A Search for Fast Radio Bursts with the GBNCC Pulsar Survey
We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm−3, while the rest (23 days; 29% of the total time) were searc...
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| Veröffentlicht in: | The Astrophysical journal 2017-08, Vol.844 (2), p.140 |
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| creator | Chawla, P. Kaspi, V. M. Josephy, A. Rajwade, K. M. Lorimer, D. R. Archibald, A. M. DeCesar, M. E. Hessels, J. W. T. Kaplan, D. L. Karako-Argaman, C. Kondratiev, V. I. Levin, L. Lynch, R. S. McLaughlin, M. A. Ransom, S. M. Roberts, M. S. E. Stairs, I. H. Stovall, K. Swiggum, J. K. Leeuwen, J. van |
| description | We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm−3, while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm−3. No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of FRBs sky−1 day−1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for > +0.35 in the absence of scattering and free-free absorption and > −0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz). |
| doi_str_mv | 10.3847/1538-4357/aa7d57 |
| format | Article |
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M. ; Josephy, A. ; Rajwade, K. M. ; Lorimer, D. R. ; Archibald, A. M. ; DeCesar, M. E. ; Hessels, J. W. T. ; Kaplan, D. L. ; Karako-Argaman, C. ; Kondratiev, V. I. ; Levin, L. ; Lynch, R. S. ; McLaughlin, M. A. ; Ransom, S. M. ; Roberts, M. S. E. ; Stairs, I. H. ; Stovall, K. ; Swiggum, J. K. ; Leeuwen, J. van</creator><creatorcontrib>Chawla, P. ; Kaspi, V. M. ; Josephy, A. ; Rajwade, K. M. ; Lorimer, D. R. ; Archibald, A. M. ; DeCesar, M. E. ; Hessels, J. W. T. ; Kaplan, D. L. ; Karako-Argaman, C. ; Kondratiev, V. I. ; Levin, L. ; Lynch, R. S. ; McLaughlin, M. A. ; Ransom, S. M. ; Roberts, M. S. E. ; Stairs, I. H. ; Stovall, K. ; Swiggum, J. K. ; Leeuwen, J. van</creatorcontrib><description>We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm−3, while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm−3. No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of FRBs sky−1 day−1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for > +0.35 in the absence of scattering and free-free absorption and > −0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz).</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aa7d57</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>ABSORPTION ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; Computer simulation ; COMPUTERIZED SIMULATION ; DATA ANALYSIS ; DISPERSIONS ; DISTRIBUTION ; Fluctuations ; FLUX DENSITY ; methods: data analysis ; methods: statistical ; MHZ RANGE 100-1000 ; PULSARS ; pulsars: general ; Pulse duration ; Radio bursts ; Scattering ; Sky surveys (astronomy) ; SPECTRA ; surveys</subject><ispartof>The Astrophysical journal, 2017-08, Vol.844 (2), p.140</ispartof><rights>2017. 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M.</creatorcontrib><creatorcontrib>Josephy, A.</creatorcontrib><creatorcontrib>Rajwade, K. M.</creatorcontrib><creatorcontrib>Lorimer, D. R.</creatorcontrib><creatorcontrib>Archibald, A. M.</creatorcontrib><creatorcontrib>DeCesar, M. E.</creatorcontrib><creatorcontrib>Hessels, J. W. T.</creatorcontrib><creatorcontrib>Kaplan, D. L.</creatorcontrib><creatorcontrib>Karako-Argaman, C.</creatorcontrib><creatorcontrib>Kondratiev, V. I.</creatorcontrib><creatorcontrib>Levin, L.</creatorcontrib><creatorcontrib>Lynch, R. S.</creatorcontrib><creatorcontrib>McLaughlin, M. A.</creatorcontrib><creatorcontrib>Ransom, S. M.</creatorcontrib><creatorcontrib>Roberts, M. S. E.</creatorcontrib><creatorcontrib>Stairs, I. H.</creatorcontrib><creatorcontrib>Stovall, K.</creatorcontrib><creatorcontrib>Swiggum, J. K.</creatorcontrib><creatorcontrib>Leeuwen, J. van</creatorcontrib><title>A Search for Fast Radio Bursts with the GBNCC Pulsar Survey</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm−3, while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm−3. No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of FRBs sky−1 day−1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for > +0.35 in the absence of scattering and free-free absorption and > −0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz).</description><subject>ABSORPTION</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>Computer simulation</subject><subject>COMPUTERIZED SIMULATION</subject><subject>DATA ANALYSIS</subject><subject>DISPERSIONS</subject><subject>DISTRIBUTION</subject><subject>Fluctuations</subject><subject>FLUX DENSITY</subject><subject>methods: data analysis</subject><subject>methods: statistical</subject><subject>MHZ RANGE 100-1000</subject><subject>PULSARS</subject><subject>pulsars: general</subject><subject>Pulse duration</subject><subject>Radio bursts</subject><subject>Scattering</subject><subject>Sky surveys (astronomy)</subject><subject>SPECTRA</subject><subject>surveys</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNp1kF1LwzAUhoMoOKf3Xga8tS4fzUfxaituCkPFKXgX0jSlHXOZSars39tScVdeHc7heV8ODwCXGN1QmYoJZlQmKWViorUomTgCo7_TMRghhNKEU_F-Cs5CWPcrybIRuJ3CldXe1LByHs51iPBFl42Ds9aHGOB3E2sYawsXs8c8h8_tJmgPV63_svtzcFLpTbAXv3MM3uZ3r_l9snxaPOTTZWKokDExBTaa0QLzUnIjMWa6sIzLLJWUMVRiXWBdFhoxiVNaEY4IJ8zwTFArMBJ0DK6GXhdio4JpojW1cdutNVERIgXLOD5QO-8-WxuiWrvWb7vHFKGcyYwRRDoKDZTxLgRvK7XzzYf2e4WR6kWq3prqralBZBe5HiKN2x06_8V_AJdscDE</recordid><startdate>20170801</startdate><enddate>20170801</enddate><creator>Chawla, P.</creator><creator>Kaspi, V. 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K.</creator><creator>Leeuwen, J. van</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-1075-3837</orcidid><orcidid>https://orcid.org/0000-0002-2185-1790</orcidid><orcidid>https://orcid.org/0000-0002-2034-2986</orcidid><orcidid>https://orcid.org/0000-0001-5229-7430</orcidid><orcidid>https://orcid.org/0000-0003-0638-3340</orcidid><orcidid>https://orcid.org/0000-0001-6295-2881</orcidid><orcidid>https://orcid.org/0000-0001-7697-7422</orcidid><orcidid>https://orcid.org/0000-0001-9345-0307</orcidid><orcidid>https://orcid.org/0000-0001-9784-8670</orcidid><orcidid>https://orcid.org/0000-0002-9396-9720</orcidid><orcidid>https://orcid.org/0000-0002-7261-594X</orcidid><orcidid>https://orcid.org/0000-0003-1301-966X</orcidid><orcidid>https://orcid.org/0000-0003-2317-1446</orcidid><orcidid>https://orcid.org/0000-0002-3426-7606</orcidid><orcidid>https://orcid.org/0000-0001-5799-9714</orcidid></search><sort><creationdate>20170801</creationdate><title>A Search for Fast Radio Bursts with the GBNCC Pulsar Survey</title><author>Chawla, P. ; Kaspi, V. M. ; Josephy, A. ; Rajwade, K. M. ; Lorimer, D. R. ; Archibald, A. M. ; DeCesar, M. E. ; Hessels, J. W. T. ; Kaplan, D. L. ; Karako-Argaman, C. ; Kondratiev, V. I. ; Levin, L. ; Lynch, R. S. ; McLaughlin, M. A. ; Ransom, S. M. ; Roberts, M. S. E. ; Stairs, I. H. ; Stovall, K. ; Swiggum, J. 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H.</au><au>Stovall, K.</au><au>Swiggum, J. K.</au><au>Leeuwen, J. van</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A Search for Fast Radio Bursts with the GBNCC Pulsar Survey</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2017-08-01</date><risdate>2017</risdate><volume>844</volume><issue>2</issue><spage>140</spage><pages>140-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm−3, while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm−3. No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of FRBs sky−1 day−1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for > +0.35 in the absence of scattering and free-free absorption and > −0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. 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| subjects | ABSORPTION ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY Computer simulation COMPUTERIZED SIMULATION DATA ANALYSIS DISPERSIONS DISTRIBUTION Fluctuations FLUX DENSITY methods: data analysis methods: statistical MHZ RANGE 100-1000 PULSARS pulsars: general Pulse duration Radio bursts Scattering Sky surveys (astronomy) SPECTRA surveys |
| title | A Search for Fast Radio Bursts with the GBNCC Pulsar Survey |
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