BEGIN:VCALENDAR PRODID:-//Microsoft Corporation//Outlook 16.0 MIMEDIR//EN VERSION:2.0 METHOD:REQUEST X-MS-OLK-FORCEINSPECTOROPEN:TRUE BEGIN:VTIMEZONE TZID:W. Europe Standard Time BEGIN:STANDARD DTSTART:16011028T030000 RRULE:FREQ=YEARLY;BYDAY=-1SU;BYMONTH=10 TZOFFSETFROM:+0200 TZOFFSETTO:+0100 END:STANDARD BEGIN:DAYLIGHT DTSTART:16010325T020000 RRULE:FREQ=YEARLY;BYDAY=-1SU;BYMONTH=3 TZOFFSETFROM:+0100 TZOFFSETTO:+0200 END:DAYLIGHT END:VTIMEZONE BEGIN:VEVENT CLASS:PUBLIC CREATED:20241011T121459Z DESCRIPTION:Monday\, October 22\n \nSession 5: Survey from Gamma-ray to sof t X-rays\n \nConvenor: Angela Bazzano (INAF\, IAPS\, Rome)\n \n14:30 Roman Krivonos ……………………………………………………… …………………………………………..INTEGRAL: 20 years of ha rd X-ray surveys and background measurements\nSpace Research Institute (IK I)\, Moscow (Presented remotely)\n \nThe INTEGRAL hard X-ray surveys have proven to be of fundamental importance. In more than twenty years of opera tion\, the INTEGRAL observatory has given us a sharper view of the hard X- ray sky\, and provided the triggers for many follow-up campaigns from radi o frequencies to gamma-rays. In addition to conducting a census of hard X- ray sources across the entire sky\, INTEGRAL has carried out unique observ ations of the Galactic X-ray background\, which will without question be i ncluded in the annals of X-ray astronomy as one of the mission’s most sa lient contribution to our understanding of the hard X-ray sky. In my talk I will review the INTEGRAL all-sky surveys\, including our recent work bas ed on 17 years of operation. Also\, I will present our current study of th e large scale morphology and spectral properties of the Galactic hard X-ra y and soft gamma-ray background emission from 25 to 200 keV.\n \n15:00 And rea Merloni……………………………………………………… ……………………………………………………….. SRG/eROS ITA: highlights from the all-sky survey first data release\nMPE\, Garching \n \nWide-area\, sensitive X-ray surveys map the hot and energetic Univers e to reveal key processes across many areas of astrophysics and Cosmology\ , including the most massive collapsed structures of the Universe (cluster s and groups of galaxies)\, the hot ISM and CGM of the Milky Way and the S upernova remnants that energise it\, the atmospheres of neutron stars\, th e magnetic coronae of accretion discs around black holes\, and many more. eROSITA (extended Roentgen Survey with an Imaging Telescope Array)\, the s oft X-ray instrument on the Russian-German Spektrum-Roentgen-Gamma (SRG) m ission is expanding the horizon of X-ray astronomy and delivering large le gacy samples thanks to its high sensitivity\, large field of view\, high s patial resolution and survey efficiency. I will present an overview of the instrument capabilities\, the current status of the mission\, and a few s cience results from the survey program selected from the first data releas e.\n \n15:30 Dominik Patryk……………………………………… ………………………….. Pacholski INTEGRAL observations of Galact ic magnetars and search for extragalactic giant flares\nINAF\, IASF\, Mila no\n \nINTEGRAL has extensively observed the Galactic plane\, where most m agnetars are located\, providing an excellent opportunity to study their h ard X-ray emission over the entire mission period. Using archival data fro m the INTEGRAL IBIS instrument\, we conducted a comprehensive analysis of both persistent hard X-ray emission and short bursts. This large dataset a llowed us to explore the variability and characteristics of the emission t hroughout the INTEGRAL mission. Additionally\, since the high luminosity o f magnetar giant flares (MGFs) makes them detectable at extragalactic dist ances\, we used archival data from observations of the Virgo Cluster and a small sample of nearby star-forming galaxies to search for MGFs. We prese nt in addition to the results of the study of Galactic magnetars\, the res ults of the search for extragalactic MGF and the resulting lower and upper limits on their occurrence rate.\n \n15:45 Dhruv Bal………………… ……………………………………………………………… …………………………………………………………..Spectr opolarimetric study of INTEGRAL-IBIS GRBs\nClemson University\, Clemson\, South Carolina\n \nGamma-ray bursts (GRBs) are among the most energetic ev ents in the Universe\, but their radiation mechanisms\, jet structure\, an d composition remain unclear. Polarization measurements have the potential to provide insights into the jet’s structure and magnetic field orienta tion. When combined with spectral analysis\, polarization measurements can help probe jet composition. However\, only a few polarized GRBs have been detected\, limiting our understanding and refraining us from arriving at concrete conclusions. INTEGRAL\, one of the few instruments capable of det ecting polarized GRBs\, has reported three detections so far. Using the IB IS polarization pipeline and the INTEGRAL-IBIS archival data\, we aim to i ncrease this number\, and I will present the spectropolarimetric analysis results at the INTEGRAL meeting.\n \nSession 6: Supernovae\, Cosmic Rays a nd Magnetars\n \nConvenor: Philippe Laurent (CEA/DRF/IRFU/DAp\, Saclay)\n \n16:30 Jordi Isern ……………………………………………… ……………………………………………………………… ………………………………………Gamma emission from Type Ia S upernova\nCSIC\, ICE\, Barcelona\n \nFor a long time\, it was assumed that the light curve of Type Ia supernovae (SNIa) was mainly powered by the ra dioactive disintegration of the 56Ni chain. The detection and measurement by INTEGRAL of the gamma-rays emitted by SN 2014J provided the first direc t proof that this hypothesis was correct and that the total amount of 56Ni synthesized was in agreement with the values predicted by light curve mod els. Because of the existence of many SNIa subtypes it is clear at present that the thermonuclear explosion of a white dwarf can occur in multiple s cenarios leading to light curves that depend not only on the total amount of 56Ni synthesized but also on its distribution within the debris and\, c onsequently\, on the line of sight as it can be seen in few examples. For instance\, the early gamma emission detected in SN2014J could be an exampl e of such effects. This fact emphasizes the convenience of an instrument a ble to detect the early emission of a significant number of SNIa events.\n \n17:00 Sandro Mereghetti ……………………………………… ……………………………………………………………… …………………………………………… INTEGRAL catching magn etar flares\nINAF\, IASF\, Milano\n \nMagnetars\, isolated neutron stars p owered mainly by magnetic energy\, are characterised by a remarkable varia bility in the X-ray/gamma-ray bands. They show a variety of phenomena span ning a broad interval in dynamic range and duration\, from short bursts of a few milliseconds to outbursts lasting several months or even years. Amo ng these\, the giant flares\, releasing up to 1047 erg in gamma-rays in le ss than one second\, are the most spectacular events and can be observed a lso from sources at distances of several megaparsecs. The unpredictable oc currence of magnetar flares complicates their accurate study\, but\, thank s to the large sky coverage and good imaging\, timing and spectroscopic ca pabilities of its instruments\, INTEGRAL has given several significant con tributions in this field. In this invited talk I will review the main resu lts on bursts and flares from galactic and extragalactic magnetars obtaine d in more than two decades of observations with INTEGRAL.\n \n17:30 Tomota ka Nishikawa……………………….. Observational prediction of gamm a-ray emission from knee-energy cosmic rays accelerated by core[1]collapse supernovae\nGraduate School of Science\, Nagoya University\, Nagoya\n \nG alactic cosmic rays are believed to be accelerated through diffusive shock acceleration (DSA) within supernova remnants (SNRs). Recent observations of SNRs aged around 100–1000 years indicate that cosmic rays do not reac h PeV energies. However\, Inoue et al. (2021) demonstrated via kinetic-MHD simulations that cosmic rays can reach up to ∼3 PeV when a blast wave s hock propagates through a dense circumstellar medium (CSM) within tens of days after the explosion. This dense CSM is assumed to be produced by a re d supergiant (RSG) wind with a mass-loss-rate of 10−3 M⊙yr−1 \, supp orted by recent supernova observations. Observing 100 TeV gamma-rays\, pro duced by PeV cosmic rays through neutral pion decay\, can confirm PeV acce lerations. However\, these gamma-rays from young SNRs are often attenuated by interactions with photons from the supernova photosphere and cosmic ba ckground radiation. Previous studies suggested it is difficult to detect t hese gamma-rays with a conventional RSG wind (∼10−5 M⊙yr−1 ). Usin g Inoue et al. (2021) kinetic-MHD simulation data\, we calculate the gamma -ray flux from a blast wave in a dense CSM\, considering environmental att enuation. We find a significantly higher gamma-ray flux than previous stud ies if we assume a modern mass-loss rate wind (∼10−3 M⊙yr−1 ). We predict that the CTA can detect 100 TeV gamma-rays with 1.3 hours of integ ration if a type II SN occurs within 5.2 Mpc. Based on observed star forma tion rates\, such an event is expected once every 6 years.\n \n17:45 Guill aume Belanger…………………………………………………… ……………………………………………………………… …………………………………………. .Using OSA in ESA Datala bs\nESA\, ESAC\, Madrid\n \n-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-~-\ n-- Do not delete or change any of the following text. -- \n \nWhen it's t ime\, join your Webex meeting here. \n \n \nMeeting number (access code): 2373 940 6614\nMeeting password: KkPwUyK8k44 \n \n \nJoin meeting \n \n Tap to join from a mobile device (attendees only) \n+44-20-3478-5289\,\, 23739406614## Unite d Kingdom Toll \n\nJoin by phone \n+44-20-3478-5289 United Kingdom Toll \nGlobal call-in numbers \n \nJoin from a video system or application\nDial 23739406614@esait.webex.com \nYou can also dial 62.109.219.4 and enter your meeting number. \ n \n \nIf you are a host\, click here and login site t o view host information. \n \n \nNeed help? Go to http://help.webex.com \n \n \n \n DTEND;TZID="W. Europe Standard Time":20241022T180000 DTSTAMP:20241011T121459Z DTSTART;TZID="W. Europe Standard Time":20241022T143000 LAST-MODIFIED:20241011T121459Z LOCATION:Rooms D1/D2 ORGANIZER;CN="Juan Pablo Vega Gonzalez":mailto:Juan.Pablo.Vega.Gonzalez@ext .esa.int PRIORITY:5 SEQUENCE:0 SUMMARY;LANGUAGE=en-gb:INTEGRAL Workshop 2024 – Day 2 – Tue Oct 22 PM – Sessions 5-6 TRANSP:OPAQUE UID:040000008200E00074C5B7101A82E00800000000D0E2FE7CD31BDB01000000000000000 01000000003F3C0F706205B419CDA23111CE0D6BF X-ALT-DESC;FMTTYPE=text/html:

Monday\, October 22

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Session 5: Surv ey from Gamma-ray to soft X-rays

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Convenor: Angela Bazzano (INAF\, IAPS\, Rome)

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14:30 Roman Krivono s ……………………………………………………… …………………………………………..INTEGRAL: 20 years of ha rd X-ray surveys and background measurements

Space Research Institute (IKI)\, Moscow (Presented r emotely)

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< p class=MsoNormal style='margin-left:36.0pt\;text-align:justify'>The INTEGRAL hard X-ray surveys have proven to be of fundamental importance. In more than twenty years of operation\, the INTE GRAL observatory has given us a sharper view of the hard X-ray sky\, and provided the triggers for many follow-up campaigns from radio frequencies to gamma-rays. In addition to conducting a census of hard X-ray sources across the entire sky\, INTEGRAL has carried out uni que observations of the Galactic X-ray background\, which will without que stion be included in the annals of X-ray astronomy as one of the mission ’s most salient contribution to our understanding of the hard X-ray sky. In my talk I will review the INTEGRAL all-sky surveys\, including our rec ent work based on 17 years of operation. Also\, I will present our current study of the large scale morphology and spectral properties of the Galactic hard X-ray and soft gamma-ray background emiss ion from 25 to 200 keV.

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15:00 Andrea Merloni………………………………… ……………………………………………………………… …………….. SRG/eROSITA: highlights from t he all-sky survey first data release

MPE\, Garching

 \;

Wide-area\, sensitive X-ray surveys map the hot and energeti c Universe to reveal key processes across many areas of astrophysics and C osmology\, including the most massive collapsed structures of the Universe (clusters and groups of galaxies)\, the hot ISM and CGM of the Milky Way and the Supernova remnants that energise it\, the atmospheres of neutron s tars\, the magnetic coronae of accretion discs around black holes\, and ma ny more. eROSITA (extended Roentgen Survey with an Imaging Telescope Array)\, the soft X-ray instrument on the Russian-Ger man Spektrum-Roentgen-Gamma (SRG) mission is expanding the horizon of X-ra y astronomy and delivering large legacy samples thanks to its high sensiti vity\, large field of view\, high spatial resolution and survey efficiency. I will present an overview of the instrument ca pabilities\, the current status of the mission\, and a few science results from the survey program selected from the first data release.

 \;

15:30 Domi nik Patryk……………………………………………………… ………….. Pacholski INTEGRAL observations of Galactic magnetars and s earch for extragalactic giant flares

INAF\, IASF\, Milano

 \;

INTEGR AL has extensively observed the Galactic plane\, where most magnetars are located\, providing an excellent opportunity to study their hard X-ray emi ssion over the entire mission period. Using archival data from the INTEGRA L IBIS instrument\, we conducted a comprehensive analysis of both persiste nt hard X-ray emission and short bursts. This large dataset allowed us to explore the variability and characteristics of the emission throughout the INTEGRAL mission. Additionally\, since the high luminosity of magnetar gi ant flares (MGFs) makes them detectable at extragalactic distances\, we us ed archival data from observations of the Virgo Cluster and a small sample of nearby star-forming galaxies to search for MGFs. We present in additio n to the results of the study of Galactic magnetars\, the results of the s earch for extragalactic MGF and the resulting lower and upper limits on th eir occurrence rate.

&nbs p\;

15:45 Dhruv Bal…………………………………………………… ……………………………………………………………… ………………………..Spectropolarimetric study of INTEGRAL-IBIS GR Bs

Clemson University\, Clemson\, South Carolina

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Gamma-ray burst s (GRBs) are among the most energetic events in the Universe\, but their r adiation mechanisms\, jet structure\, and composition remain unclear. Pola rization measurements have the potential to provide insights into the jet ’s structure and magnetic field orientation. When combined with spectral analysis\, polarization measurements can help probe jet composition. Howe ver\, only a few polarized GRBs have been detected\, limiting our understanding and refraining us from arriving at concrete conclusions. INTEGRAL\, one of the few instruments capable of detecting p olarized GRBs\, has reported three detections so far. Using the IBIS polar ization pipeline and the INTEGRAL-IBIS archival data\, we aim to increase this number\, and I will present the spectropolarimetri c analysis results at the INTEGRAL meeting.

 \;

Session 6: Superno vae\, Cosmic Rays and Magnetars

 \ ;

Convenor: Philippe Laurent (CEA/DRF/IRFU/DAp\, Saclay)

 \;

16:30 Jordi Isern …………… ……………………………………………………………… ……………………………………………………………… …………Gamma emission from Type Ia Supernov a

CSIC\, ICE\, Barcelon a

 \;

For a long time\, it was assumed that t he light curve of Type Ia supernovae (SNIa) was mainly powered by the radioactive disintegration of the 56Ni chain. The detection and measurement by INTEGRAL of the gamma -rays emitted by SN 2014J provided the first direct proof that this hypoth esis was correct and that the total amount of 56Ni synthesized was in agreement with the values predicted by light curve mo dels. Because of the existence of many SNIa subt ypes it is clear at present that the thermonuclear explosion of a white dw arf can occur in multiple scenarios leading to light curves that depend no t only on the total amount of 56Ni synthesized but also on its distributio n within the debris and\, consequently\, on the line of sight as it can be seen in few examples. For instance\, the early gamma emission detected in SN2014J could be an example of such effects. This fact emphasizes the con venience of an instrument able to detect the early emission of a significa nt number of SNIa events.

< p class=MsoNormal style='margin-left:36.0pt\;text-align:justify'> \;

17:00 Sandro Mereghetti …………… ……………………………………………………………… ……………………………………………………………… ……… INTEGRAL catching magnetar flares

INAF\, IASF\, Milano

 \;

Magnetars\, isolated neutron stars powered mainly by magnetic energy\, ar e characterised by a remarkable variability in the X-ray/gamma-ray bands. They show a variety of phenomena spanning a broad interval in dynamic rang e and duration\, from short bursts of a few milliseconds to outbursts last ing several months or even years. Among these\, the giant flares\, releasi ng up to 1047 erg in gamma-rays in less than one second\, are the most spe ctacular events and can be observed also from sources at distances of seve ral megaparsecs. The unpredictable occurrence of magnetar flares complicat es their accurate study\, but\, thanks to the large sky coverage and good imaging\, timing and spectroscopic capabilities of its instruments\, INTEG RAL has given several significant contributions in this field. In this inv ited talk I will review the main results on bursts and flares from galacti c and extragalactic magnetars obtained in more than two decades of observa tions with INTEGRAL.

& nbsp\;

< b>17:30 Tomotaka Nishikawa……………………….. Observational predi ction of gamma-ray emission from knee-energy cosmic rays accelerated by co re[1]collapse supernovae< /span>

Graduate School of Science\, Nagoy a University\, Nagoya

< o:p> \;

Galactic cosmic ray s are believed to be accelerated through diffusive shock acceleration (DSA ) within supernova remnants (SNRs). Recent observations of SNRs aged aroun d 100–1000 years indicate that cosmic rays do not reach PeV energies. However\, Inoue et al. (2021) demonstrated via kin etic-MHD simulations that cosmic rays can reach up to ∼3 PeV when a blast wave shock propagates through a dense circumst ellar medium (CSM) within tens of days after the explosion. This dense CSM is assumed to be produced by a red supergiant (RSG) wind with a mass-loss -rate of 10−3 M⊙yr−1 \, supported by r ecent supernova observations. Observing 100 TeV gamma-rays\, produced by < span class=SpellE>PeV cosmic rays through neutral pion decay\, can confirm PeV accelerations. However\, these gamma -rays from young SNRs are often attenuated by interactions with photons fr om the supernova photosphere and cosmic background radiation. Previous stu dies suggested it is difficult to detect these gamma-rays with a conventio nal RSG wind (∼10−5 M⊙yr−1 ). Using Inoue et al. (2021) kinetic-MHD simulation d ata\, we calculate the gamma-ray flux from a blast wave in a dense CSM\, c onsidering environmental attenuation. We find a significantly higher gamma -ray flux than previous studies if we assume a modern mass-loss rate wind (∼10 −3 M⊙yr−1 ). We predict that the CTA can detect 100 TeV gamma-rays with 1. 3 hours of integration if a type II SN occurs within 5.2 Mpc. Based on observed star formation rates\, such an event is ex pected once every 6 years.

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17:45 Guillaume Belanger……… ……………………………………………………………… ……………………………………………………………… ………………………. .Using OSA in ESA Datalabs

ESA\, ES AC\, Madrid

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