Fermi/Lat Study of Gamma-Ray Emission in the Direction of the Monoceros Loop Supernova Remnant

Sugiyama, S.; Ackermann, M.; Ballet, J.; Casandjian, J. M.; Hanabata, Y.; Hewitt, J. W.; Kerr, M.; Kubo, H.; Lemoine‐Goumard, M.; Ray, Paul S.

doi:10.3847/0004-637x/831/1/106

Cited by 14 publications

(14 citation statements)

References 33 publications

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“…Sizes of the red circles are enlarged to two times with respect to their angular sizes (1 ′ -2 ′ ). The large white circle indicates the best-fit Gaussian spatial model from F ERM I/LAT observations after subtracting the background and the emission from the Rosette Nebula (Katagiri et al 2016), while the two little white circles show the 2FGL sources of J0636.0+0554 and J0637.8+0737 (Nolan et al 2012). • 941)) and width of 4.…”

Section: Discussionmentioning

confidence: 99%

“…On the other hand, 2FGL sources of J0636.0+0554 and J0637.8+0737 (Nolan et al 2012) are located close to the molecular gas revealed by our new CO survey (two little circles in Figure 9). Very recently, extended gamma-ray emission from F ERMI/LAT observations was found inside the remnant (see Figures 3 and 4 in Katagiri et al 2016). According to our study, the MC concentration in the velocity intervals of 3-12 km s −1 and 18-23 km s −1 , which is shown to be associated with the remnant, is consistent well with the distribution of the backgroundsubtracted gamma-ray emission.…”

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

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Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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We present CO observations toward three large supernova remnants (SNRs) in the third Galactic quadrant using the Purple Mountain Observatory Delingha 13.7 m millimeter-wavelength telescope. The observations are part of the high-resolution CO survey of the Galactic plane between Galactic longitudes l = −10• to 250• and latitudes b = −5• to 5• . CO emission was detected toward the three SNRs: G205.5+0.5 (Monoceros Nebula), G206.9+2.3 (PKS 0646+06), and G213.0−0.6. Both of SNRs G205.5+0.5 and G213.0−0.6 exhibit the morphological agreement (or spatial correspondences) between the remnant and the surrounding molecular clouds (MCs), as well as kinematic signatures of shock perturbation in the molecular gas. We confirm that the two SNRs are physically associated with their ambient MCs and the shock of SNRs is interacting with the dense, clumpy molecular gas. SNR G206.9+2.3, which is close to the northeastern edge of the Monoceros Nebula, displays the spatial coincidence with molecular partial shell structures at V LSR ∼ 15 km s −1 . While no significant line broadening has been detected within or near the remnant, the strong morphological correspondence between the SNR and the molecular cavity implies that SNR G206.9+2.3 is probably associated with the CO gas and is evolving in the low-density environment. The physical features of individual SNRs, together with the relationship between SNRs and their nearby objects, are also discussed.

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Section: Discussionmentioning

confidence: 99%

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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“…HESS J0632+057 is located in a complicated region. Within 3 • of its location, there are several gamma-ray point sources from the preliminary seven-year source list, the Monoceros Loop Supernova Remnant, and the Rosette Nebula, which are both known to be extended gammaray sources (Katagiri et al 2016). Located ∼1 • away from the source of interest, there is PSR J0633+0632, a bright, radio-quiet gamma-ray pulsar discovered in the first six months of Fermi-LAT observations (Abdo et al 2009d).…”

Section: Gating Off the Bright Gamma-ray Pulsar Psr J0633+0632mentioning

confidence: 99%

GeV Detection of HESS J0632+057

Torres

Cheng

et al. 2017

ApJ

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HESS J0632+057 is the only gamma-ray binary that has been detected at TeV energies, but not at GeV energies yet. Based on nearly nine years of Fermi Large Area Telescope (LAT) Pass 8 data, we report here on a deep search for the gammaray emission from HESS J0632+057 in the 0.1-300 GeV energy range. We find a previously unknown gamma-ray source, Fermi J0632.6+0548, spatially coincident with HESS J0632+057. The measured flux of Fermi J0632.6+0548 is consistent with the previous flux upper limit on HESS J0632+057 and shows variability that can be related to the HESS J0632+057 orbital phase. We propose that Fermi J0632.6+0548 is the GeV counterpart of HESS J0632+057. Considering the Very High Energy (VHE) spectrum of HESS J0632+057, a possible spectral turnover above 10 GeV may exist in Fermi J0632.6+0548, as appears to be common in other established gamma-ray binaries.

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“…So, from the observational point of view, one must distinguish between "direct" clues to investigate the acceleration processes (e.g., radio observations), and "indirect" ones, i.e., those necessitating a target to be revealed such as molecular clouds for relativistic protons (Abdo et al 2010;Acciari et al 2009;Katsuta et al 2012;Katagiri et al 2016;Tavani et al 2010), or radiation from interstellar dust for electrons.…”

Section: Introductionmentioning

confidence: 99%

Runaway O-star Bow Shocks as Particle Accelerators? The Case of AE Aur Revisited

Rangelov

Montmerle

Federman

et al. 2019

ApJ

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We present results of our Chandra/ACIS observations of the field centered on the fast, runaway O star AE Aur and its bow shock. Previous XMM-Newton observations revealed an X-ray "blob" near the IR arc tracing the bow shock, possibly a nonthermal source consistent with models of Inverse Compton scattering of dust IR photons by electrons accelerated at the shock. The new, subarcsecond resolution Chandra data, while confirming the presence of the XMM-Newton source, clearly indicate that the latter is neither extended nor coincident with the IR arc and strongly suggest it is a background AGN. Motivated by results published for the bow shock of BD+43 • 3654, we extended our study to the radio domain, by analyzing archival EVLA data. We find no radio emission from the AE Aur bow shock either. The corresponding upper limits for the absorbed (unabsorbed) X-ray flux of 5.9(7.8) × 10 −15 erg cm −2 s −1 (3σ) and, in the radio range, of 2 mJy (1.4 GHz), and 0.4 mJy (5.0 GHz), are used to put constraints on model predictions for particle acceleration within the bow shock. In the "classical" framework of Diffusive Shock Acceleration, we find that the predicted X-ray and radio emission by the bow shock is at least two orders of magnitude below the current upper limits, consistent with the systematic non-detections of up to 60 stellar bow shocks. The only exception so far remains that of BD+43 • 3654, probably the result of its very large mass-loss rate among runaway O stars.

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Fermi/Lat Study of Gamma-Ray Emission in the Direction of the Monoceros Loop Supernova Remnant

Cited by 14 publications

References 33 publications

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

GeV Detection of HESS J0632+057

Runaway O-star Bow Shocks as Particle Accelerators? The Case of AE Aur Revisited

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