@Article{GuiriecGoSaKoGeMc:2016:CGDASU,
               author = "Guiriec, S. and Gonzalez, M. M. and Sacahui Reyes, Jos{\'e} 
                         Rodrigo and Kouveliotou, C. and Gehrels, N. and McEnergy, J.",
          affiliation = "{NASA Goddard Space Flight Center} and {Instituto de Astronoma 
                         (UNAM)} and {Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {George Washington University} and {NASA Goddard Space Flight 
                         Center} and {NASA Goddard Space Flight Center}",
                title = "CGRO/BATSE DATA SUPPORT the NEW PARADIGM for GRB prompt emission 
                         and the new Li nTh-Epeak, i nTh,rest relation",
              journal = "Astrophysical Journal",
                 year = "2016",
               volume = "819",
               number = "1",
                pages = "number 79",
                month = "Mar.",
             keywords = "acceleration of particles, black hole physics, distance scale, 
                         gamma-ray burst: general, radiation mechanisms: non-thermal, 
                         radiation mechanisms: thermal.",
             abstract = "The paradigm for gamma-ray burst (GRB) prompt emission is 
                         changing. Since early in the Compton Gamma Ray Observatory (CGRO) 
                         era, the empirical Band function has been considered a good 
                         description of the keV-MeV \γ-ray prompt emission spectra 
                         despite the fact that its shape was very often inconsistent with 
                         the theoretical predictions, especially those expected in pure 
                         synchrotron emission scenarios. We have recently established a new 
                         observational model analyzing data of the NASA Fermi Gamma-ray 
                         Space Telescope. In this model, GRB prompt emission would be a 
                         combination of three main emission components: (i) a thermal-like 
                         component that we have interpreted so far as emission from the jet 
                         photosphere, (ii) a non-thermal component that we have interpreted 
                         so far as either synchrotron radiation from the propagating and 
                         accelerated charged particles within the jet or reprocessed jet 
                         photospheric emission, and (iii) an additional non-thermal 
                         (cutoff) power law (PL) extending from low to high energies in 
                         \γ-rays and most likely of inverse Compton origin. In this 
                         article we reanalyze some of the bright GRBs, namely GRBs 941017, 
                         970111, and 990123, observed with the Burst And Transient Source 
                         Experiment (BATSE) on board CGRO with the new model. We conclude 
                         that BATSE data for these three GRBs are fully consistent with the 
                         recent results obtained with Fermi: some bright BATSE GRBs exhibit 
                         three separate components during the prompt phase with similar 
                         spectral parameters as those reported from Fermi data. In 
                         addition, the analysis of the BATSE GRBs with the new prompt 
                         emission model results in a relation between the time-resolved 
                         energy flux of the non-thermal component, Fi nTh, and its 
                         corresponding \νF\ν spectral peak energy, Epeak, i nTh 
                         (i.e., Fi nTh - Epeak, i nTh), which has a similar index - when 
                         fitted to a PL - as the one initially derived from Fermi data. For 
                         GRBs with known redshifts (z) this results in a possible universal 
                         relation between the luminosity of the non-thermal component, Li 
                         nTh, and its corresponding \νFv spectral peak energy in the 
                         rest frame, Epeak,i NT,rest(i.e.,Li nTh - Epeak,i NT,rest). We 
                         estimated the redshifts of GRBs 941017 and 970111 using GRB 990123 
                         - with z = 1.61 - as a reference. The estimated redshift for GRB 
                         941017 is typical for long GRBs and the estimated redshift for GRB 
                         970111 is right in the range of the expected values for this 
                         burst.",
                  doi = "10.3847/0004-637X/819/1/79",
                  url = "http://dx.doi.org/10.3847/0004-637X/819/1/79",
                 issn = "0004-637X and 1538-4357",
             language = "en",
           targetfile = "guiriec_cgro.pdf",
        urlaccessdate = "22 maio 2024"
}