Dominik Patryk Pacholski

University of Milano-Bicocca

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S. Mereghetti

National Institute for Astrophysics

R. Salvaterra

Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano

A. Tiengo

Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano

Edoardo Arrigoni

University of Milano-Bicocca

A. Bazzano

Institute for Space Astrophysics and Planetology

P. Ubertini

Institute for Space Astrophysics and Planetology

D. Götz

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

Michela Rigoselli

Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano

L. Ducci

University of Geneva

S. Campana

Brera Astronomical Observatory

Cooperative Institutions

National Institute for Astrophysics

Centre National de la Recherche Scientifique

Brera Astronomical Observatory

Institut d'Estudis Espacials de Catalunya

Institute for Space Astrophysics and Planetology

University of Geneva

Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano

Institute of Space Sciences

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

University of Amsterdam

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A magnetar giant flare in the nearby starburst galaxy M82

Nature (2024)

S. Mereghetti Michela Rigoselli R. Salvaterra Dominik Patryk Pacholski J. Rodi

Magnetar

Flare

Large Magellanic Cloud

10.1038/s41586-024-07285-4

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Citations (12)

XMM-Newton and INTEGRAL observations of the bright GRB 230307A : vanishing of the local absorption and limits on the dust in the Magellanic Bridge

arXiv (Cornell University) (2023)

S. Mereghetti Michela Rigoselli R. Salvaterra A. Tiengo Dominik Patryk Pacholski

230307A is the second brightest gamma ray burst detected in more than 50 years of observations and is located in the direction of the Magellanic Bridge. Despite its long duration, it is most likely the result of the compact merger of a binary ejected from a galaxy in the local universe (redshift z=0.065). Our XMM-Newton observation of its afterglow at 4.5 days shows a power-law spectrum with photon index $\Gamma =1.73 \pm0.10$, unabsorbed flux $F_{0.3-10\,\rm keV}=(8.8\pm0.5)\times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$ and no absorption in excess of that produced in our Galaxy and in the Magellanic Bridge. We derive a limit of $N_{\rm H}^{\rm HOST} < 5\times 10^{20}$ cm$^{-2}$ on the absorption at the GRB redshift, which is a factor $\sim\,$5 below the value measured during the prompt phase. We searched for the presence of dust scattering rings with negative results and set an upper limit of the order of $A_V<0.05$ on the absorption from dust in the Magellanic Bridge.

Large Magellanic Cloud

Extinction (optical mineralogy)

10.48550/arxiv.2307.13514

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Citations (0)

An X-Ray and Radio View of the 2022 Reactivation of the Magnetar SGR J1935+2154

The Astrophysical Journal (2024)

A. Y. Ibrahim A. Borghese F. Coti Zelati E. Parent A. Marino

Abstract Recently, the Galactic magnetar SGR J1935+2154 has garnered attention due to its emission of an extremely luminous radio burst, reminiscent of fast radio bursts (FRBs). SGR J1935+2154 is one of the most active magnetars, displaying flaring events nearly every year, including outbursts as well as short and intermediate bursts. Here, we present our results on the properties of the persistent and bursting X-ray emission from SGR J1935+2154 during the initial weeks following its outburst on 2022 October 10. The source was observed with XMM-Newton and NuSTAR (quasi-)simultaneously during two epochs, separated by ∼5 days. The persistent emission spectrum is well described by an absorbed blackbody plus power-law model up to an energy of ∼25 keV. No significant changes were observed in the blackbody temperature ( kT BB ∼ 0.4 keV) and emitting radius ( R BB ∼ 1.9 km) between the two epochs. However, we observed a slight variation in the power-law parameters. Moreover, we detected X-ray pulsations in all the data sets and derived a spin-period derivative of P ̇ = 5.52 ( 5 ) × 10 − 11 s s −1 . This is 3.8 times larger than the value measured after the first recorded outburst in 2014. Additionally, we performed quasi-simultaneous radio observations using three 25–32 m class radio telescopes for a total of 92.5 hr to search for FRB-like radio bursts and pulsed emission. However, our analysis did not reveal any radio bursts or periodic emission.

Magnetar

10.3847/1538-4357/ad293b

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Citations (4)

INTEGRAL search for magnetar giant flares from the Virgo Cluster and in nearby galaxies with high star formation rate

arXiv (Cornell University) (2024)

Dominik Patryk Pacholski Edoardo Arrigoni S. Mereghetti R. Salvaterra

Giant flares from magnetars can reach, for a fraction of a second, luminosities greater than 10$^{47}$ erg s$^{-1}$ in the hard X-ray/soft $\gamma$-ray range. This makes them visible at distances of several megaparsecs. However, at extragalactic distances (farther than the Magellanic Clouds) they are difficult to distinguish from the short $\gamma$-ray bursts, which occur much more frequently. Since magnetars are young neutron stars, nearby galaxies with a high rate of star formation are optimal targets to search for magnetar giant flares (MGFs). Here we report the results of a search for MGFs in observations of the Virgo cluster and in a small sample of nearby galaxies obtained with the IBIS instrument on the INTEGRAL satellite. From the currently known MGF sample we find that their energy distribution is well described by a power law with slope $\gamma$=2 (with 90% c.l. interval [1.7-2.2]). From the lack of detections in this extensive data set (besides 231115A in M82) we derive a 90% c.l. upper limit on the rate of MGF with $E>3\times10^{45}$ erg of $\sim2\times10^{-3}$ yr$^{-1}$ per magnetar and a lower limit of $R(E)>\sim4\times10^{-4}$ yr$^{-1}$ magnetar$^{-1}$ for $E<10^{45}$ erg.

Magnetar

Virgo Cluster

Star (game theory)

10.48550/arxiv.2411.03235

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Citations (0)

An X-ray and radio view of the 2022 reactivation of the magnetar SGRJ1935+2154

arXiv (Cornell University) (2024)

Ahmad Ibrahim A. Borghese F. Coti Zelati E. Parent A. Marino

Recently, the Galactic magnetar SGR J1935+2154 has garnered attention due to its emission of an extremely luminous radio burst, reminiscent of Fast Radio Bursts (FRBs). SGR J1935+2154 is one of the most active magnetars, displaying flaring events nearly every year, including outbursts as well as short and intermediate bursts. Here, we present our results on the properties of the persistent and bursting X-ray emission from SGR J1935+2154, during the initial weeks following its outburst on October 10, 2022. The source was observed with XMM-Newton and NuSTAR (quasi-)simultaneously during two epochs, separated by $\sim$5 days. The persistent emission spectrum is well described by an absorbed blackbody plus power-law model up to an energy of $\sim$25 keV. No significant changes were observed in the blackbody temperature ($kT_{\rm BB}\sim$ 0.4 keV) and emitting radius ($R_{\rm BB}\sim$ 1.9 km) between the two epochs. However, we observed a slight variation in the power-law parameters. Moreover, we detected X-ray pulsations in all the datasets and derived a spin period derivative of $\dot{P} = 5.52(5) \times 10^{-11}$ ss. This is 3.8 times larger than the value measured after the first recorded outburst in 2014. Additionally, we performed quasi-simultaneous radio observations using three 25--32-m class radio telescopes for a total of 92.5 hr to search for FRB-like radio bursts and pulsed emission. However, our analysis did not reveal any radio bursts or periodic emission.

Magnetar

10.48550/arxiv.2402.08596

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Citations (0)

A magnetar giant flare in the nearby starburst galaxy M82

arXiv (Cornell University) (2023)

S. Mereghetti Michela Rigoselli R. Salvaterra Dominik Patryk Pacholski J. Rodi

Giant flares, short explosive events releasing up to 10$^{47}$ erg of energy in the gamma-ray band in less than one second, are the most spectacular manifestation of magnetars, young neutron stars powered by a very strong magnetic field, 10$^{14-15}$ G in the magnetosphere and possibly higher in the star interior. The rate of occurrence of these rare flares is poorly constrained, as only three have been seen from three different magnetars in the Milky Way and in the Large Magellanic Cloud in about 50 years since the beginning of gamma-ray astronomy. This sample can be enlarged by the discovery of extragalactic events, since for a fraction of a second giant flares reach peak luminosities above 10$^{46}$ erg/s, which makes them visible by current instruments up to a few tens of Mpc. However, at these distances they appear similar to, and difficult to distinguish from, regular short gamma-ray bursts (GRBs). The latter are much more energetic events, 10$^{50-53}$ erg, produced by compact binary mergers and originating at much larger distances. Indeed, only a few short GRBs have been proposed, with different levels of confidence, as magnetar giant flare candidates in nearby galaxies. Here we report the discovery of a short GRB positionally coincident with the central region of the starburst galaxy M82. Its spectral and timing properties, together with the limits on its X-ray and optical counterparts obtained a few hours after the event and the lack of an associated gravitational wave signal, qualify with high confidence this event as a giant flare from a magnetar in M82.

Magnetar

Flare

Large Magellanic Cloud

10.48550/arxiv.2312.14645

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Citations (1)

GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?

The Astrophysical Journal Letters (2025)

J. Rodi Dominik Patryk Pacholski S. Mereghetti Edoardo Arrigoni A. Bazzano

Abstract We report the results on the short gamma-ray burst GRB 241107A, obtained with the IBIS instrument on board the INTEGRAL satellite. The burst had a duration of about 0.2 s, a fluence of 8 × 10 −7 erg cm −2 in the 20 keV–10 MeV range, and a hard spectrum, characterized by a peak energy of 680 keV. The position of GRB 241107A has been precisely determined because it fell inside the imaging field of view of the IBIS coded mask instrument. The presence of the nearby galaxy PGC 86046 in the 3′ radius error region suggests that GRB 241107A might be a giant flare from a magnetar rather than a canonical short gamma-ray burst. For the 4.1 Mpc distance of PGC 86046, the isotropic energy of 1.6 × 10 45 erg is in agreement with this hypothesis, which is also supported by the time-resolved spectral properties similar to those of the few other extragalactic magnetars giant flares detected so far.

Magnetar

Flare

10.3847/2041-8213/ada6b7

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Citations (0)

INTEGRAL observations of magnetars

arXiv (Cornell University) (2024)

Dominik Patryk Pacholski L. Ducci M. Topinka S. Mereghetti

The INTEGRAL satellite has collected a large amount of data on magnetars in our Galaxy, spanning more than 20 years starting from 2003. The large data set obtained with the IBIS/ISGRI instrument at energies above 20 keV allows us to study both the properties and long-term evolution of their persistent hard X-ray emission and the population characteristics of the short bursts emitted during active periods. We are carrying out a comprehensive analysis of the observed magnetars, exploiting the most recent calibrations and analysis software. Here we report on the long term evolution of the hard X-ray flux of the magnetars detected with ISGRI and the results of a sensitive search for short bursts in SGR J1935+2154.

Magnetar

10.48550/arxiv.2410.23484

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Citations (0)

GRB241107A: a Giant Flare from a close-by extragalactic Magnetar?

arXiv (Cornell University) (2024)

J. Rodi Dominik Patryk Pacholski S. Mereghetti Edoardo Arrigoni A. Bazzano

We report the results on the short gamma-ray burst GRB 241107A, obtained with the IBIS instrument on board the INTEGRAL satellite. The burst had a duration of about 0.2 s, a fluence of $8 \times 10^{-7}$ erg cm-2 in the 20 keV-10 MeV range and a hard spectrum, characterized by a peak energy of 680 keV. The position of GRB 241107A has been precisely determined because it fell inside the imaging field of view of the IBIS coded mask instrument. The presence of the nearby galaxy PGC 86046 in the 3 arcmin radius error region, suggests that GRB 241107A might be a giant flare from a magnetar rather than a canonical short GRB. For the 4.1 Mpc distance of PGC 86046, the isotropic energy of $1.6 \times 10^{45}$ erg is in agreement with this hypothesis, that is also supported by the time resolved spectral properties similar to those of the few other extragalactic magnetars giant flares detected so far.

Magnetar

Flare

10.48550/arxiv.2412.06668

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Citations (0)

INTEGRAL Observations of Magnetars

Astronomische Nachrichten (2024)

Dominik Patryk Pacholski L. Ducci M. Topinka S. Mereghetti

ABSTRACT The INTEGRAL satellite has collected a large amount of data on magnetars in our Galaxy, spanning more than 20 years starting from 2003. The large data set obtained with the IBIS/ISGRI instrument at energies above 20 keV allows us to study both the properties and long‐term evolution of their persistent hard X‐ray emission and the population characteristics of the short bursts emitted during active periods. We are carrying out a comprehensive analysis of the observed magnetars, exploiting the most recent calibrations and analysis software. Here we report on the long term evolution of the hard X‐ray flux of the magnetars detected with ISGRI and the results of a sensitive search for short bursts in SGR J1935+2154.

Magnetar

Ibis

10.1002/asna.20240109

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