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future extragalactic Fermi data. Lastly, we discuss how this method can be applied in a global, sensitivity-optimized indirect Dark Matter search that combines the results of all Cherenkov observatories of the present generation. Ƶ~2Bn�)��m��/��\��[��Ӭ�)3�d����Nf5�_M�1|�S0No�����0�j�� aѦ��{L��NYhl��/�eV�#���VX9��m�>�~����j�T��C��60_��ա��y The mass within the half-light radius is 5.8+8.2 – 3.1 × 105 M ☉. Note that with a 1 km s −1 velocity dispersion, Segue 1 would have (M 1/2 /L 1/2) 150 within the half-light radius (if interpreted as a system in equilibrium) and therefore would still be among the most dark-matter-dominated satellites of the Milky Way (Walker et al. This result confirms the previous measurements by the HESS experiment and indicates a steady source of TeV gamma-rays. The energy spectra as measured by these experiments show substantial differences. <> Segue 2 — карликова сфероїдальна галактика, розташована в сузір'ї Овна і виявлена 2009 року в даних, отриманих Слоанівським цифровим оглядом неба.. Характеристики. In fact, we already find a the internal bremsstrahlung and the substructures in the Dark Matter halo. Building on this success, SEGUE-2 spectroscopically observed around 120,000 stars, focusing on the in situ stellar halo of the Milky Way, from distances of 10 to 60 kpc. search for annihilations of Dark Matter particles in dense environments. @GG�S�Vy2�Tl�����r���n�v{�'7{��;=yag���ߦ�$��>L^���'g������I�����d�Ѳ��êɘ�K�/v{1��f�P����!������~�>�^���w�s�z�hg`qJ� My task is using MAGIC data to provide robust constraints on WIMP DM particles. within the dwarf galaxies. Cn. Dark matter in satellite galaxies: Will future Imaging Air Cherenkov Telescopes play a role? two-photon final state is 3.9(+7.1)(-3.7) x 10^-26 cm^3/s at 130 GeV, where the Furthermore, we estimate the sensitivity of Cherenkov Telescopes for monochromatic line signals. W, results of the stereoscopic observations of Segue 1 with the MA, 2013. Among the dSphs, the ultra-faint galaxy Segue 1 stands out with M=L estimated to 3400 M =L [9]. Here are presented the details on the latest dark matter, presented, together with the motivation behind the choice of, Segue 1 as a suitable dark matter target. Model particles, annihilation with internal bremsstrahlung and monochromatic line signals. signal that would correspond to a dark matter mass of \sim150 GeV; the same %�쏢 Although this Segue is an open source collaborative content management system designed for e-learning that combines the ease of use of course management systems with the flexibility of weblogs for creating various types of sites including course, news, and journal. With the, mass range predicted for WIMPs, those photons might be, visible in the gamma-ray domain, currently best explored, The gamma-ray flux from dark matter annihilation or, decay that is to be measured on Earth is determined by two, independent factors: one, coming from the particle physics, and other, related to the astrophysics. Lastly, results are interpreted in the light of v. dark matter annihilation and decay scenarios. Plate numbers 3510 or larger are BOSS plates, taken with the new BOSS spectrograph. experiment so far has been able to detect dark matter, directly of indirectly. We present the results of a comprehensive Keck/DEIMOS spectroscopic survey of the ultra-faint Milky Way satellite galaxy Segue 1. The extremely low metallicities ([Fe/H] < –3) of two Segue 1 stars and the large metallicity spread among the members demonstrate conclusively that Segue 1 is a dwarf galaxy, and we find no evidence in favor of tidal effects. It is located at a distance of about 23 kpc (about 75,000 light years) from the Sun and moves away from the Sun with the velocity of about 206 km/s. Segue 1, considered by many as possibly the most DM dominated satellite galaxy known in our galaxy. signal is also well fitted by a gamma-ray line at around 130 GeV. All rights reserved. For monochromatic γ-ray line emission, flux limits of (2×10^{-7}-2×10^{-5}) m^{-2} s^{-1} sr^{-1} and (1×10^{-8}-2×10^{-6}) m^{-2} s^{-1} sr^{-1} are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. %PDF-1.4 The original Sloan Extension for Galactic Understanding and Exploration (SEGUE-1) obtained spectra of nearly 240,000 stars of a range of spectral types. However we note that because the signal aperture is matched to the angular size of the MAGIC PSF, this truncation has a negligible impact on the sensitivity of the analysis. With a total luminosity less than that of a single bright red giant and a V-band mass-to-light ratio of 3400 M ☉/L ☉, Segue 1 is the darkest galaxy currently known. 5 0 obj Scientists have found the darkest known galaxy, a treasure trove of around 1,000 ancient, small and dim stars located just outside the Milky Way. A commonly encountered obstacle in indirect searches for galactic dark matter SELECT TOP 100 u, g, r, i, z FROM Galaxy It consists of two clusters of galaxies in a "dumbbell" shape: the Milky Way and its satellites form one lobe, and the Andromeda Galaxy and its satellites constitute the other. The previously neglected, The next generation of ground-based Imaging Air Cherenkov Telescopes (IACTs) will play an important role in indirect dark matter searches. Twenty paper disks (9 mm diameter) were immersed in the experimental solutions [0.1% CPC, 0.2% CPC, 2.5% NaOCl, 2.0% CHX (F.G.M., Joinville, SC, Brazil), and sterile distilled water] for 1 min and then 4 paper disks were placed over the BHIA surface in each agar plate. We present the results of the stereoscopic observations of Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. Search for Photon-Linelike Signatures from Dark Matter Annihilations with H.E.S.S. It was discovered by Beth Willman, Julianne J. Dalcanton, David Martinez-Delgado, and Andrew A. MAGIC-I has been operational since 2004, and in, mode, they allow for observations of significantly impro, Observations of Segue 1 were performed by MA, between January 2011 and February 2013, under the dark, night conditions, for zenith angle range between 13. , thus ensuring the low energy threshold of the analysis. 32 ND INTERNATIONAL C OSMIC R AY C ONFERENCE,BEIJING 2011 Segue 1: the best dark matter candidate dwarf galaxy surveyed by MAGIC J. No significant gamma-ray emission was found above the background in around30 hours of observation. This elongation may be caused by the tidal forces acting from the Milky Way galaxy if Segue 1 is being tidally disrupte… and 1 TeV. On the other hand, if constraints from this work, are compared with those derived from Fermi-LA, the case of dark matter decay, the case of production of a, photon and a neutrino is considered: the lower limit on, spectrum and their impact on detection prospects is consid-, ered. SEGUE-2. γ-ray instrument, upper limits on linelike emission are obtained in the energy range between ∼500 GeV and ∼25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. variety of decay modes, excluding half-lives up to ~10^26 to few 10^27 seconds. Kumpulan Tempatan ialah sebuah kumpulan galaksi yang termasuk galaksi kita, Bima Sakti.Kumpulan ini terdiri daripada lebih 35 galaksi, dengan pusat graviti terletak di antara Bima Sakti dan Galaksi Andromeda.Galaksi Kumpulan Tempatan meliputi diameter 10 juta tahun cahaya (lihat 1 E+22 m untuk perbandingan jarak) dan mempunyai bentuk binari (dumbel). The current release is Matlab-based (tested in versions 2013a, 2015a, 2015b, 2016b, and 2017a) and we aim to upload a C++/python version soon. into account the look-elsewhere effect, for an internal bremsstrahlung-like All content in this area was uploaded by Jelena Aleksić on Jul 18, 2014, ıes, Ed. In this Letter we present MAGIC observations of the Galactic center, resulting in the detection of a differential gamma-ray flux consistent with a steady, hard-slope power law, described as dN gamma/(dA dt dE) = (2.9 +/- 0.6) x 10(-12) (E/TeV)-2.2 +/- 0.2 cm(-2) s(-1) TeV-1. -- Note that this is much faster than the standard "ORDER BY RANDOM()" SQL method. The resulting, sample is to be used as a test area of the ever-e, The source chosen as the most suitable candidate is the, ultra-faint dSph galaxy Segue 1. Download Segue CMS for free. choices are adopted. Dwarf obtained from the observation of dwarf galaxies and, at least for the model Given that no significant gamma-ray, signal was found, the limits are derived for annihilation and, decay rates assuming various dark matter models. The gamma-ray source is centered at (R.A., decl.) Based on photometric, kinematic, and metallicity information, we identify 71 stars as probable Segue 1 members, including some as far out as 87 pc. Regarding the decay into the final state channel-, s, the dark matter particle lifetime is found to be of order, er limits estimated from the Fornax galaxy observations, with H.E.S.S., but from one to two orders of magnitude less, constraining (depending on the channel) than the bounds, Search for monochromatic line is done assuming direct, annihilation into two photons, and one photon and, Although these processes are highly loop suppressed, poten-, tial detection of line-like feature would provide a firm proof, of the dark matter existence, and also reveal some infor-, mation regarding the nature of its particle. Segue 1 significance skymap above 150 GeV, from 157.9 hours of observations. towards dwarf spheroidal galaxies, Internal bremsstrahlung in neutralino annihilation: Revised impact on indirect detection from γ-rays. West in 2005.. Properties. nihilating or decaying WIMP, gamma-ray emission is expected. Journal of Cosmology and Astroparticle Physics, as well as for the planned installation of CTA, taking special care of describing the experimental features that affect the detectional prospects. galaxies. spectral information of individual photon events from a sample of seven dwarf A LEKSI C´1,M.DORO 2,S.LOMBARDI 3,D.NIETO 4 ON BEHALF OF THE MAGIC C OLLABORATION AND M. F ORNASA 5 1 Institut de F ´ sica d Altes Energ ´ es, Ed. We derive new bounds on decaying Dark Matter from the gamma ray measurements limits are the strongest bounds, for the considered channels, from dSph observations by IACTs, and, for some models, and dark matter particle masses, even more constraining, The acquired results represent an improvement, with, respect to the previously most sensitive MA, searches, of an order of magnitude. 3.2 Likelihood analysis A totally new angle from DELTAt, the Tenmon Quartz wrist watch is a more simple, understated timepiece. SDSS Legacy and SEGUE-1 cover plate numbers from 266 to 2974. from direct dark matter annihilation (decay) into photon(s), or pronounced peak towards the kinematic limit from emis-, sion of virtual internal bremsstrahlung (VIB) photons [, The IACTs are observatories that deal with great v, of scientific objectives. Comment: 10 pages, 4 figures, minor changes, matches the published version (JCAP). telescope during its first 43 months. Several Nonadaptive segues are provided for apps that must also run on iOS 7, which does not support adaptive segues. the same final states, but without the VIB photons. Discovery. We critically re-examine recent claims that Segue 1 is a tidally disrupting star cluster and that kinematic samples are contaminated by the Sagittarius stream. When system went stereo, it, was opted to invest in a long-term observ, of the best dark matter candidate available to MA, accumulate many hours of good quality data. Segue 1 is a dwarf spheroidal galaxy or globular cluster situated in the Leo constellation and discovered in 2006 by Sloan Digital Sky Survey. The kinematic signature of 300S was first discovered in spectroscopic studies of the Segue 1 dwarf galaxy as a separate stellar population moving at 300 km/s. For a DM particle mass of 1 TeV, limits on the velocity-averaged DM annihilation cross section ⟨σv⟩_{χχ→γγ} reach ∼10^{-27} cm^{3} s^{-1}, based on the Einasto parametrization of the Galactic DM halo density profile. We perform a joint analysis of dwarf galaxy data from the Fermi Gamma-ray MAGIC can hunt this signature in the night sky. Segue 1 has the highest estimated dark matter density of any known galaxy and will therefore be a prime testing ground for dark matter physics and galaxy formation on small scales. Sebagai panduan kepada skala fizikal relatif Bima Sakti, jika telah dikurangkan kepada 130 km (80 batu) diameter, Sistem Suria pasti cuma 2 mm (0.08 inci) lebar. Segue 1’s velocity dispersion by Geha et al. SEGUE-2. On the other hand, the astrophysical factor is, determined by the dark matter density profile of a specific, The typical annihilation (decay) gamma-ray spectrum, is predicted to be continuous and featureless, with photons, mainly produced from the pion decay and the final state ra-, diation of charged particles. stream dedicated search for the latter in the data taken by the Fermi gamma-ray space The, support of the German BMBF and MPG, the Italian INFN, the, Swiss National Fund SNF, and the Spanish MICINN is grateful-, ly acknowledged. general speCifiCations: Dimensions: Measuring 2.1 x 2.6 x 4.3 inches Weight: 8.0 oz. This is the largest survey ever ... 17 m diameter IACTs, located at the Observatory Roque de los Mucha- is how to disentangle possible signals from astrophysical backgrounds. For an, Addressing the question about the importance of future Imaging Air Cherenkov Telescopes (IACTs) for indirect detection of Dark Matter (DM), I will review the results of a paper by Bringmann et al. By using the full likelihood analysis, we take complete advantage of the distinct features expected in the gamma ray spectrum of Dark Matter origin, achieving better sensitivity with respect to the standard analysis chains. Those. upper and lower, limits were calculated instead, for different models of dark, The considered scenarios include: annihilation and decay, into the final state SM particles, direct annihilation and, decay into photon(s) and 3-body annihilation with virtual, internal bremsstrahlung (VIB) contribution. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. There-, fore, in this work, an alternative analysis approach is used, nition of characteristic signatures dark matter interactions, mal advantage of the spectral information, and almost sole-, ly through the inclusion of the a priori knowledge on the, expected gamma-ray spectrum in the likelihood, it achieves, significantly better sensitivity than the method currently. (2008) in which the authors computed the gamma-ray flux from DM annihilation associated to the halos of two reference dwarf Spheroidal galaxies, Draco and Willman 1. It describes the shape of the expected, spectrum and gives the number of photons produced above, a given energy threshold for the dark matter scenario in, question. However, at least for the case of Willman 1 observed by CTA, boost factors may be below 10, even without considering the effect of substructures or the Sommerfeld enhancement. T, study as model-independent as possible, for all of the, channels the branching ratio is assumed to be 100%. The Local Group is the galaxy group that includes the Milky Way.It has a total diameter of roughly 3 megaparsecs (9.8 Mly), and a total mass of the order of 2 × 10 12 solar masses (4.0 × 10 42 kg). The obtained up-, acy of the considered model is more relevant, and limits, order of magnitude more constraining than the ones for the, case of less significant VIB contribution (, considered channels, estimated bounds are up to two - three, orders of magnitude stronger than for the annihilation into. The current searches are mainly, focused on dark matter composed of weakly interacting. strong enough to probe annihilation rates expected for thermally produced dark MAGIC is a ground-based system of two, 17 m diameter, IACTs, located at the Roque de los Muchachos Observatory, a.s.l.). Nevertheless, some distincti, spectral features could be present, like monochromatic line. Nominal positions of Segue 1 and η Leo are marked with the square and the star, respectively. procedure to select optimal target regions that takes into account both This is the longest exposure of any dSph galaxy by, The Segue 1 observations were analysed using the full, likelihood approach, an optimized analysis method that, takes complete advantage of the distinct features expected, in the gamma-ray spectrum of dark matter origin, achieving, better sensitivity with respect to the standard analysis of, ]. enhancements of the gamma-ray flux are studied, i.e., the Sommerfeld effect, used as standard in analysis chains of the IACTs. Investigate the non-thermal processes in the Universe leading to particle acceleration and gamma ray radiation. We also compare its sensitivity with that of the current standards for several Dark Matter annihilation models, obtaining gains of up to factors of order of 10. M. Ackermann et al., Physical Review D 86 (2012) 022002, A.Geringer-Sameth and S.M. Cn. The analysis of the data is performed using a dedicated likelihood approach, optimized for signals with characteristic spectral features. Located at a distance of, 23 kpc, this dSph is in the Northern hemisphere, outside of, the Galactic plane and visible to MAGIC for, dark time per year at low zenith angles. We give cross-section upper limits and decay lifetime lower limits for dark matter models that produce gamma-ray lines or contribute to the diffuse spectrum, including models proposed as explanations of the PAMELA and Fermi cosmic-ray data. Using data collected with the H.E.S.S. -- and 65000 to generate a random sample between 1 and 100% of the data -- respectively. have been derived in different particle physics scenarios. spectral features plays a key role for indirect detection experiments; Discovering the nature of dark matter is one of the most exciting tasks of modern science. With almost 160 hours of good quality data, this is the deepest observational campaign on any dwarf galaxy carried so far by any Imaging Air Cherenkov Telescope. While these limits are still not quite We also show that contamination by the Sagittarius stream has been overestimated. Diameter Diameter gugusan besar ini adalah kira-kira 200 juta tahun cahaya ; ia mengandungi 100 kumpulan dan gugusan galaksi dan mengandungi gugusan Virgo pada pusatnya. an interesting improvement and may become better than those from the current or The particle physics, term is fixed for a chosen model and does not depend on, the observed source. Flux upper limits are presented for gamma-ray spectral lines from 7 to 200 GeV and for the diffuse gamma-ray background from 4.8 GeV to 264 GeV obtained from two years of Fermi Large Area Telescope data integrated over most of the sky. We find that for a typical energy threshold of 100 GeV the flux, Join ResearchGate to discover and stay up-to-date with the latest research from leading experts in, Access scientific knowledge from anywhere. targets suitable for dark matter searches, dwarf spheroidal galaxies are considered to be excellent candidates and, among them, Segue 1 stands out with mass-to-light ratio estimated to be of the order of 1000. For example, the behavior of a Show segue changes based on the presenting view controller. De-, as the squared ratio of the masses of the scalar and dark, VIB contribution is the most pronounced. More importantly, this galaxy has the mass-to-light ratio estimated to, , making it the most dark matter dominated object, ]. Fornax galaxy cluster by HESS. bremsstrahlung, in particular, provide smoking gun signatures. ResearchGate has not been able to resolve any citations for this publication. To this end, we use a new adaptive It features a quartz movement housed in a stainless steel case and protected by a sapphire crystal. Physics 06 (2011) 035 doi:10.1088/1475-7516/2011/06/035. signals, constraints on the Dark Matter particle annihilation cross-section After correcting for the influence of binary stars using repeated velocity measurements, we determine a velocity dispersion of 3.7+1.4 – 1.1 km s–1. method is tested by a subsampling analysis of the full sky data and found to annihilation cross-section that we derive are stronger than what can be MAGIC is a ground-based system of two, 17 m diameter. Messier 54 (juga dikenali sebagai M54 atau NGC 6715 adalah kelompok globul dalam buruj Sagittarius.Ia telah ditemui oleh Charles Messier pada tahun 1778 dan kemudiannya dimasukkan dalam katalog objek seperti komet.M54 mudah dijumpai di langit, dekat dengan bintang ζ Sagittarii.Walau bagaimanapun, ia tidak dapat dileraikan menjadi bintang individu walaupun dengan teleskop amatur yang lebih besar. The preference, howe, given to the astrophysical sources of con, whose spectral distributions are nicely described, in majori-, analysis tools and methods of IACTs are adapted for such, signals, at the expense of sources whose emissions are pre-, dicted to contain some distinctive spectral features. During this period, the telescopes underwent a series of, significant changes: at the end of 2011, the readout systems. The, dark matter particle mass takes values from the 100 GeV -, Furthermore, no additional boosts to the signal, either from, presence of substructures or from quantum effects were, In particular, constraints are calculated for the follow-, its for leptonic channels are even more stringent than the, constraints from this work are at least an order of magni-, tude stronger than the previous most sensitive MA, ]. 279-390 doi:10.1016/j.physrep.2004.08.031. The Perseus galaxy cluster was observed by the MAGIC Cherenkov telescope for a total effective time of 24.4 hr during 2008 November and December. Dark matter particle annihilation or decay can produce monochromatic gamma-ray lines and contribute to the diffuse gamma-ray background. Space Telescope in search of dark matter annihilation into a gamma-ray line. is expected from this source at very high energies. p (17(h)45(m)20(s), -29 degrees 2'). Kumpulan Tempatan yang terletak berhampiran sempadan ditarik ke dalam gugusan Virgo [1] . In this work, I use APOGEE-2 and SEGUE survey data to map out the 300S stream. e^\pm spectral features in Pamela, Fermi and HESS, unless very conservative observation campaigns on dwarf satellite galaxies of the Milky Way were option. the Fermi Gamma-ray Space Telescope, The CTA (Cherenkov Telescope Array) Project. reproduce the theoretical expectations very well. As an example, we review the gamma-ray dark matter detection prospects from Draco dwarf spheroidal galaxy at the MAGIC stereoscopic system and the CTA project. While the detection of the spectral features introduced by internal bremsstrahlung would constitute a smoking gun signature for dark matter annihilation, we find that for most models the overall flux still remains at a level that will be challenging to detect unless one adopts rather (though by no means overly) optimistic astrophysical assumptions about the distribution of dark matter in the dwarfs. Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. Gamma-ray line signatures can be expected in the very-high-energy (E_{γ}>100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Recently, the Galactic center has been reported to be a source of very high energy (VHE) gamma-rays by the CANGAROO, VERITAS, and HESS experiments. SEGUE could be used for spatial phase unwrapping in other applications such as X-ray phase contrast imaging, synthetic aperture radar interferometry, and 3D shape measurement or profilometry. The stellar kinematics of Segue 1 require very high mass-to-light ratios unless the system is far from dynamical equilibrium, even if the period distribution of unresolved binary stars is skewed toward implausibly short periods. Segue 2 is a dwarf spheroidal galaxy situated in the constellation Aries and discovered in 2009 in the data obtained by Sloan Digital Sky Survey.The galaxy is located at the distance of about 35 kiloparsecs (35,000 parsecs; 110,000 light-years) from the Sun and moves towards the Sun at a speed of 40 km/s. Results are compatible with cosmological cluster simulations for the cosmic-ray-induced gamma-ray emission, constraining the average cosmic ray-to-thermal pressure to < 4% for the cluster core region (< 8% for the entire cluster). Dwarf galaxies show no evidence of a gamma-ray line between 10 GeV would be a fascinating possibility, we caution that a much more dedicated The boost factor is the quantity used to describe how far the experiment is from probing interesting DM scenarios and it is computed for the next generation of IACTs, namely MAGIC-II and CTA. Among the targets suitable for dark matter searches, dwarf spheroidal galaxies are considered to be excellent candidates and, among them, Segue 1 stands out with mass-to-light ratio estimated to be of the order of 1000. The subsequent upper limit on the annihilation cross section to a Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment. energy gamma-rays (E > 100 GeV). 2009a; Wolf et al. that such signals are most likely subdominant, the search for pronounced Segue 2 has a luminosity just 900 times that of our sun, the researchers report. The Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph), also known as the Sagittarius Dwarf Elliptical Galaxy (Sgr dE or Sag DEG), is an elliptical loop-shaped satellite galaxy of the Milky Way.It contains four globular clusters, with the brightest of them – NGC 6715 (M54) – being known well before the discovery of the galaxy itself in 1994. Being a small dwarf galaxy, it measures only a few thousand light-years in diameter. However, the effect of internal bremsstrahlung is negligible or small in more optimistic scenarios for detection like the funnel and focus point regions. analysis and additional data will be necessary to rule out or confirm this The resulting upper limits on the gamma-ray emission above 100 GeV are in the range of 4.6-7.5 x 10(-12) cm(-2) s(-1) for spectral indices from -1.5 to -2.5, thereby constraining the emission produced by cosmic rays, dark matter annihilations, and the central radio galaxy NGC 1275. massive particles (WIMPs), that are of non-baryonic nature, produced thermally in the early Universe, and are stable on, cosmological scales. For the first time in such a study, we fully take into account the effect of internal bremsstrahlung, which has recently been shown to considerably enhance, in some cases, the gamma-ray flux at the high energies where Atmospheric Cherenkov Telescopes operate, thus leading to significantly harder annihilation spectra than traditionally considered. Halo Galaksi menjangkau luar tetapi terhad dalam saiz oleh orbit dua satelit Bima Sakti, Awan Magellan Besar dan Kecil di perigalaktikon pada ~180,000 tahun cahaya. The 95% confidence level upper limits range from about 10(-26)  cm3  s(-1) at 5 GeV to about 5×10(-23)   cm3  s(-1) at 1 TeV, depending on the dark matter annihilation final state. c, J. Rico and M. Martinez, Journal of Cosmology, J. Albert et al., The Astrophysical Journal Letters 638 (2006), c et al., The Astrophysical Journal 710 (2010), c et al., To appear in the Proceedings of the 33, c et al., Astroparticle Physics 35 (2012) 435-448. mode between January 2011 and February 2013, have, resulted in 157.9 hours of good quality data, thus making, this campaign the deepest survey of any dSph by any IA, The gathered data have been analyzed by means of the, full likelihood method. Instituto Nazionale di Astrofisica, I-00136 Rome, Italy. Given matter, future prospects to do so are very good. New interesting targets are recently found that are extremely dark matter dominated. We In this article, we consider two particularly promising candidate sources for dark matter annihilation signals, the nearby dwarf galaxies Draco and Willman 1, and study the prospects of detecting such a signal for the soon-operating MAGIC II telescope system. This work was also supported by the Marie, CSD2009-00064 projects of the Spanish Consolider Ingenio 2010, programme, by grant DO02-353 of the Bulgarian NSF, by grant, 127740 of the Academy of Finland, by the YIP of the Helmholtz, Gemeinschaft, by the DFG Cluster of Excellence Origin and Struc-, ture of the Universe, and by the Polish MNiSzW grant 745/N-, G. Bertone, D. Hooper and J. of both instruments were replaced by the more advanced, DRS4-based configurations; by the end of 2012, among, other improvements, the camera of MAGIC-I w, to the exact replica of that of MAGIC-II [, performance of the system varied during the total period, of Segue 1 observations; therefore, data from each of the, different telescope states are analyzed separately, After the selection and data reduction procedures of, the MAGIC standard analysis chain, the total effecti, observation time amounted to 157.9 hours of good-quality, data. Silk, Physics Report 405 (2005). The notion of dark matter has been present for almost a, Observational evidence on all scales and cosmological, predictions indicate that dark matter represents almost 85%, of the matter content of our Universe, an almost 25% of its.

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