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1. Gravitational-wave Electromagnetic Counterpart Korean Observatory (GECKO): GECKO Follow-up Observation of GW190425

Author

Gregory S. H. Paek, Myungshin Im, Joonho Kim, Gu Lim, Bomi Park, Changsu Choi, Sophia Kim, Claudio Barbieri, Om Sharan Salafia, Insu Paek, Suhyun Shin, Jinguk Seo, Hyung Mok Lee, Chung-Uk Lee, Seung-Lee Kim, and Hyun-Il Sung

Subjects
High energy astrophysics, Time domain astronomy, Transient sources, Stellar mergers, Gravitational wave sources, Gravitational waves, Astrophysics, QB460-466
Abstract

One of the keys to the success of multimessenger astronomy is the rapid identification of the electromagnetic wave counterpart, kilonova (KN), of the gravitational-wave (GW) event. Despite its importance, it is hard to find a KN associated with a GW event, due to a poorly constrained GW localization map and numerous signals that could be confused as a KN. Here, we present the Gravitational-wave Electromagnetic wave Counterpart Korean Observatory (GECKO) project, the GECKO observation of GW190425, and prospects of GECKO in the fourth observing run (O4) of the GW detectors. We outline our follow-up observation strategies during O3. In particular, we describe our galaxy-targeted observation criteria that prioritize based on galaxy properties. Armed with this strategy, we performed an optical and/or near-infrared follow-up observation of GW190425, the first binary neutron star merger event during the O3 run. Despite a vast localization area of 7460 deg ^2 , we observed 621 host galaxy candidates, corresponding to 29.5% of the scores we assigned, with most of them observed within the first 3 days of the GW event. Ten transients were discovered during this search, including a new transient with a host galaxy. No plausible KN was found, but we were still able to constrain the properties of potential KNe using upper limits. The GECKO observation demonstrates that GECKO can possibly uncover a GW170817-like KN at a distance

Published
2024
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3. Space-borne atom interferometric gravitational wave detections. Part III. Eccentricity on dark sirens

Author

Tao Yang, Rong-Gen Cai, and Hyung Mok Lee

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Eccentricity of the inspiraling compact binaries can greatly improve the distance inference and source localization of dark sirens. In this paper, we continue the research for the space-borne atom interferometric gravitational-wave detector AEDGE and investigate the effects of eccentricity on the dark sirens observed by AEDGE in the mid-band. We simulate five types of typical compact binaries with component mass ranging from $1-100~M_{\odot}$. The largest improvement for both distance inference and localization can be as much as 1.5--3 orders of magnitude. We then construct the catalogs of dark sirens observed by AEDGE in five years. We find eccentricity is crucial to the detection of golden binary black holes (BBH) whose host galaxy can be uniquely identified. With only 5--10 golden dark BBHs one can obtain a 2 percent precision measurement of $H_0$ which is sufficient to arbitrate the Hubble tension. Regardless of eccentricity, AEDGE can also observe tens of golden binary neutron stars (BNS) and neutron star--black hole binaries (NSBH) with unique host galaxies. These golden dark sirens can serve as early warnings for the follow-up observations of gravitational waves in the high frequency band as well as the search of their electromagnetic counterparts. Our results show eccentricity is a crucial factor in the detection, data analysis, and application of GWs with the atom interferometers in the mid-band., 23 pages, 10 figures, typo corrections, published in JCAP

Published
2022

4. Space missions for astronomy and astrophysics in Korea: past, present, and future

Author

Dae-Hee Lee, Kyung-Suk Cho, Il Han Park, Woong-Seob Jeong, Young-Wook Lee, Kwang-Il Seon, Wonyong Han, Kyujin Kwak, Min Bin Kim, Jae-Jin Lee, and Hyung Mok Lee

Subjects
010302 applied physics, Schedule, Engineering, business.industry, FOS: Physical sciences, General Physics and Astronomy, Astronomy, 02 engineering and technology, Astrophysics, 021001 nanoscience & nanotechnology, 01 natural sciences, Field (computer science), Space exploration, 0103 physical sciences, Space program, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We review the history of space mission in Korea focusing on the field of astronomy and astrophysics. For each mission, scientific motivation and achievement are reviewed together with some technical details of the program including mission schedule. This review includes the ongoing and currently approved missions as well as some planned ones. Within the admitted limitations of authors' perspectives, some comments on the future direction of space program for astronomy and astrophysics in Korea are made at the end of this review., 29 pages, 31 figures, and 4 tables. To be published in the special issue of Journal of Korean Physical Society (JKPS) to celebrate the 25th anniversary of Astrophysics Division of Korean Physical Society (KPS)

Published
2021

8. Black Holes: From Imagnation to Reality

Author

Hyung Mok Lee

Subjects
General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Supermassive black holes in the central parts of galaxies have been extensively studied after a quasar was discovered in 1963. Quasars and active galactic nuclei are known to emit large amounts of electromagnetic radiation over a wide range of wavelengths within a very small volume. These objects are suggested to harbor massive black holes because a plausible mechanism for producing energy efficiently is conversion of the deep gravitational energy of a massive and compact object right after the discovery of the quasar. Astronomers also discovered that the central part of our galaxy has a strong concentration of mass as initially inferred from the rapid motion of the ionized gas near the center. In order to investigate the nature of that concentrated mass, a German group led by Reinhard Genzel and a US group led by Andrea Ghez improved the angular resolution by adopting speckle interferometry and adaptive optics in the near infrared so that very high resolution imaging of the stars in a small region around the Galactic center became possible. Since the mid 1990s, these two groups have made precision measurements of the positions of a large number of stars in the Galactic center and obtained their trajectories accurately. The gravitational field is found to be consistent with that due to a nearly point mass of about 4 million solar masses. Together with gravitational wave observations, imaging of the black hole shadow by with the Event Horizon Telescope, we now have firm observational evidence for the existence of black holes with a huge range of masses in the universe. Another big question to be answered is how these supermassive black holes are formed.

Published
2020

9. Eccentricity of Long Inspiraling Compact Binaries Sheds Light on Dark Sirens

Author

Tao Yang, Rong-Gen Cai, Zhoujian Cao, and Hyung Mok Lee

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The localization and distance inference of gravitational waves are two crucial factors for dark sirens as precise probes of cosmology, astrophysics, and fundamental physics. In this Letter, for the first time we investigate the parameter estimation of gravitational waves emitted by the eccentric compact binaries in the mid-frequency (0.1--10 Hz) band. Based on the configuration of one cluster of DECIGO (B-DECIGO), we simulate five types of typical compact binaries in GWTC-3 with component mass ranging from $\mathcal{O}(1\sim100)~M_{\odot}$. For each type of binaries, we assign discrete eccentricities from 0 to 0.4 at 0.1 Hz in $10^3$ random orientations. The multiple harmonics induced by eccentricity can break the degeneracy between parameters. We find that with eccentricity $e_0=0.4$, these typical binaries can achieve $\mathcal{O}(10^2-10^4)$ improvement for the distance inference in the near face-on orientations, compared to the circular case. More importantly, a nonvanishing eccentricity ($0.01\sim0.4$) can significantly improve the source localization of the typical binary black holes, most by $1.5\sim{3.5}$ orders of magnitude. Our result shows the remarkable significance of eccentricity for dark sirens in the mid-band as precise probes of the Universe., 6 pages, 2 figures, to match the published PRL version

Published
2022

12. Parameter estimation of eccentric gravitational waves with a decihertz observatory and its cosmological implications

Author

Tao Yang, Rong-Gen Cai, Zhoujian Cao, and Hyung Mok Lee

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Eccentricity of compact binaries can improve the parameter estimation of gravitational waves (GWs). In this paper, we first investigate the parameter estimation of eccentric GWs with decihertz observatory. We consider two scenarios for the configuration of DECIGO, i.e., the one cluster of DECIGO with its design sensitivity and B-DECIGO which also has one cluster but with inferior sensitivity as a comparison. We adopt the Fisher matrix to estimate the parameter errors. By mocking up the typical binaries in GWTC-3, we find a nonvanishing eccentricity can significantly improve the estimation for almost all waveform parameters. In particular, the localization of typical binary black holes (BBH) can achieve $\mathcal{O}(10-10^{3.5})$ factors of improvement when the initial eccentricity $e_0=0.4$ at 0.1 Hz. The precise localization of binary neutron stars (BNS) and neutron star--black hole binaries (NSBH), together with the large improvement of localization of BBH from eccentricity in the mid-band, inspire us to construct the catalogs of golden dark sirens whose host galaxies can be uniquely identified. We find that with only one cluster of DECIGO running 1 year in its design sensitivity, hundreds of golden dark BNS, NSBH, and tens of golden dark BBH can be observed. Eccentricity can greatly increase the population of golden dark BBH from $\sim 7~(e_0=0)$ to $\sim 65~(e_0=0.2)$. Such an increase of population of golden dark BBH events can improve the precision of Hubble constant measurement from 2.06\% to 0.68\%, matter density parameter from 64\% to 16\% in $\Lambda$CDM model. Through the phenomenological parameterization of GW propagation, the constraints of modified gravity can be improved from 6.2\% to 1.6\%. Our results show the remarkable significance of eccentricity for the detection and parameter estimation of GW events, allowing us to probe the Universe precisely., Comment: 29 pages, 23 figures, published in PRD

Published
2022
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13. Space-borne atom interferometric gravitational wave detections. Part II. Dark sirens and finding the one

Author

Tao Yang, Hyung Mok Lee, Rong-Gen Cai, Han Gil Choi, and Sunghoon Jung

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this paper, we investigate the potential of dark sirens by the space-borne atom interferometric gravitational-wave detectors to probe the Hubble constant. In the mid-frequency band, the sources live a long time. The motion of a detector around the Sun as well as in Earth orbit would induce large Doppler and reorientation effects, providing a precise angular resolution. Such precise localization for the GW sources makes it possible to observe the dark sirens with only one potential host galaxy, which are dubbed "golden dark sirens". We construct the catalogs of golden dark sirens and estimate that there are around 79 and 35 golden dark sirens of binary neutron stars (BNS) and binary black holes (BBH) that would be pass the detection threshold of AEDGE in 5 years. Our results show that with 5, 10, and all 79 golden dark BNS tracked by AEDGE one can constrain $H_0$ at 5.5\%, 4.1\%, and 1.8\% precision levels. With 5, 10, and all 35 golden dark BBH one can constrain $H_0$ at 2.2\%, 1.8\%, and 1.5\% precision levels, respectively. It suggests that only 5-10 golden dark BBH by AEDGE are sufficient to arbitrate the current tension between local and high-$z$ measurements of $H_0$., 16 pages, 6 figures, and 1 table. To match the published version

Published
2021

14. GECKO Optical Follow-up Observation of Three Binary Black Hole Merger Events: GW190408_181802, GW190412, and GW190503_185404

Author

Chung-Uk Lee, Gregory S. H. Paek, Sungyong Hwang, Jinguk Seo, Seo-Won Chang, Joonho Kim, Wonseok Kang, Myungshin Im, S. B. Kim, Changsu Choi, Hyun-Il Sung, Seung-Lee Kim, Tae-Woo Kim, Gu Lim, and Hyung Mok Lee

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Binary black hole, biology, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Gecko, Astrophysics, biology.organism_classification, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present optical follow-up observation results of three binary black hole merger (BBH) events, GW190408_181802, GW190412, and GW190503_185404, which were detected by the Advanced LIGO and Virgo gravitational wave (GW) detectors. Electromagnetic (EM) counterparts are generally not expected for BBH merger events. However, some theoretical models suggest that EM counterparts of BBH can possibly arise in special environments, prompting motivation to search for EM counterparts for such events. We observed high-credibility regions of the sky for the three BBH merger events with telescopes of the Gravitational-wave EM Counterpart Korean Observatory (GECKO), including the KMTNet. Our observation started as soon as 100 minutes after the GW event alerts and covered 29 - 63 deg$^2$ for each event with a depth of $\sim$ 22.5 mag in $R$-band within hours of observation. No plausible EM counterparts were found for these events, but from no detection in the GW190503_185404 event, for which we covered 69% credibility region, we place the BBH merger EM counterpart signal to be $M_{g}$ > -18.0 AB mag within about 1 day of the GW event. The comparison of our detection limits with light curves of several kilonova models suggests that a kilonova event could have been identified within hours from GW alert with GECKO observations if the compact merger happened at < 400 Mpc and the localization accuracy was of order of 50 deg$^2$. Our result gives a great promise for the GECKO facilities to find EM counterparts within a few hours from GW detection in future GW observation runs., 14 pages, 3 figures, accepted for publication in ApJ

Published
2021

16. Deep Learning Model on Gravitational Waveforms in Merging and Ringdown Phases of Binary Black Hole Coalescences

Author

Edwin J. Son, G. Cho, John J. Oh, Hyung Mok Lee, Joongoo Lee, Kyungmin Kim, and Sang Hoon Oh

Subjects
data analysis method, coalescence [black hole], neural network, black hole: binary: coalescence, FOS: Physical sciences, relativity theory [numerical calculations], mass [black hole], Markov chain [Monte Carlo], General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Monte Carlo: Markov chain, General Relativity and Quantum Cosmology, Gravitation, emission [gravitational radiation], Binary black hole, Fourier transformation, 0103 physical sciences, numerical methods, Range (statistics), Waveform, ddc:530, LIGO, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Coalescence (physics), 010308 nuclear & particles physics, binary: coalescence [black hole], black hole: mass, binary: compact, model [wave], Numerical relativity, wave: model, VIRGO, Cover (topology), black hole: coalescence, gravitational radiation: emission, compact [binary], numerical calculations: relativity theory, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Event (particle physics)
Abstract

Physical review / D 103(12), 123023 (2021). doi:10.1103/PhysRevD.103.123023, The waveform templates of the matched filtering-based gravitational-wave search ought to cover wide range of parameters for the prosperous detection. Numerical relativity (NR) has been widely accepted as the most accurate method for modeling the waveforms. Still, it is well known that NR typically requires a tremendous amount of computational costs. In this paper, we demonstrate a proof-of-concept of a novel deterministic deep learning (DL) architecture that can generate gravitational waveforms from the merger and ringdown phases of the non-spinning binary black hole coalescence. Our model takes O(1) seconds for generating approximately 1500 waveforms with a 99.9% match on average to one of the state-of-the-art waveform approximants, the effective-one-body. We also perform matched filtering with the DL-waveforms and find that the waveforms can recover the event time of the injected gravitational-wave signals., Published by Inst., Melville, NY

Published
2021
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17. Open data from the first and second observing runs of advanced LIGO and advanced Virgo

Author

Rich&nbsp, Abbott, Thomas&nbsp, Sheelu&nbsp, Abraham, Fausto&nbsp, Acernese, Kendall&nbsp, Ackley, Carl&nbsp, Adams, Rana&nbsp, Adhikari, Vaishali&nbsp, Adya, Christoph&nbsp, Affeldt, Michalis&nbsp, Agathos, Kazuhiro&nbsp, Agatsuma, Nancy&nbsp, Aggarwal, Odylio&nbsp, Aguiar, Amit&nbsp, Aich, Lorenzo&nbsp, Aiello, Anirban&nbsp, Ain, Ajith&nbsp, Parameswaran, Gabrielle&nbsp, Allen, Annalisa&nbsp, Allocca, Paul&nbsp, Altin, Alex&nbsp, Amato, Shreya&nbsp, Anand, Alena&nbsp, Ananyeva, Stuart&nbsp, Anderson, Warren&nbsp, Svetoslava, Angelova, Stefano&nbsp, Ansoldi, Sarah&nbsp, Antier, Stephen&nbsp, Appert, Koji&nbsp, Arai, Melody, Araya, Joseph, Areeda, Marc&nbsp, Arène, Nicolas&nbsp, Arnaud, Scott, Aronson, Arun, Kg, Ascenzi, Gregory&nbsp, Ashton, Stuart, Aston, Pia&nbsp, Astone, Florian&nbsp, Aubin, Peter&nbsp, Aufmuth, Kellie&nbsp, Aultoneal, Corey&nbsp, Austin, Valerie&nbsp, Avendano, Stanislav&nbsp, Babak, Philippe&nbsp, Bacon, Francesca&nbsp, Badaracco, Maria, Bader, Sangwook&nbsp, Bae, Anne, Baer, Jonathon&nbsp, Baird, Baldaccini, Giulio&nbsp, Ballardin, Stefan, Ballmer, Anna-marie&nbsp, Bals, Alexander&nbsp, Balsamo, Baltus, Sharan&nbsp, Banagiri, Deepak&nbsp, Bankar, Rameshwar, Bankar, Juan, Barayoga, Claudio&nbsp, Barbieri, Barry, Barish, David&nbsp, Barker, Kevin&nbsp, Barkett, Pablo&nbsp, Barneo, Fabrizio&nbsp, Barone, Bryan&nbsp, Barr, Lisa&nbsp, Barsotti, Matteo&nbsp, Barsuglia, Daniel&nbsp, Barta, Jeffrey&nbsp, Bartlett, Imre&nbsp, Bartos, Riccardo&nbsp, Bassiri, Andrea&nbsp, Basti, Mateusz&nbsp, Bawaj, Joseph, Bayley, Marco&nbsp, Bazzan, Bence&nbsp, Bécsy, Michal&nbsp, Bejger, Imene&nbsp, Belahcene, Angus, Bell, Deeksha&nbsp, Beniwal, Michael, Benjamin, Joe, Bentley, Fabio&nbsp, Bergamin, Beverly, Berger, Gerald&nbsp, Bergmann, Sebastiano&nbsp, Bernuzzi, Christopher, Berry, Diego&nbsp, Bersanetti, Alessandro&nbsp, Bertolini, Joseph&nbsp, Betzwieser, Rohan&nbsp, Bhandare, Ankit, Bhandari, Bidler, Edward&nbsp, Biggs, Igor, Bilenko, Garilynn&nbsp, Billingsley, Ross&nbsp, Birney, Ofek&nbsp, Birnholtz, Sebastien&nbsp, Biscans, Bischi, Sylvia&nbsp, Biscoveanu, Aparna&nbsp, Bisht, Guldauren&nbsp, Bissenbayeva, Massimiliano&nbsp, Bitossi, Marieanne, Bizouard, Kent, Blackburn, Jonathan&nbsp, Blackman, Carl, Blair, David, Blair, Ryan, Blair, Bobba, Nina&nbsp, Bode, Michel&nbsp, Boer, Yannick&nbsp, Boetzel, Gilles&nbsp, Bogaert, Francois&nbsp, Bondu, Edgard&nbsp, Bonilla, Romain&nbsp, Bonnand, Phillip&nbsp, Booker, Boris, Boom, Rolf&nbsp, Bork, Valerio&nbsp, Boschi, Sukanta&nbsp, Bose, Vladimir&nbsp, Bossilkov, Joel&nbsp, Bosveld, Yann&nbsp, Bouffanais, Antonella&nbsp, Bozzi, Carlo&nbsp, Bradaschia, Patrick, Brady, Alyssa&nbsp, Bramley, Marica&nbsp, Branchesi, Jim, Brau, Breschi, Tristan&nbsp, Briant, Joseph, Briggs, Francesco&nbsp, Brighenti, Alain&nbsp, Brillet, Brinkmann, Patrick&nbsp, Brockill, Aidan, Brooks, Brooks, Daniel, Brown, Sharon&nbsp, Brunett, Giacomo&nbsp, Bruno, Robert&nbsp, Bruntz, Aaron&nbsp, Buikema, Tomasz&nbsp, Bulik, Henk, Bulten, Alessandra&nbsp, Buonanno, Damir&nbsp, Buskulic, Robert, Byer, Miriam&nbsp, Cabero, Laura&nbsp, Cadonati, Giampietro&nbsp, Cagnoli, Craig&nbsp, Cahillane, Juan&nbsp, Calderón&nbsp, Bustillo, Jack, Callaghan, Thomas, Callister, Enrico&nbsp, Calloni, Jordan, Camp, Maurizio&nbsp, Canepa, Kipp, Cannon, Huy-tuong&nbsp, Cao, Junwei&nbsp, Giovanni&nbsp, Carapella, Franco&nbsp, Carbognani, Santiago&nbsp, Caride, Matthew, Carney, Gregorio&nbsp, Carullo, Julia&nbsp, Casanueva&nbsp, Diaz, Claudio&nbsp, Casentini, Javier&nbsp, Castañeda, Sarah&nbsp, Caudill, Marco&nbsp, Cavaglià, Fabien&nbsp, Cavalier, Roberto&nbsp, Cavalieri, Giancarlo&nbsp, Cella, Pablo&nbsp, Cerdá-Durán, Elisabetta&nbsp, Cesarini, Oualid&nbsp, Chaibi, Kabir&nbsp, Chakravarti, Chiwai&nbsp, Chan, Manleong&nbsp, Chan, Shiuh&nbsp, Chao, Philip&nbsp, Charlton, Eve, Chase, Eric&nbsp, Chassande-Mottin, Deep&nbsp, Chatterjee, Mayank&nbsp, Chaturvedi, Hsin-yu, Chen, Xu&nbsp, Chen, Yanbei&nbsp, Hai-ping&nbsp, Cheng, Chi-kit, Cheong, Hanyu, Chia, Chiadini, Roberto&nbsp, Chierici, Chincarini, Antonino&nbsp, Chiummo, Gihyuk&nbsp, Cho, Heesuk, Cho, Min-a&nbsp, Nelson&nbsp, Christensen, Qi&nbsp, Chu, Sheon&nbsp, Chua, Ka-wai, Chung, Shinkee&nbsp, Chung, Ciani, Pawel&nbsp, Ciecielag, Marek&nbsp, Cieślar, Alexei, Ciobanu, Ciolfi, Cipriano, Alessio&nbsp, Cirone, Filiberto&nbsp, Clara, James, Clark, Clearwater, Clesse, Frederic&nbsp, Cleva, Eugenio&nbsp, Coccia, Pierre-francois&nbsp, Cohadon, Cohen, Marta&nbsp, Colleoni, Christophe, Collette, Christopher&nbsp, Collins, Monica&nbsp, Colpi, Marcio&nbsp, Constancio&nbsp, Livia&nbsp, Jr., Conti, Sam, Cooper, Corban, Thomas, Corbitt, Isabel&nbsp, Cordero-Carrión, Silvia&nbsp, Corezzi, Kenneth, Corley, Neil&nbsp, Cornish, Corre, Corsi, Cortese, Cesar, Costa, Cotesta, Michael, Coughlin, Scott, Coughlin, Jeanpierre&nbsp, Coulon, Stefan, Countryman, Couvares, Pep, Covas, David, Coward, Matthew, Cowart, Dennis, Coyne, Coyne, Jolien, &nbsp, Creighton, Teviet, Creighton, Cripe, Michael&nbsp, Croquette, Sgwynne, Crowder, Jean-rene&nbsp, Cudell, Torrey, Cullen, Alan&nbsp, Cumming, Rebecca&nbsp, Cummings, Liam&nbsp, Cunningham, Elena&nbsp, Cuoco, Malgorzata&nbsp, Curylo, Tito&nbsp, Dal&nbsp, Canton, Gergely&nbsp, Dálya, Aykutlu&nbsp, Dana, Lara, Daneshgaran-Bajastani, Beatrice&nbsp, D’Angelo, Stefan, Danilishin, Sabrina&nbsp, D’Antonio, Karsten&nbsp, Danzmann, Christian&nbsp, Darsow-Fromm, Arnab&nbsp, Dasgupta, Laurence, &nbsp, Datrier, Vincenzo&nbsp, Dattilo, Ishant&nbsp, Dave, Michel&nbsp, Davier, Gareth, Davies, Derek&nbsp, Davis, Edward, Daw, Dan&nbsp, Debra, Malathi&nbsp, Deenadayalan, Jerome&nbsp, Degallaix, Martina&nbsp, De&nbsp, Laurentis, Samuel&nbsp, Deléglise, Matthew&nbsp, Delfavero, Nicola&nbsp, Lillo, Walter&nbsp, Del&nbsp, Pozzo, Lindsay, Demarchi, Virginia&nbsp, D’Emilio, Nicholas&nbsp, Demos, Dent, Pietri, Rosario&nbsp, Rosa, Camilla&nbsp, Rossi, Riccardo&nbsp, Desalvo, Omar&nbsp, de&nbsp, Varona, Sanjeev&nbsp, Dhurandhar, Mario, Díaz, Mauricio&nbsp, Diaz-Ortiz&nbsp, Tim&nbsp, Dietrich, Luciano&nbsp, Di&nbsp, Fiore, Chiara&nbsp, Fronzo, Cinzia&nbsp, Giorgio, Giovanni, Matteo&nbsp, Giovanni, Tristano&nbsp, Girolamo, Alberto&nbsp, Lieto, Binlei&nbsp, Ding, Sibilla&nbsp, Pace, Irene&nbsp, Palma, Renzo, Atul, Divakarla, Artemiy&nbsp, Dmitriev, Zoheyr&nbsp, Doctor, Fred&nbsp, Donovan, Katherine, Dooley, Suresh&nbsp, Doravari, Iain&nbsp, Dorrington, Thomas, Downes, Drago, Jenne, Driggers, Zhihui&nbsp, Jean-gregoire&nbsp, Ducoin, Dupej, Ofelia&nbsp, Durante, Domenico&nbsp, D’Urso, Sheila, Dwyer, Paul, Easter, Graeme&nbsp, Eddolls, Bruce&nbsp, Edelman, Tega, Edo, Oliver&nbsp, Edy, Anamaria&nbsp, Effler, Phil&nbsp, Ehrens, Johannes&nbsp, Eichholz, Stephen, Eikenberry, Eisenmann, Robert, Eisenstein, Aldo&nbsp, Ejlli, Lucianolucianikerrico&nbsp, Errico, Reed, Essick, Hector&nbsp, Estelles, Dimitri&nbsp, Estevez, Zachariah, Etienne, Todd&nbsp, Etzel, Matthew&nbsp, Evans, Tom, Evans, Rebecca, Ewing, Viviana&nbsp, Fafone, Fairhurst, Xilong&nbsp, Fan, Stefania&nbsp, Farinon, Benjamin&nbsp, Farr, Will, Farr, Edward, Fauchon-Jones, Favata, Maxime&nbsp, Fays, Mariana&nbsp, Fazio, Jon&nbsp, Feicht, Martin, Fejer, Fangchen&nbsp, Feng, Edit&nbsp, Fenyvesi, Deborah, Ferguson, Alvaro&nbsp, Fernandez-Galiana, Isidoro&nbsp, Ferrante, Elvis, Ferreira, Tabata, Ferreira, Fidecaro, Irene&nbsp, Fiori, Donatella&nbsp, Fiorucci, Maya&nbsp, Fishbach, Ryan, Fisher, Rosalba&nbsp, Fittipaldi, Margot&nbsp, Fitz-Axen, Vincenzo&nbsp, Fiumara, Raffaele&nbsp, Flaminio, Erik&nbsp, Floden, Flynn, Heather&nbsp, Fong, Antonio, Font, Perry&nbsp, Forsyth, Jean-daniel&nbsp, Fournier, Sergio&nbsp, Frasca, Frasconi, Zsolt&nbsp, Frei, Andreas&nbsp, Freise, Raymond&nbsp, Frey, Valentin&nbsp, Fritschel, Valery, Frolov, Gabriele&nbsp, Fronzè, Fulda, Fyffe, Hunter, Gabbard, Bhooshan, Gadre, Sebastian, Gaebel, Jonathan, Gair, Shanika&nbsp, Galaudage, Dhruva&nbsp, Ganapathy, Sharad, Gaonkar, Cecilio&nbsp, García-Quirós, Garufi, Bubba&nbsp, Gateley, Gaudio, Gayathri&nbsp, Gayathri, Gianluca&nbsp, Gemme, Genin, Alberto&nbsp, Gennai, George, Jogy&nbsp, Laszlo&nbsp, Gergely, Sudarshan&nbsp, Ghonge, Abhirup&nbsp, Ghosh, Archisman&nbsp, Shaon&nbsp, Bruno&nbsp, Giacomazzo, Joe, Giaime, Dwayne, Giardina, Des, Gibson, Chalisa&nbsp, Gier, Kiranjyot&nbsp, Gill, Jane&nbsp, Glanzer, Jan&nbsp, Gniesmer, Godwin, Evan&nbsp, Goetz, Ryan&nbsp, Niklas&nbsp, Gohlke, Boris&nbsp, Goncharov, Gabriela&nbsp, González, Gopakumar&nbsp, Gopakumar, Sarah, Gossan, Matthieu&nbsp, Gosselin, Gouaty, Grace, Aniello&nbsp, Grado, Massimo&nbsp, Granata, Alastair&nbsp, Grant, Slawomir&nbsp, Gras, Grassia, Gray, Rachel&nbsp, Giuseppe&nbsp, Greco, Anna, Green, Rhys&nbsp, Green, Elizabeth, Gretarsson, Hannah, Griggs, nbsp, Grignani, Grimaldi, Stefan, Grimm, Hartmut&nbsp, Grote, Steffen&nbsp, Grunewald, Pierre&nbsp, Gruning, Gianluca, Guidi, Andre, Guimaraes, Gerard&nbsp, Guixé, Hitesh, Gulati, Yuefan&nbsp, Guo, Anuradha&nbsp, Gupta, Anchal&nbsp, Pawan&nbsp, Eric, Gustafson, Dick&nbsp, Gustafson, Leila&nbsp, Haegel, Odysse&nbsp, Halim, Evan, Hall, Eleanor, Hamilton, Giles&nbsp, Hammond, Maria&nbsp, Haney, Manuela, Hanke, Hanks, Chad&nbsp, Hanna, Mark, Hannam, Otto, Hannuksela, Travis, Hansen, Joe&nbsp, Hanson, Harder, Terra&nbsp, Hardwick, Haris&nbsp, Haris, Harms, Gregg, Harry, Ian, Harry, Raine, Hasskew, Carl-johan&nbsp, Haster, Karen&nbsp, Haughian, Fergus, Hayes, James&nbsp, Healy, Antoine&nbsp, Heidmann, Matthew, Heintze, Joscha&nbsp, Heinze, Henrich&nbsp, Heitmann, Frances&nbsp, Hellman, Patrice&nbsp, Hello, Gary&nbsp, Hemming, Martin&nbsp, Hendry, Siong, Heng, Hennes, Jan-simon&nbsp, Hennig, Michele&nbsp, Heurs, Stefan&nbsp, Hild, Tanja&nbsp, Hinderer, Sarah, Hoback, Sven&nbsp, Hochheim, Elyssa&nbsp, Hofgard, Hofman, Aaron, Holgado, Nathan, Holland, Kathy&nbsp, Holt, Daniel, Holz, Hopkins, Horst, Hough, Eric, Howell, Charlie, Hoy, Yiwen&nbsp, Huang, Moritz, Hübner, Eliu, Huerta, Dominique&nbsp, Huet, Brennan&nbsp, Hughey, Victor&nbsp, Hui, Sascha&nbsp, Husa, Sabina, Huttner, Rachael&nbsp, Huxford, Tien&nbsp, Huynh-Dinh, Bartosz&nbsp, Idzkowski, Iess, Henri&nbsp, Inchauspe, Ingram, Intini, Jean, Isac, Max&nbsp, Isi, Bala, Iyer, Thibaut&nbsp, Jacqmin, Sameer, Jadhav, Shreejit, Jadhav, Alasdair, James, Karan&nbsp, Jani, Nagaraj, Janthalur, Piotr&nbsp, Jaranowski, Jariwala, Rafel&nbsp, Jaume, Alex, Jenkins, Jun&nbsp, Jiang, Grace, Johns, Aaron, Jones, Ian, Jones, Jeff, Jones, Philip&nbsp, Jones, Russell&nbsp, Reinier, &nbsp, Jonker, Ju&nbsp, Jonas&nbsp, Junker, Chinmay, Kalaghatgi, Vassiliki&nbsp, Kalogera, Brittany&nbsp, Kamai, Shivaraj&nbsp, Kandhasamy, Gungwon&nbsp, Kang, Jonah, Kanner, Shasvath, Kapadia, Karki, Rahul&nbsp, Kashyap, Marie&nbsp, Kasprzack, Wolfgang&nbsp, Kastaun, Stavros&nbsp, Katsanevas, Katsavounidis, William&nbsp, Katzman, Kaufer, Keita&nbsp, Kawabe, Fabien&nbsp, Kéfélian, Keitel, Azadeh&nbsp, Keivani, Kennedy, Joey, Key, Sudiksha&nbsp, Khadka, Farit, Khalili, Imran&nbsp, Khan, Sebastian&nbsp, Zaki, Khan, Efim, Khazanov, Nandita&nbsp, Khetan, Mohammad&nbsp, Khursheed, Nutsinee&nbsp, Kijbunchoo, Chunglee&nbsp, Kim, Grace, Kim, Jeongcho, Kim, Kyungmin&nbsp, Won&nbsp, Whansun, Kim, Young-min&nbsp, Charles&nbsp, Kimball, Peter, King, Kinley-Hanlon, Robin&nbsp, Kirchhoff, Jeffrey, Kissel, Kleybolte, Sergei&nbsp, Klimenko, Tyler, Knowles, Koch, Sina, Koehlenbeck, Gideon&nbsp, Koekoek, Soumen&nbsp, Koley, Veronica&nbsp, Kondrashov, Antonios&nbsp, Kontos, Nico&nbsp, Koper, Mikhail&nbsp, Korobko, William, Korth, Manoj&nbsp, Kovalam, Dan, Kozak, Volker&nbsp, Kringel, Krishnendu, Nv, Andrzej&nbsp, Królak, Natalie&nbsp, Krupinski, Gerrit&nbsp, Kuehn, Anil&nbsp, Kumar, Prayush&nbsp, Rakesh&nbsp, Sumit&nbsp, Ling-chi&nbsp, Kuo, Adam&nbsp, Kutynia, Benjamin, Lackey, Danny&nbsp, Laghi, Emile&nbsp, Lalande, Lam, Lam, Astrid&nbsp, Lamberts, Landry, Benjamin, Lane, Ryan, Lang, Jacob&nbsp, Lange, Brian&nbsp, Lantz, Robert, Lanza, Iuri&nbsp, La&nbsp, Rosa, Angelique&nbsp, Lartaux-Vollard, Paul, Lasky, Laxen, Albert&nbsp, Lazzarini, Claudia&nbsp, Lazzaro, Paola&nbsp, Leaci, Sean&nbsp, Leavey, Yannick, Lecoeuche, Chang-hwan, Lee, Hyung-mok, Lee, Hyungwon, Lee, Joongoo&nbsp, Lee, Kyung-ha&nbsp, Lehmann, Leroy, Letendre, Yuri&nbsp, Levin, Alvin, &nbsp, Jin&nbsp, Kaye&nbsp, Tjonnie, &nbsp, Xiang&nbsp, Frank&nbsp, Linde, Seth, Linker, Jethro, Linley, Tyson, Littenberg, Liu&nbsp, Liu, Xiaoshu&nbsp, Miquel&nbsp, Llorens-Monteagudo, Ka-lok&nbsp, Alexandra&nbsp, Lockwood, Lionel, London, Longo, Lorenzini, Vincent&nbsp, Loriette, Lormand, Losurdo, James, Lough, Carlos, Lousto, Geoffrey&nbsp, Lovelace, Harald&nbsp, Lück, Diana&nbsp, Lumaca, Andrew, Lundgren, Ma&nbsp, Yiqiu, Ronaldas&nbsp, Macas, Macfoy, Myron&nbsp, Macinnis, Duncan, Macleod, Ian, Macmillan, Adrian&nbsp, Macquet, Ignacio&nbsp, Magaña&nbsp, Hernandez, Fabian&nbsp, Magaña-Sandoval, Ryan, Magee, Ettore&nbsp, Majorana, Ivan&nbsp, Maksimovic, Asmita&nbsp, Malik, Catherine&nbsp, Man, Vuk&nbsp, Mandic, Valentina&nbsp, Mangano, Georgia, Mansell, Manske, Maddalena&nbsp, Mantovani, Michela&nbsp, Mapelli, Marchesoni, Frederique&nbsp, Marion, Szabolcs&nbsp, Márka, Zsuzsanna&nbsp, Charalampos&nbsp, Markakis, Ashot, Markosyan, Markowitz, Ed&nbsp, Maros, Antonio&nbsp, Marquina, Sylvain&nbsp, Marsat, Filippo&nbsp, Martelli, Ian, Martin, Rodica, Martin, Martinez, Denis, Martynov, Hossein&nbsp, Masalehdan, Ken&nbsp, Mason, Massera, Masserot, Thomas, Massinger, Mariela&nbsp, Masso-Reid, Simone&nbsp, Mastrogiovanni, Andrew&nbsp, Matas, Fabrice&nbsp, Matichard, Nergis&nbsp, Mavalvala, Emily&nbsp, Maynard, Joshua, Mccann, Richard&nbsp, Mccarthy, David, Mcclelland, Scott&nbsp, Mccormick, Lee&nbsp, Mcculler, Stephen, Mcguire, Connor&nbsp, Mcisaac, Jessica&nbsp, Mciver, David, Mcmanus, Terry&nbsp, Mcrae, Sean, Mcwilliams, Duncan&nbsp, Meacher, Grant, Meadors, Moritz&nbsp, Mehmet, Ajit, Mehta, Mejuto&nbsp, Villa, Andrew&nbsp, Melatos, Gregory&nbsp, Mendell, Adam, Mercer, Mereni, Kara&nbsp, Merfeld, Edmond, Merilh, Jonathan, Merritt, Mourad&nbsp, Merzougui, Syd&nbsp, Meshkov, Chris&nbsp, Messenger, Cody&nbsp, Messick, Remi&nbsp, Metzdorff, Patrick, Meyers, Fabian&nbsp, Meylahn, Ashish&nbsp, Mhaske, Miani, Haixing&nbsp, Miao, Ioannis&nbsp, Michaloliakos, Christophe&nbsp, Michel, Hannah&nbsp, Middleton, Leopoldo&nbsp, Milano, Andrewlawrence, Miller, Meg&nbsp, Millhouse, Joseph, Mills, Edoardo&nbsp, Milotti, Michael, Milovich-Goff, Olivier&nbsp, Minazzoli, Minenkov, Alec&nbsp, Mishkin, Chandra&nbsp, Mishra, Timesh&nbsp, Mistry, Sanjit&nbsp, Mitra, Valery, Mitrofanov, Guenakh&nbsp, Mitselmakher, Mittleman, Kentaro&nbsp, Mogushi, Satyanarayan, &nbsp, Mohapatra, Siddharth, Mohite, Manel&nbsp, Molina-Ruiz, Marina&nbsp, Mondin, Montani, Christopher, Moore, Moraru, Filip&nbsp, Morawski, Gerardo&nbsp, Moreno, Soichiro&nbsp, Morisaki, Benoit&nbsp, Mours, Conor, Mow-Lowry, Mozzon, Federico&nbsp, Muciaccia, Arunava&nbsp, Mukherjee, Debnandini&nbsp, Soma&nbsp, Subroto&nbsp, Nikhil&nbsp, Mukund, Mullavey, Jesper&nbsp, Munch, Erik, Muñiz, Peter, Murray, Nagar, Ilaria&nbsp, Nardecchia, Luca&nbsp, Naticchioni, Rajesh, Nayak, Benjamin, Neil, Joshua&nbsp, Neilson, Gijs&nbsp, Nelemans, Timothy, &nbsp, Nelson, Marina&nbsp, Nery, Ansel&nbsp, Neunzert, Kwan-yeung, Ng, Nguyen, Nichols, Shania, Nichols, Samaya&nbsp, Nissanke, Flavio&nbsp, Nocera, Minkyun&nbsp, Noh, North, Devon&nbsp, Nothard, Laura, Nuttall, Jason&nbsp, Oberling, Brendan, O’Brien, Gor&nbsp, Oganesyan, Greg, Ogin, John, Oh, Sanghoon, Oh, Ohme, Hiroaki&nbsp, Ohta, Marcos, Okada, Oliver, Olivetto, Oppermann, Oram, O’Reilly, Rich, Ormiston, Luis, Ortega, O’Shaughnessy, Serguei&nbsp, Ossokine, Osthelder, David, Ottaway, Harry&nbsp, Overmier, Ben, Owen, Alexander, Pace, Giulia&nbsp, Pagano, Michael, Page, Pagliaroli, Archana&nbsp, Pai, Siddhesh, Pai, Jordan, Palamos, Oleg&nbsp, Palashov, Cristiano&nbsp, Palomba, Howard&nbsp, Pan, Pratap, Panda, Tsun-ho&nbsp, Pang, Pankow, Pannarale, F, Brijesh, Pant, Paoletti, Paoli, Abhishek&nbsp, Parida, Parker, Daniela&nbsp, Pascucci, Pasqualetti, Passaquieti, Passuello, Barbara&nbsp, Patricelli, Ethan&nbsp, Payne, Brynley, Pearlstone, Thida, Pechsiri, Ari, Pedersen, Mike&nbsp, Pedraza, Arnaud&nbsp, Pele, Steven&nbsp, Penn, Albino&nbsp, Perego, Carlos, Perez, Perigois&nbsp, Périgois, Perreca, Stephane&nbsp, Perriès, Petermann, Harald, Pfeiffer, Phelps, Khun, Phukon, Ornella, Piccinni, Mikhael&nbsp, Pichot, Piendibene, Piergiovanni, Pierro, Gabriel&nbsp, Pillant, Laurent&nbsp, Pinard, Innocenzo, Pinto, Krzysztof&nbsp, Piotrzkowski, Pirello, Pitkin, Wolfango&nbsp, Plastino, Rosa&nbsp, Poggiani, Yat-tung, Pong, Ponrathnam, Pasquale&nbsp, Popolizio, Porter, Ed, Jade&nbsp, Powell, Atul, Prajapati, Kiran&nbsp, Prasai, Raghurama&nbsp, Prasanna, Geraint&nbsp, Pratten, Tanner&nbsp, Prestegard, Principe, Prodi, Leonid&nbsp, Prokhorov, Punturo, Puppo, Pürrer, Hong&nbsp, Quetschke, Pedro, Quinonez, Fred, Raab, Geert&nbsp, Raaijmakers, Hugh&nbsp, Radkins, Radulesco, Raffai, Hanna&nbsp, Rafferty, Sendhil&nbsp, Raja, Rajan&nbsp, Rajan, Binod&nbsp, Rajbhandari, Malik&nbsp, Rakhmanov, Karla, Ramirez, Antoni&nbsp, Ramos-Buades, Javed&nbsp, Rana, Kaushik&nbsp, Rao, Piero&nbsp, Rapagnani, Vivien&nbsp, Raymond, Razzano, Jocelyn&nbsp, Read, Tania&nbsp, Regimbau, Rei, Reid, David, Reitze, Rettegno, Fulvio&nbsp, Ricci, Colter, Richardson, Jonathan, Richardson, Paul, Ricker, Gunnar&nbsp, Riemenschneider, Keith&nbsp, Riles, Rizzo, Norna, Robertson, Florent&nbsp, Robinet, Rocchi, Ramon, Rodriguez-Soto, Loic&nbsp, Rolland, Jameson, Rollins, Vincent, Roma, Romanelli, Rocco&nbsp, Romano, Chandra, Romel, Isobel, Romero-Shaw, Janeen, Romie, Caitlin, Rose, Dakota&nbsp, Rose, Kyle&nbsp, Dorota&nbsp, Rosińska, Shawn, Rosofsky, Michael, Ross, Sheila&nbsp, Rowan, Samuel, Rowlinson, Palash, Roy, Santosh&nbsp, Roy, Paolo&nbsp, Ruggi, Guntis&nbsp, Rutins, Ryan, Surabhi&nbsp, Sachdev, Travis&nbsp, Sadecki, Mairi&nbsp, Sakellariadou, Salafia, Om, Livio&nbsp, Salconi, Muhammed&nbsp, Saleem, Samajdar, Eduardo, Sanchez, Luis, Sanchez, Sanchis-Gual, Jaclyn, Sanders, Kevin, Santiago, Edison&nbsp, Santos, Sarin, Sassolas, Sathyaprakash, B, Orion&nbsp, Sauter, Richard, Savage, Vaibhav&nbsp, Savant, Disha&nbsp, Sawant, Sihem&nbsp, Sayah, Dean&nbsp, Schaetzl, Schale, Mark&nbsp, Scheel, Scheuer, Patricia&nbsp, Schmidt, Roman&nbsp, Schnabel, Robert, &nbsp, Schofield, Axel&nbsp, Schönbeck, Emil&nbsp, Schreiber, Bernd, Schulte, Bernard, Schutz, Otto&nbsp, Schwarm, Eyal&nbsp, Schwartz, Jamie&nbsp, Scott, Susan, Scott, Seidel, Sellers, Anand, Sengupta, Noah&nbsp, Sennett, Sentenac, Valeria&nbsp, Sequino, Sergeev, Yoshinta&nbsp, Setyawati, Daniel, Shaddock, Shaffer, Selim, Shahriar, Sharma, Priyanka&nbsp, Shawhan, Hongyu&nbsp, Shen, Minori&nbsp, Shikauchi, Rosalie&nbsp, Shink, David, Shoemaker, Deirdre, Shoemaker, Keerti&nbsp, Shukla, Shyamsundar&nbsp, Shyamsundar, Karelle&nbsp, Siellez, Magdalena&nbsp, Sieniawska, Sigg, Leo, Singer, Divya&nbsp, Singh, Neha&nbsp, Ayatri&nbsp, Singha, Akshat&nbsp, Singhal, Alicia, Sintes, Sipala, Vasileios&nbsp, Skliris, Bram, &nbsp, Slagmolen, Teresa, Slaven-Blair, Jiri&nbsp, Smetana, Joshua, Smith, Rory, &nbsp, Smith, Surendranadh&nbsp, Somala, Edwin, Son, Siddharth&nbsp, Soni, Borja&nbsp, Sorazu, Viola&nbsp, Sordini, Fiodor&nbsp, Sorrentino, Tarun&nbsp, Souradeep, Sowell, Andrew, Spencer, Mario&nbsp, Spera, Amit, Srivastava, Varun&nbsp, Srivastava, Kai&nbsp, Staats, Cosmin&nbsp, Stachie, Standke, Daniele, Steer, Steinke, Steinlechner, Steinmeyer, Dane&nbsp, Stocks, David, Stops, Madeline&nbsp, Stover, Ken, Strain, Stratta, Amber&nbsp, Strunk, Sturani, Amber, Stuver, Sudhagar&nbsp, Sudhagar, Vivishek&nbsp, Sudhir, Tiffany, Summerscales, Ling&nbsp, Sun, Sunil&nbsp, Sunil, Ankan&nbsp, Sur, Jishnu&nbsp, Suresh, Patrick, Sutton, Bas, Swinkels, Marek, Szczepańczyk, Tacca, Simon, Tait, Colm&nbsp, Talbot, Andres, Tanasijczuk, David, Tanner, Duo&nbsp, Tao, Marton&nbsp, Tápai, Amauri&nbsp, Tapia, Enzo, Tapia&nbsp, San&nbsp, Martin, Jay, Tasson, Taylor, Rodrigo&nbsp, Tenorio, Lukas&nbsp, Terkowski, Manasadevi, Thirugnanasambandam, Thomas, Jonathan, Thompson, Sivananda, Thondapu, Keith, Thorne, Thrane, Calley, Tinsman, Saravanan, Saravanan, Shubhanshu&nbsp, Tiwari, Srishti&nbsp, Karl&nbsp, Toland, Mauro&nbsp, Tonelli, Zeno&nbsp, Tornasi, Alejandro&nbsp, Torres-Forné, Calum, Torrie, Iara&nbsp, Tosta&nbsp, e&nbsp, Melo, Töyrä, Emily, Trail, Travasso, Traylor, Maria, Tringali, Aashish&nbsp, Tripathee, Agata&nbsp, Trovato, Randy, Trudeau, Ka-wa, Tsang, Maggie&nbsp, Tse, Rhondale&nbsp, Tso, Leo&nbsp, Tsukada, Daichi&nbsp, Tsuna, Takuya&nbsp, Tsutsui, Margherita&nbsp, Turconi, Amit, Ubhi, Koh&nbsp, Ueno, Dennis&nbsp, Ugolini, Unnikrishnan, Cs, Alexander, Urban, Samantha, Usman, Andrei, Utina, Henning&nbsp, Vahlbruch, Vajente, Guillermo&nbsp, Valdes, Valentini, Vallisneri, Niels&nbsp, van&nbsp, Bakel, Martin&nbsp, Beuzekom, den&nbsp, Brand, Chris&nbsp, Van&nbsp, Den&nbsp, Broeck, Daniel, Vander-Hyde, der&nbsp, Schaaf, Joris, Van&nbsp, Heijningen, Marielle, van&nbsp, Veggel, Marco&nbsp, Vardaro, Vijay&nbsp, Varma, Steve&nbsp, Vass, Matyas&nbsp, Vasúth, Alberto&nbsp, Vecchio, Gabriele&nbsp, Vedovato, John&nbsp, Veitch, Peter, Veitch, Krishna&nbsp, Venkateswara, Gautam&nbsp, Venugopalan, Didier&nbsp, Verkindt, Doga&nbsp, Veske, Vetrano, Viceré, Aaron, Viets, Serena&nbsp, Vinciguerra, David, Vine, Jeanyves&nbsp, Vinet, Salvatore&nbsp, Vitale, Francisco&nbsp, Hernandez&nbsp, Vivanco, Thomas&nbsp, Helios&nbsp, Vocca, Cheryl&nbsp, Vorvick, Sergey, Vyatchanin, Andrew, Wade, Leslie, Wade, Wade, Rob&nbsp, Walet, Marissa&nbsp, Walker, Gavin, Wallace, Larry&nbsp, Wallace, Sinead&nbsp, Walsh, Jonathan, Wang, Sibo&nbsp, Wang, Wenhui, Wang, Yifan, Wang, Robert, Ward, Zane, Warden, Jim&nbsp, Warner, Was, Jennifer&nbsp, Watchi, Betsy&nbsp, Weaver, Li-wei&nbsp, Wei, Weinert, Alan, Weinstein, Rainer&nbsp, Weiss, Felix&nbsp, Wellmann, Linqing&nbsp, Wen, Weßels, Jonathan, Westhouse, Wette, John, Whelan, Bernard, 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(PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Spectroscopies optiques des matériaux verres, amorphes et à nanoparticules (SOPRANO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Etudes Scientifiques (IHES), Agencia Estatal de Investigación (España), Generalitat de Catalunya, Generalitat Valenciana, European Commission, Grav. waves and fundamental physics, RS: FSE Grav. waves and fundamental physics, RS: FSE MSP, Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aich, A., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Ansoldi, S., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Aronson, S. M., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baer, A. M., Baird, J., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Bankar, R. S., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barkett, K., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Bentley, J. D., Bergamin, F., Berger, B. K., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bhandari, A. V., Bidler, J., Biggs, E., Bilenko, I. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bissenbayeva, G., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Castañeda, J., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chan, C., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chierici, R., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciecielag, P., Cieślar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cudell, J. -R., Cullen, T. J., Cumming, A., Cummings, R., Cunningham, L., Cuoco, E., Curylo, M., Canton, T. Dal, Dálya, G., Dana, A., Daneshgaran-Bajastani, L. M., D’Angelo, B., Danilishin, S. L., D’Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davies, G. S., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Delfavero, M., De Lillo, N., Del Pozzo, W., Demarchi, L. M., D’Emilio, V., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., de Varona, O., Dhurandhar, S., Díaz, M. C., Diaz-Ortiz, M., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., D’Urso, D., Dwyer, S. E., Easter, P. J., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Feng, F., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fitz-Axen, M., Fiumara, V., Flaminio, R., Floden, E., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronzè, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Galaudage, S., Ganapathy, D., Gaonkar, S. G., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Gill, K., Glanzer, J., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., González, G., Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Griggs, H. L., Grignani, G., Grimaldi, A., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guimaraes, A. R., Guixé, G., Gulati, H. K., Guo, Y., Gupta, A., Gupta, Anchal, Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heinze, J., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hoback, S. Y., Hochheim, S., Hofgard, E., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., Hübner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Intini, G., Isac, J. - M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jiang, J., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Keivani, A., Kennedy, R., Key, J. S., Khadka, S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z. A., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, G. J., Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kovalam, M., Kozak, D. B., Kringel, V., Krishnendu, N. V., Królak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kumar, S., Kuo, L., Kutynia, A., Lackey, B. D., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Leroy, N., Letendre, N., Levin, Y., Li, A. K. Y., Li, J., Li, K., Li, T. G. F., Li, X., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, J., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., Hernandez, I. Magaña, Magaña-Sandoval, F., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, V., Martynov, D. V., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Mavalvala, N., Maynard, E., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Villa, E. Mejuto, Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Middleton, H., Milano, L., Miller, A. L., Millhouse, M., Mills, J. C., Milotti, E., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Mogushi, K., Mohapatra, S. R. P., Mohite, S. 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R., Palashov, O., Palomba, C., Pan, H., Panda, P. K., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Payne, E., Pearlstone, B. L., Pechsiri, T. C., Pedersen, A. J., Pedraza, M., Pele, A., Penn, S., Perego, A., Perez, C. J., Périgois, C., Perreca, A., Perriès, S., Petermann, J., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Piotrzkowski, K., Pirello, M., Pitkin, M., Plastino, W., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Principe, M., Prodi, G. A., Prokhorov, L., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Raab, F. 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P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stocks, D., Stops, D. J., Stover, M., Strain, K. A., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Tanasijczuk, A. J., Tanner, D. B., Tao, D., Tápai, M., Tapia, A., Martin, E. N. Tapia San, Tasson, J. D., Taylor, R., Tenorio, R., Terkowski, L., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tinsman, C. L., Saravanan, T. R., Tiwari, Shubhanshu, Tiwari, S., Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Tosta e Melo, I., Töyrä, D., Trail, E. A., Travasso, F., Traylor, G., Tringali, M. C., Tripathee, A., Trovato, A., Trudeau, R. J., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tsutsui, T., Turconi, M., Ubhi, A. S., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Utina, A. C., Vahlbruch, H., Vajente, G., Valdes, G., Valentini, M., Vallisneri, M., van Bakel, N., van Beuzekom, M., 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, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Veske, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vivanco, Francisco Hernandez, Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J. Z., Wang, S., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Wong, C., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Zadrożny, A. K., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhao, G., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Nice Sophia Antipolis (... - 2019) (UNS), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Abbott, R, Abbott, T, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aich, A, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Altin, P, Amato, A, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Ansoldi, S, Antier, S, Appert, S, Arai, K, Araya, M, Areeda, J, Arene, M, Arnaud, N, Aronson, S, Arun, K, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baer, A, Baird, J, Baldaccini, F, Ballardin, G, Ballmer, S, Bals, A, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Bankar, R, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barkett, K, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I, Bell, A, Beniwal, D, Benjamin, M, Bentley, J, Bergamin, F, Berger, B, Bergmann, G, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bhandari, A, Bidler, J, Biggs, E, Bilenko, I, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Bissenbayeva, G, Bitossi, M, Bizouard, M, Blackburn, J, Blackman, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, S, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Camp, J, Canepa, M, Cannon, K, Cao, H, Cao, J, Carapella, G, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Castaneda, J, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, O, Chakravarti, K, Chan, C, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chen, H, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chiadini, F, Chierici, R, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Ciecielag, P, Cieslar, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Cohadon, P, Cohen, D, Colleoni, M, Collette, C, Collins, C, Colpi, M, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Curylo, M, Canton, T, Dalya, G, Dana, A, Daneshgaran-Bajastani, L, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Delfavero, M, De Lillo, N, Del Pozzo, W, Demarchi, L, D'Emilio, V, Demos, N, Dent, T, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M, Diaz-Ortiz, M, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Ducoin, J, Dupej, P, Durante, O, D'Urso, D, Dwyer, S, Easter, P, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, V, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Feng, F, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Fidecaro, F, Fiori, I, Fiorucci, D, Fishbach, M, Fisher, R, Fittipaldi, R, Fitz-Axen, M, Fiumara, V, Flaminio, R, Floden, E, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fritschel, P, Frolov, V, Fronze, G, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Galaudage, S, Ganapathy, D, Gaonkar, S, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Gibson, D, Gier, C, Gill, K, Glanzer, J, Gniesmer, J, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonzalez, G, Gopakumar, A, Gossan, S, Gosselin, M, Gouaty, R, Grace, B, Grado, A, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Griggs, H, Grignani, G, Grimaldi, A, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guidi, G, Guimaraes, A, Guixe, G, Gulati, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hasskew, R, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heinze, J, Heitmann, H, Hellman, F, Hello, P, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Heurs, M, Hild, S, Hinderer, T, Hoback, S, Hochheim, S, Hofgard, E, Hofman, D, Holgado, A, Holland, N, Holt, K, Holz, D, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Huang, Y, Hubner, M, Huerta, E, Huet, D, Hughey, B, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Idzkowski, B, Iess, A, Inchauspe, H, Ingram, C, Intini, G, Isac, J, Isi, M, Iyer, B, Jacqmin, T, Jadhav, S, James, A, Jani, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jiang, J, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kapadia, S, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Kefelian, F, Keitel, D, Keivani, A, Kennedy, R, Key, J, Khadka, S, Khalili, F, Khan, I, Khan, S, Khan, Z, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, G, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kovalam, M, Kozak, D, Kringel, V, Krishnendu, N, Krolak, A, Krupinski, N, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Lackey, B, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, La Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Leroy, N, Letendre, N, Levin, Y, Li, A, Li, J, Li, K, Li, T, Li, X, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, J, Liu, X, Llorens-Monteagudo, M, Lo, R, Lockwood, A, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Luck, H, Lumaca, D, Lundgren, A, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magana-Sandoval, F, Magee, R, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, V, Martynov, D, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Mavalvala, N, Maynard, E, Mccann, J, Mccarthy, R, Mcclelland, D, Mccormick, S, Mcculler, L, Mcguire, S, Mcisaac, C, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Meadors, G, Mehmet, M, Mehta, A, Villa, E, Melatos, A, Mendell, G, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merritt, J, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P, Meylahn, F, Mhaske, A, Miani, A, Miao, H, Michaloliakos, I, Michel, C, Middleton, H, Milano, L, Miller, A, Millhouse, M, Mills, J, Milotti, E, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Mo, G, Mogushi, K, Mohapatra, S, Mohite, S, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moraru, D, Morawski, F, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C, Mozzon, S, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E, Murray, P, Nagar, A, Nardecchia, I, Naticchioni, L, Nayak, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nichols, D, Nichols, S, Nissanke, S, Nocera, F, Noh, M, North, C, Nothard, D, Nuttall, L, Oberling, J, O'Brien, B, Oganesyan, G, Ogin, G, Oh, J, Oh, S, Ohme, F, Ohta, H, Okada, M, Oliver, M, Olivetto, C, Oppermann, P, Oram, R, O'Reilly, B, Ormiston, R, Ortega, L, O'Shaughnessy, R, Ossokine, S, Osthelder, C, Ottaway, D, Overmier, H, Owen, B, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, H, Panda, P, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patricelli, B, Payne, E, Pearlstone, B, Pechsiri, T, Pedersen, A, Pedraza, M, Pele, A, Penn, S, Perego, A, Perez, C, Perigois, C, Perreca, A, Perries, S, Petermann, J, Pfeiffer, H, Phelps, M, Phukon, K, Piccinni, O, Pichot, M, Piendibene, M, Piergiovanni, F, Pierro, V, Pillant, G, Pinard, L, Pinto, I, Piotrzkowski, K, Pirello, M, Pitkin, M, Plastino, W, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, G, Prokhorov, L, Punturo, M, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Rafferty, H, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Rettegno, P, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, N, Robinet, F, Rocchi, A, Rodriguez-Soto, R, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romero-Shaw, I, Romie, J, Rose, C, Rose, D, Rose, K, Rosinska, D, Rosofsky, S, Ross, M, Rowan, S, Rowlinson, S, Roy, P, Roy, S, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salafia, O, Salconi, L, Saleem, M, Samajdar, A, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sanders, J, Santiago, K, Santos, E, Sarin, N, Sassolas, B, Sathyaprakash, B, Sauter, O, Savage, R, Savant, V, Sawant, D, Sayah, S, Schaetzl, D, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R, Schonbeck, A, Schreiber, E, Schulte, B, Schutz, B, Schwarm, O, Schwartz, E, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, D, Shaffer, T, Shahriar, M, Sharma, A, Sharma, P, Shawhan, P, Shen, H, Shikauchi, M, Shink, R, Shoemaker, D, Shukla, K, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singha, A, Singhal, A, Sintes, A, Sipala, V, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smetana, J, Smith, J, Smith, R, Somala, S, Son, E, Soni, S, Sorazu, B, Sordini, V, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A, Spera, M, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, D, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stocks, D, Stops, D, Stover, M, Strain, K, Stratta, G, Strunk, A, Sturani, R, Stuver, A, Sudhagar, S, Sudhir, V, Summerscales, T, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Swinkels, B, Szczepanczyk, M, Tacca, M, Tait, S, Talbot, C, Tanasijczuk, A, Tanner, D, Tao, D, Tapai, M, Tapia, A, Martin, E, Tasson, J, Taylor, R, Tenorio, R, Terkowski, L, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tinsman, C, Saravanan, T, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, C, Tosta e Melo, I, Toyra, D, Trail, E, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Trovato, A, Trudeau, R, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tsutsui, T, Turconi, M, Ubhi, A, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Utina, A, Vahlbruch, H, Vajente, G, Valdes, G, Valentini, M, Vallisneri, M, van Bakel, N, van Beuzekom, M, van den Brand, J, Van Den Broeck, C, Vander-Hyde, D, van der Schaaf, L, Van Heijningen, J, van Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Veske, D, Vetrano, F, Vicere, A, Viets, A, Vinciguerra, S, Vine, D, Vinet, J, Vitale, S, Vivanco, F, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, S, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, R, Williamson, A, Willis, J, Willke, B, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Wong, C, Wright, J, Wu, D, Wysocki, D, Xiao, L, Yamamoto, H, Yang, L, Yang, Y, Yang, Z, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Zadrozny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhao, G, Zhou, M, Zhou, Z, Zhu, X, Zimmerman, A, Zucker, M, Zweizig, J, IoP (FNWI), Faculty of Science, Gravitation and Astroparticle Physics Amsterdam, Other Research IHEF (IoP, FNWI), Astroparticle Physics (IHEF, IoP, FNWI), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), The LIGO Scientific Collaboration, The Virgo Collaboration, Arene, M., Becsy, B., Bustillo, J. C., Diaz, J. C., Castaneda, J., Cavaglia, M., Cerda-Duran, P., Cieslar, M., Cordero-Carrion, I., Canton, T. D., Dalya, G., D'Angelo, B., D'Antonio, S., Deleglise, S., D'Emilio, V., Diaz, M. C., D'Urso, D., Fronze, G., Garcia-Quiros, C., Ghosh, A., Gonzalez, G., Guixe, G., Hubner, M. T., Isac, J. -M., Kefelian, F., Kim, C., Krolak, A., Kumar, R., Luck, H., Hernandez, I. M., Magana-Sandoval, F., Marka, S., Marka, Z., Villa, E. M., Mukherjee, A., Muniz, E. A., O'Brien, B. D., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Perigois, C., Perries, S., Pinto, I., Purrer, M., Rana, J., Rosinska, D., Roy, S., Schonbeck, A., Szczepanczyk, M. J., Tapai, M., Martin, E. N. T. S., Torres-Forne, A., Toyra, D., Vasuth, M., Vicere, A., Vivanco, F. H., Wessels, P., Yu, H., Zadrozny, A. K., and Zadrozny, A.

Subjects
Technology, Gravitational Waves, Open Data, O1, O2, LIGO, Virgo, Astronomy, Strain measurement, Gravitational Wave, open data, Data representation and management, Gravitational Waves, GWOSC, Scientific databases, gravitational waves, 01 natural sciences, General Relativity and Quantum Cosmology, Software, Documentation, DESIGN, Open Data, Computer software, Data products, LIGO, QC, 12-AXIS VIBRATION ISOLATION, media_common, Settore FIS/01, 0303 health sciences, Gravitational effects, BINARY MERGERS, Computer Science Applications, Open data, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Open science, Astrophysics - Instrumentation and Methods for Astrophysics, data analysis method, gr-qc, media_common.quotation_subject, Real-time computing, FOS: Physical sciences, O2, PUBLIC ADVANCED LIGO, General Relativity and Quantum Cosmology (gr-qc), Gravity waves, programming, O1, 03 medical and health sciences, QA76.75-76.765, Dewey Decimal Classification::000 | Allgemeines, Wissenschaft::000 | Informatik, Wissen, Systeme::004 | Informatik, SDG 17 - Partnerships for the Goals, GWOSC, Scientific databases, Data representation and management, Gravitational Waves, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, GRAVITATIONAL-WAVE CATALOG, Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, Astrophysique, 030304 developmental biology, Science & Technology, business.industry, Gravitational wave, Virgo, gravitational radiation, RCUK, Strain data, Data-quality information, Computer Science, Software Engineering, gravitational radiation detector, detector: sensitivity, Scientific database, monitoring, VIRGO, Sky, gravitational radiation: emission, Computer Science, ddc:004, business, astro-ph.IM
Abstract

Abbot, Rich, et al. (Virgo and MAGIC Collaboration), Advanced LIGO and Advanced Virgo are monitoring the sky and collecting gravitational-wave strain data with sufficient sensitivity to detect signals routinely. In this paper we describe the data recorded by these instruments during their first and second observing runs. The main data products are gravitational-wave strain time series sampled at 16384 Hz. The datasets that include this strain measurement can be freely accessed through the Gravitational Wave Open Science Center at http://gw-openscience.org, together with data-quality information essential for the analysis of LIGO and Virgo data, documentation, tutorials, and supporting software., The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources.

Published
2021

18. NEPSC2, the North Ecliptic Pole SCUBA-2 survey: 850-μm map and catalogue of 850-μm selected sources over 2 deg2

Author

Glenn J. White, Hyunjong Seo, T. Goto, Hideo Matsuhara, L. Barrufet, Stephen Serjeant, M. P. Koprowski, Harriet Parsons, Yoshiki Toba, Michał J. Michałowski, Seong Jin Kim, Albert K. H. Kong, Chris Pearson, Dongseob Lee, Woong-Seob Jeong, Lucia Marchetti, Tetsuya Hashimoto, Hyunjin Shim, Douglas Scott, Ho Seong Hwang, Hyung Mok Lee, Linhua Jiang, Scott Chapman, Yiping Ao, Minjin Kim, Christopher J. Conselice, Thomas R. Greve, Yeonsik Kim, Myungshin Im, and David L. Clements

Subjects
MU-M, Ecliptic pole, DUST, 01 natural sciences, Cosmology, IDENTIFICATIONS, STAR-FORMATION, Observatory, 0103 physical sciences, galaxies [submillimetre], Source counts, 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, evolution [galaxies], POPULATION, Physics, DEGREE EXTRAGALACTIC SURVEY, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, starburst [galaxies], ALMA SURVEY, Astronomy, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, photometry [galaxies], DEEP-FIELD-SOUTH, Millimeter, COSMOLOGY LEGACY SURVEY
Abstract

We present an 850-μm mosaic map and extracted catalogue of submillimetre sources in the extended North Ecliptic Pole (NEP) region over about 2 deg2. The 850-μm map is constructed using newly obtained observations by SCUBA-2 at the East Asian Observatory’s James Clerk Maxwell Telescope, carried out using the observatory’s large programme opportunities. The recent 850-μm survey has extended the submillimetre data coverage by almost a factor of 4 compared to previous surveys, with a depth of σrms = 1.0–2.3 mJy beam−1. The catalogue contains 549 sources selected above a significance level of 4σ, where the false-detection rate is 10 per cent; a higher threshold of 4.5σ is required in order to achieve a false-detection rate below 3 per cent, which results in 342 sources being selected. Despite the large spatial variation of the noise, the deboosted flux density of sources is comparable to results from the SCUBA-2 Cosmology Legacy Survey (S2CLS), which covered the central 0.6 deg2 of our survey area with better sensitivity. We construct the source counts at 850 μm, finding results in agreement with other 850-μm surveys in cosmological blank fields over S850 = 4–15 mJy. We find a slight excess of bright galaxies (S850 > 15 mJy), which can be considered to be at ɀphot = 2–4. The 850-μm data adds valuable long-wavelength information to mid-infrared-selected sources from the AKARI NEP-deep and NEP-wide surveys, which will be helpful in preparing for future near-infrared to millimetre wavelength observations in the NEP region. Our 850-μm mosaic map and source catalogue will be made publicly available.

Published
2020

21. AKARI SPECTROSCOPY OF QUASARS AT 2.5 - 5 MICRON

Author

Hyung Mok Lee, Qsong Team, Takao Nakagawa, Myungshin Im, Ji-Hoon Kim, Hyunsung David Jun, Dohyeong Kim, and Youichi Ohyama

Subjects
Physics, Luminous infrared galaxy, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, General Medicine, Astrophysics, Redshift, Black hole, Grism, Astrophysics::Earth and Planetary Astrophysics, Spectroscopy, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

Utilizing a unique capability of AKARI that allows deep spectroscopy at 2.5- 5.0μm, we performed a spectroscopy study of more than 200 quasars through one of the AKARI mission programs, QSONG (Quasar Spectroscopic Observation with NIR Grism). QSONG targeted 155 high redshift (3:3 3:3. The low redshift part of QSONG is geared to uncover the rest-frame 2.5-5.0μm spectral features of active galactic nuclei to gain useful information such as the dust-extinction-free black hole mass estimators based on the Brackett lines and the temperatures of the hot dust torus. We outline the program strategy, and present some of the scientific highlights from QSONG, including the detection of the Hα line from a quasar at z > 4:5 which indicates a rigorous growth of black holes in the early universe, and the Brβ-based black hole mass estimators and the hot dust temperatures (~1100 K) of low redshift AGNs.

Published
2017

22. Analytic Keplerian-type parametrization for general spinning compact binaries with the leading order spin-orbit interaction

Author

Hyung Mok Lee and G. Cho

Subjects
Physics, media_common.quotation_subject, Binary number, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Mass ratio, Gauge (firearms), General Relativity and Quantum Cosmology, Orbit, Classical mechanics, Eccentricity (behavior), Spin (physics), Parametrization, Spinning, media_common
Abstract

We derive a fully analytic Keplerian-type parametrization solution to conservative motion of spinning binary in ADM gauge. This solution is able to describe three dimensional motion of binaries of arbitrary eccentricity, mass ratio and initial configuration of spin angular momentum up to the leading order of post-Newtonian(PN) approximation and a linear order in spin. Based on our results waveforms can be quickly computed with high accuracy.

Published
2019
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24. Long Journey toward the Detection of Gravitational Waves and New Era of Gravitational Wave Astrophysics

Author

Hyung Mok Lee

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), General relativity, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, 01 natural sciences, Gravitational-wave astronomy, LIGO, Black hole, Neutron star, General Relativity and Quantum Cosmology, 0103 physical sciences, Moment (physics), 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics)
Abstract

The gravitational waves were detected directly for the first time on September 14, 2015 by two LIGO detectors at Livingston, Louisiana and Hanford, Washington, USA. Careful analysis revealed that this signal was produced by the last moment of inspiral and merger of two black holes that have been orbiting each other. Since the first detection, several other gravitational wave sources, including one neutron star merger event in August 201,7 have been observed by the LIGO together with Virgo. This article provides a very brief overview of the history toward the understanding the nature of gravitational waves, detectors, types of sources and achievements of the gravitational wave detectors. We then discuss astrophysical implications of the recent detections of black hole and neutron star binaries and provide short term and long term prospects of gravitational wave astronomy., 38 pages, 5 figures, Review article for the Journal of the Korean Physical Society

Published
2018

28. Gravitational-wave Capture in Spinning Black Hole Encounters

Author

Yeong-Bok Bae, Hyung Mok Lee, and Gungwon Kang

Subjects
Physics, Angular momentum, 010504 meteorology & atmospheric sciences, General relativity, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Two-body problem, 01 natural sciences, Black hole, Numerical relativity, Star cluster, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

The orbits of two black holes (BHs) that are initially unbound can be transformed into bound orbits by emitting gravitational waves during close encounters in a star cluster, which is called gravitational-wave (GW) capture. The effects of spin of BHs on GW capture are investigated in the context of numerical relativity. The radiated energy during the encounter is dependent on the effective spin when the BHs have equal masses, as expected from post-Newtonian approximation. The strongest emission is produced when the spins of both BHs are anti-aligned to the orbital angular momentum in the case of fly-by encounters. But the opposite is true in the case of direct merging: the strongest emission comes from the BHs with aligned spins to the orbital angular momentum. The fraction of direct merging among the GW captures increases in proportion to v 4/7, assuming the uniform distribution of pericenter distances in the encounters, where v is the velocity dispersion of the cluster, which means about 5% of GW capture leads to the direct merging for star clusters with v = 150 km s−1.

Published
2020

29. Gravitational waves from compact binaries in post-Newtonian accurate hyperbolic orbits

Author

Achamveedu Gopakumar, G. Cho, Hyung Mok Lee, M. Haney, and University of Zurich

Subjects
Harmonic coordinates, Orbital elements, Physics, Angular momentum, Physics and Astronomy (miscellaneous), 530 Physics, 010308 nuclear & particles physics, Gravitational wave, Analytic continuation, FOS: Physical sciences, 10192 Physics Institute, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Specific orbital energy, Classical mechanics, 0103 physical sciences, Orbital motion, Astrophysics::Earth and Planetary Astrophysics, 3101 Physics and Astronomy (miscellaneous), 010306 general physics, Parametric statistics
Abstract

We derive from first principles a third post-Newtonian (3PN) accurate Keplerian-type parametric solution to describe PN accurate dynamics of nonspinning compact binaries in hyperbolic orbits. Orbital elements and functions of the parametric solution are obtained in terms of the conserved orbital energy and angular momentum in both Arnowitt-Deser-Misner-type and modified harmonic coordinates. Elegant checks are provided that include a modified analytic continuation prescription to obtain our independent hyperbolic parametric solution from its eccentric version. A prescription to model gravitational wave polarization states for hyperbolic compact binaries experiencing 3.5PN accurate orbital motion is presented that employs our 3PN accurate parametric solution.

Published
2018

30. Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era

Author

Michael Boyle, Nick Demos, Chaitanya Afle, Daniel A. Hemberger, Anuradha Gupta, Sanjit Mitra, P. Kumar, Han Gil Choi, B. U. Gadre, Geoffrey Lovelace, Harald P. Pfeiffer, Mark A. Scheel, Hyung Mok Lee, Lawrence E. Kidder, and Béla Szilágyi

Subjects
Physics, Supermassive black hole, Angular momentum, 010308 nuclear & particles physics, Gravitational wave, gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, LIGO, General Relativity and Quantum Cosmology, Computational physics, Black hole, Numerical relativity, 0103 physical sciences, Precession, Chirp, 010306 general physics
Abstract

In this paper, we test the performance of templates in detection and characterization of Spin-orbit resonant (SOR) binaries. We use precessing SEOBNRv3 waveforms as well as {\it four} numerical relativity (NR) waveforms to model GWs from SOR binaries and filter them through IMRPhenomD, SEOBNRv4 (non-precessing) and IMRPhenomPv2 (precessing) approximants. We find that IMRPhenomD and SEOBNRv4 recover only $\sim70\%$ of injections with fitting factor (FF) higher than 0.97 (or 90\% of injections with ${\rm FF} >0.9$).However, using the sky-maxed statistic, IMRPhenomPv2 performs magnificently better than their non-precessing counterparts with recovering $99\%$ of the injections with FFs higher than 0.97. Interestingly, injections with $\Delta \phi = 180^{\circ}$ have higher FFs ($\Delta \phi$ is the angle between the components of the black hole spins in the plane orthogonal to the orbital angular momentum) as compared to their $\Delta \phi =0^{\circ}$ and generic counterparts. This implies that we will have a slight observation bias towards $\Delta \phi=180^{\circ}$ SORs while using non-precessing templates for searches. All template approximants are able to recover most of the injected NR waveforms with FFs $>0.95$. For all the injections including NR, the error in estimating chirp mass remains below $, Comment: 27 pages, 15 figures. Abstract shortened due to word limit

Published
2018

32. Distance and properties of NGC 4993 as the host galaxy of a gravitational wave source, GW170817

Author

Myungshin Im, Seung-Lee Kim, Gu Lim, Hyung Mok Lee, Yongmin Yoon, Joonho Kim, Eleonora Troja, Jongwan Ko, Chung-Uk Lee, Seong-Kook Lee, Changsu Choi, and Hyunjin Shim

Subjects
Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Star formation, Gravitational wave, Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, LIGO, Black hole, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Recently, the optical counterpart of a gravitational wave source GW170817 has been identified in NGC 4993 galaxy. Together with evidence from observations in electromagnetic waves, the event has been suggested as a result of a merger of two neutron stars. We analyze the multi-wavelength data to characterize the host galaxy property and its distance to examine if the properties of NGC 4993 are consistent with this picture. Our analysis shows that NGC 4993 is a bulge-dominated galaxy with reff ~ 2-3 kpc and the Sersic index of n = 3-4 for the bulge component. The spectral energy distribution from 0.15 to 24 micron indicates that this galaxy has no significant ongoing star formation, the mean stellar mass of (0.3 - 1.2) times 10^11 Msun,the mean stellar age greater than ~3 Gyr, and the metallicity of about 20% to 100% of solar abundance. Optical images reveal dust lanes and extended features that suggest a past merging activity. Overall, NGC 4993 has characteristics of normal, but slightly disturbed elliptical galaxies. Furthermore, we derive the distance to NGC 4993 with the fundamental plane relation using 17 parameter sets of 7 different filters and the central stellar velocity dispersion from literature, finding an angular diameter distance of 37.7 +- 8.7 Mpc. NGC 4993 is similar to some host galaxies of short gamma-ray bursts but much different from those of long gamma-ray bursts, supporting the picture of GW170817 as a result of a merger of two NSs., 7 pages, 2 figures, 3 tables, accepted for publication in ApJL

Published
2017

33. Black hole binaries in galactic nuclei and gravitational wave sources

Author

Jongsuk Hong and Hyung Mok Lee

Subjects
Physics, X-ray binary, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, LIGO, Black hole, Astrophysics - Solar and Stellar Astrophysics, Binary black hole, Space and Planetary Science, Intermediate-mass black hole, Astrophysics of Galaxies (astro-ph.GA), Stellar black hole, Spin-flip, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

Stellar black hole (BH) binaries are one of the most promising gravitational wave (GW) sources for GW detection by the ground-based detectors. Nuclear star clusters (NCs) located at the centre of galaxies are known to harbour massive black holes (MBHs) and to be bounded by a gravitational potential by other galactic components such as the galactic bulge. Such an environment of NCs provides a favourable conditions for the BH-BH binary formation by the gravitational radiation capture due to the high BH number density and velocity dispersion. We carried out detailed numerical study of the formation of BH binaries in the NCs using a series of N-body simulations for equal-mass cases. There is no mass segregation introduced. We have derived scaling relations of the binary formation rate with the velocity dispersion of the stellar system beyond the radius of influence and made estimates of the rate of formation of black hole binaries per unit comoving volume and thus expected detection rate by integrating the binary formation rate over galaxy population within the detection distance of the advanced detectors. We find that the overall formation rates for BH-BH binaries per NC is 10^(-10)/yr for the Milky-Way-like galaxies and weakly dependent on the mass of MBH as M^(3/28). We estimate the detection rate of 0.02-14/yr for advanced LIGO/Virgo considering several factors such as the dynamical evolution of NCs, the variance of the number density of stars and the mass range of MBH giving uncertainties., Comment: 17 pages, 19 figures, 2 tables, published in MNRAS

Published
2015

34. Black Hole Binaries Dynamically Formed in Globular Clusters

Author

Krzysztof Belczynski, Chunglee Kim, Hyung Mok Lee, Yeong Bok Bae, and Dawoo Park

Subjects
Metallicity, Population, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, Cluster (physics), education, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, Mass ratio, Astrophysics - Astrophysics of Galaxies, Black hole, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena
Abstract

We investigate properties of black hole (BH) binaries formed in globular clusters via dynamical processes, using direct N-body simulations. We pay attention to effects of BH mass function on the total mass and mass ratio distributions of BH binaries ejected from clusters. Firstly, we consider BH populations with two different masses in order to learn basic differences from models with single-mass BHs only. Secondly, we consider continuous BH mass functions adapted from recent studies on massive star evolution in a low metallicity environment, where globular clusters are formed. In this work, we consider only binaries that are formed by three-body processes and ignore stellar evolution and primordial binaries for simplicity. Our results imply that most BH binary mergers take place after they get ejected from the cluster. Also, mass ratios of dynamically formed binaries should be close to one or likely to be less than 2:1. Since the binary formation efficiency is larger for higher-mass BHs, it is likely that a BH mass function sampled by gravitational-wave observations would be weighed toward higher masses than the mass function of single BHs for a dynamically formed population. Applying conservative assumptions regarding globular cluster populations such as small BH mass fraction and no primordial binaries, the merger rate of BH binaries originated from globular clusters is estimated to be at least 6.5 per yr per Gpc^3. Actual rate can be up to more than several times of our conservative estimate., 11 pages, 2 tables, 8 figures, accepted for publication in MNRAS after minor revisions

Published
2017

35. Galaxies on diet: feedback signatures in radio-AGN host galaxies

Author

Hideo Matsuhara, Myungshin Im, Stephen Serjeant, Matthew A. Malkan, Ji-Hoon Kim, Tomogotsu Goto, Nagisa Oi, Marios Karouzos, Seong-Jin Kim, Hitoshi Hanami, Hyung Mok Lee, Toshinobu Takagi, Kensuke Wada, Ángel Ruiz, Hyunjin Shim, Kazumi Murata, Markos Trichas, Chris Pearson, Yiseul Jeon, Takehiko Wada, Glenn J. White, and Youichi Ohyama

Subjects
Physics, Luminous infrared galaxy, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Quasar, General Medicine, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Peculiar galaxy, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, Disc, Lenticular galaxy, Astrophysics::Galaxy Astrophysics
Abstract

There exists strong evidence supporting the co-evolution of central supermassive black holes and their host galaxies; however it is still under debate how such a relation comes about and whether it is relevant for all or only a subset of galaxies. An important mechanism connecting AGN to their host galaxies is AGN feedback, potentially heating up or even expelling gas from galaxies. AGN feedback may hence be responsible for the eventual quenching of star formation and halting of galaxy growth. A rich multi-wavelength dataset ranging from the X-ray regime (Chandra), to far-IR (Herschel), and radio (WSRT) is available for the North Ecliptic Pole field, most notably surveyed by the AKARI infrared space telescope, covering a total area on the sky of 5.4 sq. degrees. We investigate the star formation properties and possible signatures of radio feedback mechanisms in the host galaxies of 237 radio sources below redshift z

Published
2017

36. The X-ray counterpart to the gravitational-wave event GW170817

Author

Eleonora Troja, R. Sanchez-Ramirez, Oleg Korobkin, P. D'Avanzo, Alexander Kutyrev, H. G. Khandrika, Stefano Covino, Y.Y. Yoon, R. E. Ryan, Hyung Mok Lee, G. Lim, H. van Eerten, Myungshin Im, Ryan Wollaeger, Nathaniel R. Butler, Sylvain Veilleux, Roberto Ricci, Luigi Piro, Changsu Choi, A. Y. Lien, Christopher J. Fontes, M. H. Wieringa, Selyeong Lee, Seung-Lee Kim, C.-U. Lee, William H. Lee, Alan M. Watson, O. D. Fox, J. H. Kim, Chris L. Fryer, S. B. Cenko, J. Becerra González, J. M. Burgess, T. Sakamoto, and ITA

Subjects
astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kilonova, 01 natural sciences, Neutron star, 13. Climate action, Coincident, 0103 physical sciences, Outflow, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics::Galaxy Astrophysics, Radio wave
Abstract

A long-standing paradigm in astrophysics is that collisions- or mergers- of two neutron stars (NSs) form highly relativistic and collimated outflows (jets) powering gamma-ray bursts (GRBs) of short (< 2 s) duration. However, the observational support for this model is only indirect. A hitherto outstanding prediction is that gravitational wave (GW) events from such mergers should be associated with GRBs, and that a majority of these GRBs should be off-axis, that is, they should point away from the Earth. Here we report the discovery of the X-ray counterpart associated with the GW event GW170817. While the electromagnetic counterpart at optical and infrared frequencies is dominated by the radioactive glow from freshly synthesized r-process material in the merger ejecta, known as kilonova, observations at X-ray and, later, radio frequencies exhibit the behavior of a short GRB viewed off-axis. Our detection of X-ray emission at a location coincident with the kilonova transient provides the missing observational link between short GRBs and GWs from NS mergers, and gives independent confirmation of the collimated nature of the GRB emission., 38 pages, 10 figures, Nature, in press

Published
2017

37. Compact binaries ejected from globular clusters as gravitational wave sources

Author

Yeong Bok Bae, Chunglee Kim, and Hyung Mok Lee

Subjects
Physics, Gravitational wave, Astronomy, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Escape velocity, Astrophysics, Galaxy, Black hole, Space and Planetary Science, Globular cluster, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Gamma-ray burst, Astrophysics::Galaxy Astrophysics
Abstract

Performing N-body simulations, we examine the dynamics of BH-BH (10 Msun each) and NS-NS (1.4 Msun each) binaries formed in a cluster and its implications for gravitational wave detection. A significant fraction of compact binaries are ejected from a globular cluster after core collapse. Among the total number of ejected compact objects, 30 per cent of them are in binaries. Merging time-scales of ejected binaries, which depend on the cluster's velocity dispersion, are in some cases shorter than the age of the universe. During the merging event, these dynamically formed compact mergers are expected to produce gravitational waves that can be detectable by the advanced ground-based interferometers. Based on our reference assumptions, merger rates of ejected BH-BH and NS-NS binaries per globular cluster are estimated to be 2.5 and 0.27 per Gyr, respectively. Assuming the spatial density of globular clusters to be 8.4 h^3 clusters Mpc^-3 and extrapolating the merger rate estimates to the horizon distance of the advanced LIGO-Virgo network, we expect the detection rates for BH-BH and NS-NS binaries with cluster origin are to be 15 and 0.024 yr^-1, respectively. We find out that some of the dynamically formed binaries are ejected with a large escape velocity. They can be responsible for short gamma-ray bursts whose locations are far from host galaxies.

Published
2014

38. Comparative study between N-body and Fokker–Planck simulations for rotating star clusters – II. Two-component models

Author

Eunhyeuk Kim, Rainer Spurzem, Hyung Mok Lee, and Jongsuk Hong

Subjects
Physics, Angular momentum, Star cluster, Space and Planetary Science, Total angular momentum quantum number, Cluster (physics), Astronomy and Astrophysics, Atomic physics, Rotation, Instability, Equipartition theorem, Rotational energy
Abstract

To understand the effects of the initial rotation on the evolution of the tidally limited clusters with mass spectrum, we have performed N-body simulations of the clusters with different initial rotations and compared the results with those of the Fokker-Planck (FP) simulations. We confirmed that the cluster evolution is accelerated by not only the initial rotation but also the mass spectrum. For the slowly rotating models, the time evolutions of mass, energy and angular momentum show good agreements between N-body and FP simulations. On the other hand, for the rapidly rotating models, there are significant differences between these two approaches at the early stage of the evolutions because of the development of bar instability in N-body simulations. The shape of the cluster for N-body simulations becomes tri-axial or even prolate, which cannot be produced by the 2-dimensional FP simulations. The total angular momentum and the total mass of the cluster decrease rapidly while bar-like structure persists. After the rotational energy becomes smaller than the critical value for the bar instability, the shape of the cluster becomes nearly axisymmetric again, and follows the evolutionary track predicted by the FP equation. We have confirmed again that the energy equipartiton is not completely achieved when M2/M1(m2>/m1)^(3/2) > 0.16. By examining the angular momentum at each mass component, we found that the exchange of angular momentum between different mass components occurs, similar to the energy exchange leading to the equipartition.

Published
2013

39. A fully general relativistic numerical simulation code for spherically symmetric matter

Author

Hyung Mok Lee, G. Kang, Inyong Cho, and Dong-Ho Park

Subjects
Physics, Computer simulation, Astrophysics::High Energy Astrophysical Phenomena, Isotropy, General Physics and Astronomy, Perfect fluid, Eulerian path, General Relativity and Quantum Cosmology, Stars, symbols.namesake, Riemann hypothesis, Classical mechanics, Spatial reference system, symbols, Blast wave
Abstract

We present a fully general relativistic open-source code that can be used for simulating a system of spherically symmetric perfect fluid matter. It is based on the Arnowitt-Deser-Misner 3+1 formalism with maximal slicing and isotropic spatial coordinates. For hydrodynamic matter High Resolution Shock Capturing (HRSC) schemes with a monotonized central-difference limiter and approximated Riemann solvers are used in the Eulerian viewpoint. The accuracy and the convergence of our numerical code are verified by performing several test problems. These include a relativistic blast wave, relativistic spherical accretion of matter into a black hole, Tolman-Oppenheimer-Volkoff (TOV) stars and Oppenheimer-Snyder (OS) dust collapses. In particular, a dynamical code test is done for the OS collapse by explicitly performing numerical coordinate transformations between our coordinate 8system and the one used for the analytic solution. Finally, some TOV star solutions are presented for the Eddington-inspired Born-Infeld gravity theory.

Published
2013

40. A deep ATCA 20 cm radio survey of theAKARIDeep Field South near the South Ecliptic Pole

Author

Woong-Seob Jeong, David L. Clements, Takao Nakagawa, Chris Pearson, Shinki Oyabu, Stephen Serjeant, Sophia A. Khan, Katarzyna Małek, Toshinobu Takagi, Chris Sedgwick, Glenn J. White, Issei Yamamura, Mai Shirahata, Tomotsugu Goto, Hyung Mok Lee, Shuji Matsuura, Kotaro Kohno, Bunyo Hatsukade, Hideo Matsuhara, Sin'itirou Makiuti, and Hitoshi Hanami

Subjects
Physics, education.field_of_study, Hubble Deep Field, Population, Astronomy and Astrophysics, Ecliptic pole, Astrophysics, Galaxy, Redshift, law.invention, Luminosity, Telescope, Space and Planetary Science, law, Source counts, education
Abstract

The results of a deep 20 cm radio survey at 20 cm are reported of the AKARI Deep Field South (ADF-S) near the South Ecliptic Pole (SEP), using the Australia Telescope Compact Array telescope, ATCA. The survey has 1 sigma detection limits ranging from 18.7--50 microJy per beam over an area of ~1.1 sq degrees, and ~2.5 sq degrees to lower sensitivity. The observations, data reduction and source count analysis are presented, along with a description of the overall scientific objectives, and a catalogue containing 530 radio sources detected with a resolution of 6.2" x 4.9". The derived differential source counts show a pronounced excess of sources fainter than ~1 mJy, consistent with an emerging population of star forming galaxies. Cross-correlating the radio with AKARI sources and archival data we find 95 cross matches, with most galaxies having optical R-magnitudes in the range 18-24 mag, and 52 components lying within 1" of a radio position in at least one further catalogue (either IR or optical). We have reported redshifts for a sub-sample of our catalogue finding that they vary between galaxies in the local universe to those having redshifts of up to 0.825. Associating the radio sources with the Spitzer catalogue at 24 microns, we find 173 matches within one Spitzer pixel, of which a small sample of the identifications are clearly radio loud compared to the bulk of the galaxies. The radio luminosity plot and a colour-colour analysis suggest that the majority of the radio sources are in fact luminous star forming galaxies, rather than radio-loud AGN. There are additionally five cross matches between ASTE or BLAST submillimetre galaxies and radio sources from this survey, two of which are also detected at 90 microns, and 41 cross-matches with submillimetre sources detected in the Herschel HerMES survey Public Data release.

Published
2012

41. NORTH ECLIPTIC POLE WIDE SURVEY

Author

Hyung Mok Lee, Seong Jin Kim, and NEP-Wide Team NEP-Wide Team

Subjects
Physics, Luminous infrared galaxy, Stars, Infrared, Magnitude (astronomy), Astronomy, Ecliptic pole, General Medicine, Astrophysics, AB magnitude, Redshift, Galaxy
Abstract

The North Ecliptic Pole (NEP) Wide survey covered about 5.4 deg², a nearly circular area centered on the NEP, using nine passbands of InfraRed Camera (IRC). We present the photometric properties of the data sets, and the nature of the sources detected in this field. The number of detected sources varied according to the filter band: with about 109,000 sources in the NIR, about 20,000 sources in the MIR-S, and about 16,000 sources seen in the MIR-L channel. The 5¾ detection limits are about 21 mag in the NIR and 19.5 ? 18.5 mag in the MIR bands in terms of the AB magnitude. 50% completeness levels are about 19.8 mag at 3 ㎛, 18.6 mag at 9 ㎛, and 18 mag at 18 ㎛ band (in AB magnitude), respectively. In order to validate the detected sources, all of them are confirmed by matching tests with those in other bands. The ‘star-like’ sources, defined by the high stellarity and magnitude cut from the optical ancillary data, appear statistically to have a high probability of being stars. The nature of the various types of extragalactic sources in this field are discussed using the color-color diagrams of the NIR and MIR bands with the redshift tracks of galaxies providing useful guidelines.

Published
2012

42. A Study on the Effects of Service Quality of Financial Industry on Service Performance-Based on Mutual Savings Bank

Author

Jong-Weon Kim, Hyung-Mok Lee, and Sang-Shik Lee

Subjects
Service (business), Service quality, Customer retention, Customer advocacy, Customer Service Assurance, Service level objective, Service level requirement, Business, Service guarantee, Marketing
Abstract

Mutual savings banks have today met many difficulties because of various reasons. To overcome these difficulties, they have to change to be more customer centric and to adopt customer satisfaction management so that they can satisfy customers asking for diversified and professional service. This study aims to investigate the relationship between various dimensions of service quality and service performance such as customer satisfaction, customer trust, and repurchase intension. This study categorized service quality as interaction quality, outcome quality, and physical environment quality. Moreover, this study examined whether interest sensitivity and bank reputation had the moderating effects between service quality and service performance. The study results may provide practitioners and researchers in financial industry with some implications and guidelines for mutual savings banks` competitiveness.

Published
2012

43. Axially symmetric pseudo-Newtonian hydrodynamics code

Author

Hee Il Kim, Matthew W. Choptuik, Jinho Kim, and Hyung Mok Lee

Subjects
Physics, Partial differential equation, Finite volume method, Mathematical analysis, Method of lines, Astronomy and Astrophysics, 010103 numerical & computational mathematics, 01 natural sciences, Gravitational potential, Multigrid method, Space and Planetary Science, Ordinary differential equation, 0103 physical sciences, 0101 mathematics, Poisson's equation, Shock tube, 010303 astronomy & astrophysics
Abstract

We develop a numerical hydrodynamics code using a pseudo-Newtonian formulation that uses the weak field approximation for the geometry, and a generalized source term for the Poisson equation that takes into account relativistic effects. The code was designed to treat moderately relativistic systems such as rapidly rotating neutron stars. The hydrodynamic equations are solved using a finite volume method with High Resolution Shock Capturing (HRSC) techniques. We implement several different slope limiters for second order reconstruction schemes and also investigate higher order reconstructions. We use the method of lines (MoL) to convert the mixed spatial-time partial differential equations into ordinary differential equations (ODEs) that depend only on time. These ODEs are solved using 2nd and 3rd order Runge-Kutta methods. The Poisson equation for the gravitational potential is solved with a multigrid method. In order to confirm the validity of our code, we carry out four different tests including one and two dimensional shock tube tests, stationary star tests of both non-rotating and rotating models and radial oscillation mode tests for spherical stars. In the shock tube tests, the code shows good agreement with analytic solutions which include shocks, rarefaction waves and contact discontinuities. The code is found to be stable and accurate: for example, when solving a stationary stellar model the fractional changes in the maximum density, total mass, and total angular momentum per dynamical time are found to be $3 \times 10^{-6}$, $5 \times 10^{-7}$ and $2 \times 10^{-6}$, respectively. We also find that the frequencies of the radial modes obtained by the numerical simulation of the steady state star agree very well with those obtained by linear analysis.

Published
2012

44. Gravitational wave astrophysics, data analysis and multimessenger astronomy

Author

Eric-Olivier Le Bigot, Hyung Mok Lee, Xi-Long Fan, ZhangXi Lin, Xiangyu Guo, Vihan Pandey, Linqing Wen, Khun Sang Phukon, Zhihui Du, Suvadeep Bose, and Martin Hendry

Subjects
FOS: Computer and information sciences, General relativity, Gravitational wave, Computer science, FOS: Physical sciences, General Physics and Astronomy, Astronomy, General Relativity and Quantum Cosmology (gr-qc), Electromagnetic radiation, General Relativity and Quantum Cosmology, Gravitation, symbols.namesake, Computer Science - Distributed, Parallel, and Cluster Computing, Binary black hole, Physics - Data Analysis, Statistics and Probability, symbols, Chirp, Distributed, Parallel, and Cluster Computing (cs.DC), Einstein, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Infinite impulse response, Data Analysis, Statistics and Probability (physics.data-an)
Abstract

This paper reviews gravitational wave sources and their detection. One of the most exciting potential sources of gravitational waves are coalescing binary black hole systems. They can occur on all mass scales and be formed in numerous ways, many of which are not understood. They are generally invisible in electromagnetic waves, and they provide opportunities for deep investigation of Einstein's general theory of relativity. Sect. 1 of this paper considers ways that binary black holes can be created in the universe, and includes the prediction that binary black hole coalescence events are likely to be the first gravitational wave sources to be detected. The next parts of this paper address the detection of chirp waveforms from coalescence events in noisy data. Such analysis is computationally intensive. Sect. 2 reviews a new and powerful method of signal detection based on the GPU-implemented summed parallel infinite impulse response filters. Such filters are intrinsically real time alorithms, that can be used to rapidly detect and localise signals. Sect. 3 of the paper reviews the use of GPU processors for rapid searching for gravitational wave bursts that can arise from black hole births and coalescences. In sect. 4 the use of GPU processors to enable fast efficient statistical significance testing of gravitational wave event candidates is reviewed. Sect. 5 of this paper addresses the method of multimessenger astronomy where the discovery of electromagnetic counterparts of gravitational wave events can be used to identify sources, understand their nature and obtain much greater science outcomes from each identified event.

Published
2015

45. Infrared luminosity functions of AKARI Sloan Digital Sky Survey galaxies

Author

Stephen Serjeant, Takehiko Wada, Chris Pearson, Shinki Oyabu, Hanae Inami, Hyung Mok Lee, Chris Sedgwick, David B. Sanders, Emeric Le Floc, Matthew A. Malkan, Tsutomu T. Takeuchi, Hideo Matsuhara, Daisuke Ishihara, Chisato Yamauchi, Woong-Seob Jeong, Takao Nakagawa, Stephane Arnouts, Tomotsugu Goto, and Toshinobu Takagi

Subjects
Luminous infrared galaxy, Physics, Hubble Deep Field, Infrared, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Luminosity, Photometry (optics), Space and Planetary Science, Sky, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract

By cross-correlating AKARI all sky survey in 6 infrared (IR) bands (9, 18, 65, 90, 140, and 160�m ) with the SDSS galaxies, we identified 2357 infrared galaxie s with a spectroscopic redshift. This is not just one of the largest samples of local IR galaxies, but AKARI provides crucial FIR bands in accurately measuring galaxy SED across the peak of the dust emission at > 100�m . By fitting modern IR SED models to the AKARI photometry, we measured the total infrared luminosity (LIR) of individual galaxies. Using this LIR, we constructed the luminosity functions of infrared galaxies at a median redshift of z=0.031. The LF agrees well with that at z=0.0082 (the RBGS), showing smooth and continuous evolution toward higher redshift LFs measured in the AKARI NEP deep field. By integrating the IR LF weighted by LIR, we measured the local cosmic IR luminosity density of IR= (3.8 +5.8

Published
2011

46. Equilibrium and dynamical evolution of a self-gravitating system embedded in a potential well

Author

Hyung Mok Lee, Jongsuk Hong, and Ilsang Yoon

Subjects
Thermal equilibrium, Physics, business.industry, Dark matter, Velocity dispersion, Astronomy and Astrophysics, Mechanics, Astrophysics, Kinetic energy, Isothermal process, Space and Planetary Science, Boundary value problem, Density contrast, business, Thermal energy
Abstract

Isothermal and self-gravitating systems bound by non-conducting and conducting walls are known to be unstable if the density contrast between the center and the boundary exceeds critical values. We investigate the equilibrium and dynamical evolution of isothermal and self-gravitating system embedded in potential well, which can be the situation of many astrophysical objects such as the central parts of the galaxies, or clusters of galaxies with potential dominated by dark matter, but is still limited to the case where the potential well is fixed during the evolution. As the ratio between the depth of surrounding potential well and potential of embedded system becomes large, the potential well becomes effectively the same boundary condition as conducting wall, which behaves like a thermal heat bath. We also use the direct N-body simulation code, NBODY6 to simulate the dynamical evolution of stellar system embedded in potential wells and propose the equilibrium models for this system. In deep potential well, which is analogous to the heat bath with high temperature, the embedded self-gravitating system is dynamically hot, and loosely bound or can be unbound since the kinetic energy increases due to the heating by the potential well. On the other hand, the system undergoes core collapse by self-gravity when potential well is shallow. Binary heating can stop the collapse and leads to the expansion, but the evolution is very slow because the potential as a heat bath can absorb the energy generated by the binaries. The system can be regarded as quasi-static. Density and velocity dispersion profiles from the N-body simulations in the final quasi-equilibrium state are similar to our equilibrium models assumed to be in thermal equilibrium with the potential well.

Published
2011

47. Introduction to AMUSES: AKARI survey with a window of opportunity

Author

Hyung Mok Lee, Myungshin Im, Myung Gyoon Lee, and Ji Hoon Kim

Subjects
Physics, Infrared, Star formation, Infrared wavelength, General Engineering, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Spectral line, Redshift, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Spectroscopy, Astrophysics::Galaxy Astrophysics
Abstract

With advancement of infrared space telescopes during the past decade, infrared wavelength regime has been a focal point to study various properties of galaxies with respect to evolution of galaxies. Polycyclic Aromatic Hydrocarbons (PAHs) have emerged as one of the most important features since these features dominate the mid-infrared spectra of galaxies. These PAH features provide a great handle to calibrate star formation rates and diagnose ionized states of grains. However, the PAH 3.3 μ m feature has not been studied as much as other PAH features since it is weaker than others and resides outside of Spitzer capability, although it will be the only PAH feature accessible by JWST for high-z galaxies. AKARI mJy Unbiased Survey of Extragalactic Sources in 5MUSES (AMUSES) intends to take advantage of AKARI capability of spectroscopy in the 2 ~ 5 μ m to provide an unbiased library of 44 sample galaxies selected from a parent sample of 5MUSES, one of Spitzer legacy projects. For these 3.6 μ m flux limited sample galaxies whose redshifts range between 0 z μ m as a star formation rate (SFR) indicator while measuring ratios between PAH features. We present preliminary results of AMUSES.

Published
2011

48. Luminosity functions of local infrared galaxies with AKARI: implications for the cosmic star formation history and AGN evolution

Author

Takao Nakagawa, Stephane Arnouts, Chisato Yamauchi, Tsutomu T. Takeuchi, Emeric Le Floc'h, Woong-Seob Jeong, Toshinobu Takagi, Daisuke Ishihara, Chris Pearson, Shinki Oyabu, Chris Sedgwick, Hyung Mok Lee, Hanae Inami, Takehiko Wada, Tomotsugu Goto, Stephen Serjeant, Ezequiel Treister, and Hideo Matsuhara

Subjects
Luminous infrared galaxy, Physics, Spitzer Space Telescope, Space and Planetary Science, Star formation, Astronomy and Astrophysics, Astrophysics, Omega, Redshift, Galaxy, Luminosity function (astronomy), Luminosity
Abstract

Infrared (IR) luminosity is fundamental to understanding the cosmic star formation history and AGN evolution. The AKARI IR space telescope performed all sky survey in 6 IR bands (9, 18, 65, 90, 140, and 160um) with 3-10 times better sensitivity than IRAS, covering the crucial far-IR wavelengths across the peak of the dust emission. Combined with a better spatial resolution, AKARI can much more precisely measure the total infrared luminosity (L_TIR) of individual galaxies, and thus, the total infrared luminosity density in the local Universe. By fitting IR SED models, we have re-measured L_TIR of the IRAS Revised Bright Galaxy Sample. We present mid-IR monochromatic luminosity to L_TIR conversions for Spitzer 8,24um, AKARI 9,18um, IRAS 12um, WISE 12,22um, and ISO 15um filters, with scatter ranging 13-44%. The resulting AKARI IR luminosity function (LF) agrees well with that from the IRAS. We integrate the LF weighted by L_TIR to obtain a cosmic IR luminosity density of Omega_TIR= (8.5^{+1.5}_{-2.3})x 10^7 L Mpc^-3, of which 7+-1% is produced by LIRGs, and only 0.4+-0.1% is from ULIRGs in the local Universe. Once IR contributions from AGN and star-forming galaxies (SFG) are separated, SFG IR LF shows a steep decline at the bright-end. Compared with high-redshift results from the AKARI NEP deep survey, these data show a strong evolution of Omega_TIRSF propto (1+z)^4.0+-0.5, and Omega_TIRAGN propto (1+z)^4.4+-0.4. For Omega_TIRAGN, the ULIRG contribution exceeds that from LIRG already by z~1. A rapid evolution in both Omega_TIRAGN and Omega_TIRSFG suggests the correlation between star formation and black hole accretion rate continues up to higher redshifts. We compare the evolution of Omega_TIRAGN to that of X-ray luminosity density. The Omega_TIRAGN/Omega_X-rayAGN ratio shows a possible increase at z>1, suggesting an increase of obscured AGN at z>1.

Published
2010

49. OPTICAL IMAGES AND SOURCE CATALOG OF AKARI NORTH ECLIPTIC POLE WIDE SURVEY FIELD

Author

Yiseul Jeon, Mansur Ibrahimov, Myungshin Im, Induk Lee, Hyung Mok Lee, and Myung Gyoon Lee

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Ecliptic pole, Galaxy, law.invention, Telescope, Photometry (optics), Wavelength, Space and Planetary Science, Observatory, law, Galaxy formation and evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the source catalog and the properties of the $B-, R-$, and $I-$band images obtained to support the {\it AKARI} North Ecliptic Pole Wide (NEP-Wide) survey. The NEP-Wide is an {\it AKARI} infrared imaging survey of the north ecliptic pole covering a 5.8 deg$^2$ area over 2.5 -- 6 $\micron$ wavelengths. The optical imaging data were obtained at the Maidanak Observatory in Uzbekistan using the Seoul National University 4k $\times$ 4k Camera on the 1.5m telescope. These images cover 4.9 deg$^2$ where no deep optical imaging data are available. Our $B-, R-$, and $I-$band data reach the depths of $\sim$23.4, $\sim$23.1, and $\sim$22.3 mag (AB) at 5$\sigma$, respectively. The source catalog contains 96,460 objects in the $R-$band, and the astrometric accuracy is about 0.15$\arcsec$ at 1$\sigma$ in each RA and Dec direction. These photometric data will be useful for many studies including identification of optical counterparts of the infrared sources detected by {\it AKARI}, analysis of their spectral energy distributions from optical through infrared, and the selection of interesting objects to understand the obscured galaxy evolution., Comment: 39 pages, 12 figures

Published
2010

50. SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES): Faint-end Counts at 450 μm

Author

James E. Geach, Linhua Jiang, Wei-Hao Wang, Christopher J. Conselice, Chian-Chou Chen, Helmut Dannerbauer, Yu-Yen Chang, Yoshiki Toba, Junxian Wang, Ian Smail, Andrew Bunker, Ran Wang, Chen-Fatt Lim, James Dunlop, Douglas Scott, Nathan Bourne, Kotaro Kohno, Rob Ivison, Tomotsugu Goto, W. I. Cowley, Hyung Mok Lee, Elisabetta Valiante, Tadayuki Kodama, Omar Almaini, Chien-Hsu Lee, Julie Wardlow, James Simpson, Michał J. Michałowski, Yiping Ao, X. W. Shu, Xianzhong Zheng, Woong-Seob Jeong, Wei-Leong Tee, Xu Kong, Hyunjin Shim, Andrew Blain, Wei-Ching Lin, David L. Clements, Minju Lee, Marcin Sawicki, Ivan Oteo, Scott Chapman, Dani C.-Y. Chao, and Astronomy

Subjects
submillimeter: galaxies, 0306 Physical Chemistry (Incl. Structural), REDSHIFT SUBMILLIMETER GALAXIES, Population, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astronomy & Astrophysics, 01 natural sciences, Power law, 0305 Organic Chemistry, Luminosity, galaxies: high-redshift, galaxies - cosmology, 0103 physical sciences, galaxies, STAR-FORMING GALAXIES, Surface brightness, Noise level, education, DUSTY GALAXIES, NUMBER COUNTS, 010303 astronomy & astrophysics, evolution - submillimeter, Spatial density, Physics, education.field_of_study, FORMATION HISTORY, Science & Technology, 010308 nuclear & particles physics, Center (category theory), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, 0201 Astronomical And Space Sciences, high-redshift - galaxies, Space and Planetary Science, cosmology: cosmic background radiation, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), FIELD-SOUTH, Physical Sciences, LENSING CLUSTERS, P(D) FLUCTUATION ANALYSIS, galaxies: evolution, COSMOLOGY LEGACY SURVEY
Abstract

The SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) is a three-year JCMT Large Program aiming at reaching the 450 $\mu$m confusion limit in the COSMOS-CANDELS region, to study a representative sample of the high-redshift far-infrared galaxy population that gives rise to the bulk of the far-infrared background. We present the first-year data from STUDIES. We have reached a 450 $\mu$m noise level of 0.91~mJy for point sources at the map center, covered an area of 151 arcmin$^2$, and detected 98 and 141 sources at 4.0 and 3.5 $\sigma$, respectively. Our derived counts are best constrained in the 3.5-25 mJy regime using directly detected sources. Below the detection limits, our fluctuation analysis further constrains the slope of the counts down to 1 mJy. The resulting counts at 1-25 mJy are consistent with a power law having a slope of $-2.59$ ($\pm0.10$ for 3.5-25 mJy, and $^{+0.4}_{-0.7}$ for 1-3.5 mJy). There is no evidence of a faint-end termination or turn-over of the counts in this flux density range. Our counts are also consistent with previous SCUBA-2 blank-field and lensing cluster surveys. The integrated surface brightness from our counts down to 1 mJy is $90.0\pm17.2$ Jy deg$^{-2}$, which can account for up to $83^{+15}_{-16}\%$ of the COBE 450 $\mu$m background. We show that Herschel counts at 350 and 500 $\mu$m are significantly higher than our 450 $\mu$m counts, likely caused by its large beam and source clustering. High-angular resolution instruments like SCUBA-2 at 450 $\mu$m are therefore highly beneficial for measuring the luminosity and spatial density of high-redshift dusty galaxies., Comment: ApJ accepted. revised version uploaded

Published
2017

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