J/A+A/627/A100 HESS and Suzaku observations of Vela X (HESS Coll+, 2019)
H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula.
H.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.
<Astron. Astrophys. 627, A100 (2019)>
=2019A&A...627A.100H 2019A&A...627A.100H (SIMBAD/NED BibCode)
ADC_Keywords: Pulsars ; Gamma rays ; X-ray sources
Keywords: stars: winds, outflows - gamma-rays: stars -
pulsars : individual PSR B0833-45 (Vela pulsar) -
acceleration of particles - radiation mechanisms: non-thermal
Abstract:
Pulsar 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 10-12erg/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.
Description:
Spectra from H.E.S.S. and Suzaku XIS observations of three regions in
the Vela X cocoon referred to in the paper as pointing 0 (p0),
pointing 1 (p1), and pointing (p2).
Errors combine statistical and systematic uncertainties of
instrumental origin and from the analysis method.
HESS spectra contain Centre of energy bin (energy, eV), Lower width of
energy bin (energyerrorlo, eV), Higher width of energy bin
(energyerrorhi, eV), Flux (flux, 1/cm2/TeV), Lower flux error
(fluxerrorlo, 1/cm2/TeV) and Higher flux error (fluxerrorhi,
1/cm2/TeV)
Suzaku XIS spectra contain Centre of energy bin (energy, eV), Width of
energy bin (energy_error, eV), Flux (flux, 1/cm2/TeV), and Flux error
(flux_error, 1/cm2/TeV)
Objects:
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RA (2000) DE Designation(s)
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08 33 08.88 -45 11 24.4 Vela X = HESS J0835-455
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 63 6 List of fits spectra
fits/* . 6 Indididual fits spectra
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See also:
J/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)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 deg RAdeg Right Ascension of center (J2000)
8- 13 F6.2 deg DEdeg Declination of center (J2000)
15- 16 I2 --- Nx Number of pixels along X-axis
18 I1 Kibyte size Size of FITS file
20- 30 A11 --- FileName Name of FITS file, in subdirectory fits
32- 63 A32 --- Title Title of the FITS file
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Acknowledgements:
H.E.S.S. Collaboration, contact.hess(at)hess-experiment.eu
(End) H.E.S.S. Collaboration [HESS], Patricia Vannier [CDS] 03-Jun-2019