A search for a dark matter annihilation signal towards the Canis Major overdensity with H.E.S.S
A search for a dark matter (DM) annihilation signal into $\gamma$-rays toward the direction of the Canis Major (CMa) overdensity is presented. The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A...
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| Veröffentlicht in: | The Astrophysical journal 2009, Vol.691, p.175-181 |
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| creator | Aharonian, F. Akhperjanian, A.G. Barres de Almeida, U. Bazer-Bachi, A.R. Behera, B. Beilicke, M. Benbow, W. Bernlöhr, K. Boisson, C. Borrel, V. Braun, I. Brion, E. Brucker, J. Bühler, R. Bulik, T. Büsching, I. Boutelier, T. Carrigan, S. Chadwick, P.M. Chaves, R. Chounet, L.-M. Coignet, G. Cornils, R. Costamante, L. Dalton, M. Degrange, B. Dickinson, H.J. Djannati-Ataï, A. Domainko, W. Drury, L.O'C. Dubois, F. Dubus, G. Dyks, J. Egberts, K. Emmanoulopoulos, D. Espigat, P. Farnier, C. Feinstein, F. Fiasson, A. Förster, A. Fontaine, G. Füssling, M. Gabici, S. Gallant, Y.A. Gérard, L. Giebels, B. Glicenstein, J.F. Glück, B. Goret, P. Hadjichristidis, C. Hauser, D. Hauser, M. Heinzelmann, G. Henri, G. Hermann, G. Hinton, J.A. Hoffmann, A. Hofmann, W. Holleran, M. Hoppe, S. Horns, D. Jacholkowska, A. de Jager, O.C. Jung, I. Katarzy'Nski, K. Kendziorra, E. Kerschhaggl, M. Khangulyan, D. Khélifi, B. Keogh, D. Komin, Nu Kosack, K. Lamanna, G. Latham, I.J. Lenain, J.-P. Lohse, T. Martin, J.M. Martineau-Huynh, O. Marcowith, A. Masterson, C. Maurin, D. Mccomb, T.J.L. Moderski, R. Moulin, Emmanuel Naumann-Godo, M. de Naurois, M. Nedbal, D. Nekrassov, D. Nolan, S.J. Ohm, S. Olive, J.-P. de Oña Wilhelmi, E. Orford, K.J. Osborne, J.L. Ostrowski, M. Panter, M. Pedaletti, G. Pelletier, G. Petrucci, P.-O. Pita, S. |
| description | A search for a dark matter (DM) annihilation signal into $\gamma$-rays toward the direction of the Canis Major (CMa) overdensity is presented. The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A total of 9.6 hours of high quality data were collected with the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes (IACTs) and no evidence for a very high energy $\gamma$-ray signal is found. Upper limits on the CMa dwarf galaxy mass of the order of 10$^{9}$ M$_{\odot}$ are derived at the 95% C.L. assuming neutralino masses in the range 500 GeV - 10 TeV and relatively large annihilation cross-sections. Constraints on the velocity-weighted annihilation cross section $$, are calculated for specific WIMP scenarios, using a NFW model for the DM halo profile and taking advantage of numerical simulations of hierarchical structure formation. 95% C.L. exclusion limits of the order of 5 $\times$ 10$^{-24}$ cm$^{3}$ s$^{-1}$ are reached in the 500 GeV - 10 TeV DM particle mass interval, assuming a total halo mass of 3 $\times$ 10$^{8}$ M$_{\odot}$. |
| doi_str_mv | 10.1088/0004-637X/691/1/175 |
| format | Article |
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The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A total of 9.6 hours of high quality data were collected with the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes (IACTs) and no evidence for a very high energy $\gamma$-ray signal is found. Upper limits on the CMa dwarf galaxy mass of the order of 10$^{9}$ M$_{\odot}$ are derived at the 95% C.L. assuming neutralino masses in the range 500 GeV - 10 TeV and relatively large annihilation cross-sections. Constraints on the velocity-weighted annihilation cross section $<\sigma v>$, are calculated for specific WIMP scenarios, using a NFW model for the DM halo profile and taking advantage of numerical simulations of hierarchical structure formation. 95% C.L. exclusion limits of the order of 5 $\times$ 10$^{-24}$ cm$^{3}$ s$^{-1}$ are reached in the 500 GeV - 10 TeV DM particle mass interval, assuming a total halo mass of 3 $\times$ 10$^{8}$ M$_{\odot}$.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/691/1/175</identifier><language>eng</language><publisher>American Astronomical Society</publisher><subject>Astrophysics ; Cosmology and Extra-Galactic Astrophysics ; Physics ; Sciences of the Universe</subject><ispartof>The Astrophysical journal, 2009, Vol.691, p.175-181</ispartof><rights>Distributed under a Creative Commons Attribution 4.0 International 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G.</creatorcontrib><creatorcontrib>Pelletier, G.</creatorcontrib><creatorcontrib>Petrucci, P.-O.</creatorcontrib><creatorcontrib>Pita, S.</creatorcontrib><title>A search for a dark matter annihilation signal towards the Canis Major overdensity with H.E.S.S</title><title>The Astrophysical journal</title><description>A search for a dark matter (DM) annihilation signal into $\gamma$-rays toward the direction of the Canis Major (CMa) overdensity is presented. The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A total of 9.6 hours of high quality data were collected with the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes (IACTs) and no evidence for a very high energy $\gamma$-ray signal is found. Upper limits on the CMa dwarf galaxy mass of the order of 10$^{9}$ M$_{\odot}$ are derived at the 95% C.L. assuming neutralino masses in the range 500 GeV - 10 TeV and relatively large annihilation cross-sections. Constraints on the velocity-weighted annihilation cross section $<\sigma v>$, are calculated for specific WIMP scenarios, using a NFW model for the DM halo profile and taking advantage of numerical simulations of hierarchical structure formation. 95% C.L. exclusion limits of the order of 5 $\times$ 10$^{-24}$ cm$^{3}$ s$^{-1}$ are reached in the 500 GeV - 10 TeV DM particle mass interval, assuming a total halo mass of 3 $\times$ 10$^{8}$ M$_{\odot}$.</description><subject>Astrophysics</subject><subject>Cosmology and Extra-Galactic Astrophysics</subject><subject>Physics</subject><subject>Sciences of the 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search for a dark matter annihilation signal towards the Canis Major overdensity with H.E.S.S</title><author>Aharonian, F. ; Akhperjanian, A.G. ; Barres de Almeida, U. ; Bazer-Bachi, A.R. ; Behera, B. ; Beilicke, M. ; Benbow, W. ; Bernlöhr, K. ; Boisson, C. ; Borrel, V. ; Braun, I. ; Brion, E. ; Brucker, J. ; Bühler, R. ; Bulik, T. ; Büsching, I. ; Boutelier, T. ; Carrigan, S. ; Chadwick, P.M. ; Chaves, R. ; Chounet, L.-M. ; Coignet, G. ; Cornils, R. ; Costamante, L. ; Dalton, M. ; Degrange, B. ; Dickinson, H.J. ; Djannati-Ataï, A. ; Domainko, W. ; Drury, L.O'C. ; Dubois, F. ; Dubus, G. ; Dyks, J. ; Egberts, K. ; Emmanoulopoulos, D. ; Espigat, P. ; Farnier, C. ; Feinstein, F. ; Fiasson, A. ; Förster, A. ; Fontaine, G. ; Füssling, M. ; Gabici, S. ; Gallant, Y.A. ; Gérard, L. ; Giebels, B. ; Glicenstein, J.F. ; Glück, B. ; Goret, P. ; Hadjichristidis, C. ; Hauser, D. ; Hauser, M. ; Heinzelmann, G. ; Henri, G. ; Hermann, G. ; Hinton, J.A. ; Hoffmann, A. ; Hofmann, W. ; Holleran, M. ; Hoppe, S. ; Horns, D. ; Jacholkowska, A. ; de Jager, O.C. ; Jung, I. ; Katarzy'Nski, K. ; Kendziorra, E. ; Kerschhaggl, M. ; Khangulyan, D. ; Khélifi, B. ; Keogh, D. ; Komin, Nu ; Kosack, K. ; Lamanna, G. ; Latham, I.J. ; Lenain, J.-P. ; Lohse, T. ; Martin, J.M. ; Martineau-Huynh, O. ; Marcowith, A. ; Masterson, C. ; Maurin, D. ; Mccomb, T.J.L. ; Moderski, R. ; Moulin, Emmanuel ; Naumann-Godo, M. ; de Naurois, M. ; Nedbal, D. ; Nekrassov, D. ; Nolan, S.J. ; Ohm, S. ; Olive, J.-P. ; de Oña Wilhelmi, E. ; Orford, K.J. ; Osborne, J.L. ; Ostrowski, M. ; Panter, M. ; Pedaletti, G. ; Pelletier, G. ; Petrucci, P.-O. ; Pita, S.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-hal_primary_oai_HAL_in2p3_00324687v13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2009</creationdate><topic>Astrophysics</topic><topic>Cosmology and Extra-Galactic Astrophysics</topic><topic>Physics</topic><topic>Sciences of the Universe</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aharonian, F.</creatorcontrib><creatorcontrib>Akhperjanian, A.G.</creatorcontrib><creatorcontrib>Barres de Almeida, U.</creatorcontrib><creatorcontrib>Bazer-Bachi, A.R.</creatorcontrib><creatorcontrib>Behera, B.</creatorcontrib><creatorcontrib>Beilicke, M.</creatorcontrib><creatorcontrib>Benbow, W.</creatorcontrib><creatorcontrib>Bernlöhr, K.</creatorcontrib><creatorcontrib>Boisson, C.</creatorcontrib><creatorcontrib>Borrel, V.</creatorcontrib><creatorcontrib>Braun, I.</creatorcontrib><creatorcontrib>Brion, E.</creatorcontrib><creatorcontrib>Brucker, J.</creatorcontrib><creatorcontrib>Bühler, R.</creatorcontrib><creatorcontrib>Bulik, T.</creatorcontrib><creatorcontrib>Büsching, I.</creatorcontrib><creatorcontrib>Boutelier, T.</creatorcontrib><creatorcontrib>Carrigan, S.</creatorcontrib><creatorcontrib>Chadwick, P.M.</creatorcontrib><creatorcontrib>Chaves, R.</creatorcontrib><creatorcontrib>Chounet, L.-M.</creatorcontrib><creatorcontrib>Coignet, G.</creatorcontrib><creatorcontrib>Cornils, R.</creatorcontrib><creatorcontrib>Costamante, L.</creatorcontrib><creatorcontrib>Dalton, M.</creatorcontrib><creatorcontrib>Degrange, B.</creatorcontrib><creatorcontrib>Dickinson, H.J.</creatorcontrib><creatorcontrib>Djannati-Ataï, A.</creatorcontrib><creatorcontrib>Domainko, W.</creatorcontrib><creatorcontrib>Drury, L.O'C.</creatorcontrib><creatorcontrib>Dubois, F.</creatorcontrib><creatorcontrib>Dubus, G.</creatorcontrib><creatorcontrib>Dyks, J.</creatorcontrib><creatorcontrib>Egberts, K.</creatorcontrib><creatorcontrib>Emmanoulopoulos, D.</creatorcontrib><creatorcontrib>Espigat, P.</creatorcontrib><creatorcontrib>Farnier, C.</creatorcontrib><creatorcontrib>Feinstein, F.</creatorcontrib><creatorcontrib>Fiasson, A.</creatorcontrib><creatorcontrib>Förster, A.</creatorcontrib><creatorcontrib>Fontaine, G.</creatorcontrib><creatorcontrib>Füssling, 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I.</creatorcontrib><creatorcontrib>Katarzy'Nski, K.</creatorcontrib><creatorcontrib>Kendziorra, E.</creatorcontrib><creatorcontrib>Kerschhaggl, M.</creatorcontrib><creatorcontrib>Khangulyan, D.</creatorcontrib><creatorcontrib>Khélifi, B.</creatorcontrib><creatorcontrib>Keogh, D.</creatorcontrib><creatorcontrib>Komin, Nu</creatorcontrib><creatorcontrib>Kosack, K.</creatorcontrib><creatorcontrib>Lamanna, G.</creatorcontrib><creatorcontrib>Latham, I.J.</creatorcontrib><creatorcontrib>Lenain, J.-P.</creatorcontrib><creatorcontrib>Lohse, T.</creatorcontrib><creatorcontrib>Martin, J.M.</creatorcontrib><creatorcontrib>Martineau-Huynh, O.</creatorcontrib><creatorcontrib>Marcowith, A.</creatorcontrib><creatorcontrib>Masterson, C.</creatorcontrib><creatorcontrib>Maurin, D.</creatorcontrib><creatorcontrib>Mccomb, T.J.L.</creatorcontrib><creatorcontrib>Moderski, R.</creatorcontrib><creatorcontrib>Moulin, Emmanuel</creatorcontrib><creatorcontrib>Naumann-Godo, M.</creatorcontrib><creatorcontrib>de Naurois, M.</creatorcontrib><creatorcontrib>Nedbal, D.</creatorcontrib><creatorcontrib>Nekrassov, D.</creatorcontrib><creatorcontrib>Nolan, S.J.</creatorcontrib><creatorcontrib>Ohm, S.</creatorcontrib><creatorcontrib>Olive, J.-P.</creatorcontrib><creatorcontrib>de Oña Wilhelmi, E.</creatorcontrib><creatorcontrib>Orford, K.J.</creatorcontrib><creatorcontrib>Osborne, J.L.</creatorcontrib><creatorcontrib>Ostrowski, M.</creatorcontrib><creatorcontrib>Panter, M.</creatorcontrib><creatorcontrib>Pedaletti, G.</creatorcontrib><creatorcontrib>Pelletier, G.</creatorcontrib><creatorcontrib>Petrucci, P.-O.</creatorcontrib><creatorcontrib>Pita, S.</creatorcontrib><collection>Hyper Article en Ligne (HAL)</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Aharonian, F.</au><au>Akhperjanian, A.G.</au><au>Barres de Almeida, U.</au><au>Bazer-Bachi, A.R.</au><au>Behera, B.</au><au>Beilicke, M.</au><au>Benbow, W.</au><au>Bernlöhr, K.</au><au>Boisson, C.</au><au>Borrel, V.</au><au>Braun, I.</au><au>Brion, E.</au><au>Brucker, J.</au><au>Bühler, R.</au><au>Bulik, T.</au><au>Büsching, I.</au><au>Boutelier, T.</au><au>Carrigan, S.</au><au>Chadwick, P.M.</au><au>Chaves, R.</au><au>Chounet, L.-M.</au><au>Coignet, G.</au><au>Cornils, R.</au><au>Costamante, L.</au><au>Dalton, M.</au><au>Degrange, B.</au><au>Dickinson, H.J.</au><au>Djannati-Ataï, A.</au><au>Domainko, W.</au><au>Drury, L.O'C.</au><au>Dubois, F.</au><au>Dubus, G.</au><au>Dyks, J.</au><au>Egberts, K.</au><au>Emmanoulopoulos, D.</au><au>Espigat, P.</au><au>Farnier, C.</au><au>Feinstein, F.</au><au>Fiasson, A.</au><au>Förster, A.</au><au>Fontaine, G.</au><au>Füssling, M.</au><au>Gabici, S.</au><au>Gallant, Y.A.</au><au>Gérard, L.</au><au>Giebels, B.</au><au>Glicenstein, J.F.</au><au>Glück, B.</au><au>Goret, P.</au><au>Hadjichristidis, C.</au><au>Hauser, D.</au><au>Hauser, M.</au><au>Heinzelmann, G.</au><au>Henri, G.</au><au>Hermann, G.</au><au>Hinton, J.A.</au><au>Hoffmann, A.</au><au>Hofmann, W.</au><au>Holleran, M.</au><au>Hoppe, S.</au><au>Horns, D.</au><au>Jacholkowska, A.</au><au>de Jager, O.C.</au><au>Jung, I.</au><au>Katarzy'Nski, K.</au><au>Kendziorra, E.</au><au>Kerschhaggl, M.</au><au>Khangulyan, D.</au><au>Khélifi, B.</au><au>Keogh, D.</au><au>Komin, Nu</au><au>Kosack, K.</au><au>Lamanna, G.</au><au>Latham, I.J.</au><au>Lenain, J.-P.</au><au>Lohse, T.</au><au>Martin, J.M.</au><au>Martineau-Huynh, O.</au><au>Marcowith, A.</au><au>Masterson, C.</au><au>Maurin, D.</au><au>Mccomb, T.J.L.</au><au>Moderski, R.</au><au>Moulin, Emmanuel</au><au>Naumann-Godo, M.</au><au>de Naurois, M.</au><au>Nedbal, D.</au><au>Nekrassov, D.</au><au>Nolan, S.J.</au><au>Ohm, S.</au><au>Olive, J.-P.</au><au>de Oña Wilhelmi, E.</au><au>Orford, K.J.</au><au>Osborne, J.L.</au><au>Ostrowski, M.</au><au>Panter, M.</au><au>Pedaletti, G.</au><au>Pelletier, G.</au><au>Petrucci, P.-O.</au><au>Pita, S.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A search for a dark matter annihilation signal towards the Canis Major overdensity with H.E.S.S</atitle><jtitle>The Astrophysical journal</jtitle><date>2009</date><risdate>2009</risdate><volume>691</volume><spage>175</spage><epage>181</epage><pages>175-181</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>A search for a dark matter (DM) annihilation signal into $\gamma$-rays toward the direction of the Canis Major (CMa) overdensity is presented. The nature of CMa is still controversial and one scenario represents it as a dwarf galaxy, making it an interesting candidate for DM annihilation searches. A total of 9.6 hours of high quality data were collected with the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes (IACTs) and no evidence for a very high energy $\gamma$-ray signal is found. Upper limits on the CMa dwarf galaxy mass of the order of 10$^{9}$ M$_{\odot}$ are derived at the 95% C.L. assuming neutralino masses in the range 500 GeV - 10 TeV and relatively large annihilation cross-sections. Constraints on the velocity-weighted annihilation cross section $<\sigma v>$, are calculated for specific WIMP scenarios, using a NFW model for the DM halo profile and taking advantage of numerical simulations of hierarchical structure formation. 95% C.L. exclusion limits of the order of 5 $\times$ 10$^{-24}$ cm$^{3}$ s$^{-1}$ are reached in the 500 GeV - 10 TeV DM particle mass interval, assuming a total halo mass of 3 $\times$ 10$^{8}$ M$_{\odot}$.</abstract><pub>American Astronomical Society</pub><doi>10.1088/0004-637X/691/1/175</doi><orcidid>https://orcid.org/0000-0002-9751-7633</orcidid><orcidid>https://orcid.org/0000-0001-8424-3621</orcidid><orcidid>https://orcid.org/0000-0002-9199-7031</orcidid><orcidid>https://orcid.org/0000-0002-4710-2165</orcidid><orcidid>https://orcid.org/0000-0002-7576-7869</orcidid><orcidid>https://orcid.org/0000-0001-8065-3252</orcidid><orcidid>https://orcid.org/0000-0002-4388-5625</orcidid><orcidid>https://orcid.org/0000-0001-5893-1797</orcidid><orcidid>https://orcid.org/0000-0001-6061-3480</orcidid><orcidid>https://orcid.org/0000-0002-2203-4880</orcidid><orcidid>https://orcid.org/0000-0003-1157-3915</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0003-0452-3805</orcidid><orcidid>https://orcid.org/0000-0001-9077-4058</orcidid><orcidid>https://orcid.org/0000-0002-6204-0409</orcidid><orcidid>https://orcid.org/0000-0002-5130-2514</orcidid><orcidid>https://orcid.org/0000-0003-4187-9560</orcidid><orcidid>https://orcid.org/0000-0002-7245-201X</orcidid><orcidid>https://orcid.org/0000-0003-3280-0582</orcidid><orcidid>https://orcid.org/0000-0003-1334-2993</orcidid><orcidid>https://orcid.org/0000-0002-3474-2243</orcidid><orcidid>https://orcid.org/0000-0002-1229-278X</orcidid><orcidid>https://orcid.org/0000-0003-1945-0119</orcidid><orcidid>https://orcid.org/0000-0002-5331-0606</orcidid><orcidid>https://orcid.org/0000-0002-2666-4812</orcidid><orcidid>https://orcid.org/0000-0002-3971-0910</orcidid><orcidid>https://orcid.org/0000-0001-9669-645X</orcidid><orcidid>https://orcid.org/0000-0002-9516-1581</orcidid><orcidid>https://orcid.org/0000-0003-1187-4240</orcidid><orcidid>https://orcid.org/0000-0001-7284-9220</orcidid><orcidid>https://orcid.org/0000-0002-7576-7869</orcidid><orcidid>https://orcid.org/0000-0001-8424-3621</orcidid><orcidid>https://orcid.org/0000-0001-7284-9220</orcidid><orcidid>https://orcid.org/0000-0003-1157-3915</orcidid><orcidid>https://orcid.org/0000-0003-3280-0582</orcidid><orcidid>https://orcid.org/0000-0002-9751-7633</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0002-5331-0606</orcidid><orcidid>https://orcid.org/0000-0002-3971-0910</orcidid><orcidid>https://orcid.org/0000-0001-8065-3252</orcidid><orcidid>https://orcid.org/0000-0002-9199-7031</orcidid><orcidid>https://orcid.org/0000-0003-1945-0119</orcidid><orcidid>https://orcid.org/0000-0001-6061-3480</orcidid><orcidid>https://orcid.org/0000-0002-5130-2514</orcidid><orcidid>https://orcid.org/0000-0001-5893-1797</orcidid><orcidid>https://orcid.org/0000-0002-6204-0409</orcidid><orcidid>https://orcid.org/0000-0003-1187-4240</orcidid><orcidid>https://orcid.org/0000-0002-7245-201X</orcidid><orcidid>https://orcid.org/0000-0002-3474-2243</orcidid></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2009, Vol.691, p.175-181 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_in2p3_00324687v1 |
| source | IOP Publishing Free Content; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astrophysics Cosmology and Extra-Galactic Astrophysics Physics Sciences of the Universe |
| title | A search for a dark matter annihilation signal towards the Canis Major overdensity with H.E.S.S |
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