@Article{MartinsHengMeloAgui:2024:SeGrBu,
               author = "Martins, J{\'u}lio C{\'e}sar and Heng, Ik Siong and Melo, Iara 
                         Tosta E. and Aguiar, Odylio Denys de",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {University 
                         of Glasgow} and INFN and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)}",
                title = "Search for gravitational-wave bursts in LIGO data at the Schenberg 
                         antenna sensitivity range",
              journal = "Physical Review D",
                 year = "2024",
               volume = "109",
               number = "2",
                pages = "e023026",
                month = "Jan.",
             abstract = "The Brazilian Mario Schenberg gravitational-wave detector was 
                         initially designed in the early 2000s and remained operational 
                         until 2016 when it was disassembled. To assess the feasibility of 
                         reassembling the Schenberg antenna, its capability to detect 
                         gravitational waves (GW) within its designed sensitivity 
                         parameters needs to be evaluated. Detection of significant signals 
                         would serve as a catalyst for rebuilding the detector. Although 
                         the antenna is currently disassembled, insights can be gleaned 
                         from the third observing run (O3) data of the LIGO detectors, 
                         given the similarities between Schenberg's ultimate sensitivity 
                         and the interferometers' sensitivity in the [3150-3260] Hz band. 
                         The search focused on signals lasting from milliseconds to 
                         seconds, with no assumptions about their morphology, polarization, 
                         and arrival sky direction. Data analysis was performed using the 
                         coherent WaveBurst pipeline in the frequency range between 512 Hz 
                         and 4096 Hz, specifically targeting signals with bandwidths 
                         overlapping the Schenberg frequency band. However, the O3 data did 
                         not yield statistically significant evidence of GW bursts. This 
                         null result allowed for the characterization of the search 
                         efficiency in identifying simulated signal morphologies and 
                         setting upper limits on the GW burst event rate as a function of 
                         strain amplitude. The current search, and by extension the 
                         advanced version of the Schenberg antenna (aSchenberg), can detect 
                         sources emitting isotropically 5×10-6M{\^a} c2 in GWs from a 
                         distance of 10 kiloparsecs with a 50% detection efficiency at a 
                         false alarm rate of 1 per 100 years. Moreover, we revisited 
                         estimations of detecting f modes of neutron stars excited by 
                         glitches, setting the upper limit of the f-mode energy for the 
                         population of Galactic pulsars to \∼8×10-8M{\^a} c2 at 
                         3205 Hz. Our simulations and the defined detection criteria 
                         suggest f modes are a very unlikely source of gravitational waves 
                         for the aSchenberg. Nevertheless, its potential in probing other 
                         types of gravitational wave short transients, such as those 
                         arising from supernova explosions, giant flares from magnetars, 
                         postmerger phase of binary neutron stars, or the inspiral of 
                         binaries of primordial black holes with subsolar masses, remains 
                         promising.",
                  doi = "10.1103/PhysRevD.109.023026",
                  url = "http://dx.doi.org/10.1103/PhysRevD.109.023026",
                 issn = "1550-2368 and 1550-7998",
             language = "en",
        urlaccessdate = "27 abr. 2024"
}