Probing the very high energy γ-ray spectral curvature in the blazar PG 1553+113 with the MAGIC telescopes
PG 1553+113 is a very high energy (VHE, E > 100 GeV) γ-ray emitter classified as a BL Lac object. Its redshift is constrained by intergalactic absorption lines in the range 0.4
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| Veröffentlicht in: | Monthly Notices of the Royal Astronomical Society 2015-07, Vol.450 (4), p.4399-4410 |
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| creator | Aleksić, J Ansoldi, S Babic, A Bangale, P Barrio, J. A Becerra González, J Bednarek, W Bernardini, E Biasuzzi, B Biland, A Bonnefoy, S Bonnoli, G Carmona, E Carosi, A Colin, P Contreras, J. L Cortina, J Covino, S Da Vela, P Dazzi, F De Lotto, B de Oña Wilhelmi, E Delgado Mendez, C Dominis Prester, D Doro, M Einecke, S Elsaesser, D Fidalgo, D Font, L Frantzen, K Fruck, C García López, R. J Garczarczyk, M Garrido Terrats, D Godinović, N González Muñoz, A Gozzini, S. R Hadasch, D Herrera, J Hose, J Hrupec, D Idec, W Kellermann, H Knoetig, M. L Krause, J La Barbera, A Lewandowska, N Lindfors, E Longo, F López, M López-Oramas, A Lorenz, E Makariev, M Maneva, G Maraschi, L Martínez, M Miranda, J. M Mirzoyan, R Moralejo, A Munar-Adrover, P Neustroev, V Niedzwiecki, A Nilsson, K Orito, R Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes-Fortuny, X Poutanen, J Reinthal, R Rhode, W Rügamer, S Saito, T Scalzotto, V Scapin, V Schultz, C Schweizer, T Sillanpää, A Sitarek, J Snidaric, I Stamerra, A Storz, J Strzys, M Takalo, L Tavecchio, F Terzić, T Tescaro, D Teshima, M Toyama, T Vogler, P Will, M Zanin, R Collaboration), (The MAGIC D'Ammando, F Buson, S Lähteenmäki, A Hovatta, T Readhead, A. C. S Richards, J. L |
| description | PG 1553+113 is a very high energy (VHE, E > 100 GeV) γ-ray emitter classified as a BL Lac object. Its redshift is constrained by intergalactic absorption lines in the range 0.4 |
| doi_str_mv | 10.1093/mnras/stv811 |
| format | Article |
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A ; Becerra González, J ; Bednarek, W ; Bernardini, E ; Biasuzzi, B ; Biland, A ; Bonnefoy, S ; Bonnoli, G ; Carmona, E ; Carosi, A ; Colin, P ; Contreras, J. L ; Cortina, J ; Covino, S ; Da Vela, P ; Dazzi, F ; De Lotto, B ; de Oña Wilhelmi, E ; Delgado Mendez, C ; Dominis Prester, D ; Doro, M ; Einecke, S ; Elsaesser, D ; Fidalgo, D ; Font, L ; Frantzen, K ; Fruck, C ; García López, R. J ; Garczarczyk, M ; Garrido Terrats, D ; Godinović, N ; González Muñoz, A ; Gozzini, S. R ; Hadasch, D ; Herrera, J ; Hose, J ; Hrupec, D ; Idec, W ; Kellermann, H ; Knoetig, M. L ; Krause, J ; La Barbera, A ; Lewandowska, N ; Lindfors, E ; Longo, F ; López, M ; López-Oramas, A ; Lorenz, E ; Makariev, M ; Maneva, G ; Maraschi, L ; Martínez, M ; Miranda, J. M ; Mirzoyan, R ; Moralejo, A ; Munar-Adrover, P ; Neustroev, V ; Niedzwiecki, A ; Nilsson, K ; Orito, R ; Paiano, S ; Palatiello, M ; Paneque, D ; Paoletti, R ; Paredes-Fortuny, X ; Poutanen, J ; Reinthal, R ; Rhode, W ; Rügamer, S ; Saito, T ; Scalzotto, V ; Scapin, V ; Schultz, C ; Schweizer, T ; Sillanpää, A ; Sitarek, J ; Snidaric, I ; Stamerra, A ; Storz, J ; Strzys, M ; Takalo, L ; Tavecchio, F ; Terzić, T ; Tescaro, D ; Teshima, M ; Toyama, T ; Vogler, P ; Will, M ; Zanin, R ; Collaboration), (The MAGIC ; D'Ammando, F ; Buson, S ; Lähteenmäki, A ; Hovatta, T ; Readhead, A. C. S ; Richards, J. L</creator><creatorcontrib>Aleksić, J ; Ansoldi, S ; Babic, A ; Bangale, P ; Barrio, J. A ; Becerra González, J ; Bednarek, W ; Bernardini, E ; Biasuzzi, B ; Biland, A ; Bonnefoy, S ; Bonnoli, G ; Carmona, E ; Carosi, A ; Colin, P ; Contreras, J. L ; Cortina, J ; Covino, S ; Da Vela, P ; Dazzi, F ; De Lotto, B ; de Oña Wilhelmi, E ; Delgado Mendez, C ; Dominis Prester, D ; Doro, M ; Einecke, S ; Elsaesser, D ; Fidalgo, D ; Font, L ; Frantzen, K ; Fruck, C ; García López, R. J ; Garczarczyk, M ; Garrido Terrats, D ; Godinović, N ; González Muñoz, A ; Gozzini, S. R ; Hadasch, D ; Herrera, J ; Hose, J ; Hrupec, D ; Idec, W ; Kellermann, H ; Knoetig, M. L ; Krause, J ; La Barbera, A ; Lewandowska, N ; Lindfors, E ; Longo, F ; López, M ; López-Oramas, A ; Lorenz, E ; Makariev, M ; Maneva, G ; Maraschi, L ; Martínez, M ; Miranda, J. M ; Mirzoyan, R ; Moralejo, A ; Munar-Adrover, P ; Neustroev, V ; Niedzwiecki, A ; Nilsson, K ; Orito, R ; Paiano, S ; Palatiello, M ; Paneque, D ; Paoletti, R ; Paredes-Fortuny, X ; Poutanen, J ; Reinthal, R ; Rhode, W ; Rügamer, S ; Saito, T ; Scalzotto, V ; Scapin, V ; Schultz, C ; Schweizer, T ; Sillanpää, A ; Sitarek, J ; Snidaric, I ; Stamerra, A ; Storz, J ; Strzys, M ; Takalo, L ; Tavecchio, F ; Terzić, T ; Tescaro, D ; Teshima, M ; Toyama, T ; Vogler, P ; Will, M ; Zanin, R ; Collaboration), (The MAGIC ; D'Ammando, F ; Buson, S ; Lähteenmäki, A ; Hovatta, T ; Readhead, A. C. S ; Richards, J. L ; for the Fermi-LAT Collaboration ; SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><description>PG 1553+113 is a very high energy (VHE, E > 100 GeV) γ-ray emitter classified as a BL Lac object. Its redshift is constrained by intergalactic absorption lines in the range 0.4 < z < 0.58. The MAGIC telescopes have monitored the source's activity since 2005. In early 2012, PG 1553+113 was found in a high state, and later, in April of the same year, the source reached its highest VHE flux state detected so far. Simultaneous observations carried out in X-rays during 2012 April show similar flaring behaviour. In contrast, the γ-ray flux at E < 100 GeV observed by Fermi-LAT is compatible with steady emission. In this paper, a detailed study of the flaring state is presented. The VHE spectrum shows clear curvature, being well fitted either by a power law with an exponential cut-off or by a log-parabola. A simple power-law fit hypothesis for the observed shape of the PG 1553+113 VHE γ-ray spectrum is rejected with a high significance (fit probability P = 2.6 × 10−6). The observed curvature is compatible with the extragalactic background light (EBL) imprint predicted by current generation EBL models assuming a redshift z ∼ 0.4. New constraints on the redshift are derived from the VHE spectrum. These constraints are compatible with previous limits and suggest that the source is most likely located around the optical lower limit, z = 0.4, based on the detection of Lyα absorption. Finally, we find that the synchrotron self-Compton model gives a satisfactory description of the observed multiwavelength spectral energy distribution during the flare.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stv811</identifier><language>eng</language><publisher>United States: Oxford University Press</publisher><subject>AGNs ; blazar ; Compatibility ; Curvature ; Flares ; Flux ; gamma rays ; INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY ; Mathematical analysis ; Mathematical models ; PG 1553+113 ; Red shift ; Telescopes</subject><ispartof>Monthly Notices of the Royal Astronomical Society, 2015-07, Vol.450 (4), p.4399-4410</ispartof><rights>2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c434t-de99e55a3a872b725405d0dcdf768f8903da982544d7ddb3ea25abcf28bc7fe53</citedby><cites>FETCH-LOGICAL-c434t-de99e55a3a872b725405d0dcdf768f8903da982544d7ddb3ea25abcf28bc7fe53</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stv811$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc><backlink>$$Uhttps://www.osti.gov/servlets/purl/1354935$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Aleksić, J</creatorcontrib><creatorcontrib>Ansoldi, S</creatorcontrib><creatorcontrib>Babic, A</creatorcontrib><creatorcontrib>Bangale, P</creatorcontrib><creatorcontrib>Barrio, J. 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C. S</creatorcontrib><creatorcontrib>Richards, J. L</creatorcontrib><creatorcontrib>for the Fermi-LAT Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><title>Probing the very high energy γ-ray spectral curvature in the blazar PG 1553+113 with the MAGIC telescopes</title><title>Monthly Notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>PG 1553+113 is a very high energy (VHE, E > 100 GeV) γ-ray emitter classified as a BL Lac object. Its redshift is constrained by intergalactic absorption lines in the range 0.4 < z < 0.58. The MAGIC telescopes have monitored the source's activity since 2005. In early 2012, PG 1553+113 was found in a high state, and later, in April of the same year, the source reached its highest VHE flux state detected so far. Simultaneous observations carried out in X-rays during 2012 April show similar flaring behaviour. In contrast, the γ-ray flux at E < 100 GeV observed by Fermi-LAT is compatible with steady emission. In this paper, a detailed study of the flaring state is presented. The VHE spectrum shows clear curvature, being well fitted either by a power law with an exponential cut-off or by a log-parabola. A simple power-law fit hypothesis for the observed shape of the PG 1553+113 VHE γ-ray spectrum is rejected with a high significance (fit probability P = 2.6 × 10−6). The observed curvature is compatible with the extragalactic background light (EBL) imprint predicted by current generation EBL models assuming a redshift z ∼ 0.4. New constraints on the redshift are derived from the VHE spectrum. These constraints are compatible with previous limits and suggest that the source is most likely located around the optical lower limit, z = 0.4, based on the detection of Lyα absorption. Finally, we find that the synchrotron self-Compton model gives a satisfactory description of the observed multiwavelength spectral energy distribution during the flare.</description><subject>AGNs</subject><subject>blazar</subject><subject>Compatibility</subject><subject>Curvature</subject><subject>Flares</subject><subject>Flux</subject><subject>gamma rays</subject><subject>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</subject><subject>Mathematical analysis</subject><subject>Mathematical models</subject><subject>PG 1553+113</subject><subject>Red shift</subject><subject>Telescopes</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqN0UtOwzAQBmALgUQp7DiAxQYkCLXjOLGXVQUFqYguYG05zqRJlSbBdorKtbgHZyJ9rBErS-NvRjP6Ebqk5J4SyUar2mo3cn4tKD1CA8piHoQyjo_RgBDGA5FQeorOnFsSQiIWxgO0nNsmLesF9gXgNdgNLspFgaEGu9jgn-_A6g12LRhvdYVNZ9fadxZwWe860kp_aYvnU0w5Z7eUMvxZ-mL39zKePk-whwqcaVpw5-gk15WDi8M7RO-PD2-Tp2D22sPxLDARi3yQgZTAuWZaJGGahDwiPCOZyfIkFrmQhGVair4cZUmWpQx0yHVq8lCkJsmBsyG62s9tnC-VM6UHU5imrvsjFGU8kmyLbvaotc1HB86rVekMVJWuoemcogmRSShILP5DaSSJoFFP7_bU2MY5C7lqbbnSdqMoUduI1C4itY-o59eHTbv2b_kLmCyTAA</recordid><startdate>20150711</startdate><enddate>20150711</enddate><creator>Aleksić, J</creator><creator>Ansoldi, S</creator><creator>Babic, A</creator><creator>Bangale, P</creator><creator>Barrio, J. 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C. S</creator><creator>Richards, J. L</creator><general>Oxford University Press</general><general>Royal Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OIOZB</scope><scope>OTOTI</scope></search><sort><creationdate>20150711</creationdate><title>Probing the very high energy γ-ray spectral curvature in the blazar PG 1553+113 with the MAGIC telescopes</title><author>Aleksić, J ; Ansoldi, S ; Babic, A ; Bangale, P ; Barrio, J. A ; Becerra González, J ; Bednarek, W ; Bernardini, E ; Biasuzzi, B ; Biland, A ; Bonnefoy, S ; Bonnoli, G ; Carmona, E ; Carosi, A ; Colin, P ; Contreras, J. L ; Cortina, J ; Covino, S ; Da Vela, P ; Dazzi, F ; De Lotto, B ; de Oña Wilhelmi, E ; Delgado Mendez, C ; Dominis Prester, D ; Doro, M ; Einecke, S ; Elsaesser, D ; Fidalgo, D ; Font, L ; Frantzen, K ; Fruck, C ; García López, R. J ; Garczarczyk, M ; Garrido Terrats, D ; Godinović, N ; González Muñoz, A ; Gozzini, S. R ; Hadasch, D ; Herrera, J ; Hose, J ; Hrupec, D ; Idec, W ; Kellermann, H ; Knoetig, M. L ; Krause, J ; La Barbera, A ; Lewandowska, N ; Lindfors, E ; Longo, F ; López, M ; López-Oramas, A ; Lorenz, E ; Makariev, M ; Maneva, G ; Maraschi, L ; Martínez, M ; Miranda, J. M ; Mirzoyan, R ; Moralejo, A ; Munar-Adrover, P ; Neustroev, V ; Niedzwiecki, A ; Nilsson, K ; Orito, R ; Paiano, S ; Palatiello, M ; Paneque, D ; Paoletti, R ; Paredes-Fortuny, X ; Poutanen, J ; Reinthal, R ; Rhode, W ; Rügamer, S ; Saito, T ; Scalzotto, V ; Scapin, V ; Schultz, C ; Schweizer, T ; Sillanpää, A ; Sitarek, J ; Snidaric, I ; Stamerra, A ; Storz, J ; Strzys, M ; Takalo, L ; Tavecchio, F ; Terzić, T ; Tescaro, D ; Teshima, M ; Toyama, T ; Vogler, P ; Will, M ; Zanin, R ; Collaboration), (The MAGIC ; D'Ammando, F ; Buson, S ; Lähteenmäki, A ; Hovatta, T ; Readhead, A. C. S ; Richards, J. L</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c434t-de99e55a3a872b725405d0dcdf768f8903da982544d7ddb3ea25abcf28bc7fe53</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>AGNs</topic><topic>blazar</topic><topic>Compatibility</topic><topic>Curvature</topic><topic>Flares</topic><topic>Flux</topic><topic>gamma rays</topic><topic>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</topic><topic>Mathematical analysis</topic><topic>Mathematical models</topic><topic>PG 1553+113</topic><topic>Red shift</topic><topic>Telescopes</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aleksić, J</creatorcontrib><creatorcontrib>Ansoldi, S</creatorcontrib><creatorcontrib>Babic, A</creatorcontrib><creatorcontrib>Bangale, P</creatorcontrib><creatorcontrib>Barrio, J. A</creatorcontrib><creatorcontrib>Becerra González, J</creatorcontrib><creatorcontrib>Bednarek, W</creatorcontrib><creatorcontrib>Bernardini, E</creatorcontrib><creatorcontrib>Biasuzzi, B</creatorcontrib><creatorcontrib>Biland, A</creatorcontrib><creatorcontrib>Bonnefoy, S</creatorcontrib><creatorcontrib>Bonnoli, G</creatorcontrib><creatorcontrib>Carmona, E</creatorcontrib><creatorcontrib>Carosi, A</creatorcontrib><creatorcontrib>Colin, P</creatorcontrib><creatorcontrib>Contreras, J. 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R</creatorcontrib><creatorcontrib>Hadasch, D</creatorcontrib><creatorcontrib>Herrera, J</creatorcontrib><creatorcontrib>Hose, J</creatorcontrib><creatorcontrib>Hrupec, D</creatorcontrib><creatorcontrib>Idec, W</creatorcontrib><creatorcontrib>Kellermann, H</creatorcontrib><creatorcontrib>Knoetig, M. L</creatorcontrib><creatorcontrib>Krause, J</creatorcontrib><creatorcontrib>La Barbera, A</creatorcontrib><creatorcontrib>Lewandowska, N</creatorcontrib><creatorcontrib>Lindfors, E</creatorcontrib><creatorcontrib>Longo, F</creatorcontrib><creatorcontrib>López, M</creatorcontrib><creatorcontrib>López-Oramas, A</creatorcontrib><creatorcontrib>Lorenz, E</creatorcontrib><creatorcontrib>Makariev, M</creatorcontrib><creatorcontrib>Maneva, G</creatorcontrib><creatorcontrib>Maraschi, L</creatorcontrib><creatorcontrib>Martínez, M</creatorcontrib><creatorcontrib>Miranda, J. M</creatorcontrib><creatorcontrib>Mirzoyan, R</creatorcontrib><creatorcontrib>Moralejo, A</creatorcontrib><creatorcontrib>Munar-Adrover, P</creatorcontrib><creatorcontrib>Neustroev, V</creatorcontrib><creatorcontrib>Niedzwiecki, A</creatorcontrib><creatorcontrib>Nilsson, K</creatorcontrib><creatorcontrib>Orito, R</creatorcontrib><creatorcontrib>Paiano, S</creatorcontrib><creatorcontrib>Palatiello, M</creatorcontrib><creatorcontrib>Paneque, D</creatorcontrib><creatorcontrib>Paoletti, R</creatorcontrib><creatorcontrib>Paredes-Fortuny, X</creatorcontrib><creatorcontrib>Poutanen, J</creatorcontrib><creatorcontrib>Reinthal, R</creatorcontrib><creatorcontrib>Rhode, W</creatorcontrib><creatorcontrib>Rügamer, S</creatorcontrib><creatorcontrib>Saito, T</creatorcontrib><creatorcontrib>Scalzotto, V</creatorcontrib><creatorcontrib>Scapin, V</creatorcontrib><creatorcontrib>Schultz, C</creatorcontrib><creatorcontrib>Schweizer, T</creatorcontrib><creatorcontrib>Sillanpää, A</creatorcontrib><creatorcontrib>Sitarek, J</creatorcontrib><creatorcontrib>Snidaric, I</creatorcontrib><creatorcontrib>Stamerra, A</creatorcontrib><creatorcontrib>Storz, J</creatorcontrib><creatorcontrib>Strzys, M</creatorcontrib><creatorcontrib>Takalo, L</creatorcontrib><creatorcontrib>Tavecchio, F</creatorcontrib><creatorcontrib>Terzić, T</creatorcontrib><creatorcontrib>Tescaro, D</creatorcontrib><creatorcontrib>Teshima, M</creatorcontrib><creatorcontrib>Toyama, T</creatorcontrib><creatorcontrib>Vogler, P</creatorcontrib><creatorcontrib>Will, M</creatorcontrib><creatorcontrib>Zanin, R</creatorcontrib><creatorcontrib>Collaboration), (The MAGIC</creatorcontrib><creatorcontrib>D'Ammando, F</creatorcontrib><creatorcontrib>Buson, S</creatorcontrib><creatorcontrib>Lähteenmäki, A</creatorcontrib><creatorcontrib>Hovatta, T</creatorcontrib><creatorcontrib>Readhead, A. C. S</creatorcontrib><creatorcontrib>Richards, J. L</creatorcontrib><creatorcontrib>for the Fermi-LAT Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Monthly Notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Aleksić, J</au><au>Ansoldi, S</au><au>Babic, A</au><au>Bangale, P</au><au>Barrio, J. A</au><au>Becerra González, J</au><au>Bednarek, W</au><au>Bernardini, E</au><au>Biasuzzi, B</au><au>Biland, A</au><au>Bonnefoy, S</au><au>Bonnoli, G</au><au>Carmona, E</au><au>Carosi, A</au><au>Colin, P</au><au>Contreras, J. L</au><au>Cortina, J</au><au>Covino, S</au><au>Da Vela, P</au><au>Dazzi, F</au><au>De Lotto, B</au><au>de Oña Wilhelmi, E</au><au>Delgado Mendez, C</au><au>Dominis Prester, D</au><au>Doro, M</au><au>Einecke, S</au><au>Elsaesser, D</au><au>Fidalgo, D</au><au>Font, L</au><au>Frantzen, K</au><au>Fruck, C</au><au>García López, R. J</au><au>Garczarczyk, M</au><au>Garrido Terrats, D</au><au>Godinović, N</au><au>González Muñoz, A</au><au>Gozzini, S. R</au><au>Hadasch, D</au><au>Herrera, J</au><au>Hose, J</au><au>Hrupec, D</au><au>Idec, W</au><au>Kellermann, H</au><au>Knoetig, M. L</au><au>Krause, J</au><au>La Barbera, A</au><au>Lewandowska, N</au><au>Lindfors, E</au><au>Longo, F</au><au>López, M</au><au>López-Oramas, A</au><au>Lorenz, E</au><au>Makariev, M</au><au>Maneva, G</au><au>Maraschi, L</au><au>Martínez, M</au><au>Miranda, J. M</au><au>Mirzoyan, R</au><au>Moralejo, A</au><au>Munar-Adrover, P</au><au>Neustroev, V</au><au>Niedzwiecki, A</au><au>Nilsson, K</au><au>Orito, R</au><au>Paiano, S</au><au>Palatiello, M</au><au>Paneque, D</au><au>Paoletti, R</au><au>Paredes-Fortuny, X</au><au>Poutanen, J</au><au>Reinthal, R</au><au>Rhode, W</au><au>Rügamer, S</au><au>Saito, T</au><au>Scalzotto, V</au><au>Scapin, V</au><au>Schultz, C</au><au>Schweizer, T</au><au>Sillanpää, A</au><au>Sitarek, J</au><au>Snidaric, I</au><au>Stamerra, A</au><au>Storz, J</au><au>Strzys, M</au><au>Takalo, L</au><au>Tavecchio, F</au><au>Terzić, T</au><au>Tescaro, D</au><au>Teshima, M</au><au>Toyama, T</au><au>Vogler, P</au><au>Will, M</au><au>Zanin, R</au><au>Collaboration), (The MAGIC</au><au>D'Ammando, F</au><au>Buson, S</au><au>Lähteenmäki, A</au><au>Hovatta, T</au><au>Readhead, A. C. S</au><au>Richards, J. L</au><aucorp>for the Fermi-LAT Collaboration</aucorp><aucorp>SLAC National Accelerator Lab., Menlo Park, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Probing the very high energy γ-ray spectral curvature in the blazar PG 1553+113 with the MAGIC telescopes</atitle><jtitle>Monthly Notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2015-07-11</date><risdate>2015</risdate><volume>450</volume><issue>4</issue><spage>4399</spage><epage>4410</epage><pages>4399-4410</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>PG 1553+113 is a very high energy (VHE, E > 100 GeV) γ-ray emitter classified as a BL Lac object. Its redshift is constrained by intergalactic absorption lines in the range 0.4 < z < 0.58. The MAGIC telescopes have monitored the source's activity since 2005. In early 2012, PG 1553+113 was found in a high state, and later, in April of the same year, the source reached its highest VHE flux state detected so far. Simultaneous observations carried out in X-rays during 2012 April show similar flaring behaviour. In contrast, the γ-ray flux at E < 100 GeV observed by Fermi-LAT is compatible with steady emission. In this paper, a detailed study of the flaring state is presented. The VHE spectrum shows clear curvature, being well fitted either by a power law with an exponential cut-off or by a log-parabola. A simple power-law fit hypothesis for the observed shape of the PG 1553+113 VHE γ-ray spectrum is rejected with a high significance (fit probability P = 2.6 × 10−6). The observed curvature is compatible with the extragalactic background light (EBL) imprint predicted by current generation EBL models assuming a redshift z ∼ 0.4. New constraints on the redshift are derived from the VHE spectrum. These constraints are compatible with previous limits and suggest that the source is most likely located around the optical lower limit, z = 0.4, based on the detection of Lyα absorption. Finally, we find that the synchrotron self-Compton model gives a satisfactory description of the observed multiwavelength spectral energy distribution during the flare.</abstract><cop>United States</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stv811</doi><tpages>12</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly Notices of the Royal Astronomical Society, 2015-07, Vol.450 (4), p.4399-4410 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1354935 |
| source | Oxford Journals Open Access Collection |
| subjects | AGNs blazar Compatibility Curvature Flares Flux gamma rays INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY Mathematical analysis Mathematical models PG 1553+113 Red shift Telescopes |
| title | Probing the very high energy γ-ray spectral curvature in the blazar PG 1553+113 with the MAGIC telescopes |
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