Perturbative charm production and the prompt atmospheric neutrino flux in light of RHIC and LHC

Bhattacharya, Atri; Enberg, Rikard; Reno, Mary Hall; Sarčević, Ina; Staśto, Anna

doi:10.1007/jhep06(2015)110

Cited by 109 publications

(178 citation statements)

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“…The charm production cross-sections are also important in evaluating the rate of highenergy neutrinos created from the decay of charm hadrons produced in cosmic ray interactions with atmospheric nuclei [1,14]. Such neutrinos constitute an important background for experiments such as IceCube [15] searching for neutrinos produced from astrophysical sources.…”

Section: Jhep03(2016)159mentioning

confidence: 99%

“…In this region the uncertainties on the gluon parton density functions are large, exceeding 30% [1,13], and LHCb measurements can be used to constrain them. For example, the predictions provided in ref.[1] have made direct use of these constraints from LHCb data, taking as input a set of parton density functions that is weighted to match the LHCb measurements at √ s = 7 TeV.The charm production cross-sections are also important in evaluating the rate of highenergy neutrinos created from the decay of charm hadrons produced in cosmic ray interactions with atmospheric nuclei [1,14]. Such neutrinos constitute an important background for experiments such as IceCube Charm mesons produced at the pp collision point, either directly or as decay products of excited charm resonances, are referred to as promptly produced.…”

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confidence: 99%

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Measurements of prompt charm production cross-sections in pp collisions at s = 13 $$ \sqrt{s}=13 $$ TeV

Aaij¹,

Beteta²,

Adeva³

et al. 2016

J. High Energ. Phys.

131

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Production cross-sections of prompt charm mesons are measured with the first data from pp collisions at the LHC at a centre-of-mass energy of 13 TeV. The data sample corresponds to an integrated luminosity of 4.98 ± 0.19 pb −1 collected by the LHCb experiment. The production cross-sections of D 0 , D + , D + s , and D * + mesons are measured in bins of charm meson transverse momentum, p T , and rapidity, y, and cover the range 0 < p T < 15 GeV/c and 2.0 < y < 4.5. The inclusive cross-sections for the four mesons, including charge conjugation, within the range of 1 < p T < 8 GeV/c are found to bewhere the uncertainties are due to statistical and systematic uncertainties, respectively.Keywords: Charm physics, Forward physics, Hadron-Hadron scattering, Heavy quark production, QCD A Absolute cross-sections 20 B Cross-section ratios at different energies 24 C Cross-section ratios for different mesons 28The LHCb collaboration 38 IntroductionMeasurements of charm production cross-sections in proton-proton collisions are important tests of the predictions of perturbative quantum chromodynamics [1][2][3]. Predictions of charm meson cross-sections have been made at next-to-leading order using the generalized mass variable flavour number scheme (GMVFNS) [3][4][5][6][7][8] and at fixed order with next-to-leading-log resummation (FONLL) [1,2,[9][10][11][12]. These are based on a factorisation approach, where the cross-sections are calculated as a convolution of three terms: the parton distribution functions of the incoming protons; the partonic hard scattering rate, estimated as a perturbative series in the coupling constant of the strong interaction; and a fragmentation function that parametrises the hadronisation of the charm quark into a -1 - JHEP03(2016)159given type of charm hadron. The range of y and p T accessible to LHCb enables quantum chromodynamics calculations to be tested in a region where the momentum fraction, x, of the initial state partons can reach values below 10 −4 . In this region the uncertainties on the gluon parton density functions are large, exceeding 30% [1,13], and LHCb measurements can be used to constrain them. For example, the predictions provided in ref.[1] have made direct use of these constraints from LHCb data, taking as input a set of parton density functions that is weighted to match the LHCb measurements at √ s = 7 TeV.The charm production cross-sections are also important in evaluating the rate of highenergy neutrinos created from the decay of charm hadrons produced in cosmic ray interactions with atmospheric nuclei [1,14]. Such neutrinos constitute an important background for experiments such as IceCube Charm mesons produced at the pp collision point, either directly or as decay products of excited charm resonances, are referred to as promptly produced. No attempt is made to distinguish between these two sources. This paper presents measurements of the crosssections for the prompt production of D 0 , D + , D + s , and D * (2010) + (henceforth denoted as D * + ) mesons, based ...

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Section: Jhep03(2016)159mentioning

confidence: 99%

mentioning

confidence: 99%

Measurements of prompt charm production cross-sections in pp collisions at s = 13 $$ \sqrt{s}=13 $$ TeV

Aaij¹,

Beteta²,

Adeva³

et al. 2016

J. High Energ. Phys.

131

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“…Several more recent calculations of the prompt flux have been published: GMS (H3p) (Garzelli et al 2015), BERSS (H3p) (Bhattacharya et al 2015) and GRRST (H3p) (Gauld et al 2016). Figure 21 shows multiple predictions for the prompt flux as well as the upper limit calculated here using the prediction from Enberg et al (2008) and taking into account a more realistic cosmic-ray model (Gaisser 2012).…”

Section: Search For a Signature Of Prompt Atmospheric Neutrinosmentioning

confidence: 98%

“…For the first time, it is possible to constrain such a flux in this range of theoretical predictions. However, recent perturbative QCD calculations from Garzelli et al (2015), Bhattacharya et al (2015) and (Gauld et al 2016) predict lower prompt neutrino fluxes which are not yet constrained by the upper limit.…”

Section: Search For a Signature Of Prompt Atmospheric Neutrinosmentioning

confidence: 99%

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

ApJ

462

664

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The IceCube Collaboration has previously discovered a high-energy astrophysical neutrino flux using neutrino events with interaction vertices contained within the instrumented volume of the IceCube detector. We present a complementary measurement using charged current muon neutrino events where the interaction vertex can be outside this volume. As a consequence of the large muon range the effective area is significantly larger but the field of view is restricted to the Northern Hemisphere. IceCube data from 2009 through 2015 have been analyzed using a likelihood approach based on the reconstructed muon energy and zenith angle. At the highest neutrino energies between and a significant astrophysical contribution is observed, excluding a purely atmospheric origin of these events at significance. The data are well described by an isotropic, unbroken power-law flux with a normalization at neutrino energy of and a hard spectral index of . The observed spectrum is harder in comparison to previous IceCube analyses with lower energy thresholds which may indicate a break in the astrophysical neutrino spectrum of unknown origin. The highest-energy event observed has a reconstructed muon energy of which implies a probability of less than for this event to be of atmospheric origin. Analyzing the arrival directions of all events with reconstructed muon energies above no correlation with known γ-ray sources was found. Using the high statistics of atmospheric neutrinos we report the current best constraints on a prompt atmospheric muon neutrino flux originating from charmed meson decays which is below 1.06 in units of the flux normalization of the model in Enberg et al.

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“…3 is shown an updated version of our plot from [6]. It compares more popular calculations ERS [12], TIG [13] and MRS [14] with the more recent BERSS [15] and GMS [16] calculations. The band around the GMS line represents uncertainties from the inputs of the nextto-leading order (NLO) perturbative calculation, i.e.…”

Section: Comments On Prompt Neutrino Calculationsmentioning

confidence: 99%

Phenomenology of atmospheric neutrinos

Fedynitch

2016

EPJ Web of Conferences

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Abstract. The detection of astrophysical neutrinos, certainly a break-through result, introduced new experimental challenges and fundamental questions about acceleration mechanisms of cosmic rays. On one hand IceCube succeeded in finding an unambiguous proof for the existence of a diffuse astrophysical neutrino flux, on the other hand the precise determination of its spectral index and normalization requires a better knowledge about the atmospheric background at hundreds of TeV and PeV energies. Atmospheric neutrinos in this energy range originate mostly from decays of heavy-flavor mesons, which production in the phase space relevant for prompt leptons is uncertain. Current acceleratorbased experiments are limited by detector acceptance and not so much by the collision energy. This paper recaps phenomenological aspects of atmospheric leptons and calculation methods, linking recent progress in flux predictions with particle physics at colliders, in particular the Large Hadron Collider.

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Perturbative charm production and the prompt atmospheric neutrino flux in light of RHIC and LHC

Cited by 109 publications

References 85 publications

Measurements of prompt charm production cross-sections in pp collisions at s = 13 $$ \sqrt{s}=13 $$ TeV

Measurements of prompt charm production cross-sections in pp collisions at s = 13 $$ \sqrt{s}=13 $$ TeV

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Phenomenology of atmospheric neutrinos

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