MAGIC reveals a complex morphology within the unidentified gamma-ray source HESS J1857+026

Aleksić, J.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babić, Ana; Bangale, P.; Almeida, U. Barres de; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bernardini, E.; Biland, A.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Carmona, E.; Carosi, A.; Fidalgo, D.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Vela, P. Da; Dazzi, F.; Angelis, A. De; Caneva, G. De; Lotto, B. De; Mendez, C. Delgado; Doert, M.; Domínguez, A.; Prester, D. Dominis; Dorner, D.; Doro, M.; Einecke, S.; Eisenacher, D.; Elsäesser, D.; Farina, Emanuele Paolo; Ferenc, D.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; López, R. J. García; Garczarczyk, M.; Terrats, D. Garrido; Gaug, M.; Godinović, N.; Muñoz, A. González; Gozzini, S. R.; Hadasch, D.; Hayashida, M.; Herrera, Javier; Herrero, A.; Hildebrand, D.; Hose, J.; Hrupec, Dario; Idec, W.; Kadenius, V.; Kellermann, H.; Klepser, S.; Kodani, K.; Konno, Y.; Krause, J.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lewandowska, N.; Lindfors, E.; Lombardi, S.; López, M.; López-Coto, R.; López-Oramas, Alicia; Lorenz, E.; Lozano, Irene Albarrán; Makariev, M.; Mallot, K.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Marcote, B.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Menzel, U.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Moralejo, A.; Munar-Adrover, P.; Nakajima, D.; Niedźwiecki, A.; Nilsson, K.; Nishijima, K.; Noda, K.; Nowak, N.; Oña-Wilhelmi, E.; Orito, R.; Overkemping, A.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Partini, S.; Peršić, M.; Prada, Francisco; Moroni, P. G. Prada; Prandini, E.; Preziuso, S.; Puljak, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Garcia, J. Rodriguez; Ruegamer, S.; Saggion, A.; Saito, T.; Saito, Koji; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, D.; Spanier, F.; Stamatescu, V.; Stamerra, A.; Steinbring, T.; Storz, J.; Strzys, M.; Sun, S.; Surić, T.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thaele, J.; Tibolla, O.; Torres, D. F.; Toyama, Takeshi; Treves, A.; Uellenbeck, M.; Vogler, P.; Wagner, R. M.; Zandanel, F.; Zanin, R.

doi:10.1051/0004-6361/201423517

Cited by 15 publications

(3 citation statements)

References 35 publications

(47 reference statements)

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“…(Deil et al 2015;Donath et al 2017), and in ongoing surveys by the recently completed HAWC array (Abeysekara et al 2017). Similar sources have also been reported by MILAGRO (Abdo et al 2007), ARGO (Bartoli et al 2013), VERITAS (Weinstein et al 2009) and MAGIC (Aleksić et al 2014). As of August 2017, TeVCat (Wakely & Horan 2008) lists ∼55 sources located within ∼ 10 • of the Galactic Plane with type "unidentified".…”

Section: Hvc Accretion Origin Of High-energymentioning

confidence: 55%

Cosmic Rays and Non-thermal Emission Induced by Accretion of Cool Gas onto the Galactic Disk

Inoue

Uchiyama

Arakawa

et al. 2017

ApJ

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On both observational and theoretical grounds, the disk of our Galaxy should be accreting cool gas with temperature 10 5 K via the halo at a rate ∼ 1 M ⊙ yr −1 . At least some of this accretion is mediated by high velocity clouds (HVCs), observed to be traveling in the halo with velocities of a few 100 km s −1 and occasionally impacting the disk at such velocities, especially in the outer regions of the Galaxy. We address the possibility of particle acceleration in shocks triggered by such HVC accretion events, and the detectability of consequent non-thermal emission in the radio to gamma-ray bands and high-energy neutrinos. For plausible shock velocities ∼ 300 km s −1 and magnetic field strengths ∼ 0.3 − 10 µG, electrons and protons may be accelerated up to ∼ 1 − 10 TeV and ∼ 30 − 10 3 TeV, respectively, in sufficiently strong adiabatic shocks during their lifetime of ∼ 10 6 yr. The resultant pion decay and inverse Compton gamma-rays may be the origin of some unidentified Galactic GeV-TeV sources, particularly the "dark" source HESS J1503-582 that is spatially coincident with anomalous HI structure known as "forbidden-velocity wings". Correlation of their locations with star-forming regions may be weak, absent, or even opposite. Non-thermal radio and X-ray emission from primary and/or secondary electrons may be detectable with deeper observations. The contribution of HVC accretion to Galactic cosmic rays is subdominant, but could be non-negligible in the outer Galaxy. As the thermal emission induced by HVC accretion is likely difficult to detect, observations of such phenomena may offer a unique perspective on probing gas accretion onto the Milky Way and other galaxies.

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Section: Hvc Accretion Origin Of High-energymentioning

confidence: 55%

Cosmic Rays and Non-thermal Emission Induced by Accretion of Cool Gas onto the Galactic Disk

Inoue

Uchiyama

Arakawa

et al. 2017

ApJ

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“…Over 15 sources within this region were discovered by H.E.S.S. Similar surveys within this region have been performed by Milagro (Abdo et al 2007) and ARGO (Bartoli et al 2013b), along with targeted observations by the IACTs VERITAS and MAGIC (for example, Albert et al 2006;Acciari et al 2009;Aleksić et al 2012Aleksić et al , 2014Aliu et al 2014a). At lower energies, the Fermi Large Area Telescope (Fermi-LAT) has published its third source catalog in the 100 MeV-300 GeV energy range (3FGL), based on the first four years of science operation (Acero et al 2015).…”

Section: Introductionmentioning

confidence: 60%

“…Both of the HESS sources were detected as extended, with HESS J1857+026 as the larger of the two. Aleksić et al (2014) reported energy-dependent morphology for HESS J1857+026 with two distinct components, MAGIC J1857.2+0263 and MAGIC J1857.6+0297. These sources cannot be resolved with these data from the partial HAWC array.…”

Section: Source Detectionsmentioning

confidence: 99%

SEARCH FOR TeV GAMMA-RAY EMISSION FROM POINT-LIKE SOURCES IN THE INNER GALACTIC PLANE WITH A PARTIAL CONFIGURATION OF THE HAWC OBSERVATORY

Abeysekara¹,

Alfaro²,

Álvarez³

et al. 2016

ApJ

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Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B

Hampton

Rowell

Hofmann

et al. 2016

Journal of High Energy Astrophysics

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We present the results of our investigation, using a Chandra X-ray observation, into the stellar population of the massive star formation region G5.89-0.39, and its potential connection to the coincident TeV gamma-ray source HESSJ1800-240B. G5.89-0.39 comprises two separate HII regions G5.89-0.39A and G5.89-0.39B (an ultra-compact HII region). We identified 159 individual X-ray point sources in our observation using the source detection algorithm wavdetect. 35 X-ray sources are associated with the HII complex G5.89-0.39. The 35 X-ray sources represent an average unabsorbed luminosity (0.3-10 keV) of ∼ 10 30.5 erg/s, typical of B7-B5 type stars. The potential ionising source of G5.89-0.39B known as Feldt's star is possibly identified in our observation with an unabsorbed X-ray luminosity suggestive of a B7-B5 star. The stacked energy spectra of these sources is well-fitted with a single thermal plasma APEC model with kT∼5 keV, and column density N H = 2.6 × 10 22 cm −2 (A V ∼ 10). The residual (source-subtracted) X-ray emission towards G5.89-0.39A and B is about 30% and 25% larger than their respective stacked source luminosities. Assuming this residual emission is from unresolved stellar sources, the total B-type-equivalent stellar content in G5.89-0.39A and B would be 75 stars, consistent with an earlier estimate of the total stellar mass of hot stars in G5.89-0.39. We have also looked at the variability of the 35 X-ray sources in G5.89-0.39. Ten of these sources are flagged as being variable. Further studies are needed to determine the exact causes of the variability, however the variability could point towards pre-main sequence stars. Such a stellar population could provide sufficient kinetic energy to account for a part of the GeV to TeV gamma-ray emission in the source HESSJ1800-240B. However, future arc-minute angular resolution gamma-ray imaging will be needed to disentangle the potential gamma-ray components powered by G5.89-0.39 from those powered by the W28 SNR.

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MAGIC reveals a complex morphology within the unidentified gamma-ray source HESS J1857+026

Cited by 15 publications

References 35 publications

Cosmic Rays and Non-thermal Emission Induced by Accretion of Cool Gas onto the Galactic Disk

Cosmic Rays and Non-thermal Emission Induced by Accretion of Cool Gas onto the Galactic Disk

SEARCH FOR TeV GAMMA-RAY EMISSION FROM POINT-LIKE SOURCES IN THE INNER GALACTIC PLANE WITH A PARTIAL CONFIGURATION OF THE HAWC OBSERVATORY

Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B

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