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Ultra-high-energy $γ$-ray emission associated with the tail of a bow-shock pulsar wind nebula
Authors:
Zhen Cao,
F. Aharonian,
Y. X. Bai,
Y. W. Bao,
D. Bastieri,
X. J. Bi,
Y. J. Bi,
W. Bian,
A. V. Bukevich,
C. M. Cai,
W. Y. Cao,
Zhe Cao,
J. Chang,
J. F. Chang,
A. M. Chen,
E. S. Chen,
H. X. Chen,
Liang Chen,
Long Chen,
M. J. Chen,
M. L. Chen,
Q. H. Chen,
S. Chen,
S. H. Chen,
S. Z. Chen
, et al. (274 additional authors not shown)
Abstract:
In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) $γ$-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1$σ$ (9.4$σ$) above 25$\,$TeV (100$\,$TeV). The source energy spectrum extended up to 300$\,$TeV, which was well fitted by a log-parabola f…
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In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) $γ$-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1$σ$ (9.4$σ$) above 25$\,$TeV (100$\,$TeV). The source energy spectrum extended up to 300$\,$TeV, which was well fitted by a log-parabola function with $N0 = (1.93\pm0.23) \times 10^{-16} \rm{TeV^{-1}\,cm^{-2}\,s^{-2}}$, $α= 2.14\pm0.27$, and $β= 1.20\pm0.41$ at E0 = 30$\,$TeV. The associated pulsar, PSR J1740+1000, resides at a high galactic latitude and powers a bow-shock pulsar wind nebula (BSPWN) with an extended X-ray tail. The best-fit position of the gamma-ray source appeared to be shifted by $0.2^{\circ}$ with respect to the pulsar position. As the (i) currently identified pulsar halos do not demonstrate such offsets, and (ii) centroid of the gamma-ray emission is approximately located at the extension of the X-ray tail, we speculate that the UHE $γ$-ray emission may originate from re-accelerated electron/positron pairs that are advected away in the bow-shock tail.
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Submitted 24 February, 2025; v1 submitted 21 February, 2025;
originally announced February 2025.
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Constraints on Ultra Heavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations
Authors:
Zhen Cao,
F. Aharonian,
Q. An,
Axikegu,
Y. X. Bai,
Y. W. Bao,
D. Bastieri,
X. J. Bi,
Y. J. Bi,
J. T. Cai,
Q. Cao,
W. Y. Cao,
Zhe Cao,
J. Chang,
J. F. Chang,
A. M. Chen,
E. S. Chen,
Liang Chen,
Lin Chen,
Long Chen,
M. J. Chen,
M. L. Chen,
Q. H. Chen,
S. H. Chen,
S. Z. Chen
, et al. (255 additional authors not shown)
Abstract:
In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes…
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In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes of astrophysical $γ$-ray background while large amount of dark matter. By analyzing more than 700 days observational data at LHAASO, no significant dark matter signal from 1 TeV to 1 EeV is detected. Accordingly we derive the most stringent constraints on the ultra-heavy dark matter annihilation cross-section up to EeV. The constraints on the lifetime of dark matter in decay mode are also derived.
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Submitted 12 June, 2024;
originally announced June 2024.
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The First LHAASO Catalog of Gamma-Ray Sources
Authors:
Zhen Cao,
F. Aharonian,
Q. An,
Axikegu,
Y. X. Bai,
Y. W. Bao,
D. Bastieri,
X. J. Bi,
Y. J. Bi,
J. T. Cai,
Q. Cao,
W. Y. Cao,
Zhe Cao,
J. Chang,
J. F. Chang,
A. M. Chen,
E. S. Chen,
Liang Chen,
Lin Chen,
Long Chen,
M. J. Chen,
M. L. Chen,
Q. H. Chen,
S. H. Chen,
S. Z. Chen
, et al. (255 additional authors not shown)
Abstract:
We present the first catalog of very-high energy and ultra-high energy gamma-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). The catalog was compiled using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022.…
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We present the first catalog of very-high energy and ultra-high energy gamma-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). The catalog was compiled using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022. This catalog represents the main result from the most sensitive large coverage gamma-ray survey of the sky above 1 TeV, covering declination from $-$20$^{\circ}$ to 80$^{\circ}$. In total, the catalog contains 90 sources with an extended size smaller than $2^\circ$ and a significance of detection at $> 5σ$. Based on our source association criteria, 32 new TeV sources are proposed in this study. Among the 90 sources, 43 sources are detected with ultra-high energy ($E > 100$ TeV) emission at $> 4σ$ significance level. We provide the position, extension, and spectral characteristics of all the sources in this catalog.
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Submitted 27 November, 2023; v1 submitted 26 May, 2023;
originally announced May 2023.
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Exploring TeV candidates of Fermi blazars through machine learning
Authors:
J. T. Zhu,
C. Lin,
H. B. Xiao,
J. H. Fan,
D. Bastieri,
G. G. Wang
Abstract:
In this work, we make use of a supervised machine learning algorithm based on Logistic Regression (LR) to select TeV blazar candidates from the 4FGL-DR2 / 4LAC-DR2, 3FHL, 3HSP, and 2BIGB catalogs. LR constructs a hyperplane based on a selection of optimal parameters, named features, and hyper-parameters whose values control the learning process and determine the values of features that a learning…
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In this work, we make use of a supervised machine learning algorithm based on Logistic Regression (LR) to select TeV blazar candidates from the 4FGL-DR2 / 4LAC-DR2, 3FHL, 3HSP, and 2BIGB catalogs. LR constructs a hyperplane based on a selection of optimal parameters, named features, and hyper-parameters whose values control the learning process and determine the values of features that a learning algorithm ends up learning, to discriminate TeV blazars from non-TeV blazars. In addition, it gives the probability (or logistic) that a source may be considered as a TeV blazar candidate. Non-TeV blazars with logistics greater than 80% are considered high-confidence TeV candidates. Using this technique, we identify 40 high-confidence TeV candidates from the 4FGL-DR2 / 4LAC-DR2 blazars and we build the feature hyper-plane to distinguish TeV and non-TeV blazars. We also calculate the hyper-planes for the 3FHL, 3HSP, and 2BIGB. Finally, we construct the broadband spectral energy distributions (SED) for the 40 candidates, testing for their detectability with various instruments. We find that 7 of them are likely to be detected by existing or upcoming IACT observatories, while 1 could be observed with EAS particle detector arrays.
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Submitted 18 March, 2023;
originally announced March 2023.
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Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre
Authors:
The Cherenkov Telescope Array Consortium,
:,
A. Acharyya,
R. Adam,
C. Adams,
I. Agudo,
A. Aguirre-Santaella,
R. Alfaro,
J. Alfaro,
C. Alispach,
R. Aloisio,
R. Alves Batista,
L. Amati,
G. Ambrosi,
E. O. Angüner,
L. A. Antonelli,
C. Aramo,
A. Araudo,
T. Armstrong,
F. Arqueros,
K. Asano,
Y. Ascasíbar,
M. Ashley,
C. Balazs,
O. Ballester
, et al. (427 additional authors not shown)
Abstract:
We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models giv…
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We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies.
"Full likelihood tables complementing our analysis are provided here [ https://doi.org/10.5281/zenodo.4057987 ]"
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Submitted 30 January, 2021; v1 submitted 31 July, 2020;
originally announced July 2020.
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Unresolved Gamma-Ray Sky through its Angular Power Spectrum
Authors:
M. Ackermann,
M. Ajello,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
R. Bellazzini,
E. Bissaldi,
R. D. Blandford,
R. Bonino,
E. Bottacini,
J. Bregeon,
P. Bruel,
R. Buehler,
E. Burns,
S. Buson,
R. A. Cameron,
R. Caputo,
P. A. Caraveo,
E. Cavazzuti,
S. Chen,
G. Chiaro,
S. Ciprini,
D. Costantin,
A. Cuoco
, et al. (85 additional authors not shown)
Abstract:
The gamma-ray sky has been observed with unprecedented accuracy in the last decade by the Fermi large area telescope (LAT), allowing us to resolve and understand the high-energy Universe. The nature of the remaining unresolved emission (unresolved gamma-ray background, UGRB) below the LAT source detection threshold can be uncovered by characterizing the amplitude and angular scale of the UGRB fluc…
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The gamma-ray sky has been observed with unprecedented accuracy in the last decade by the Fermi large area telescope (LAT), allowing us to resolve and understand the high-energy Universe. The nature of the remaining unresolved emission (unresolved gamma-ray background, UGRB) below the LAT source detection threshold can be uncovered by characterizing the amplitude and angular scale of the UGRB fluctuation field. This work presents a measurement of the UGRB autocorrelation angular power spectrum based on eight years of Fermi LAT Pass 8 data products. The analysis is designed to be robust against contamination from resolved sources and noise systematics. The sensitivity to subthreshold sources is greatly enhanced with respect to previous measurements. We find evidence (with $\sim$3.7$σ$ significance) that the scenario in which two classes of sources contribute to the UGRB signal is favored over a single class. A double power law with exponential cutoff can explain the anisotropy energy spectrum well, with photon indices of the two populations being 2.55 $\pm$ 0.23 and 1.86 $\pm$ 0.15.
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Submitted 3 May, 2019; v1 submitted 5 December, 2018;
originally announced December 2018.
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Search for extended gamma-ray emission from the Virgo galaxy cluster with Fermi-LAT
Authors:
M. Ackermann,
M. Ajello,
A. Albert,
W. B. Atwood,
L. Baldini,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
E. Bissaldi,
E. D. Bloom,
R. Bonino,
E. Bottacini,
T. J. Brandt,
J. Bregeon,
P. Bruel,
R. Buehler,
S. Buson,
G. A. Caliandro,
R. A. Cameron,
R. Caputo,
M. Caragiulo,
P. A. Caraveo,
J. M. Casandjian,
E. Cavazzuti
, et al. (96 additional authors not shown)
Abstract:
Galaxy clusters are one of the prime sites to search for dark matter (DM) annihilation signals. Depending on the substructure of the DM halo of a galaxy cluster and the cross sections for DM annihilation channels, these signals might be detectable by the latest generation of $γ$-ray telescopes. Here we use three years of Fermi Large Area Telescope (LAT) data, which are the most suitable for search…
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Galaxy clusters are one of the prime sites to search for dark matter (DM) annihilation signals. Depending on the substructure of the DM halo of a galaxy cluster and the cross sections for DM annihilation channels, these signals might be detectable by the latest generation of $γ$-ray telescopes. Here we use three years of Fermi Large Area Telescope (LAT) data, which are the most suitable for searching for very extended emission in the vicinity of nearby Virgo galaxy cluster. Our analysis reveals statistically significant extended emission which can be well characterized by a uniformly emitting disk profile with a radius of 3°that moreover is offset from the cluster center. We demonstrate that the significance of this extended emission strongly depends on the adopted interstellar emission model (IEM) and is most likely an artifact of our incomplete description of the IEM in this region. We also search for and find new point source candidates in the region. We then derive conservative upper limits on the velocity-averaged DM pair annihilation cross section from Virgo. We take into account the potential $γ$-ray flux enhancement due to DM sub-halos and its complex morphology as a merging cluster. For DM annihilating into $b\overline{b}$, assuming a conservative sub-halo model setup, we find limits that are between 1 and 1.5 orders of magnitude above the expectation from the thermal cross section for $m_{\mathrm{DM}}\lesssim100\,\mathrm{GeV}$. In a more optimistic scenario, we exclude $\langle σv \rangle\sim3\times10^{-26}\,\mathrm{cm^{3}\,s^{-1}}$ for $m_{\mathrm{DM}}\lesssim40\,\mathrm{GeV}$ for the same channel. Finally, we derive upper limits on the $γ$-ray-flux produced by hadronic cosmic-ray interactions in the inter cluster medium. We find that the volume-averaged cosmic-ray-to-thermal pressure ratio is less than $\sim6\%$.
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Submitted 30 September, 2015;
originally announced October 2015.
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Anisotropies in the diffuse gamma-ray background measured by the Fermi LAT
Authors:
M. Ackermann,
M. Ajello,
A. Albert,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
T. J. Brandt,
J. Bregeon,
M. Brigida,
P. Bruel,
R. Buehler,
S. Buson,
G. A. Caliandro,
R. A. Cameron,
P. A. Caraveo,
C. Cecchi,
E. Charles,
A. Chekhtman,
J. Chiang
, et al. (112 additional authors not shown)
Abstract:
The contribution of unresolved sources to the diffuse gamma-ray background could induce anisotropies in this emission on small angular scales. We analyze the angular power spectrum of the diffuse emission measured by the Fermi LAT at Galactic latitudes |b| > 30 deg in four energy bins spanning 1 to 50 GeV. At multipoles \ell \ge 155, corresponding to angular scales \lesssim 2 deg, angular power ab…
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The contribution of unresolved sources to the diffuse gamma-ray background could induce anisotropies in this emission on small angular scales. We analyze the angular power spectrum of the diffuse emission measured by the Fermi LAT at Galactic latitudes |b| > 30 deg in four energy bins spanning 1 to 50 GeV. At multipoles \ell \ge 155, corresponding to angular scales \lesssim 2 deg, angular power above the photon noise level is detected at >99.99% CL in the 1-2 GeV, 2-5 GeV, and 5-10 GeV energy bins, and at >99% CL at 10-50 GeV. Within each energy bin the measured angular power takes approximately the same value at all multipoles \ell \ge 155, suggesting that it originates from the contribution of one or more unclustered source populations. The amplitude of the angular power normalized to the mean intensity in each energy bin is consistent with a constant value at all energies, C_P/<I>^2 = 9.05 +/- 0.84 x 10^{-6} sr, while the energy dependence of C_P is consistent with the anisotropy arising from one or more source populations with power-law photon spectra with spectral index Γ_s = 2.40 +/- 0.07. We discuss the implications of the measured angular power for gamma-ray source populations that may provide a contribution to the diffuse gamma-ray background.
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Submitted 13 February, 2012;
originally announced February 2012.
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Search for Dark Matter Satellites using the FERMI-LAT
Authors:
The Fermi LAT Collaboration,
M. Ackermann,
A. Albert,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
R. D. Blandford,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
E. Bottacini,
T. J. Brandt,
J. Bregeon,
M. Brigida,
P. Bruel,
R. Buehler,
T. H. Burnett,
G. A. Caliandro,
R. A. Cameron,
P. A. Caraveo,
J. M. Casandjian,
C. Cecchi
, et al. (111 additional authors not shown)
Abstract:
Numerical simulations based on the Lambda-CDM model of cosmology predict a large number of as yet unobserved Galactic dark matter satellites. We report the results of a Large Area Telescope (LAT) search for these satellites via the gamma-ray emission expected from the annihilation of weakly interacting massive particle (WIMP) dark matter. Some dark matter satellites are expected to have hard gamma…
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Numerical simulations based on the Lambda-CDM model of cosmology predict a large number of as yet unobserved Galactic dark matter satellites. We report the results of a Large Area Telescope (LAT) search for these satellites via the gamma-ray emission expected from the annihilation of weakly interacting massive particle (WIMP) dark matter. Some dark matter satellites are expected to have hard gamma-ray spectra, finite angular extents, and a lack of counterparts at other wavelengths. We sought to identify LAT sources with these characteristics, focusing on gamma-ray spectra consistent with WIMP annihilation through the $b \bar b$ channel. We found no viable dark matter satellite candidates using one year of data, and we present a framework for interpreting this result in the context of numerical simulations to constrain the velocity-averaged annihilation cross section for a conventional 100 GeV WIMP annihilating through the $b \bar b$ channel.
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Submitted 12 January, 2012;
originally announced January 2012.
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Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope
Authors:
The Fermi-LAT Collaboration,
:,
M. Ackermann,
M. Ajello,
A. Albert,
W. B. Atwood,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
B. Berenji,
R. D. Blandford,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
J. Bregeon,
M. Brigida,
P. Bruel,
R. Buehler,
T. H. Burnett,
S. Buson,
G. A. Caliandro,
R. A. Cameron
, et al. (129 additional authors not shown)
Abstract:
Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. 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. No dark matter signal is detected. Including the uncertainty in the dark matter…
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Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. 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. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 1e-26 cm^3 s^-1 at 5 GeV to about 5e-23 cm^3 s^-1 at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section (~3e-26 cm^3 s^-1 for a purely s-wave cross section), without assuming additional boost factors.
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Submitted 12 December, 2011; v1 submitted 17 August, 2011;
originally announced August 2011.
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Constraints on Cosmological Dark Matter Annihilation from the Fermi-LAT Isotropic Diffuse Gamma-Ray Measurement
Authors:
The Fermi-LAT collaboration,
:,
A. A. Abdo,
M. Ackermann,
M. Ajello,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
B. Berenji,
R. D. Blandford,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
A. Bouvier,
J. Bregeon,
A. Brez,
M. Brigida,
P. Bruel,
T. H. Burnett,
S. Buson,
G. A. Caliandro,
R. A. Cameron
, et al. (126 additional authors not shown)
Abstract:
The first published Fermi large area telescope (Fermi-LAT) measurement of the isotropic diffuse gamma-ray emission is in good agreement with a single power law, and is not showing any signature of a dominant contribution from dark matter sources in the energy range from 20 to 100 GeV. We use the absolute size and spectral shape of this measured flux to derive cross section limits on three types…
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The first published Fermi large area telescope (Fermi-LAT) measurement of the isotropic diffuse gamma-ray emission is in good agreement with a single power law, and is not showing any signature of a dominant contribution from dark matter sources in the energy range from 20 to 100 GeV. We use the absolute size and spectral shape of this measured flux to derive cross section limits on three types of generic dark matter candidates: annihilating into quarks, charged leptons and monochromatic photons. Predicted gamma-ray fluxes from annihilating dark matter are strongly affected by the underlying distribution of dark matter, and by using different available results of matter structure formation we assess these uncertainties. We also quantify how the dark matter constraints depend on the assumed conventional backgrounds and on the Universe's transparency to high-energy gamma-rays. In reasonable background and dark matter structure scenarios (but not in all scenarios we consider) it is possible to exclude models proposed to explain the excess of electrons and positrons measured by the Fermi-LAT and PAMELA experiments. Derived limits also start to probe cross sections expected from thermally produced relics (e.g. in minimal supersymmetry models) annihilating predominantly into quarks. For the monochromatic gamma-ray signature, the current measurement constrains only dark matter scenarios with very strong signals.
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Submitted 24 February, 2010;
originally announced February 2010.
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Fermi LAT Search for Photon Lines from 30 to 200 GeV and Dark Matter Implications
Authors:
The Fermi LAT Collaboration,
A. A. Abdo,
M. Ackermann,
M. Ajello,
W. B. Atwood,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
B. Berenji,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
A. Bouvier,
J. Bregeon,
A. Brez,
M. Brigida,
P. Bruel,
T. H. Burnett,
S. Buson,
G. A. Caliandro,
R. A. Cameron,
P. A. Caraveo
, et al. (138 additional authors not shown)
Abstract:
Dark matter (DM) particle annihilation or decay can produce monochromatic $γ$-rays readily distinguishable from astrophysical sources. $γ$-ray line limits from 30 GeV to 200 GeV obtained from 11 months of Fermi Large Area Space Telescope data from 20-300 GeV are presented using a selection based on requirements for a $γ$-ray line analysis, and integrated over most of the sky. We obtain $γ$-ray l…
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Dark matter (DM) particle annihilation or decay can produce monochromatic $γ$-rays readily distinguishable from astrophysical sources. $γ$-ray line limits from 30 GeV to 200 GeV obtained from 11 months of Fermi Large Area Space Telescope data from 20-300 GeV are presented using a selection based on requirements for a $γ$-ray line analysis, and integrated over most of the sky. We obtain $γ$-ray line flux upper limits in the range $0.6-4.5\times 10^{-9}\mathrm{cm}^{-2}\mathrm{s}^{-1}$, and give corresponding DM annihilation cross-section and decay lifetime limits. Theoretical implications are briefly discussed.
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Submitted 26 January, 2010;
originally announced January 2010.
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Observations of Milky Way Dwarf Spheroidal galaxies with the Fermi-LAT detector and constraints on Dark Matter models
Authors:
Fermi-LAT Collaboration,
:,
A. A. Abdo,
M. Ackermann,
M. Ajello,
W. B. Atwood,
L. Baldini,
J. Ballet,
G. Barbiellini,
D. Bastieri,
K. Bechtol,
R. Bellazzini,
B. Berenji,
E. D. Bloom,
E. Bonamente,
A. W. Borgland,
J. Bregeon,
A. Brez,
M. Brigida,
P. Bruel,
T. H. Burnett,
S. Buson,
G. A. Caliandro,
R. A. Cameron,
P. A. Caraveo
, et al. (139 additional authors not shown)
Abstract:
We report on the observations of 14 dwarf spheroidal galaxies with the Fermi Gamma-Ray Space Telescope taken during the first 11 months of survey mode operations. The Fermi telescope provides a new opportunity to test particle dark matter models through the expected gamma-ray emission produced by pair annihilation of weakly interacting massive particles (WIMPs). Local Group dwarf spheroidal gala…
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We report on the observations of 14 dwarf spheroidal galaxies with the Fermi Gamma-Ray Space Telescope taken during the first 11 months of survey mode operations. The Fermi telescope provides a new opportunity to test particle dark matter models through the expected gamma-ray emission produced by pair annihilation of weakly interacting massive particles (WIMPs). Local Group dwarf spheroidal galaxies, the largest galactic substructures predicted by the cold dark matter scenario, are attractive targets for such indirect searches for dark matter because they are nearby and among the most extreme dark matter dominated environments. No significant gamma-ray emission was detected above 100 MeV from the candidate dwarf galaxies. We determine upper limits to the gamma-ray flux assuming both power-law spectra and representative spectra from WIMP annihilation. The resulting integral flux above 100 MeV is constrained to be at a level below around 10^-9 photons cm^-2 s^-1. Using recent stellar kinematic data, the gamma-ray flux limits are combined with improved determinations of the dark matter density profile in 8 of the 14 candidate dwarfs to place limits on the pair annihilation cross-section of WIMPs in several widely studied extensions of the standard model. With the present data, we are able to rule out large parts of the parameter space where the thermal relic density is below the observed cosmological dark matter density and WIMPs (neutralinos here) are dominantly produced non-thermally, e.g. in models where supersymmetry breaking occurs via anomaly mediation. The gamma-ray limits presented here also constrain some WIMP models proposed to explain the Fermi and PAMELA e^+e^- data, including low-mass wino-like neutralinos and models with TeV masses pair-annihilating into muon-antimuon pairs. (Abridged)
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Submitted 25 January, 2010;
originally announced January 2010.
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Science with the new generation high energy gamma- ray experiments
Authors:
M. Alvarez,
D. D'Armiento,
G. Agnetta,
A. Alberdi,
A. Antonelli,
A. Argan,
P. Assis,
E. A. Baltz,
C. Bambi,
G. Barbiellini,
H. Bartko,
M. Basset,
D. Bastieri,
P. Belli,
G. Benford,
L. Bergstrom,
R. Bernabei,
G. Bertone,
A. Biland,
B. Biondo,
F. Bocchino,
E. Branchini,
M. Brigida,
T. Bringmann,
P. Brogueira
, et al. (175 additional authors not shown)
Abstract:
This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invaria…
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This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invariance.
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Submitted 4 December, 2007;
originally announced December 2007.