Publisher’s Note: HESS Observations of the Galactic Center Region and Their Possible Dark Matter Interpretation [Phys. Rev. Lett.<b>97</b>, 221102 (2006)]

Aharonian, F.; Akhperjanian, A. G.; Bazer‐Bachi, A. R.; Beilicke, M.; Benbow, W.; Berge, D.; Bernlöhr, K.; Boisson, C.; Bolz, O.; Borrel, V.; Braun, I.; Breitling, F.; Brown, A. M.; Bühler, R.; Büsching, I.; Carrigan, S.; Chadwick, P. M.; Chounet, L.‐M.; Cornils, R.; Costamante, L.; Degrange, B.; Dickinson, H. J.; Djannati‐Ataï, A.; Drury, L. O’c.; Dubus, G.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Feinstein, F.; Ferrero, E.; Fiaßon, A.; Fontaine, G.; Funk, Sebastian; Gallant, Y. A.; Giebels, B.; Glicenstein, J. F.; Goret, P.; Hadjichristidis, C.; Hauser, D.; Hauser, M. G.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Holleran, M.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Khélifi, B.; Komin, Nu.; Konopelko, A.; Kosack, K.; Latham, I. J.; Gallou, R. Le; Lemière, A.; Lemoine‐Goumard, M.; Löhse, T.; Martin, J. M.; Martineau‐Huynh, O.; Marcowith, A.; Masterson, C.; McComb, T. J. L.; Naurois, M. de; Nedbal, D.; Nolan, S. J.; Noutsos, A.; Orford, K. J.; Osborne, J. L.; Ouchrif, M.; Panter, M.; Pelletier, G.; Pita, S.; Pühlhofer, G.; Punch, M.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Reimer, A.; Reimer, O.; Ripken, J.; Rob, L.; Rolland, L.; Rowell, G.; Sahakian, V.; Saugé, L.; Schlenker, S.; Schlickeiser, R.; Schwanke, U.; Sol, H.; Spangler, D.; Spanier, F.; Steenkamp, R.; Stegmann, C.; Superina, G.; Tavernet, J.‐P.; Terrier, R.; Théoret, C. G.; Tluczykont, M.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Vincent, P.; Völk, H. J.; Wagner, S. J.; Ward, M.

doi:10.1103/physrevlett.97.249901

Cited by 83 publications

(94 citation statements)

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“…The bestfitting probability is 12 per cent. The best-fitting position is, within 8 ± 9 stat ± 9 sys , coincident with the position of Sgr A * and fully compatible with the position reported from the 2004 data set (Aharonian et al 2006b). Changing the background subtraction technique, the image binning or the fit boundaries did not affect the position by more than 2 arcsec.…”

Section: P O S I T I O N O F H E S S J 1 7 5 −2 9supporting

confidence: 85%

“…As shown with deep observations in 2004, HESS J1745−290 is a point source for H.E.S.S. (rms spatial extension of <1.2 arcmin at 95 per cent CL) and is within 7 ± 14 stat ± 28 sys , positionally coincident with the bright radio source Sgr A * (Aharonian et al 2006b). The measured energy spectrum does not fit dark matter (DM) model spectra -at least for the most popular models of DM annihilation -ruling out the fact that the bulk of the TeV emission can solely be of a DM origin (Aharonian et al 2006b).…”

Section: Vhe γ -R Ay S F Ro M T H E G a L Ac T I C C E N T R Esupporting

confidence: 62%

“…In this paper, a refined measurement of HESS J1745−290's emission centroid is reported. Using improved telescope pointing control, the systematic error of the measurement is decreased by a factor of 3 compared to previous results, and the total error on the centroid position is reduced to 13 arcsec (68 per cent containment radius) compared to 34 arcsec in Aharonian et al (2006b).…”

Section: Vhe γ -R Ay S F Ro M T H E G a L Ac T I C C E N T R Ementioning

confidence: 67%

“…In a circular region of 0. • 1 around the centroid position, this background is at a level of ≈15 per cent of the total flux observed from the source (Aharonian et al 2006b(Aharonian et al , 2009). In the position determination, the background γ -ray diffuse emission was therefore taken into account by adding an independent term in the fit function with free normalization.…”

Section: P O S I T I O N O F H E S S J 1 7 5 −2 9mentioning

confidence: 99%

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Localizing the VHE γ-ray source at the Galactic Centre

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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The inner 10 pc of our Galaxy contains many counterpart candidates of the very high energy (VHE; >100 GeV) γ-ray point source HESS J1745−290. Within the point spread function of the H.E.S.S. measurement, at least three objects are capable of accelerating particles to VHE and beyond and of providing the observed γ-ray flux. Previous attempts to address this source confusion were hampered by the fact that the projected distances between these objects were of the order of the error circle radius of the emission centroid (34 arcsec, dominated by the pointing uncertainty of the H.E.S.S. instrument). Here we present H.E.S.S. data of the Galactic Centre region, recorded with an improved control of the instrument pointing compared to H.E.S.S. standard pointing procedures. Stars observed during γ-ray observations by optical guiding cameras mounted on each H.E.S.S. telescope are used for off-line pointing calibration, thereby decreasing the systematic pointing uncertainties from 20 to 6 arcsec per axis. The position of HESS J1745−290 is obtained by fitting a multi-Gaussian profile to the background-subtracted γ-ray count map. A spatial comparison of the best-fitting position of HESS J1745−290 with the position and morphology of candidate counterparts is performed. The position is, within a total error circle radius of 13 arcsec, coincident with the position of the supermassive black hole Sgr A* and the recently discovered pulsar wind nebula candidate G359.95−0.04. It is significantly displaced from the centroid of the supernova remnant Sgr A East, excluding this object with high probability as the dominant source of the VHE γ-ray emission

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Section: P O S I T I O N O F H E S S J 1 7 5 −2 9supporting

confidence: 85%

Section: Vhe γ -R Ay S F Ro M T H E G a L Ac T I C C E N T R Esupporting

confidence: 62%

Section: Vhe γ -R Ay S F Ro M T H E G a L Ac T I C C E N T R Ementioning

confidence: 67%

Section: P O S I T I O N O F H E S S J 1 7 5 −2 9mentioning

confidence: 99%

See 2 more Smart Citations

Localizing the VHE γ-ray source at the Galactic Centre

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

Monthly Notices of the Royal Astronomical Society

Self Cite

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show abstract

“…For comparison, we also show the exclusion plot obtained by the observation of the GC with the HESS telescope. HESS has extensively observed the GCsource, measuring an integrated flux above 160 GeV of (>160 TeV) = 1.87 × 10 −11 ph cm −2 s −1 in 2003 and 2004 (Aharonian et al 2006).…”

Section: O M Pa R I S O N W I T H T H E E X P E R I M E N Ta L Datamentioning

confidence: 99%

Constraining the dark matter annihilation cross-section with Cherenkov telescope observations of dwarf galaxies

Pieri

Lattanzi

Silk

2009

Monthly Notices of the Royal Astronomical Society

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The presence of dark matter in the halo of our Galaxy could be revealed through indirect detection of its annihilation products. Dark matter annihilation is one possible interpretation of the recently measured excesses in positron and electron fluxes, provided that boost factors of the order of 103 or more are taken into account. Such boost factors are actually achievable through the velocity‐dependent Sommerfeld enhancement of the annihilation cross‐section. Here, we study the expected γ‐ray flux from two local dwarf galaxies for which Cherenkov telescope measurements are available, namely Draco and Sagittarius. We use recent stellar kinematical measurements to model the dark matter haloes of the dwarfs and the results of numerical simulations to model the presence of an associated population of subhaloes. We incorporate the Sommerfeld enhancement of the annihilation cross‐section. We compare our predictions with the observations of Draco and Sagittarius performed by MAGIC and HESS, respectively, and derive exclusion limits on the effective annihilation cross‐section. We also study the sensitivities of Fermi and of the future Cherenkov telescope array to cross‐section enhancements. We find that the boost factor due to the Sommerfeld enhancement is already constrained by the MAGIC and HESS data, with enhancements greater than ∼104 being excluded.

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Dark matter evidence, particle physics candidates and detection methods

Bergström¹

2012

Annalen der Physik

173

177

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The problem of the dark matter in the universe is reviewed. A short history of the subject is given, and several of the most obvious particle candidates for dark matter are identified. Particular focus is given to weakly interacting, massive particles (WIMPs) of which the lightest supersymmetric particle is an interesting special case and a useful template. The three detection methods: in particle accelerators, by direct detections of scattering in terrestrial detectors, and indirect detection of products from dark matter particle annihilation in the galactic halo, are discussed and their complementarity is explained. Direct detection experiments have revealed some possible indications of a dark matter signal, but the situation is quite confusing at the moment. Very recently, also indirect detection has entered a sensitivity region where some particle candidates could be detectable. Indeed, also here there are some (presently non‐conclusive) indications of possible dark matter signals, like an interesting structure at 130 GeV γ‐ray energy found in publicly available data from the Fermi‐LAT space detector. The future of the field will depend on whether WIMPs are indeed the dark matter, something that may realistically be probed in the next few years. If this exciting scenario turns out to be true, we can expect a host of other, complementary experiments in the coming decade. If it is not true, the time scale and methods for detection will be much more uncertain.

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Publisher’s Note: HESS Observations of the Galactic Center Region and Their Possible Dark Matter Interpretation [Phys. Rev. Lett.97, 221102 (2006)]

Cited by 83 publications

References 0 publications

Localizing the VHE γ-ray source at the Galactic Centre

Localizing the VHE γ-ray source at the Galactic Centre

Constraining the dark matter annihilation cross-section with Cherenkov telescope observations of dwarf galaxies

Dark matter evidence, particle physics candidates and detection methods

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