Author: "Kanner, Jonah" / Publication Type: Electronic Resources - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Kanner, Jonah"' showing total 38 results

Start Over Author "Kanner, Jonah" Publication Type Electronic Resources

38 results on '"Kanner, Jonah"'

1. A search for intermediate-mass black holes mergers in the second LIGO--Virgo observing run with the Bayes Coherence Ratio

Author: Vajpeyi, Avi, Smith, Rory, Thrane, Eric, Ashton, Gregory, Alford, Thomas, Garza, Sierra, Isi, Maximiliano, Kanner, Jonah, Massinger, T. J., Xiao, Liting, Vajpeyi, Avi, Smith, Rory, Thrane, Eric, Ashton, Gregory, Alford, Thomas, Garza, Sierra, Isi, Maximiliano, Kanner, Jonah, Massinger, T. J., and Xiao, Liting
Abstract: The detection of an intermediate-mass black hole population ($10^2-10^6\ M_\odot$) will provide clues to their formation environments (e.g., disks of active galactic nuclei, globular clusters) and illuminate a potential pathway to produce supermassive black holes. Ground-based gravitational-wave detectors are sensitive to a subset of such mergers and have been used to detect one $142^{+28}_{-16}\ M_\odot$ intermediate-mass black hole formation event. However, ground-based detector data contain numerous incoherent short duration noise transients that can mimic the gravitational-wave signals from merging intermediate-mass black holes, limiting the sensitivity of searches. Here we search for binary black hole mergers using a Bayesian-inspired ranking statistic which measures the coherence or incoherence of triggers in multiple-detector data. We use this statistic to identify candidate events with lab-frame total masses $\gtrsim55\ M_\odot$ using data from LIGO's second observing run. Our analysis does not yield evidence for new intermediate-mass black holes. However, we find support for some stellar-mass binary black holes not reported in the first LIGO--Virgo gravitational-wave transient catalog, GWTC-1.
Published: 2021

2. A follow-up on intermediate-mass black hole candidates in the second LIGO-Virgo observing run with the Bayes Coherence Ratio

Author: Vajpeyi, Avi, Smith, Rory, Thrane, Eric, Ashton, Gregory, Alford, Thomas, Garza, Sierra, Isi, Maximiliano, Kanner, Jonah, Massinger, T. J., Xiao, Liting, Vajpeyi, Avi, Smith, Rory, Thrane, Eric, Ashton, Gregory, Alford, Thomas, Garza, Sierra, Isi, Maximiliano, Kanner, Jonah, Massinger, T. J., and Xiao, Liting
Abstract: The detection of an intermediate-mass black hole population ($10^2-10^6$ $M_{\odot}$) will provide clues to their formation environments (e.g., disks of active galactic nuclei, globular clusters) and illuminate a potential pathway to produce supermassive black holes. Ground-based gravitational-wave detectors are sensitive to mergers that can form intermediate-mass black holes weighing up to $\sim 450\ M_{\odot}$. However, ground-based detector data contain numerous incoherent short duration noise transients that can mimic the gravitational-wave signals from merging intermediate-mass black holes, limiting the sensitivity of searches. Here we follow-up on binary black hole merger candidates using a ranking statistic that measures the coherence or incoherence of triggers in multiple-detector data. We use this statistic to rank candidate events, initially identified by all-sky search pipelines, with lab-frame total masses $>55\ M_{\odot}$ using data from LIGO's second observing run. Our analysis does not yield evidence for new intermediate-mass black holes. However, we find support for eight stellar-mass binary black holes not reported in the first LIGO-Virgo gravitational wave transient catalog GWTC-1, seven of which have been previously reported by other catalogs., Comment: 10 pages, 3 figures
Published: 2021
Full Text: View/download PDF

3. The US Program in Ground-Based Gravitational Wave Science: Contribution from the LIGO Laboratory

Author: Reitze, David, Abbott, Rich, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry, Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, GariLynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Tom, Feicht, Jon, Fernandez-Galiana, Alvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Max, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Syd, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard, Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna, Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo, Sanchez, Luis, Savage, Richard, Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, Randy, Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiro, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, Zweizig, John, Reitze, David, Abbott, Rich, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry, Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, GariLynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Tom, Feicht, Jon, Fernandez-Galiana, Alvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Max, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Syd, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard, Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna, Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo, Sanchez, Luis, Savage, Richard, Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, Randy, Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiro, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, and Zweizig, John
Abstract: Recent gravitational-wave observations from the LIGO and Virgo observatories have brought a sense of great excitement to scientists and citizens the world over. Since September 2015,10 binary black hole coalescences and one binary neutron star coalescence have been observed. They have provided remarkable, revolutionary insight into the "gravitational Universe" and have greatly extended the field of multi-messenger astronomy. At present, Advanced LIGO can see binary black hole coalescences out to redshift 0.6 and binary neutron star coalescences to redshift 0.05. This probes only a very small fraction of the volume of the observable Universe. However, current technologies can be extended to construct "$3^\mathrm{rd}$ Generation" (3G) gravitational-wave observatories that would extend our reach to the very edge of the observable Universe. The event rates over such a large volume would be in the hundreds of thousands per year (i.e.tens per hour). Such 3G detectors would have a 10-fold improvement in strain sensitivity over the current generation of instruments, yielding signal-to-noise ratios of 1000 for events like those already seen. Several concepts are being studied for which engineering studies and reliable cost estimates will be developed in the next 5 years., Comment: For the 2020 Astro decadal
Published: 2019

4. The US Program in Ground-Based Gravitational Wave Science: Contribution from the LIGO Laboratory

Author: Reitze, David, Abbott, Richard, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry C., Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, Garilynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Thomas, Feicht, Jon, Fernández-Galiana, Álvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Maximiliano, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Sydney, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard J., Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna A., Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo J., Sanchez, Luis, Savage, Richard L., Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, R., Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiroaki, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, Zweizig, John, Reitze, David, Abbott, Richard, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry C., Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, Garilynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Thomas, Feicht, Jon, Fernández-Galiana, Álvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Maximiliano, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Sydney, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard J., Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna A., Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo J., Sanchez, Luis, Savage, Richard L., Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, R., Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiroaki, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, and Zweizig, John
Abstract: Recent gravitational-wave observations from the LIGO and Virgo observatories have brought a sense of great excitement to scientists and citizens the world over. Since September 2015,10 binary black hole coalescences and one binary neutron star coalescence have been observed. They have provided remarkable, revolutionary insight into the "gravitational Universe" and have greatly extended the field of multi-messenger astronomy. At present, Advanced LIGO can see binary black hole coalescences out to redshift 0.6 and binary neutron star coalescences to redshift 0.05. This probes only a very small fraction of the volume of the observable Universe. However, current technologies can be extended to construct "3rd Generation" (3G) gravitational-wave observatories that would extend our reach to the very edge of the observable Universe. The event rates over such a large volume would be in the hundreds of thousands per year (i.e. tens per hour). Such 3G detectors would have a 10-fold improvement in strain sensitivity over the current generation of instruments, yielding signal-to-noise ratios of 1000 for events like those already seen. Several concepts are being studied for which engineering studies and reliable cost estimates will be developed in the next 5 years.
Published: 2019

5. The US Program in Ground-Based Gravitational Wave Science: Contribution from the LIGO Laboratory

Author: Reitze, David, Abbott, Rich, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry, Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, GariLynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Tom, Feicht, Jon, Fernandez-Galiana, Alvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Max, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Syd, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard, Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna, Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo, Sanchez, Luis, Savage, Richard, Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, Randy, Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiro, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, Zweizig, John, Reitze, David, Abbott, Rich, Adams, Carl, Adhikari, Rana, Aggarwal, Nancy, Anand, Shreya, Ananyeva, Alena, Anderson, Stuart, Appert, Stephen, Arai, Koji, Araya, Melody, Aston, Stuart, Barayoga, Juan, Barish, Barry, Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Betzwieser, Joseph, Billingsley, GariLynn, Biscans, Sebastien, Biscoveanu, Sylvia, Blackburn, Kent, Blair, Carl, Blair, Ryan, Bockelman, Brian, Bork, Rolf, Bramley, Alyssa, Brooks, Aidan, Brunett, Sharon, Buikema, Aaron, Cahillane, Craig, Callister, Thomas, Carruthers, Tom, Clara, Filiberto, Corban, Paul, Coughlin, Michael, Couvares, Peter, Cowart, Matthew, Coyne, Dennis, Demos, Nicholas, Donovan, Fred, Driggers, Jenne, Dwyer, Sheila, Effler, Anamaria, Eisenstein, Robert, Etzel, Todd, Evans, Matthew, Evans, Tom, Feicht, Jon, Fernandez-Galiana, Alvaro, Fritschel, Peter, Frolov, Valery, Fyffe, Michael, Gateley, Bubba, Giaime, Joe, Giardina, Dwayne, Goetz, Evan, Gossan, Sarah, Gras, Slawomir, Grassia, Philippe, Gray, Corey, Gupta, Anchal, Gustafson, Eric, Guthman, Les, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hasskew, Raine, Haster, Carl-Johan, Heintze, Matthew, Hernandez, Edgar, Holt, Kathy, Huang, Yiwen, Huynh-Dinh, Tien, Isi, Max, Jones, Jeff, Kamai, Brittany, Kanner, Jonah, Kasprzack, Marie, Katsavounidis, Erik, Katzman, William, Kawabe, Keita, King, Peter, Kissel, Jeffrey, Kondrashov, Veronica, Korth, William, Kozak, Dan, Kumar, Rahul, Landry, Michael, Lane, Benjamin, Lanza, Robert, Laxen, Michael, Lazzarini, Albert, Lecoeuche, Yannick, Libbrecht, Ken, Lo, Ka-Lok, London, Lionel, Lormand, Marc, MacInnis, Myron, Mansell, Georgia, Markowitz, Aaron, Maros, Ed, Marx, Jay, Mason, Ken, Massinger, Thomas, Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McCormick, Scott, McCuller, Lee, McIver, Jessica, Mendell, Gregory, Merilh, Edmond, Meshkov, Syd, Mittleman, Richard, Moraru, Dan, Moreno, Gerardo, Mullavey, Adam, Nelson, Timothy, Ng, Kwan-Yeung, Noh, Minkyun, O'Reilly, Brian, Oberling, Jason, Oram, Richard, Osthelder, Charles, Overmier, Harry, Parker, William, Pedraza, Mike, Pele, Arnaud, Perez, Carlos, Petterson, Danielle, Pirello, Marc, Raab, Fred, Radkins, Hugh, Mohapatra, Satyanarayan Ray Pitambar, Richardson, Jonathan, Robertson, Norna, Rollins, Jameson, Romel, Chandra, Romie, Janeen, Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo, Sanchez, Luis, Savage, Richard, Schaetzl, Dean, Sellers, Danny, Shaffer, Thomas, Shoemaker, David, Sigg, Daniel, Strunk, Amber, Sudhir, Vivishek, Sun, Ling, Tao, Duo, Taylor, Robert, Thomas, Michael, Thomas, Patrick, Thorne, Keith, Torrie, Calum, Traylor, Gary, Trudeau, Randy, Tse, Maggie, Vajente, Gabriele, Vass, Steve, Venugopalan, Gautam, Vitale, Salvatore, Vorvick, Cheryl, Wade, Andrew, Wallace, Larry, Warner, Jim, Weaver, Betsy, Weinstein, Alan, Weiss, Rainer, Whitcomb, Stan, Whittle, Chris, Willis, Joshua, Wipf, Christopher, Xiao, Sophia, Yamamoto, Hiro, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael, and Zweizig, John
Abstract: Recent gravitational-wave observations from the LIGO and Virgo observatories have brought a sense of great excitement to scientists and citizens the world over. Since September 2015,10 binary black hole coalescences and one binary neutron star coalescence have been observed. They have provided remarkable, revolutionary insight into the "gravitational Universe" and have greatly extended the field of multi-messenger astronomy. At present, Advanced LIGO can see binary black hole coalescences out to redshift 0.6 and binary neutron star coalescences to redshift 0.05. This probes only a very small fraction of the volume of the observable Universe. However, current technologies can be extended to construct "$3^\mathrm{rd}$ Generation" (3G) gravitational-wave observatories that would extend our reach to the very edge of the observable Universe. The event rates over such a large volume would be in the hundreds of thousands per year (i.e.tens per hour). Such 3G detectors would have a 10-fold improvement in strain sensitivity over the current generation of instruments, yielding signal-to-noise ratios of 1000 for events like those already seen. Several concepts are being studied for which engineering studies and reliable cost estimates will be developed in the next 5 years., Comment: For the 2020 Astro decadal
Published: 2019

6. Gravitational-Wave Geodesy: A New Tool for Validating Detection of the Stochastic Gravitational-Wave Background

Author: Callister, Thomas, Coughlin, Michael, Kanner, Jonah, Callister, Thomas, Coughlin, Michael, and Kanner, Jonah
Abstract: A valuable target for advanced gravitational-wave detectors is the stochastic gravitational-wave background. The stochastic background imparts a weak correlated signal into networks of gravitational-wave detectors, and so standard searches for the gravitational-wave background rely on measuring cross-correlations between pairs of widely-separated detectors. Stochastic searches, however, can be affected by any other correlated effects which may also be present, including correlated frequency combs and magnetic Schumann resonances. As stochastic searches become sensitive to ever-weaker signals, it is increasingly important to develop methods to separate a true astrophysical signal from other spurious and/or terrestrial signals. Here, we describe a novel method to achieve this goal -- gravitational-wave geodesy. Just as radio geodesy allows for the localization of radio telescopes, so too can observations of the gravitational-wave background be used to infer the positions and orientations of gravitational-wave detectors. By demanding that a true observation of the gravitational-wave background yield constraints consistent with the baseline's known geometry, we demonstrate that we can successfully validate true observations of the gravitational-wave background while rejecting spurious signals due to correlated terrestrial effects., Comment: Minor typos corrected
Published: 2018
Full Text: View/download PDF

7. Enhancing confidence in the detection of gravitational waves from compact binaries using signal coherence

Author: Isi, Maximiliano, Smith, Rory, Vitale, Salvatore, Massinger, T. J., Kanner, Jonah, Vajpeyi, Avi, Isi, Maximiliano, Smith, Rory, Vitale, Salvatore, Massinger, T. J., Kanner, Jonah, and Vajpeyi, Avi
Abstract: We show that gravitational-wave signals from compact binary mergers may be better distinguished from instrumental noise transients by using Bayesian models that look for signal coherence across a detector network. This can be achieved even when the signal power is below the usual threshold for detection. This method could reject the vast majority of noise transients, and therefore increase sensitivity to weak gravitational waves. We demonstrate this using simulated signals, as well as data for GW150914 and LVT151012. Finally, we explore ways of incorporating our method into existing Advanced LIGO and Virgo searches to make them significantly more powerful.
Published: 2018
Full Text: View/download PDF

8. Full band all-sky search for periodic gravitational waves in the O1 LIGO data

Author: Abbott, Benjamin P., Abbott, Rich, Abbott, Thomas D., Acernese, Fausto, Ackley, Kendall, Adams, Carl, Adams, Thomas, Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali B., Affeldt, Christoph, Afrough, Mohammad, Agarwal, Bhanu, Agathos, Michalis, Agatsuma, Kazuhiro, Aggarwal, Nancy, Aguiar, Odylio D., Aiello, Lorenzo, Ain, Anirban, Allen, Bruce, Allen, Gabrielle, Allocca, Annalisa, Altin, Paul A., Amato, Alex, Ananyeva, Alena, Anderson, Stuart B., Anderson, Warren G., Angelova, Svetoslava V., Antier, Sarah, Appert, Stephen, Arai, Koji, Araya, Melody C., Areeda, Joseph S., Arnaud, Nicolas, Ascenzi, Stefano, Ashton, Gregory, Ast, M., Aston, Stuart M., Astone, Pia, Atallah, Dany V., Aufmuth, Peter, Aulbert, Carsten, AultONeal, K., Austin, Corey, Avila-Alvarez, A., Babak, Stanislav, Bacon, Philippe, Bader, Maria K.M., Bae, Sangwook, Baker, Paul T., Baldaccini, Francesca, Ballardin, Giulio, Ballmer, Stefan W., Banagiri, Sharan, Barayoga, Juan C., Barclay, Sheena E., Barish, Barry C., Barker, David, Barkett, Kevin, Barone, Fabrizio, Barr, Bryan, Barsotti, Lisa, Barsuglia, Matteo, Barta, Daniel, Bartlett, Jeffrey, Bartos, Imre, Bassiri, Riccardo, Basti, Andrea, Batch, James C., Bawaj, Mateusz, Bayley, Joseph C., Bazzan, Marco, Bécsy, Bence, Beer, Christian, Bejger, Michal, Belahcene, Imene, Bell, Angus S., Berger, Beverly K., Bergmann, Gerald, Bero, John J., Berry, Christopher P.L., Bersanetti, Diego, Bertolini, Alessandro, Betzwieser, Joseph, Bhagwat, Swetha, Bhandare, Rohan, Bilenko, Igor A., Billingsley, Garilynn, Billman, Chris R., Birch, Jeremy, Birney, Ross, Birnholtz, Ofek, Biscans, Sebastien, Biscoveanu, Sylvia, Bisht, Aparna, Bitossi, Massimiliano, Biwer, Christopher, Bizouard, Marieanne A., Blackburn, J.K., Blackman, Jonathan, Blair, Carl D., Blair, David G., Blair, Ryan M., Bloemen, Steven, Bock, Oliver, Bode, Nina, Boer, Michel, Bogaert, Gilles, Bohe, Alejandro, Bondu, Francois, Bonilla, Edgard, Bonnand, Romain, Boom, Boris A., Bork, Rolf, Boschi, Valerio, Bose, Sukanta, Bossie, Ken, Bouffanais, Yann, Bozzi, Antonella, Bradaschia, Carlo, Brady, Patrick R., Branchesi, Marica, Brau, Jim E., Briant, Tristan, Brillet, Alain, Brinkmann, Marc, Brisson, Violette, Brockill, Patrick, Broida, Jacob E., Brooks, Aidan F., Brown, Duncan A., Brown, Daniel D., Brunett, Sharon, Buchanan, Christopher C., Buikema, Aaron, Bulik, Tomasz, Bulten, Henk J., Buonanno, Alessandra, Buskulic, Damir, Buy, Christelle, Byer, Robert L., Cabero, Miriam, Cadonati, Laura, Cagnoli, Giampietro, Cahillane, Craig, Calderón Bustillo, J., Callister, Thomas A., Calloni, Enrico, Camp, Jordan B., Canepa, Maurizio, Canizares, Priscilla, Cannon, Kipp C., Cao, H., Cao, Junwei, Capano, Collin D., Capocasa, Eleonora, Carbognani, Franco, Caride, Santiago, Carney, Matthew F., Casanueva Diaz, J., Casentini, Claudio, Caudill, Sarah, Cavaglià, Marco, Cavalier, Fabien, Cavalieri, Roberto, Cella, Giancarlo, Cepeda, Christian B., Cerdá-Durán, P., Cerretani, Giovanni, Cesarini, Elisabetta, Chamberlin, Sydney J., Chan, Manleong, Chao, Shiuh, Charlton, Philip, Chase, Eve, Chassande-Mottin, E., Chatterjee, Deep, Cheeseboro, Belinda D., Chen, H.Y., Chen, Xu, Chen, Yanbei, Cheng, H.-P., Chia, Hanyu Y., Chincarini, Andrea, Chiummo, Antonino, Chmiel, Theresa, Cho, Heesuk S., Cho, M., Chow, Jong H., Christensen, Nelson, Chu, Qi, Chua, Alvin J.K., Chua, Sheon, Chung, A.K.W., Chung, Shinkee, Ciani, Giacomo, Ciecielag, P., Ciolfi, Riccardo, Cirelli, Carissa E., Cirone, Alessio, Clara, Filiberto, Clark, James A., Clearwater, Patrick, Cleva, Frederic, Cocchieri, Camillo, Coccia, Eugenio, Cohadon, P.-F., Cohen, David, Colla, Alberto, Collette, Christophe G., Cominsky, Lynn R., Constancio, M., Conti, Livia, Cooper, Sam J., Corban, Paul, Corbitt, Thomas R., Cordero-Carrión, I., Corley, Kenneth R., Cornish, Neil, Corsi, Alessandra, Cortese, Stefano, Costa, Cesar A., Coughlin, Eric T., Coughlin, Michael W., Coughlin, Scott B., Coulon, J.-P., Countryman, Stefan T., Couvares, Peter, Covas, Pep B., Cowan, Erika E., Coward, David M., Cowart, Matthew J., Coyne, Dennis C., Coyne, Robert, Creighton, Jolien D.E., Creighton, Teviet D., Cripe, Jonathan, Crowder, Sgwynne G., Cullen, Torrey J., Cumming, Alan, Cunningham, Liam, Cuoco, Elena, Dal Canton, Tito, Dálya, Gergely, Danilishin, Stefan L., D'Antonio, S., Danzmann, Karsten, Dasgupta, Arnab, Da Silva Costa, C.F., Dattilo, Vincenzo, Dave, Ishant, Davier, Michel, Davis, Derek, Daw, Edward J., Day, Brian, De, Soumi, Debra, D., Degallaix, Jerome, De Laurentis, M., Deléglise, Samuel, Del Pozzo, W., Demos, Nicholas, Denker, Timo, Dent, Thomas, De Pietri, R., Dergachev, Vladimir, De Rosa, R., DeRosa, R.T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, Jan, Dhurandhar, Sanjeev, Díaz, Mario C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Zoheyr, Dolique, Vincent, Donovan, Fred, Dooley, Katherine L., Doravari, Suresh, Dorosh, O., Dorrington, Iain, Douglas, Rebecca, Dovale Álvarez, M., Downes, Thomas P., Drago, Marco, Dreissigacker, Christoph, Driggers, Jenne C., Du, Zhihui, Ducrot, Marine, Dupej, Peter, Dwyer, Sheila E., Edo, Tega B., Edwards, Matthew C., Effler, Anamaria, Eggenstein, H.-B., Ehrens, Phil, Eichholz, Johannes, Eikenberry, Stephen S., Eisenstein, Robert A., Essick, Reed C., Estevez, Dimitri, Etienne, Zachariah B., Etzel, Todd, Evans, Matthew, Evans, Tom M., Factourovich, Maxim, Fafone, Viviana, Fair, Hannah, Fairhurst, Stephen, Fan, Xilong, Farinon, Stefania, Farr, Benjamin, Farr, Will M., Fauchon-Jones, E.J., Favata, Marc, Fays, Maxime, Fee, Campbell, Fehrmann, Henning, Feicht, Jon, Fejer, Martin M., Fernandez-Galiana, A., Ferrante, Isidoro, Ferreira, Elvis C., Ferrini, Federico, Fidecaro, Francesco, Finstad, Daniel, Fiori, Irene, Fiorucci, Donatella, Fishbach, Maya, Fisher, Ryan P., Fitz-Axen, M., Flaminio, Raffaele, Fletcher, Mark, Fong, Heather, Font, J.A., Forsyth, Perry W.F., Forsyth, Steven S., Fournier, J.-D., Frasca, Sergio, Frasconi, Franco, Frei, Zsolt, Freise, Andreas, Frey, Raymond, Frey, Valentin, Fries, Eric M., Fritschel, Peter, Frolov, Valery V., Fulda, Paul, Fyffe, Michael, Gabbard, Hunter, Gadre, Bhooshan U., Gaebel, Sebastian M., Gair, Jonathan R., Gammaitoni, Luca, Ganija, Miftar R., Gaonkar, Sharad G., Garcia-Quiros, C., Garufi, Fabio, Gateley, B., Gaudio, Sergio, Gaur, Gurudatt, Gayathri, V., Gehrels, Neil, Gemme, Gianluca, Genin, Eric, Gennai, Alberto, George, Daniel, George, Jogy, Gergely, Laszlo, Germain, Vincent, Ghonge, Sudarshan, Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Giaime, Joe A., Giardina, K.D., Giazotto, Adalberto, Gill, Kiranjyot, Glover, Lamar, Goetz, Evan, Goetz, Ryan, Gomes, Sandra, Goncharov, Boris, González, Gabriela, Gonzalez Castro, J.M., Gopakumar, A., Gorodetsky, Michael L., Gossan, Sarah E., GOSSELIN, Matthieu, Gouaty, Romain, Grado, Aniello, Graef, Christian, Granata, Massimo, Grant, Alastair, Gras, Slawomir, Gray, Corey, Greco, Giuseppe, Green, Anna C., Gretarsson, Elizabeth M., Groot, Paul, Grote, Hartmut, Grunewald, Steffen, Gruning, Pierre, Guidi, Gianluca M., Guo, Xiangyu, Gupta, Anuradha, Gupta, Manojipr K., Gushwa, Kaitlin E., Gustafson, Eric K., Gustafson, R., Halim, O., Hall, Bernard R., Hall, Evan D., Hamilton, Eleanor Z., Hammond, Giles, Haney, Maria, Hanke, Manuela M., Hanks, Jonathan, Hanna, Chad, Hannam, Mark D., Hannuksela, Otto A., Hanson, Joe, Hardwick, Terra, Harms, Jan, Harry, Gregg M., Harry, Ian W., Hart, Martin J., Haster, C.-J., Haughian, Karen, Healy, James, Heidmann, Antoine, Heintze, Matthew C., Heitmann, Henrich, Hello, Patrice, Hemming, Gary, Hendry, Martin, Heng, I.S., Hennig, J., Heptonstall, Alastair W., Heurs, Michele, Hild, Stefan, Hinderer, Tanja, Hoak, Daniel, Hofman, David, Holt, Kathy, Holz, Daniel E., Hopkins, Paul, Horst, Christian, Hough, James, Houston, Ewan A., Howell, Eric J., Hreibi, A., Hu, Yiming M., Huerta, Eliu A., Huet, Dominique, Hughey, Brennan, Husa, Sascha, Huttner, Sabina H., Huynh-Dinh, T., Indik, Nathaniel, Inta, Ra, Intini, Giuseppe, Isa, Hafizah N., Isac, J.-M., Isi, Max, Iyer, Bala R., Izumi, Kiwamu, Jacqmin, Thibaut, Jani, Karan, Jaranowski, Piotr, Jawahar, Sharat, Jiménez-Forteza, F., Johnson, Warren W., Jones, D.I., Jones, Russell, Jonker, Reinier J.G., Ju, L., Junker, Jonas, Kalaghatgi, Chinmay V., Kalogera, Vassiliki, Kamai, Brittany, Kandhasamy, Shivaraj, Kang, Gungwon, Kanner, Jonah B., Kapadia, Shasvath J., Karki, Sudarshan, Karvinen, Kai S., Kasprzack, Marie, Katolik, Michael, Katsavounidis, Erik, Katzman, William, Kaufer, Steffen, Kawabe, Keita, Kéfélian, Fabien, Keitel, David, Kemball, Athol J., Kennedy, Ross, Kent, Christopher, Key, Joey S., Khalili, Farit Y., Khan, I., Khan, Sebastian, Khan, Ziauddin, Khazanov, Efim A., Kijbunchoo, Nutsinee, Kim, Chunglee, Kim, Jeongcho C., Kim, Kyungmin, Kim, Won, Kim, Whansun S., Kim, Y.-M., Kimbrell, Seth J., King, Eleanor J., King, Peter J., Kinley-Hanlon, M., Kirchhoff, Robin, Kissel, Jeffrey S., Kleybolte, Lisa, Klimenko, Sergei, Knowles, Tyler D., Koch, Philip, Koehlenbeck, Sina M., Koley, Soumen, Kondrashov, Veronica, Kontos, Antonios, Korobko, Mikhail, Korth, William Z., Kowalska, Izabela, Kozak, Dan B., Krämer, Christina, Kringel, Volker, Krishnan, Badri, Królak, Andrzej, Kuehn, Gerrit, Kumar, Prayush, Kumar, Rakesh, Kumar, Sumit, Kuo, L., Kutynia, Adam, Kwang, Shawn, Lackey, Benjamin D., Lai, K.H., Landry, Michael, Lang, Ryan N., Lange, Jacob, Lantz, Brian, Lanza, Robert K., Lartaux-Vollard, A., Lasky, Paul D., Laxen, Michael, Lazzarini, Albert, Lazzaro, Claudia, Leaci, Paola, Leavey, Sean, Lee, C.H., Lee, Hyunkyu K., Lee, H.M., Lee, Hyungwon W., Lee, K., Lehmann, Johannes, Lenon, Amber, Leonardi, Matteo, Leroy, Nicolas, Letendre, Nicolas, Levin, Yuri, Li, Tjonnie G.F., Linker, Seth D., Littenberg, Tyson B., Liu, J., Lo, R.K.L., Lockerbie, Nick A., London, Lionel T., Lord, Jaysin E., Lorenzini, Matteo, Loriette, Vincent, Lormand, Marc, Losurdo, Giovanni, Lough, James D., Lovelace, Geoffrey, Lück, Harald, Lumaca, Diana, Lundgren, Andrew P., Lynch, Ryan, Ma, Y., Macas, Ronaldas, Macfoy, Sean, Machenschalk, Bernd, Macinnis, M., Macleod, Duncan M., Magaña Hernandez, I., Magaña-Sandoval, F., Magaña Zertuche, L., Magee, Ryan M., Majorana, Ettore, Maksimovic, Ivan, Man, N., Mandic, Vuk, Mangano, Valentina, Mansell, Georgia L., Manske, Michael, Mantovani, Maddalena, Marchesoni, Fabio, Marion, Frederique, Márka, Szabolcs, Márka, Zsuzsanna, Markakis, Charalampos, Markosyan, Ashot S., Markowitz, Aaron, Maros, E., Marquina, Antonio, Martelli, Filippo, Martellini, Lionel, Martin, Ian W., Martin, Rodica M., Martynov, Denis V., Mason, Ken, Massera, Elena, Masserot, Alain, Massinger, Thomas J., Masso-Reid, M., Mastrogiovanni, Simone, Matas, Andrew, Matichard, Fabrice, Matone, Luca, Mavalvala, Nergis, Mazumder, Nairwita, McCarthy, R., Mcclelland, D.E., Mccormick, S., McCuller, L., McGuire, S.C., Mcintyre, G., Mciver, J., McManus, David J., McNeill, L., McRae, T., McWilliams, S.T., Meacher, Duncan, Meadors, Grant D., Mehmet, Moritz, Meidam, Jeroen, Mejuto-Villa, E., Melatos, Andrew, Mendell, Gregory, Mercer, R.A., Merilh, Edmond L., Merzougui, Mourad, Meshkov, Syd, Messenger, Chris, Messick, Cody, Metzdorff, R., Meyers, Patrick M., Miao, Haixing, Michel, Christophe, Middleton, Hannah, Mikhailov, Eugeniy E., Milano, Leopoldo, Miller, Andrewlawrence L., Miller, Brandon B., Miller, John, Millhouse, Meg, Milovich-Goff, M.C., Minazzoli, Olivier, Minenkov, Yuri, Ming, Jing, Mishra, Chandra, Mitra, Sanjit, Mitrofanov, Valery P., Mitselmakher, Guenakh, Mittleman, Richard, Moffa, Donald, Moggi, Andrea, Mogushi, Kentaro, Mohan, Martin, Mohapatra, S.R.P., Montani, Matteo, Moore, Christopher J., Moraru, Dan, Moreno, Gerardo, Morriss, Sean R., Mours, Benoit, Mow-Lowry, C.M., Mueller, Guido, Muir, Alistair W., Mukherjee, Arunava, Mukherjee, Debnandini, Mukherjee, Soma, Mukund, Nikhil, Mullavey, Adam, Munch, Jesper, Muñiz, Erik A., Muratore, Martina, Murray, Peter G., Napier, Kate, Nardecchia, Ilaria, Naticchioni, Luca, Nayak, Rajesh K., Neilson, Joshua, Nelemans, Gijs, Nelson, Timothy J.N., Nery, Marina, Neunzert, Ansel, Nevin, Lydia, Newport, Jonathan M., Newton, Gavin, Ng, K.Y., Nguyen, Thanh T., Nichols, David, Nielsen, Alex B., Nissanke, Samaya, Nitz, Alex, Noack, Andreas, Nocera, Flavio, Nolting, David, North, Chris, Nuttall, Laura K., Oberling, Jason, O'Dea, G.D., Ogin, Greg H., Oh, John J., Oh, Sanghoon H., Ohme, Frank, Okada, Marcos A., Oliver, Miquel, Oppermann, Patrick, Oram, Richard J., O'Reilly, B., Ormiston, Rich, Ortega, Luis F., O'Shaughnessy, R., Ossokine, Serguei, Ottaway, David J., Overmier, Harry, Owen, Ben J., Pace, Alexander E., Page, Jessica, Page, Michael A., Pai, Archana, Pai, Siddhesh A., Palamos, Jordan R., Palashov, Oleg, Palomba, Cristiano, Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, Belinda, Pang, P.T.H., Pankow, Chris, Pannarale, Francesco, Pant, Brijesh C., Paoletti, Federico, PAOLI, Andrea, Papa, Maria A., Parida, Abhishek, Parker, William, Pascucci, Daniela, Pasqualetti, Antonio, Passaquieti, Roberto, Passuello, Diego, Patil, M., Patricelli, Barbara, Pearlstone, Brynley L., Pedraza, Mike, Pedurand, Richard, Pekowsky, L., Pele, Arnaud, Penn, Steven, Perez, Carlos J., Perreca, Antonio, Perri, Leah M., Pfeiffer, Harald P., Phelps, Margot, Piccinni, Ornella J., Pichot, Mikhael, Piergiovanni, Francesco, Pierro, Vincenzo, Pillant, Gabriel, Pinard, Laurent, Pinto, Innocenzo M., Pirello, Marc, Pisarski, A., Pitkin, Matthew, Poe, Mark, Poggiani, Rosa, Popolizio, Pasquale, Porter, K., Post, Alexander, Powell, Jade, Prasad, Jayanti, Pratt, James W.W., Pratten, Geraint, Predoi, Valeriu, Prestegard, Tanner, Prijatelj, Mirko, Principe, Maria, Privitera, Stephen, Prodi, Giovanni A., Prokhorov, Leonid G., Puncken, Oliver, Punturo, Michele, Puppo, Paola, Pürrer, Michael, Qi, Hong, Quetschke, Volker, Quintero, Eric A., Quitzow-James, R., Raab, Fred J., Rabeling, David S., Radkins, Hugh, Raffai, Peter, Raja, Sendhil, Rajan, C., Rajbhandari, Binod, Rakhmanov, Malik, Ramirez, Karla E., Ramos-Buades, A., Rapagnani, Piero, Raymond, Vivien, Razzano, Massimiliano, Read, Jocelyn, Regimbau, Tania, Rei, Luca, Reid, Stuart, Reitze, David H., Ren, Wei, Reyes, Steven D., Ricci, Fulvio, Ricker, Paul M., Rieger, Sascha, Riles, Keith, Rizzo, Monica, Robertson, Norna A., Robie, Raymond, Robinet, Florent, Rocchi, Alessio, ROLLAND, Loic, Rollins, Jameson G., Roma, Vincent J., Romano, Rocco, Romel, Chandra L., Romie, Janeen H., Rosińska, Dorota, Ross, Michael P., Rowan, Sheila, Rüdiger, Albrecht, Ruggi, Paolo, Rutins, Guntis, Ryan, Kyle, Sachdev, Surabhi, Sadecki, Travis, Sadeghian, Laleh, Sakellariadou, Mairi, Salconi, Livio, Saleem, Muhammed, Salemi, Francesco, Samajdar, Anuradha, Sammut, Letizia, Sampson, Laura M., Sanchez, Eduardo J., Sanchez, Luis E., Sanchis-Gual, N., Sandberg, Vernon, Sanders, Jaclyn R., Sassolas, Benoit, Saulson, Peter R., Sauter, Orion, Savage, Richard L., Sawadsky, Andreas, Schale, Paul, Scheel, Mark, Scheuer, Jacob, Schmidt, Justus, Schmidt, Patricia, Schnabel, Roman, Schofield, Robert M.S., Schönbeck, Axel, Schreiber, Emil, Schuette, Dirk, Schulte, Bernd W., Schutz, Bernard F., Schwalbe, Sophia G., Scott, Jamie, Scott, Susan M., Seidel, E., Sellers, Danny, Sengupta, Anand S., Sentenac, Daniel, Sequino, Valeria, Sergeev, Alexander, Shaddock, Daniel A., Shaffer, Thomas J., Shah, Ankur A., Shahriar, M.S., Shaner, Morgan B., Shao, Lijing, Shapiro, Brett, Shawhan, Peter, Sheperd, Alec, Shoemaker, David H., Shoemaker, Deirdre M., Siellez, Karelle, Siemens, Xavier, Sieniawska, Magdalena, Sigg, Daniel, Silva, Allan D., Singer, Leo P., Singh, Avneet, Singhal, Akshat, Sintes, Alicia M., Slagmolen, Bram J.J., Smith, Bryan, Smith, Joshua R., Smith, Rory J.E., Somala, Surendranadh, Son, Edwin J., Sonnenberg, Jacob A., Sorazu, Borja, Sorrentino, Fiodor, Souradeep, Tarun, Spencer, Andrew P., Srivastava, Amit K., Staats, Kai, Staley, Alexan, Steinke, Michael, Steinlechner, Jessica, Steinlechner, Sebastian, Steinmeyer, Daniel, Stevenson, Simon P., Stone, Robert, Stops, David J., Strain, Ken A., Stratta, Giulia, Strigin, Sergey E., Strunk, A., Sturani, Riccardo, Stuver, Amber L., Summerscales, Tiffany Z., Sun, Ling, Sunil, S., Suresh, Jishnu, Sutton, Patrick J., Swinkels, Bas L., Szczepańczyk, Marek J., Tacca, Matteo, Tait, Simon C., Talbot, Colm, Talukder, Dipongkar, Tanner, David B., Tao, Duo, Tápai, Marton, Taracchini, Andrea, Tasson, Jay D., Taylor, Jordan A., Taylor, Robert, Tewari, Shivam V., Theeg, Thomas, Thies, Fabian, Thomas, E.G., Thomas, Michael, Thomas, Patrick, Thorne, Keith A., Thrane, Eric, Tiwari, Shubhanshu, Tiwari, Vaibhav, Tokmakov, Kirill V., Toland, Karl, Tonelli, Mauro, Tornasi, Zeno, Torres-Forné, A., Torrie, Calum I., Töyrä, Daniel, Travasso, Flavio, Traylor, Gary, Trinastic, Jonathan, Tringali, Maria C., Trozzo, Lucia, Tsang, K.W., Tse, Maggie, Tso, Rhondale, Tsukada, Leo, Tsuna, Daichi, Tuyenbayev, Darkhan, Ueno, Koh, Ugolini, Dennis, Unnikrishnan, Cs S., Urban, Alexander L., Usman, Samantha A., Vahlbruch, Henning, Vajente, Gabriele, Valdes, Guillermo, Van Bakel, N., van Beuzekom, Martin, Van Den Brand, J.F.J., Van Den Broeck, C., Vander-Hyde, D.C., van der Schaaf, L., van Heijningen, J.V., van Veggel, A.A., Vardaro, Marco, Varma, Vijay, Vass, Steve, Vasúth, Matyas, Vecchio, Alberto, Vedovato, Gabriele, Veitch, John, Veitch, Peter J., Venkateswara, Krishna, Venugopalan, Gautam, Verkindt, Didier, Vetrano, Flavio, Viceré, Andrea, Viets, Aaron D., Vinciguerra, Serena, Vine, David J., Vinet, J.-Y., Vitale, Salvatore, Vo, Thomas, Vocca, Helios, Vorvick, Cheryl, Vyatchanin, Sergey P., Wade, Andrew R., Wade, Leslie E., Wade, Madeline, Walet, Rob, Walker, Marissa, Wallace, Larry, Walsh, Sinead, Wang, Gang, Wang, Haoyu, Wang, Jonathan Z., Wang, Wenhui H., Wang, Yifan F., Ward, Robert L., Warner, Jim, Was, Michal, Watchi, Jennifer, Weaver, Betsy, Wei, L.-W., Weinert, Michael, Weinstein, Alan J., Weiss, Rainer, Wen, Linqing, Wessel, Erik K., Weßels, Peter, Westerweck, Julian, Westphal, Tobias, Wette, Karl, Whelan, John T., Whiting, Bernard F., Whittle, Chris, Wilken, D., Williams, Daniel, Williams, Roy D., Williamson, Andrew R., Willis, Joshua L., Willke, Benno, Wimmer, Maximilian H., Winkler, Walter, Wipf, Christopher C., Wittel, Holger, Woan, Graham, Woehler, Janis, Wofford, Jared, Wong, W.K., Worden, John, Wright, Jennifer L., Wu, David S., Wysocki, Daniel M., Xiao, Sophia, Yamamoto, Hiro, Yancey, Cregg C., Yang, Le, Yap, M.J., Yazback, Maher, Yu, Hang, Yu, Haocun, Yvert, Michel, Zadrożny, Adam, Zanolin, Michele, Zelenova, Tatiana, Zendri, J.-P., Zevin, Michael, Zhang, Liyuan, Zhang, Mi, Zhang, Teng, Zhang, Y.-H., Zhao, Chunnong, Zhou, Minchuan, Zhou, Zifan, Zhu, Sylvia J., Zhu, Xingjiang J., Zucker, Michael E., Zweizig, J., Abbott, Benjamin P., Abbott, Rich, Abbott, Thomas D., Acernese, Fausto, Ackley, Kendall, Adams, Carl, Adams, Thomas, Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali B., Affeldt, Christoph, Afrough, Mohammad, Agarwal, Bhanu, Agathos, Michalis, Agatsuma, Kazuhiro, Aggarwal, Nancy, Aguiar, Odylio D., Aiello, Lorenzo, Ain, Anirban, Allen, Bruce, Allen, Gabrielle, Allocca, Annalisa, Altin, Paul A., Amato, Alex, Ananyeva, Alena, Anderson, Stuart B., Anderson, Warren G., Angelova, Svetoslava V., Antier, Sarah, Appert, Stephen, Arai, Koji, Araya, Melody C., Areeda, Joseph S., Arnaud, Nicolas, Ascenzi, Stefano, Ashton, Gregory, Ast, M., Aston, Stuart M., Astone, Pia, Atallah, Dany V., Aufmuth, Peter, Aulbert, Carsten, AultONeal, K., Austin, Corey, Avila-Alvarez, A., Babak, Stanislav, Bacon, Philippe, Bader, Maria K.M., Bae, Sangwook, Baker, Paul T., Baldaccini, Francesca, Ballardin, Giulio, Ballmer, Stefan W., Banagiri, Sharan, Barayoga, Juan C., Barclay, Sheena E., Barish, Barry C., Barker, David, Barkett, Kevin, Barone, Fabrizio, Barr, Bryan, Barsotti, Lisa, Barsuglia, Matteo, Barta, Daniel, Bartlett, Jeffrey, Bartos, Imre, Bassiri, Riccardo, Basti, Andrea, Batch, James C., Bawaj, Mateusz, Bayley, Joseph C., Bazzan, Marco, Bécsy, Bence, Beer, Christian, Bejger, Michal, Belahcene, Imene, Bell, Angus S., Berger, Beverly K., Bergmann, Gerald, Bero, John J., Berry, Christopher P.L., Bersanetti, Diego, Bertolini, Alessandro, Betzwieser, Joseph, Bhagwat, Swetha, Bhandare, Rohan, Bilenko, Igor A., Billingsley, Garilynn, Billman, Chris R., Birch, Jeremy, Birney, Ross, Birnholtz, Ofek, Biscans, Sebastien, Biscoveanu, Sylvia, Bisht, Aparna, Bitossi, Massimiliano, Biwer, Christopher, Bizouard, Marieanne A., Blackburn, J.K., Blackman, Jonathan, Blair, Carl D., Blair, David G., Blair, Ryan M., Bloemen, Steven, Bock, Oliver, Bode, Nina, Boer, Michel, Bogaert, Gilles, Bohe, Alejandro, Bondu, Francois, Bonilla, Edgard, Bonnand, Romain, Boom, Boris A., Bork, Rolf, Boschi, Valerio, Bose, Sukanta, Bossie, Ken, Bouffanais, Yann, Bozzi, Antonella, Bradaschia, Carlo, Brady, Patrick R., Branchesi, Marica, Brau, Jim E., Briant, Tristan, Brillet, Alain, Brinkmann, Marc, Brisson, Violette, Brockill, Patrick, Broida, Jacob E., Brooks, Aidan F., Brown, Duncan A., Brown, Daniel D., Brunett, Sharon, Buchanan, Christopher C., Buikema, Aaron, Bulik, Tomasz, Bulten, Henk J., Buonanno, Alessandra, Buskulic, Damir, Buy, Christelle, Byer, Robert L., Cabero, Miriam, Cadonati, Laura, Cagnoli, Giampietro, Cahillane, Craig, Calderón Bustillo, J., Callister, Thomas A., Calloni, Enrico, Camp, Jordan B., Canepa, Maurizio, Canizares, Priscilla, Cannon, Kipp C., Cao, H., Cao, Junwei, Capano, Collin D., Capocasa, Eleonora, Carbognani, Franco, Caride, Santiago, Carney, Matthew F., Casanueva Diaz, J., Casentini, Claudio, Caudill, Sarah, Cavaglià, Marco, Cavalier, Fabien, Cavalieri, Roberto, Cella, Giancarlo, Cepeda, Christian B., Cerdá-Durán, P., Cerretani, Giovanni, Cesarini, Elisabetta, Chamberlin, Sydney J., Chan, Manleong, Chao, Shiuh, Charlton, Philip, Chase, Eve, Chassande-Mottin, E., Chatterjee, Deep, Cheeseboro, Belinda D., Chen, H.Y., Chen, Xu, Chen, Yanbei, Cheng, H.-P., Chia, Hanyu Y., Chincarini, Andrea, Chiummo, Antonino, Chmiel, Theresa, Cho, Heesuk S., Cho, M., Chow, Jong H., Christensen, Nelson, Chu, Qi, Chua, Alvin J.K., Chua, Sheon, Chung, A.K.W., Chung, Shinkee, Ciani, Giacomo, Ciecielag, P., Ciolfi, Riccardo, Cirelli, Carissa E., Cirone, Alessio, Clara, Filiberto, Clark, James A., Clearwater, Patrick, Cleva, Frederic, Cocchieri, Camillo, Coccia, Eugenio, Cohadon, P.-F., Cohen, David, Colla, Alberto, Collette, Christophe G., Cominsky, Lynn R., Constancio, M., Conti, Livia, Cooper, Sam J., Corban, Paul, Corbitt, Thomas R., Cordero-Carrión, I., Corley, Kenneth R., Cornish, Neil, Corsi, Alessandra, Cortese, Stefano, Costa, Cesar A., Coughlin, Eric T., Coughlin, Michael W., Coughlin, Scott B., Coulon, J.-P., Countryman, Stefan T., Couvares, Peter, Covas, Pep B., Cowan, Erika E., Coward, David M., Cowart, Matthew J., Coyne, Dennis C., Coyne, Robert, Creighton, Jolien D.E., Creighton, Teviet D., Cripe, Jonathan, Crowder, Sgwynne G., Cullen, Torrey J., Cumming, Alan, Cunningham, Liam, Cuoco, Elena, Dal Canton, Tito, Dálya, Gergely, Danilishin, Stefan L., D'Antonio, S., Danzmann, Karsten, Dasgupta, Arnab, Da Silva Costa, C.F., Dattilo, Vincenzo, Dave, Ishant, Davier, Michel, Davis, Derek, Daw, Edward J., Day, Brian, De, Soumi, Debra, D., Degallaix, Jerome, De Laurentis, M., Deléglise, Samuel, Del Pozzo, W., Demos, Nicholas, Denker, Timo, Dent, Thomas, De Pietri, R., Dergachev, Vladimir, De Rosa, R., DeRosa, R.T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, Jan, Dhurandhar, Sanjeev, Díaz, Mario C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Zoheyr, Dolique, Vincent, Donovan, Fred, Dooley, Katherine L., Doravari, Suresh, Dorosh, O., Dorrington, Iain, Douglas, Rebecca, Dovale Álvarez, M., Downes, Thomas P., Drago, Marco, Dreissigacker, Christoph, Driggers, Jenne C., Du, Zhihui, Ducrot, Marine, Dupej, Peter, Dwyer, Sheila E., Edo, Tega B., Edwards, Matthew C., Effler, Anamaria, Eggenstein, H.-B., Ehrens, Phil, Eichholz, Johannes, Eikenberry, Stephen S., Eisenstein, Robert A., Essick, Reed C., Estevez, Dimitri, Etienne, Zachariah B., Etzel, Todd, Evans, Matthew, Evans, Tom M., Factourovich, Maxim, Fafone, Viviana, Fair, Hannah, Fairhurst, Stephen, Fan, Xilong, Farinon, Stefania, Farr, Benjamin, Farr, Will M., Fauchon-Jones, E.J., Favata, Marc, Fays, Maxime, Fee, Campbell, Fehrmann, Henning, Feicht, Jon, Fejer, Martin M., Fernandez-Galiana, A., Ferrante, Isidoro, Ferreira, Elvis C., Ferrini, Federico, Fidecaro, Francesco, Finstad, Daniel, Fiori, Irene, Fiorucci, Donatella, Fishbach, Maya, Fisher, Ryan P., Fitz-Axen, M., Flaminio, Raffaele, Fletcher, Mark, Fong, Heather, Font, J.A., Forsyth, Perry W.F., Forsyth, Steven S., Fournier, J.-D., Frasca, Sergio, Frasconi, Franco, Frei, Zsolt, Freise, Andreas, Frey, Raymond, Frey, Valentin, Fries, Eric M., Fritschel, Peter, Frolov, Valery V., Fulda, Paul, Fyffe, Michael, Gabbard, Hunter, Gadre, Bhooshan U., Gaebel, Sebastian M., Gair, Jonathan R., Gammaitoni, Luca, Ganija, Miftar R., Gaonkar, Sharad G., Garcia-Quiros, C., Garufi, Fabio, Gateley, B., Gaudio, Sergio, Gaur, Gurudatt, Gayathri, V., Gehrels, Neil, Gemme, Gianluca, Genin, Eric, Gennai, Alberto, George, Daniel, George, Jogy, Gergely, Laszlo, Germain, Vincent, Ghonge, Sudarshan, Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Giaime, Joe A., Giardina, K.D., Giazotto, Adalberto, Gill, Kiranjyot, Glover, Lamar, Goetz, Evan, Goetz, Ryan, Gomes, Sandra, Goncharov, Boris, González, Gabriela, Gonzalez Castro, J.M., Gopakumar, A., Gorodetsky, Michael L., Gossan, Sarah E., GOSSELIN, Matthieu, Gouaty, Romain, Grado, Aniello, Graef, Christian, Granata, Massimo, Grant, Alastair, Gras, Slawomir, Gray, Corey, Greco, Giuseppe, Green, Anna C., Gretarsson, Elizabeth M., Groot, Paul, Grote, Hartmut, Grunewald, Steffen, Gruning, Pierre, Guidi, Gianluca M., Guo, Xiangyu, Gupta, Anuradha, Gupta, Manojipr K., Gushwa, Kaitlin E., Gustafson, Eric K., Gustafson, R., Halim, O., Hall, Bernard R., Hall, Evan D., Hamilton, Eleanor Z., Hammond, Giles, Haney, Maria, Hanke, Manuela M., Hanks, Jonathan, Hanna, Chad, Hannam, Mark D., Hannuksela, Otto A., Hanson, Joe, Hardwick, Terra, Harms, Jan, Harry, Gregg M., Harry, Ian W., Hart, Martin J., Haster, C.-J., Haughian, Karen, Healy, James, Heidmann, Antoine, Heintze, Matthew C., Heitmann, Henrich, Hello, Patrice, Hemming, Gary, Hendry, Martin, Heng, I.S., Hennig, J., Heptonstall, Alastair W., Heurs, Michele, Hild, Stefan, Hinderer, Tanja, Hoak, Daniel, Hofman, David, Holt, Kathy, Holz, Daniel E., Hopkins, Paul, Horst, Christian, Hough, James, Houston, Ewan A., Howell, Eric J., Hreibi, A., Hu, Yiming M., Huerta, Eliu A., Huet, Dominique, Hughey, Brennan, Husa, Sascha, Huttner, Sabina H., Huynh-Dinh, T., Indik, Nathaniel, Inta, Ra, Intini, Giuseppe, Isa, Hafizah N., Isac, J.-M., Isi, Max, Iyer, Bala R., Izumi, Kiwamu, Jacqmin, Thibaut, Jani, Karan, Jaranowski, Piotr, Jawahar, Sharat, Jiménez-Forteza, F., Johnson, Warren W., Jones, D.I., Jones, Russell, Jonker, Reinier J.G., Ju, L., Junker, Jonas, Kalaghatgi, Chinmay V., Kalogera, Vassiliki, Kamai, Brittany, Kandhasamy, Shivaraj, Kang, Gungwon, Kanner, Jonah B., Kapadia, Shasvath J., Karki, Sudarshan, Karvinen, Kai S., Kasprzack, Marie, Katolik, Michael, Katsavounidis, Erik, Katzman, William, Kaufer, Steffen, Kawabe, Keita, Kéfélian, Fabien, Keitel, David, Kemball, Athol J., Kennedy, Ross, Kent, Christopher, Key, Joey S., Khalili, Farit Y., Khan, I., Khan, Sebastian, Khan, Ziauddin, Khazanov, Efim A., Kijbunchoo, Nutsinee, Kim, Chunglee, Kim, Jeongcho C., Kim, Kyungmin, Kim, Won, Kim, Whansun S., Kim, Y.-M., Kimbrell, Seth J., King, Eleanor J., King, Peter J., Kinley-Hanlon, M., Kirchhoff, Robin, Kissel, Jeffrey S., Kleybolte, Lisa, Klimenko, Sergei, Knowles, Tyler D., Koch, Philip, Koehlenbeck, Sina M., Koley, Soumen, Kondrashov, Veronica, Kontos, Antonios, Korobko, Mikhail, Korth, William Z., Kowalska, Izabela, Kozak, Dan B., Krämer, Christina, Kringel, Volker, Krishnan, Badri, Królak, Andrzej, Kuehn, Gerrit, Kumar, Prayush, Kumar, Rakesh, Kumar, Sumit, Kuo, L., Kutynia, Adam, Kwang, Shawn, Lackey, Benjamin D., Lai, K.H., Landry, Michael, Lang, Ryan N., Lange, Jacob, Lantz, Brian, Lanza, Robert K., Lartaux-Vollard, A., Lasky, Paul D., Laxen, Michael, Lazzarini, Albert, Lazzaro, Claudia, Leaci, Paola, Leavey, Sean, Lee, C.H., Lee, Hyunkyu K., Lee, H.M., Lee, Hyungwon W., Lee, K., Lehmann, Johannes, Lenon, Amber, Leonardi, Matteo, Leroy, Nicolas, Letendre, Nicolas, Levin, Yuri, Li, Tjonnie G.F., Linker, Seth D., Littenberg, Tyson B., Liu, J., Lo, R.K.L., Lockerbie, Nick A., London, Lionel T., Lord, Jaysin E., Lorenzini, Matteo, Loriette, Vincent, Lormand, Marc, Losurdo, Giovanni, Lough, James D., Lovelace, Geoffrey, Lück, Harald, Lumaca, Diana, Lundgren, Andrew P., Lynch, Ryan, Ma, Y., Macas, Ronaldas, Macfoy, Sean, Machenschalk, Bernd, Macinnis, M., Macleod, Duncan M., Magaña Hernandez, I., Magaña-Sandoval, F., Magaña Zertuche, L., Magee, Ryan M., Majorana, Ettore, Maksimovic, Ivan, Man, N., Mandic, Vuk, Mangano, Valentina, Mansell, Georgia L., Manske, Michael, Mantovani, Maddalena, Marchesoni, Fabio, Marion, Frederique, Márka, Szabolcs, Márka, Zsuzsanna, Markakis, Charalampos, Markosyan, Ashot S., Markowitz, Aaron, Maros, E., Marquina, Antonio, Martelli, Filippo, Martellini, Lionel, Martin, Ian W., Martin, Rodica M., Martynov, Denis V., Mason, Ken, Massera, Elena, Masserot, Alain, Massinger, Thomas J., Masso-Reid, M., Mastrogiovanni, Simone, Matas, Andrew, Matichard, Fabrice, Matone, Luca, Mavalvala, Nergis, Mazumder, Nairwita, McCarthy, R., Mcclelland, D.E., Mccormick, S., McCuller, L., McGuire, S.C., Mcintyre, G., Mciver, J., McManus, David J., McNeill, L., McRae, T., McWilliams, S.T., Meacher, Duncan, Meadors, Grant D., Mehmet, Moritz, Meidam, Jeroen, Mejuto-Villa, E., Melatos, Andrew, Mendell, Gregory, Mercer, R.A., Merilh, Edmond L., Merzougui, Mourad, Meshkov, Syd, Messenger, Chris, Messick, Cody, Metzdorff, R., Meyers, Patrick M., Miao, Haixing, Michel, Christophe, Middleton, Hannah, Mikhailov, Eugeniy E., Milano, Leopoldo, Miller, Andrewlawrence L., Miller, Brandon B., Miller, John, Millhouse, Meg, Milovich-Goff, M.C., Minazzoli, Olivier, Minenkov, Yuri, Ming, Jing, Mishra, Chandra, Mitra, Sanjit, Mitrofanov, Valery P., Mitselmakher, Guenakh, Mittleman, Richard, Moffa, Donald, Moggi, Andrea, Mogushi, Kentaro, Mohan, Martin, Mohapatra, S.R.P., Montani, Matteo, Moore, Christopher J., Moraru, Dan, Moreno, Gerardo, Morriss, Sean R., Mours, Benoit, Mow-Lowry, C.M., Mueller, Guido, Muir, Alistair W., Mukherjee, Arunava, Mukherjee, Debnandini, Mukherjee, Soma, Mukund, Nikhil, Mullavey, Adam, Munch, Jesper, Muñiz, Erik A., Muratore, Martina, Murray, Peter G., Napier, Kate, Nardecchia, Ilaria, Naticchioni, Luca, Nayak, Rajesh K., Neilson, Joshua, Nelemans, Gijs, Nelson, Timothy J.N., Nery, Marina, Neunzert, Ansel, Nevin, Lydia, Newport, Jonathan M., Newton, Gavin, Ng, K.Y., Nguyen, Thanh T., Nichols, David, Nielsen, Alex B., Nissanke, Samaya, Nitz, Alex, Noack, Andreas, Nocera, Flavio, Nolting, David, North, Chris, Nuttall, Laura K., Oberling, Jason, O'Dea, G.D., Ogin, Greg H., Oh, John J., Oh, Sanghoon H., Ohme, Frank, Okada, Marcos A., Oliver, Miquel, Oppermann, Patrick, Oram, Richard J., O'Reilly, B., Ormiston, Rich, Ortega, Luis F., O'Shaughnessy, R., Ossokine, Serguei, Ottaway, David J., Overmier, Harry, Owen, Ben J., Pace, Alexander E., Page, Jessica, Page, Michael A., Pai, Archana, Pai, Siddhesh A., Palamos, Jordan R., Palashov, Oleg, Palomba, Cristiano, Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, Belinda, Pang, P.T.H., Pankow, Chris, Pannarale, Francesco, Pant, Brijesh C., Paoletti, Federico, PAOLI, Andrea, Papa, Maria A., Parida, Abhishek, Parker, William, Pascucci, Daniela, Pasqualetti, Antonio, Passaquieti, Roberto, Passuello, Diego, Patil, M., Patricelli, Barbara, Pearlstone, Brynley L., Pedraza, Mike, Pedurand, Richard, Pekowsky, L., Pele, Arnaud, Penn, Steven, Perez, Carlos J., Perreca, Antonio, Perri, Leah M., Pfeiffer, Harald P., Phelps, Margot, Piccinni, Ornella J., Pichot, Mikhael, Piergiovanni, Francesco, Pierro, Vincenzo, Pillant, Gabriel, Pinard, Laurent, Pinto, Innocenzo M., Pirello, Marc, Pisarski, A., Pitkin, Matthew, Poe, Mark, Poggiani, Rosa, Popolizio, Pasquale, Porter, K., Post, Alexander, Powell, Jade, Prasad, Jayanti, Pratt, James W.W., Pratten, Geraint, Predoi, Valeriu, Prestegard, Tanner, Prijatelj, Mirko, Principe, Maria, Privitera, Stephen, Prodi, Giovanni A., Prokhorov, Leonid G., Puncken, Oliver, Punturo, Michele, Puppo, Paola, Pürrer, Michael, Qi, Hong, Quetschke, Volker, Quintero, Eric A., Quitzow-James, R., Raab, Fred J., Rabeling, David S., Radkins, Hugh, Raffai, Peter, Raja, Sendhil, Rajan, C., Rajbhandari, Binod, Rakhmanov, Malik, Ramirez, Karla E., Ramos-Buades, A., Rapagnani, Piero, Raymond, Vivien, Razzano, Massimiliano, Read, Jocelyn, Regimbau, Tania, Rei, Luca, Reid, Stuart, Reitze, David H., Ren, Wei, Reyes, Steven D., Ricci, Fulvio, Ricker, Paul M., Rieger, Sascha, Riles, Keith, Rizzo, Monica, Robertson, Norna A., Robie, Raymond, Robinet, Florent, Rocchi, Alessio, ROLLAND, Loic, Rollins, Jameson G., Roma, Vincent J., Romano, Rocco, Romel, Chandra L., Romie, Janeen H., Rosińska, Dorota, Ross, Michael P., Rowan, Sheila, Rüdiger, Albrecht, Ruggi, Paolo, Rutins, Guntis, Ryan, Kyle, Sachdev, Surabhi, Sadecki, Travis, Sadeghian, Laleh, Sakellariadou, Mairi, Salconi, Livio, Saleem, Muhammed, Salemi, Francesco, Samajdar, Anuradha, Sammut, Letizia, Sampson, Laura M., Sanchez, Eduardo J., Sanchez, Luis E., Sanchis-Gual, N., Sandberg, Vernon, Sanders, Jaclyn R., Sassolas, Benoit, Saulson, Peter R., Sauter, Orion, Savage, Richard L., Sawadsky, Andreas, Schale, Paul, Scheel, Mark, Scheuer, Jacob, Schmidt, Justus, Schmidt, Patricia, Schnabel, Roman, Schofield, Robert M.S., Schönbeck, Axel, Schreiber, Emil, Schuette, Dirk, Schulte, Bernd W., Schutz, Bernard F., Schwalbe, Sophia G., Scott, Jamie, Scott, Susan M., Seidel, E., Sellers, Danny, Sengupta, Anand S., Sentenac, Daniel, Sequino, Valeria, Sergeev, Alexander, Shaddock, Daniel A., Shaffer, Thomas J., Shah, Ankur A., Shahriar, M.S., Shaner, Morgan B., Shao, Lijing, Shapiro, Brett, Shawhan, Peter, Sheperd, Alec, Shoemaker, David H., Shoemaker, Deirdre M., Siellez, Karelle, Siemens, Xavier, Sieniawska, Magdalena, Sigg, Daniel, Silva, Allan D., Singer, Leo P., Singh, Avneet, Singhal, Akshat, Sintes, Alicia M., Slagmolen, Bram J.J., Smith, Bryan, Smith, Joshua R., Smith, Rory J.E., Somala, Surendranadh, Son, Edwin J., Sonnenberg, Jacob A., Sorazu, Borja, Sorrentino, Fiodor, Souradeep, Tarun, Spencer, Andrew P., Srivastava, Amit K., Staats, Kai, Staley, Alexan, Steinke, Michael, Steinlechner, Jessica, Steinlechner, Sebastian, Steinmeyer, Daniel, Stevenson, Simon P., Stone, Robert, Stops, David J., Strain, Ken A., Stratta, Giulia, Strigin, Sergey E., Strunk, A., Sturani, Riccardo, Stuver, Amber L., Summerscales, Tiffany Z., Sun, Ling, Sunil, S., Suresh, Jishnu, Sutton, Patrick J., Swinkels, Bas L., Szczepańczyk, Marek J., Tacca, Matteo, Tait, Simon C., Talbot, Colm, Talukder, Dipongkar, Tanner, David B., Tao, Duo, Tápai, Marton, Taracchini, Andrea, Tasson, Jay D., Taylor, Jordan A., Taylor, Robert, Tewari, Shivam V., Theeg, Thomas, Thies, Fabian, Thomas, E.G., Thomas, Michael, Thomas, Patrick, Thorne, Keith A., Thrane, Eric, Tiwari, Shubhanshu, Tiwari, Vaibhav, Tokmakov, Kirill V., Toland, Karl, Tonelli, Mauro, Tornasi, Zeno, Torres-Forné, A., Torrie, Calum I., Töyrä, Daniel, Travasso, Flavio, Traylor, Gary, Trinastic, Jonathan, Tringali, Maria C., Trozzo, Lucia, Tsang, K.W., Tse, Maggie, Tso, Rhondale, Tsukada, Leo, Tsuna, Daichi, Tuyenbayev, Darkhan, Ueno, Koh, Ugolini, Dennis, Unnikrishnan, Cs S., Urban, Alexander L., Usman, Samantha A., Vahlbruch, Henning, Vajente, Gabriele, Valdes, Guillermo, Van Bakel, N., van Beuzekom, Martin, Van Den Brand, J.F.J., Van Den Broeck, C., Vander-Hyde, D.C., van der Schaaf, L., van Heijningen, J.V., van Veggel, A.A., Vardaro, Marco, Varma, Vijay, Vass, Steve, Vasúth, Matyas, Vecchio, Alberto, Vedovato, Gabriele, Veitch, John, Veitch, Peter J., Venkateswara, Krishna, Venugopalan, Gautam, Verkindt, Didier, Vetrano, Flavio, Viceré, Andrea, Viets, Aaron D., Vinciguerra, Serena, Vine, David J., Vinet, J.-Y., Vitale, Salvatore, Vo, Thomas, Vocca, Helios, Vorvick, Cheryl, Vyatchanin, Sergey P., Wade, Andrew R., Wade, Leslie E., Wade, Madeline, Walet, Rob, Walker, Marissa, Wallace, Larry, Walsh, Sinead, Wang, Gang, Wang, Haoyu, Wang, Jonathan Z., Wang, Wenhui H., Wang, Yifan F., Ward, Robert L., Warner, Jim, Was, Michal, Watchi, Jennifer, Weaver, Betsy, Wei, L.-W., Weinert, Michael, Weinstein, Alan J., Weiss, Rainer, Wen, Linqing, Wessel, Erik K., Weßels, Peter, Westerweck, Julian, Westphal, Tobias, Wette, Karl, Whelan, John T., Whiting, Bernard F., Whittle, Chris, Wilken, D., Williams, Daniel, Williams, Roy D., Williamson, Andrew R., Willis, Joshua L., Willke, Benno, Wimmer, Maximilian H., Winkler, Walter, Wipf, Christopher C., Wittel, Holger, Woan, Graham, Woehler, Janis, Wofford, Jared, Wong, W.K., Worden, John, Wright, Jennifer L., Wu, David S., Wysocki, Daniel M., Xiao, Sophia, Yamamoto, Hiro, Yancey, Cregg C., Yang, Le, Yap, M.J., Yazback, Maher, Yu, Hang, Yu, Haocun, Yvert, Michel, Zadrożny, Adam, Zanolin, Michele, Zelenova, Tatiana, Zendri, J.-P., Zevin, Michael, Zhang, Liyuan, Zhang, Mi, Zhang, Teng, Zhang, Y.-H., Zhao, Chunnong, Zhou, Minchuan, Zhou, Zifan, Zhu, Sylvia J., Zhu, Xingjiang J., Zucker, Michael E., and Zweizig, J.
Abstract: We report on a new all-sky search for periodic gravitational waves in the frequency band 475-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Potential signals could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the data from Advanced LIGO's first observational run O1. No gravitational-wave signals were observed, and upper limits were placed on their strengths. For completeness, results from the separately published low-frequency search 20-475 Hz are included as well. Our lowest upper limit on worst-case (linearly polarized) strain amplitude h0 is ∼4×10-25 near 170 Hz, while at the high end of our frequency range, we achieve a worst-case upper limit of 1.3×10-24. For a circularly polarized source (most favorable orientation), the smallest upper limit obtained is ∼1.5×10-25. © 2018 American Physical Society.
Published: 2018

9. Enhancing confidence in the detection of gravitational waves from compact binaries using signal coherence

Author: LIGO (Observatory : Massachusetts Institute of Technology), Vitale, Salvatore, Isi, Maximiliano, Smith, Rory, Massinger, T. J., Kanner, Jonah, Vajpeyi, Avi, LIGO (Observatory : Massachusetts Institute of Technology), Vitale, Salvatore, Isi, Maximiliano, Smith, Rory, Massinger, T. J., Kanner, Jonah, and Vajpeyi, Avi
Abstract: We show that gravitational-wave signals from compact binary mergers may be better distinguished from instrumental noise transients by using Bayesian models that look for signal coherence across a detector network. This can be achieved even when the signal power is below the usual threshold for detection. This method could reject the vast majority of noise transients, and therefore increase sensitivity to weak gravitational waves. We demonstrate this using simulated signals, as well as data for GW150914 and LVT151012. Finally, we explore ways of incorporating our method into existing Advanced LIGO and Virgo searches to make them significantly more powerful., National Science Foundation (U.S.) (Grant PHY-0757058)
Published: 2018

10. Gravitational-Wave Geodesy: A New Tool for Validating Detection of the Stochastic Gravitational-Wave Background

Author: Callister, Thomas, Coughlin, Michael, Kanner, Jonah, Callister, Thomas, Coughlin, Michael, and Kanner, Jonah
Abstract: A valuable target for advanced gravitational-wave detectors is the stochastic gravitational-wave background. The stochastic background imparts a weak correlated signal into networks of gravitational-wave detectors, and so standard searches for the gravitational-wave background rely on measuring cross-correlations between pairs of widely-separated detectors. Stochastic searches, however, can be affected by any other correlated effects which may also be present, including correlated frequency combs and magnetic Schumann resonances. As stochastic searches become sensitive to ever-weaker signals, it is increasingly important to develop methods to separate a true astrophysical signal from other spurious and/or terrestrial signals. Here, we describe a novel method to achieve this goal -- gravitational-wave geodesy. Just as radio geodesy allows for the localization of radio telescopes, so too can observations of the gravitational-wave background be used to infer the positions and orientations of gravitational-wave detectors. By demanding that a true observation of the gravitational-wave background yield constraints consistent with the baseline's known geometry, we demonstrate that we can successfully validate true observations of the gravitational-wave background while rejecting spurious signals due to correlated terrestrial effects., Comment: Minor typos corrected
Published: 2018
Full Text: View/download PDF

11. Enhancing confidence in the detection of gravitational waves from compact binaries using signal coherence

Author: Isi, Maximiliano, Smith, Rory, Vitale, Salvatore, Massinger, T. J., Kanner, Jonah, Vajpeyi, Avi, Isi, Maximiliano, Smith, Rory, Vitale, Salvatore, Massinger, T. J., Kanner, Jonah, and Vajpeyi, Avi
Abstract: We show that gravitational-wave signals from compact binary mergers may be better distinguished from instrumental noise transients by using Bayesian models that look for signal coherence across a detector network. This can be achieved even when the signal power is below the usual threshold for detection. This method could reject the vast majority of noise transients, and therefore increase sensitivity to weak gravitational waves. We demonstrate this using simulated signals, as well as data for GW150914 and LVT151012. Finally, we explore ways of incorporating our method into existing Advanced LIGO and Virgo searches to make them significantly more powerful.
Published: 2018
Full Text: View/download PDF

12. Mitigation of the instrumental noise transient in gravitational-wave data surrounding GW170817

Author: Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), Evans, Matthew J, Pankow, Chris, Chatziioannou, Katerina, Chase, Eve A., Littenberg, Tyson B., McIver, Jessica, Cornish, Neil J., Haster, Carl-Johan, Kanner, Jonah, Raymond, Vivien, Vitale, Salvatore, Zimmerman, Aaron, Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), Evans, Matthew J, Pankow, Chris, Chatziioannou, Katerina, Chase, Eve A., Littenberg, Tyson B., McIver, Jessica, Cornish, Neil J., Haster, Carl-Johan, Kanner, Jonah, Raymond, Vivien, Vitale, Salvatore, and Zimmerman, Aaron
Abstract: In the coming years gravitational-wave detectors will undergo a series of improvements, with an increase in their detection rate by about an order of magnitude. Routine detections of gravitational-wave signals promote novel astrophysical and fundamental theory studies, while simultaneously leading to an increase in the number of detections temporally overlapping with instrumentally- or environmentally-induced transients in the detectors (glitches), often of unknown origin. Indeed, this was the case for the very first detection by the LIGO and Virgo detectors of a gravitational-wave signal consistent with a binary neutron star coalescence, GW170817. A loud glitch in the LIGO-Livingston detector, about one second before the merger, hampered coincident detection (which was initially achieved solely with LIGO-Hanford data). Moreover, accurate source characterization depends on specific assumptions about the behavior of the detector noise that are rendered invalid by the presence of glitches. In this paper, we present the various techniques employed for the initial mitigation of the glitch to perform source characterization of GW170817 and study advantages and disadvantages of each mitigation method. We show that, despite the presence of instrumental noise transients louder than the one affecting GW170817, we are still able to produce unbiased measurements of the intrinsic parameters from simulated injections with properties similar to GW170817., National Science Foundation (U.S.), Laser Interferometer Gravitational Wave Observatory
Published: 2018

13. Parameter Estimation for Gravitational-wave Bursts with the BayesWave Pipeline

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Essick, Reed Clasey, Katsavounidis, Erotokritos, Vitale, Salvatore, Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Kanner, Jonah, Littenberg, Tyson B., Millhouse, Margaret, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Essick, Reed Clasey, Katsavounidis, Erotokritos, Vitale, Salvatore, Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Kanner, Jonah, Littenberg, Tyson B., and Millhouse, Margaret
Abstract: We provide a comprehensive multi-aspect study of the performance of a pipeline used by the LIGO-Virgo Collaboration for estimating parameters of gravitational-wave bursts. We add simulated signals with four different morphologies (sine-Gaussians (SGs), Gaussians, white-noise bursts, and binary black hole signals) to simulated noise samples representing noise of the two Advanced LIGO detectors during their first observing run. We recover them with the BayesWave (BW) pipeline to study its accuracy in sky localization, waveform reconstruction, and estimation of model-independent waveform parameters. BW localizes sources with a level of accuracy comparable for all four morphologies, with the median separation of actual and estimated sky locations ranging from 25.°1 to 30.°3. This is a reasonable accuracy in the two-detector case, and is comparable to accuracies of other localization methods studied previously. As BW reconstructs generic transient signals with SG wavelets, it is unsurprising that BW performs best in reconstructing SG and Gaussian waveforms. The BW accuracy in waveform reconstruction increases steeply with the network signal-to-noise ratio (S/N), reaching a 85% and 95% match between the reconstructed and actual waveform below S/N and S/N, respectively, for all morphologies. The BW accuracy in estimating central moments of waveforms is only limited by statistical errors in the frequency domain, and is also affected by systematic errors in the time domain as BW cannot reconstruct low-amplitude parts of signals that are overwhelmed by noise. The figures of merit we introduce can be used in future characterizations of parameter estimation pipelines.
Published: 2017

14. Parameter estimation for gravitational-wave bursts with the BayesWave pipeline

Author: Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Essick, Reed, Kanner, Jonah, Katsavounidis, Erik, Littenberg, Tyson B., Millhouse, Margaret, Vitale, Salvatore, Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Essick, Reed, Kanner, Jonah, Katsavounidis, Erik, Littenberg, Tyson B., Millhouse, Margaret, and Vitale, Salvatore
Abstract: We provide a comprehensive multi-aspect study on the performance of a pipeline used by the LIGO-Virgo Collaboration for estimating parameters of gravitational-wave bursts. We add simulated signals with four different morphologies (sine-Gaussians, Gaussians, white-noise bursts, and binary black hole signals) to simulated noise samples representing noise of the two Advanced LIGO detectors during their first observing run. We recover them with the BayesWave (BW) pipeline to study its accuracy in sky localization, waveform reconstruction, and estimation of model-independent waveform parameters. BW localizes sources with a level of accuracy comparable for all four morphologies, with the median separation of actual and estimated sky locations ranging from 25.1$^{\circ}$ to 30.3$^{\circ}$. This is a reasonable accuracy in the two-detector case, and is comparable to accuracies of other localization methods studied previously. As BW reconstructs generic transient signals with sine-Gaussian wavelets, it is unsurprising that BW performs the best in reconstructing sine-Gaussian and Gaussian waveforms. BW's accuracy in waveform reconstruction increases steeply with network signal-to-noise ratio (SNR$_{\rm net}$), reaching a $85\%$ and $95\%$ match between the reconstructed and actual waveform below SNR$_{\rm net} \approx 20$ and SNR$_{\rm net} \approx 50$, respectively, for all morphologies. BW's accuracy in estimating central moments of waveforms is only limited by statistical errors in the frequency domain, and is affected by systematic errors too in the time domain as BW cannot reconstruct low-amplitude parts of signals overwhelmed by noise. The figures of merit we introduce can be used in future characterizations of parameter estimation pipelines., Comment: 14 pages, 9 figures
Published: 2016
Full Text: View/download PDF

15. Gravitational-Wave Constraints on the Progenitors of Fast Radio Bursts

Author: Callister, Thomas, Kanner, Jonah, Weinstein, Alan, Callister, Thomas, Kanner, Jonah, and Weinstein, Alan
Abstract: The nature of fast radio bursts (FRBs) remains enigmatic. Highly energetic radio pulses of millisecond duration, FRBs are observed with dispersion measures consistent with an extragalactic source. A variety of models have been proposed to explain their origin. One popular class of theorized FRB progenitor is the coalescence of compact binaries composed of neutron stars and/or black holes. Such coalescence events are strong gravitational-wave emitters. We demonstrate that measurements made by the LIGO and Virgo gravitational-wave observatories can be leveraged to severely constrain the validity of FRB binary coalescence models. Existing measurements constrain the binary black hole rate to approximately $5\%$ of the FRB rate, and results from Advanced LIGO's O1 and O2 observing runs may place similarly strong constraints on the fraction of FRBs due to binary neutron star and neutron star--black hole progenitors., Comment: 5 pages, 2 figures, published in ApJL. Additional minor updates to match published version, updating metadata
Published: 2016
Full Text: View/download PDF

16. Parameter estimation for gravitational-wave bursts with the BayesWave pipeline

Author: Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Essick, Reed, Kanner, Jonah, Katsavounidis, Erik, Littenberg, Tyson B., Millhouse, Margaret, Vitale, Salvatore, Bécsy, Bence, Raffai, Peter, Cornish, Neil J., Essick, Reed, Kanner, Jonah, Katsavounidis, Erik, Littenberg, Tyson B., Millhouse, Margaret, and Vitale, Salvatore
Abstract: We provide a comprehensive multi-aspect study on the performance of a pipeline used by the LIGO-Virgo Collaboration for estimating parameters of gravitational-wave bursts. We add simulated signals with four different morphologies (sine-Gaussians, Gaussians, white-noise bursts, and binary black hole signals) to simulated noise samples representing noise of the two Advanced LIGO detectors during their first observing run. We recover them with the BayesWave (BW) pipeline to study its accuracy in sky localization, waveform reconstruction, and estimation of model-independent waveform parameters. BW localizes sources with a level of accuracy comparable for all four morphologies, with the median separation of actual and estimated sky locations ranging from 25.1$^{\circ}$ to 30.3$^{\circ}$. This is a reasonable accuracy in the two-detector case, and is comparable to accuracies of other localization methods studied previously. As BW reconstructs generic transient signals with sine-Gaussian wavelets, it is unsurprising that BW performs the best in reconstructing sine-Gaussian and Gaussian waveforms. BW's accuracy in waveform reconstruction increases steeply with network signal-to-noise ratio (SNR$_{\rm net}$), reaching a $85\%$ and $95\%$ match between the reconstructed and actual waveform below SNR$_{\rm net} \approx 20$ and SNR$_{\rm net} \approx 50$, respectively, for all morphologies. BW's accuracy in estimating central moments of waveforms is only limited by statistical errors in the frequency domain, and is affected by systematic errors too in the time domain as BW cannot reconstruct low-amplitude parts of signals overwhelmed by noise. The figures of merit we introduce can be used in future characterizations of parameter estimation pipelines., Comment: 14 pages, 9 figures
Published: 2016
Full Text: View/download PDF

17. Gravitational-Wave Constraints on the Progenitors of Fast Radio Bursts

Author: Callister, Thomas, Kanner, Jonah, Weinstein, Alan, Callister, Thomas, Kanner, Jonah, and Weinstein, Alan
Abstract: The nature of fast radio bursts (FRBs) remains enigmatic. Highly energetic radio pulses of millisecond duration, FRBs are observed with dispersion measures consistent with an extragalactic source. A variety of models have been proposed to explain their origin. One popular class of theorized FRB progenitor is the coalescence of compact binaries composed of neutron stars and/or black holes. Such coalescence events are strong gravitational-wave emitters. We demonstrate that measurements made by the LIGO and Virgo gravitational-wave observatories can be leveraged to severely constrain the validity of FRB binary coalescence models. Existing measurements constrain the binary black hole rate to approximately $5\%$ of the FRB rate, and results from Advanced LIGO's O1 and O2 observing runs may place similarly strong constraints on the fraction of FRBs due to binary neutron star and neutron star--black hole progenitors., Comment: 5 pages, 2 figures, published in ApJL. Additional minor updates to match published version, updating metadata
Published: 2016
Full Text: View/download PDF

18. Enabling high confidence detections of gravitational-wave bursts

Author: Littenberg, Tyson B., Kanner, Jonah B., Cornish, Neil J., Millhouse, Margaret, Littenberg, Tyson B., Kanner, Jonah B., Cornish, Neil J., and Millhouse, Margaret
Abstract: With the advanced LIGO and Virgo detectors taking observations the detection of gravitational waves is expected within the next few years. Extracting astrophysical information from gravitational wave detections is a well-posed problem and thoroughly studied when detailed models for the waveforms are available. However, one motivation for the field of gravitational wave astronomy is the potential for new discoveries. Recognizing and characterizing unanticipated signals requires data analysis techniques which do not depend on theoretical predictions for the gravitational waveform. Past searches for short-duration un-modeled gravitational wave signals have been hampered by transient noise artifacts, or "glitches," in the detectors. In some cases, even high signal-to-noise simulated astrophysical signals have proven difficult to distinguish from glitches, so that essentially any plausible signal could be detected with at most 2-3 $\sigma$ level confidence. We have put forth the BayesWave algorithm to differentiate between generic gravitational wave transients and glitches, and to provide robust waveform reconstruction and characterization of the astrophysical signals. Here we study BayesWave's capabilities for rejecting glitches while assigning high confidence to detection candidates through analytic approximations to the Bayesian evidence. Analytic results are tested with numerical experiments by adding simulated gravitational wave transient signals to LIGO data collected between 2009 and 2010 and found to be in good agreement., Comment: 15 pages, 6 figures, submitted to PRD
Published: 2015
Full Text: View/download PDF

19. Multi-messenger astronomy of gravitational-wave sources with flexible wide-area radio transient surveys

Author: Yancey, Cregg C., Bear, Brandon E., Akukwe, Bernadine, Chen, Kevin, Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kavic, Michael, Obenberger, Kenneth, Shawhan, Peter, Simonetti, John H., Taylor, Gregory B., Tsai, Jr-Wei, Yancey, Cregg C., Bear, Brandon E., Akukwe, Bernadine, Chen, Kevin, Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kavic, Michael, Obenberger, Kenneth, Shawhan, Peter, Simonetti, John H., Taylor, Gregory B., and Tsai, Jr-Wei
Abstract: We explore opportunities for multi-messenger astronomy using gravitational waves (GWs) and prompt, transient low-frequency radio emission to study highly energetic astrophysical events. We review the literature on possible sources of correlated emission of gravitational waves and radio transients, highlighting proposed mechanisms that lead to a short-duration, high-flux radio pulse originating from the merger of two neutron stars or from a superconducting cosmic string cusp. We discuss the detection prospects for each of these mechanisms by low-frequency dipole array instruments such as LWA1, LOFAR and MWA. We find that a broad range of models may be tested by searching for radio pulses that, when de-dispersed, are temporally and spatially coincident with a LIGO/Virgo GW trigger within a $\usim 30$ second time window and $\usim 200 \mendash 500 \punits{deg}^{2}$ sky region. We consider various possible observing strategies and discuss their advantages and disadvantages. Uniquely, for low-frequency radio arrays, dispersion can delay the radio pulse until after low-latency GW data analysis has identified and reported an event candidate, enabling a \emph{prompt} radio signal to be captured by a deliberately targeted beam. If neutron star mergers do have detectable prompt radio emissions, a coincident search with the GW detector network and low-frequency radio arrays could increase the LIGO/Virgo effective search volume by up to a factor of $\usim 2$. For some models, we also map the parameter space that may be constrained by non-detections., Comment: 31 pages, 4 figures
Published: 2015
Full Text: View/download PDF

20. Leveraging waveform complexity for confident detection of gravitational waves

Author: Kanner, Jonah B., Littenberg, Tyson B., Cornish, Neil, Millhouse, Meg, Xhakaj, Enia, Salemi, Francesco, Drago, Marco, Vedovato, Gabriele, Klimenko, Sergey, Kanner, Jonah B., Littenberg, Tyson B., Cornish, Neil, Millhouse, Meg, Xhakaj, Enia, Salemi, Francesco, Drago, Marco, Vedovato, Gabriele, and Klimenko, Sergey
Abstract: The recent completion of Advanced LIGO suggests that gravitational waves (GWs) may soon be directly observed. Past searches for gravitational-wave transients have been impacted by transient noise artifacts, known as glitches, introduced into LIGO data due to instrumental and environmental effects. In this work, we explore how waveform complexity, instead of signal-to-noise ratio, can be used to rank event candidates and distinguish short duration astrophysical signals from glitches. We test this framework using a new hierarchical pipeline that directly compares the Bayesian evidence of explicit signal and glitch models. The hierarchical pipeline is shown to have strong performance, and in particular, allows high-confidence detections of a range of waveforms at realistic signal-to-noise ratio with a two detector network., Comment: 9 pages, 11 figures. This draft was accepted by PRD
Published: 2015
Full Text: View/download PDF

21. Galaxy Strategy for LIGO-Virgo Gravitational Wave Counterpart Searches

Author: Gehrels, Neil, Cannizzo, John K., Kanner, Jonah, Kasliwal, Mansi M., Nissanke, Samaya, Singer, Leo P., Gehrels, Neil, Cannizzo, John K., Kanner, Jonah, Kasliwal, Mansi M., Nissanke, Samaya, and Singer, Leo P.
Abstract: In this work we continue a line of inquiry begun in Kanner et al. which detailed a strategy for utilizing telescopes with narrow fields of view, such as the Swift X-ray Telescope (XRT), to localize gravity wave (GW) triggers from LIGO/Virgo. If one considers the brightest galaxies that produce ~50% of the light, then the number of galaxies inside typical GW error boxes will be several tens. We have found that this result applies both in the early years of Advanced LIGO when the range is small and the error boxes large, and in the later years when the error boxes will be small and the range large. This strategy has the beneficial property of reducing the number of telescope pointings by a factor 10 to 100 compared with tiling the entire error box. Additional galaxy count reduction will come from a GW rapid distance estimate which will restrict the radial slice in search volume. Combining the bright galaxy strategy with a convolution based on anticipated GW localizations, we find that the searches can be restricted to about 18+/-5 galaxies for 2015, about 23+/-4 for 2017, and about 11+/-2 for 2020. This assumes a distance localization at or near the putative NS-NS merger range for each target year, and these totals are integrated out to the range. Integrating out to the horizon would roughly double the totals. For nearer localizations the totals would decrease. The galaxy strategy we present in this work will enable numerous sensitive optical and X-ray telescopes with small fields of view to participate meaningfully in searches wherein the prospects for rapidly fading afterglow place a premium on a fast response time., Comment: 8 pages, 4 figures, The Astrophysical Journal, submitted
Published: 2015
Full Text: View/download PDF

22. Observations of Giant Pulses from Pulsar PSR B0950+08 using LWA1

Author: Tsai, Jr-Wei, Simonetti, John H., Akukwe, Bernadine, Bear, Brandon, Cutchin, Sean E., Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kassim, Namir E., Schinzel, Frank K., Shawhan, Peter, Taylor, Gregory B., Yancey, Cregg C., Quezada, Leandro, Kavic, Michael, Tsai, Jr-Wei, Simonetti, John H., Akukwe, Bernadine, Bear, Brandon, Cutchin, Sean E., Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kassim, Namir E., Schinzel, Frank K., Shawhan, Peter, Taylor, Gregory B., Yancey, Cregg C., Quezada, Leandro, and Kavic, Michael
Abstract: We report the detection of giant pulse emission from PSR B0950+08 in 24 hours of observations made at 39.4 MHz, with a bandwidth of 16 MHz, using the first station of the Long Wavelength Array, LWA1. We detected 119 giant pulses from PSR B0950+08 (at its dispersion measure), which we define as having SNRs at least 10 times larger than for the mean pulse in our data set. These 119 pulses are 0.035% of the total number of pulse periods in the 24 hours of observations. The rate of giant pulses is about 5.0 per hour. The cumulative distribution of pulse strength $S$ is a steep power law, $N(>S)\propto S^{-4.7}$, but much less steep than would be expected if we were observing the tail of a Gaussian distribution of normal pulses. We detected no other transient pulses in a dispersion measure range from 1 to 90 pc cm$^{-3}$, in the beam tracking PSR B0950+08. The giant pulses have a narrower temporal width than the mean pulse (17.8 ms, on average, vs. 30.5 ms). The pulse widths are consistent with a previously observed weak dependence on observing frequency, which may be indicative of a deviation from a Kolmogorov spectrum of electron density irregularities along the line of sight. The rate and strength of these giant pulses is less than has been observed at $\sim$100 MHz. Additionally, the mean (normal) pulse flux density we observed is less than at $\sim$100 MHz. These results suggest this pulsar is weaker and produces less frequent giant pulses at 39 MHz than at 100 MHz., Comment: 27 pages, 12 figures, typos corrected
Published: 2015
Full Text: View/download PDF

23. Enabling high confidence detections of gravitational-wave bursts

Author: Littenberg, Tyson B., Kanner, Jonah B., Cornish, Neil J., Millhouse, Margaret, Littenberg, Tyson B., Kanner, Jonah B., Cornish, Neil J., and Millhouse, Margaret
Abstract: With the advanced LIGO and Virgo detectors taking observations the detection of gravitational waves is expected within the next few years. Extracting astrophysical information from gravitational wave detections is a well-posed problem and thoroughly studied when detailed models for the waveforms are available. However, one motivation for the field of gravitational wave astronomy is the potential for new discoveries. Recognizing and characterizing unanticipated signals requires data analysis techniques which do not depend on theoretical predictions for the gravitational waveform. Past searches for short-duration un-modeled gravitational wave signals have been hampered by transient noise artifacts, or "glitches," in the detectors. In some cases, even high signal-to-noise simulated astrophysical signals have proven difficult to distinguish from glitches, so that essentially any plausible signal could be detected with at most 2-3 $\sigma$ level confidence. We have put forth the BayesWave algorithm to differentiate between generic gravitational wave transients and glitches, and to provide robust waveform reconstruction and characterization of the astrophysical signals. Here we study BayesWave's capabilities for rejecting glitches while assigning high confidence to detection candidates through analytic approximations to the Bayesian evidence. Analytic results are tested with numerical experiments by adding simulated gravitational wave transient signals to LIGO data collected between 2009 and 2010 and found to be in good agreement., Comment: 15 pages, 6 figures, submitted to PRD
Published: 2015
Full Text: View/download PDF

24. Multi-messenger astronomy of gravitational-wave sources with flexible wide-area radio transient surveys

Author: Yancey, Cregg C., Bear, Brandon E., Akukwe, Bernadine, Chen, Kevin, Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kavic, Michael, Obenberger, Kenneth, Shawhan, Peter, Simonetti, John H., Taylor, Gregory B., Tsai, Jr-Wei, Yancey, Cregg C., Bear, Brandon E., Akukwe, Bernadine, Chen, Kevin, Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kavic, Michael, Obenberger, Kenneth, Shawhan, Peter, Simonetti, John H., Taylor, Gregory B., and Tsai, Jr-Wei
Abstract: We explore opportunities for multi-messenger astronomy using gravitational waves (GWs) and prompt, transient low-frequency radio emission to study highly energetic astrophysical events. We review the literature on possible sources of correlated emission of gravitational waves and radio transients, highlighting proposed mechanisms that lead to a short-duration, high-flux radio pulse originating from the merger of two neutron stars or from a superconducting cosmic string cusp. We discuss the detection prospects for each of these mechanisms by low-frequency dipole array instruments such as LWA1, LOFAR and MWA. We find that a broad range of models may be tested by searching for radio pulses that, when de-dispersed, are temporally and spatially coincident with a LIGO/Virgo GW trigger within a $\usim 30$ second time window and $\usim 200 \mendash 500 \punits{deg}^{2}$ sky region. We consider various possible observing strategies and discuss their advantages and disadvantages. Uniquely, for low-frequency radio arrays, dispersion can delay the radio pulse until after low-latency GW data analysis has identified and reported an event candidate, enabling a \emph{prompt} radio signal to be captured by a deliberately targeted beam. If neutron star mergers do have detectable prompt radio emissions, a coincident search with the GW detector network and low-frequency radio arrays could increase the LIGO/Virgo effective search volume by up to a factor of $\usim 2$. For some models, we also map the parameter space that may be constrained by non-detections., Comment: 31 pages, 4 figures
Published: 2015
Full Text: View/download PDF

25. Leveraging waveform complexity for confident detection of gravitational waves

Author: Kanner, Jonah B., Littenberg, Tyson B., Cornish, Neil, Millhouse, Meg, Xhakaj, Enia, Salemi, Francesco, Drago, Marco, Vedovato, Gabriele, Klimenko, Sergey, Kanner, Jonah B., Littenberg, Tyson B., Cornish, Neil, Millhouse, Meg, Xhakaj, Enia, Salemi, Francesco, Drago, Marco, Vedovato, Gabriele, and Klimenko, Sergey
Abstract: The recent completion of Advanced LIGO suggests that gravitational waves (GWs) may soon be directly observed. Past searches for gravitational-wave transients have been impacted by transient noise artifacts, known as glitches, introduced into LIGO data due to instrumental and environmental effects. In this work, we explore how waveform complexity, instead of signal-to-noise ratio, can be used to rank event candidates and distinguish short duration astrophysical signals from glitches. We test this framework using a new hierarchical pipeline that directly compares the Bayesian evidence of explicit signal and glitch models. The hierarchical pipeline is shown to have strong performance, and in particular, allows high-confidence detections of a range of waveforms at realistic signal-to-noise ratio with a two detector network., Comment: 9 pages, 11 figures. This draft was accepted by PRD
Published: 2015
Full Text: View/download PDF

26. Galaxy Strategy for LIGO-Virgo Gravitational Wave Counterpart Searches

Author: Gehrels, Neil, Cannizzo, John K., Kanner, Jonah, Kasliwal, Mansi M., Nissanke, Samaya, Singer, Leo P., Gehrels, Neil, Cannizzo, John K., Kanner, Jonah, Kasliwal, Mansi M., Nissanke, Samaya, and Singer, Leo P.
Abstract: In this work we continue a line of inquiry begun in Kanner et al. which detailed a strategy for utilizing telescopes with narrow fields of view, such as the Swift X-ray Telescope (XRT), to localize gravity wave (GW) triggers from LIGO/Virgo. If one considers the brightest galaxies that produce ~50% of the light, then the number of galaxies inside typical GW error boxes will be several tens. We have found that this result applies both in the early years of Advanced LIGO when the range is small and the error boxes large, and in the later years when the error boxes will be small and the range large. This strategy has the beneficial property of reducing the number of telescope pointings by a factor 10 to 100 compared with tiling the entire error box. Additional galaxy count reduction will come from a GW rapid distance estimate which will restrict the radial slice in search volume. Combining the bright galaxy strategy with a convolution based on anticipated GW localizations, we find that the searches can be restricted to about 18+/-5 galaxies for 2015, about 23+/-4 for 2017, and about 11+/-2 for 2020. This assumes a distance localization at or near the putative NS-NS merger range for each target year, and these totals are integrated out to the range. Integrating out to the horizon would roughly double the totals. For nearer localizations the totals would decrease. The galaxy strategy we present in this work will enable numerous sensitive optical and X-ray telescopes with small fields of view to participate meaningfully in searches wherein the prospects for rapidly fading afterglow place a premium on a fast response time., Comment: 8 pages, 4 figures, The Astrophysical Journal, submitted
Published: 2015
Full Text: View/download PDF

27. Observations of Giant Pulses from Pulsar PSR B0950+08 using LWA1

Author: Tsai, Jr-Wei, Simonetti, John H., Akukwe, Bernadine, Bear, Brandon, Cutchin, Sean E., Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kassim, Namir E., Schinzel, Frank K., Shawhan, Peter, Taylor, Gregory B., Yancey, Cregg C., Quezada, Leandro, Kavic, Michael, Tsai, Jr-Wei, Simonetti, John H., Akukwe, Bernadine, Bear, Brandon, Cutchin, Sean E., Dowell, Jayce, Gough, Jonathan D., Kanner, Jonah, Kassim, Namir E., Schinzel, Frank K., Shawhan, Peter, Taylor, Gregory B., Yancey, Cregg C., Quezada, Leandro, and Kavic, Michael
Abstract: We report the detection of giant pulse emission from PSR B0950+08 in 24 hours of observations made at 39.4 MHz, with a bandwidth of 16 MHz, using the first station of the Long Wavelength Array, LWA1. We detected 119 giant pulses from PSR B0950+08 (at its dispersion measure), which we define as having SNRs at least 10 times larger than for the mean pulse in our data set. These 119 pulses are 0.035% of the total number of pulse periods in the 24 hours of observations. The rate of giant pulses is about 5.0 per hour. The cumulative distribution of pulse strength $S$ is a steep power law, $N(>S)\propto S^{-4.7}$, but much less steep than would be expected if we were observing the tail of a Gaussian distribution of normal pulses. We detected no other transient pulses in a dispersion measure range from 1 to 90 pc cm$^{-3}$, in the beam tracking PSR B0950+08. The giant pulses have a narrower temporal width than the mean pulse (17.8 ms, on average, vs. 30.5 ms). The pulse widths are consistent with a previously observed weak dependence on observing frequency, which may be indicative of a deviation from a Kolmogorov spectrum of electron density irregularities along the line of sight. The rate and strength of these giant pulses is less than has been observed at $\sim$100 MHz. Additionally, the mean (normal) pulse flux density we observed is less than at $\sim$100 MHz. These results suggest this pulsar is weaker and produces less frequent giant pulses at 39 MHz than at 100 MHz., Comment: 27 pages, 12 figures, typos corrected
Published: 2015
Full Text: View/download PDF

28. The LIGO Open Science Center

Author: Vallisneri, Michele, Kanner, Jonah, Williams, Roy, Weinstein, Alan, Stephens, Branson, Vallisneri, Michele, Kanner, Jonah, Williams, Roy, Weinstein, Alan, and Stephens, Branson
Abstract: The LIGO Open Science Center (LOSC) fulfills LIGO's commitment to release, archive, and serve LIGO data in a broadly accessible way to the scientific community and to the public, and to provide the information and tools necessary to understand and use the data. In August 2014, the LOSC published the full dataset from Initial LIGO's "S5" run at design sensitivity, the first such large-scale release and a valuable testbed to explore the use of LIGO data by non-LIGO researchers and by the public, and to help teach gravitational-wave data analysis to students across the world. In addition to serving the S5 data, the LOSC web portal (losc.ligo.org) now offers documentation, data-location and data-quality queries, tutorials and example code, and more. We review the mission and plans of the LOSC, focusing on the S5 data release., Comment: 8 pages, 1 figure, proceedings of the 10th LISA Symposium, University of Florida, Gainesville, May 18-23, 2014; final published version; see losc.ligo.org for the S5 data release and more information about the LIGO Open Science Center
Published: 2014
Full Text: View/download PDF

29. The LIGO Open Science Center

Author: Vallisneri, Michele, Kanner, Jonah, Williams, Roy, Weinstein, Alan, Stephens, Branson, Vallisneri, Michele, Kanner, Jonah, Williams, Roy, Weinstein, Alan, and Stephens, Branson
Abstract: The LIGO Open Science Center (LOSC) fulfills LIGO's commitment to release, archive, and serve LIGO data in a broadly accessible way to the scientific community and to the public, and to provide the information and tools necessary to understand and use the data. In August 2014, the LOSC published the full dataset from Initial LIGO's "S5" run at design sensitivity, the first such large-scale release and a valuable testbed to explore the use of LIGO data by non-LIGO researchers and by the public, and to help teach gravitational-wave data analysis to students across the world. In addition to serving the S5 data, the LOSC web portal (losc.ligo.org) now offers documentation, data-location and data-quality queries, tutorials and example code, and more. We review the mission and plans of the LOSC, focusing on the S5 data release., Comment: 8 pages, 1 figure, proceedings of the 10th LISA Symposium, University of Florida, Gainesville, May 18-23, 2014; final published version; see losc.ligo.org for the S5 data release and more information about the LIGO Open Science Center
Published: 2014
Full Text: View/download PDF

30. X-ray Transients in the Advanced LIGO/Virgo Horizon

Author: Kanner, Jonah, Baker, John, Blackburn, Lindy, Camp, Jordan, Mooley, Kunal, Mushotzky, Richard, Ptak, Andy, Kanner, Jonah, Baker, John, Blackburn, Lindy, Camp, Jordan, Mooley, Kunal, Mushotzky, Richard, and Ptak, Andy
Abstract: Advanced LIGO and Advanced Virgo will be all-sky monitors for merging compact objects within a few hundred Mpc. Finding the electromagnetic counterparts to these events will require an understanding of the transient sky at low red-shift (z<0.1). We performed a systematic search for extragalactic, low red-shift, transient events in the XMM-Newton Slew Survey. In a flux limited sample, we found that highly-variable objects comprised 10% of the sample, and that of these, 10% were spatially coincident with cataloged optical galaxies. This led to 4x10^-4 transients per square degree above a flux threshold of 3x10^-12 erg cm-2 s-1 [0.2-2 keV] which might be confused with LIGO/Virgo counterparts. This represents the first extragalactic measurement of the soft X-ray transient rate within the Advanced LIGO/Virgo horizon. Our search revealed six objects that were spatially coincident with previously cataloged galaxies, lacked evidence for optical AGNs, displayed high luminosities around 10^43 erg s-1, and varied in flux by more than a factor of ten when compared with the ROSAT All-Sky Survey. At least four of these displayed properties consistent with previously observed tidal disruption events., Comment: 10 pages, accepted for publication in ApJ
Published: 2013
Full Text: View/download PDF

31. Using ISS Telescopes for Electromagnetic Follow-up of Gravitational Wave Detections of NS-NS and NS-BH Mergers

Author: Camp, Jordan, Barthelmy, Scott D., Blackburn, Lindy, Carpenter, Kenneth, Gehrels, Neil, Kanner, Jonah, Marshall, Frank E., Racusin, Judith L., Sakamoto, Takanori, Camp, Jordan, Barthelmy, Scott D., Blackburn, Lindy, Carpenter, Kenneth, Gehrels, Neil, Kanner, Jonah, Marshall, Frank E., Racusin, Judith L., and Sakamoto, Takanori
Abstract: The International Space Station offers a unique platform for rapid and inexpensive deployment of space telescopes. A scientific opportunity of great potential later this decade is the use of telescopes for the electromagnetic follow-up of ground-based gravitational wave detections of neutron star and black hole mergers. We describe this possibility for OpTIIX, an ISS technology demonstration of a 1.5 m diffraction limited optical telescope assembled in space, and ISS-Lobster, a wide-field imaging X-ray telescope now under study as a potential NASA mission. Both telescopes will be mounted on pointing platforms, allowing rapid positioning to the source of a gravitational wave event. Electromagnetic follow-up rates of several per year appear likely, offering a wealth of complementary science on the mergers of black holes and neutron stars.
Published: 2013
Full Text: View/download PDF

32. X-ray Transients in the Advanced LIGO/Virgo Horizon

Author: Kanner, Jonah, Baker, John, Blackburn, Lindy, Camp, Jordan, Mooley, Kunal, Mushotzky, Richard, Ptak, Andy, Kanner, Jonah, Baker, John, Blackburn, Lindy, Camp, Jordan, Mooley, Kunal, Mushotzky, Richard, and Ptak, Andy
Abstract: Advanced LIGO and Advanced Virgo will be all-sky monitors for merging compact objects within a few hundred Mpc. Finding the electromagnetic counterparts to these events will require an understanding of the transient sky at low red-shift (z<0.1). We performed a systematic search for extragalactic, low red-shift, transient events in the XMM-Newton Slew Survey. In a flux limited sample, we found that highly-variable objects comprised 10% of the sample, and that of these, 10% were spatially coincident with cataloged optical galaxies. This led to 4x10^-4 transients per square degree above a flux threshold of 3x10^-12 erg cm-2 s-1 [0.2-2 keV] which might be confused with LIGO/Virgo counterparts. This represents the first extragalactic measurement of the soft X-ray transient rate within the Advanced LIGO/Virgo horizon. Our search revealed six objects that were spatially coincident with previously cataloged galaxies, lacked evidence for optical AGNs, displayed high luminosities around 10^43 erg s-1, and varied in flux by more than a factor of ten when compared with the ROSAT All-Sky Survey. At least four of these displayed properties consistent with previously observed tidal disruption events., Comment: 10 pages, accepted for publication in ApJ
Published: 2013
Full Text: View/download PDF

33. Using ISS Telescopes for Electromagnetic Follow-up of Gravitational Wave Detections of NS-NS and NS-BH Mergers

Author: Camp, Jordan, Barthelmy, Scott D., Blackburn, Lindy, Carpenter, Kenneth, Gehrels, Neil, Kanner, Jonah, Marshall, Frank E., Racusin, Judith L., Sakamoto, Takanori, Camp, Jordan, Barthelmy, Scott D., Blackburn, Lindy, Carpenter, Kenneth, Gehrels, Neil, Kanner, Jonah, Marshall, Frank E., Racusin, Judith L., and Sakamoto, Takanori
Abstract: The International Space Station offers a unique platform for rapid and inexpensive deployment of space telescopes. A scientific opportunity of great potential later this decade is the use of telescopes for the electromagnetic follow-up of ground-based gravitational wave detections of neutron star and black hole mergers. We describe this possibility for OpTIIX, an ISS technology demonstration of a 1.5 m diffraction limited optical telescope assembled in space, and ISS-Lobster, a wide-field imaging X-ray telescope now under study as a potential NASA mission. Both telescopes will be mounted on pointing platforms, allowing rapid positioning to the source of a gravitational wave event. Electromagnetic follow-up rates of several per year appear likely, offering a wealth of complementary science on the mergers of black holes and neutron stars.
Published: 2013
Full Text: View/download PDF

34. Seeking Counterparts to Advanced LIGO/Virgo Transients with Swift

Author: Kanner, Jonah, Camp, Jordan, Racusin, Judith, Gehrels, Neil, White, Darren, Kanner, Jonah, Camp, Jordan, Racusin, Judith, Gehrels, Neil, and White, Darren
Abstract: Binary neutron star (NS) mergers are among the most promising astrophysical sources of gravitational wave emission for Advanced LIGO and Advanced Virgo, expected to be operational in 2015. Finding electromagnetic counterparts to these signals will be essential to placing them in an astronomical context. The Swift satellite carries a sensitive X-ray telescope (XRT), and can respond to target-of-opportunity requests within 1-2 hours, and so is uniquely poised to find the X-ray counterparts to LIGO/Virgo triggers. Assuming NS mergers are the progenitors of short gamma-ray bursts (GRBs), some percentage of LIGO/Virgo triggers will be accompanied by X-ray band afterglows that are brighter than 10^-12 erg/s/cm^2 in the XRT band one day after the trigger time. We find that a soft X-ray transient of this flux is bright enough to be extremely rare, and so could be confidently associated with even a moderately localized GW signal. We examine two possible search strategies with the Swift XRT to find bright transients in LIGO/Virgo error boxes. In the first strategy, XRT could search a volume of space with a ~100 Mpc radius by observing ~30 galaxies over the course of a day, with sufficient depth to observe the expected X-ray afterglow. For an extended LIGO/Virgo horizon distance, the XRT could employ 100 s exposures to cover an area of ~ 35 square degrees in about a day, remain sensitive enough to image GW discovered GRB afterglows. These strategies demonstrate that discovery of X-ray band counterparts to GW triggers will be possible., Comment: Submitted to ApJ, 8 pages
Published: 2012
Full Text: View/download PDF

35. Seeking Counterparts to Advanced LIGO/Virgo Transients with Swift

Author: Kanner, Jonah, Camp, Jordan, Racusin, Judith, Gehrels, Neil, White, Darren, Kanner, Jonah, Camp, Jordan, Racusin, Judith, Gehrels, Neil, and White, Darren
Abstract: Binary neutron star (NS) mergers are among the most promising astrophysical sources of gravitational wave emission for Advanced LIGO and Advanced Virgo, expected to be operational in 2015. Finding electromagnetic counterparts to these signals will be essential to placing them in an astronomical context. The Swift satellite carries a sensitive X-ray telescope (XRT), and can respond to target-of-opportunity requests within 1-2 hours, and so is uniquely poised to find the X-ray counterparts to LIGO/Virgo triggers. Assuming NS mergers are the progenitors of short gamma-ray bursts (GRBs), some percentage of LIGO/Virgo triggers will be accompanied by X-ray band afterglows that are brighter than 10^-12 erg/s/cm^2 in the XRT band one day after the trigger time. We find that a soft X-ray transient of this flux is bright enough to be extremely rare, and so could be confidently associated with even a moderately localized GW signal. We examine two possible search strategies with the Swift XRT to find bright transients in LIGO/Virgo error boxes. In the first strategy, XRT could search a volume of space with a ~100 Mpc radius by observing ~30 galaxies over the course of a day, with sufficient depth to observe the expected X-ray afterglow. For an extended LIGO/Virgo horizon distance, the XRT could employ 100 s exposures to cover an area of ~ 35 square degrees in about a day, remain sensitive enough to image GW discovered GRB afterglows. These strategies demonstrate that discovery of X-ray band counterparts to GW triggers will be possible., Comment: Submitted to ApJ, 8 pages
Published: 2012
Full Text: View/download PDF

36. LOOC UP: SEEKING OPTICAL COUNTERPARTS TO GRAVITATIONAL WAVE SIGNALS

Author: Kanner, Jonah Brian and Kanner, Jonah Brian
Abstract: Far-reaching investigations into astrophysics, precision measurements of cosmological parameters, and tests of fundamental physics are expected to be enabled through observations of gravitational wave (GW) signals. The gravitational waveform traces the bulk motion of matter in distant sources, and so observations of GWs would reveal the details of interesting astrophysical mechanisms that are inaccessible by any other means. Currently, the most sensitive GW instruments in the world are the Laser Interferometer Gravitational Wave Observatory (LIGO) and the Virgo observatory. These kilometer scale observatories make use of sensitive optics to record miniscule changes in the space-time metric induced by GW signals, and are located at three sites in the United States and Europe. Some models for sources of observable, transient GW signals predict that an electromagnetic (EM) counterpart will accompany the GW signal. These counterparts would be identifiable as transients which fade over the course of hours or days. Finding the EM counterpart to a GW signal would present significant benefits. The EM counterpart could confirm the astrophysical origin of the signal, and would also enhance the scientific investigations possible with the observation. This work describes the first prompt search for EM counterparts to GW event candidates. For the search, carried out between December 2009 and October 2010, event candidates from the LIGO/Virgo network were identified with latencies of only a few minutes. The sky position of each potential source was estimated, and was delivered to a collection of radio, optical, and x-ray telescopes with roughly thirty minutes of latency. The telescopes then observed the estimated source position, in an attempt to discover an EM counterpart. The low-latency GW data analysis, the methods for estimating source positions, and the observing strategy that guides telescopes based on GW data are all novel features of the search. The ability of the LIGO/V
Published: 2011

37. LOOC UP: Locating and observing optical counterparts to gravitational wave bursts

Author: Kanner, Jonah, Huard, Tracy L., Marka, Szabolcs, Murphy, David C., Piscionere, Jennifer, Reed, Molly, Shawhan, Peter, Kanner, Jonah, Huard, Tracy L., Marka, Szabolcs, Murphy, David C., Piscionere, Jennifer, Reed, Molly, and Shawhan, Peter
Abstract: Gravitational wave (GW) bursts (short duration signals) are expected to be associated with highly energetic astrophysical processes. With such high energies present, it is likely these astrophysical events will have signatures in the EM spectrum as well as in gravitational radiation. We have initiated a program, "Locating and Observing Optical Counterparts to Unmodeled Pulses in Gravitational Waves" (LOOC UP) to promptly search for counterparts to GW burst candidates. The proposed method analyzes near real-time data from the LIGO-Virgo network, and then uses a telescope network to seek optical-transient counterparts to candidate GW signals. We carried out a pilot study using S5/VSR1 data from the LIGO-Virgo network to develop methods and software tools for such a search. We will present the method, with an emphasis on the potential for such a search to be carried out during the next science run of LIGO and Virgo, expected to begin in 2009., Comment: 11 pages, 2 figures; v2) added acknowledgments, additional references, and minor text changes v3) added 1 figure, additional references, and minor text changes. v4) Updated references and acknowledgments. To be published in the GWDAW 12 Conf. Proc. by Classical and Quantum Gravity
Published: 2008
Full Text: View/download PDF

38. LOOC UP: Locating and observing optical counterparts to gravitational wave bursts

Author: Kanner, Jonah, Huard, Tracy L., Marka, Szabolcs, Murphy, David C., Piscionere, Jennifer, Reed, Molly, Shawhan, Peter, Kanner, Jonah, Huard, Tracy L., Marka, Szabolcs, Murphy, David C., Piscionere, Jennifer, Reed, Molly, and Shawhan, Peter
Abstract: Gravitational wave (GW) bursts (short duration signals) are expected to be associated with highly energetic astrophysical processes. With such high energies present, it is likely these astrophysical events will have signatures in the EM spectrum as well as in gravitational radiation. We have initiated a program, "Locating and Observing Optical Counterparts to Unmodeled Pulses in Gravitational Waves" (LOOC UP) to promptly search for counterparts to GW burst candidates. The proposed method analyzes near real-time data from the LIGO-Virgo network, and then uses a telescope network to seek optical-transient counterparts to candidate GW signals. We carried out a pilot study using S5/VSR1 data from the LIGO-Virgo network to develop methods and software tools for such a search. We will present the method, with an emphasis on the potential for such a search to be carried out during the next science run of LIGO and Virgo, expected to begin in 2009., Comment: 11 pages, 2 figures; v2) added acknowledgments, additional references, and minor text changes v3) added 1 figure, additional references, and minor text changes. v4) Updated references and acknowledgments. To be published in the GWDAW 12 Conf. Proc. by Classical and Quantum Gravity
Published: 2008
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Publication Year Range

Publication Type

Database

Publisher

38 results on '"Kanner, Jonah"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources