The
                    <i>ASCA</i>
                    Catalog of Potential X‐Ray Counterparts of GeV Sources

Roberts, M. S. E.; Romani, Roger W.; Kawai, N.

doi:10.1086/320352

Cited by 90 publications

(111 citation statements)

References 42 publications

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“…The radio-quiet pulsar PSR J1826−1256 (P2), which powers the diffuse X-ray nebula PWN G018.5−0.4 (Roberts, Romani & Kawai 2001;Roberts et al 2007), may also be a candidate for the origin of HESS J1826−130. The distance d = 1.2 − 1.4 kpc suggested by Wang (2011) infers a TeV γ-ray efficiency ηγ ∼ 2 × 10 −4 which is at the lower end of typical ηγ values forĖSD ∼ 10 36−37 erg s −1 (Kargaltsev, Rangelov & Pavlov 2013).…”

Section: Other Potential Particle Acceleratorsmentioning

confidence: 99%

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

Voisin¹,

Rowell²,

Burton³

et al. 2016

Mon. Not. R. Astron. Soc.

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HESS J1825−137 is a pulsar wind nebula (PWN) whose TeV emission extends across ∼ 1 deg. Its large asymmetric shape indicates that its progenitor supernova interacted with a molecular cloud located in the north of the PWN as detected by previous CO Galactic survey (e.g Lemiere, Terrier & Djannati-Ataï 2006).Here we provide a detailed picture of the ISM towards the region north of HESS J1825−137, with the analysis of the dense molecular gas from our 7mm and 12mm Mopra survey and the more diffuse molecular gas from the Nanten CO(1-0) and GRS 13 CO(1-0) surveys. Our focus is the possible association between HESS J1825−137 and the unidentified TeV source to the north, HESS J1826−130. We report several dense molecular regions whose kinematic distance matched the dispersion measured distance of the pulsar. Among them, the dense molecular gas located at (RA, Dec)=(18.421h,−13.282 • ) shows enhanced turbulence and we suggest that the velocity structure in this region may be explained by a cloud-cloud collision scenario.Furthermore, the presence of a Hα rim may be the first evidence of the progenitor SNR of the pulsar PSR J1826-1334 as the distance between the Hα rim and the TeV source matched with the predicted SNR radius R SNR ∼ 120 pc.From our ISM study, we identify a few plausible origins of the HESS J1826−130 emission, including the progenitor SNR of PSR J1826−1334 and the PWN G018.5−0.4 powered by PSR J1826−1256. A deeper TeV study however, is required to fully identify the origin of this mysterious TeV source.Key words: molecular data -pulsars: individual: PSR J1826−1334 -ISM: cloudscosmic-rays -gamma-rays: ISM. INTRODUCTIONHESS J1825−137 is one of the brightest and most extensive pulsar wind nebulae (PWNe) detected in TeV γ-rays (Aharonian et al. 2006). It is powered by the high spin-down power (ĖSD = 2.8 × 10 36 erg/s) pulsar PSR J1826−1334 with a dispersion measure distance of 3.9±0.4 kpc and characteristic age τc ∼ 20 kyr.PWNe represent a significant fraction of the Galactic TeV γ-ray source population. They convert a varying fraction of their pulsars' spin down energyĖSD into high energy E-mail:fabien.voisin@adelaide.edu.au (AVR); fabien.voisin@adelaide.edu.au (ANO) electrons. The electron flow is temporally randomized and re-accelerated at a termination shock resulting from pressure from the surrounding interstellar medium (ISM). InverseCompton (IC) up-scattering of soft photons then leads to TeV γ-rays, and associated synchrotron radio to X-ray emission.The morphology of PWNe can be heavily influenced by the ISM. The interaction of the progenitor supernova shock with adjacent molecular clouds can lead to a reverse shock propagating back into the PWN (Blondin, Chevalier & Frierson 2001), giving rise to an asymmetry in the radio, X-ray and γ-ray emission that can trail away from the pulsar along the pulsar-molecular cloud axis.HESS J1825−137 is an excellent example of this situa- Lemiere, Terrier & Djannati-Ataï (2006), with the bulk of the TeV γ-ray extending up to a degree south of the pulsar. In...

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Section: Other Potential Particle Acceleratorsmentioning

confidence: 99%

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

Voisin¹,

Rowell²,

Burton³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Another suggested possibility has been that of a point- [42]), and Cygnus X-3. The center of gravity with statistical errors and intrinsic size (standard deviation of a 2-dim Gaussian, σsrc) are indicated by the white cross and white circle, respectively.…”

Section: Tev J2032+4130mentioning

confidence: 99%

TeVγrays and neutrinos from photodisintegration of nuclei in Cygnus OB2

et al. 2007

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TeV γ-rays may provide significant information about high energy astrophysical accelerators. Such γ-rays can result from the photo-de-excitation of PeV nuclei after their parents have undergone photo-disintegration in an environment of ultraviolet photons. This process is proposed as a candidate explanation of the recently discovered HEGRA source at the edge of the Cygnus OB2 association. The Lyman-α background is provided by the rich O and B stellar environment. It is found that (1) the HEGRA flux can be obtained if there is efficient acceleration at the source of lower energy nuclei; (2) the requirement that the Lorentz-boosted ultraviolet photons can excite the Giant Dipole Resonance implies a strong suppression of the γ-ray spectrum compared to an E −2 γ behavior at energies 1 TeV (some of these energies will be probed by the upcoming GLAST mission); (3) a TeV neutrino counterpart from neutron decay following helium photo-disintegration will be observed at IceCube only if a major proportion of the kinetic energy budget of the Cygnus OB2 association is expended in accelerating nuclei.

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“…The source with the highest V 12 value in the Galactic plane without a potential Blazar identification is GeV J1809−2327. An X-ray nebulae was discovered in its error box with ASCA (Roberts et al, 2001) which subsequent Chandra and VLA imaging showed to be a RPWN (Braje et al, 2002). An XMM-Newton EPIC-PN observation, which was unfortunately taken in small window mode, suggests a fainter X-ray halo surrounding the X-ray trail seen in the short Chandra exposure, strongly reminiscent of the Mouse (Fig.…”

Section: Rapidly Moving Pulsar Wind Nebulae Associated Withmentioning

confidence: 99%

Pulsar Wind Nebulae in Egret Error Boxes

Roberts

Brogan

Gaensler

et al. 2005

Astrophys Space Sci

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Abstract. A remarkable number of pulsar wind nebulae (PWN) are coincident with EGRET γ-ray sources. X-ray and radio imaging studies of unidentified EGRET sources have resulted in the discovery of at least 6 new pulsar wind nebulae (PWN). Stationary PWN (SPWN) appear to be associated with steady EGRET sources with hard spectra, typical for γ-ray pulsars. Their toroidal morphologies can help determine the geometry of the pulsar which is useful for constraining models of pulsed γ-ray emission. Rapidly moving PWN (RPWN) with more cometary morphologies seem to be associated with variable EGRET sources in regions where the ambient medium is dense compared to what is typical for the ISM.

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The ASCA Catalog of Potential X‐Ray Counterparts of GeV Sources

Cited by 90 publications

References 42 publications

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

TeVγrays and neutrinos from photodisintegration of nuclei in Cygnus OB2

Pulsar Wind Nebulae in Egret Error Boxes

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