Pranjupriya Goswami
Tezpur University
H-index: 7
Asia-India
About Pranjupriya Goswami
Pranjupriya Goswami, With an exceptional h-index of 7 and a recent h-index of 7 (since 2020), a distinguished researcher at Tezpur University, specializes in the field of High Energy Astrophysics, Astrophysical Blazars, Neutrino Physics, Machine Learning.
His recent articles reflect a diverse array of research interests and contributions to the field:
Searches for neutrino counterparts of gravitational waves from the LIGO/Virgo third observing run with KM3NeT
The variety of extreme blazars in the AstroSat view
Search for Neutrino Emission from GRB 221009A using the KM3NeT ARCA and ORCA detectors
TeV flaring activity of the AGN PKS 0625-354 in November 2018
Unveiling extended gamma-ray emission around HESS J1813-178
Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and HESS analysis
Astronomy potential of KM3NeT/ARCA
Atmospheric muons measured with the KM3NeT detectors in comparison with updated numeric predictions
Pranjupriya Goswami Information
University | Tezpur University |
|---|---|
Position | Reseach Scholar |
Citations(all) | 92 |
Citations(since 2020) | 92 |
Cited By | 10 |
hIndex(all) | 7 |
hIndex(since 2020) | 7 |
i10Index(all) | 4 |
i10Index(since 2020) | 4 |
University Profile Page | Tezpur University |
Pranjupriya Goswami Skills & Research Interests
High Energy Astrophysics
Astrophysical Blazars
Neutrino Physics
Machine Learning
Top articles of Pranjupriya Goswami
Searches for neutrino counterparts of gravitational waves from the LIGO/Virgo third observing run with KM3NeT
Authors
S Aiello,A Albert,S Alves Garre,Z Aly,A Ambrosone,F Ameli,M Andre,E Androutsou,M Anguita,L Aphecetche,M Ardid,S Ardid,H Atmani,J Aublin,L Bailly-Salins,Z Bardačová,B Baret,A Bariego-Quintana,S Basegmez Du Pree,Y Becherini,M Bendahman,F Benfenati,M Benhassi,DM Benoit,E Berbee,V Bertin,S Biagi,M Boettcher,D Bonanno,J Boumaaza,M Bouta,M Bouwhuis,C Bozza,RM Bozza,H Brânzaş,F Bretaudeau,R Bruijn,J Brunner,R Bruno,E Buis,R Buompane,J Busto,B Caiffi,D Calvo,S Campion,A Capone,F Carenini,V Carretero,T Cartraud,P Castaldi,V Cecchini,S Celli,L Cerisy,M Chabab,M Chadolias,A Chen,S Cherubini,T Chiarusi,M Circella,R Cocimano,JAB Coelho,A Coleiro,R Coniglione,P Coyle,A Creusot,G Cuttone,R Dallier,Y Darras,A De Benedittis,B De Martino,G De Wasseige,V Decoene,R Del Burgo,I Del Rosso,UM Di Cerbo,LS Di Mauro,I Di Palma,AF Díaz,C Diaz,D Diego-Tortosa,C Distefano,A Domi,C Donzaud,D Dornic,M Dörr,E Drakopoulou,D Drouhin,R Dvornický,T Eberl,E Eckerová,A Eddymaoui,T van Eeden,M Eff,D van Eijk,I El Bojaddaini,S El Hedri,A Enzenhöfer,G Ferrara,MD Filipović,F Filippini,D Franciotti,LA Fusco,J Gabriel,S Gagliardini,T Gal,J García Méndez,A Garcia Soto,C Gatius Oliver,N Geißelbrecht,H Ghaddari,L Gialanella,BK Gibson,E Giorgio,I Goos,P Goswami,D Goupilliere,SR Gozzini,R Gracia,K Graf,C Guidi,B Guillon,M Gutiérrez,H van Haren,A Heijboer,A Hekalo,L Hennig,JJ Hernández-Rey,W Idrissi Ibnsalih,G Illuminati,M de Jong,P de Jong,BJ Jung,P Kalaczyński,O Kalekin,UF Katz,A Khatun,G Kistauri,C Kopper,A Kouchner,V Kueviakoe,V Kulikovskiy,R Kvatadze,M Labalme,R Lahmann,M Lamoureux,G Larosa,C Lastoria,A Lazo,S Le Stum,G Lehaut
Journal
Journal of Cosmology and Astroparticle Physics
Published Date
2024/4/9
The first detection of a gravitational wave (GW) signal from a binary compact merger [1] initiated in 2015 a new era in multi-messenger astronomy. The subsequent observation in 2017 of a GW signal from the binary neutron star merger event GW170817 and of prompt and afterglow electromagnetic emissions from the associated short gamma-ray burst [2] was the first and so far unique multi-messenger observation of its kind. Models exist of production of neutrinos from these compact mergers, especially for mergers involving neutron stars such as binary neutron star mergers (BNS)[3] or neutron star-black hole mergers (NSBH)[4], though some models also predict neutrino emissions from binary black hole mergers (BBH)[5]. Although most of the studies focus on hadronic processes leading to high-energy neutrino production (Eν≳ GeV), thermal neutrinos in the MeV regime may also be produced [6].Searches for …
The variety of extreme blazars in the AstroSat view
Authors
Pranjupriya Goswami,Michael Zacharias,Andreas Zech,Sunil Chandra,Markus Boettcher,Iurii Sushch
Journal
Astronomy & Astrophysics
Published Date
2024/2/1
Context Among the blazar class, extreme blazars have exceptionally hard intrinsic X-ray/TeV spectra, and extreme peak energies in their spectral energy distribution (SED). Observational evidence suggests that the non-thermal emission from extreme blazars is typically non-variable. All these unique features present a challenging case for blazar emission models, especially regarding those sources with hard TeV spectra.Aims We aim to explore the X-ray and GeV observational features of a variety of extreme blazars, including extreme-TeV, extreme-synchrotron (extreme-Syn), and regular high-frequency-peaked BL Lac objects (HBLs). Furthermore, we aim to test the applicability of various blazar emission models that could explain the very hard TeV spectra.Methods We conducted a detailed spectral analysis of X-ray data collected with AstroSat and Swift-XRT, along with quasi-simultaneous γ-ray data from Fermi …
Search for Neutrino Emission from GRB 221009A using the KM3NeT ARCA and ORCA detectors
Authors
S Aiello,A Albert,M Alshamsi,S Alves Garre,A Ambrosone,F Ameli,M Andre,E Androutsou,M Anguita,L Aphecetche,M Ardid,S Ardid,H Atmani,J Aublin,F Badaracco,L Bailly-Salins,Z Bardačová,B Baret,A Bariego-Quintana,S Pree,Y Becherini,M Bendahman,F Benfenati,M Benhassi,DM Benoit,E Berbee,V Bertin,S Biagi,M Boettcher,D Bonanno,J Boumaaza,M Bouta,M Bouwhuis,C Bozza,RM Bozza,H Brânzaş,F Bretaudeau,M Breuhaus,R Bruijn,J Brunner,R Bruno,E Buis,R Buompane,J Busto,B Caiffi,D Calvo,S Campion,A Capone,F Carenini,V Carretero,T Cartraud,P Castaldi,V Cecchini,S Celli,L Cerisy,M Chabab,M Chadolias,A Chen,S Cherubini,T Chiarusi,M Circella,R Cocimano,JAB Coelho,A Coleiro,A Condorelli,R Coniglione,P Coyle,A Creusot,G Cuttone,R Dallier,Y Darras,A De Benedittis,B De Martino,V Decoene,R Del Burgo,I Del Rosso,LS Di Mauro,I Di Palma,AF Díaz,C Diaz,D Diego-Tortosa,C Distefano,A Domi,C Donzaud,D Dornic,M Dörr,E Drakopoulou,D Drouhin,JG Ducoin,R Dvornický,T Eberl,E Eckerová,A Eddymaoui,T van Eeden,M Eff,D van Eijk,I El Bojaddaini,S El Hedri,A Enzenhöfer,G Ferrara,MD Filipović,F Filippini,D Franciotti,LA Fusco,S Gagliardini,T Gal,J García Méndez,A Garcia Soto,C Gatius Oliver,N Geißelbrecht,H Ghaddari,L Gialanella,BK Gibson,E Giorgio,I Goos,P Goswami,SR Gozzini,R Gracia,K Graf,C Guidi,B Guillon,M Gutiérrez,C Haack,H van Haren,A Heijboer,A Hekalo,L Hennig,JJ Hernández-Rey,W Idrissi Ibnsalih,G Illuminati,D Joly,M de Jong,P de Jong,BJ Jung,O Kalekin,UF Katz,L Kharkhelauri,G Kistauri,C Kopper,A Kouchner,V Kueviakoe,V Kulikovskiy,R Kvatadze,M Labalme,R Lahmann,G Larosa,C Lastoria,A Lazo,S Le Stum,G Lehaut
Journal
arXiv preprint arXiv:2404.05354
Published Date
2024/4/8
Gamma-ray bursts are promising candidate sources of high-energy astrophysical neutrinos. The recent GRB 221009A event, identified as the brightest gamma-ray burst ever detected, provides a unique opportunity to investigate hadronic emissions involving neutrinos. The KM3NeT undersea neutrino detectors participated in the worldwide follow-up effort triggered by the event, searching for neutrino events. In this letter, we summarize subsequent searches, in a wide energy range from MeV up to a few PeVs. No neutrino events are found in any of the searches performed. Upper limits on the neutrino emission associated with GRB 221009A are computed.
TeV flaring activity of the AGN PKS 0625-354 in November 2018
Authors
HESS Collaboration,F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,A Baktash,V Barbosa Martins,J Barnard,R Batzofin,Y Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M de Lavergne,J Borowska,F Bradascio,M Breuhaus,R Brose,A Brown,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,T Bylund,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,J Mbarubucyeye,ID Davids,J Djuvsland,A Dmytriiev,V Doroshenko,K Egberts,S Einecke,J-P Ernenwein,G Fontaine,M Füßling,S Funk,S Gabici,S Ghafourizadeh,G Giavitto,D Glawion,JF Glicenstein,J Glombitza,P Goswami,G Grolleron,L Haerer,JA Hinton,TL Holch,M Holler,D Horns,M Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,R Khatoon,B Kh'elifi,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,J-P Lenain,F Leuschner,A Luashvili,J Mackey,R Marx,A Mehta,M Meyer,A Mitchell,R Moderski,A Montanari,E Moulin,M de Naurois,J Niemiec,P O'Brien,S Ohm,L Olivera-Nieto,E Wilhelmi,M Ostrowski,S Panny,RD Parsons,S Pita,DA Prokhorov,G Pühlhofer,M Punch,A Quirrenbach,P Reichherzer,A Reimer,O Reimer,H Ren,F Rieger,B Rudak,V Sahakian,H Salzmann,DA Sanchez,M Sasaki,F Schüssler,HM Schutte,JNS Shapopi,H Sol,A Specovius,S Spencer,R Steenkamp,S Steinmassl,K Streil,I Sushch,H Suzuki,T Takahashi,T Tanaka,C van Eldik,M Vecchi,J Veh,C Venter,SJ Wagner,A Wierzcholska,M Zacharias,D Zargaryan,AA Zdziarski,A Zech,S Zouari,N Żywucka
Journal
arXiv preprint arXiv:2401.07071
Published Date
2024/1/13
Most -ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its -ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and UVOT taken in November 2018. The H.E.S.S. light curve above 200 GeV shows an outburst in the first night of observations followed by a declining flux with a halving time scale of 5.9h. The -opacity constrains the upper limit of the angle between the jet and the line of sight to . The broad-band spectral energy distribution shows two humps and can be well fitted with a single-zone synchrotron self Compton emission model. We conclude that PKS 0625-354, as an object showing clear features of both blazars and radio galaxies, can be classified as an intermediate active galactic nuclei. Multi-wavelength studies of such intermediate objects exhibiting features of both blazars and radio galaxies are sparse but crucial for the understanding of the broad-band emission of -ray detected active galactic nuclei in general.
Unveiling extended gamma-ray emission around HESS J1813-178
Authors
F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,A Baktash,V Barbosa Martins,J Barnard,R Batzofin,Y Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M de Lavergne,J Borowska,M Bouyahiaoui,M Breuhaus,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,P Chambery,T Chand,A Chen,J Chibueze,O Chibueze,G Cotter,J Mbarubucyeye,A Djannati-Ataï,A Dmytriiev,V Doroshenko,S Einecke,J-P Ernenwein,K Feijen,M Filipovic,G Fontaine,M Füßling,S Funk,S Gabici,YA Gallant,S Ghafourizadeh,G Giavitt,D Glawion,JF Glicenstein,P Goswami,G Grolleron,M-H Grondin,JA Hinton,W Hofmann,TL Holch,M Holler,M Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,K Katarzyński,R Khatoon,B Khélifi,S Klepser,W Kluźniak,Nu Komin,K Kosack,D Kostunin,A Kundu,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,J Mackey,D Malyshev,V Marandon,P Marinos,G Martí-Devesa,R Marx,A Mehta,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,T Murach,M de Naurois,J Niemiec,A Priyana Noel,P O'Brien,S Ohm,L Olivera-Nieto,E Wilhelmi,M Ostrowski,S Panny,M Panter,RD Parsons,DA Prokhorov,G Pühlhofer,M Punch,A Quirrenbach,M Regeard,P Reichherzer,A Reimer,O Reimer,H Ren,M Renaud,B Reville,F Rieger,G Roellinghoff,B Rudak,V Sahakian,H Salzmann,M Sasaki,F Schüssler,HM Schutte,JNS Shapopi,A Specovius,S Spencer,R Steenkamp,S Steinmassl,C Steppa,I Sushch,H Suzuki,T Takahashi,T Tanaka,R Terrier,M Tluczykont,N Tsuji,T Unbehaun,C van Eldik,M Vecchi,J Veh,C Venter,J Vink,T Wach,SJ Wagner,A Wierzcholska,M Zacharias,D Zargaryan,AA Zdziarski,S Zouari,N Żywucka
Journal
arXiv preprint arXiv:2403.16802
Published Date
2024/3/25
HESS J1813178 is a very-high-energy -ray source spatially coincident with the young and energetic pulsar PSR J18131749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813178 region, taking advantage of improved analysis methods and an extended data set. Using data taken by the High Energy Stereoscopic System (H.E.S.S.) experiment and the Fermi-LAT, we aim to describe the -ray emission in the region with a consistent model, to provide insights into its origin. We performed a likelihood-based analysis on 32 hours of H.E.S.S. data and 12 years of Fermi-LAT data and fit a spectro-morphological model to the combined datasets. These results allowed us to develop a physical model for the origin of the observed -ray emission in the region. In addition to the compact very-high-energy -ray emission centered on the pulsar, we find a significant yet previously undetected component along the Galactic plane. With Fermi-LAT data, we confirm extended high-energy emission consistent with the position and elongation of the extended emission observed with H.E.S.S. These results establish a consistent description of the emission in the region from GeV energies to several tens of TeV. This study suggests that HESS J1813178 is associated with a -ray PWN powered by PSR J18131749. A possible origin of the extended emission component is inverse Compton emission from electrons and positrons that have escaped the confines …
Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and HESS analysis
Authors
F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,A Baktash,V Barbosa Martins,R Batzofin,Y Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M de Lavergne,J Borowska,F Bradascio,M Breuhaus,R Brose,A Brown,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,T Bylund,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,P Chambery,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,P Cristofari,J Devin,A Djannati-Ataï,J Djuvsland,A Dmytriiev,S Einecke,J-P Ernenwein,S Fegan,K Feijen,M Filipović,G Fontaine,M Füßling,S Funk,S Gabici,YA Gallant,G Giavitto,D Glawion,JF Glicenstein,J Glombitza,P Goswami,G Grolleron,M-H Grondin,L Haerer,JA Hinton,W Hofmann,TL Holch,M Holler,D Horns,M Jamrozy,F Jankowsky,V Joshi,E Kasai,K Katarzyński,R Khatoon,B Khélifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,A Kundu,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,A Luashvili,J Mackey,D Malyshev,V Marandon,P Marinos,G Martí-Devesa,R Marx,A Mehta,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,T Murach,M de Naurois,J Niemiec,P O'Brien,S Ohm,L Olivera-Nieto,E Wilhelmi,M Ostrowski,S Panny,M Panter,RD Parsons,G Peron,DA Prokhorov,G Pühlhofer,M Punch,A Quirrenbach,M Regeard,P Reichherzer,A Reimer,O Reimer,H Ren,M Renaud,B Reville,F Rieger,G Roellinghoff,B Rudak,V Sahakian,H Salzmann,M Sasaki,F Schüssler,HM Schutte,JNS Shapopi,A Specovius,S Spencer,Ł Stawarz,R Steenkamp,S Steinmassl,C Steppa,K Streil,I Sushch,H Suzuki,T Takahashi,T Tanaka,R Terrier,M Tluczykont,N Tsuji,T Unbehaun,C van Eldik,M Vecchi,J Veh,C Venter
Journal
arXiv preprint arXiv:2403.12608
Published Date
2024/3/19
The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's -ray emission between 1 GeV and 100 TeV, that is over five orders of magnitude in energy. Using the open-source software package Gammapy, we combine 11.4 yr of data from the Fermi Large Area Telescope and 80 h of High Energy Stereoscopic System (H.E.S.S.) data at the event level and provide a measurement of the spatial extension of the nebula and its energy spectrum. We find evidence for a shrinking of the nebula with increasing -ray energy. Furthermore, we fit several phenomenological models to the measured data, finding that none of them can fully describe the spatial extension and the spectral energy distribution at the same time. Especially the extension measured at TeV energies appears too large when compared to the X-ray emission. Our measurements probe the structure of the magnetic field between the pulsar wind termination shock and the dust torus, and we conclude that the magnetic field strength decreases with increasing distance from the pulsar. We complement our study with a careful assessment of systematic uncertainties.
Astronomy potential of KM3NeT/ARCA
Authors
S Aiello,A Albert,M Alshamsi,S Alves Garre,Z Aly,A Ambrosone,F Ameli,M Andre,E Androutsou,M Anguita,L Aphecetche,M Ardid,S Ardid,H Atmani,J Aublin,F Badaracco,L Bailly-Salins,Z Bardacová,B Baret,A Bariego-Quintana,A Baruzzi,S Basegmez du Pree,Y Becherini,M Bendahman,F Benfenati,M Benhassi,DM Benoit,E Berbee,V Bertin,S Biagi,M Boettcher,D Bonanno,J Boumaaza,M Bouta,M Bouwhuis,C Bozza,RM Bozza,H Brânzas,F Bretaudeau,M Breuhaus,R Bruijn,J Brunner,R Bruno,E Buis,R Buompane,J Busto,B Caiffi,D Calvo,S Campion,A Capone,F Carenini,V Carretero,T Cartraud,P Castaldi,V Cecchini,S Celli,L Cerisy,M Chabab,M Chadolias,A Chen,S Cherubini,T Chiarusi,M Circella,R Cocimano,JAB Coelho,A Coleiro,R Coniglione,P Coyle,A Creusot,G Cuttone,R Dallier,Y Darras,A De Benedittis,B De Martino,V Decoene,R Del Burgo,I Del Rosso,LS Di Mauro,I Di Palma,AF Díaz,C Diaz,D Diego-Tortosa,C Distefano,A Domi,C Donzaud,D Dornic,M Dörr,E Drakopoulou,D Drouhin,JG Ducoin,R Dvornický,T Eberl,E Eckerová,A Eddymaoui,T van Eeden,M Eff,D van Eijk,I El Bojaddaini,S El Hedri,A Enzenhöfer,G Ferrara,MD Filipovic,F Filippini,D Franciotti,LA Fusco,J Gabriel,S Gagliardini,T Gal,J García Méndez,A Garcia Soto,C Gatius Oliver,N Geißelbrecht,H Ghaddari,L Gialanella,BK Gibson,E Giorgio,I Goos,P Goswami,D Goupilliere,SR Gozzini,R Gracia,K Graf,C Guidi,B Guillon,M Gutiérrez,H van Haren,A Heijboer,A Hekalo,L Hennig,JJ Hernández-Rey,W Idrissi Ibnsalih,G Illuminati,M de Jong,P de Jong,BJ Jung,P Kalaczynski,O Kalekin,UF Katz,G Kistauri,C Kopper,A Kouchner,V Kueviakoe,V Kulikovskiy,R Kvatadze,M Labalme,R Lahmann,G Larosa,C Lastoria,A Lazo,S Le Stum
Journal
arXiv e-prints
Published Date
2024/2
The KM3NeT/ARCA neutrino detector is currently under construction at 3500 m depth offshore Capo Passero, Sicily, in the Mediterranean Sea. The main science objectives are the detection of high-energy cosmic neutrinos and the discovery of their sources. Simulations were conducted for the full KM3NeT/ARCA detector, instrumenting a volume of 1 km , to estimate the sensitivity and discovery potential to point-like neutrino sources and an all-sky diffuse neutrino flux. This paper covers the reconstruction of track-and shower-like signatures, as well as the criteria employed for neutrino event selection. By leveraging both the track and shower observation channels, the KM3NeT/ARCA detector demonstrates the capability to detect the diffuse astrophysical neutrino flux within half a year of operation, achieving a 5 statistical significance. With an angular resolution below 0.1 for tracks and under 2 for showers, the …
Atmospheric muons measured with the KM3NeT detectors in comparison with updated numeric predictions
Authors
S Aiello,A Albert,M Alshamsi,S Alves Garre,A Ambrosone,F Ameli,M Andre,E Androutsou,M Anguita,L Aphecetche,M Ardid,S Ardid,A Arsenic,H Atmani,J Aublin,F Badaracco,L Bailly-Salins,Z Bardačová,B Baret,A Bariego-Quintana,S Basegmez Du Pree,Y Becherini,M Bendahman,F Benfenati,M Benhassi,DM Benoit,E Berbee,V Bertin,S Biagi,M Boettcher,D Bonanno,J Boumaaza,M Bouta,M Bouwhuis,C Bozza,RM Bozza,H Brânzaş,F Bretaudeau,M Breuhaus,R Bruijn,J Brunner,R Bruno,E Buis,R Buompane,J Busto,B Caiffi,D Calvo,S Campion,A Capone,F Carenini,V Carretero,T Cartraud,P Castaldi,V Cecchini,S Celli,L Cerisy,M Chabab,M Chadolias,A Chen,S Cherubini,T Chiarusi,M Circella,R Cocimano,JAB Coelho,A Coleiro,A Condorelli,R Coniglione,P Coyle,A Creusot,G Cuttone,R Dallier,Y Darras,A de Benedittis,B de Martino,V Decoene,R del Burgo,I del Rosso,LS Di Mauro,I Di Palma,AF Díaz,C Diaz,D Diego-Tortosa,C Distefano,A Domi,C Donzaud,D Dornic,M Dörr,E Drakopoulou,D Drouhin,J-G Ducoin,R Dvornický,T Eberl,E Eckerová,A Eddymaoui,T van Eeden,M Eff,D van Eijk,I El Bojaddaini,S El Hedri,A Enzenhöfer,G Ferrara,MD Filipović,F Filippini,D Franciotti,LA Fusco,S Gagliardini,T Gal,J García Méndez,A Garcia Soto,C Gatius Oliver,N Geißelbrecht,H Ghaddari,L Gialanella,BK Gibson,E Giorgio,I Goos,P Goswami,SR Gozzini,R Gracia,K Graf,C Guidi,B Guillon,M Gutiérrez,C Haack,H van Haren,A Heijboer,A Hekalo,L Hennig,JJ Hernández-Rey,W Idrissi Ibnsalih,G Illuminati,D Joly,M de Jong,P de Jong,BJ Jung,P Kalaczyński,O Kalekin,UF Katz,A Khatun,G Kistauri,C Kopper,A Kouchner,V Kueviakoe,V Kulikovskiy,R Kvatadze,M Labalme,R Lahmann,G Larosa,C Lastoria,A Lazo
Published Date
2024/4/23
The measurement of the flux of muons produced in cosmic ray air showers is essential for the study of primary cosmic rays. Such measurements are important in extensive air shower detectors to assess the energy spectrum and the chemical composition of the cosmic ray flux, complementary to the information provided by fluorescence detectors. Detailed simulations of the cosmic ray air showers are carried out, using codes such as CORSIKA, to estimate the muon flux at sea level. These simulations are based on the choice of hadronic interaction models, for which improvements have been implemented in the post-LHC era. In this work, a deficit in simulations that use state-of-the-art QCD models with respect to the measurement deep underwater with the KM3NeT neutrino detectors is reported. The KM3NeT/ARCA and KM3NeT/ORCA neutrino telescopes are sensitive to TeV muons originating mostly from primary cosmic rays with energies around 10 TeV. The predictions of state-of-the-art QCD models show that the deficit with respect to the data is constant in zenith angle; no dependency on the water overburden is observed. The observed deficit at a depth of several kilometres is compatible with the deficit seen in the comparison of the simulations and measurements at sea level.
Multiwavelength Observations of the Blazar PKS 0735+ 178 in Spatial and Temporal Coincidence with an Astrophysical Neutrino Candidate IceCube-211208A
Authors
A Acharyya,CB Adams,A Archer,P Bangale,JT Bartkoske,P Batista,W Benbow,A Brill,JH Buckley,JL Christiansen,AJ Chromey,M Errando,A Falcone,Q Feng,GM Foote,L Fortson,A Furniss,G Gallagher,W Hanlon,D Hanna,O Hervet,CE Hinrichs,J Hoang,J Holder,TB Humensky,W Jin,P Kaaret,M Kertzman,M Kherlakian,D Kieda,TK Kleiner,N Korzoun,S Kumar,MJ Lang,M Lundy,G Maier,CE McGrath,MJ Millard,J Millis,CL Mooney,P Moriarty,R Mukherjee,S O’Brien,RA Ong,M Pohl,E Pueschel,J Quinn,K Ragan,PT Reynolds,D Ribeiro,E Roache,I Sadeh,AC Sadun,L Saha,M Santander,GH Sembroski,R Shang,M Splettstoesser,A Kaushik Talluri,JV Tucci,VV Vassiliev,A Weinstein,DA Williams,SL Wong,J Woo,F Aharonian,J Aschersleben,M Backes,V Barbosa Martins,R Batzofin,Yvonne Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M De Bony De Lavergne,J Borowska,M Bouyahiaoui,F Bradascio,M Breuhaus,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,S Dai,J Damascene Mbarubucyeye,A Djannati-Atai,A Dmytriiev,V Doroshenko,S Einecke,J-P Ernenwein,G Fichet De Clairfontaine,M Filipovic,G Fontaine,M Füßling,S Funk,S Gabici,S Ghafourizadeh,G Giavitto,D Glawion,JF Glicenstein,P Goswami,G Grolleron,L Haerer,JA Hinton,TL Holch,M Holler,D Horns,Marek Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,R Khatoon,B Khelifi,S Klepser,W Kluźniak,K Kosack,D Kostunin,RG Lang,S Le Stum,A Lemiere,J-P Lenain,F Leuschner,T Lohse,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,G Martí-Devesa,R Marx,A Mitchell
Journal
The Astrophysical Journal
Published Date
2023/8/23
We report on multiwavelength target-of-opportunity observations of the blazar PKS 0735+ 178, located 2 fdg 2 away from the best-fit position of the IceCube neutrino event IceCube-211208A detected on 2021 December 8. The source was in a high-flux state in the optical, ultraviolet, X-ray, and GeV γ-ray bands around the time of the neutrino event, exhibiting daily variability in the soft X-ray flux. The X-ray data from Swift-XRT and NuSTAR characterize the transition between the low-energy and high-energy components of the broadband spectral energy distribution (SED), and the γ-ray data from Fermi-LAT, VERITAS, and HESS require a spectral cutoff near 100 GeV. Both the X-ray and γ-ray measurements provide strong constraints on the leptonic and hadronic models. We analytically explore a synchrotron self-Compton model, an external Compton model, and a lepto-hadronic model. Models that are entirely based …
Constraints on the intergalactic magnetic field using Fermi-LAT and HESS blazar observations
Authors
F Aharonian,J Aschersleben,M Backes,V Barbosa Martins,R Batzofin,Yvonne Becherini,D Berge,B Bi,M Bouyahiaoui,M Breuhaus,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,Tomas Bylund,S Caroff,S Casanova,J Celic,M Cerruti,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,M De Bony,K Egberts,J-P Ernenwein,G Fichet De Clairfontaine,Miroslav Filipovic,G Fontaine,M Füssling,S Funk,S Gabici,S Ghafourizadeh,G Giavitto,D Glawion,JF Glicenstein,P Goswami,M-H Grondin,L Haerer,TL Holch,M Holler,D Horns,Marek Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,R Khatoon,B Khélifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,J-P Lenain,F Leuschner,T Lohse,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,G Martí-Devesa,R Marx,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,J Muller,T Murach,K Nakashima,J Niemiec,S Ohm,L Olivera-Nieto,E de Ona Wilhelmi,S Panny,M Panter,RD Parsons,G Peron,DA Prokhorov,H Prokoph,G Pühlhofer,M Punch,A Quirrenbach,P Reichherzer,A Reimer,O Reimer,B Reville,F Rieger,G Rowell,B Rudak,E Ruiz-Velasco,V Sahakian,DA Sanchez,M Sasaki,F Schüssler,HM Schutte,U Schwanke,JNS Shapopi,H Sol,S Spencer,S Steinmassl,H Suzuki,T Takahashi,T Tanaka,AM Taylor,R Terrier,C Thorpe-Morgan,M Tsirou,N Tsuji,Y Uchiyama,C Van Eldik,J Veh,C Venter,SJ Wagner,R White,Alicja Wierzcholska,Yu Wun Wong,M Zacharias,D Zargaryan,AA Zdziarski,S Zouari,N Żywucka,HESS Collaboration,Fermi-LAT Collaboration
Journal
The Astrophysical Journal Letters
Published Date
2023/6/21
Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy gamma rays from distant blazars. Gamma rays interact with the extragalactic background light to produce electron− positron pairs, which can subsequently initiate electromagnetic cascades. The gamma-ray signature of the cascade depends on the IGMF since it deflects the pairs. Here we report on a new search for this cascade emission using a combined data set from the Fermi Large Area Telescope and the High Energy Stereoscopic System. Using state-of-the-art Monte Carlo predictions for the cascade signal, our results place …
HESS follow-up observations of GRB221009A
Authors
HESS Collaboration,F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,A Baktash,V Barbosa Martins,R Batzofin,Y Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M de Lavergne,J Borowska,M Bouyahiaoui,F Bradascio,M Breuhaus,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,S Caroff,S Casanova,J Celic,M Cerruti,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,S Dai,J Mbarubucyeye,J Devin,A Djannati-Ataï,A Dmytriiev,V Doroshenko,K Egberts,S Einecke,J-P Ernenwein,S Fegan,G Fichet de Clairfontaine,M Filipovic,G Fontaine,M Füßling,S Funk,S Gabici,S Ghafourizadeh,G Giavitto,D Glawion,JF Glicenstein,P Goswami,G Grolleron,M-H Hinton,TL Holch,M Holler,D Horns,Zhiqiu Huang,M Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,R Khatoon,B Khélifi,W Kluźniak,Nu Komin,R Konno,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,JP Lenain,F Leuschner,T Lohse,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,G Martí-Devesa,R Marx,M Meyer,A Mitchell,L Mohrmann,A Montanari,E Moulin,T Murach,K Nakashima,M de Naurois,J Niemiec,A Priyana Noel,P O'Brien,S Ohm,L Olivera-Nieto,E Wilhelmi,M Ostrowski,S Panny,M Panter,RD Parsons,G Peron,DA Prokhorov,H Prokoph,G Pühlhofer,M Punch,A Quirrenbach,P Reichherzer,A Reimer,O Reimer,H Ren,M Renaud,B Reville,F Rieger,G Rowell,B Rudak,E Ruiz-Velasco,V Sahakian,H Salzmann,A Santangelo,M Sasaki,J Schäfer,F Schüssler,HM Schutte,U Schwanke,JNS Shapopi,A Specovius,S Spencer,Ł Stawarz,R Steenkamp,S Steinmassl,C Steppa,I Sushch,H Suzuki,T Takahashi,T Tanaka,R Terrier,N Tsuji,Y Uchiyama,M Vecchi,C Venter
Journal
arXiv preprint arXiv:2303.10558
Published Date
2023/3/19
GRB221009A is the brightest gamma-ray burst ever detected. To probe the very-high-energy (VHE, \!100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hours after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of above GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the SED occurring above the X-ray band. Compared to the VHE-bright GRB190829A, the upper limits for GRB221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB221009A, effectively ruling out an IC dominated scenario.
The Vanishing of the Primary Emission Region in PKS 1510–089
Authors
F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,V Barbosa Martins,J Barnard,R Batzofin,Yvonne Becherini,D Berge,K Bernlöhr,B Bi,M de Bony de Lavergne,M Böttcher,C Boisson,J Bolmont,J Borowska,M Bouyahiaoui,F Bradascio,M Breuhaus,R Brose,AM Brown,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,J Damascene Mbarubucyeye,ID Davids,A Djannati-Atai,A Dmytriiev,V Doroshenko,K Egberts,S Einecke,J-P Ernenwein,S Fegan,G Fontaine,M Fuessling,S Funk,S Gabici,S Ghafourizadeh,G Giavitto,D Glawion,JF Glicenstein,P Goswami,G Grolleron,L Haerer,W Hofmann,TL Holch,M Holler,D Horns,Marek Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,R Khatoon,B Khelifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,J-P Lenain,F Leuschner,A Luashvili,J Mackey,V Marandon,P Marchegiani,G Martí-Devesa,R Marx,A Mehta,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,M de Naurois,J Niemiec,A Priyana Noel,P O’Brien,S Ohm,L Olivera-Nieto,E de Ona Wilhelmi,Michał Ostrowski,S Panny,M Panter,G Peron,DA Prokhorov,G Pühlhofer,M Punch,A Quirrenbach,P Reichherzer,A Reimer,O Reimer,H Ren,F Rieger,G Rowell,B Rudak,H Rueda Ricarte,E Ruiz-Velasco,V Sahakian,H Salzmann,DA Sanchez,A Santangelo,M Sasaki,F Schüssler,HM Schutte,U Schwanke,JNS Shapopi,H Sol,A Specovius,S Spencer,R Steenkamp,S Steinmassl,C Steppa,I Sushch,H Suzuki,T Takahashi,T Tanaka,R Terrier,N Tsuji,C van Eldik,B van Soelen,M Vecchi,J Veh,J Vink,T Wach,SJ Wagner,A Wierzcholska,M Zacharias,D Zargaryan,AA Zdziarski,A Zech,S Zouari
Journal
The Astrophysical Journal Letters
Published Date
2023/8/1
In 2021 July, PKS 1510− 089 exhibited a significant flux drop in the high-energy γ-ray (by a factor 10) and optical (by a factor 5) bands and remained in this low state throughout 2022. Similarly, the optical polarization in the source vanished, resulting in the optical spectrum being fully explained through the steady flux of the accretion disk and the broad-line region. Unlike the aforementioned bands, the very-high-energy γ-ray and X-ray fluxes did not exhibit a significant flux drop from year to year. This suggests that the steady-state very-high-energy γ-ray and X-ray fluxes originate from a different emission region than the vanished parts of the high-energy γ-ray and optical jet fluxes. The latter component has disappeared through either a swing of the jet away from the line of sight or a significant drop in the photon production efficiency of the jet close to the black hole. Either change could become visible in high …
Detection of extended γ-ray emission around the Geminga pulsar with HESS
Authors
F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,V Barbosa Martins,R Batzofin,Yvonne Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,J Borowska,M Bouyahiaoui,F Bradascio,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,F Cangemi,S Caroff,S Casanova,J Celic,M Cerruti,P Chambery,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,J Damascene Mbarubucyeye,J Devin,A Djannati-Ataï,A Dmytriiev,K Egberts,S Einecke,J-P Ernenwein,K Feijen,G Fichet De Clairfontaine,Miroslav Filipovic,G Fontaine,M Füßling,S Funk,S Gabici,YA Gallant,S Ghafourizadeh,G Giavitto,L Giunti,D Glawion,JF Glicenstein,P Goswami,G Grolleron,M-H Grondin,L Haerer,M Haupt,G Hermann,JA Hinton,W Hofmann,TL Holch,M Holler,D Horns,Zhiqiu Huang,Marek Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,B Khélifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,T Lohse,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,P Marinos,G Martí-Devesa,R Marx,G Maurin,PJ Meintjes,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,J Muller,K Nakashima,M de Naurois,J Niemiec,A Priyana Noel,P O’Brien,S Ohm,L Olivera-Nieto,E de Ona Wilhelmi,Michał Ostrowski,S Panny,M Panter,RD Parsons,G Peron,DA Prokhorov,G Pühlhofer,A Quirrenbach,A Reimer,O Reimer,M Renaud,B Reville,F Rieger,G Rowell,B Rudak,H Rueda Ricarte,E Ruiz-Velasco,V Sahakian,H Salzmann,A Santangelo,M Sasaki,F Schüssler,HM Schutte,U Schwanke,JNS Shapopi,A Sinha,H Sol,A Specovius,S Spencer,S Steinmassl,I Sushch,H Suzuki,T Takahashi,T Tanaka,T Tavernier,AM Taylor,R Terrier,C Thorpe-Morgan
Journal
Astronomy & Astrophysics
Published Date
2023/5/1
Geminga is an enigmatic radio-quiet γ-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy γ-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenkov telescopes (IACTs) despite targeted observations. The detection of γ-ray emission on angular scales ≳2º poses a considerable challenge for the background estimation in IACT data analysis. With recent developments in understanding the complementary background estimation techniques of water Cherenkov and atmospheric Cherenkov instruments, the H.E.S.S. IACT array can now confirm the detection of highly extended γ-ray emission around the Geminga pulsar with a radius of at least 3º in the energy …
Probing hadronic cosmic ray acceleration in infrared bright SNRs with Fermi-LAT
Authors
Pranjupriya Goswami,Enrique Mestre,Iurii Sushch,Emma de Oña
Published Date
2023/7/26
Supernova remnants (SNRs) have long been recognized as the primary candidates for production of Galactic cosmic rays. Although the evidence of acceleration to PeV energies needed to explain the ‘knee’feature in the cosmic-ray spectrum is elusive it is clear that particles can be accelerated to relativistic energies at SNR shocks through the diffusive shock acceleration. Accelerated protons and heavier nuclei subsequently interact with the surrounding matter, including dense molecular clouds (MCs), resulting in the generation of ????0 mesons that subsequently decay into ????-rays. The spectral energy distribution (SED) of hadronic gamma-ray sources exhibits a distinctive pion-decay bump, characterized by a rising spectrum below 200 MeV followed by a hard component extending up to the maximum energy. This characteristic spectral feature directly indicates the signature of proton-proton interactions. This feature can be used to differentiate hadronic scenarios from leptonic mechanisms of gamma-ray emission production such as inverse Compton (IC) scattering and/or bremsstrahlung. Identification of hadronic accelerators among SNRs is important in the view of understanding the origins of cosmic rays that consist mainly of protons.Recent observations by the Fermi Large Area Telescope (LAT) have revealed this characteristic hadronic spectrum for several supernova remnants, including IC 443, W44, W49B, W51C, and HB 21 [6, 8, 9] indicating their interaction with molecular clouds. In a comprehensive study of 4FGL catalog sources situated within 5◦ from the Galactic plane, the Fermi-LAT collaboration [6] confirmed 13 SNRs, such as G31. 9 …
The Power Board of the KM3NeT Digital Optical Module: design, upgrade, and production
Authors
S Aiello,A Albert,S Alves Garre,Z Aly,A Ambrosone,F Ameli,M Andre,E Androutsou,M Anguita,L Aphecetche,M Ardid,S Ardid,H Atmani,J Aublin,F Badaracco,L Bailly-Salins,Z Bardacova,B Baret,A Bariego Quintana,S Pree,Y Becherini,M Bendahman,F Benfenati,M Benhassi,DM Benoit,E Berbee,V Bertin,V van Beveren,S Biagi,M Boettcher,D Bonanno,J Boumaaza,M Bouta,M Bouwhuis,C Bozza,RM Bozza,H Branzas,F Bretaudeau,R Bruijn,J Brunner,R Bruno,E Buis,R Buompane,J Busto,B Caiffi,D Calvo,S Campion,A Capone,F Careniniu,V Carretero,T Cartraud,P Castaldi,V Cecchini,S Celli,L Cerisy,M Chabab,M Chadolias,C Champion,A Chena,S Cherubini,T Chiarusi,M Circella,R Cocimano,JAB Coelho,A Coleiro,S Colonges,R Coniglione,P Coyle,A Creusot,G Cuttone,R Dallier,Y Darras,A De Benedittis,B De Martino,V Decoene,R Del Burgo,I Del Rosso,UM Di Cerbo,LS Di Mauro,I Di Palma,AF Díaz,C Diaz,D Diego-Tortosa,C Distefano,A Domia,C Donzaud,D Dornic,M Dorra,E Drakopoulou,D Drouhin,R Dvornicky,T Eberla,E Eckerova,A Eddymaoui,T van Eeden,M Eff,D van Eijk,I El Bojaddaini,S El Hedri,A Enzenhofer,G Ferrara,MD Filipovica,F Filippini,D Franciotti,LA Fusco,O Gabellaa,J Gabriela,S Gagliardini,T Gal,J Garcıa Mendez,A Garcia Soto,C Gatius Oliver,N Geißelbrecht,H Ghaddari,L Gialanella,BK Gibson,E Giorgio,I Goos,P Goswami,D Goupilliere,SR Gozzini,R Gracia,K Grafa,C Guidi,B Guillon,M Gutierrez,H van Haren,A Heijboer,A Hekalo,L Henniga,JJ Hernandez-Rey,W Idrissi Ibnsalih,G Illuminati,P Jansweijer,M de Jonga,P de Jonga,BJ Jung,P Kalaczynski,O Kalekin,UF Katz,A Khatun,G Kistauri,C Kopper,A Kouchner,V Kueviakoe,V Kulikovskiy,R Kvatadze,M Labalme,R Lahmann,G Larosa
Journal
arXiv preprint arXiv:2311.14872
Published Date
2023/11/24
The KM3NeT Collaboration is building an underwater neutrino observatory at the bottom of the Mediterranean Sea consisting of two neutrino telescopes, both composed of a three-dimensional array of light detectors, known as digital optical modules. Each digital optical module contains a set of 31 three inch photomultiplier tubes distributed over the surface of a 0.44 m diameter pressure-resistant glass sphere. The module includes also calibration instruments and electronics for power, readout and data acquisition. The power board was developed to supply power to all the elements of the digital optical module. The design of the power board began in 2013, and several prototypes were produced and tested. After an exhaustive validation process in various laboratories within the KM3NeT Collaboration, a mass production batch began, resulting in the construction of over 1200 power boards so far. These boards were integrated in the digital optical modules that have already been produced and deployed, 828 until October 2023. In 2017, an upgrade of the power board, to increase reliability and efficiency, was initiated. After the validation of a pre-production series, a production batch of 800 upgraded boards is currently underway. This paper describes the design, architecture, upgrade, validation, and production of the power board, including the reliability studies and tests conducted to ensure the safe operation at the bottom of the Mediterranean Sea throughout the observatory's lifespan
Detection of extended gamma-ray emission around the Geminga pulsar with HESS
Authors
HESS Collaboration,F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,V Barbosa Martins,R Batzofin,Y Becherini,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,J Borowska,M Bouyahiaoui,F Bradascio,R Brose,F Brun,B Bruno,T Bulik,C Burger Scheidlin,F Cangemi,S Caroff,S Casanova,J Celic,M Cerruti,P Chambery,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,G Cotter,J Mbarubucyeye,J Devin,A Djannati-Ataï,A Dmytriiev,K Egberts,S Einecke,JP Ernenwein,K Feijen,G Fichet de Clairfontaine,M Filipovic,G Fontaine,M Füssling,S Funk,S Gabici,YA Gallant,S Ghafourizadeh,G Giavitto,L Giunti,D Glawion,JF Glicenstein,P Goswami,G Grolleron,M-H Grondin,L Haerer,M Haupt,G Hermann,JA Hinton,W Hofmann,TL Holch,M Holler,D Horns,Zhiqiu Huang,M Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,B Khélifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,T Lohse,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,P Marinos,G Martí-Devesa,R Marx,G Maurin,PJ Meintjes,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,J Muller,K Nakashima,M de Naurois,J Niemiec,A Priyana Noel,P O'Brien,S Ohm,L Olivera-Nieto,E Wilhelmi,M Ostrowski,S Panny,M Panter,RD Parsons,G Peron,DA Prokhorov,G Pühlhofer,A Quirrenbach,A Reimer,O Reimer,M Renaud,B Reville,F Rieger,G Rowell,B Rudak,H Rueda Ricarte,E Ruiz-Velasco,V Sahakian,H Salzmann,A Santangelo,M Sasaki,F Schüssler,HM Schutte,U Schwanke,JNS Shapopi,A Sinha,H Sol,A Specovius,S Spencer,Ł Stawarz,S Steinmassl,I Sushch,H Suzuki,T Takahashi,T Tanaka,T Tavernier,AM Taylor
Journal
arXiv preprint arXiv:2304.02631
Published Date
2023/4/5
Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenkov telescopes (IACTs) despite targeted observations. The detection of gamma-ray emission on angular scales > 2 deg poses a considerable challenge for the background estimation in IACT data analysis. With recent developments in understanding the complementary background estimation techniques of water Cherenkov and atmospheric Cherenkov instruments, the H.E.S.S. IACT array can now confirm the detection of highly extended gamma-ray emission around the Geminga pulsar with a radius of at least 3 deg in the energy range 0.5-40 TeV. We find no indications for statistically significant asymmetries or energy-dependent morphology. A flux normalisation of cmsTeV at 1 TeV is obtained within a 1 deg radius region around the pulsar. To investigate the particle transport within the halo of energetic leptons around the pulsar, we fitted an electron diffusion model to the data. The normalisation of the diffusion coefficient obtained of cms, at an electron energy of 100 TeV, is compatible with values previously reported for the pulsar halo around Geminga, which is considerably below the Galactic average.
Searching for gamma-ray counterparts of FRBs with HESS
Authors
F Aharonian,F Ait Benkhali,A Alkan,J Aschersleben,H Ashkar,M Backes,A Baktash,V Barbosa Martins,A Barnacka,J Barnard,R Batzofin,Y Becherini,G Beck,D Berge,K Bernlöhr,B Bi,M Böttcher,C Boisson,J Bolmont,M de Bony de Lavergne,J Borowska,M Bouyahiaoui,F Bradascio,M Breuhaus,R Brose,A Brown,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,T Bylund,F Cangemi,S Caroff,S Casanova,R Cecil,J Celic,M Cerruti,P Chambery,T Chand,S Chandra,A Chen,J Chibueze,O Chibueze,T Collins,G Cotter,P Cristofari,J Damascene Mbarubucyeye,ID Davids,J Davies,L de Jonge,J Devin,A Djannati-Ataï,A Dmytriiev,V Doroshenko,L Dreyer,L Du Plessis,K Egberts,S Einecke,J-P Ernenwein,S Fegan,K Feijen,G Fichet de Clairfontaine,G Fontaine,F Lott,M Füßling,S Funk,S Gabici,YA Gallant,S Ghafourizadeh,G Giavitto,L Giunti,D Glawion,JF Glicenstein,J Glombitza,P Goswami,G Grolleron,M-H Grondin,L Haerer,S Hattingh,M Haupt,G Hermann,JA Hinton,W Hofmann,TL Holch,M Holler,D Horns,Zhiqiu Huang,A Jaitly,M Jamrozy,F Jankowsky,A Jardin-Blicq,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,H Katjaita,D Khangulyan,R Khatoon,B Khélifi,S Klepser,W Kluźniak,Nu Komin,R Konno,K Kosack,D Kostunin,A Kundu,G Lamanna,RG Lang,S Le Stum,V Lefranc,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,A Marcowith,P Marinos,G Martí-Devesa,R Marx,G Maurin,A Mehta,PJ Meintjes,M Meyer,A Mitchell,R Moderski,L Mohrmann,A Montanari,C Moore,E Moulin,T Murach,K Nakashima,M de Naurois,H Ndiyavala,J Niemiec,A Priyana Noel,P O'Brien,S Ohm,L Olivera-Nieto,E de Ona Wilhelmi,M Ostrowski,E Oukacha,S Panny,M Panter,RD Parsons,U Pensec
Published Date
2023/7/26
Fast Radio Bursts (FRBs) are highly energetic, extremely short-lived bursts of radio flashes.Despite extensive research, the exact cause of these outbursts remains a mystery. One of themost accredited models suggests that they originate from highly magnetized and rapidly spinningneutron stars known as magnetars. The high luminosity, short duration, and high dispersionmeasure of these events suggest they result from extreme, high-energy astrophysical processesof extragalactic origin. The number of detected FRBs, including repeating ones, has grownrapidly in recent years. Except for FRB20200428, that is associated to the galactic magnetarSGR1925+2154, no multi-wavelength counterparts to any FRB has been detected yet. The HighEnergy Stereoscopic System (H.E.S.S.) telescope has developed a program to uncover the natureof these mysterious events by searching for their gamma-ray counterparts. This contributionprovides an overview of the searches for FRB sources conducted by H.E.S.S., including follow-upobservations and simultaneous multi-wavelength campaigns with radio and X-ray observatories
Discovery of a radiation component from the Vela pulsar reaching 20 teraelectronvolts
Journal
Nature astronomy
Published Date
2023/11
Gamma-ray observations have established energetic isolated pulsars as outstanding particle accelerators and antimatter factories. However, many questions are still open regarding the acceleration and radiation processes involved, as well as the locations where they occur. The radiation spectra of all gamma-ray pulsars observed to date show strong cutoffs or a break above energies of a few gigaelectronvolts. Using the High Energy Stereoscopic System’s Cherenkov telescopes, we discovered a radiation component from the Vela pulsar which emerges beyond this generic cutoff and extends up to energies of at least 20 teraelectronvolts. This is an order of magnitude larger than in the case of the Crab pulsar, the only other pulsar detected in the teraelectronvolt energy range. Our results challenge the state-of-the-art models for the high-energy emission of pulsars. Furthermore, they pave the way for investigating …
HESS J1809− 193: A halo of escaped electrons around a pulsar wind nebula?
Authors
F Aharonian,F Ait Benkhali,J Aschersleben,H Ashkar,M Backes,V Barbosa Martins,R Batzofin,Yvonne Becherini,D Berge,M Böttcher,C Boisson,J Bolmont,J Borowska,M Bouyahiaoui,F Bradascio,M Breuhaus,R Brose,F Brun,B Bruno,T Bulik,C Burger-Scheidlin,Tomas Bylund,S Caroff,S Casanova,J Celic,M Cerruti,P Chambery,T Chand,A Chen,J Chibueze,O Chibueze,J Damascene Mbarubucyeye,A Djannati-Ataï,A Dmytriiev,S Einecke,J-P Ernenwein,K Feijen,Miroslav Filipovic,G Fontaine,M Füßling,S Funk,S Gabici,YA Gallant,S Ghafourizadeh,G Giavitto,L Giunti,D Glawion,P Goswami,G Grolleron,M-H Grondin,L Haerer,JA Hinton,W Hofmann,TL Holch,M Holler,D Horns,Zhiqiu Huang,Marek Jamrozy,F Jankowsky,V Joshi,I Jung-Richardt,E Kasai,K Katarzyński,B Khélifi,W Kluźniak,Nu Komin,K Kosack,D Kostunin,RG Lang,S Le Stum,F Leitl,A Lemière,M Lemoine-Goumard,J-P Lenain,F Leuschner,T Lohse,A Luashvili,I Lypova,J Mackey,D Malyshev,V Marandon,P Marchegiani,A Marcowith,P Marinos,G Martí-Devesa,R Marx,A Mitchell,R Moderski,L Mohrmann,A Montanari,E Moulin,J Muller,K Nakashima,M de Naurois,J Niemiec,A Priyana Noel,S Ohm,L Olivera-Nieto,E de Ona Wilhelmi,Michał Ostrowski,S Panny,M Panter,RD Parsons,DA Prokhorov,G Pühlhofer,M Punch,A Quirrenbach,P Reichherzer,A Reimer,O Reimer,M Renaud,B Reville,F Rieger,G Rowell,B Rudak,V Sahakian,A Santangelo,M Sasaki,HM Schutte,U Schwanke,JNS Shapopi,H Sol,A Specovius,S Spencer,R Steenkamp,S Steinmassl,I Sushch,H Suzuki,T Takahashi,T Tanaka,R Terrier,C Thorpe-Morgan,M Tsirou,N Tsuji,Y Uchiyama,C van Eldik,M Vecchi,J Veh,C Venter,J Vink,T Wach,SJ Wagner,R White,A Wierzcholska,Yu Wun Wong,M Zacharias,D Zargaryan,AA Zdziarski,A Zech,S Zouari
Journal
Astronomy & Astrophysics
Published Date
2023/4/1
Context HESS J1809−193 is an unassociated very-high-energy γ-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809−1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of γ-ray emission up to energies of ∼100 TeV with the HAWC observatory has led to renewed interest in HESS J1809−193.Aims We aim to understand the origin of the γ-ray emission of HESS J1809−193.Methods We analysed 93.2 h of data taken on HESS J1809−193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809−193. The obtained results are interpreted in a time-dependent modelling framework …
Gamma-ray detection of newly discovered Ancora SNR: G288. 8-6.3
Authors
Christopher Burger-Scheidlin,Robert Brose,Jonathan Mackey,MD Filipović,Pranjupriya Goswami,E Mestre Guillen,E Wilhelmi,Iurii Sushch
Journal
arXiv preprint arXiv:2310.14431
Published Date
2023/10/22
The supernova remnant (SNR) G288.8-6.3 was recently discovered as a faint radio shell at large Galactic latitude using observations with ASKAP in the EMU survey. Here, we make the first detailed investigation of the -ray emission from the G288.8-6.3 region, aiming to characterise the high-energy emission in the GeV regime from the newly discovered SNR, dubbed Ancora. 15 years of Fermi-Large Area Telescope (LAT) data were analysed at energies between 400 MeV and 1 TeV and the excess seen in the region was modelled using different spatial and spectral models. We detect spatially extended -ray emission coinciding with the radio SNR, with detection significance up to 8.8 . A radial disk spatial model in combination with a power-law spectral model with an energy flux of , with the spectrum extending up to around 5 GeV was found to be the preferred model. Morphologically, hotspots seen above 1 GeV are well-correlated with the bright western part of the radio shell. The emission is more likely to be of leptonic origin given the estimated gas density in the region and the estimated distance and age of the SNR, but a hadronic scenario cannot be ruled out. Ancora is the eighth SNR detected at high Galactic latitude with Fermi-LAT. This new population of remnants has the potential to constrain the physics of particle diffusion and escape from SNRs into the Galaxy.
Pranjupriya Goswami FAQs
What is Pranjupriya Goswami's h-index at Tezpur University?
The h-index of Pranjupriya Goswami has been 7 since 2020 and 7 in total.
What are Pranjupriya Goswami's top articles?
The articles with the titles of
Searches for neutrino counterparts of gravitational waves from the LIGO/Virgo third observing run with KM3NeT
The variety of extreme blazars in the AstroSat view
Search for Neutrino Emission from GRB 221009A using the KM3NeT ARCA and ORCA detectors
TeV flaring activity of the AGN PKS 0625-354 in November 2018
Unveiling extended gamma-ray emission around HESS J1813-178
Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and HESS analysis
Astronomy potential of KM3NeT/ARCA
Atmospheric muons measured with the KM3NeT detectors in comparison with updated numeric predictions
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are the top articles of Pranjupriya Goswami at Tezpur University.
What are Pranjupriya Goswami's research interests?
The research interests of Pranjupriya Goswami are: High Energy Astrophysics, Astrophysical Blazars, Neutrino Physics, Machine Learning
What is Pranjupriya Goswami's total number of citations?
Pranjupriya Goswami has 92 citations in total.
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