J/A+A/627/A100ivo://CDS.VizieR/J/A+A/627/A100doi:10.26093/cds/vizier.36270100CDSH.E.S.S. Collaboration,Abdalla H.Aharonian F.Ait Benkhali F.Anguener E.O.Arakawa M.,Arcaro C.Armand C.Backes M.Barnard M.Becherini Y.Berge D.,Bernloehr K.Blackwell R.Boettcher M.Boisson C.Bolmont J.,Bonnefoy S.Bregeon J.Brun F.Brun P.Bryan M.Buechele M.Bulik T.,Bylund T.Capasso M.Caro S.Carosi A.Casanova S.Cerruti M.,Chakraborty N.Chand T.Chandra S.Chaves R.C.G.Chen A.,Colafrancesco S.Condon B.Davids I.D.Deil C.Devin J.deWilt P.,Dirson L.Djannati-Atai A.Dmytriiev A.Donath A.Doroshenko V.,Drury L.O'C.Dyks J.Egberts K.Emery G.Ernenwein J.-P.Eschbach S.,Feijen K.Fegan S.Fiasson A.Fontaine G.Funk S.Fuessling M.,Gabici S.Gallant Y.A.Gate F.Giavitto G.Glawion D.Glicenstein J.F.,Gottschall D.Grondin M.-H.Hahn J.Haupt M.Heinzelmann G.Henri G.,Hermann G.Hinton J.A.Hofmann W.Hoischen C.Holch T.L.Holler M.,Horns D.Huber D.Iwasaki H.Jacholkowska y A.Jamrozy M.Jankowsky D.,Jankowsky F.Jouvin L.Jung-Richardt I.Kastendieck M.A.,Katarzy'nski K.Katsuragawa M.Katz U.Khangulyan D.Khelifi B.,King J.Klepser S.Klu'zniak W.Komin Nu.Kosack K.Kostunin D.,Kraus M.Lamanna G.Lau J.Lemiere A.Lemoine-Goumard M.Lenain J.-P.,Leser E.Lohse T.Lopez-Coto R.Lypova I.Malyshev D.Marandon V.,Marcowith A.Mariaud C.Marti-Devesa G.Marx R.Maurin G.Maxted N.I.,Meintjes P.J.Mitchell A.M.W.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.,de Ona Wilhelmi E.Ostrowski M.Oya I.Panter M.Parsons R.D.,Perennes C.Petrucci P.-O.Peyaud B.Piel Q.Pita S.Poireau V.,Priyana Noel A.Prokhorov D.A.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 D.A.Santangelo A.Sasaki M.,Schlickeiser R.Schuessler F.Schulz A.Schutte H.Schwanke U.,Schwemmer S.Seglar-Arroyo M.Senniappan M.Seyert A.S.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 J.-P.Tavernier T.Taylor A.M.Terrier R.,Tibaldo L.Tiziani D.Tluczykont M.Trichard C.Tsirou M.Tsuji N.,Tus R.Uchiyama Y.van der Walt D.J.van Eldik C.van Rensburg C.,van Soelen B.Vasileiadis G.Veh J.Venter C.Vincent P.Vink J.,Voisin F.Voelk H.J.Vuillaume T.Wadiasingh Z.Wagner S.J.White R.,Wierzcholska A.Yang R.Yoneda H.Zaborov D.Zacharias M.Zanin R.,Zdziarski A.A.Zech A.Ziegler A.Zorn J.Zywucka N.2019-09-20T05:12:02Z2019-07-08T07:07:43ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frpulsarsgamma-ray-astronomyx-ray-sourcesPulsar Wind Nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission toward an elongated structure called the cocoon. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. We use data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3pc to 4pc from the pulsar along the cocoon. We obtain gamma-ray spectra of the same regions from H.E.S.S. observations and fit a radiative model to the multi-wavelength spectra. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10^-12^erg/cm^-3^. The data indicate the presence of a cutoff in the electron spectrum at energies of 100TeV and a magnetic field strength of 6G. Constraints on the presence of turbulent magnetic fields are weak. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot account completely for the missing pressure, that may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range >~10keV.2019A&A...627A.100Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/627/A100CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/377/925 : Radial velocity curves of Vela X-1 (Barziv+, 2001)J/A+A/395/129 : Cyclotron lines in Vela X-1 (Kreykenbohm+, 2002)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/627/A100https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/627/A100http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/627/A100https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/627/A100https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/627/A100http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/627/A100GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/627/A100/list (List of fits spectra)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/627/A100/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/627/A100/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/627/A100/list?GETtext/xml+votable180.050000true128.81-45.280.005555555555555556Associated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/627/A1006/39235 39241https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/627/A100?format=asciiRadioGamma-rayX-raydefaultJ/A+A/627/A100/listList of fits spectraspShow the spectrummeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar