TeV<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>γ</mml:mi></mml:math>rays and neutrinos from photodisintegration of nuclei in Cygnus OB2

Anchordoqui, Luis A.; Beacom, J. F.; Goldberg, Haim; Palomares‐Ruiz, Sergio; Weiler, Thomas J.

doi:10.1103/physrevd.75.063001

Cited by 64 publications

(66 citation statements)

References 125 publications

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“…(Abdo et al 2007b). Hadronic models have been postulated to explain the Milagro flux measurements in the Cygnus region (Beacom & Kistler 2007;Anchordoqui et al 2007Anchordoqui et al , 2009.Given the observation in the IC-40 analysis of a significant a posteriori p-value from this catalog, we considered a prescription for future samples, and therefore, the IC-40 data are not used in this analysis to avoid bias. Recent publications by the Milagro collaboration (Abdo et al 2012) ruled out some of the assumptions about γ -ray fluxes used in Halzen et al (2008), so we use an equal weight for each source in the likelihood, with the intention of keeping our sensitivity optimal for all possible signal hypothesis.…”

Section: The Likelihood Search Methodsmentioning

confidence: 99%

SEARCH FOR TIME-INDEPENDENT NEUTRINO EMISSION FROM ASTROPHYSICAL SOURCES WITH 3 yr OF IceCube DATA

Aartsen

Abbasi

Abdou

et al. 2013

ApJ

105

129

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We present the results of a search for neutrino point sources using the IceCube data collected between 2008 April and 2011 May with three partially completed configurations of the detector: the 40-, 59-, and 79-string configurations. The live-time of this data set is 1040 days. An unbinned maximum likelihood ratio test was used to search for an excess of neutrinos above the atmospheric background at any given direction in the sky. By adding two more years of data with improved event selection and reconstruction techniques, the sensitivity was improved by a factor of 3.5 or more with respect to the previously published results obtained with the 40-string configuration of IceCube. We performed an all-sky survey and a dedicated search using a catalog of a priori selected objects observed by other telescopes. In both searches, the data are compatible with the background-only hypothesis. In the absence of evidence for a signal, we set upper limits on the flux of muon neutrinos. For an E −2 neutrino spectrum, the observed limits are (0.9-5) × 10 −12 TeV −1 cm −2 s −1 for energies between 1 TeV and 1 PeV in the northern sky and (0.9-23.2) × 10 −12 TeV −1 cm −2 s −1 for energies between 10 2 TeV and 10 2 PeV in the southern sky. We also report upper limits for neutrino emission from groups of sources that were selected according to theoretical models or observational parameters and analyzed with a stacking approach. Some of the limits presented already reach the level necessary to quantitatively test current models of neutrino emission.

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Section: The Likelihood Search Methodsmentioning

confidence: 99%

SEARCH FOR TIME-INDEPENDENT NEUTRINO EMISSION FROM ASTROPHYSICAL SOURCES WITH 3 yr OF IceCube DATA

Aartsen

Abbasi

Abdou

et al. 2013

ApJ

105

129

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“…The average density in the region depends on the temperatures T OB and T SG of O, B, and red supergiant stars, respectively, and the dilution due to the inverse square law. Specifically, for a region with N OB OB stars and N SG red supergiant stars, the photon density was estimated to be [51] n = 9 4…”

Section: Starburstsmentioning

confidence: 99%

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

Anchordoqui

Hooper

Sarkar

et al. 2008

Astroparticle Physics

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Ongoing experimental efforts to detect cosmic sources of high energy neutrinos are guided by the expectation that astrophysical accelerators of cosmic ray protons would also generate neutrinos through interactions with ambient matter and/or photons. However there will be a reduction in the predicted neutrino flux if cosmic ray sources accelerate not only protons but also significant numbers of heavier nuclei, as is indicated by recent air shower data. We consider plausible extragalactic sources such as active galactic nuclei, gamma-ray bursts and starburst galaxies and demand consistency with the observed cosmic ray composition and energy spectrum at Earth after allowing for propagation through intergalactic radiation fields. This allows us to calculate the expected neutrino fluxes from the sources, normalized to the observed cosmic ray spectrum. We find that the likely signals are still within reach of next generation neutrino telescopes such as IceCube.PACS numbers: 95.85. Ry, 98.70.Rz, 98.54.Cm, 98.54.Ep

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“…Actually, the disintegration rate also depends on the energy of the de-excitation photon. The differential rate is defined as (Anchordoqui et al 2007b)…”

Section: Photodisintegration Of Uhe Nucleimentioning

confidence: 99%

“…The mildly relativistic ejecta can accelerate cosmic-ray protons or nuclei up to energies 4 × 10 18 ZeV (Wang et al 2007;Budnik et al 2008). Inspired by the work of Anchordoqui et al (2007aAnchordoqui et al ( , 2007b, Wang et al (2008) and Murase et al (2008) pointed out that, in LLGRBs, the UHE nuclei can survive photodisintegration. The heavy and intermediate mass nuclei originate from the stellar wind of Wolf-Rayet (W-R) stars, which are thought to be the progenitors of HNe and long-duration GRBs.…”

Section: Introductionmentioning

confidence: 99%

“…The promising sites for TeV emission via this mechanism, in an astrophysical context, should have adequate high-energy nuclei and intense UV/optical photon fields, such as starburst regions (Anchordoqui et al 2007b). In this work, we concentrate on another possible type of such TeV sources: nearby long-duration, low-luminosity gamma-ray bursts (LLGRBs) (with luminosity L γ < 10 50 erg s −1 and redshift z < 0.2) associated with Type Ibc supernovae (SNe).…”

Section: Introductionmentioning

confidence: 99%

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MODELING PHOTODISINTEGRATION-INDUCED TeV PHOTON EMISSION FROM LOW-LUMINOSITY GAMMA-RAY BURSTS

Liu

2012

The Astronomical Journal

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Ultra-high-energy cosmic-ray heavy nuclei have recently been considered as originating from nearby low-luminosity gamma-ray bursts that are associated with Type Ibc supernovae. Unlike the power-law decay in long duration gamma-ray bursts, the light curve of these bursts exhibits complex UV/optical behavior: shock breakout dominated thermal radiation peaks at about 1 day, and, after that, nearly constant emission sustained by radioactive materials for tens of days. We show that the highly boosted heavy nuclei at PeV energy interacting with the UV/optical photon field will produce considerable TeV photons via the photodisintegration/photo-de-excitation process. It was later predicted that a thermal-like γ -ray spectrum peaks at about a few TeV, which may serve as evidence of nucleus acceleration. The future observations by the space telescope Fermi and by the ground atmospheric Cherenkov telescopes such as H.E.S.S., VERITAS, and MAGIC will shed light on this prediction.

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TeVγrays and neutrinos from photodisintegration of nuclei in Cygnus OB2

Cited by 64 publications

References 125 publications

SEARCH FOR TIME-INDEPENDENT NEUTRINO EMISSION FROM ASTROPHYSICAL SOURCES WITH 3 yr OF IceCube DATA

SEARCH FOR TIME-INDEPENDENT NEUTRINO EMISSION FROM ASTROPHYSICAL SOURCES WITH 3 yr OF IceCube DATA

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

MODELING PHOTODISINTEGRATION-INDUCED TeV PHOTON EMISSION FROM LOW-LUMINOSITY GAMMA-RAY BURSTS

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