Particle transport within the pulsar wind nebula HESS J1825-137

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Details zur Publikation

Autorinnen und Autoren: Abdalla H, Aharonian F, Benkhali FA, Anguner EO, Arakawa M, Arcaro C, Armand C, Arrieta M, Backes M, Barnard M, Becherini Y, Tjus JB, Berge D, Bernloehr K, Blackwell R, Bottcher M, Boisson C, Bolmont J, Bonnefoy S, Bordas P, Bregeon J, Brun F, Brun P, Bryan M, Büchele M, Bulik T, Bylund T, Capasso M, Caroff S, Carosi A, Casanova S, Cerruti M, Chakraborty N, Chand T, Chandra S, Chaves RCG, Chen A, Colafrancesco S, Condon B, Davids ID, Deil C, Devin J, Dewilt P, Dirson L, Djannati-Atai A, Dmytriiev A, Donath A, Doroshenko V, Drury LO, Dyks J, Egberts K, Emery G, Ernenwein JP, Eschbach S, Fegan S, Fiasson A, Fontaine G, Funk S, Fuessling M, Gabici S, Gallant YA, Gate F, Giavitto G, Glawion D, Glicenstein JF, Gottschall D, Grondin MH, Hahn J, Haupt M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Hoischen C, Holch TL, Holler M, Horns D, Huber D, Iwasaki H, Jacholkowska A, Jamrozy M, Jankowsky D, Jankowsky F, Jouvin L, Jung-Richardt I, Kastendieck MA, Katarzynski K, Katsuragawa M, Katz U, Kerszberg D, Khangulyan D, Khelifi B, King J, Klepser S, Kluzniak W, Komin N, Kosack K, Kraus M, Lamanna G, Lau J, Lefaucheur J, Lemiere A, Lemoine-Goumard M, Lenain JP, Leser E, Lohse T, Lopez-Coto R, Lypova A, Malyshev D, Marandon V, Marcowith A, Mariaud C, Marti-Devesa G, Marx R, Maurin G, Meintjes PJ, Mitchell AMW, Moderski R, Mohamed M, Mohrmann L, Moore C, Moulin E, Murach T, Nakashima S, De Naurois M, Ndiyavala H, Niederwanger F, Niemiec J, Oakes L, O'Brien P, Odaka H, Ohm S, Ostrowski M, Oya I, Panter M, Parsons RD, Perennes C, Petrucci PO, Peyaud B, Piel Q, Pita S, Poireau V, Noel AP, Prokhorov DA, Prokoph H, Puehlhofer G, Punch M, Quirrenbach A, Raab S, Rauth R, Reimer A, Reimer O, Renaud M, Rieger F, Rinchiuso L, Romoli C, Rowell G, Rudak B, Ruiz-Velasco E, Sahakian V, Saito S, Sanchez DA, Santangelo A, Sasaki M, Schlickeiser R, Schussler F, Schulz A, Schutte H, Schwanke U, Schwemmer S, Seglar-Arroyo M, Senniappan M, Seyffert AS, Shafi N, Shilon I, Shiningayamwe K, Simoni R, Sinha A, Sol H, Specovius A, Spir-Jacob M, Stawarz L, Steenkamp R, Stegmann C, Steppa C, Takahashi T, Tavernet JP, Tavernier T, Taylor AM, Terrier R, Tibaldo L, Tiziani D, Tluczykont M, Trichard C, Tsirou M, Tsuji N, Tuffs R, Uchiyama Y, Van Der Walt DJ, van Eldik C, Van Rensburg C, Van Soelen B, Vasileiadis G, Veh J, Venter C, Vincent P, Vink J, Voisin F, Voelk HJ, Vuillaume T, Wadiasingh Z, Wagner SJ, Wagner RM, White R, Wierzcholska A, Yang R, Yoneda H, Zaborov D, Zacharias M, Zanin R, Zdziarski AA, Zech A, Zefi F, Ziegler A, Zorn J, Zywucka N
Zeitschrift: Astronomy & Astrophysics
Jahr der Veröffentlichung: 2019
Band: 621
ISSN: 1432-0746


Abstract

Context. We present a detailed view of the pulsar wind nebula (PWN) HESS J1825-137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics. Aims. The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5° from the pulsar, ∼1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of ∼100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of RE
α
with α = -0.29 ± 0.04
stat
± 0.05
sys
disfavours a pure diffusion scenario for particle transport within the nebula. The total γ-ray flux of the nebula above 1 TeV is found to be (1.12 ± 0.03
stat
± 0.25
sys
) × 10
-11
cm
-2
s
-1
, corresponding to ∼64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE γ-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.


FAU-Autorinnen und Autoren / FAU-Herausgeberinnen und Herausgeber

Büchele, Matthias
Lehrstuhl für Physik
Eschbach, Stefan
Lehrstuhl für Physik
Funk, Stefan Prof. Dr.
Lehrstuhl für Physik
Jankowsky, David
Lehrstuhl für Physik
Jung-Richardt, Ira PD Dr.
Lehrstuhl für Physik
Katz, Uli Prof. Dr.
Lehrstuhl für Experimentalphysik (Astroteilchenphysik)
Mohrmann, Lars Dr.
Lehrstuhl für Physik
Raab, Susanne
Lehrstuhl für Physik
Sasaki, Manami Prof. Dr.
Professur für Multiwellenlängenastronomie
Specovius, Andreas
Professur für Experimentalphysik
Tiziani, Domenico
Professur für Experimentalphysik
van Eldik, Christopher Prof. Dr.
Professur für Experimentalphysik
Veh, Johannes Dr.
Professur für Experimentalphysik
Ziegler, Alexander
Professur für Experimentalphysik


Zitierweisen

APA:
Abdalla, H., Aharonian, F., Benkhali, F.A., Anguner, E.O., Arakawa, M., Arcaro, C.,... Zywucka, N. (2019). Particle transport within the pulsar wind nebula HESS J1825-137. Astronomy & Astrophysics, 621. https://dx.doi.org/10.1051/0004-6361/201834335

MLA:
Abdalla, H., et al. "Particle transport within the pulsar wind nebula HESS J1825-137." Astronomy & Astrophysics 621 (2019).

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Zuletzt aktualisiert 2019-06-05 um 09:23