J/ApJ/907/L30 Gamma-Ray spectral energy in HAWC J1825-134 region (Albert+, 2021)
Evidence of 200 TeV Photons from HAWC J1825-134.
Albert A., Alfaro R., Alvarez C., Camacho J.R.A., Arteaga-Velazquez J.C.,
Arunbabu K.P., Rojas D.A., Ayala Solares H.A., Baghmanyan V.,
Belmont-Moreno E., BenZvi S.Y., Brisbois C., Capistran T., Carraminana A.,
Casanova S., Cotti U., Cotzomi J., De la Fuente E., Hernandez R.D.,
Dingus B.L., DuVernois M.A., Durocher M., Diaz-Velez J.C., Engel K.,
Espinoza C., Fang K., Fleischhack H., Fraija N., Galvan-Gamez A., Garcia D.,
Garcia-Gonzalez J.A., Garfias F., Giacinti G., Gonzalez M.M., Goodman J.A.,
Harding J.P., Hona B., Huang D., Hueyotl-Zahuantitla F., Huntemeyer P.,
Iriarte A., Jardin-Blicq A., Joshi V., Kunde G.J., Lara A., Lee W.H.,
Vargas H.L., Linnemann J.T., Longinotti A.L., Luis-Raya G., Lundeen J.,
Malone K., Marandon V., Martinez O., Martinez-Castro J., Matthews J.A.,
Miranda-Romagnoli P., Moreno E., Mostafa M., Nayerhoda A., Nellen L.,
Newbold M., Nisa M.U., Noriega-Papaqui R., Omodei N., Peisker A.,
Araujo Y.P., Perez-Perez E.G., Rho C.D., Rosa-Gonzalez D., Salazar H.,
Greus F.S., Sandoval A., Schneider M., Serna F., Springer R.W.,
Tollefson K., Torres I., Torres-Escobedo R., Urena-Mena F., Villasenor L.,
Willox E., Zhou H., de Leon C.
<Astrophys. J., 907, L30 (2021)>
=2021ApJ...907L..30A 2021ApJ...907L..30A
ADC_Keywords: Gamma rays; Energy distributions
Keywords: Gamma-ray astronomy ; Gamma-ray sources ; Gamma-rays ; Gamma-ray
observatories
Abstract:
The Earth is bombarded by ultrarelativistic particles, known as cosmic
rays (CRs). CRs with energies up to a few PeV (=1015eV), the knee in
the particle spectrum, are believed to have a Galactic origin. One or
more factories of PeV CRs, or PeVatrons, must thus be active within
our Galaxy. The direct detection of PeV protons from their sources is
not possible since they are deflected in the Galactic magnetic fields.
Hundred TeV γ-rays from decaying π0, produced when PeV CRs
collide with the ambient gas, can provide the decisive evidence of
proton acceleration up to the knee. Here we report the discovery by
the High Altitude Water Cerenkov (HAWC) observatory of the γ-ray
source, HAWCJ1825-134, whose energy spectrum extends well beyond
200TeV without a break or cutoff. The source is found to be coincident
with a giant molecular cloud. The ambient gas density is as high as
700protons/cm3. While the nature of this extreme accelerator remains
unclear, CRs accelerated to energies of several PeV colliding with the
ambient gas likely produce the observed radiation.
Description:
High Altitude Water Cerenkov (HAWC) is a cosmic and γ-ray
observatory located at a latitude of 19deg north and an altitude of
4100m on the slope of the Sierra Negra volcano close to Puebla, in
central Mexico. The HAWC detector has a large field of view (2sr),
high duty cycle (>90% uptime), an angular resolution, which can be as
good as 0.1deg, and unprecedented sensitivity for γ-ray sources
beyond 100TeV. HAWC has carried out the deepest ever survey of the
Galactic plane in the unexplored range of γ-rays with energies
beyond 50TeV.
Objects:
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RA (2000) DE Designation(s)
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18 25.8 -13 25 HAWC J1825-134 = HAWC J1825-134
18 25.5 -13 52 HAWC J1825-138 = HAWC J1825-138
18 26.0 -12 52 HAWC J1826-128 = HAWC J1826-128
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fig2.dat 59 30 γ-ray spectral energy distributions
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See also:
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
J/A+A/275/67 : Velocity Field of the outer Galaxy (Brand+ 1993)
J/A+A/404/223 : 2MASS IR star clusters in the Galaxy (Bica+, 2003)
J/ApJ/649/759 : Bubbles in the galactic disk (Churchwell+, 2006)
J/ApJS/212/1 : The WISE catalog of Galactic HII regions (Anderson+, 2014)
J/A+A/594/A116 : HI4PI spectra and column density maps (HI4PI team+, 2016)
J/A+A/585/A101 : Milky Way global survey star clusters. V. (Kharchenko+, 2016)
J/ApJ/834/57 : Milky Way molecular cloud from 12CO (Miville-Deschenes+, 2017)
J/A+A/612/A1 : H.E.S.S. Galactic Plane Survey (HESS+, 2018)
J/A+A/621/A116 : HESSJ1825-137 particle transport (H.E.S.S.Collaboration, 2019)
Byte-by-byte Description of file: fig2.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- ID Identifier
15- 20 F6.2 TeV Emed [1.22/225] Median energy
22- 31 E10.4 TeV/cm2/s Flux [4.9e-13/1.6e-11]? Flux
33- 42 E10.4 TeV/cm2/s E_Flux [2e-13/5e-12]? Upper limit on Flux
44- 53 E10.4 TeV/cm2/s e_Flux [2e-13/6e-12]? Lower limit on Flux
55- 59 A5 --- Limit Upper limit flag; True or False
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 09-Jun-2022