Erratum: Detection of a 
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-ray halo around Geminga with the Fermi-LAT data and implications for the positron flux [Phys. Rev. D 
<b>100</b>
, 123015 (2019)]

Mauro, Mattia Di; Manconi, Silvia; Donato, Fiorenza

doi:10.1103/physrevd.104.089903

Cited by 27 publications

(73 citation statements)

References 3 publications

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“…The High-Altitude Water Cherenkov Observatory (HAWC) recently reported discovery of spatially extended TeV sources surrounding two middle-aged (t age = 100 − 400 kyr) pulsars, namely, Geminga and Monogem (or PSR B0656+14) (Abey-sekara et al 2017, see also Abdo et al 2009). The intensity profile of the TeV sources can be explained with the inverse Compton (IC) scatterings of diffusing electrons, which are injected from the pulsars, on the cosmic microwave background (CMB) and the interstellar radiation field (ISRF) (Abeysekara et al 2017;López-Coto & Giacinti 2018;Tang & Piran 2019;Liu et al 2019a,b;Di Mauro et al 2019). The physical extension of the sources is at least 30 pc which is much larger than the size of the PWN of the corresponding pulsars, indicating that accelerated electrons escape the PWN and produce the halo-like emissions in the ambient ISM of the pulsars.…”

Section: Introductionmentioning

confidence: 99%

“…E. S. S. Collaboration et al 2018b). Although the offset may be explained with the proper motion of the pulsar (H. E. S. S. Collaboration et al 2018b;Di Mauro et al 2020), it is not straightforward to connect a γ-ray sources and the associated pulsar in the case of large offset being detected, especially without a knowledge on the pulsar's proper motion velocity. On the other hand, various factors such as continuous injection of electrons, cooling of electrons, and the limit of the angular resolution of instruments (i.e., the PSF), could smear out the offset, making the identification more complex.…”

Section: Introductionmentioning

confidence: 99%

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Morphology of Gamma-Ray Halos around Middle-Aged Pulsars: Influence of the Pulsar Proper Motion

Zhang,

Liu,

Chen

et al. 2020

Preprint

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Recently, γ-ray halos of a few degree extension have been detected around two middle-aged pulsars, Geminga and PSR B0656+14 by the High Altitude Water Cherenkov observatory (HAWC). The measurements of surface brightness profile of the pulsar halos suggest that the transport of particles therein is dominated by diffusion, and the diffusion coefficient is significantly lower than the average value in the Galactic disk. Since pulsars typically have a proper velocity of 400 − 500 km/s, the displacement of these middle-aged pulsars due to the proper motion could be important in shaping the morphology of the pulsar halos. Motivated by this, we study the morphology of pulsar halos considering proper motion in the diffusion-dominated scenario. We find that the morphology of the pulsar halo can be basically classified into three evolutionary phases, depending on the velocity of the proper motion, cooling of the emitting electrons and the age of the pulsar. Generally, the morphology would appear highly asymmetric at 1 TeV while keeps more or less spherical at 10 TeV for middle-aged pulsars. We also study the offset between the position of pulsars and the center of the intensity map of the corresponding halo. We find that proper motion can induce observable offsets seen by Fermi-LAT, HESS, HAWC and LHAASO from GeV up to a few TeV energies provided that the source is located within several kpc from Earth. It is more difficult to produce resolvable offset in the pulsar halo at higher energy due to more rapid cooling of emitting electrons. Our result can provide constraints on the origins of those extended sources at very high energies.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Morphology of Gamma-Ray Halos around Middle-Aged Pulsars: Influence of the Pulsar Proper Motion

Zhang,

Liu,

Chen

et al. 2020

Preprint

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“…5.3. The transitional PWN -TeV halo nature of HESS J1825−137The discovery of extended TeV emission around the Geminga pulsar(Abeysekara et al 2017a), whose properties are consistent with free particle propagation in the interstellar medium (ISM), suggests the presence of such halo phenomena in other sources(Abeysekara et al 2017b) as well as its presence also at GeV energies (DiMauro et al 2019).Following the approach of Giacinti et al (2020), we estimated the energy densities for the PWN HESS J1825−137, and compared it with the typical energy density of the ISM, ISM = 0.1 eV cm −3 , in order to determine to a first approximation whether the electrons that are responsible for the γ-ray emission occupy the relatively unperturbed ISM (TeV halo like, e ISM ), or if they are still contained in a region energetically and dynamically dominated by the pulsar (PWN like, e > ISM ).…”

mentioning

confidence: 99%

Energy dependent morphology of the pulsar wind nebula HESS J1825-137 with Fermi-LAT

Principe,

Mitchell,

Caroff

et al. 2020

Preprint

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Aims. Taking advantage of more than 11 years of Fermi-LAT data, we perform a new and deep analysis of the pulsar wind nebula (PWN) HESS J1825-137. Combining this analysis with recent H.E.S.S. results we investigate and constrain the particle transport mechanisms at work inside the source as well as the system evolution. Methods. The PWN is studied using 11.6 years of Fermi-LAT data between 1 GeV and 1 TeV. In particular, we present the results of the spectral analysis and the first energy-resolved morphological study of the PWN HESS J1825−137 at GeV energies, which provide new insights into the γ-ray characteristics of the nebula.Results. An optimised analysis of the source returns an extended emission region larger than 2 • , corresponding to an intrinsic size of about 150 pc, making HESS J1825−137 the most extended γ-ray PWN currently known. The nebula presents a strong energy dependent morphology within the GeV range, moving from a radius of ∼ 1.4 • below 10 GeV to a radius of ∼0.8 • above 100 GeV, with a shift in the centroid location. Conclusions. Thanks to the large extension and peculiar energy-dependent morphology, it is possible to constrain the particle transport mechanisms inside the PWN HESS J1825−137. Using the variation of the source extension and position, as well as the constraints on the particle transport mechanisms, we present a scheme for the possible evolution of the system. Finally, we provide an estimate of the electron energy density and we discuss its nature in the PWN and TeV halo-like scenario.

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“…However, this was calculated assuming a similar diffusion in the local bubble and in the rest of the disc and halo, which may be questionable. Recent γ-ray observations (Abeysekara et al 2017;Di Mauro et al 2019)-interpreted as pockets of slow diffusion around pulsars (e.g., Profumo et al 2018)-, and the indication that the local ISM properties are affected by several SN explosions a few Myr ago (Fields et al 2019) provide enough motivation to revisit this issue in a future study.…”

Section: Actual Constraints On Lmentioning

confidence: 99%

“…3.4, which could be very sensitive to the local ISM. However, similarly to radioactive nuclei, inhomogeneous spatial diffusion zones around CR sources (Abeysekara et al 2017;Di Mauro et al 2019), could also affect primary and secondary lepton spectra in different and very non trivial ways. These complications go beyond the scope of this analysis.…”

Section: Flux Calculation and Uncertaintiesmentioning

confidence: 99%

Galactic halo size in the light of recent AMS-02 data

Weinrich,

Boudaud,

Derome

et al. 2020

Preprint

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Context. The vertical diffusive halo size of the Galaxy, L, is a key parameter for dark matter indirect searches. It can be better determined thanks to recent AMS-02 data. Aims. We set constraints on L from Be/B and 10 Be/Be data, and perform a consistency check with positron data. We detail the dependence of Be/B and 10 Be/Be on L and forecast on which energy range better data would be helpful for future L improvements. Methods. We use usine v3.5 for the propagation of nuclei, and e + are calculated with the pinching method of Boudaud et al. (2017).Results. The current AMS-02 Be/B (∼ 3% precision) and ACE-CRIS 10 Be/Be (∼ 10% precision) data bring similar and consistent constraints on L. The AMS-02 Be/B data alone constrain L = 5 +3−2 kpc at 1σ, a range for which most models do not overproduce positrons. Future experiments need to deliver percent-level accuracy on 10 Be/ 9 Be anywhere below 10 GV to further constrain L. Conclusions. Forthcoming AMS-02, HELIX, and PAMELA 10 Be/ 9 Be results will further test and possibly tighten the limits derived here. Elemental ratios involving radioactive species with different lifetimes (e.g., Al/Mg and Cl/Ar) are also awaited to provide complementary and robuster constraints.

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Erratum: Detection of a γ -ray halo around Geminga with the Fermi-LAT data and implications for the positron flux [Phys. Rev. D 100 , 123015 (2019)]

Cited by 27 publications

References 3 publications

Morphology of Gamma-Ray Halos around Middle-Aged Pulsars: Influence of the Pulsar Proper Motion

Morphology of Gamma-Ray Halos around Middle-Aged Pulsars: Influence of the Pulsar Proper Motion

Energy dependent morphology of the pulsar wind nebula HESS J1825-137 with Fermi-LAT

Galactic halo size in the light of recent AMS-02 data

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