A Study of the Interstellar Medium Towards the Unidentified Dark TeV γ-Ray Sources HESS J1614–518 and HESS J1616–508

Lau, J.; Rowell, G.; Voisin, F.; Braiding, Catherine; Burton, M. G.; Fukui, Y.; Pointon, Stephanie K.; Ashley, M. C. B.; Jordan, C.; Walsh, A. J.

doi:10.1017/pasa.2017.59

Cited by 7 publications

(7 citation statements)

References 69 publications

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“…The values inferred were in the range of 100-1 000 times the Solar value (Lau et al 2017b). Similarly, CO and CS observations that identify filamentary molecular features towards the unidentified objects HESS J1614−518 and HESS J1616−508 (Lau et al 2017a) represent the first steps in forming an understanding of the nature of gamma-ray emitters. Maxted et al (2018) compared line of sight column densities from Mopra CO and the SGPS H I emission to X-ray absorption column densities for the bright shell-type gammaray SNR, HESS J1731−347.…”

Section: Gamma-ray Observationsmentioning

confidence: 68%

The Mopra Southern Galactic Plane CO Survey—Data Release 3

Braiding

Wong

Maxted

et al. 2018

Publ. Astron. Soc. Aust.

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We present observations of fifty square degrees of the Mopra carbon monoxide (CO) survey of the Southern Galactic Plane, covering Galactic longitudes l = 300-350 • and latitudes |b| ≤ 0.5 • . These data have been taken at 0.6 arcminute spatial resolution and 0.1 km s −1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the Southern Galactic Plane in the 109-115 GHz J = 1-0 transitions of 12 CO, 13 CO, C 18 O and C 17 O.We present a series of velocity-integrated maps, spectra and position-velocity plots that illustrate Galactic arm structures and trace masses on the order of ∼10 6 M per square degree; and include a preliminary catalogue of C 18 O clumps located between l = 330-340 • . Together with information about the noise statistics of the survey these data can be retrieved from the Mopra CO website, the PASA data store and the Harvard Dataverse.

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Section: Gamma-ray Observationsmentioning

confidence: 68%

The Mopra Southern Galactic Plane CO Survey—Data Release 3

Braiding

Wong

Maxted

et al. 2018

Publ. Astron. Soc. Aust.

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“…Detailed studies at radio wavelengths were conducted by Lau et al [75] using results from the Mopra Southern Galactic Plane CO Survey, the Millimetre Astronomer's Legacy Team-45 GHz survey, the HEAT telescope, and HI archival data from the Southern Galactic Plane Survey. They did not find any conclusive evidence to link HESS J1616-508 to any known counterparts, and considered an association with the two SNRs or a PWN powered by the young energetic pulsar PSR J1617-5055 to be unlikely.…”

Section: Hess J1616-508mentioning

confidence: 99%

“…However, the killer blow to this scenario is provided by the flux of the X-ray PWN powered by PSR J1617-5055, which represents a crucial constraint. If PSR J1617-5055 powers the TeV PWN, i.e., HESS J1616-508, as well, there should be high flux at radio energies, and no such flux has been detected [75,77].…”

Section: Hess J1616-508mentioning

confidence: 99%

Pulsar Wind Nebulae and Unidentified Galactic Very High Energy Sources

Tibolla

Kaufmann

Chadwick

2022

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The riddle of the origin of Cosmic Rays (CR) has been an open question for over a century. Gamma ray observations above 100 MeV reveal the sites of cosmic ray acceleration to energies where they are unaffected by solar modulation; recent evidence supports the existence of hadronic acceleration in Supernova Remnants (SNR), as expected in the standard model of cosmic ray acceleration. Nevertheless, the results raise new questions, and no final answer has been provided thus far. Among the suggested possible alternative accelerators in the Very High Energy (VHE) gamma ray sky, pulsar wind nebulae (PWNe, which together with dark matter are the main candidates to explain the local positron excess as well) are the dominant population among known Galactic sources. However, the most numerous population in absolute terms is represented by unidentified sources (~50% of VHE gamma ray sources). The relationship between PWNe and unidentified sources seems very close; in fact, in a PWN, the lifetime of inverse Compton (IC) emitting electrons not only exceeds the lifetime of its progenitor pulsar, but also exceeds the age of the electrons that emit via synchrotron radiation. Therefore, during its evolution, a PWN can remain bright in IC such that its GeV-TeV gamma ray flux remains high for timescales much larger than the lifetimes of the pulsar and the X-ray PWN. In addition, the shell-type remnant of the supernova explosion in which the pulsar was formed has a much shorter lifetime than the electrons responsible for IC emission. Hence, understanding PWNe and VHE unidentified sources is a crucial piece of the solution to the riddle of the origin of cosmic rays. Both theoretical aspects (with particular emphasis on the ancient pulsar wind nebulae scenario) and their observational proofs are discussed in this paper. Specifically, the scientific cases of HESS J1616-508 and HESS J1813-126 are examined in detail.

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“…However, since there is no strong and convincing evidence linking other sources in the field (SNR, star cluster, etc.) to HESS J1616−508 [33,34], we consider this association to be valid for further consideration.…”

Section: Soft γ-Ray Pulsars/pwn With Tev Emissionmentioning

confidence: 99%

INTEGRAL View of TeV Sources: A Legacy for the CTA Project

et al. 2021

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Investigations that were carried out over the last two decades with novel and more sensitive instrumentation have dramatically improved our knowledge of the more violent physical processes taking place in galactic and extra-galactic Black-Holes, Neutron Stars, Supernova Remnants/Pulsar Wind Nebulae, and other regions of the Universe where relativistic acceleration processes are in place. In particular, simultaneous and/or combined observations with γ-ray satellites and ground based high-energy telescopes, have clarified the scenario of the mechanisms responsible for high energy photon emission by leptonic and hadronic accelerated particles in the presence of magnetic fields. Specifically, the European Space Agency INTEGRAL soft γ-ray observatory has detected more than 1000 sources in the soft γ-ray band, providing accurate positions, light curves and time resolved spectral data for them. Space observations with Fermi-LAT and observations that were carried out from the ground with H.E.S.S., MAGIC, VERITAS,and other telescopes sensitive in the GeV-TeV domain have, at the same time, provided evidence that a substantial fraction of the cosmic sources detected are emitting in the keV to TeV band via Synchrotron-Inverse Compton processes, in particular from stellar galactic BH systems as well as from distant black holes. In this work, employing a spatial cross correlation technique, we compare the INTEGRAL/IBIS and TeV all-sky data in search of secure or likely associations. Although this analysis is based on a subset of the INTEGRAL all-sky observations (1000 orbits), we find that there is a significant correlation: 39 objects (∼20% of the VHE γ-ray catalogue) show emission in both soft γ-ray and TeV wavebands. The full INTEGRAL database, now comprising almost 19 years of public data available, will represent an important legacy that will be useful for the Cherenkov Telescope Array (CTA) and other ground based large projects.

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A Study of the Interstellar Medium Towards the Unidentified Dark TeV γ-Ray Sources HESS J1614–518 and HESS J1616–508

Cited by 7 publications

References 69 publications

The Mopra Southern Galactic Plane CO Survey—Data Release 3

The Mopra Southern Galactic Plane CO Survey—Data Release 3

Pulsar Wind Nebulae and Unidentified Galactic Very High Energy Sources

INTEGRAL View of TeV Sources: A Legacy for the CTA Project

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