EMITTING ELECTRONS AND SOURCE ACTIVITY IN MARKARIAN 501
We study the variation of the broadband spectral energy distribution (SED) of the BL Lac object Mrk 501 as a function of source activity, from quiescent to flaring. Through chi super(2)-minimization we model eight simultaneous SED data sets with a one-zone synchrotron self-Compton (SSC) model, and e...
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| Veröffentlicht in: | The Astrophysical journal 2012-07, Vol.753 (2), p.1-7 |
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| container_title | The Astrophysical journal |
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| creator | Mankuzhiyil, Nijil Ansoldi, Stefano Persic, Massimo Rivers, Elizabeth Rothschild, Richard Tavecchio, Fabrizio |
| description | We study the variation of the broadband spectral energy distribution (SED) of the BL Lac object Mrk 501 as a function of source activity, from quiescent to flaring. Through chi super(2)-minimization we model eight simultaneous SED data sets with a one-zone synchrotron self-Compton (SSC) model, and examine how model parameters vary with source activity. The emerging variability pattern of Mrk 501 is complex, with the Compton component arising from gamma -e scatterings that sometimes are (mostly) Thomson and sometimes (mostly) extreme Klein-Nishina. This can be seen from the variation of the Compton to synchrotron peak distance according to source state. The underlying electron spectra are faint/soft in quiescent states and bright/hard in flaring states. A comparison with Mrk 421 suggests that the typical values of the SSC parameters are different in the two sources: however, in both jets the energy density is particle-dominated in all states. |
| doi_str_mv | 10.1088/0004-637X/753/2/154 |
| format | Article |
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Through chi super(2)-minimization we model eight simultaneous SED data sets with a one-zone synchrotron self-Compton (SSC) model, and examine how model parameters vary with source activity. The emerging variability pattern of Mrk 501 is complex, with the Compton component arising from gamma -e scatterings that sometimes are (mostly) Thomson and sometimes (mostly) extreme Klein-Nishina. This can be seen from the variation of the Compton to synchrotron peak distance according to source state. The underlying electron spectra are faint/soft in quiescent states and bright/hard in flaring states. 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Through chi super(2)-minimization we model eight simultaneous SED data sets with a one-zone synchrotron self-Compton (SSC) model, and examine how model parameters vary with source activity. The emerging variability pattern of Mrk 501 is complex, with the Compton component arising from gamma -e scatterings that sometimes are (mostly) Thomson and sometimes (mostly) extreme Klein-Nishina. This can be seen from the variation of the Compton to synchrotron peak distance according to source state. The underlying electron spectra are faint/soft in quiescent states and bright/hard in flaring states. A comparison with Mrk 421 suggests that the typical values of the SSC parameters are different in the two sources: however, in both jets the energy density is particle-dominated in all states.</description><subject>ASTRONOMY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>BL LACERTAE OBJECTS</subject><subject>Broadband</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>COMPTON EFFECT</subject><subject>COSMIC ELECTRONS</subject><subject>DISTANCE</subject><subject>Elastic scattering</subject><subject>ELECTRON SPECTRA</subject><subject>ENERGY DENSITY</subject><subject>ENERGY SPECTRA</subject><subject>GAMMA RADIATION</subject><subject>JETS</subject><subject>KLEIN-NISHINA FORMULA</subject><subject>MARKARIAN GALAXIES</subject><subject>Mathematical models</subject><subject>Spectra</subject><subject>Spectral energy distribution</subject><subject>Synchrotrons</subject><subject>VARIATIONS</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqNzEFLwzAYxvEgCs7pJ_AS8OKlNnnfZG96LLXO4NZB14meSpemOJmrmu77q0w8e3p44MefsUspbqQwJhZCqGiC9BSTxhhiqdURG0mNJlKo6ZiN_sQpOwvh9edCkowY5XNbVbaY8nyWZ1W5KJY8LW75crEqs5ynWWUfbfXMbcHnafmQljYtuBbynJ10zTb4i98ds9VdXmX30WwxtVk6i3pQyRC1WiE505IWoKFD47HT5LVXJFWjFApNTdJB266TxjlQEwffdbX2Rqy7BnHMrg7dPgybOrjN4N2L63c774YaQGCCJL_V9UG9f_Yfex-G-m0TnN9um53v96GWRAJITYD-QREMaK0MfgGkRF4O</recordid><startdate>20120710</startdate><enddate>20120710</enddate><creator>Mankuzhiyil, Nijil</creator><creator>Ansoldi, Stefano</creator><creator>Persic, Massimo</creator><creator>Rivers, Elizabeth</creator><creator>Rothschild, Richard</creator><creator>Tavecchio, Fabrizio</creator><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20120710</creationdate><title>EMITTING ELECTRONS AND SOURCE ACTIVITY IN MARKARIAN 501</title><author>Mankuzhiyil, Nijil ; Ansoldi, Stefano ; Persic, Massimo ; Rivers, Elizabeth ; Rothschild, Richard ; Tavecchio, Fabrizio</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-o249t-d5437c8d750252f38e3f57e5e4714a443057a9f2ddb9acc246c25014be80bfa33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>ASTRONOMY</topic><topic>ASTROPHYSICS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>BL LACERTAE OBJECTS</topic><topic>Broadband</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>COMPTON EFFECT</topic><topic>COSMIC ELECTRONS</topic><topic>DISTANCE</topic><topic>Elastic scattering</topic><topic>ELECTRON SPECTRA</topic><topic>ENERGY DENSITY</topic><topic>ENERGY SPECTRA</topic><topic>GAMMA RADIATION</topic><topic>JETS</topic><topic>KLEIN-NISHINA FORMULA</topic><topic>MARKARIAN GALAXIES</topic><topic>Mathematical models</topic><topic>Spectra</topic><topic>Spectral energy distribution</topic><topic>Synchrotrons</topic><topic>VARIATIONS</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Mankuzhiyil, Nijil</creatorcontrib><creatorcontrib>Ansoldi, Stefano</creatorcontrib><creatorcontrib>Persic, Massimo</creatorcontrib><creatorcontrib>Rivers, Elizabeth</creatorcontrib><creatorcontrib>Rothschild, Richard</creatorcontrib><creatorcontrib>Tavecchio, Fabrizio</creatorcontrib><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</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mankuzhiyil, Nijil</au><au>Ansoldi, Stefano</au><au>Persic, Massimo</au><au>Rivers, Elizabeth</au><au>Rothschild, Richard</au><au>Tavecchio, Fabrizio</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>EMITTING ELECTRONS AND SOURCE ACTIVITY IN MARKARIAN 501</atitle><jtitle>The Astrophysical journal</jtitle><date>2012-07-10</date><risdate>2012</risdate><volume>753</volume><issue>2</issue><spage>1</spage><epage>7</epage><pages>1-7</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We study the variation of the broadband spectral energy distribution (SED) of the BL Lac object Mrk 501 as a function of source activity, from quiescent to flaring. Through chi super(2)-minimization we model eight simultaneous SED data sets with a one-zone synchrotron self-Compton (SSC) model, and examine how model parameters vary with source activity. The emerging variability pattern of Mrk 501 is complex, with the Compton component arising from gamma -e scatterings that sometimes are (mostly) Thomson and sometimes (mostly) extreme Klein-Nishina. This can be seen from the variation of the Compton to synchrotron peak distance according to source state. The underlying electron spectra are faint/soft in quiescent states and bright/hard in flaring states. A comparison with Mrk 421 suggests that the typical values of the SSC parameters are different in the two sources: however, in both jets the energy density is particle-dominated in all states.</abstract><cop>United States</cop><doi>10.1088/0004-637X/753/2/154</doi><tpages>7</tpages></addata></record> |
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| subjects | ASTRONOMY ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY BL LACERTAE OBJECTS Broadband COMPARATIVE EVALUATIONS COMPTON EFFECT COSMIC ELECTRONS DISTANCE Elastic scattering ELECTRON SPECTRA ENERGY DENSITY ENERGY SPECTRA GAMMA RADIATION JETS KLEIN-NISHINA FORMULA MARKARIAN GALAXIES Mathematical models Spectra Spectral energy distribution Synchrotrons VARIATIONS |
| title | EMITTING ELECTRONS AND SOURCE ACTIVITY IN MARKARIAN 501 |
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