Search

M. Dixon et al., We use stacked spectra of the host galaxies of photometrically identified Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) to search for correlations between Hubble diagram residuals and the spectral properties of the host galaxies. Utilizing full spectrum fitting techniques on stacked spectra binned by Hubble residual, we find no evidence for trends between Hubble residuals and properties of the host galaxies that rely on spectral absorption features (, MD would like to acknowledge support through an Australian Government Research Training Program Scholarship. This research was supported by the Australian Research Council The Centre of Excellence for Dark Matter Particle Physics (CDM; project number CE200100008) and the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav; project number CE170100004). This project/publication was made possible through the support of a grant from the John Templeton Foundation. The authors gratefully acknowledge this grant ID 61807, Two Standard Models Meet. The opinions expressed in this publication are those of the author(s) and do not necessarily reflect the views of the John Templeton Foundation. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. Based on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional custodians of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present.

For the past decade, SALT2 has been the most common model used to fit Type Ia supernova (SN Ia) light curves for dark energy analyses. Recently, the SALT3 model was released, which upgraded a number of model features but has not yet been used for measurements of dark energy. Here, we evaluate the impact of switching from SALT2 to SALT3 for a SN cosmology analysis. We train SALT2 and SALT3 on an identical training sample of 1083 well-calibrated Type Ia supernovae, ensuring that any differences found come from the underlying model framework. We publicly release the results of this training (the SALT "surfaces"). We then run a cosmology analysis on the public Dark Energy Survey 3-Year Supernova data sample (DES-SN3YR), and on realistic simulations of those data. We provide the first estimate of the SN+CMB systematic uncertainty arising from the choice of SALT model framework (i.e. SALT2 versus SALT3), $\Delta w = +0.001 \pm 0.005$ -- a negligible effect at the current level of dark energy analyses. We also find that the updated surfaces are less sensitive to photometric calibration uncertainties than previous SALT2 surfaces, with the average spectral energy density dispersion reduced by a factor of two over optical wavelengths. This offers an opportunity to reduce the contribution of calibration errors to SN cosmology uncertainty budgets., Comment: 19 pages, 13 figures, accepted by MNRAS

The He I 1 micron line is a high excitation line which allows us to probe the innermost regions of protostellar disks, and to trace both accreting and outflowing material. We use X-Shooter observations of a sample of 107 young stars in the Lupus (1-3 Myr) and Upper Scorpius (5-10 Myr) star-forming regions to search for correlations between the line properties, as well as the disk inclination and accretion luminosity. We identified eight distinct profile types in the sample. We fitted Gaussian curves to the line features to measure the maximum velocities traced in absorption, the full-width half-maximum (FWHM) of the line features, and the Gaussian area of the features. We compare the proportion of each profile type in our sample to previous studies in Taurus. We find significant variations between Taurus and Lupus in the proportion of P Cygni and inverse P Cygni profiles, and between Lupus and Upper Scorpius in the number of emission-only and combination profile types. We find that the blue-shifted absorption features appear less blue-shifted at disk inclinations close to edge-on, but no such trend with inclination is observed in sources with only red-shifted features. Higher accretion rates were observed in sources with strong blue-shifted features which, along with the changes in the proportions of each profile type observed in the two regions, indicates that younger sources may drive stronger jets or winds. Overall, we observe variations in the proportion of each profile type and in the line properties which indicates and evolution of accretion and ejection signatures over time, and with source properties. These results confirm past works and models of the He I line, but for a larger sample and for multiple star-forming regions. The work highlights the power of the He I line as a probe of the gas in the innermost regions of the disk., Comment: 24 pages, 21 figures, 4 tables - accepted by A&A on 01/08/2022

Wiseman, P., et al. DES Collaboration, We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M*/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = −1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10−13 SNe M⊙−1 yr−1, which corresponds to an overall SN Ia production efficiency NIa/M∗=0.9 +4.0−0.7×10−3 SNe M−1⊙⁠. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors., The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007–2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).

This work was supported by the Science and Technology Facilities Council [grant number ST/P006760/1] through the DISCnet Centre for Doctoral Training. MS acknowledges support from EU/FP7-ERC grant 615929. LG was funded by the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). Funding for the DES Projects has been provided by the US Department of Energy, the US '0:funding-source 3:href="http://dx.doi.org/10.13039/100000001"' National Science Foundation'/0:funding-source', the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This paper is based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. This paper is based in part on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting this paper for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this paper, or allow others to do so, for United States Government purposes. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr −19.3mag 20 d after explosion. This object does not show a linear decline tail in the light curve until 60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d−1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1–2.4 per cent of cases in DES, depending on the probability threshold used for a positive classification., Science and Technology Facilities Council through the DISCnet Centre for Doctoral Training, EU/FP7-ERC grant 615929, European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant 839090, Spanish grant within the European Funds for Regional Development (FEDER) PGC2018-095317-B-C21, United States Department of Energy (DOE), National Science Foundation (NSF), Spanish Government, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Financiadora de Inovacao e Pesquisa (Finep), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Ministerio da Ciencia, Tecnologia e Inovacao, German Research Foundation (DFG), Collaborating Institutions in the Dark Energy Survey, National Science Foundation (NSF) AST-1138766 AST-1536171, MINECO AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV-2016-0588 SEV-2016-0597 MDM-2015-0509, European Commission, CERCA program of the Generalitat de Catalunya, European Research Council (ERC) FP7/2007-2013, European Research Council (ERC) European Commission 240672 291329 306478, Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant) 465376/2014-2, Fermi Research Alliance, LLC DE-AC02-07CH11359, Anglo-Australian Telescope A/2013B/012, National Aeronautics & Space Administration (NASA)

DES Collaboration: et al., Rapidly evolving transients (RETs), also termed fast blue optical transients, are a recently discovered group of astrophysical events that display rapid luminosity evolution. RETs typically rise to peak in less than 10 d and fade within 30, a time-scale unlikely to be compatible with the decay of Nickel-56 that drives conventional supernovae (SNe). Their peak luminosity spans a range of −15 < Mg < −22.5, with some events observed at redshifts greater than 1. Their evolution on fast time-scales has hindered high-quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper, we present the largest sample of RETs to date, comprising 106 objects discovered by the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission lines from OzDES spectroscopy, we derive stellar masses and star formation rates (SFRs) for 49 host galaxies, and metallicities ([O/H]) for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to samples of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs (〈log (sSFR)〉 ∼ −9.6), indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long-duration gamma-ray bursts and superluminous SN host galaxies (〈12 + log (O/H)〉 ∼ 9.4). There are no clear relationships between mass or SFR of the host galaxies and the peak magnitudes or decline rates of the transients themselves., We acknowledge support from STFC grant ST/R000506/1. MSm, MSu, and CPG acknowledge support from from the European Union’s 7th Framework Programme (EU/FP7) European Research Council (ERC) grant no. 615929. LG was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). LK was supported by the Science and Technology Facilities Council (grant number ST/P006760/1) through the DISCnet Centre for Doctoral Training. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2)

DES Collaboration: et al., We present an analysis of DES17X1boj and DES16E2bjy, two peculiar transients discovered by the Dark Energy Survey (DES). They exhibit nearly identical double-peaked light curves that reach very different maximum luminosities (Mr = −15.4 and −17.9, respectively). The light-curve evolution of these events is highly atypical and has not been reported before. The transients are found in different host environments: DES17X1boj was found near the nucleus of a spiral galaxy, while DES16E2bjy is located in the outskirts of a passive red galaxy. Early photometric data are well fitted with a blackbody and the resulting moderate photospheric expansion velocities (1800 km s−1 for DES17X1boj and 4800 km s−1 for DES16E2bjy) suggest an explosive or eruptive origin. Additionally, a feature identified as high-velocity Ca II absorption (⁠v ≈ 9400 km s−1) in the near-peak spectrum of DES17X1boj may imply that it is a supernova. While similar light-curve evolution suggests a similar physical origin for these two transients, we are not able to identify or characterize the progenitors., We acknowledge support from the European Union’s 7th Framework Programme (EU/FP7) European Research council (ERC) grant 615929, and Science and Technology Facilities Council (STFC) grant ST/R000506/1. LG was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

In immunocompromised patients, Aspergillus infections are important causes of morbidity and mortality. We describe a patient with cryoglobulinemic vasculitis who developed disseminated invasive aspergillosis with thyrotoxicosis caused by Aspergillus fumigatus. The diagnosis was based upon radiological, microbiological and pathological findings. The patient was treated successfully with voriconazole and caspofungin treatment followed by total thyroidectomy. We provide an overview of published reports on Aspergillus thyroiditis with an emphasis on therapeutic approaches.

International audience; The Nearby Supernova Factory presents an interim data release of spectrophotometric timeseries of 210 SNe Ia. Two slightly different versions of the data are included, corresponding to the training data sets used for the SNEMO and SUGAR Type Ia models. The data has been shifted to the restframe and is blinded with respect to cosmology.

The analysis of current and future cosmological surveys of Type Ia supernovae (SNe Ia) at high redshift depends on the accurate photometric classification of the SN events detected. Generating realistic simulations of photometric SN surveys constitutes an essential step for training and testing photometric classification algorithms, and for correcting biases introduced by selection effects and contamination arising from core-collapse SNe in the photometric SN Ia samples. We use published SN time-series spectrophotometric templates, rates, luminosity functions, and empirical relationships between SNe and their host galaxies to construct a framework for simulating photometric SN surveys. We present this framework in the context of the Dark Energy Survey (DES) 5-yr photometric SN sample, comparing our simulations of DES with the observed DES transient populations. We demonstrate excellent agreement in many distributions, including Hubble residuals, between our simulations and data. We estimate the core collapse fraction expected in the DES SN sample after selection requirements are applied and before photometric classification. After testing different modelling choices and astrophysical assumptions underlying our simulation, we find that the predicted contamination varies from 7.2 to 11.7 per cent, with an average of 8.8 per cent and an r.m.s. of 1.1 per cent. Our simulations are the first to reproduce the observed photometric SN and host galaxy properties in high-redshift surveys without fine-tuning the input parameters. The simulation methods presented here will be a critical component of the cosmology analysis of the DES photometric SN Ia sample: correcting for biases arising from contamination, and evaluating the associated systematic uncertainty.

We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. Fitting spectral energy distributions to the $griz$ photometric measurements of the DES-SN host galaxies, we derive stellar masses and star-formation rates. For the DES-SN sample, when considering a 5D ($z$, $x_1$, $c$, $\alpha$, $\beta$) bias correction, we find evidence of a Hubble residual `mass step', where SNe Ia in high mass galaxies ($>10^{10} \textrm{M}_{\odot}$) are intrinsically more luminous (after correction) than their low mass counterparts by $\gamma=0.040\pm0.019$mag. This value is larger by $0.031$mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\gamma=0.066\pm0.020$mag. The 1D-5D $\gamma$ difference for DES-SN is $0.026\pm0.009$mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the $x_1$ component of the 5D distance-bias correction. To better understand this effect, we include an intrinsic correlation between light-curve width and stellar mass in simulated SN Ia samples. We show that a 5D fit recovers $\gamma$ with $-9$mmag bias compared to a $+2$mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modeling correlations between galaxy properties and SN is necessary to determine the implications for $\gamma$ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST., Comment: 27 pages, 13 figures; Submitted to MNRAS

We present measurements of the local core collapse supernova (SN) rate using SN discoveries from the Palomar Transient Factory (PTF). We use a Monte Carlo simulation of hundreds of millions of SN light curve realizations coupled with the detailed PTF survey detection efficiencies to forward-model the SN rates in PTF. Using a sample of 86 core collapse SNe, including 26 stripped-envelope SNe (SESNe), we show that the overall core collapse SN volumetric rate is $r^\mathrm{CC}_v=9.10_{-1.27}^{+1.56}\times10^{-5}\,\text{SNe yr}^{-1}\,\text{Mpc}^{-3}\, h_{70}^{3}$ at $ \langle z \rangle = 0.028$, and the SESN volumetric rate is $r^\mathrm{SE}_v=2.41_{-0.64}^{+0.81}\times10^{-5}\, \text{SNe yr}^{-1}\,\text{Mpc}^{-3}\, h_{70}^{3}$. We further measure a volumetric rate for hydrogen-free superluminous SNe (SLSNe-I) using 8 events at $z{\le}0.2$ of $r^\mathrm{SLSN-I}_v=35_{-13}^{+25}\, \text{SNe yr}^{-1}\text{Gpc}^{-3}\, h_{70}^{3}$, which represents the most precise SLSN-I rate measurement to date. Using a simple cosmic star-formation history to adjust these volumetric rate measurements to the same redshift, we measure a local ratio of SLSN-I to SESN of $\sim1/810^{+1500}_{-94}$, and of SLSN-I to all CCSN types of $\sim 1/3500^{+2800}_{-720}$. However, using host galaxy stellar mass as a proxy for metallicity, we also show that this ratio is strongly metallicity dependent: in low-mass ($\mathrm{log} M_{*} < 9.5 \mathrm{M}_\odot$) galaxies, which are the only environments that host SLSN-I in our sample, we measure a SLSN-I to SESN fraction of $1/300^{+380}_{-170}$ and $1/1700^{+1800}_{-720}$ for all CCSN. We further investigate the SN rates a function of host galaxy stellar mass and show that the specific rates of all core collapse SNe decrease with increasing stellar mass., 17 pages, 10 figures, submitted to MNRAS

The design and analysis of time-domain sky surveys require the ability to simulate accurately realistic populations of core-collapse supernova (SN) events. We present a set of spectral time-series templates designed for this purpose, for both hydrogen-rich (Type II, IIn, and IIb) and stripped-envelope (Type Ib, Ic, and Ic-BL) core-collapse SNe. We use photometric and spectroscopic data for 67 core-collapse SNe from the literature, and for each generate a time-series spectral template. The techniques used to build the templates are fully data driven with no assumption of any parametric form or model for the light curves. The template-building code is open source, and can be applied to any transient for which well-sampled multiband photometry and multiple spectroscopic observations are available. We extend these spectral templates into the near-ultraviolet to λ ≃ 1600 Å using observer-frame ultraviolet photometry. We also provide a set of templates corrected for host galaxy dust extinction, and provide a set of luminosity functions that can be used with our spectral templates in simulations. We give an example of how these templates can be used by integrating them within the popular SN simulation package snana, and simulating core-collapse SNe in photometrically selected cosmological Type Ia SN samples, prone to contamination from core-collapse events.

Summary In addition to being an essential organ related to alimentation, nutrition and metabolism, the gut plays a central role in the defence against inner microbial aggression and in enhancing the immunological response. The gut's complex structure and its relations with other body organs are balanced by an intrinsic biological susceptibility to various derangements. This makes the negative involvement of the gastrointestinal tract crucial in intensive care patients. The gut is involved in sepsis and multiple organ failure (MOF), but whether it is the source or victim remains a matter of debate. Splanchnic haemodynamics are often compromised in critically ill patients due to both the underlying disease and therapeutic interventions. Splanchnic hypoperfusion may contribute to the pathogenesis of systemic inflammation, sepsis and MOF via several mechanisms, including ischaemia and reperfusion injury, increased mucosal permeability, translocation of endotoxin and bacteria, and local activation of cytokines and their inflammatory mediators. In addition, inadequate perfusion, dysoxia, and ischaemia-reperfusion may trigger and enhance a local inflammatory response that may itself damage remote organs. Under severe insult, the gut is considered to have an important role in promoting septic complications and multiple organ failure from the viewpoint of altered intestinal epithelium, incompetent local immune system and overgrowth of pathogenic bacteria. When the mucosal barrier is permeable, gut flora can sustain bacteraemia and induce gut-origin sepsis.

Cobalamin A deficiency (cblA) is an inherited disorder of intracellular cobalamin metabolism, caused by impaired 5'-deoxy-adenosylcobalamin (AdoCbl) synthesis. Hydroxocobalamin (OHCbl) is the cornerstone of cblA treatment because vitamin B12 may completely restore AdoCbl deficiency. Parenteral administration, intravenous, subcutaneous or intramuscular, is generally required to achieve effect. Daily injections represent a problem for the parents and the caregivers, and this may lead to poor compliance and scarce adherence to the long-term treatment.Our report describes the case of a patient with cblA deficiency, diagnosed by newborn screening, positively treated with daily OHCbl administration by a subcutaneous injection port (i-port advanceTM). After the insertion of the device, we checked methylmalonic acid (MMA) levels weekly for the first month and then monthly. MMA level remained always in the normal range.To date, placement of a subcutaneous catheter to minimize the pain related to parenteral vitamin B12 punctures has been described only in a patient with deficiency of the enzyme methylmalonyl-CoA mutase (MUT). No other experiences are described in the literature.Our case shows that OHCbl administration using a subcutaneous catheter is safe and effective even in patients with cblA deficiency. The use of subcutaneous devices may reduce difficulties in providing parenteral daily injections which is the main reason discouraging physicians and families to use such an invasive treatment. Moreover, our experience may be translated to other inherited metabolic disorders, such as cobalamin C (cblC) disease, which may require daily parenteral drug administration.

Background: There are no recommendations about admission to an ICU after a major lung resection and there are considerable differences among institutions in this respect. Objectives: To audit the practice of admission to an ICU after a major lung resection and evaluate factors predicting the need for intensive care. Methods: Clinicalrecords of all patients who underwent major pulmonary resections in a 14-month period were reviewed retrospectively. The criteria for postoperative admission to the ICU were: (1) standard pneumonectomy if comorbidity index (CI) >0 and/or ASA score >1, and/or abnormal spirometry or arterial gas analysis; (2) extended pneumonectomy; (3) lobectomy if CI ≧4 and/or ASA ≧3; (4) lobectomy if FEV1 1 is between 60 and 80% and hypercapnia. Results: Among the 49 patients postoperatively admitted to the surgical ward, only 1 needed late intensive care. Among the 55 patients admitted to the ICU, 25 did not require specific intensive care and were discharged 24 h postoperatively, whereas the remaining 30 patients required specific intensive care. Multivariate analysis identified ASA score, predictive postoperative DLCO, and predictive postoperative product (PPP) as independent predictors of a need for admission to an ICU. Conclusion: This empirical protocol was useful in identifying patients not likely to need admission to the ICU. ASA score, predictive postoperative DLCO, and PPP are independent predictors of a need for admission to an ICU.

Con la morte cerebrale (o meglio encefalica, ovvero cessazione irreversibile di tutte le funzioni del cervello e del tronco encefalico), attualmente definita più correttamente come morte diagnosticata con criteri neurologici, compare un peculiare e unico quadro clinico, neurologico e somatico che tende alla disgregazione funzionale organica e al decadimento perfusivo che, se non contrastato, conduce all’ arresto cardiaco e quindi alla cessazione della perfusione stessa degli organi e della loro funzione. In tali condizioni viene intrapreso un percorso diagnostico (dettagliatamente normato da Leggi e Regolamento applicativo) finalizzato a rendere possibile l’accertamento della morte, e, qualora ne sussistano tutti i requisiti, al suo termine il prelievo dal soggetto deceduto, a scopo di trapianto terapeutico, degli organi: questi mantengono la loro funzionalità grazie alla persistenza della funzione cardiaca ed emodinamica (perfusione e metabolismo) e respiratoria (scambio gassoso) artificialmente mantenute. Il periodo di accertamento della avvenuta morte (non meno di sei ore nell’ adulto) richiede un attivo e mirato intervento da parte dell’ equipe intensivologica finalizzato a “mantenere” la biologia del soggetto correggendo o contrastando gli effetti della morte encefalica (assenza dei controlli regolatori per la venuta meno delle funzioni svolte fisiologicamente dall’encefalo). Il prevenire o l’ attenuare le disfunzioni degli organi del potenziale donatore a cuore battente richiede l’ approfondita conoscenza delle conseguenze fisiopatologiche che seguono alla morte encefalica. Per trattamento (meglio che mantenimento) del donatore d’organi si intende la gestione intensivologica di un organismo che ha perso l’omeostasi corporea. Consiste nell’ insieme delle attività diagnostico – terapeutiche, di monitoraggio, nursing e organizzative usualmente praticate nei reparti di Rianimazione, orientate al mantenimento e al miglioramento delle funzioni degli organi prelevabili e trapiantabili e occupa il periodo che va dal momento in cui è stata effettuata la diagnosi di morte ed iniziato il periodo di accertamento, fino al termine del periodo dell’osservazione. Gli organi prelevabili e trapiantabili con successo sono quelli con alta vitalità biologica e con prerogative funzionali conservate in quanto precedentemente normoperfusi e privi di potenziale lesività per il ricevente. Il trattamento del donatore è, quindi, un’ azione sanitaria complessa e multi-disciplinare da attuare in un concentrato periodo di tempo (tra comparsa dei segni clinici e strumentali di morte e completamento del periodo formale di accertamento di essa, ovvero più esattamente sino alla fine delle attività chirurgiche di prelievo degli organi). Si basa sui principi e gli strumenti della buona pratica clinica intensivologica orientata alla “rianimazione biologica” del soggetto donatore in stato di morte a cuore battente (specificità fisiopatologica) e alla protezione degli organi prelevabili e trapiantabili (finalità terapeutica primaria). Il trattamento del donatore comprende inoltre l’assistenza intensiva durante il trasporto dalla Rianimazione a sedi esterne di diagnosi (Imaging neuroradiologico e radiologico) e alla Sala operatoria e nel corso dell’intervento chirurgico di prelievo.

Le infezioni gravi sono riscontrabili frequentemente nei pazienti critici: riconoscibili sia all’ ingresso in Terapia Intensiva (e spesso causa del ricovero) che acquisite durante la degenza (infezioni nosocomiali) e l’ epidemiologia di queste condizioni è al centro di attenzioni diagnostiche e preventive. Il noto incremento del rischio infettivo determinato dalla risposta al trauma, dalla malnutrizione, dalla immunodepressione e da alcune terapie primarie è, inoltre, divenuto un end-point primario per giudicare l’ efficacia di molti interventi di governo clinico e terapeutici come il supporto nutrizionale artificiale, tanto è che alcune delle più forti raccomandazioni (A-B) per la nutrizione nel paziente critico sono basate appunto sui benefici inducibili nella riduzione degli eventi infettivi (nutrizione enterale precoce, pronto raggiungimento e mantenimento dell’ obiettivo di apporti, uso di alcuni farmaconutrienti). Il supporto metabolico mediante nutrizione artificiale adeguata alle specificità dei pazienti con episodi di sepsie e sepsi severa è un campo relativamente giovane sia di ricerca che di discussione e permane tuttora aperto in quanto la complessità e la variabilità dei quadri clinici è in questo ambito assai ampia. La sepsi e l’ insufficienza multiorganica sono caratterizzate da un rilascio eccessivo di mediatori dell’ infiammazione e da una marcata stimolazione e increzione di ormoni dello stress: questo comporta profondi effetti sul metabolismo energetico e dei substrati: l’ iperglicemia (marker di gravità) e l’ iperlattacidemia (marker dell’ ipoperfusione) sono due indici che csi sono dimostrati correlare sia con l’ esito clinico che con l’ efficacia delle terapie.Vi sono, da tempo, varie evidenze chedocumentano come l’ apporto di singoli farmaconutrienti (FA n-3) e miscele arricchite con farmaconutrienti specie per via enterale (Arginina, FA n-3, nucleotidi, antiossidanti) risultano benefici non solo nei pazienti sottoposti ad alta chirurgia gastroenterologica o traumatizzati, ma anche con sepsi di grado moderato (a basso MOF).

Much has been learned over the past 20 years about traumatic brain injury (TBI). The surgical management of TBI has changed little during this period and continues to concentrate on early evacuation of significant space-occupying lesions. In contrast, there have been major changes in our approach to the critical care management of TBI during this period, and this is refl ected in the progressive and signifi cant reduction in severe TBI mortality from 50% to 10% over the last 30 years. This trend in reduced mortality and improved outcomes has, for the most part, been subsequent to the use of evidence-based critical care management protocols that emphasize assessment and monitoring. The main reasons for clinical assessment and monitoring neurocritical and neurotrauma patients could be summarized as follows: 1. detect the severity of trauma and recognize early neurological worsening before irreversible brain damage occurs; 2. individualise patient care decisions; 3. guide patient management; 4. monitor therapeutic response of some interventions and avoid any consequent adverse effects; 5. assist clinicians to understand the pathophysiology of complex disorders; 6. design and implement management protocols; 7. improve neurological outcome and quality of life in survivors of severe brain injuries

La sempre crescente pressione che viene esercitata sull’ organizzazione sanitaria da parte di percorsi assistenziali e terapeutici per i pazienti chirurgici ha portato ad un forte impatto economico, al cui contenimento positivamente contribuisce un nuovo concetto: la chirurgia a rapida dimissione (Fast-track), ormai diffusa in varie tipologie di interventi anche di chirurgia maggiore, tra cui quella colica e toraco-polmonare. Questo principio è basato sull’ applicazione di una serie di strategie di provata e rilevante efficacia sperimentale (EBM) il cui scopo è quello di ottimizzare la gestione perioperatoria dei pazienti in ordine a ridurre la morbilità, accelerare la guarigione, ridurre i tempi di degenza e i costi ospedalieri. Tra le tante strategie di volta in volta poste in essere, un gruppo di queste verte sulla ottimizzazione dello stato nutrizizonale, sul contenimento del digiuno e sul supporto nutrizionale precoce se la rialimentazione precoce non può essere attuata. Le strategie preoperatorie efficaci sono la minimizzazione del digiuno, la abolizione della preparazione intstinale, il supporto metabolico e nutrizionale pre-operatorio e l’ educazione del paziente per migliorarne la cooperazione. Tra le pratiche metabolico-nutrizionali postoperatorie si analizza la dimostrazione di efficacia della ripresa precoce dell’ alimentazione, dell supporto nutrizionale artificiale preperatorio e di quello postoperatorio, in cui la nutrizione enterale precoce immunomodulante, anti-infiammatoria e enterotrofica, ne rappresenta la componente farmacoterapeutica. Poiché è difficile cambiare la routine e la pratica comune, si esplorano le barriere concettuali, organizzative e pratiche di riconosciuto peso per formare a superarle.

Uno dei principali problemi in neurochirurgia e in neurorianimazione e costituito dal mantenimento di un adeguato flusso ematico cerebrale. Condizioni patologiche di varia natura (traumatica, neoplastica, ischemica, emorragica, infettiva) possono, alterando l’equilibrio della dinamica intracranica, innescare un meccanismo di risposte che, se fino a un certo limite possono rappresentare un meccanismo di adattamento prima e di compenso subito dopo, superato quel limite tendono a provocare alterazioni che possono condurre a lesioni irreversibili del parenchima cerebrale (ischemia). Un adeguato e costante Flusso Ematico Cerebrale (FEC) e indispensabile per un ottimale funzionamento dell’encefalo e, poiche l’attivita cerebrale e strettamente correlata al metabolismo, deve esistere una continua regolazione del flusso ematico che ne permetta l’adeguamento rispetto alle esigenze metaboliche tissutali: si parla di accoppiamento flusso-metabolismo. Il flusso ematico cerebrale rappresenta il volume di sangue che affluisce all’encefalo nell’unita di tempo garantendo un ottimale apporto di ossigeno e glucosio; rappresenta circa il 15% della gittata cardiaca ed e pari a circa 750 ml/min. I fattori che presiedono alla regolazione del FEC sono vari, spesso riportati come sigle: Pressione Arteriosa (PAS) e Pressione Arteriosa Sistemica Media (PAM), Pressione Intracranica (PIC), Pressione di Perfusione Cerebrale (PPC), Resistenze Vascolari Cerebrali (RVC), fabbisogno cerebrale di O2 (Cerebral Metabolic Rate for Oxygen, CMRO2).

La morte encefalica è una diagnosi clinica definibile utilizzando usuali strumenti dell’ esplorazione neurologica, sia clinici che strumentali. Richiede una corretta metodologia e si basa sul rilievo contemporaneo del coma areattivo, dell’ assenza dei riflessi del tronco encefalico e della mancanza di respirazione spontanea in condizioni documentate di ipercapnia (test dell’ apnea). L’ esame clinico deve venire completato con indagini confirmatorie strumentali che consistono, sempre, nell’ elettroencefalogramma e, in casi particolari, da una prova di flusso cerebrale (angiografia, o altro esame specifico). Le indagini cliniche e strumentali possono essere attuate dopo aver avuto la certezza della causa del coma ed aver escluso o corretto eventuali fattori interferenti, di cui la presenza di farmaci neurodepressori è la più frequente. Per condurre l’ esame clinico e le indagini strumentali è necessaria la competente collaborazione infermieristica che assume anche un importante ruolo di allerta medica nel precoce rilievo dei segni di spegnimento delle attività encefaliche.

La nutrizione nel malato con insufficienza respiratoria Obiettivi del presente Capitolo sono i seguenti: 1. riconoscere l’ esposizione al rischio di malnutrizione dei pazienti con grave insufficienza respiratoria acutamente insorta o cronica; 2. conoscere le principali interazioni tra nutrienti, metabolismo e funzione polmonare da tenerli presenti nella corretta gestione nutrizionale; 3. rilevare le peculiarità che caratterizzano il supporto nutrizionale artificiale nei pazienti con ALI/ARDS e il potenziale terapeutico di recenti regimi specifici; 4. rilevare le analoghe caratteristiche del supporto nutrizionale nei malati con insufficienza respiratoria cronica stabile o esacerbata.