PoS(ICRC2021)809 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Cosmic Ray Conference Ray Cosmic [1], 1 ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY − https://pos.sissa.it/ yr on behalf of

3 " 2 − 10 -ray emission $ ONLINE and Stuart Ryder . Although its nature still remains ) could be reached during the early 2 eV 15 8 Mpc . 10 9 ), within a few weeks after discovery. After -ray emission towards nearby core-collapse ∼ W at their present evolutionary stages, recent studies 10 Mpc ∼ decay in hadronic interactions, potentially detectable eV Rachel Simoni 0 1 14 c 10 ∼ -ray emission from W Matthieu Renaud, -ray emission from core-collapse supernovae. ∗ W 0, [email protected] International Cosmic Ray Conference (ICRC 2021) Presenter ∗ th unclear, the derived H.E.S.S. constraints onexpected this VHE transient are placed in the general context of the stages of a core-collapse , when the high-velocitycircumstellar forward shock medium expands into shaped the by dense thethe stellar type progenitor IIn wind. SNe Such whose environments, progenitors in may particular exhibitwith mass-loss current rates Cherenkov telescopes as at high very-highevidence as energies. for efficient Such acceleration of a CR detection protons/nuclei wouldthe in provide long-standing supernovae, direct and issue hence of new the insights on originStereoscopic of System Galactic (H.E.S.S.) Cosmic has Rays. been2016 In to that carrying context, search out the for a High such Energy an Target of early very-high-energy Opportunity program since While the youngest known supernova remnants, such as Cassiopeiato A, accelerate have been cosmic proven rays to be only able uphave to shown that particle energies larger than a few PeV ( could thus lead to supernovae and supernova candidates (up to School of Physics, Wits University, Johannesburg LUPM/CNRS, Montpellier, France University of Amsterdam, Netherlands Macquarie University, Sydney, Australia E-mail: giving an overview of this H.E.S.S. Target of Opportunityfrom program, we the present July the results 2019 obtained observations towardsIIn the supernova, which transient occurred AT2019krl, in originally the classified galaxy as M74 a at type Copyright owned by the author(s) under the terms of the Creative Commons 2 0 1 3 © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 37 July 12th – 23rd, 2021 Online – Berlin, Germany the H.E.S.S. Collaboration (a complete list of authors can be found at the end of the proceedings) Nukri Komin, H.E.S.S. ToO program on nearby core-collapse Supernovae: search for very-high energy towards the SN candidate AT2019krl in M74 PoS(ICRC2021)809 = (1) 2-3 ` ∼ 3 PeV). ∼ -LAT data and a shock -LAT2,3], [ Nukri Komin 1 ) into a dense − 1 − Fermi . 1 Fermi − km s 2. s km s -ray spectrum at 2 10 . , 4 − W w -ray flux derived in [9], D 10 W cm 10 & 1 8 yr. From the best-fit values = − day ∼ sh C E w 2 D (for a mean mass per particle  3 5 10 − , − ¤ w " D decay signature. The latest combined cm -LAT. The analysis of -ray flux from SN 1993J amounts to  0 W 15 c , 2 2 − sh − Mpc Fermi 3 ' erg over the first 5 1 10 2 − , 49 -ray spectrum measured with − TeV , a wind velocity ¤ w and " W 1 D  10 − , most likely due to the CR resonant and nonresonant 7 1 × 12 yr − G 10 7

1 10 × ∼ AGILE − " ) 5 3 × − CR ¤ 2 " ∼  5 1day − / 2 C sh ( ' ) ∼ 10  -rays are expected to be mostly unaffected by photon fields from the = 50 TeV ¤ W " `< ¤ ∼ w " cm. Tatischeff [6] has shown that the extensive spectro-morphological radio cD 4 15 ,  >  ( sh -ray emitting supernova remnants (SNRs), no indisputable evidence for the = W ) circumstellar medium (CSM)]. [6–12 Such an environment is formed by the W ' ) 3  − 15 sh ' 10 ( cm = = 9 − 7 sh ' -LAT/VERITAS spectrum clearly shows an exponential cutoff of the 10 In the GeV domain, Among the at least two orders of higher than the equipartition value of a Red SuperGiant (RSG) progenitor wind, in & 1 = Similar calculations have been performed, [9 16–18]thought in to the be case of powered by the superluminous thecollisionless type interaction IIn shock between SNe, propagates the in ejecta the and wind, a[20, efficient very21], CR dense and acceleration CSM these [19]. has been SNvery-high-energy Once shown events the neutrinos to could detected take thus place with be IceCubeonce privileged applied [17]. source on candidates SN The 1993J, to expected is explain compatible (part with of)1 equation within the a factor of source [9], so that thesewith flux current estimates can HE be instruments readily such used to as estimate the visibility of these SNe 1) with a mass-loss rate line with several previous studies [13, 14]. instabilities operating in the shockand precursor nuclei (but would see then] [15 be(see for accelerated [12]), a to with different PeV a energies interpretation). total within CR the Protons energy first few days after the radius observations of the synchrotron emission fromcan the be nearby, described and well-monitored, by type athe IIb detailed SN SN model 1993J hydrodynamics. coupling the The non-linearexplosion DSA magnetic at with the field self-similar level was of solutions found for to be strongly amplified shortly after the of the relevant parameters obtained by [6], the hadronic H.E.S.S. observations of core-collapse SNe and AT2019krl 1. Introduction: probing particle acceleration in core-collapse supernovae presence of PeV Cosmic Ray (CR)yet. particles being accelerated Cassiopeia at A their (Cas shockhas fronts A), long has been with been considered an found as age theIts of best high-energy/very-high-energy candidate about to (HE/VHE) 350 accelerate years particles one up to of the the CR youngest knee Galactic ( SNRs, VERITAS [4] and MAGIC [3]seen is better below explained 1 by GeV, hadronic reminiscent interactions of owing to the the characteristic TeV turnover [5]. This demonstratesTeV, regardless of that the the details maximum ofpoints the energy towards broadband of the spectral the modeling idea accelerated of thatpreviously Cas particles thought PeV A during CRs is [5]. the could below SNR Such be(DSA) 20 mechanism a evolution. accelerated have low shown that at value Recent particle the studies energies larger of shockwhen than a the the front few PeV diffusive supernova could much actually shock (SN) be earlier acceleration reached shock than ( is propagating at high velocity ( Fermi wind from the stellar progenitor priorbe to steady: explosion, whose density profile is commonly assumed to PoS(ICRC2021)809 Nukri Komin for SN 1993J 3.5 Mpc) type ∼ WW g Mpc) do the derived 20 (http://dark.physics.ucdavis. . 10 days. 3 ∼ ) and their stellar winds (mass-loss sh D , and DLT40 interaction, have recently been applied sh W - ' W in the radiation field from the SN 150 Mpc [24] and the nearby ( − ∼ 4 3 + + 4 -rays from SNe by means of a variable-size sliding- W anisotropic → W + W -LAT data has confirmed the variable signal in the direction -ray flux, shown to be sensitive to the photospheric properties ) are very diverse and are still the topic of intense investigation W 2 allow for a determination of the SN subclass within a few days and 3 Fermi source of UV/optical photons, the full opacity calculations, including -ray emission. Since progenitor mass-loss rates and wind velocities do W isotropic projects are yielding the cadence necessary to ensure that nearby southern cc-SNe can be caught -LAT data have reported marginally significant variable HE emission towards the (http://www.astronomy.ohio-state.edu/~assassin/) Fermi 3 days after the explosion. < Based on the above-mentioned calculations from Tatischeff [6] and Cristofari et al. [27], a One should note that all these calculations are subject to large uncertainties in the different Recent observations show that some type Ibn/IIn SN progenitors (possibly Luminous Blue Variables)ASAS-SN experience 3 2 H.E.S.S. Target of Opportunity (ToO)to program probe has early been VHE set up towards nearby cc-SNe in order rate, wind velocity and structure [1, 30]. Also,until the detailed time analyses of of pre- the andUV/Optical/NIR SN’s post-explosion observations explosion data are is performed. usuallyprovide not Nevertheless, important high-cadence insights known on at the SN the photosphere,and the time kinematics stellar progenitor (e.g. of and [31, its on the32 ]). discovery ejectacore-collapse Finally, chemistry radio supernovae observations (cc-SNe), provide as a well probe as ofCSM the the produced mass-loss magnetic rate by fields the and in pre-SN the stellar density wind distribution (e.g. of the [33] and references therein). 2. H.E.S.S. Target of Opportunity program on cc-SNe greatly vary among the different cc-SN sub-classes, with no univocal relationship with the stellar some episodic mass-loss outbursts during theof latest shell-like phases structures before [29]. explosion, resulting in a complicated CSM [28] made edu/dlt40/DLT40) within parameters highlighted above, as mostwavelength of (MWL) them observations are have estimated been throughparticle indirect carried acceleration means, out. capability once multi- of First thesegeometry, of the SNe nature all, and are many growth still timescale details of poorlythe impacting the constrained characteristics instabilities the (e.g. and of the cc-SN particle the light-curves injection).pacting and magnetic the Moreover, spectra, time field evolution the of the properties photospheric parameters of the stellar progenitors (im- to SN 1993J [27].and The SN resulting hydrodynamics, is then strongly attenuated during the first temporal and geometrical effects due to the peculiar H-rich super-luminous SN iPTF14hls at H.E.S.S. observations of core-collapse SNe and AT2019krl towards an ensemble of 147 type IInexcess SNe in [22]. different time windows has Onlyupper not for revealed limits any the significant start brightest to constrain andbased the on closest theoretical type expectations IIn [23]. events Nevertheless, ( two recent studies IIP SN 2004dj [25]. The latest search for of iPTF14hls and revealedand two AT2018iwp, new with excesses a in fluxdomain, increase the the within pair direction production six process of months after theis the SN expected discovery to candidates date be [26]. AT2019bvr effective.by In assuming While the an Tatischeff TeV [6] has overestimated the opacity time-window analysis of the PoS(ICRC2021)809 = 10 h, 12913). # obs ) Nukri Komin 10 Mpc [38], emission lines, < U ) cc-SNe. Since 2020, several ◦ -40 < 2 cc-SNe per year at − . This on-going ToO program has been 1 − 12934). The mid-IR brightness measured at this 4 # 9.8 Mpc [41]. On 9th July AT2019krl was shown ∼ . Owing to the uncertainties in defining meaningful trigger 4 Mpc), southern (Dec. 40 . with H.E.S.S., at day 10 after the SN explosion and for 3 f opacity and CR acceleration efficiency as in SN 1993J, the corresponding W type IIb SN in Cen A. No significant excess has been found towards any of − 5 ) = (1,2,2,5,20) for type (II-P,Ib/c,II-L,IIb,IIn) SNe, respectively [1, 34–37]. By W 10 , w D / 5 − ¤ " So far, H.E.S.S. has serendipitously observed nine nearby cc-SNe within a year after their On 6th July 2019 a transient originally named ZTF19abehwhj was discovered by ZTF (later The first three values, originally estimated to amount toType IIb 0.4-0.8 SNe Mpc, are have thought been to rounded have to more 1 compact and Mpc, less below luminous which stellar progenitor with faster and lower-density 5 4 discovery date and triggered ToO observations on one cc-SN aa few days (possibly after compact) discovery: SN 2016adj, renamed as AT2019krl) in the M74 galaxy at members of the DLT40program. and Thus, ASAS-SN the optical H.E.S.S.cc-SN surveys event Collaboration are within can a also get few days informed involved in in about order to the this make properties a H.E.S.S. of reliable ToO trigger any decision. nearby these cc-SNe. The analysis and interpretationpublished of [40]. the H.E.S.S. data That towards theseassumptions study cc-SNe on provides have been the interesting acceleration upperSN efficiency limits 1993J), (among on in other the particular on parameters CSMlonger SN as density than 2016adj, what described under even is though in several considered most here. the ofobservations In case of the the AT2019krl, data of following originally these set classified results spreads as will over a be timescales type complemented IIn with SN ToO candidate, in the3. galaxy M74. AT2019krl in M74 3.1 Discovery and multi-wavelength observations to have a type IInalthough SN several optical types spectrum, of exhibitingor CSM-interacting narrow other SNe, and intermediate-luminosity intermediate a transients H- LuminousFollowing could these Blue reports, not Variable a be (LBV) H.E.S.S.candidate ruled in ToO on was out outburst, 11th triggered July at on (see that this detailsdata (possibly to below). stage very look (ATel Then, at young) the on type mid-IR 12th IIn pre-discoverylocation July, evolution SN the of of the analysis AT2019krl transient of showing revealed the a a Spitzer quiescent moderatewhile source archival the brightening at transient the between became December a 2018 verythe bright and transient mid-IR April source has 2019, in been mid-May discovered 2019, by i.e. ZTF about (ATel 50 days before there is no major -forming galaxy visible from the Southern Hemispherewind except the [39]. LMC/SMC. criteria as described inbe the triggered previous towards any section, cc-SNinteresting (lower-rank) or MWL H.E.S.S. SN information. ToO candidate observations Given occurring a may at predicted also less rate of than 1 10enriched by Mpc the implementation if of several there partnerships with is groupsof dealing some cc-SNe. with MWL observations In particular, oneat of 1-20 us GHz (S. towards Ryder) nearby has ( been leading a radio ToO program with ATCA have been derived to be (1,1,1,2,8) Mpc the expected trigger rate does certainly not exceed 2 yr H.E.S.S. observations of core-collapse SNe and AT2019krl progenitor and the SN type (seefollows: e.g. ( [30]), the most representative values have been considered as horizons of detectability at 5 assuming the same PoS(ICRC2021)809 , off . f U# − on as described 2 # Nukri Komin \ = excess # 5 -ray excess was computed using W Significance map (left) and radial distribution of the excess at the source position, in the ON to OFF exposure ratio. The statistical significance was estimated using [47, eq. U Observations were conducted with the High Energy Stereoscopic System (H.E.S.S.), an array of five imaging atmosphericNamibia Cherenkov at telescopes an (IACTs) altitude located of 1800 infour m 12 the m-diameter above telescopes sea Khomas (CT1-4, level. operating Highland since AT2019krl December wastelescope of 2003) observed (CT5, and with operating the the fifth since 28 full September m-diameter array, 2012).the the "H.E.S.S.-II-phase" The as analysis performances described are in thusevents [43]. triggering the at ones The least of data 3 telescopes were180 including taken GeV compared CT5, in to which an 210 allows GeV "hybrid for for a mode", thenights, lower CT1-4 selecting from energy array. threshold 11th AT2019krl of was to observed 13th onmean July three offset 2019. consecutive angle of These 0.5 observations degA were around total made the of source in 10 and calibrated wobble organized runsImPACT mode reconstruction in passing [42] [45], 28-minute the with with exposures standard hybrid a called quality configuration runs. criteria andlivetime with standard [see a cuts.44] mean were This zenith analysed led angle using torings of the around 4.5 47.2 each deg. hours sky of bin, The applying background the forON-region ring the background (with sky method a map [46]. radius was For obtained of the from 0.086were spectral extraction selected deg) an was with defined the at same thereflected angular SN background distance position, method from and [46]. the multiple camera OFF The centre regions as the ON region, using the Figure 1: in [42] (right). The reported statistics are explained in the text. The significance of the emission is 0.4 3.2 Observations and data analysis with 17]. The results wereModel++ confirmed framework [48] by with an standard independent quality data cuts and calibration the and same analysis reflected chain background using method. the H.E.S.S. observations of core-collapse SNe and AT2019krl last epoch suggested that AT2019krllikely occurred is between rather 21st a April and SN 17th than May. a LBV outburst, whose final explosion PoS(ICRC2021)809 1 2 = − w -ray D W Γ = . g cm 1 ) with a for − Γ 16 1 ) amounts − . Since the − w 1 10  D − yr . Fluxes are Nukri Komin erg s / × 1 ∝ = 3.5 [6] and

¤ − " 5 40 " − 2.2 ¤ 3 ) 10 " ∼ / 3 × − distance to the source 3# 2 (10 \ = 1 (solid lines) and 12 4 − C 10 -ray emission from AT2019krl is set to 10 km s Predicted flux above 1 TeV as a W ∼ w D days. H.E.S.S. (CT1-4) and CTA 7 between 10 and 1000 km s = computed for Figure 2: function of the distance to the source based on [6]. (dashed lines) weeks aftersion. the SN The explo- expectedis flux computed from assuming SN 1993J integrated sensitivities for 50servations h are long taken ob- fromfrom which [42] those for and t= 5 [50], hblack, are ULs derived. on the In flux above 1 TeV derived in [40] are also shown (see text). C w D . Assuming a distance to M74 of 9.8 Mpc -ray flux from AT2019krl is at a comparable 1 TeV have been computed in order to compare W − 1 s 1 − 1 TeV) 2 sensitivity > − yr =2, the UL on the CSM density ( 6 σ sensitivity Γ  > σ

cm M 3 10 [28], for

− ∼ 13 AT2019krl F( SN 1993J (t=7d) t = 1 week t = 12 weeks H.E.S.S. 5 CTA 5 10 − 10 10 × -ray emission model. For example, the absence of detectable 12934), the UL on the CSM density increases to W # 1 1

− − Distance in Mpc yr yr

M M , equivalent to a progenitor mass-loss rate of 4 5 1 − and 2.4. Integrated ULs at − − 2 TeV) = 3.85 [2.95] 10 10 1 = = , as shown in2. Fig. Such a constraint is at the same level as the lowest wind densities g cm 1 Γ = − 10 10 15 u u -ray emission suggest a low density wind, AT2019krl must either be an atypical SN IIn, ˙ ˙ W

 > M M 10 1 confidence level under the assumption of a power law spectrum ( × 50h 5h 50h 5h % 2 Figure shows that the upper limit on the VHE After 4.5 h of observations no significant excess has been found. As shown in1, Figure the 15 12 13 14 11 6.3

− − − − −

− −

e) (cm TeV)) 1 > log(Flux( ) s ∼

1 2 4. Discussion and Conclusion [41], these flux ULs above 1 TeV translate into luminosity ULs of 3.25 [1.56] level as the other cc-SNe studied in [40].suggests in The a absence hadronic of model significant a low densitywith of the the target material. model The target of densityproduction can [6] be effect. estimated and Considering using t equation = (1) 1 week assuming and a distance of d = 9.8 Mpc and no pair- with ULs previously derived towards cc-SNe [40] using a log-likelihood approach [49]. For significance map is isotropic, and the photon counts as a function of the H.E.S.S. observations of core-collapse SNe and AT2019krl 3.3 Results exhibit no excess above the backgroundthe level. 95 Flux upper limitsphoton index (ULs) have thus been derived at [2.4], UL( to 10 (100) km s required to make a type IIntypical mass-loss SN rates [28], higher knowing by a that factor most of absence of of the well-studied type IInor events point exhibit to a problem with the emission can also indicate a strongphotons attenuation from due the to the SN pair-production photosphere,explosion. process which with Bearing is UV/optical in mind particularly that important theSN during date occurred of the on the first 21st explosion of April week AT2019krl (i.e. after isof t Spitzer poorly the constrained, = archival data if 12 (ATel the weeks before thebut H.E.S.S. still ToO) falls as in suggested by the the lower analysis part of the estimated values for known type IIn SNe [see Fig. 3 in 28]. PoS(ICRC2021)809 1 Mpc. ∼ Nukri Komin -ray emission W -ray emission from a W -ray emission is absorbed, W 7 The support of the Namibian authorities and of the University of Namibia in facili- -ray emission from cc-SNe at a much lower level. W -ray observations. While shortly after the explosion the W Estimating the date of the SN explosion is necessary to chose the optimal time window to -ray emission at a distance of about 10 Mpc while the other types could be detectable at [1] Smith, N. 2014, ARA&A[2] 52 487-528 Yuan, Y., et al.[3] 2013, ApJ 779Ahnen, 117 M. (6 L., pp.) et[4] al. (MAGICKumar, Collaboration) S., 2017, et MNRAS al.[5] 472 (VERITAS p.2956-2962 Collaboration)Abeysekara, 2015, A. Proceedings U., of et the al. 34th 2020, ICRC ApJ arXiv:1508.07453 894, Issue 1, id.51 (13 pp.) W trigger VHE H.E.S.S. observations of core-collapse SNe and AT2019krl Finally, AT2019krl may not have beenHST, a Spitzer SN and explosion LBT at observations, all. it2008S-like transient has Indeed, due to recently based a been on Blue suggested SuperGiant extensive (BSG)the that archival eruption AT2019krl model or is an discussed LBV either outburst here]. [51 a cannotand SN In be this the case, applied. disputed nature Irrespective oftype of AT2019krl IIn the the SN study non-detection at a presented of distance hereTelescopes of like shows about H.E.S.S., that 10 provided Mpc that could the be nuclearnot detectable interaction limiting with losses the current in acceleration Imaging such of high-density Air PeV CSM Cherenkov CRsemission are [see would,12 be for a detailed clear calculation]. proof ofonce The efficient the observation particle progenitor’s of parameters acceleration such during are the known thanks early stages to of multi-wavelength a observations. cc-SN, several weeks later the emission mayThe have declined type to of a the level SN undetectablethe explosion by TeV current is domain. instruments. important Only to type estimate IIn the SNe horizon can of provide detectabilityThe a with detection sufficiently IACTs of dense in a CSM good toa candidate produce few might detectable tens necessitate of observations hours. longerobservations than to be considered The triggered here, each H.E.S.S. year. of ToO Aimportant program non-detection constraints by on on H.E.S.S. the of cc-SNe ability a is of nearby cc-SNe suchfuture ongoing, can very Cherenkov provide Telescope young allowing Array SNe (CTA, for to [50]), accelerate a with CRs a fewto to higher probe ToO PeV sensitivity energies. the than VHE The H.E.S.S., will be able Acknowledgements tating the construction and operation of H.E.S.S.Ministry is for gratefully Education acknowledged, as and is the Research(DFG), support (BMBF), the by the Helmholtz the German Association, Max the Planck AlexanderEducation, von Society, Humboldt the Research Foundation, and German the French Innovation, Research Ministry the Foundation CNRS/INSU), of Centre Higher the Commissariat National à de l’énergie laand atomique Recherche Technology et Facilities Scientifique Council aux (STFC), (CNRS/IN2P3 énergies the alternatives and KnutCentre, (CEA), and Poland the Alice grant Wallenberg U.K. Foundation, no. Science the National 2016/22/M/ST9/00382, Science and the National South Research African Foundation, Department the ofence University Science & of and Technology Namibia, of Technology Namibia the (NCRST), National the Commissionand Austrian Federal on the Ministry Research, of Austrian Sci- Education, Science Science and FundPromotion Research (FWF), of the Science and Australian Research bynical the Council support University (ARC), staff of the in Amsterdam. Berlin, Japanconstruction Zeuthen, Society We and Heidelberg, appreciate for operation Palaiseau, the the Paris, of excellent Saclay, the workVirtual Tübingen equipment. and of Organisation, supported in the This by Namibia tech- work the in benefitted national the from resource providers services of provided the by EGI the Federation. H.E.S.S. References PoS(ICRC2021)809 Nukri Komin 8 -LAT Collaboration) 2015, ApJ 807 169 (15 pp.) Fermi [6] Tatischeff, V. 2009, A&A[7] 499 191-213 Bell, A. 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Dreyer 6 12 10 11 29 , R. Zanin 15 , , D. Malyshev , T. L. Holch , J. Damascene Mbarubucyeye , R. Konno , M. Lemoine-Goumard 16 23 , D. Glawion 11 1 23 , A. Sinha , F. Aharonian , F. Cangemi , H. Rueda Ricarte , J. Schäfer , G. Fichet de Clairfontaine 9 13 21 , R.D. Parsons , , S.J. Wagner 1 , G. Maurin 7 , E. Moulin 35 3 , I. Jung-Richardt 3 14 32 19 8 21 29 19 , M. Böttcher 15 Instytut Fizyki PAN, ul. Ja¸drowej Radzikowskiego 152, 31-342DESY, D-15738 Kraków, Poland Zeuthen, Germany Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. OrlaSchool 171, of 30-244 Physics, University Kraków, of Poland theDepartment Witwatersrand, 1 of Jan Physics and Smuts Electrical Avenue, Braamfontein, Engineering,Institut Johannesburg, Linnaeus für 2050 University, Astronomie South 351 und Africa 95 Astrophysik, Växjö, Universität Sweden Laboratoire Tübingen, Sand Univers et 1, Théories, D 72076 Observatoire de Tübingen,Sorbonne Germany Paris, Université, Université Université PSL, Paris CNRS, Diderot, Université de Sorbonne Paris, Paris 92190 Cité, Meudon, CNRS/IN2P3, France LaboratoireAstronomical de Observatory, The Physique Nucléaire University of et Warsaw, Al. deFriedrich-Alexander-Universität Hautes Erlangen-Nürnberg, Ujazdowskie 4, Erlangen 00-478 Warsaw, Centre Poland for Astroparticle Physics, Erwin-Rommel-Str.Université Bordeaux, CNRS/IN2P3, 1, Centre d’Études D NucléairesUniversité de 91058 de Bordeaux Paris, Gradignan, CNRS, 33175 Astroparticule Gradignan, etDepartment France Cosmologie, of F-75013 Physics Paris, and France Astronomy, TheInstitut University für of Physik Leicester, und University Road, Astronomie, Leicester, Universität LE1School Potsdam, 7RH, of Karl-Liebknecht-Strasse 24/25, United Physical Sciences, Kingdom D University 14476 of Potsdam,Laboratoire Adelaide, Germany Leprince-Ringuet, Adelaide 5005, École Australia Polytechnique, CNRS, InstitutLaboratoire Polytechnique de Univers Paris, et F-91128 Particules Palaiseau, France de Montpellier, Université Montpellier, CNRS/IN2P3,Institut für CC Astro- 72, und Place Teilchenphysik, Leopold-Franzens-Universität Innsbruck, EugèneUniversität A-6020 Hamburg, Bataillon, Innsbruck, Institut Austria für F-34095 Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany University of Namibia, Department of Physics,Dublin Private Institute Bag for 13301, Advanced Windhoek Studies, 10005, 31 Namibia Max-Planck-Institut Fitzwilliam für Place, Kernphysik, Dublin P.O. 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Fiasson H.E.S.S. observations of core-collapse SNe and AT2019krl Full Authors List: H.E.S.S. Collaboration H. Abdalla T. Bylund H. Dalgleish V. Doroshenko V. Baghmanyan B. Bi PoS(ICRC2021)809 Nukri Komin 10 Landessternwarte, Universität Heidelberg, Königstuhl, D 69117Institute Heidelberg, Germany of Astronomy, Faculty of Physics, Astronomy andDepartment Informatics, of Nicolaus Physics, Rikkyo Copernicus University, 3-34-1 University, Nishi-Ikebukuro,Nicolaus Grudziadzka Toshima-ku, Copernicus Tokyo Astronomical 171-8501, 5, Center, Japan 87-100 Polish AcademyInstitut of für Sciences, Physik, ul. Humboldt-Universität zu Bartycka Berlin, 18,Department Newtonstr. 00-716 of 15, Warsaw, Poland Physics, D University 12489 of Berlin, the Germany GRAPPA, Free Anton Pannekoek State, Institute PO for Box Astronomy, University 339, of Bloemfontein Amsterdam, 9300, Science South Park 904, Africa 1098 XHYerevan Amsterdam, Physics The Institute, Nether- 2 Alikhanian Brothers St., 375036 Yerevan, Armenia H.E.S.S. observations of core-collapse SNe and AT2019krl 29 30 Torun, Poland 31 32 33 34 35 lands 36