Observing peculiar γ-ray pulsars with AGILE

Pilia, M.; Burgay, M.; D’Amico, N.; Esposito, P.; Possenti, A.

doi:10.1063/1.3615123

Cited by 8 publications

(12 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In the context of a systematic monitoring of the high-energy activity of FRB 180916.J0158+65, our observations help constrain the rate of possible GFs with a unique broad-band sensitivity from 1 to 100 keV, with upper limits on the released energy of possible bursts of E 10 46 erg or even less for durations, ∆ t 0.1 s. Considering the different energy bands, these values are comparable with those obtained in the X-rays with Chandra and XMM-Newton (Scholz et al 2020;Pilia et al 2020) and they are significantly more sensitive than those obtained with all-sky monitors such as Fermi/GBM (Scholz et al 2020). Under the assumption that the frequency of radio bursts of FRB 180916.J0158+65 around peak is the same for all periods, our observations almost certainly cover one or more of them.…”

Section: Discussionsupporting

confidence: 78%

“…Although no radio burst has been reported to date during the Insight-HXMT observing window, it is worth estimating the probability that FRB 180916.J0158+65 gave no FRBs. Ignoring the complex dependence on frequency (CHIME/FRB Collaboration 2020b; Pilia et al 2020;Chawla et al 2020), here we focus on the homogeneous sample detected with CHIME. Considering the ±0.9 d interval centred on the peak of radio activity, which has a burst rate of 1.8 +1.3 −0.8 h −1 (CHIME/FRB Collaboration 2020b), the net exposure of Insight-HXMT is ∼8.5 h. The probability of no FRBs over the duration of the Insight-HXMT observation is 2 × 10 −4 at most.…”

Section: Detection Of Radio Bursts During Insight-hxmt Observationsmentioning

confidence: 99%

“…They also derived an upper limit of 6 × 10 46 erg in the 10−100 keV band for 12 bursts from FRB 180916.J0158+65 that were visible with Fermi/Gamma-ray Burst Monitor (GBM; Meegan et al 2009). The XMM-Newton detected no source down to E < 10 45 erg in the 0.3−10 keV energy band at the times of three radio bursts, which were discovered at 328 MHz with the Sardinia Radio Telescope (Pilia et al 2020). Comparable upper limits of 3 × 10 46 erg on the energy released in the optical band, simultaneous with FRBs, from FRB 180916.J0158+65 were also derived in a statistical framework using survey data from the Zwicky Transient Facility (Andreoni et al 2020).…”

Section: Introductionmentioning

confidence: 98%

See 2 more Smart Citations

Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight–HXMT follow-up observations

Guidorzi¹,

Orlandini²,

Frontera³

et al. 2020

A&A

View full text Add to dashboard Cite

Context. A link has finally been established between magnetars and fast radio burst (FRB) sources. Within this context, a major issue that remains unresolved pertains to whether sources of extragalactic FRBs exhibit X/γ-ray outbursts and whether this is correlated with radio activity. If so, the subsequent goal is to identify these sources. Aims. We aim to constrain possible X/γ-ray burst activity from one of the nearest extragalactic FRB sources currently known. This is to be done over a broad energy range by looking for bursts over a range of timescales and energies that are compatible with those of powerful flares from extragalactic magnetars. Methods. We followed up on the observation of the as-yet nearest extragalactic FRB source, located at a mere 149 Mpc distance, namely, the periodic repeater FRB 180916.J0158+65. This took place during the active phase between 4 and 7 February 2020, using the Insight–Hard X-ray Modulation Telescope (Insight–HXMT). By taking advantage of the combination of broad-band wavelengths, a large effective area, and several independent detectors at our disposal, we searched for bursts over a set of timescales from 1 ms to 1.024 s with a sensitive algorithm that had been previously characterised and optimised. Moreover, through simulations, we studied the sensitivity of our technique in the released energy-duration phase space for a set of synthetic flares and assuming a range of different energy spectra. Results. We constrain the possible occurrence of flares in the 1−100 keV energy band to E < 1046 erg for durations Δ t < 0.1 s over several tens of ks exposure. Conclusions. We can rule out the occurrence of giant flares similar to the ones that were observed in the few cases of Galactic magnetars. The absence of reported radio activity during our observations prevents us from making any determinations regarding the possibility of simultaneous high-energy emission.

show abstract

Section: Discussionsupporting

confidence: 78%

Section: Detection Of Radio Bursts During Insight-hxmt Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

See 1 more Smart Citation

Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight–HXMT follow-up observations

Guidorzi¹,

Orlandini²,

Frontera³

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…In addition, we assume a homogeneous population of FRB sources, which may not be the case, and it is also possible that some (e.g., soft X-ray, or blue optical) FRB counterparts are absorbed or scattered in dense surrounding media. Multiwavelength observations of nearby individual sources (e.g., Casentini et al 2020;Pilia et al 2020;Tavani et al 2020) are a complementary means to address the nature of the FRB engine and emission mechanism.…”

Section: Discussionmentioning

confidence: 99%

The Multiwavelength Counterparts of Fast Radio Bursts

Chen

Ravi

2020

ApJ

View full text Add to dashboard Cite

The engines that produce extragalactic fast radio bursts (FRBs), and the mechanism by which the emission is generated, remain unknown. Many FRB models predict prompt multiwavelength counterparts, which can be used to refine our knowledge of these fundamentals of the FRB phenomenon. However, several previous targeted searches for prompt FRB counterparts have yielded no detections and have additionally not reached sufficient sensitivity with respect to the predictions. In this work, we demonstrate a technique to estimate the ratio, η, between the energy outputs of FRB counterparts at various wavelengths and the radio-wavelength emission. Our technique combines the fluence distribution of the FRB population with results from several wide-field blind surveys for fast transients from the optical to the TeV bands. We present constraints on η that improve upon previous observations even in the case where all unclassified transient events in existing surveys are FRB counterparts. In some scenarios for the FRB engine and emission mechanism, we find that FRB counterparts should have already been detected, thus demonstrating that our technique can successfully test predictions for η. However, it is possible that FRB counterparts are lurking among catalogs of unclassified transient events. Although our technique is robust to the present uncertainty in the FRB fluence distribution, its ultimate application to accurately estimate or bound η will require the careful analysis of all candidate fast transient events in multiwavelength survey data sets.

show abstract

“…PSR B1509 is unique among the known γ -ray spin-down powered pulsars for its very soft γ -ray spectrum and a very strong surface magnetic field. It is suggested that there may be a new class of spin-down powered pulsar with high magnetic field (>10 13 G) and soft γ -ray radiation, called soft γ -ray pulsar (Pilia & Pellizzoni 2011). Also, there is at least another pulsar that is similar to PSR B1509, PSR J1846−0258, a young pulsar with P ∼ 324 ms and surface magnetic field B s ∼ 4.9 × 10 13 G, which cannot be detected by Fermi but is seen by X-ray telescopes (Kuiper & Hermsen 2009;Parent et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Mechanism of the X-Ray and Soft Gamma-Ray Emissions From High Magnetic Field Pulsar: PSR B1509–58

Wang

Takata

Cheng

2013

ApJ

View full text Add to dashboard Cite

We use the outer gap model to explain the spectrum and the energy-dependent light curves of the X-ray and soft γ -ray radiations of the spin-down powered pulsar PSR B1509-58. In the outer gap model, most pairs inside the gap are created around the null charge surface and the gap's electric field separates the two charges to move in opposite directions. Consequently, the region from the null charge surface to the light cylinder is dominated by the outflow current while that from the null charge surface to the star is dominated by the inflow current. We suggest that the viewing angle of PSR B1509−58 only receives the inflow radiation. The incoming curvature photons are converted to pairs by the strong magnetic field of the star. The X-rays and soft γ -rays of PSR B1509−58 result from the synchrotron radiation of these pairs. Magnetic pair creation requires a large pitch angle, which makes the pulse profile of the synchrotron radiation distinct from that of the curvature radiation. We carefully trace the pulse profiles of the synchrotron radiation with different pitch angles. We find that the differences between the light curves of different energy bands are due to the different pitch angles of the secondary pairs, and that the second peak appearing at E > 10 MeV comes from the region near the star, where the stronger magnetic field allows pair creation to happen with a smaller pitch angle.

show abstract

Observing peculiar γ-ray pulsars with AGILE

Cited by 8 publications

References 25 publications

Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight–HXMT follow-up observations

Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight–HXMT follow-up observations

The Multiwavelength Counterparts of Fast Radio Bursts

Mechanism of the X-Ray and Soft Gamma-Ray Emissions From High Magnetic Field Pulsar: PSR B1509–58

Contact Info

Product

Resources

About