Evidence of 200 TeV photons from HAWC J1825-134

Albert, A.; Alfaro, R.; Alvarez, C.; Camacho, J. R. Angeles; Arteaga-Velázquez, J. C.; Arunbabu, K. P.; Rojas, D. Avila; Solares, H. A. Ayala; Baghmanyan, V.; Belmont-Moreno, E.; BenZvi, S. Y.; Brisbois, C.; Capistrán, T.; Carramiñana, A.; Casanova, S.; Cotti, U.; Cotzomi, J.; De la Fuente, E.; Hernandez, R. Diaz; Dingus, B. L.; DuVernois, M. A.; Durocher, M.; Díaz-Vélez, J. C.; Engel, K.; Espinoza, C.; Fang, K.; Fleischhack, H.; Fraija, N.; Galván-Gámez, A.; Garcia, D.; García-González, J. A.; Garfias, F.; Giacinti, G.; González, M. M.; Goodman, J. A.; Harding, J. P.; Hona, B.; Huang, D.; Hueyotl-Zahuantitla, F.; Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Kunde, G. J.; Lara, A.; Lee, W. H.; Vargas, H. León; Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; Lundeen, J.; Malone, K.; Marandon, V.; Martinez, O.; Martínez-Castro, J.; Matthews, J. A.; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Omodei, N.; Peisker, A.; Araujo, Y. Pérez; Pérez-Pérez, E. G.; Rho, C. D.; Rosa-González, D.; Salazar, H.; Greus, F. Salesa; Sandoval, A.; Schneider, M.; Serna, F.; Springer, R. W.; Tollefson, K.; Torres, I.; Torres-Escobedo, R.; Ureña-Mena, F.; Villaseñor, L.; Willox, E.; Zhou, H.; de León, C.

doi:10.48550/arxiv.2012.15275

Cited by 3 publications

(6 citation statements)

References 33 publications

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“…The spectral energy distribution (SED= E 2 γ dN γ /dE γ ) of HAWC J1825-134 according to Albert et al (2020) is shown in Figure 1. Three model γ-ray SEDs are also shown in this Figure, assuming a hadronuclear (more precisely, proton-proton) mechanism of γ-ray production on an optically thin matter.…”

Section: Examples Of the Primary Proton Spectrummentioning

confidence: 99%

“…The spectrum does not reveal any steepening or cutoff. Albert et al (2020) argue that the observed γ-rays were produced by the hadronic mechanism.…”

Section: Introductionmentioning

confidence: 95%

“…Very recently, the High Altitude Water Cherenkov (HAWC) collaboration reported a measurement of the γ-ray spectrum of the source HAWC J1825-134 up to the energy of 300 TeV (Albert et al 2020). The spectrum does not reveal any steepening or cutoff.…”

Section: Introductionmentioning

confidence: 99%

“…that is, neglecting the contribution of cascade γ-rays to the observable γ-ray spectrum; given that the average gas column density from the region of HAWC J1825-134 is N H = 3 × 10 22 cm −2(Albert et al 2020), this assumption is justified…”

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confidence: 99%

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The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134

Dzhatdoev,

Podlesnyi,

Vaiman

2021

Preprint

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The γ-ray spectrum of the source HAWC J1825-134 measured with the High Altitude Water Cherenkov (HAWC) observatory extends beyond 200 TeV without any evidence for a steepening or cutoff. There are some indications that the γ-rays detected with HAWC were produced by cosmic ray protons or nuclei colliding with the ambient gas. Assuming primary protons, we inquire which shape of the primary proton spectrum is compatible with the HAWC measurements. We find that the primary proton spectrum with the power-law shape of γ p = 2.2 and the cutoff energy E c−p > 700 TeV describes the data well. However, much harder spectra with γ p down to 1.3 and E c−p as low as 200 TeV also do not contradict the HAWC measurements. The former option might be realized if the accelerator is inside or very near to the γ-ray production zone. The latter option is viable for the case of a cosmic ray source which effectively confines low-energy (E p < 100 TeV) accelerated protons.

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Section: Examples Of the Primary Proton Spectrummentioning

confidence: 99%

“…The spectrum does not reveal any steepening or cutoff. Albert et al (2020) argue that the observed γ-rays were produced by the hadronic mechanism.…”

Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

See 2 more Smart Citations

The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134

Dzhatdoev,

Podlesnyi,

Vaiman

2021

Preprint

View full text Add to dashboard Cite

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“…The centroid of the highest energy emission >100 TeV from eHWC J1825-134 is located between the two known sources HESS J1825-137 and HESS J1826-130. A recent detailed study attempts to disentangle contributions from multiple components in the region, with indications for an independent emission region emerging at the highest energies, potentially associated with molecular material (Albert et al 2020).…”

Section: Potentially Bright Clouds Observable By Hawcmentioning

confidence: 99%

Using Interstellar Clouds to Search for Galactic PeVatrons: Gamma-ray Signatures from Supernova Remnants

Mitchell,

Rowell,

Celli

et al. 2021

Preprint

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Interstellar clouds can act as target material for hadronic cosmic rays; gamma rays subsequently produced through inelastic proton-proton collisions and spatially associated with such clouds can provide a key indicator of efficient particle acceleration. However, even in the case that particle acceleration proceeds up to PeV energies, the system of accelerator and nearby target material must fulfil a specific set of conditions in order to produce a detectable gamma-ray flux. In this study, we rigorously characterise the necessary properties of both cloud and accelerator. By using available Supernova Remnant (SNR) and interstellar cloud catalogues, we produce a ranked shortlist of the most promising target systems, those for which a detectable gamma-ray flux is predicted, in the case that particles are accelerated to PeV energies in a nearby SNR. We discuss detection prospects for future facilities including CTA, LHAASO and SWGO; and compare our predictions with known gamma-ray sources. The four interstellar clouds with the brightest predicted fluxes >100 TeV identified by this model are located at (l,b) = (330.05, 0.13), (15.82, -0.46), (271.09, -1.26), and (21.97, -0.29). These clouds are consistently bright under a range of model scenarios, including variation in the diffusion coefficient and particle spectrum. On average, a detectable gamma-ray flux is more likely for more massive clouds; systems with lower separation distance between the SNR and cloud; and for slightly older SNRs.

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The Highest Energy HAWC Sources are Likely Leptonic and Powered by Pulsars

Sudoh,

Linden,

Hooper

2021

Preprint

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The HAWC Collaboration has observed gamma rays at energies above 56 TeV from a collection of nine sources. It has been suggested that this emission could be hadronic in nature, requiring that these systems accelerate cosmic-ray protons or nuclei up to PeV-scale energies. In this paper, we instead show that the spectra of these objects favors a leptonic (inverse Compton) origin for their emission. More specifically, the gamma-ray emission from these objects can be straightforwardly accommodated within a model in which ∼ 10-20% of the host pulsar's spindown power is transferred into the acceleration of electrons and positrons with a power-law spectrum that extends to several hundred TeV or higher. The spectral break that is observed among these sources is naturally explained within the context of this simple model, and occurs at the energy where the timescale for energy losses matches the age of the pulsar. In contrast, this spectral feature cannot be straightforwardly accommodated in hadronic scenarios. Furthermore, hadronic models predict that these sources should produce more emission at GeV-scale energies than is observed. In light of these considerations, we conclude that HAWC's highest energy sources should be interpreted as TeV halos or pulsar wind nebulae, which produce their emission through inverse Compton scattering, and are powered by the rotational kinetic energy of their host pulsar.

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Evidence of 200 TeV photons from HAWC J1825-134

Cited by 3 publications

References 33 publications

The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134

The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134

Using Interstellar Clouds to Search for Galactic PeVatrons: Gamma-ray Signatures from Supernova Remnants

The Highest Energy HAWC Sources are Likely Leptonic and Powered by Pulsars

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