How Many Kilonovae Can Be Found in Past, Present, and Future Survey Data Sets?
The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present, and future surveys withou...
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| Veröffentlicht in: | Astrophysical journal. Letters 2018-01, Vol.852 (1), p.L3 |
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| creator | Scolnic, D. Kessler, R. Brout, D. Cowperthwaite, P. S. Soares-Santos, M. Annis, J. Herner, K. Chen, H.-Y. Sako, M. Doctor, Z. Butler, R. E. Palmese, A. Diehl, H. T. Frieman, J. Holz, D. E. Berger, E. Chornock, R. Villar, V. A. Nicholl, M. Biswas, R. Hounsell, R. Foley, R. J. Metzger, J. Rest, A. García-Bellido, J. Möller, A. Nugent, P. Abbott, T. M. C. Abdalla, F. B. Allam, S. Bechtol, K. Benoit-Lévy, A. Bertin, E. Brooks, D. Buckley-Geer, E. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Castander, F. J. Cunha, C. E. D'Andrea, C. B. Costa, L. N. da Davis, C. Doel, P. Drlica-Wagner, A. Eifler, T. F. Flaugher, B. Fosalba, P. Gaztanaga, E. Gerdes, D. W. Gruen, D. Gruendl, R. A. Gschwend, J. Gutierrez, G. Hartley, W. G. Honscheid, K. James, D. J. Johnson, M. W. G. Johnson, M. D. Krause, E. Kuehn, K. Kuhlmann, S. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. March, M. Marshall, J. L. Menanteau, F. Miquel, R. Neilsen, E. Plazas, A. A. Sanchez, E. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Smith, M. Smith, R. C. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thomas, R. C. Tucker, D. L. Walker, A. R. |
| description | The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present, and future surveys without a gravitational-wave trigger. For the simulation, we construct a spectral time-series model based on the DES-GW multi-band light curve from the single known KN event, and we use an average of BNS rates from past studies of , consistent with the one event found so far. Examining past and current data sets from transient surveys, the number of KNe we expect to find for ASAS-SN, SDSS, PS1, SNLS, DES, and SMT is between 0 and 0.3. We predict the number of detections per future survey to be 8.3 from ATLAS, 10.6 from ZTF, 5.5/69 from LSST (the Deep Drilling/Wide Fast Deep), and 16.0 from WFIRST. The maximum redshift of KNe discovered for each survey is for WFIRST, for LSST, and for ZTF and ATLAS. This maximum redshift for WFIRST is well beyond the sensitivity of aLIGO and some future GW missions. For the LSST survey, we also provide contamination estimates from Type Ia and core-collapse supernovae: after light curve and template-matching requirements, we estimate a background of just two events. More broadly, we stress that future transient surveys should consider how to optimize their search strategies to improve their detection efficiency and to consider similar analyses for GW follow-up programs. |
| doi_str_mv | 10.3847/2041-8213/aa9d82 |
| format | Article |
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S. ; Soares-Santos, M. ; Annis, J. ; Herner, K. ; Chen, H.-Y. ; Sako, M. ; Doctor, Z. ; Butler, R. E. ; Palmese, A. ; Diehl, H. T. ; Frieman, J. ; Holz, D. E. ; Berger, E. ; Chornock, R. ; Villar, V. A. ; Nicholl, M. ; Biswas, R. ; Hounsell, R. ; Foley, R. J. ; Metzger, J. ; Rest, A. ; García-Bellido, J. ; Möller, A. ; Nugent, P. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Bechtol, K. ; Benoit-Lévy, A. ; Bertin, E. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Castander, F. J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruen, D. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Honscheid, K. ; James, D. J. ; Johnson, M. W. G. ; Johnson, M. D. ; Krause, E. ; Kuehn, K. ; Kuhlmann, S. ; Lahav, O. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Menanteau, F. ; Miquel, R. ; Neilsen, E. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, R. C. ; Tucker, D. L. ; Walker, A. R.</creator><creatorcontrib>Scolnic, D. ; Kessler, R. ; Brout, D. ; Cowperthwaite, P. S. ; Soares-Santos, M. ; Annis, J. ; Herner, K. ; Chen, H.-Y. ; Sako, M. ; Doctor, Z. ; Butler, R. E. ; Palmese, A. ; Diehl, H. T. ; Frieman, J. ; Holz, D. E. ; Berger, E. ; Chornock, R. ; Villar, V. A. ; Nicholl, M. ; Biswas, R. ; Hounsell, R. ; Foley, R. J. ; Metzger, J. ; Rest, A. ; García-Bellido, J. ; Möller, A. ; Nugent, P. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Bechtol, K. ; Benoit-Lévy, A. ; Bertin, E. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Castander, F. J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruen, D. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Honscheid, K. ; James, D. J. ; Johnson, M. W. G. ; Johnson, M. D. ; Krause, E. ; Kuehn, K. ; Kuhlmann, S. ; Lahav, O. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Menanteau, F. ; Miquel, R. ; Neilsen, E. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, R. C. ; Tucker, D. L. ; Walker, A. R. ; DES Collaboration ; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States) ; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States) ; Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States) ; Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><description>The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present, and future surveys without a gravitational-wave trigger. For the simulation, we construct a spectral time-series model based on the DES-GW multi-band light curve from the single known KN event, and we use an average of BNS rates from past studies of , consistent with the one event found so far. Examining past and current data sets from transient surveys, the number of KNe we expect to find for ASAS-SN, SDSS, PS1, SNLS, DES, and SMT is between 0 and 0.3. We predict the number of detections per future survey to be 8.3 from ATLAS, 10.6 from ZTF, 5.5/69 from LSST (the Deep Drilling/Wide Fast Deep), and 16.0 from WFIRST. The maximum redshift of KNe discovered for each survey is for WFIRST, for LSST, and for ZTF and ATLAS. This maximum redshift for WFIRST is well beyond the sensitivity of aLIGO and some future GW missions. For the LSST survey, we also provide contamination estimates from Type Ia and core-collapse supernovae: after light curve and template-matching requirements, we estimate a background of just two events. More broadly, we stress that future transient surveys should consider how to optimize their search strategies to improve their detection efficiency and to consider similar analyses for GW follow-up programs.</description><identifier>ISSN: 2041-8205</identifier><identifier>ISSN: 2041-8213</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/aa9d82</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; Computer simulation ; Datasets ; Drilling ; General Relativity and Quantum Cosmology ; Gravitational collapse ; Gravitational waves ; Instrumentation and Detectors ; INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY ; Kilonovae ; Light curve ; neutron ; Physics ; Polls & surveys ; Red shift ; stars ; Stars: Neutron ; Supernovae ; Template matching</subject><ispartof>Astrophysical journal. Letters, 2018-01, Vol.852 (1), p.L3</ispartof><rights>2017. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Jan 01, 2018</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c448t-a003d6c0a4242f0a2dee6b1ef9d23b51e61507ff461250062128cf99455e34b93</citedby><cites>FETCH-LOGICAL-c448t-a003d6c0a4242f0a2dee6b1ef9d23b51e61507ff461250062128cf99455e34b93</cites><orcidid>0000-0002-0609-3987 ; 0000-0002-5814-4061 ; 0000-0002-7123-8943 ; 0000-0002-2478-6939 ; 0000-0002-4588-6517 ; 0000-0002-9646-8198 ; 0000-0002-0175-5064 ; 0000-0003-0710-9474 ; 0000-0002-6610-4836 ; 0000-0001-7316-4573 ; 0000-0002-3389-0586 ; 0000-0001-6082-8529 ; 0000-0001-8251-933X ; 0000-0003-1704-0781 ; 0000-0002-9392-9681 ; 0000-0003-3270-7644 ; 0000-0002-1510-5214 ; 0000000224786939 ; 0000000201755064 ; 0000000266104836 ; 0000000245886517 ; 0000000296468198 ; 0000000293929681 ; 0000000307109474 ; 0000000317040781 ; 0000000233890586 ; 0000000258144061 ; 0000000271238943 ; 000000018251933X ; 0000000173164573 ; 0000000332707644 ; 0000000206093987 ; 0000000160828529</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/aa9d82/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,780,784,885,27924,27925,38868,38890,53840,53867</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/aa9d82$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-01704406$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/servlets/purl/1434944$$D View this record in Osti.gov$$Hfree_for_read</backlink><backlink>$$Uhttps://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-151178$$DView record from Swedish Publication Index$$Hfree_for_read</backlink></links><search><creatorcontrib>Scolnic, D.</creatorcontrib><creatorcontrib>Kessler, R.</creatorcontrib><creatorcontrib>Brout, D.</creatorcontrib><creatorcontrib>Cowperthwaite, P. 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N. da</creatorcontrib><creatorcontrib>Davis, C.</creatorcontrib><creatorcontrib>Doel, P.</creatorcontrib><creatorcontrib>Drlica-Wagner, A.</creatorcontrib><creatorcontrib>Eifler, T. F.</creatorcontrib><creatorcontrib>Flaugher, B.</creatorcontrib><creatorcontrib>Fosalba, P.</creatorcontrib><creatorcontrib>Gaztanaga, E.</creatorcontrib><creatorcontrib>Gerdes, D. W.</creatorcontrib><creatorcontrib>Gruen, D.</creatorcontrib><creatorcontrib>Gruendl, R. A.</creatorcontrib><creatorcontrib>Gschwend, J.</creatorcontrib><creatorcontrib>Gutierrez, G.</creatorcontrib><creatorcontrib>Hartley, W. G.</creatorcontrib><creatorcontrib>Honscheid, K.</creatorcontrib><creatorcontrib>James, D. J.</creatorcontrib><creatorcontrib>Johnson, M. W. G.</creatorcontrib><creatorcontrib>Johnson, M. D.</creatorcontrib><creatorcontrib>Krause, E.</creatorcontrib><creatorcontrib>Kuehn, K.</creatorcontrib><creatorcontrib>Kuhlmann, S.</creatorcontrib><creatorcontrib>Lahav, O.</creatorcontrib><creatorcontrib>Li, T. S.</creatorcontrib><creatorcontrib>Lima, M.</creatorcontrib><creatorcontrib>Maia, M. A. G.</creatorcontrib><creatorcontrib>March, M.</creatorcontrib><creatorcontrib>Marshall, J. L.</creatorcontrib><creatorcontrib>Menanteau, F.</creatorcontrib><creatorcontrib>Miquel, R.</creatorcontrib><creatorcontrib>Neilsen, E.</creatorcontrib><creatorcontrib>Plazas, A. A.</creatorcontrib><creatorcontrib>Sanchez, E.</creatorcontrib><creatorcontrib>Scarpine, V.</creatorcontrib><creatorcontrib>Schubnell, M.</creatorcontrib><creatorcontrib>Sevilla-Noarbe, I.</creatorcontrib><creatorcontrib>Smith, M.</creatorcontrib><creatorcontrib>Smith, R. C.</creatorcontrib><creatorcontrib>Sobreira, F.</creatorcontrib><creatorcontrib>Suchyta, E.</creatorcontrib><creatorcontrib>Swanson, M. E. C.</creatorcontrib><creatorcontrib>Tarle, G.</creatorcontrib><creatorcontrib>Thomas, R. C.</creatorcontrib><creatorcontrib>Tucker, D. L.</creatorcontrib><creatorcontrib>Walker, A. R.</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><title>How Many Kilonovae Can Be Found in Past, Present, and Future Survey Data Sets?</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present, and future surveys without a gravitational-wave trigger. For the simulation, we construct a spectral time-series model based on the DES-GW multi-band light curve from the single known KN event, and we use an average of BNS rates from past studies of , consistent with the one event found so far. Examining past and current data sets from transient surveys, the number of KNe we expect to find for ASAS-SN, SDSS, PS1, SNLS, DES, and SMT is between 0 and 0.3. We predict the number of detections per future survey to be 8.3 from ATLAS, 10.6 from ZTF, 5.5/69 from LSST (the Deep Drilling/Wide Fast Deep), and 16.0 from WFIRST. The maximum redshift of KNe discovered for each survey is for WFIRST, for LSST, and for ZTF and ATLAS. This maximum redshift for WFIRST is well beyond the sensitivity of aLIGO and some future GW missions. For the LSST survey, we also provide contamination estimates from Type Ia and core-collapse supernovae: after light curve and template-matching requirements, we estimate a background of just two events. More broadly, we stress that future transient surveys should consider how to optimize their search strategies to improve their detection efficiency and to consider similar analyses for GW follow-up programs.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Computer simulation</subject><subject>Datasets</subject><subject>Drilling</subject><subject>General Relativity and Quantum Cosmology</subject><subject>Gravitational collapse</subject><subject>Gravitational waves</subject><subject>Instrumentation and Detectors</subject><subject>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</subject><subject>Kilonovae</subject><subject>Light curve</subject><subject>neutron</subject><subject>Physics</subject><subject>Polls & surveys</subject><subject>Red shift</subject><subject>stars</subject><subject>Stars: Neutron</subject><subject>Supernovae</subject><subject>Template matching</subject><issn>2041-8205</issn><issn>2041-8213</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kc1LAzEUxBdR8PPuMehJaPUlm6S7J6mttWLVQtVrSHff2pWa1CRb6X_vlpUWD57eMPwY3jBRdErhMk5454oBp-2E0fhK6zRP2E50sLF2NxrEfnTo_QcAA0mTg-hpaL_JozYr8lDOrbFLjaSnDblBMrCVyUlpyFj70CJjhx5NLXTtDqpQOSSTyi1xRfo6aDLB4K-Po71Czz2e_N6j6HVw-9IbtkfPd_e97qidcZ6EtgaIc5mB5oyzAjTLEeWUYpHmLJ4KipIK6BQFl5QJAMkoS7IiTbkQGPNpGh9FrSbXf-OimqqFKz-1WymrS9Uv37rKunflK0UFpZ2kxs8a3PpQKp-VAbNZZo3BLCjKY55yXkMXDTTT8z-Bw-5IrT2gHeAc5JLW7HnDLpz9qtAH9WErZ-rKisVSSJHUr9cUNFTmrPcOi00sBbVeTa1nUeuJVLPatlhpF9vMf_EfZ3STmA</recordid><startdate>20180101</startdate><enddate>20180101</enddate><creator>Scolnic, D.</creator><creator>Kessler, R.</creator><creator>Brout, D.</creator><creator>Cowperthwaite, P. 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R.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>Bristol : IOP Publishing</general><general>Institute of Physics (IOP)</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>OIOZB</scope><scope>OTOTI</scope><scope>ADTPV</scope><scope>AOWAS</scope><scope>DG7</scope><orcidid>https://orcid.org/0000-0002-0609-3987</orcidid><orcidid>https://orcid.org/0000-0002-5814-4061</orcidid><orcidid>https://orcid.org/0000-0002-7123-8943</orcidid><orcidid>https://orcid.org/0000-0002-2478-6939</orcidid><orcidid>https://orcid.org/0000-0002-4588-6517</orcidid><orcidid>https://orcid.org/0000-0002-9646-8198</orcidid><orcidid>https://orcid.org/0000-0002-0175-5064</orcidid><orcidid>https://orcid.org/0000-0003-0710-9474</orcidid><orcidid>https://orcid.org/0000-0002-6610-4836</orcidid><orcidid>https://orcid.org/0000-0001-7316-4573</orcidid><orcidid>https://orcid.org/0000-0002-3389-0586</orcidid><orcidid>https://orcid.org/0000-0001-6082-8529</orcidid><orcidid>https://orcid.org/0000-0001-8251-933X</orcidid><orcidid>https://orcid.org/0000-0003-1704-0781</orcidid><orcidid>https://orcid.org/0000-0002-9392-9681</orcidid><orcidid>https://orcid.org/0000-0003-3270-7644</orcidid><orcidid>https://orcid.org/0000-0002-1510-5214</orcidid><orcidid>https://orcid.org/0000000224786939</orcidid><orcidid>https://orcid.org/0000000201755064</orcidid><orcidid>https://orcid.org/0000000266104836</orcidid><orcidid>https://orcid.org/0000000245886517</orcidid><orcidid>https://orcid.org/0000000296468198</orcidid><orcidid>https://orcid.org/0000000293929681</orcidid><orcidid>https://orcid.org/0000000307109474</orcidid><orcidid>https://orcid.org/0000000317040781</orcidid><orcidid>https://orcid.org/0000000233890586</orcidid><orcidid>https://orcid.org/0000000258144061</orcidid><orcidid>https://orcid.org/0000000271238943</orcidid><orcidid>https://orcid.org/000000018251933X</orcidid><orcidid>https://orcid.org/0000000173164573</orcidid><orcidid>https://orcid.org/0000000332707644</orcidid><orcidid>https://orcid.org/0000000206093987</orcidid><orcidid>https://orcid.org/0000000160828529</orcidid></search><sort><creationdate>20180101</creationdate><title>How Many Kilonovae Can Be Found in Past, Present, and Future Survey Data Sets?</title><author>Scolnic, D. ; Kessler, R. ; Brout, D. ; Cowperthwaite, P. S. ; Soares-Santos, M. ; Annis, J. ; Herner, K. ; Chen, H.-Y. ; Sako, M. ; Doctor, Z. ; Butler, R. E. ; Palmese, A. ; Diehl, H. T. ; Frieman, J. ; Holz, D. E. ; Berger, E. ; Chornock, R. ; Villar, V. A. ; Nicholl, M. ; Biswas, R. ; Hounsell, R. ; Foley, R. J. ; Metzger, J. ; Rest, A. ; García-Bellido, J. ; Möller, A. ; Nugent, P. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Bechtol, K. ; Benoit-Lévy, A. ; Bertin, E. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Castander, F. J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruen, D. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Honscheid, K. ; James, D. J. ; Johnson, M. W. G. ; Johnson, M. D. ; Krause, E. ; Kuehn, K. ; Kuhlmann, S. ; Lahav, O. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Menanteau, F. ; Miquel, R. ; Neilsen, E. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, R. C. ; Tucker, D. L. ; Walker, A. R.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c448t-a003d6c0a4242f0a2dee6b1ef9d23b51e61507ff461250062128cf99455e34b93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>Computer simulation</topic><topic>Datasets</topic><topic>Drilling</topic><topic>General Relativity and Quantum Cosmology</topic><topic>Gravitational collapse</topic><topic>Gravitational waves</topic><topic>Instrumentation and Detectors</topic><topic>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</topic><topic>Kilonovae</topic><topic>Light curve</topic><topic>neutron</topic><topic>Physics</topic><topic>Polls & surveys</topic><topic>Red shift</topic><topic>stars</topic><topic>Stars: Neutron</topic><topic>Supernovae</topic><topic>Template matching</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Scolnic, D.</creatorcontrib><creatorcontrib>Kessler, R.</creatorcontrib><creatorcontrib>Brout, D.</creatorcontrib><creatorcontrib>Cowperthwaite, P. S.</creatorcontrib><creatorcontrib>Soares-Santos, M.</creatorcontrib><creatorcontrib>Annis, J.</creatorcontrib><creatorcontrib>Herner, K.</creatorcontrib><creatorcontrib>Chen, H.-Y.</creatorcontrib><creatorcontrib>Sako, M.</creatorcontrib><creatorcontrib>Doctor, Z.</creatorcontrib><creatorcontrib>Butler, R. E.</creatorcontrib><creatorcontrib>Palmese, A.</creatorcontrib><creatorcontrib>Diehl, H. T.</creatorcontrib><creatorcontrib>Frieman, J.</creatorcontrib><creatorcontrib>Holz, D. E.</creatorcontrib><creatorcontrib>Berger, E.</creatorcontrib><creatorcontrib>Chornock, R.</creatorcontrib><creatorcontrib>Villar, V. A.</creatorcontrib><creatorcontrib>Nicholl, M.</creatorcontrib><creatorcontrib>Biswas, R.</creatorcontrib><creatorcontrib>Hounsell, R.</creatorcontrib><creatorcontrib>Foley, R. J.</creatorcontrib><creatorcontrib>Metzger, J.</creatorcontrib><creatorcontrib>Rest, A.</creatorcontrib><creatorcontrib>García-Bellido, J.</creatorcontrib><creatorcontrib>Möller, A.</creatorcontrib><creatorcontrib>Nugent, P.</creatorcontrib><creatorcontrib>Abbott, T. M. C.</creatorcontrib><creatorcontrib>Abdalla, F. B.</creatorcontrib><creatorcontrib>Allam, S.</creatorcontrib><creatorcontrib>Bechtol, K.</creatorcontrib><creatorcontrib>Benoit-Lévy, A.</creatorcontrib><creatorcontrib>Bertin, E.</creatorcontrib><creatorcontrib>Brooks, D.</creatorcontrib><creatorcontrib>Buckley-Geer, E.</creatorcontrib><creatorcontrib>Rosell, A. Carnero</creatorcontrib><creatorcontrib>Kind, M. Carrasco</creatorcontrib><creatorcontrib>Carretero, J.</creatorcontrib><creatorcontrib>Castander, F. J.</creatorcontrib><creatorcontrib>Cunha, C. E.</creatorcontrib><creatorcontrib>D'Andrea, C. B.</creatorcontrib><creatorcontrib>Costa, L. 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R.</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><collection>SwePub</collection><collection>SwePub Articles</collection><collection>SWEPUB Stockholms universitet</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Scolnic, D.</au><au>Kessler, R.</au><au>Brout, D.</au><au>Cowperthwaite, P. S.</au><au>Soares-Santos, M.</au><au>Annis, J.</au><au>Herner, K.</au><au>Chen, H.-Y.</au><au>Sako, M.</au><au>Doctor, Z.</au><au>Butler, R. E.</au><au>Palmese, A.</au><au>Diehl, H. T.</au><au>Frieman, J.</au><au>Holz, D. E.</au><au>Berger, E.</au><au>Chornock, R.</au><au>Villar, V. A.</au><au>Nicholl, M.</au><au>Biswas, R.</au><au>Hounsell, R.</au><au>Foley, R. J.</au><au>Metzger, J.</au><au>Rest, A.</au><au>García-Bellido, J.</au><au>Möller, A.</au><au>Nugent, P.</au><au>Abbott, T. M. C.</au><au>Abdalla, F. B.</au><au>Allam, S.</au><au>Bechtol, K.</au><au>Benoit-Lévy, A.</au><au>Bertin, E.</au><au>Brooks, D.</au><au>Buckley-Geer, E.</au><au>Rosell, A. Carnero</au><au>Kind, M. Carrasco</au><au>Carretero, J.</au><au>Castander, F. J.</au><au>Cunha, C. E.</au><au>D'Andrea, C. B.</au><au>Costa, L. N. da</au><au>Davis, C.</au><au>Doel, P.</au><au>Drlica-Wagner, A.</au><au>Eifler, T. F.</au><au>Flaugher, B.</au><au>Fosalba, P.</au><au>Gaztanaga, E.</au><au>Gerdes, D. W.</au><au>Gruen, D.</au><au>Gruendl, R. A.</au><au>Gschwend, J.</au><au>Gutierrez, G.</au><au>Hartley, W. G.</au><au>Honscheid, K.</au><au>James, D. J.</au><au>Johnson, M. W. G.</au><au>Johnson, M. D.</au><au>Krause, E.</au><au>Kuehn, K.</au><au>Kuhlmann, S.</au><au>Lahav, O.</au><au>Li, T. S.</au><au>Lima, M.</au><au>Maia, M. A. G.</au><au>March, M.</au><au>Marshall, J. L.</au><au>Menanteau, F.</au><au>Miquel, R.</au><au>Neilsen, E.</au><au>Plazas, A. A.</au><au>Sanchez, E.</au><au>Scarpine, V.</au><au>Schubnell, M.</au><au>Sevilla-Noarbe, I.</au><au>Smith, M.</au><au>Smith, R. C.</au><au>Sobreira, F.</au><au>Suchyta, E.</au><au>Swanson, M. E. C.</au><au>Tarle, G.</au><au>Thomas, R. C.</au><au>Tucker, D. L.</au><au>Walker, A. R.</au><aucorp>DES Collaboration</aucorp><aucorp>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</aucorp><aucorp>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</aucorp><aucorp>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</aucorp><aucorp>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>How Many Kilonovae Can Be Found in Past, Present, and Future Survey Data Sets?</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2018-01-01</date><risdate>2018</risdate><volume>852</volume><issue>1</issue><spage>L3</spage><pages>L3-</pages><issn>2041-8205</issn><issn>2041-8213</issn><eissn>2041-8213</eissn><abstract>The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present, and future surveys without a gravitational-wave trigger. For the simulation, we construct a spectral time-series model based on the DES-GW multi-band light curve from the single known KN event, and we use an average of BNS rates from past studies of , consistent with the one event found so far. Examining past and current data sets from transient surveys, the number of KNe we expect to find for ASAS-SN, SDSS, PS1, SNLS, DES, and SMT is between 0 and 0.3. We predict the number of detections per future survey to be 8.3 from ATLAS, 10.6 from ZTF, 5.5/69 from LSST (the Deep Drilling/Wide Fast Deep), and 16.0 from WFIRST. The maximum redshift of KNe discovered for each survey is for WFIRST, for LSST, and for ZTF and ATLAS. This maximum redshift for WFIRST is well beyond the sensitivity of aLIGO and some future GW missions. For the LSST survey, we also provide contamination estimates from Type Ia and core-collapse supernovae: after light curve and template-matching requirements, we estimate a background of just two events. More broadly, we stress that future transient surveys should consider how to optimize their search strategies to improve their detection efficiency and to consider similar analyses for GW follow-up programs.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/aa9d82</doi><tpages>7</tpages><orcidid>https://orcid.org/0000-0002-0609-3987</orcidid><orcidid>https://orcid.org/0000-0002-5814-4061</orcidid><orcidid>https://orcid.org/0000-0002-7123-8943</orcidid><orcidid>https://orcid.org/0000-0002-2478-6939</orcidid><orcidid>https://orcid.org/0000-0002-4588-6517</orcidid><orcidid>https://orcid.org/0000-0002-9646-8198</orcidid><orcidid>https://orcid.org/0000-0002-0175-5064</orcidid><orcidid>https://orcid.org/0000-0003-0710-9474</orcidid><orcidid>https://orcid.org/0000-0002-6610-4836</orcidid><orcidid>https://orcid.org/0000-0001-7316-4573</orcidid><orcidid>https://orcid.org/0000-0002-3389-0586</orcidid><orcidid>https://orcid.org/0000-0001-6082-8529</orcidid><orcidid>https://orcid.org/0000-0001-8251-933X</orcidid><orcidid>https://orcid.org/0000-0003-1704-0781</orcidid><orcidid>https://orcid.org/0000-0002-9392-9681</orcidid><orcidid>https://orcid.org/0000-0003-3270-7644</orcidid><orcidid>https://orcid.org/0000-0002-1510-5214</orcidid><orcidid>https://orcid.org/0000000224786939</orcidid><orcidid>https://orcid.org/0000000201755064</orcidid><orcidid>https://orcid.org/0000000266104836</orcidid><orcidid>https://orcid.org/0000000245886517</orcidid><orcidid>https://orcid.org/0000000296468198</orcidid><orcidid>https://orcid.org/0000000293929681</orcidid><orcidid>https://orcid.org/0000000307109474</orcidid><orcidid>https://orcid.org/0000000317040781</orcidid><orcidid>https://orcid.org/0000000233890586</orcidid><orcidid>https://orcid.org/0000000258144061</orcidid><orcidid>https://orcid.org/0000000271238943</orcidid><orcidid>https://orcid.org/000000018251933X</orcidid><orcidid>https://orcid.org/0000000173164573</orcidid><orcidid>https://orcid.org/0000000332707644</orcidid><orcidid>https://orcid.org/0000000206093987</orcidid><orcidid>https://orcid.org/0000000160828529</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophysical journal. Letters, 2018-01, Vol.852 (1), p.L3 |
| issn | 2041-8205 2041-8213 2041-8213 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1434944 |
| source | Institute of Physics Open Access Journal Titles |
| subjects | ASTRONOMY AND ASTROPHYSICS Astrophysics Computer simulation Datasets Drilling General Relativity and Quantum Cosmology Gravitational collapse Gravitational waves Instrumentation and Detectors INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY Kilonovae Light curve neutron Physics Polls & surveys Red shift stars Stars: Neutron Supernovae Template matching |
| title | How Many Kilonovae Can Be Found in Past, Present, and Future Survey Data Sets? |
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