Pith. sign in

REVIEW 3 cited by

Discovery of TeV Gamma Ray Emission from Tycho's Supernova Remnant

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 1102.3871 v2 pith:AR237MBR submitted 2011-02-18 astro-ph.HE

Discovery of TeV Gamma Ray Emission from Tycho's Supernova Remnant

V. A. Acciari , E. Aliu , T. Arlen , T. Aune , M. Beilicke , W. Benbow , S. M. Bradbury , J. H. Buckley
show 77 more authors
V. Bugaev K. Byrum A. Cannon A. Cesarini L. Ciupik E. Collins-Hughes W. Cui R. Dickherber C. Duke M. Errando J. P. Finley G. Finnegan L. Fortson A. Furniss N. Galante D. Gall G. H. Gillanders S. Godambe S. Griffin J. Grube R. Guenette G. Gyuk D. Hanna J. Holder J. P. Hughes C. M. Hui T. B. Humensky P. Kaaret N. Karlsson M. Kertzman D. Kieda H. Krawczynski F. Krennrich M. J. Lang S. LeBohec A. S Madhavan G. Maier P. Majumdar S. McArthur A. McCann P. Moriarty R. Mukherjee R. A. Ong M. Orr A. N. Otte D. Pandel N. Park J. S. Perkins M. Pohl J. Quinn K. Ragan L. C. Reyes P. T. Reynolds E. Roache H. J. Rose D. B. Saxon M. Schroedter G. H. Sembroski G. Demet Senturk P. Slane A. W. Smith G. Te\v{s}i\'c M. Theiling S. Thibadeau K. Tsurusaki A. Varlotta V. V. Vassiliev S. Vincent M. Vivier S. P. Wakely J. E. Ward T. C. Weekes A. Weinstein T. Weisgarber D. A. Williams M. Wood B. Zitzer
This is my paper
classification astro-ph.HE
keywords emissiongammaremnantprimesupernovaabovediscoveryfield
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

We report the discovery of TeV gamma-ray emission from the Type Ia supernova remnant (SNR) G120.1+1.4, known as Tycho's supernova remnant. Observations performed in the period 2008-2010 with the VERITAS ground-based gamma-ray observatory reveal weak emission coming from the direction of the remnant, compatible with a point source located at $00^{\rm h} \ 25^{\rm m} \ 27.0^{\rm s},\ +64^{\circ} \ 10^{\prime} \ 50^{\prime\prime}$ (J2000). The TeV photon spectrum measured by VERITAS can be described with a power-law $dN/dE = C(E/3.42\;\textrm{TeV})^{-\Gamma}$ with $\Gamma = 1.95 \pm 0.51_{stat} \pm 0.30_{sys}$ and $C = (1.55 \pm 0.43_{stat} \pm 0.47_{sys}) \times 10^{-14}$ cm$^{-2}$s$^{-1}$TeV$^{-1}$. The integral flux above 1 TeV corresponds to $\sim 0.9%$ percent of the steady Crab Nebula emission above the same energy, making it one of the weakest sources yet detected in TeV gamma rays. We present both leptonic and hadronic models which can describe the data. The lowest magnetic field allowed in these models is $\sim 80 \mu$G, which may be interpreted as evidence for magnetic field amplification.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics

    astro-ph.HE 2026-06 unverdicted novelty 5.0

    A self-consistent multi-zone kinetic model reproduces SN 1006's spectrum and morphology, finding ~20% CR acceleration efficiency in quasi-parallel shocks, <1% in quasi-perpendicular shocks, and predominantly leptonic ...

  2. On The Nonthermal Power Laws In Magnetized Turbulent Plasmas

    physics.plasm-ph 2026-05 unverdicted novelty 5.0

    Derives and validates via PIC simulations a scaling law for nonthermal spectral tails in mildly to strongly magnetized turbulent plasmas, with application to black-hole coronae.

  3. On The Nonthermal Power Laws In Magnetized Turbulent Plasmas

    physics.plasm-ph 2026-05 unverdicted novelty 4.0

    A scaling law for nonthermal power-law tails in magnetized turbulent plasmas is derived from particle transport principles and confirmed by PIC simulations with escape, with applications to black hole coronae.