation rates than Type IIb and II SNe. These differences are less pronounced than previously thought. H-poor superluminous supernovae (SLSNe) and SNe Ic-BL are scarce in galaxies above 1010 M o˙. Their progenitors require environments with metallicities of < 0.4 and < 1 solar, respectively. In addition, the hosts of H-poor SLSNe are dominated by a younger stellar population than all other classes of CCSNe. Our findings corroborate the notion that low metallicity and young age play an important role in the formation of SLSN progenitors.
Published: 2021

42. Search for $C\!P$ violation and observation of $P$ violation in $\Lambda_b^0 \to p \pi^- \pi^+ \pi^-$ decays

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Birnkraut, A., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Büchler-Germann, A., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Craik, D. C., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dordei, F., Dorigo, M., Reis, A. C. dos, Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dufour, L., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ekelhof, R., Ek-In, S., Eklund, L., Ely, S., Ene, A., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Farley, N., Farry, S., Fazzini, D., Féo, M., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Fuehring, Q., Funk, W., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Pardiñas, J. García, Plana, B. Garcia, Rosales, F. A. Garcia, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Göbel, C., Golobardes, E., Golubkov, D., Golutvin, A., Gomes, A., Gorbounov, P., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Hadavizadeh, T., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Huard, Z. C., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Korolev, M., Kostiuk, I., Kot, O., Kotriakhova, S., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Lefèvre, R., Leflat, A., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, P. -R., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mödden, A., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Müller, D., Müller, J., Müller, K., Müller, V., Murphy, C. H., Murray, D., Muzzetto, P., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., O'Hanlon, D. P., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Penso, G., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. Silva, Simi, G., Simone, S., Skiba, I., Skidmore, N., Skwarnicki, T., Slater, M. W., Smeaton, J. G., Smith, E., Smith, I. T., Smith, M., Snoch, A., Soares, M., Lavra, L. Soares, Sokoloff, M. D., Soler, F. J. P., De Paula, B. Souza, Spaan, B., Norella, E. Spadaro, Spradlin, P., Stagni, F., Stahl, M., Stahl, S., Stefko, P., Stefkova, S., Steinkamp, O., Stemmle, S., Stenyakin, O., Stepanova, M., Stevens, H., Stone, S., Stracka, S., Stramaglia, M. E., Straticiuc, M., Straumann, U., Strokov, S., Sun, J., Sun, L., Sun, Y., Svihra, P., Swientek, K., Szabelski, A., Szumlak, T., Szymanski, M., Taneja, S., Tang, Z., Tekampe, T., Tellarini, G., Teubert, F., Thomas, E., Thomson, K. A., Tilley, M. J., Tisserand, V., T'Jampens, S., Tobin, M., Tolk, S., Tomassetti, L., Tonelli, D., Tou, D. Y., Tournefier, E., Traill, M., Tran, M. T., Trisovic, A., Tsaregorodtsev, A., Tuci, G., Tully, A., Tuning, N., Ukleja, A., Usachov, A., Ustyuzhanin, A., Uwer, U., Vagner, A., Vagnoni, V., Valassi, A., Valenti, G., van Beuzekom, M., Van Hecke, H., van Herwijnen, E., Van Hulse, C. B., van Tilburg, J., van Veghel, M., Gomez, R. Vazquez, Regueiro, P. Vazquez, Sierra, C. Vázquez, Vecchi, S., Velthuis, J. J., Veltri, M., Venkateswaran, A., Vernet, M., Veronesi, M., Vesterinen, M., Barbosa, J. V. Viana, Vieira, D., Diaz, M. Vieites, Viemann, H., Vilasis-Cardona, X., Vitkovskiy, A., Vollhardt, A., Bruch, D. Vom, Vorobyev, A., Vorobyev, V., Voropaev, N., Waldi, R., Walsh, J., Wang, J., Wang, M., Wang, Y., Wang, Z., Ward, D. R., Wark, H. M., Watson, N. K., Websdale, D., Weiden, A., Weisser, C., Westhenry, B. D. C., White, D. J., Whitehead, M., Wiedner, D., Wilkinson, G., Wilkinson, M., Williams, I., Williams, M., Williams, M. R. J., Williams, T., Wilson, F. F., Winn, M., Wislicki, W., Witek, M., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: A search for $C\!P$ violation in the $\Lambda_b^0 \to p \pi^- \pi^+ \pi^-$ decay is performed using LHCb data corresponding to an integrated luminosity of 6.6$\,fb^{-1}$ collected in $pp$ collisions at centre-of-mass energies of 7, 8 and 13$\,Te\kern -0.1em V$. The analysis uses both triple product asymmetries and the unbinned energy test method. The highest significances of $C\!P$ asymmetry are 2.9 standard deviations from triple product asymmetries and 3.0 standard deviations for the energy test method. Once the global $p$-value is considered, all results are consistent with no $C\!P$ violation. Parity violation is observed at a significance of $5.5$ standard deviations for the triple product asymmetry method and $5.3$ standard deviations for the energy test method., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-028.html (LHCb public pages)
Published: 2019
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43. Determining the $^{56}$Ni distribution of type Ia supernovae from observations within days of explosion

Author: Magee, M. R., Maguire, K., Kotak, R., Sim, S. A., Gillanders, J. H., Prentice, S. J., and Skillen, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Recent studies have shown how the distribution of $^{56}$Ni within the ejecta of type Ia supernovae can have profound consequences on the observed light curves. Observations at early times can therefore provide important details on the explosion physics in thermonuclear supernovae. We present a series of radiative transfer calculations that explore variations in the $^{56}$Ni distribution. Our models also show the importance of the density profile in shaping the light curve, which is often neglected in the literature. Using our model set, we investigate the observations that are necessary to determine the $^{56}$Ni distribution as robustly as possible within the current model set. We find that this includes observations beginning at least $\sim$14 days before $B$-band maximum, extending to approximately maximum light with a high ($\lesssim$3 day) cadence, and in at least one blue and one red band are required (such as $B$ and $R$, or $g$ and $r$). We compare a number of well-observed type Ia supernovae that meet these criteria to our models and find that the light curves of $\sim$70-80\% of objects in our sample are consistent with being produced solely by variations in the $^{56}$Ni distributions. The remaining supernovae show an excess of flux at early times, indicating missing physics that is not accounted for within our model set, such as an interaction or the presence of short-lived radioactive isotopes. Comparing our model light curves and spectra to observations and delayed detonation models demonstrates that while a somewhat extended $^{56}$Ni distribution is necessary to reproduce the observed light curve shape, this does not negatively affect the spectra at maximum light. Investigating current explosion models shows that observations typically require a shallower decrease in the $^{56}$Ni mass towards the outer ejecta than is produced for models of a given $^{56}$Ni mass., Comment: 31 pages, 32 figures, 2 tables. Accepted for publication in A&A. Model light curves available at https://github.com/MarkMageeAstro/TURTLS-Light-curves
Published: 2019
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44. Monte Carlo radiative transfer for the nebular phase of Type Ia supernovae

Author: Shingles, L. J., Sim, S. A., Kromer, M., Maguire, K., Bulla, M., Collins, C., Ballance, C. P., Michel, A. S., Ramsbottom, C. A., Roepke, F. K., Seitenzahl, I. R., and Tyndall, N. B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We extend the range of validity of the ARTIS 3D radiative transfer code up to hundreds of days after explosion, when Type Ia supernovae are in their nebular phase. To achieve this, we add a non-local thermodynamic equilibrium (non-LTE) population and ionisation solver, a new multi-frequency radiation field model, and a new atomic dataset with forbidden transitions. We treat collisions with non-thermal leptons resulting from nuclear decays to account for their contribution to excitation, ionisation, and heating. We validate our method with a variety of tests including comparing our synthetic nebular spectra for the well-known one-dimensional W7 model with the results of other studies. As an illustrative application of the code, we present synthetic nebular spectra for the detonation of a sub-Chandrasekhar white dwarf in which the possible effects of gravitational settling of Ne22 prior to explosion have been explored. Specifically, we compare synthetic nebular spectra for a 1.06 M$_\odot$ white dwarf model obtained when 5.5 Gyr of very-efficient settling is assumed to a similar model without settling. We find that this degree of Ne22 settling has only a modest effect on the resulting nebular spectra due to increased Ni58 abundance. Due to the high ionisation in sub-Chandrasekhar models, the nebular [Ni II] emission remains negligible, while the [Ni III] line strengths are increased and the overall ionisation balance is slightly lowered in the model with Ne22 settling. In common with previous studies of sub-Chandrasekhar models at nebular epochs, these models overproduce [Fe III] emission relative to [Fe II] in comparison to observations of normal Type Ia supernovae., Comment: 15 pages, 12 figures. Accepted for publication by MNRAS
Published: 2019
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45. Determination of quantum numbers for several excited charmed mesons observed in $B^- \to D^{*+} \pi^- \pi^-$ decays

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Birnkraut, A., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Boubdir, M., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Cowan, G. A., Craik, D. C., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dordei, F., Dorigo, M., Reis, A. C. dos, Suárez, A. Dosil, Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dufour, L., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ekelhof, R., Ek-In, S., Eklund, L., Ely, S., Ene, A., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Farley, N., Farry, S., Fazzini, D., Féo, M., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Funk, W., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Pardiñas, J. García, Plana, B. Garcia, Rosales, F. A. Garcia, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gazzoni, G., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Göbel, C., Golubkov, D., Golutvin, A., Gomes, A., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Hadavizadeh, T., Hadjivasiliou, C., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., Heß, M., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Huard, Z. C., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Karodia, S., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Khurewathanakul, C., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Kostiuk, I., Kot, O., Kotriakhova, S., Kozeiha, M., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Lefèvre, R., Leflat, A., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, P. -R., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Michielin, E., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mödden, A., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Müller, D., Müller, J., Müller, K., Müller, V., Murphy, C. H., Murray, D., Muzzetto, P., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., O'Hanlon, D. P., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Penso, G., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. Silva, Simi, G., Simone, S., Skiba, I., Skidmore, N., Skwarnicki, T., Slater, M. W., Smeaton, J. G., Smith, E., Smith, I. T., Smith, M., Soares, M., Lavra, L. Soares, Sokoloff, M. D., Soler, F. J. P., De Paula, B. Souza, Spaan, B., Norella, E. Spadaro, Spradlin, P., Stagni, F., Stahl, M., Stahl, S., Stefko, P., Stefkova, S., Steinkamp, O., Stemmle, S., Stenyakin, O., Stepanova, M., Stevens, H., Stone, S., Stracka, S., Stramaglia, M. E., Straticiuc, M., Straumann, U., Strokov, S., Sun, J., Sun, L., Sun, Y., Svihra, P., Swientek, K., Szabelski, A., Szumlak, T., Szymanski, M., Taneja, S., Tang, Z., Tekampe, T., Tellarini, G., Teubert, F., Thomas, E., Thomson, K. A., Tilley, M. J., Tisserand, V., T'Jampens, S., Tobin, M., Tolk, S., Tomassetti, L., Tonelli, D., Tou, D. Y., Tournefier, E., Traill, M., Tran, M. T., Trisovic, A., Tsaregorodtsev, A., Tuci, G., Tully, A., Tuning, N., Ukleja, A., Usachov, A., Ustyuzhanin, A., Uwer, U., Vagner, A., Vagnoni, V., Valassi, A., Valat, S., Valenti, G., van Beuzekom, M., Van Hecke, H., van Herwijnen, E., Van Hulse, C. B., van Tilburg, J., van Veghel, M., Gomez, R. Vazquez, Regueiro, P. Vazquez, Sierra, C. Vázquez, Vecchi, S., Velthuis, J. J., Veltri, M., Venkateswaran, A., Vernet, M., Veronesi, M., Vesterinen, M., Barbosa, J. V. Viana, Vieira, D., Diaz, M. Vieites, Viemann, H., Vilasis-Cardona, X., Vitkovskiy, A., Volkov, V., Vollhardt, A., Bruch, D. Vom, Voneki, B., Vorobyev, A., Vorobyev, V., Voropaev, N., Waldi, R., Walsh, J., Wang, J., Wang, M., Wang, Y., Wang, Z., Ward, D. R., Wark, H. M., Watson, N. K., Websdale, D., Weiden, A., Weisser, C., Westhenry, B. D. C., White, D. J., Whitehead, M., Wiedner, D., Wilkinson, G., Wilkinson, M., Williams, I., Williams, M., Williams, M. R. J., Williams, T., Wilson, F. F., Winn, M., Wislicki, W., Witek, M., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: A four-body amplitude analysis of the $B^- \to D^{*+} \pi^- \pi^-$ decay is performed, where fractions and relative phases of the various resonances contributing to the decay are measured. Several quasi-model-independent analyses are performed aimed at searching for the presence of new states and establishing the quantum numbers of previously observed charmed meson resonances. In particular the resonance parameters and quantum numbers are determined for the $D_1(2420)$, $D_1(2430)$, $D_0(2550)$, $D^*_1(2600)$, $D_2(2740)$ and $D^*_3(2750)$ states. The mixing between the $D_1(2420)$ and $D_1(2430)$ resonances is studied and the mixing parameters are measured. The dataset corresponds to an integrated luminosity of 4.7 $fb^{-1}$, collected in proton-proton collisions at center-of-mass energies of 7, 8 and 13 TeV with the LHCb detector., Comment: 35 pages, 17 figures, submitted to PHys. Rev. D. All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-027.html
Published: 2019
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46. Measurement of the $\eta_c(1S)$ production cross-section in $pp$ collisions at $\sqrt{s} = 13$ TeV

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., d'Argent, P., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Ben-Haim, E., Bencivenni, G., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., van Beuzekom, M., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Birnkraut, A., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Boubdir, M., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Cowan, G. A., Craik, D. C., Crocombe, A., Torres, M. Cruz, Currie, R., D'Ambrosio, C., Da Silva, C. L., Dall'Occo, E., Dalseno, J., Danilina, A., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dordei, F., Dorigo, M., Suárez, A. Dosil, Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dufour, L., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ek-In, S., Ekelhof, R., Eklund, L., Ely, S., Ene, A., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Farley, N., Farry, S., Fazzini, D., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Funk, W., Féo, M., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Plana, B. Garcia, Rosales, F. A. Garcia, Pardiñas, J. García, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gazzoni, G., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Golubkov, D., Golutvin, A., Gomes, A., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Guo, X., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Göbel, C., Hadavizadeh, T., Hadjivasiliou, C., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., van Herwijnen, E., Heuel, J., Heß, M., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Huard, Z. C., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Karodia, S., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Khurewathanakul, C., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Kostiuk, I., Kot, O., Kotriakhova, S., Kozeiha, M., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Leflat, A., Lefèvre, R., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, P. -R., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Ling, P., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Ma, R., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Michielin, E., Milanes, D. 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A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhovkovska, V., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: Using a data sample corresponding to an integrated luminosity of $2.0\,fb^{-1}$, collected by the LHCb experiment, the production of the $\eta_c(1S)$ state in proton-proton collisions at a centre-of-mass energy of $\sqrt{s}=13 \text{ TeV}$ is studied in the rapidity range ${2.0 < y < 4.5}$ and in the transverse momentum range ${6.5 < p_{T} < 14.0\text{ GeV}}$. The cross-section for prompt production of $\eta_c(1S)$ mesons relative to that of the $J/\psi$ meson is measured using the ${p\bar{p}}$ decay mode and is found to be ${\sigma_{\eta_c(1S)}/\sigma_{J/\psi} = 1.69 \pm 0.15 \pm 0.10 \pm 0.18}$. The quoted uncertainties are, in order, statistical, systematic and due to uncertainties on the branching fractions of the ${J/\psi\to p \bar{p}}$ and ${\eta_c\to p \bar{p}}$ decays. The prompt $\eta_c(1S)$ production cross-section is determined to be ${\sigma_{\eta_c(1S)} = 1.26 \pm 0.11\pm 0.08 \pm 0.14 \,\mu b}$, where the last uncertainty includes that on the ${J/\psi}$ meson cross-section. The ratio of the branching fractions of $b$-hadron decays to the $\eta_c(1S)$ and ${J/\psi}$ states is measured to be ${\mathcal{B}_{b\to\eta_c X}/\mathcal{B}_{b\to J/\psi X} = 0.48 \pm 0.03 \pm 0.03 \pm 0.05}$, where the last uncertainty is due to those on the branching fractions of the ${J/\psi \to p \bar{p}}$ and ${\eta_c\to p \bar{p}}$ decays. The difference between the ${J/\psi}$ and $\eta_c(1S)$ masses is also determined to be ${113.0 \pm 0.7 \pm 0.1\text{ MeV}}$, which is the most precise single measurement of this quantity to date., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-024.html (LHCb public pages)
Published: 2019
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47. Updated measurement of decay-time-dependent CP asymmetries in $D^0 \to K^+K^-$ and $D^0 \to \pi^+\pi^-$ decays

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., d'Argent, P., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Ben-Haim, E., Bencivenni, G., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., van Beuzekom, M., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Diaz, L. Calero, Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Craik, D. C., Crkovska, J., Crocombe, A., Torres, M. Cruz, Currie, R., D'Ambrosio, C., Da Silva, C. L., Dall'Occo, E., Dalseno, J., Danilina, A., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., Dean, C. T., Dean, W., Decamp, D., Del Buono, L., Delaney, B., Dembinski, H. -P., Demmer, M., Dendek, A., Denysenko, V., Derkach, D., Deschamps, O., Desse, F., Dettori, F., Dey, B., Di Canto, A., Di Nezza, P., Didenko, S., Dijkstra, H., Dordei, F., Dorigo, M., Douglas, L., Dovbnya, A., Dreimanis, K., Dudek, M. W., Dufour, L., Dujany, G., Durante, P., Durham, J. M., Dutta, D., Dzhelyadin, R., Dziewiecki, M., Dziurda, A., Dzyuba, A., Easo, S., Egede, U., Egorychev, V., Eidelman, S., Eisenhardt, S., Ek-In, S., Ekelhof, R., Eklund, L., Ely, S., Ene, A., Escher, S., Esen, S., Evans, T., Falabella, A., Fan, J., Farley, N., Farry, S., Fazzini, D., Declara, P. Fernandez, Prieto, A. Fernandez, Ferrari, F., Lopes, L. Ferreira, Rodrigues, F. Ferreira, Sole, S. Ferreres, Ferrillo, M., Ferro-Luzzi, M., Filippov, S., Fini, R. A., Fiorini, M., Firlej, M., Fischer, K. M., Fitzpatrick, C., Fiutowski, T., Fleuret, F., Fontana, M., Fontanelli, F., Forty, R., Lima, V. Franco, Sevilla, M. Franco, Frank, M., Frei, C., Friday, D. A., Fu, J., Fuehring, M., Funk, W., Féo, M., Gabriel, E., Torreira, A. Gallas, Galli, D., Gallorini, S., Gambetta, S., Gan, Y., Gandelman, M., Gandini, P., Gao, Y., Martin, L. M. Garcia, Plana, B. Garcia, Rosales, F. A. Garcia, Pardiñas, J. García, Tico, J. Garra, Garrido, L., Gascon, D., Gaspar, C., Gerick, D., Gersabeck, E., Gersabeck, M., Gershon, T., Gerstel, D., Ghez, Ph., Gibson, V., Gioventù, A., Girard, O. G., Gironell, P. Gironella, Giubega, L., Giugliano, C., Gizdov, K., Gligorov, V. V., Golubkov, D., Golutvin, A., Gomes, A., Gorbounov, P., Gorelov, I. V., Gotti, C., Govorkova, E., Grabowski, J. P., Diaz, R. Graciani, Grammatico, T., Cardoso, L. A. Granado, Graugés, E., Graverini, E., Graziani, G., Grecu, A., Greim, R., Griffith, P., Grillo, L., Gruber, L., Cazon, B. R. Gruberg, Gu, C., Guo, X., Gushchin, E., Guth, A., Guz, Yu., Gys, T., Göbel, C., Hadavizadeh, T., Haefeli, G., Haen, C., Haines, S. C., Hamilton, P. M., Han, Q., Han, X., Hancock, T. H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., van Herwijnen, E., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Kostiuk, I., Kot, O., Kotriakhova, S., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Leflat, A., Lefèvre, R., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Ling, P., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lu, Y., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Ma, R., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meier, G., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Mikhasenko, M., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Murphy, C. H., Murray, D., Muzzetto, P., Mödden, A., Müller, D., Müller, K., Müller, V., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Nunez, C., O'Hanlon, D. P., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Pappenheimer, C., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Trejo, R. I. Rabadan, Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reis, A. C. dos, Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. Silva, Simi, G., Simone, S., Skiba, I., Skidmore, N., Skwarnicki, T., Slater, M. W., Smeaton, J. G., Smetkina, A., Smith, E., Smith, I. T., Smith, M., Snoch, A., Soares, M., Lavra, L. Soares, Sokoloff, M. D., Soler, F. J. P., De Paula, B. Souza, Spaan, B., Norella, E. Spadaro, Spradlin, P., Stagni, F., Stahl, M., Stahl, S., Stefko, P., Stefkova, S., Steinkamp, O., Stemmle, S., Stenyakin, O., Stepanova, M., Stevens, H., Stocchi, A., Stone, S., Stracka, S., Stramaglia, M. E., Straticiuc, M., Strokov, S., Sun, J., Sun, L., Sun, Y., Svihra, P., Swientek, K., Szabelski, A., Szumlak, T., Szymanski, M., T'Jampens, S., Taneja, S., Tang, Z., Tekampe, T., Tellarini, G., Teubert, F., Thomas, E., Thomson, K. A., van Tilburg, J., Tilley, M. J., Tisserand, V., Tobin, M., Tolk, S., Tomassetti, L., Tonelli, D., Tou, D. Y., Tournefier, E., Traill, M., Tran, M. T., Trippl, C., Trisovic, A., Tsaregorodtsev, A., Tuci, G., Tully, A., Tuning, N., Ukleja, A., Unverzagt, D. J., Usachov, A., Ustyuzhanin, A., Uwer, U., Vagner, A., Vagnoni, V., Valassi, A., Valenti, G., Van Hecke, H., Van Hulse, C. B., Gomez, R. Vazquez, Regueiro, P. Vazquez, Vecchi, S., van Veghel, M., Velthuis, J. J., Veltri, M., Venkateswaran, A., Vernet, M., Veronesi, M., Vesterinen, M., Barbosa, J. V. Viana, Vieira, D., Diaz, M. Vieites, Viemann, H., Vilasis-Cardona, X., Vitkovskiy, A., Volkov, V., Vollhardt, A., Bruch, D. Vom, Vorobyev, A., Vorobyev, V., Voropaev, N., de Vries, J. A., Sierra, C. Vázquez, Waldi, R., Walsh, J., Wang, J., Wang, M., Wang, Y., Wang, Z., Ward, D. R., Wark, H. M., Watson, N. K., Websdale, D., Weiden, A., Weisser, C., Westhenry, B. D. C., White, D. J., Whitehead, M., Wiedner, D., Wilkinson, G., Wilkinson, M., Williams, I., Williams, M. R. J., Williams, M., Williams, T., Wilson, F. F., Winn, M., Wislicki, W., Witek, M., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: A search for decay-time-dependent charge-parity ($CP$) asymmetry in $D^0 \to K^+K^-$ and $D^0 \to \pi^+\pi^-$ decays is performed at the LHCb experiment using proton-proton collision data recorded at a center-of-mass energy of 13TeV, and corresponding to an integrated luminosity of 5.4fb$^{-1}$. The $D^0$ mesons are required to originate from semileptonic decays of $b$ hadrons, such that the charge of the muon identifies the flavor of the neutral $D$ meson at production. The asymmetries in the effective decay widths of $D^0$ and $\overline{D}^0$ mesons are determined to be $A_{\Gamma}(K^+K^-) = ( -4.3 \pm 3.6 \pm 0.5 )\times 10^{-4}$ and $A_{\Gamma}(\pi^+\pi^-) = ( 2.2 \pm 7.0 \pm 0.8)\times 10^{-4}$, where the uncertainties are statistical and systematic, respectively. The results are consistent with $CP$ symmetry and, when combined with previous LHCb results, yield $A_{\Gamma}(K^+K^-) = ( -4.4 \pm 2.3 \pm 0.6 )\times 10^{-4}$ and $A_{\Gamma}(\pi^+\pi^-) = ( 2.5 \pm 4.3 \pm 0.7)\times 10^{-4}$., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-032.html (LHCb public pages)
Published: 2019
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48. GRB171010A / SN2017htp: a GRB-SN at z=0.33

Author: Melandri, A., Malesani, D. B., Izzo, L., Japelj, J., Vergani, S. D., Schady, P., Carracedo, A. Sagues, Postigo, A. de Ugarte, Anderson, J. P., Barbarino, C., Bolmer, J., Breeveld, A., Calissendorff, P., Campana, S., Cano, Z., Carini, R., Covino, S., D'Avanzo, P., D'Elia, V., della Valle, M., De Pasquale, M., Fynbo, J. P. U., Gromadzki, M., Hammer, F., Hartmann, D. H., Heintz, K. E., Inserra, C., Jakobsson, P., Kann, D. A., Kotilainen, J., Maguire, K., Masetti, N., Nicholl, M., E., F. Olivares, Pugliese, G., Rossi, A., Salvaterra, R., Sollerman, J., Stone, M. B., Tagliaferri, G., Tomasella, L., Thone, C. C., Xu, D., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The number of supernovae known to be connected with long-duration gamma-ray bursts is increasing and the link between these events is no longer exclusively found at low redshift ($z \lesssim 0.3$) but is well established also at larger distances. We present a new case of such a liaison at $z = 0.33$ between GRB\,171010A and SN\,2017htp. It is the second closest GRB with an associated supernova of only three events detected by Fermi-LAT. The supernova is one of the few higher redshift cases where spectroscopic observations were possible and shows spectral similarities with the well-studied SN\,1998bw, having produced a similar Ni mass ($M_{\rm Ni}=0.33\pm0.02 ~\rm{M_{\odot}}$) with slightly lower ejected mass ($M_{\rm ej}=4.1\pm0.7~\rm{M_{\odot}}$) and kinetic energy ($E_{\rm K} = 8.1\pm2.5 \times 10^{51} ~\rm{erg}$). The host-galaxy is bigger in size than typical GRB host galaxies, but the analysis of the region hosting the GRB revealed spectral properties typically observed in GRB hosts and showed that the progenitor of this event was located in a very bright HII region of its face-on host galaxy, at a projected distance of $\sim$ 10 kpc from its galactic centre. The star-formation rate (SFR$_{GRB} \sim$ 0.2 M$_{\odot}$~yr$^{-1}$) and metallicity (12 + log(O/H) $\sim 8.15 \pm 0.10$) of the GRB star-forming region are consistent with those of the host galaxies of previously studied GRB-SN systems., Comment: Accepted for publication by MNRAS, 10 pages, 8 figures, 5 tables
Published: 2019
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49. Search for $A'\!\to\!\mu^+\mu^-$ decays

Author: LHCb collaboration, Aaij, R., Beteta, C. Abellán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Diaz, L. Calero, Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Craik, D. C., Crkovska, J., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. 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H., Hansmann-Menzemer, S., Harnew, N., Harrison, T., Hart, R., Hasse, C., Hatch, M., He, J., Hecker, M., Heijhoff, K., Heinicke, K., Heister, A., Hennequin, A. M., Hennessy, K., Henry, L., Heuel, J., Hicheur, A., Charman, R. Hidalgo, Hill, D., Hilton, M., Hopchev, P. H., Hu, J., Hu, W., Huang, W., Hulsbergen, W., Humair, T., Hunter, R. J., Hushchyn, M., Hutchcroft, D., Hynds, D., Ibis, P., Idzik, M., Ilten, P., Inglessi, A., Inyakin, A., Ivshin, K., Jacobsson, R., Jakobsen, S., Jalocha, J., Jans, E., Jashal, B. K., Jawahery, A., Jevtic, V., Jiang, F., John, M., Johnson, D., Jones, C. R., Jost, B., Jurik, N., Kandybei, S., Karacson, M., Kariuki, J. M., Kazeev, N., Kecke, M., Keizer, F., Kelsey, M., Kenzie, M., Ketel, T., Khanji, B., Kharisova, A., Kim, K. E., Kirn, T., Kirsebom, V. S., Klaver, S., Klimaszewski, K., Koliiev, S., Kondybayeva, A., Konoplyannikov, A., Kopciewicz, P., Kopecna, R., Koppenburg, P., Kostiuk, I., Kot, O., Kotriakhova, S., Kravchuk, L., Krawczyk, R. D., Kreps, M., Kress, F., Kretzschmar, S., Krokovny, P., Krupa, W., Krzemien, W., Kucewicz, W., Kucharczyk, M., Kudryavtsev, V., Kuindersma, H. S., Kunde, G. J., Kuonen, A. K., Kvaratskheliya, T., Lacarrere, D., Lafferty, G., Lai, A., Lancierini, D., Lane, J. J., Lanfranchi, G., Langenbruch, C., Latham, T., Lazzari, F., Lazzeroni, C., Gac, R. Le, Lefèvre, R., Leflat, A., Lemaitre, F., Leroy, O., Lesiak, T., Leverington, B., Li, H., Li, X., Li, Y., Li, Z., Liang, X., Lindner, R., Lionetto, F., Lisovskyi, V., Liu, G., Liu, X., Loh, D., Loi, A., Castro, J. Lomba, Longstaff, I., Lopes, J. H., Loustau, G., Lovell, G. H., Lu, Y., Lucchesi, D., Martinez, M. Lucio, Luo, Y., Lupato, A., Luppi, E., Lupton, O., Lusiani, A., Lyu, X., Maccolini, S., Machefert, F., Maciuc, F., Macko, V., Mackowiak, P., Maddrell-Mander, S., Mohan, L. R. Madhan, Maev, O., Maevskiy, A., Maguire, K., Maisuzenko, D., Majewski, M. W., Malde, S., Malecki, B., Malinin, A., Maltsev, T., Malygina, H., Manca, G., Mancinelli, G., Escalero, R. Manera, Manuzzi, D., Marangotto, D., Maratas, J., Marchand, J. F., Marconi, U., Mariani, S., Benito, C. Marin, Marinangeli, M., Marino, P., Marks, J., Marshall, P. J., Martellotti, G., Martinazzoli, L., Martinelli, M., Santos, D. Martinez, Vidal, F. Martinez, Massafferri, A., Materok, M., Matev, R., Mathad, A., Mathe, Z., Matiunin, V., Matteuzzi, C., Mattioli, K. R., Mauri, A., Maurice, E., McCann, M., Mcconnell, L., McNab, A., McNulty, R., Mead, J. V., Meadows, B., Meaux, C., Meier, G., Meinert, N., Melnychuk, D., Meloni, S., Merk, M., Merli, A., Mikhasenko, M., Milanes, D. A., Millard, E., Minard, M. -N., Mineev, O., Minzoni, L., Mitchell, S. E., Mitreska, B., Mitzel, D. S., Mödden, A., Mogini, A., Moise, R. D., Mombächer, T., Monroy, I. A., Monteil, S., Morandin, M., Morello, G., Morello, M. J., Moron, J., Morris, A. B., Morris, A. G., Mountain, R., Mu, H., Muheim, F., Mukherjee, M., Mulder, M., Müller, D., Müller, K., Müller, V., Murphy, C. H., Murray, D., Muzzetto, P., Naik, P., Nakada, T., Nandakumar, R., Nandi, A., Nanut, T., Nasteva, I., Needham, M., Neri, N., Neubert, S., Neufeld, N., Newcombe, R., Nguyen, T. D., Nguyen-Mau, C., Niel, E. M., Nieswand, S., Nikitin, N., Nolte, N. S., Nunez, C., Oblakowska-Mucha, A., Obraztsov, V., Ogilvy, S., O'Hanlon, D. P., Oldeman, R., Onderwater, C. J. G., Osborn, J. D., Ossowska, A., Goicochea, J. M. Otalora, Ovsiannikova, T., Owen, P., Oyanguren, A., Pais, P. R., Pajero, T., Palano, A., Palutan, M., Panshin, G., Papanestis, A., Pappagallo, M., Pappalardo, L. L., Pappenheimer, C., Parker, W., Parkes, C., Passaleva, G., Pastore, A., Patel, M., Patrignani, C., Pearce, A., Pellegrino, A., Altarelli, M. Pepe, Perazzini, S., Pereima, D., Perret, P., Pescatore, L., Petridis, K., Petrolini, A., Petrov, A., Petrucci, S., Petruzzo, M., Pietrzyk, B., Pietrzyk, G., Pikies, M., Pili, M., Pinci, D., Pinzino, J., Pisani, F., Piucci, A., Placinta, V., Playfer, S., Plews, J., Casasus, M. Plo, Polci, F., Lener, M. Poli, Poliakova, M., Poluektov, A., Polukhina, N., Polyakov, I., Polycarpo, E., Pomery, G. J., Ponce, S., Popov, A., Popov, D., Poslavskii, S., Prasanth, K., Promberger, L., Prouve, C., Pugatch, V., Navarro, A. Puig, Pullen, H., Punzi, G., Qian, W., Qin, J., Quagliani, R., Quintana, B., Raab, N. V., Trejo, R. I. Rabadan, Rachwal, B., Rademacker, J. H., Rama, M., Pernas, M. Ramos, Rangel, M. S., Ratnikov, F., Raven, G., Salzgeber, M. Ravonel, Reboud, M., Redi, F., Reichert, S., Reiss, F., Alepuz, C. Remon, Ren, Z., Renaudin, V., Ricciardi, S., Richards, S., Rinnert, K., Robbe, P., Robert, A., Rodrigues, A. B., Rodrigues, E., Lopez, J. A. Rodriguez, Roehrken, M., Roiser, S., Rollings, A., Romanovskiy, V., Lamas, M. Romero, Vidal, A. Romero, Roth, J. D., Rotondo, M., Rudolph, M. S., Ruf, T., Vidal, J. Ruiz, Ryzka, J., Silva, J. J. Saborido, Sagidova, N., Saitta, B., Gras, C. Sanchez, Mayordomo, C. Sanchez, Sedes, B. Sanmartin, Santacesaria, R., Rios, C. Santamarina, Santimaria, M., Santovetti, E., Sarpis, G., Sarti, A., Satriano, C., Satta, A., Saur, M., Savrina, D., Smead, L. G. Scantlebury, Schael, S., Schellenberg, M., Schiller, M., Schindler, H., Schmelling, M., Schmelzer, T., Schmidt, B., Schneider, O., Schopper, A., Schreiner, H. F., Schubiger, M., Schulte, S., Schune, M. H., Schwemmer, R., Sciascia, B., Sciubba, A., Sellam, S., Semennikov, A., Sergi, A., Serra, N., Serrano, J., Sestini, L., Seuthe, A., Seyfert, P., Shangase, D. M., Shapkin, M., Shears, T., Shekhtman, L., Shevchenko, V., Shmanin, E., Shupperd, J. D., Siddi, B. G., Coutinho, R. Silva, de Oliveira, L. 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F., Winn, M., Wislicki, W., Witek, M., Wormser, G., Wotton, S. A., Wu, H., Wyllie, K., Xiang, Z., Xiao, D., Xie, Y., Xing, H., Xu, A., Xu, L., Xu, M., Xu, Q., Xu, Z., Yang, Z., Yao, Y., Yeomans, L. E., Yin, H., Yu, J., Yuan, X., Yushchenko, O., Zarebski, K. A., Zavertyaev, M., Zdybal, M., Zeng, M., Zhang, D., Zhang, L., Zhang, S., Zhang, W. C., Zhang, Y., Zhelezov, A., Zheng, Y., Zhou, X., Zhou, Y., Zhu, X., Zhukov, V., Zonneveld, J. B., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: Searches are performed for both prompt-like and long-lived dark photons, $A'$, produced in proton-proton collisions at a center-of-mass energy of 13 TeV. These searches look for $A'\!\to\!\mu^+\mu^-$ decays using a data sample corresponding to an integrated luminosity of 5.5/fb collected with the LHCb detector. Neither search finds evidence for a signal, and 90% confidence-level exclusion limits are placed on the $\gamma$-$A'$ kinetic-mixing strength. The prompt-like $A'$ search explores the mass region from near the dimuon threshold up to 70 GeV, and places the most stringent constraints to date on dark photons with $214 < m(A') \lesssim 740$ MeV and $10.6 < m(A') \lesssim 30$ GeV. The search for long-lived $A'\!\to\!\mu^+\mu^-$ decays places world-leading constraints on low-mass dark photons with lifetimes $\mathcal{O}(1)$ ps., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-031.html (LHCb public pages)
Published: 2019
Full Text: View/download PDF

50. Search for the doubly charmed baryon $\Xi_{cc}^{+}$

Author: LHCb collaboration, Aaij, R., Beteta, C. Abelán, Ackernley, T., Adeva, B., Adinolfi, M., Afsharnia, H., Aidala, C. A., Aiola, S., Ajaltouni, Z., Akar, S., Albicocco, P., Albrecht, J., Alessio, F., Alexander, M., Albero, A. Alfonso, Alkhazov, G., Cartelle, P. Alvarez, Alves Jr, A. A., Amato, S., Amhis, Y., An, L., Anderlini, L., Andreassi, G., Andreotti, M., Archilli, F., Romeu, J. Arnau, Artamonov, A., Artuso, M., Arzymatov, K., Aslanides, E., Atzeni, M., Audurier, B., Bachmann, S., Back, J. J., Baker, S., Balagura, V., Baldini, W., Baranov, A., Barlow, R. J., Barsuk, S., Barter, W., Bartolini, M., Baryshnikov, F., Bassi, G., Batozskaya, V., Batsukh, B., Battig, A., Battista, V., Bay, A., Becker, M., Bedeschi, F., Bediaga, I., Beiter, A., Bel, L. J., Belavin, V., Belin, S., Beliy, N., Bellee, V., Belous, K., Belyaev, I., Bencivenni, G., Ben-Haim, E., Benson, S., Beranek, S., Berezhnoy, A., Bernet, R., Berninghoff, D., Bernstein, H. C., Bertholet, E., Bertolin, A., Betancourt, C., Betti, F., Bettler, M. O., Bezshyiko, Ia., Bhasin, S., Bhom, J., Bieker, M. S., Bifani, S., Billoir, P., Birnkraut, A., Bizzeti, A., Bjørn, M., Blago, M. P., Blake, T., Blanc, F., Blusk, S., Bobulska, D., Bocci, V., Garcia, O. Boente, Boettcher, T., Boldyrev, A., Bondar, A., Bondar, N., Borghi, S., Borisyak, M., Borsato, M., Borsuk, J. T., Bowcock, T. J. V., Bozzi, C., Braun, S., Rodriguez, A. Brea, Brodski, M., Brodzicka, J., Gonzalo, A. Brossa, Brundu, D., Buchanan, E., Buonaura, A., Burr, C., Bursche, A., Butter, J. S., Buytaert, J., Byczynski, W., Cadeddu, S., Cai, H., Calabrese, R., Cali, S., Calladine, R., Calvi, M., Gomez, M. Calvo, Camboni, A., Campana, P., Perez, D. H. Campora, Capriotti, L., Carbone, A., Carboni, G., Cardinale, R., Cardini, A., Carniti, P., Akiba, K. Carvalho, Vidal, A. Casais, Casse, G., Cattaneo, M., Cavallero, G., Cenci, R., Cerasoli, J., Chapman, M. G., Charles, M., Charpentier, Ph., Chatzikonstantinidis, G., Chefdeville, M., Chekalina, V., Chen, C., Chen, S., Chernov, A., Chitic, S. -G., Chobanova, V., Chrzaszcz, M., Chubykin, A., Ciambrone, P., Cicala, M. F., Vidal, X. Cid, Ciezarek, G., Cindolo, F., Clarke, P. E. L., Clemencic, M., Cliff, H. V., Closier, J., Cobbledick, J. L., Coco, V., Coelho, J. A. B., Cogan, J., Cogneras, E., Cojocariu, L., Collins, P., Colombo, T., Comerma-Montells, A., Contu, A., Cooke, N., Coombs, G., Coquereau, S., Corti, G., Sobral, C. M. Costa, Couturier, B., Craik, D. C., Crkovska, J., Crocombe, A., Torres, M. Cruz, Currie, R., Da Silva, C. L., Dall'Occo, E., Dalseno, J., D'Ambrosio, C., Danilina, A., d'Argent, P., Davis, A., Francisco, O. De Aguiar, De Bruyn, K., De Capua, S., De Cian, M., De Miranda, J. M., De Paula, L., De Serio, M., De Simone, P., de Vries, J. A., Dean, C. 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Subjects: High Energy Physics - Experiment
Abstract: A search for the doubly charmed baryon $\Xi_{cc}^{+}$ is performed through its decay to the $\Lambda_c^+ K^- \pi^+$ final state, using proton-proton collision data collected with the LHCb detector at centre-of-mass energies of 7, 8 and 13$\mathrm{\,Te\kern -0.1em V}$. The data correspond to a total integrated luminosity of $9\,\mathrm{fb}^{-1}$. No significant signal is observed in the mass range from 3.4 to 3.8$\mathrm{\,Ge\kern -0.1em V}/c^2$. Upper limits are set at $95\%$ credibility level on the ratio of the $\Xi_{cc}^{+}$ production cross-section times the branching fraction to that of $\Lambda_c^+$ and $\Xi_{cc}^{++}$ baryons. The limits are determined as functions of the $\Xi_{cc}^{+}$ mass for different lifetime hypotheses, in the rapidity range from 2.0 to 4.5 and the transverse momentum range from 4 to 15$\mathrm{\,Ge\kern -0.1em V}/c$., Comment: All figures and tables, along with any supplementary material and additional information, are available at https://cern.ch/lhcbproject/Publications/p/LHCb-PAPER-2019-029.html
Published: 2019
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