Simulated gamma-ray pulse profile of the Crab pulsar with the Cherenkov Telescope Array

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F16%3A00538416" target="_blank" >RIV/68378271:_____/16:00538416 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1093/mnras/stw883" target="_blank" >https://doi.org/10.1093/mnras/stw883</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stw883" target="_blank" >10.1093/mnras/stw883</a>

Result language

angličtina

Original language name

Simulated gamma-ray pulse profile of the Crab pulsar with the Cherenkov Telescope Array

Original language description

We present simulations of the very high energy (VHE) gamma-ray light curve of the Crab pulsar as observed by the Cherenkov Telescope Array (CTA). The CTA pulse profile of the Crab pulsar is simulated with the specific goal of determining the accuracy of the position of the interpulse. We fit the pulse shape obtained by the Major Atmospheric Gamma-Ray Imaging Cherenkov (MAGIC) telescope with a three-Gaussian template and rescale it to account for the different CTA instrumental and observational configurations. Simulations are performed for different configurations of CTA and for the ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) mini-array. The northern CTA configuration will provide an improvement of a factor of similar to 3 in accuracy with an observing time comparable to that of MAGIC (73 h). Unless the VHE spectrum above 1 TeV behaves differently from what we presently know, unreasonably long observing times are required for a significant detection of the pulsations of the Crab pulsar with the high-energy-range sub-arrays. We also found that an independent VHE timing analysis is feasible with Large Size Telescopes. CTA will provide a significant improvement in determining the VHE pulse shape parameters necessary to constrain theoretical models of the gamma-ray emission of the Crab pulsar. One of such parameters is the shift in phase between peaks in the pulse profile at VHE and in other energy bands that, if detected, may point to different locations of the emission regions.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10303 - Particles and field physics

Project

—

Continuities

—

Publication year

2016

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Volume of the periodical

459

Issue of the periodical within the volume

4

Country of publishing house

GB - UNITED KINGDOM

Number of pages

9

Pages from-to

3783-3791

UT code for WoS article

000379830700031

EID of the result in the Scopus database

2-s2.0-84983087524