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HighlightsParents did not see themselves as role models for children regarding use of quad bikes.Parents seemed to misjudge their children’s maturity and capabilities.Risk acceptance was a common issue, due to risk normalization.There is a need for an age limit for drivers of adult-size quad bikes.Abstract.When seeking to explain the many accidents involving children on quad bikes, it is critical to understand the norms and risk perceptions of their parents, because parents are responsible for their children’s safety. This study explored attitudes and behavior among parents of rural children using quad bikes and their experiences of incidents and injuries. Information obtained from two focus group discussions, one with young adults and one with parents, and an in-depth interview with a quad bike distributor was used to develop an interview guide. The guide was used in telephone interviews with Swedish parents (n = 41) and some children ages 5 to 14 (n = 9) between autumn 2015 and spring 2016. Analysis of the results revealed eight themes: (1) how quad bikes are used, (2) risk awareness, (3) safety information could help other parents, (4) parents’ perception of children’s abilities, (5) children’s learning, (6) children`s perspective, (7) rules and responsibilities, and (8) risk acceptance. Major findings were that parents were aware of the risks and had a strong commitment to children’s safety, but also showed risk acceptance. To increase the safety of quad bike use, recommendations to organizations and authorities are presented, such as an age limit for drivers of all adult-size quad bikes and safety labeling of quad bikes, with information clarifying the rules for specific vehicles. Keywords: Acceptance, Accident, Agriculture, All-terrain vehicle, ATV, Awareness, Farm, Child, Incident, Parent, Quad bike, Risk, Rural, Sweden, Youth.

The proportion of elderly citizens is continuously increasing in most of the industrial world [...]

Svensk grisproduktion har genomgått stora förändringar och omstruktureringar under de senaste decennierna, vilket resulterat i allt färre företag. I dagsläget finns det drygt 1100 aktiva grisföretagare, spridda över landet. Trots strukturomvandlingen med allt fler stora specialiserade grisföretag finns det även en hel del företag med ett mindre antal djur. Föreliggande rapport med fokus på erfarenheter gällande arbetsförhållanden inom grisproduktionen baseras på svar från 288 företagare av totalt 814 (35%) möjliga och relevanta med angiven epostadress i SCB.s lantbruksregister. Av dessa var närmare 25% kvinnor och hälften av grisföretagarna hade varit verksamma mer än 20 år. Smågrisproduktion bedrevs av 20%, slaktsvinsproduktion 40% och integrerad produktion stod för 40% av svaren. Ca 90% av företagen bedrevs konventionellt, medan drygt 10% hade någon form av ekologisk produktion. Vidare framkom att mer än hälften av företagen hade anställd personal. En stor del av frågeställningarna i studien var inriktade på skador och hälsobesvär, goda exempel, problem samt lösningar och åtgärder vid olika arbetsmoment. Vad gäller utfodringsarbetet var det inte så vanligt med skador och hälsobesvär, men incidenter med galtar och sinsuggor, andningsbesvär och besvär i rörelseorganen rapporterades. Fördelar med automatisk utfodring och blötutfodring framhölls i en hel del svar. Problem vid utfodring gällde t ex: larm under nattetid, ständig jour och ensamarbete. Manuell utfodring där man bar spannar och utfodrade smågrisar framhölls som fysiskt påfrestande. De som hade utegrisar berättade att dåligt väder under höst och vinter kunde göra utfodringsarbetet tungt och besvärligt. Andra risker gällde bl.a. dammig miljö samt stress och skaderisker vid krånglande utfodringssystem. Vad gäller behov av åtgärder var det främst tekniska lösningar som önskades för att förbättra arbetsmiljön vid utfodringsarbetet. Vid utgödsling, rengöring/tvätt samt halmhantering framkom främst besvär gällande luftmiljöns påverkan på andningsorganen, oron för gödselgaser samt det påfrestande arbetet med maunell högtrycksrengöring. Vad gäller goda exempel framhöll man främst tvättroboten som ett hjälpmedel som verkligen förbättrade arbetsmiljön. Ett annat exempel var automatisk halmspridning och transport av halm på räls. Problem och förbättringsförslag gällde främst manuell högtrycksvätt och svårigheter med användning av andningsskydd vid detta arbete. Andra förbättringsbehov framkom gällande krånglande utgödslingsanläggningar och den slitsamma manuella skrapningen av boxar. Rapporter gällande skador och hälsobesvär vid skötsel av djur gällde bl.a. aggressiva suggor och incidenter vid vaccinationer. Kläm- och trampskador och handledsproblem vid arbete med smågrisar var också vanligt förekommande. Lugna djur och lugna djurskötare togs upp som goda exempel tillsammans med slopande av konventionell grisvägning. Problem som upplevdes var främst stora, tunga och ibland aggressiva djur, seminering och vaccinationer samt stämpling av djur och vägning. Behov av tekniska lösningar, t.ex. gällande vägning samt bättre avelsarbete framfördes. Andra arbetsuppgifter gällde djurhantering och djurförflyttning, där det främst rapporterades kläm-, halk- och bitskador. Kadavervagn, stora utlastningsrum och drivgångar var bland de goda exempel som framkom. Rapporter gällande problem handlade om avlivning av stora suggor och svårigheten att flytta stora tunga kroppar som låg illa till. Andra problem som förekom var flyttning av grisar vid dåligt väder och med okunnig personal samt urskiljning av slaktfärdiga grisar i boxarna. Tekniklösningar var det man främst tänkte sig för att förbättra arbetsmiljön, men mer personal underlättade också arbetet. Användning av personlig skyddsutrustning var ganska vanligt förekommande vid stallarbetet, främst stålhätta/skyddsskor, hörselskydd och andningsskydd, ca 60-80% använde detta, beroende på arbetsuppgift. Gaslarm användes på tre av de 34 arbetsplatser med vaccumutgödslingssystem, men flera skrev att de borde skaffa gaslarm. Andra viktiga faktorer i grisföretagarnas arbetsmiljö gällde personal och psykosociala aspekter. Svårigheter att hitta personal med lämplig kompetens var problematiskt, där man påpekade att språk och kommunikation var viktigt. När det gällde orosfaktorer var det främst ekonomin, djurrättsaktivister samt administrativa krav som upplevdes som påfrestande. Bland de faktorer som skapar arbetsglädje var välmående djur, välfungerande personal och goda produktionsresultat det som flest uppskattade. Studiens resultat har visat att det fortfarande finns arbetsmiljöproblem inom svensk grisproduktion, men att det i många fall även finns goda exempel på tekniska och organisatoriska lösningar. Ett bra exempel är arbetet med tvätt av stallar som upplevs som väldigt påfrestande vid manuell högtryckstvätt, medan tvättrobotar upplevs som en stor förbättring. Andra tekniska lösningar med stor potential att förbättra arbetsmiljön är automatiska halmfördelningssystem , automatiserad vägning och kvalitetsförbättrade utgödslingssystem. Även bättre design och ergonomi för handhållna hjälpmedel för vaccinationer, tandslipning och märkning hade varit till stor nytta. Luftmiljön i grisstall behöver fortsatt utveckling och förbättring och så länge det inte finns optimala lösningar är det viktigt med bra andningsskydd som är enkla och bekväma att använda. Användningen av tillförlitliga gaslarm i alla stallar med vaccumutgödsling borde vara självklart och obligatoriskt. Det är viktigt att inte glömma vikten av att grisnäringen har tillgång till kompetent och motiverad stallpersonal, vilket kan vara ett problem för en del av de medverkande företagarna. Att ha goda ekonomiska förutsättningar, uppleva trygghet mot att drabbas av aktivism, friska djur och en minskad byråkrati hade gjort livet ännu bättre för Sveriges grisproducenter!

Z globalnego punktu widzenia rolnictwo jest jednym z najbardziej niebezpiecznych sektorów gospodarki. Podobna sytuacja ma miejsce również w Szwecji, gdzie występuje wiele wypadków – zarówno ze skutkiem śmiertelnym, jak i zakończone obrażeniami ciała. Celem niniejszego artykułu jest próba dokonania całościowej oceny krajowego programu interwencyjnego na rzecz zapobiegania urazom (2009–2013). Aby osiągnąć ten cel, zbadano rozwój wypadków śmiertelnych przy pracy w szwedzkim rolnictwie w okresie 15 lat: pięć lat przed wdrożeniem programu prewencyjnego, podczas jego trwania i pięć lat po zakończeniu programu. W artykule wykorzystano zarówno statystyki oficjalne, jak i nieoficjalne, oparte na publikacjach prasowych. Wyniki analizy wykazały spadek liczby ofiar śmiertelnych o około 45% w ciągu pięciu lat trwania programu prewencyjnego (według oficjalnych statystyk). Efekt ten jednak prawie zanikł w okresie pięciu lat po zakończeniu ww. programu. Po dodaniu informacji z publikacji prasowych ukazuje się szerszy obraz wypadków śmiertelnych w rolnictwie z uwzględnieniem dzieci, osób odwiedzających, a także wypadków niezwiązanych z pracą. W artykule omówiono rekomendacje dotyczące znaczenia długoterminowych programów, możliwości zdigitalizowanego systemu BHP dla rolników, współpracy międzynarodowej oraz wartości strategii „Wizja Zero” stworzonej przez Międzynarodową Sekcję ISSA ds. Prewencji w Rolnictwie.

Swedish media have revealed an increase in crimes against animal production (CAAP) in the last decade. We investigate the nature of such crimes (especially against mink, pig, and rabbit farms), with a focus on those crimes whose suspects are animal rights groups by utilizing data from media archives from 2009 to 2019. Newspaper articles show that while vandalism and trespassing are often committed against mink farms, property crimes occur more often against pig and rabbit farms. Because there are indications that crime suspects are not a homogeneous group and express different motivations to commit CAAP, a multipronged approach is needed to prevent CAAP. The use of newspaper articles from media archives has proven to be successful for obtaining a general perspective of CAAP, but it is limited for capturing crime incidence or for investigating CAAP spatiotemporal nature when using geographical information systems. The automated usage of digital media archives should be further explored and critically assessed in future research in criminology. QC 20211206

In this article, we investigate the nature of fear among farmers working with animal production with particular focus on the impact of harassment and crimes linked to animal rights activism. The study is based on responses from 3815 animal farmers to a national survey in 2020 in Sweden. Cross-table analysis and logistic regression models underlie the methodology of the study. Findings show that three out of ten of those farmers feel afraid of being victimized by the actions of animal rights activists; the proportion is two-thirds among farmers with previous experience of victimization, and fear of victimization varies across Sweden and by type of activity. Perceived lack of support from the police, exacerbated by geographical isolation, are common determinants of farmers’ declared fear, particularly those whose families live on the farms and who have employees. While understanding the factors that affect farmers’ safety perceptions is important, the article ends by calling for further research on the ways by which fear of animal activism impacts farmers’ personal lives, those of their family and employees, and not least their livelihood.

The occupational injury rate of the dairy industry (6.6 per 100 full-time workers) is twice that of the national average across all industries (3.3 per 100 full-time workers). While dairy farms are becoming larger in size and fewer in number, this rate has not changed. A scoping review was conducted to identify published reports of occupational safety interventions in the dairy industry. An additional criterion was that the study included an evaluation of the intervention. Out of 22 articles that met the first criterion (discussion of interventions specific to the dairy industry), 19 met the second of having an evaluative component. These 19 articles corresponded to 16 unique studies, because 4 articles corresponded to the same study. Of the 16 unique studies, only 3 had a comparison of treatment vs. control effects, and none measured the impact of the intervention on injuries and fatalities. Of the 16 interventions, 6 were focused on training or informational campaigns in which the evaluations primarily measured knowledge acquisition. Additionally, none of these studies had a sufficient sample size to compare injury rates as an outcome. Our study demonstrates that the literature lacks any rigorous evaluation of whether dairy safety interventions are making an impact on injury prevention. Given this, it is not possible to determine how work-related injuries and deaths can be prevented in the dairy industry. Recommendations for future research include incorporating rigorous evaluation into research designs and attempting to develop low-cost, unobtrusive methods for collecting data on intermediate and final outcomes.

We present observations of the pulsar-wind nebula (PWN) region ofSNR 0540-69.3. The observations were made with the Atacama Compact Array (ACA) in Bands 4 and 6. We also add radio observations from the Australia Compact Array (ATCA) at 3 cm. For 1.449 - 233.50 GHz we obtain a synchrotron spectrum $F_{\nu} \propto \nu^{-\alpha_{\nu}}$, with the spectral index $\alpha_{\nu} = 0.17\pm{0.02}$. To conclude how this joins the synchrotron spectrum at higher frequencies we include hitherto unpublished AKARI mid-infrared data, and evaluate published data in the ultraviolet (UV), optical and infrared (IR). In particular, some broad-band filter data in the optical must be discarded from our analysis due to contamination by spectral line emission. For the UV/IR part of the synchrotron spectrum, we arrive at $\alpha_{\nu} = 0.87^{+0.08}_{-0.10}$. There is room for $2.5\times10^{-3}$ solar masses of dust with temperature $\sim 55$ K if there are dual breaks in the synchrotron spectrum, one around $\sim 9\times10^{10}$ Hz, and another at $\sim 2\times10^{13}$ Hz. The spectral index then changes at $\sim 9\times10^{10}$ Hz from $\alpha_{\nu} = 0.14\pm0.07$ in the radio, to $\alpha_{\nu} = 0.35^{-0.07}_{+0.05}$ in the millimetre to far-IR range. The ACA Band 6 data marginally resolves the PWN. In particular, the strong emission 1.5" south-west of the pulsar, seen at other wavelengths, and resolved in the 3-cm data with its 0.8" spatial resolution, is also strong in the millimeter range. The ACA data clearly reveal the supernova remnant shell 20-35 arcsec west of the pulsar, and for the shell we derive $\alpha_{\nu} = 0.64\pm{0.05}$ for the range $8.6-145$~GHz., Comment: MNRAS, accepted

Conflicts between animal production and animal rights activism are becoming more common in a number of countries, including Sweden. Although most animal rights advocates would not consider committing a crime, there have been numerous accounts in which farmers have been victimized because they are animal producers. This study investigates the extent and characteristics of crimes committed against animal farmers and their families. The analysis is based on answers from a survey of 3,815 animal farmers in Sweden in 2020. Cross-table analysis, logistic regression models, and geographical information systems (GIS) underlie the methodology of the study. One in eight respondents declared being exposed to crimes because they are animal producers (from thefts, trespassing, sabotage, and threats to physical violence, most face-to-face but also online), but 60 percent of the victims never report to the police. Among nonvictims, half of the respondents knew someone who had been a victim of crime. Findings indicate that farmers’ victimization for theft or robbery show different motivations than those that are directed at them because they work with animal production. These findings highlight the importance of incorporating farmers’ safety needs into sustainable rural development policies. QC 20220221

Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf (WD) stars destabilized by mass accretion from a companion star, but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds or binary interaction prior to explosion, and the SN ejecta crashing into this nearby circumstellar material (CSM) should result in radio synchrotron emission. However, despite extensive efforts, no SN Ia has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate WD star. Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich CSM, as revealed by its spectral features, infrared emission and, for the first time in a SN Ia, a radio counterpart. Based on our modeling, we conclude the CSM likely originates from a single-degenerate (SD) binary system where a WD accretes material from a helium donor star, an often hypothesized formation channel for SNe Ia. We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems., Comment: 62 pages, 10 figures, 4 tables

Agriculture and forestry are among the most dangerous professions in Europe, with a high level of accidents affecting the sustainability and viability of the sector. International conventions, EU directives and national legislation build the fundamental basis for prevention. The aim of the study is to describe and categorize national mechanisms of occupational safety and health (OSH) for agricultural workers in Europe, to assess the extent of implementing safety regulation, the body in charge, and to give examples of health and safety initiatives.Results of a questionnaire-survey on basic safety regulations on farms sent by e-mail to the representatives of 30 participating European countries in the context of the Sacurima COST action network (CA 16123) are presented. Due to the complexity, only selected countries are described in this study highlighting the regulative bodies, occupational health services or specific training offers, as well as the complexity of the mechanisms.One of the most serious issues and deficits of EU OSH regulation is the exclusion of self-employed farmers who compose nearly 90% of the farming population. This leads to serious under-reporting of accidents, and because one of the most common measures for the performance of health and safety initiatives are the injury and ill health statistics, better registration systems are urgently needed in almost all countries as a basis for preventive efforts.The results of the study provide a basis for raising awareness about the current OSH systems in Europe, and the importance of developing sector specific OSH strategies. The proposed activities should assist in tackling high accident rates and poor occupational health for self-employed farmers.

The structure, elemental abundances, physical conditions of the LMC supernova remnant (SNR) 0540-69.3 and its surroundings were investigated using [O III] imaging and spectroscopy. Several new spectral lines are identified, both in central filaments and in interstellar clouds shocked by the supernova blast wave. The central lines are redshifted by $440\pm80$ km s$^{-1}$ with respect to the LMC, and the [O III] emission displays a symmetry axis of ring-like structures which could indicate that the pulsar shares the same general redshift as the central supernova ejecta. [O II], [S II], [Ar III] and H$\beta$ have more compact structures than [O III], and possibly [Ne III]. The average [O III] temperature is $23\,500 \pm 1\,800$ K, and the electron density from [S II] is typically $10^3$ cm$^{-3}$. By mass, the relative elemental abundances of the central shocked ejecta are ${\rm O:Ne:S:Ar} \approx 1:0.07:0.10:0.02$, consistent with explosion models of $13-20$ solar mass progenitors, and similar to that of SN 1987A, as is also the mixing of hydrogen and helium into the center. [O III] is also seen in freely coasting ejecta outside the pulsar-wind nebula out to well above $2\,000$ km s$^{-1}$. From this a pulsar age of $\approx 1\,200$ years is estimated. Four filaments of shocked interstellar medium with a wide range in degree of ionization of iron are identified. One was observed in X-rays, and another has a redshift of $85\pm30$ km~s$^{-1}$ relative to LMC. From this the electron density of the [O III]-emitting gas is estimated to be $10^3$ cm$^{-3}$. The line of the most highly ionized ion, [Fe XIV] $\lambda$5303, likely comes from an evaporation zone in connection with the radiatively cooled gas emitting, e.g., [O III]., Comment: Submitted to Astronomy and Astrophysics Aug. 2, 2021. 30 pages, 26 figures and 5 tables

Cay, Y. Z., et al., 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 × 1040 erg s-1 and their total radiated energies are on the order of (0.3-3) × 1047 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 56Co decay. If the late-time power source is indeed radioactive decay, these transients produce 56Ni masses on the order of 10-4 to 10-3 M⊙. 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] λ7291,7324 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.

Background: This paper provides background and a process description for a national initiative ('Safe Farmer Common Sense') on prevention of occupational injuries in Swedish agriculture.Methods: This initiative, which received investment funding of 65 million SEK (6.5 million USD) from the European Union (EU) over the 5-year period 2009-2013, was jointly developed by researchers, agricultural organizations, authorities, and politicians. The program had a farmer-centered perspective and included short courses, on-farm visits by supervisors, and a number of education events and awareness-promoting activities.Results: Our analysis showed that the concept was successful, since it involved farmers to a greater extent and prompted a high proportion of these to introduce injury prevention measures on their farms compared with a control group. The analysis also confirmed that these activities continued two-three years after participation in the program.Conclusion: The program was not found to have any major effect on the number of occupational injuries, although the level of occupational fatalities was lower during the intervention period. Thus the investment can be questioned as regards the limited impact on the number of work-related injuries in Swedish agriculture and may have been too short to have a lasting effect.

We present high-cadence optical and ultraviolet light curves of the normal Type Ia supernova (SN) 2021aefx, which shows an early bump during the first two days of observation. This bump may be a signature of interaction between the exploding white dwarf and a nondegenerate binary companion, or it may be intrinsic to the white dwarf explosion mechanism. In the case of the former, the short duration of the bump implies a relatively compact main-sequence companion star, although this conclusion is viewing-angle dependent. Our best-fit companion-shocking and double-detonation models both overpredict the UV luminosity during the bump, and existing nickel-shell models do not match the strength and timescale of the bump. We also present nebular spectra of SN 2021aefx, which do not show the hydrogen or helium emission expected from a nondegenerate companion, as well as a radio nondetection that rules out all symbiotic progenitor systems and most accretion disk winds. Our analysis places strong but conflicting constraints on the progenitor of SN 2021aefx; no current model can explain all of our observations., Comment: updated to match accepted version

ASASSN-18am/SN 2018gk is a newly discovered member of the rare group of luminous, hydrogen-rich supernovae (SNe) with a peak absolute magnitude of MV ≈ −20 mag that is in between normal core-collapse SNe and superluminous SNe. These SNe show no prominent spectroscopic signatures of ejecta interacting with circumstellar material (CSM), and their powering mechanism is debated. ASASSN-18am declines extremely rapidly for a Type II SN, with a photospheric-phase decline rate of ∼6.0 mag (100 d)−1. Owing to the weakening of H i and the appearance of He i in its later phases, ASASSN-18am is spectroscopically a Type IIb SN with a partially stripped envelope. However, its photometric and spectroscopic evolution shows significant differences from typical SNe IIb. Using a radiative diffusion model, we find that the light curve requires a high synthesized 56Ni mass $M_{\rm Ni} \sim 0.4\, \rm {M_{\odot }}$ and ejecta with high kinetic energy Ekin = (7–10) × 1051 erg. Introducing a magnetar central engine still requires $M_{\rm Ni} \sim 0.3\, \rm {M_{\odot }}$ and Ekin = 3 × 1051 erg. The high 56Ni mass is consistent with strong iron-group nebular lines in its spectra, which are also similar to several SNe Ic-BL with high 56Ni yields. The earliest spectrum shows ‘flash ionization’ features, from which we estimate a mass-loss rate of $\dot{M}\approx 2\times 10^{-4} \, \rm \rm {M_{\odot }}\,yr^{-1}$. This wind density is too low to power the luminous light curve by ejecta–CSM interaction. We measure expansion velocities as high as 17 000 $\rm {\, km\, s^{-1}}$ for Hα, which is remarkably high compared to other SNe II. We estimate an oxygen core mass of 1.8–3.4 M⊙ using the [O i] luminosity measured from a nebular-phase spectrum, implying a progenitor with a zero-age main-sequence mass of 19–26 M⊙.

We are now well into the year 2021 - fully into a new decade, and still, those who work in agriculture do so at great risk serving an industry with one of the highest rates of fatalities worldwide....

Context The Swedish Transport Administration together with major stakeholders including researchers from the Swedish University of Agricultural Sciences (SLU) developed a joint up-dated strategy for safe use of Quadbikes. Process and analysis An evaluation of the previous strategy (2014–2020) was done regarding injury statistics, the development of safety features, education, training and research both in Sweden and at an international level. The development in Australia regarding ‘Crush Protection Device (CPD)’ on Quads was one of the major developments since last strategy. Outcome The joint strategy prioritize a number of areas for further actions: a) Increased use of helmets, b) Increased use of Crush Protection Device (CPD) c) Increased use of alcohol interlocks, d) Decreased use of Quads on public roads, e) Children should not be using Quads and f) Improved information and increased education and training regarding risk awareness and safe driving. The strategy also points out the importance of further research, development and information regarding the Crush Protection Device (CPD); alternative vehicles such as side-by-sides, small tractors or off-road motorcycles; the development and use of warning/alarm systems for roll-over situations; children and Quad bikes; risks with passengers and loads as well as further education and training issues. Each of the stakeholders stated their ambitions in order to reach the joint goal to reduce the number of fatalities with 50% by the year 2030. SLU will now work with a full-scale test with Crush Protection Device (CPD) on Quad bikes, mainly during off-road use, with 100 professional users.

Background Farmers with animal production in Sweden can experience different types of criticisms directed against their activities from consumers, the media and inspecting government agencies. On another level, threats, damage, tampering, robbery and other criminal acts are directed against the farm’s activities, but also against the farmer, family members and employees. The farmers organization state the problems as a major health & safety issue. The goal is to investigate the nature of the experiences of threats, crimes and criticism against animal production in Sweden. Methods The research is achieved by assessing the consequences for individuals and farms, health, social and economic conditions. Interviews with farmers, web-based enquieries, data from official statistics and media coverage will underlie the methodology of this study. We focus on farmers not as ‘victims’ but rather as ‘active agents’, by illustrating ways that farmers handle, cope and respond to the criticisms and threats they are exposed in a daily basis. Results Preliminary results of our ongoing research show that farmers of all types of animal production feel an increased level of worries and stress due to rural crime and external critizism. They also report that family members and employees are affected. Farmers try to cope with the new stress by investments in increased security measures at the farm, interacting more with other farmers, but also less public contacts. Learning Outcomes It is obvious that rural crime and external critizism is adding further stress to the daily life of animal farmers and needs to be further investigated

We present the follow-up campaign of the luminous red nova (LRN) AT 2019zhd, the third event of this class observed in M 31. The object was followed by several sky surveys for about five months before the outburst, during which it showed a slow luminosity rise. In this phase, the absolute magnitude ranged from Mr =-2.8 ± 0.2 mag to Mr =-5.6 ± 0.1 mag. Then, over a four to five day period, AT 2019zhd experienced a major brightening, reaching a peak of Mr =-9.61 ± 0.08 mag and an optical luminosity of 1.4 × 1039 erg s-1. After a fast decline, the light curve settled onto a short-duration plateau in the red bands. Although less pronounced, this feature is reminiscent of the second red maximum observed in other LRNe. This phase was followed by a rapid linear decline in all bands. At maximum, the spectra show a blue continuum with prominent Balmer emission lines. The post-maximum spectra show a much redder continuum, resembling that of an intermediate-type star. In this phase, Hα becomes very weak, Hβ is no longer detectable, and a forest of narrow absorption metal lines now dominate the spectrum. The latest spectra, obtained during the post-plateau decline, show a very red continuum (Teff ≈ 3000 K) with broad molecular bands of TiO, similar to those of M-type stars. The long-lasting, slow photometric rise observed before the peak resembles that of LRN V1309 Sco, which was interpreted as the signature of the common-envelope ejection. The subsequent outburst is likely due to the gas outflow following a stellar merging event. The inspection of archival HST images taken 22 years before the LRN discovery reveals a faint red source (MF555W = 0.21 ± 0.14 mag, with F555W-F814W = 2.96 ± 0.12 mag) at the position of AT 2019zhd, which is the most likely quiescent precursor. The source is consistent with expectations for a binary system including a predominant M5-type star.

We present the discovery with Keck of the extremely infrared (IR) luminous transient AT 2017gbl, coincident with the Northern nucleus of the luminous infrared galaxy (LIRG) IRAS 23436+5257. Our extensive multiwavelength follow-up spans similar to 900 d, including photometry and spectroscopy in the optical and IR, and (very long baseline interferometry) radio and X-ray observations. Radiative transfer modelling of the host galaxy spectral energy distribution and long-term pre-outburst variability in the mid-IR indicate the presence of a hitherto undetected dust obscured active galactic nucleus (AGN). The optical and near-IR spectra show broad similar to 2000 km s(-1) hydrogen, He I, and OI emission features that decrease in flux over time. Radio imaging shows a fast evolving compact source of synchrotron emission spatially coincident with AT 2017gbl. We infer a lower limit for the radiated energy of 7.3 x 10(50) erg from the IR photometry. An extremely energetic supernova would satisfy this budget, but is ruled out by the radio counterpart evolution. Instead, we propose AT 2017gbl is related to an accretion event by the central supermassive black hole, where the spectral signatures originate in the AGN broad line region and the IR photometry is consistent with re-radiation by polar dust. Given the fast evolution of AT 2017gbl, we deem a tidal disruption event (TDE) of a star a more plausible scenario than a dramatic change in the AGN accretion rate. This makes AT 2017gbl the third TDE candidate to be hosted by a LIRG, in contrast to the so far considered TDE population discovered at optical wavelengths and hosted preferably by post-starburst galaxies., ECKacknowledges support from the Gravitational Radiation and Electromagnetic Astrophysical Transients (GREAT) research environment funded by Vetenskapsradet under project no. 2016-06012, financial support from the visitor and mobility program of the Finnish Centre for Astronomy with ESO (FINCA), funded by the Academy of Finland grant no. 306531, and support from The Wenner-Gren Foundations under project no. UPD2019-0070. TMR acknowledges the financial support of the Jenny and Antti Wihuri foundation and the Vilho, Yrjo and Kalle Vaisala Foundation of the Finnish Academy of Science and Letters. MPT acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofisica de Andaluc ' ia (SEV-2017-0709) and through grant PGC2018-098915-B-C21 (MCI/AEI/FEDER). CRC acknowledges support by the Chinese Academy of Sciences (CAS), through grant CAS16013 of the CAS South America Center for Astronomy (CASSACA) and Programa de Astronomia CONICYT, Chile. PGJ and GC acknowledge support from European Research Council Consolidator Grant 647208. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. GEA is the recipient of an Australian Research Council Discovery Early Career Researcher Award (project DE180100346) and acknowledges partial support through the Australian Research Council's Discovery Projects funding scheme (project DP200102471). ST acknowledges financial support from the Russian Foundation for Basic Research project 1752-80139 BRICS-a. RMcD is the recipient of an Australian Research Council Future Fellowship Award (project number FT150100333). WL is supported by the David and Ellen Lee Fellowship at Caltech. The NOT Unbiased Transient Survey 2 (NUTS2) is funded in part by the Instrument Center for Danish Astronomy. Some of the data (PI: S. Ryder; program IDs Z229N2L, Z271N2L) presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authorswish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank the Mullard Radio Astronomy Observatory for carrying out the AMI-LA observations. Thiswork is based in part on observations (PIs: E. Kool, K. Maeda; program IDs GN-2017B-DD-2, GN-2018B-FT-109) obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). The scientific results reported in this article are based in part on observations (PI: T. Heikkila; program ID 18208589) made by the Chandra X-ray Observatory, and this research has made use of the CIAO software package provided by the ChandraX-rayCenter (CXC). This article includes results based on observations made by the Neil Gehrels Swift observatory. The authors thank Chandra and Swift teams for the approval and rapid scheduling of our observations. This work is based in part on observations made with theWilliam Herschel Telescope (WHT). The WHT is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The ISIS and ACAM data were obtained as part of (17A)N4/N6, (18A)N4, and (18B)N5. This work is based in part on observations (PI: S. Mattila; program IDs 13226, 14054) made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This work is based in part on observations from programs RP028B and BP225 (PI: M. Perez-Torres) obtained with the European VLBI Network (EVN) and the Very Long Baseline Array (VLBA), respectively. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, theMax Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the MaxPlanck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.

We present X-ray and radio observations of the Fast Blue Optical Transient (FBOT) CRTS-CSS161010 J045834-081803 (CSS161010 hereafter) at t=69-531 days. CSS161010 shows luminous X-ray ($L_x\sim5\times 10^{39}\,\rm{erg\,s^{-1}}$) and radio ($L_{\nu}\sim10^{29}\,\rm{erg\,s^{-1}Hz^{-1}}$) emission. The radio emission peaked at ~100 days post transient explosion and rapidly decayed. We interpret these observations in the context of synchrotron emission from an expanding blastwave. CSS161010 launched a mildly relativistic outflow with velocity $\Gamma\beta c\ge0.55c$ at ~100 days. This is faster than the non-relativistic AT2018cow ($\Gamma\beta c\sim0.1c$) and closer to ZTF18abvkwla ($\Gamma\beta c\ge0.3c$ at 63 days). The inferred initial kinetic energy of CSS161010 ($E_k\gtrsim10^{51}$ erg) is comparable to that of long Gamma Ray Bursts (GRBs), but the ejecta mass that is coupled to the mildly relativistic outflow is significantly larger ($\sim0.01-0.1\,\rm{M_{\odot}}$). This is consistent with the lack of observed gamma-rays. The luminous X-rays were produced by a different emission component to the synchrotron radio emission. CSS161010 is located at ~150 Mpc in a dwarf galaxy with stellar mass $M_{*}\sim10^{7}\,\rm{M_{\odot}}$ and specific star formation rate $sSFR\sim 0.3\,\rm{Gyr^{-1}}$. This mass is among the lowest inferred for host-galaxies of explosive transients from massive stars. Our observations of CSS161010 are consistent with an engine-driven aspherical explosion from a rare evolutionary path of a H-rich stellar progenitor, but we cannot rule out a stellar tidal disruption event on a centrally-located intermediate mass black hole. Regardless of the physical mechanism, CSS161010 establishes the existence of a new class of rare (rate $, Comment: Accepted to ApJL

We present observations of the unusually luminous Type II supernova (SN) 2016gsd. With a peak absolute magnitude of V = -19.95 ± 0.08, this object is one of the brightest Type II SNe, and lies in the gap of magnitudes between the majority of Type II SNe and the superluminous SNe. Its light curve shows little evidence of the expected drop from the optically thick phase to the radioactively powered tail. The velocities derived from the absorption in H α are also unusually high with the blue edge tracing the fastest moving gas initially at 20 000 km s-1, and then declining approximately linearly to 15 000 km s-1 over ∼100 d. The dwarf host galaxy of the SN indicates a low-metallicity progenitor which may also contribute to the weakness of the metal lines in its spectra. We examine SN 2016gsd with reference to similarly luminous, linear Type II SNe such as SNe 1979C and 1998S, and discuss the interpretation of its observational characteristics. We compare the observations with a model produced by the jekyll code and find that a massive star with a depleted and inflated hydrogen envelope struggles to reproduce the high luminosity and extreme linearity of SN 2016gsd. Instead, we suggest that the influence of interaction between the SN ejecta and circumstellar material can explain the majority of the observed properties of the SN. The high velocities and strong H α absorption present throughout the evolution of the SN may imply a circumstellar medium configured in an asymmetric geometry., MF acknowledges the support of a Royal Society – Science Foundation Ireland University Research Fellowship. The JEKYLL simulations were performed on resources provided by the Swedish National Infrastructure for Computing (SNIC) at Parallelldatorcentrum (PDC). PL acknowledges support from the Swedish Research Council. MS is supported by a generous grant (13261) from Villum Fonden and a project grant (8021-00170B) from the Independent Research Fund Denmark (IRFD). NUTS2 is funded in part by the Instrument Center for Danish Astronomy (IDA). This work is based (in part) on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO (the Public ESO Spectroscopic Survey for Transient Objects) ESO program 188.D−3003, 191.D−0935, more ESO acknowledgements. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST−1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. The SCUSS is funded by the Main Direction Program of Knowledge Innovation of Chinese Academy of Sciences (No. KJCX2−EW−T06). It is also an international cooperative project between National Astronomical Observatories, Chinese Academy of Sciences, and Steward Observatory, University of Arizona, USA. Technical support and observational assistance from the Bok telescope are provided by Steward Observatory. The project is managed by the National Astronomical Observatory of China and Shanghai Astronomical Observatory. Data resources are supported by Chinese Astronomical Data Center (CAsDC). SD and PC acknowledge Project 11573003 supported by NSFC. This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories of China, the Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance. SJS acknowledges STFC grant ST/P000312/1. This work has made use of data from the Asteroid Terrestial-impact Last Alert System (ATLAS) Project. ATLAS is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogues from the survey area. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s Univeristy Belfast, the Space Telescope Science Institute, and the South African Astronomical Observatory. OR acknowledges support by projects IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Iniciativa Científica Milenio del Ministerio de Economía, Fomento y Turismo de Chile and CONICYT PAI/INDUSTRIA 79090016. JH acknowledges financial support from the Finnish Cultural Foundation. Some data were taken with the Las Cumbres Observatory Network. GH and DAH are supported by NSF grant AST-1313484. GH thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. 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 also makes use of observations collected at the European Southern Observatory under ESO programme 0103.D-0338(A). CPG acknowledges support from EU/FP7-ERC grant no. [615929].

Full author list: L. Tartaglia, A. Pastorello, J. Sollerman, C. Fransson, S. Mattila, M. Fraser, F. Taddia, L. Tomasella, M. Turatto, A. Morales-Garoffolo, N. Elias-Rosa, P. Lundqvist, J. Harmanen, T. Reynolds, E. Cappellaro, C. Barbarino, A. Nyholm, E. Kool, E. Ofek, X. Gao, Z. Jin, H. Tan, D. J. Sand, F. Ciabattari, X. Wang, J. Zhang, F. Huang, W. Li, J. Mo, L. Rui, D. Xiang, T. Zhang, G. Hosseinzadeh, D. A. Howell, C. McCully, S. Valenti, S. Benetti, E. Callis, A. S. Carracedo, C. Fremling, T. Kangas, A. Rubin, A. Somero and G. Terreran, In this paper we report the results of the first ~four years of spectroscopic and photometric monitoring of the Type IIn supernova SN 2015da (also known as PSN J13522411+3941286, or iPTF16tu). The supernova exploded in the nearby spiral galaxy NGC 5337 in a relatively highly extinguished environment. The transient showed prominent narrow Balmer lines in emission at all times and a slow rise to maximum in all bands. In addition, early observations performed by amateur astronomers give a very well-constrained explosion epoch. The observables are consistent with continuous interaction between the supernova ejecta and a dense and extended H-rich circumstellar medium. The presence of such an extended and dense medium is difficult to reconcile with standard stellar evolution models, since the metallicity at the position of SN 2015da seems to be slightly subsolar. Interaction is likely the mechanism powering the light curve, as confirmed by the analysis of the pseudo bolometric light curve, which gives a total radiated energy ≳ 1051 erg. Modeling the light curve in the context of a supernova shock breakout through a dense circumstellar medium allowed us to infer the mass of the prexisting gas to be ≂ 8 MO , with an extreme mass-loss rate for the progenitor star ≂ 0.6 MO yr-1, suggesting that most of the circumstellar gas was produced during multiple eruptive events. Near- and mid-infrared observations reveal a fluxexcess in these domains, similar to those observed in SN 2010jl and other interacting transients, likely due to preexisting radiatively heated dust surrounding the supernova. By modeling the infrared excess, we infer a mass ≳ 0.4 × 10-3 MO for the dust., The Oskar Klein Centre is funded by the Swedish Research Council. We acknowledge the support of the staff of the Xinglong 2.16 m telescope. This work was partially supported by the Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences. M.F. is supported by a Royal Society – Science Foundation Ireland University Research Fellowship. J.H. acknowledges financial support from the Finnish Cultural Foundation and the Vilho, Yrjö and Kalle Väisälä Foundation of the Finnish Academy of Science and Letters. Research by D.J.S. is supported by NSF grants AST-1821987, AST-1821967, AST-1813708, AST-1813466 and AST-1908972. S.B., L.T.and M.T. are partially supported by the PRIN-INAF 2016 with the project “Towards the SKA and CTA era: discovery, localisation, and physics of transient sources” (PI: M. Giroletti). N E.-R. acknowledges support from the Spanish MICINN grant ESP2017–82674–R and FEDER funds. D.A.H., C.M., and G.H. were supported by NSF AST-1313484 The work of X.W. is supported by the National Natural Science Foundation of China (NSFC grants 11325313, 11633002, and 11761141001), and the National Program on Key Research and Development Project (grant no. 2016YFA0400803). Research by S.V. is supported by NSF grant AST-1813176. J.Z. is supported by the National Natural Science Foundation of China (NSFC, grants 11773067, 11403096), the Youth Innovation Promotion Association of the CAS (grants 2018081), and the Western Light Youth Project. Based on observations collected at: ESO La Silla Observatory under program “Optical & NIR monitoring of bright supernovae with REM” during AOT30. The Gemini Observatory, under program GN– 2016B-Q-57, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Tthe Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association and the Gran Telescopio Canarias (GTC), both installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofìsica de Canarias, on the island of La Palma (Spain). The Copernico Telescope (Asiago, Italy) operated by INAF – Osservatorio Astronomico di Padova. The 3 m Shane Reflector, located at the Lick Observatory (7281 Mt Hamilton Rd, Mt Hamilton, CA 95140, USA.) owned and operated by the University of California. This work makes use of observations from the Las Cumbres Observatory network of telescopes. We acknowledge the support of the staff of the Li–Jiang 2.4 m telescope (LJT). Funding for the LJT has been provided by the Chinese Academy of Sciences (CAS) and the People’s Government of Yunnan Province. The LJT is jointly operated and administrated by Yunnan Observatories and Center for Astronomical Mega–Science, CAS. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This publication makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, founded by the Planetary Science Division of the National Aeronautics and Space Administration. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. 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. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. The intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. IRAF is distributed by the 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. SNOOPY is a package for SN photometry using PSF fitting and/or template subtraction developed by E. Cappellaro. A package description can be found at http:// sngroup.oapd.inaf.it/snoopy.html. FOSCGUI is a graphic user interface aimed at extracting SN spectroscopy and photometry obtained with FOSC-like instruments. It was developed by E. Cappellaro. A package description can be found at http://sngroup.oapd.inaf.it/foscgui.html

We report deep radio observations of nearby Type Ia supernovae (SNe Ia) with the electronic Multi-Element Radio Linked Interferometer Network and the Australia Telescope Compact Array. No detections were made. With standard assumptions for the energy densities of relativistic electrons going into a power-law energy distribution and the magnetic field strength ( e = B = 0.1), we arrive at upper limits on mass-loss rate for the progenitor system of SN 2013dy (SN 2016coj, SN 2018gv, SN 2018pv, SN 2019np) of, where v w is the wind speed of the mass loss. To SN 2016coj, SN 2018gv, SN 2018pv, and SN 2019np we add radio data for 17 other nearby SNe Ia and model their nondetections. With the same model as described, all 21 SNe Ia have. We compare those limits with the expected mass-loss rates in different single-degenerate progenitor scenarios. We also discuss how information on e and B can be obtained from late observations of SNe Ia and the youngest SN Ia remnant detected in radio, G1.9+0.3, as well as stripped-envelope core-collapse SNe. We highlight SN 2011dh and argue for e ≈ 0.1 and B ≈ 0.0033. Finally, we discuss strategies to observe at radio frequencies to maximize the chance of detection, given the time since explosion, the distance to the SN, and the telescope sensitivity. © 2020. The American Astronomical Society. All rights reserved., We thank Subo Dong for sharing data for SN.2018gv and SN 2018pv prior to publication, Stephen Reynolds for discussions and comments on an early version of the manuscript, and Nancy Elias-Rosa for discussions on SN.2019np. P. L. acknowledges support from the Swedish Research Council, and M.P.T. acknowledges financial support from the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709) and through the MINECO grants AYA2012-38491-C02-02 and AYA2015-63939-C2-1-P. J.M. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709) and from the grant RTI2018-096228-B-C31 (MICIU/FEDER, EU). The research leading to these results has received funding from the European Commission Horizon 2020 Research and Innovation Programme under grant agreement No. 730562 (RadioNet). The electronic Multi-Element Radio Linked Interferometer Network (e-MERLIN) is the UK's facility for high-resolution radio astronomy observations, operated by the University of Manchester for the Science and Technology Facilities Council (STFC). The Australia Telescope Compact Array (ATCA) is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. The ATCA data reported here were obtained under program C1303 (P.I. P. Lundqvist). This research has made use of the NASA Astrophysics Data System (ADS) Bibliographic Services and 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.

Strong acid accidental ingestion is a common case in rural society and children. The effect of strong acids may cause injuries of the gastrointestinal tract. We present a case obstruction in the distal part of gastric after accidental sulfuric acid ingestion in children. Sulfuric acid ingestion is potential in children since its commercial product physical appearance looks like drink water. Then the patient was diagnosed with pyloric obstruction after barium meal examination and was treated using Jaboulay gastroduodenostomy procedure.

We present optical photometric and spectroscopic observations of the faint-and-fast evolving type Iax SN 2019gsc, extending from the time of g-band maximum until about fifty days post maximum, when the object faded to an apparent r-band magnitude m_r = 22.48+/-0.11 mag. SN 2019gsc reached a peak luminosity of only M_g = -13.58 +/- 0.15 mag, and is characterised with a post-maximum decline rate Delta(m_15)_g = 1.08 +/- 0.14 mag. These light curve parameters are comparable to those measured for SN 2008ha of M_g = -13.89 +/- 0.14 mag at peak and Delta(m_15)_g = 1.80 +/- 0.03 mag. The spectral features of SN 2019gsc also resemble those of SN 2008ha at similar phases. This includes both the extremely low ejecta velocity at maximum, about 3,000 km/s, and at late-time (phase +54 d) strong forbidden iron and cobalt lines as well as both forbidden and permitted calcium features. Furthermore, akin to SN 2008ha, the bolometric light curve of SN 2019gsc is consistent with the production of 0.003 +/- 0.001 Msol of nickel. The explosion parameters, M_ej = 0.13 Msol and E_k = 12 x 10E48 erg, are also similar to those inferred for SN 2008ha. We estimate a sub-solar oxygen abundance for the host galaxy of SN 2019gsc, (12 + log10(O/H) = 8.10 +/- 0.18 dex), consistent with the equally metal-poor environment of SN 2008ha. Altogether, our dataset of SN 2019gsc indicates that this is a member of a small but growing group of extreme SN Iax that includes SN 2008ha and SN 2010ae., Comment: 13 pages, 10 figures. ACCEPTED 2020 June 04 MNRAS

A comprehensive survey of injuries in Swedish agriculture was completed in 2013. The aim was to update the statistics on injuries and to compare them with data for 2004. The results were intended to provide a basis for evaluating the effect of Swedish initiatives to reduce occupational injuries in agriculture. In 2013, there were about 63,000 active farms in Sweden, and questionnaires with 21 questions were sent out to a sample of 6000 of these farms. The most important question was whether any injuries had occurred during 2013. Farms that reported injuries were contacted by telephone with additional questions about the injuries. A total of 3375 farms (56%) responded to the questionnaire. After population-level extrapolation, there were approximately 4400 injuries in Swedish agriculture during 2013 (66% in farming, 18% in mixed farming-forestry, and 14% in other related business activities). According to official statistics, there were only about 344 registered occupational injuries, which means that only 7% of the injuries reported in the questionnaire responses were listed in official statistics. In all, at least one injury occurred on about 7% of all enterprises with farming or combined farming-forestry. About 70% of the affected farms had animals, and 17% of all dairy farms had one or more injuries during 2013. According to this study, the overall number of injuries on farms had fallen by about 12% in 2013 compared with the corresponding study in 2004. Taking into account the reduced labor demand in agriculture and the decline in the number of farms since 2004, the rate of injury has not been reduced. To reduce occupational injuries in agriculture, in recent years the industry and government have been working intensively on work environment advice and training for farmers. Our study showed that farmers who received work environment advice and training introduced more measures to prevent injuries than those without any advisory input. It is alarming that despite all efforts to reduce injuries in agriculture, the level is still very high compared with other industries. Safety campaigns and more permanent safety initiatives in agriculture are needed to raise awareness of occupational risk factors and encourage safe behaviors. Keywords: Agriculture, Extension, Farming, Injury prevention, Injury statistics, Occupational injuries.

We have identified a new population of luminous, optical, narrow-lined transients (FWHM ∼1000 km s−1) coincident with the nuclear region of Seyfert galaxies. According to extensive spectrophotometric follow-ups of the main event (PS1-10adi), we could exclude both normal active galactic nucleus activity and changing-look quasars as the origin. The integrated energy output and spectral evolution over a time-scale of several years point to two possible paths of origin: a tidal disruption of a star by a supermassive black hole, or an extremely energetic supernova occurring within the Seyfert galaxy’s narrow-line (or broad-line) region. The former model would require invoking a specific variant of a tidal disruption, while the latter would require an extremely efficient conversion of kinetic energy via shock interaction between the supernova ejecta and the dense ambient medium.

The radio non-detection of two Type Ia supernovae (SNe) SN 2011fe and SN 2014J has been modeled considering synchrotron radiation from shock accelerated electrons in the SN shock fronts. With 10% each of the bulk kinetic energy in electric and magnetic fields, a very low density of the medium around both the SNe has been estimated from the null detection of radio emission, around 1 and 4 years after the explosion of SNe 2014J and 2011fe, respectively. Keeping the fraction of energy in electrons fixed at 10%, a medium with particle density ~ 1cm−3 is found when 1% of the post shock energy is in magnetic fields. In case of a wind medium, the former predicts the mass loss rate Ṁ to be −9M⊙ yr−1, and the latter gives an upper limit ~10−9M⊙ yr−1, for wind velocity of 100 kms−1, for both the SNe. The tenuous media obtained from this study favor the double degenerate as well as a spin up/down model for both SNe 2011fe and 2014J.

Supernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO.We find a dip in the SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities causes mixing of gas, with heavier elements much more disturbed, making more elongated structure.Using 28SiO and its isotopologues, Si isotope ratios were estimated for the first time in SN 1987A. The estimated ratios appear to be consistent with theoretical predictions of inefficient formation of neutron rich atoms at lower metallicity, such as observed in the Large Magellanic Cloud (about half a solar metallicity).The deduced large HCO+ mass and small SiS mass, which are inconsistent to the predictions of chemical model, might be explained by some mixing of elements immediately after the explosion. The mixing might have made some hydrogen from the envelope to sink into carbon and oxygen-rich zone during early days after the explosion, enabling the formation of a substantial mass of HCO+. Oxygen atoms may penetrate into silicon and sulphur zone, suppressing formation of SiS.Our ALMA observations open up a new window to investigate chemistry, dynamics and explosive-nucleosynthesis in supernovae.

The nearby SN 1987A offers a spatially resolved view of the evolution of a young supernova remnant. Here we precent recent Hubble Space Telescope imaging observations of SN 1987A, which we use to study the evolution of the ejecta, the circumstellar equatorial ring (ER) and the increasing emission from material outside the ER. We find that the inner ejecta have been brightening at a gradually slower rate and that the western side has been brighter than the eastern side since ~7000 days. This is expected given that the X-rays from the ER are most likely powering the ejecta emission. At the same time the optical emission from the ER continues to fade linearly with time. The ER is expanding at 680\pm 50 km/s, which reflects the typical velocity of transmitted shocks in the dense hotspots. A dozen spots and a rim of diffuse H-alpha emission have appeared outside the ER since 9500 days. The new spots are more than an order of magnitude fainter than the spots in the ER and also fade faster. We show that the spots and diffuse emission outside the ER may be explained by fast ejecta interacting with high-latitude material that extends from the ER toward the outer rings. Further observations of this emission will make it possible to determine the detailed geometry of the high-latitude material and provide insight into the formation of the rings and the mass-loss history of the progenitor., Accepted for publication in ApJ