Molecular Gas Distribution around the Supernova Remnant G40.5–0.5

Yang, Ji; Zhang, Jie-Long; Cai, Zhi-Yong; Lu, Dong-Fei; Tan, Y. H.

doi:10.1088/1009-9271/6/2/8

Cited by 23 publications

(26 citation statements)

References 32 publications

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“…A scenario consisting of a SNR-molecular cloud association, such as that possibly at work for SNR W 28 (Aharonian et al 2008b) where the γ-rays are produced through interactions of accelerated cosmic rays with molecular matter in the vicinity of the source, along with the contribution of a nearby unresolved source to the south-west could lead to such a difference in angular extension. However, the dense region reported by Yang et al (2006) is located north of the SNR and does not correspond to the observed γ-ray emission.…”

Section: Search For Counterpartsmentioning

confidence: 71%

“…Downes et al (1980), using various Σ−D relations derived a linear diameter of 40-65 pc, an age of (2-4) ×10 4 yr, and estimated the distance to the SNR to be in the range 5.5 to 8.5 kpc, corresponding to a location either in the inter-arm region between the Scutum and the Sagittarius arms, or on the inner edge of the latter. Yang et al (2006) investigated the distribution of molecular gas around the SNR direction through the 12 CO (J = 1-0) transition line, and provided evidence for interaction between the SNR and its neighboring dense ISM at a central velocity V LSR = 55 km s −1 . The corresponding kinematic distance of 3-3.4 kpc implied a source diameter of 25 pc and a younger age, at variance with the initial estimates of Downes et al (1980).…”

Section: Search For Counterpartsmentioning

confidence: 99%

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Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Aharonian

Akhperjanian

Anton

et al. 2009

A&A

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Aims. Detection of a γ-ray source above 300 GeV is reported, confirming the unidentified source MGRO J1908+06, discovered by the Milagro collaboration at a median energy of 20 TeV. Methods. The source was observed during 27 h as part of the extension of the HESS Galactic plane survey to longitudes >30• . Results. HESS J1908+063 is detected at a significance level of 10.9σ with an integral flux above 1 TeV of (3.76 ± 0.29 stat ± 0.75 sys ) × 10 −12 ph cm −2 s −1 , and a spectral photon index Γ = 2.10 ± 0.07 stat ± 0.2 sys . The positions and fluxes of HESS J1908+063 and MGRO J1908+06 are in good agreement. Possible counterparts at other wavelengths and the origin of the γ-ray emission are discussed. The nearby unidentified GeV source, GRO J1908+0556 (GeV) which also remains unidentified and the new Fermi pulsar 0FGL J1907.5+0617, may be connected to the TeV source.

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Section: Search For Counterpartsmentioning

confidence: 71%

Section: Search For Counterpartsmentioning

confidence: 99%

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Aharonian

Akhperjanian

Anton

et al. 2009

A&A

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“…The pulsar may also be associated with the SNR G40.5-0.5 [8]. The estimated age (20-40 kyr [9]) and distance (3.6 kpc [10]) of the SNR are consistent with those of the pulsar. However, if the pulsar originated at the center of the SNR, its characteristic age would imply a transverse velocity of ∼1400 km s −1 .…”

Section: Introductionmentioning

confidence: 66%

Investigating the X-ray emission from the Galactic TeV Gamma-ray Source MGRO J1908+06

Pandel¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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MGRO J1908+06 is a bright, extended TeV gamma-ray source located near the Galactic plane. The TeV emission has previously been attributed to the pulsar wind nebula of the radio-faint gamma-ray pulsar PSR J1907+0602 discovered with Fermi. However, studies of the TeV morphology with VERITAS have shown that MGRO J1908+06 is somewhat larger than other pulsar wind nebulae of similar age and that the TeV spectrum does not soften with distance from the pulsar as is observed for other pulsar wind nebulae. Although MGRO J1908+06 is very bright in gamma rays with a flux corresponding to ∼80% of the Crab Nebula flux at 20 TeV, no extended emission at other energies has so far been detected. We report on our analysis of X-ray data obtained with XMM-Newton of the region near MGRO J1908+06. We searched the data for point-like sources and detected several hard-spectrum X-ray sources that could be associated with the TeV emission, including the gamma-ray pulsar PSR J1907+0602. We also performed an extended source analysis to search for diffuse emission from MGRO J1908+06 but found no evidence of diffuse X-ray emission coincident with the TeV source. We place an upper limit of 8.7 × 10 33 erg s −1 on the X-ray luminosity of MGRO J1908+06 in the 1-10 keV energy range. The corresponding limit on the ratio of gamma-ray to X-ray luminosity is consistent with the ratios found for other pulsar wind nebulae of similar age.

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“…The small light blue line is the Milagro significance contour of the significance level σ = 8, and the large white line that encloses the entire region is the Milagro significance contour of σ = 5. The dashed ellipse shows SNR G40.5-0.5, following Yang et al (2006). Its center is positioned at (RA, Dec)=(19:07:08.6, +06:29:53.0) (Abdo et al, 2010b), its size is 28'×24' (=25 pc) (Yang et al, 2006), and the angle of major axis in galactic coordinates is 31 • .…”

Section: Pulsar Wind Nebulamentioning

confidence: 99%

“…The dashed ellipse shows SNR G40.5-0.5, following Yang et al (2006). Its center is positioned at (RA, Dec)=(19:07:08.6, +06:29:53.0) (Abdo et al, 2010b), its size is 28'×24' (=25 pc) (Yang et al, 2006), and the angle of major axis in galactic coordinates is 31 • . The light blue arrow inside a circle on the lower left corner indicates North for RA/Dec.…”

Section: Pulsar Wind Nebulamentioning

confidence: 99%

VERITAS observations of galactic gamma-ray sources

Tsurusaki¹

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The main topic of this thesis is analysis of an unidentified Galactic TeV gammaray source, MGRO J1908+06, discovered by Milagro instrument in 2007. We analyzed 54 hours of observational data from the Very Energetic Radiation Imaging Telescope Array System (VERITAS), a ground-based gamma-ray observatory in southern Arizona comprised of an array of four Cherenkov Telescopes that reconstructs the energy and direction of astrophysical gamma-rays by imaging Cherenkov light emitted by energetic particles in air showers produced by the primary gamma-rays. MGRO J1908+06 is located between a supernova remnant SNR G40.5-0.5 and a young, energetic pulsar PSR J1907+0602. We studied the energy dependent morphology of the TeV emission from the source and measured the source extent and spectrum. The source extends well past the boundary of the SNR and is not correlated with strong radio continuum or molecular line emission which likely excludes an origin for the emission as solely due to the SNR. While emission in the 0.5-1.25 TeV band was centered around the pulsar, higher energy emission was observed near the supernova remnant. This morphology is opposite that observed in other pulsar wind nebulae. We proposed two models for the high energy emission located well away from the pulsar but close to the SNR: (1) shock acceleration at the shock front created by an interaction between the pulsar wind and the dense gas at the edge of the SNR or (2) molecular clouds around the SNR provides seed photons with energies higher than those from Cosmic Microwave Backgrounds for inverse Compton scattering. The former model can be tested by looking for molecular emission lines that trace shocks and by measuring the pulsar velocity. In addition, we investigated the gamma-ray emission from the nova explosion of V407 Cygni that occurred in March 2010. The Fermi-LAT observed this event in the energy range of E >100 MeV. The origins of the gamma-ray emission that the Fermi-LAT team proposed are either protons (hadronic model) or electrons (leptonic Allured, Thomas Brantseg, Casey DeRoo and Scott Griffiths. Lastly, I would like to express my special thanks to my family in Japan for their never ending encouragement and support.

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Molecular Gas Distribution around the Supernova Remnant G40.5–0.5

Cited by 23 publications

References 32 publications

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Investigating the X-ray emission from the Galactic TeV Gamma-ray Source MGRO J1908+06

VERITAS observations of galactic gamma-ray sources

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