Galactic Working Group

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The Galaxy seen from both hemispheres. Credit: Petr Horálek/Juan Carlos Casado

Introduction

The Galactic Working Group focuses on the spectral and morphological study of Galactic gamma-ray sources and their time properties at VHE gamma-rays.

Current Coordinators: Pol Bordas (Leader), Jakub Jurysek (Deputy)

Past Coordinators: Ruben Lopez-Coto

Channels

Mailing list: CTA sharepoint

Slack channel: CTA North Slack workspace

Meetings

Galactic calls (2022)

Galactic calls (2023)

Ongoing Projects

RS Oph

• PI: Team:
• Abstract:
• Link: Project Webpage

Galactic Center

• PI: Team:
• Abstract:
• Link: Project Webpage

Crab Nebula Performance

• PI: Abelardo Moralejo, Rubén López-Coto
• Team: Abelardo Moralejo, Rubén López-Coto, Thomas Vuillaume, Seiya Nozaki, Daniel Morcuende
• Abstract:

CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at
the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to ≃20 GeV. LST-1
started performing astronomical observations in November 2019, during its commissioning phase, and it has been taking data since then. We present the first LST-1 observations of the Crab Nebula,
the standard candle of very-high energy gamma-ray astronomy, and use them, together with simulations, to assess the basic performance parameters of the telescope. The data sample consists of
around 36 hours of observations at low zenith angles collected between November 2020 and March 2022. LST-1 has reached the expected performance during its commissioning period - only a minor
adjustment of the preexisting simulations was needed to match the telescope behavior. The energy threshold at trigger level is estimated to be around 20 GeV, rising to ≃30 GeV after data analysis.
Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.12 to 0.40 degrees, and energy resolution
from 15 to 50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50-h observation (12% for 30 minutes). The spectral energy distribution (in the 0.03 - 30 TeV range) and
the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at
the center of the Nebula. 

• Link: Project Webpage

Crab Pulsar

• PI: Team:
• Abstract:
• Link: Project Webpage

Boomerang SNR

• PI: Team: F. Cassol
• Abstract:
• Link: Project Webpage

T CrB

• PI: Team:
• Abstract:
• Link: Project Webpage

Geminga Pulsar

• PI: Team:
• Abstract:
• Link: Project Webpage

SGR 1935+2154

• PI: Team:
• Abstract:
• Link: Project Webpage

Publications

Papers Status

Proceedings

Observed Galactic Sources

Full up-to-date list of all observed sources: Sources observed with LST-1

Data collected (4 May 2023):

Crab: 301.4 hours, LHAASOJ2108+5157: 93.7 hours, GalacticCenter: 50.3 hours, G106.3+2.7: 49.6 hours, Geminga: 40.4 hours, SGR1935+2154: 37.7 hours LHAASOJ0341+5258: 28.7 hours, Nova_RS_Oph: 15.0 hours, U_Sco: 10.9 hours, LHAASOJ1956+2845: 6.9 hours, PSRJ1402+13: 5.7 hours, PSRJ2021+3651: 5.7 hours, HESS1857+026: 4.7 hours, LSV+4417: 4.6 hours, N-Her_2021: 4.4 hours, LSI+61: 4.0 hours, Cyg-X3: 3.9 hours, Cygnus_XNorth: 3.4 hours, V1405Cas: 3.3 hours, AGLJ2114+6249: 2.4 hours, G17.8+16.7: 2.2 hours, 4FGLJ1723.5-0501e: 1.6 hours PSRJ2229+6114: 1.4 hours, MAXIJ1848-015: 1.3 hours, PSRJ2032: 1.1 hours, HESS J1848-018: 0.3 hours, Nova_V1405_Cas: 0.3 hours,

Proposals

File:LST MAGIC Engineering proposal CycleXVII.pdf

Conferences

Please refer to the LSTCOS webpage for a list of upcoming conferences attended by LST members.

Relevant arXiv's (per month)

May 2023: File:May2023.pdf

June-July 2023:

July - September 2023:

September - October 2023:

• Link: Project Webpage

Useful Tools

• Coordinate converter http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/convcoord/convcoord.pl
• Distance converter http://www.convertworld.com/en/length/Parsec.html
• Energy/frequency/wavelength converter http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/energyconv/energyConv.pl
• A Date/Time Conversion Utility http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/xTime/xTime.pl
• Flux/count rate converter http://heasarc.gsfc.nasa.gov/Tools/w3pimms.html
• Catalog of TeV source http://tevcat.uchicago.edu/
• Publication of HESS, MAGIC and VERITAS
• To calculate source observability (you may have to introduce LST-1 coordinates 28.76195, -17.89005) http://www.magic.iac.es/scheduler/ or https://www.mpi-hd.mpg.de/hfm/HESS/public/Visibility.html