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1. Gear Up for the Action Replay: Leveraging Lensing for Enhanced Gravitational-wave Early Warning

Author

Sourabh Magare, Shasvath J. Kapadia, Anupreeta More, Mukesh Kumar Singh, Parameswaran Ajith, and A. N. Ramprakash

Subjects
Gravitational waves, Gravitational lensing, Astrophysics, QB460-466
Abstract

Premerger gravitational-wave (GW) sky localization of binary neutron star (BNS) and neutron star–black hole (NSBH) coalescence events would enable telescopes to capture precursors and electromagnetic (EM) emissions around the time of the merger. We propose an astrophysical scenario that could provide early-warning times of hours to days before coalescence with subarcsecond localization, provided that these events are gravitationally lensed. The key idea is that if the BNS/NSBH is lensed, then so is the host galaxy identified via the EM counterpart. From the angular separation of the lensed host galaxy images, as well as its redshift and the (foreground) lens redshift, we demonstrate that, for galaxy-scale lenses, we can predict the time delays/arrival time differences assuming a standard lens model. We further assess the feasibility and benefits of lensing as a tool for early warning in various GW observing runs of the LIGO–Virgo–Kagra network, including Voyager and the third-generation network. To that end, we study the effect of the limited angular resolution of the telescopes on our ability to predict the time delays. We find that with an angular resolution of 0.05″ we can predict time delays of >1 day with 1 σ error bar of ${ \mathcal O }$ (hours) at best. We also construct realistic time delay distributions of detectable lensed BNSs/NSBHs to forecast the early-warning times we might expect in the observing scenarios we consider.

Published
2023
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2. The impact of human expert visual inspection on the discovery of strong gravitational lenses

Author

Karina Rojas, Thomas E Collett, Daniel Ballard, Mark R Magee, Simon Birrer, Elizabeth Buckley-Geer, James H H Chan, Benjamin Clément, José M Diego, Fabrizio Gentile, Jimena González, Rémy Joseph, Jorge Mastache, Stefan Schuldt, Crescenzo Tortora, Tomás Verdugo, Aprajita Verma, Tansu Daylan, Martin Millon, Neal Jackson, Simon Dye, Alejandra Melo, Guillaume Mahler, Ricardo L C Ogando, Frédéric Courbin, Alexander Fritz, Aniruddh Herle, Javier A Acevedo Barroso, Raoul Cañameras, Claude Cornen, Birendra Dhanasingham, Karl Glazebrook, Michael N Martinez, Dan Ryczanowski, Elodie Savary, Filipe Góis-Silva, L Arturo Ureña-López, Matthew P Wiesner, Joshua Wilde, Gabriel Valim Calçada, Rémi Cabanac, Yue Pan, Isaac Sierra, Giulia Despali, Micaele V Cavalcante-Gomes, Christine Macmillan, Jacob Maresca, Aleksandra Grudskaia, Jackson H O’Donnell, Eric Paic, Anna Niemiec, Lucia F de la Bella, Jane Bromley, Devon M Williams, Anupreeta More, and Benjamin C Levine

Published
2023
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3. X-ray study of the double source plane gravitational lens system Eye of Horus observed with XMM–Newton

Author

Keigo Tanaka, Ayumi Tsuji, Hiroki Akamatsu, J H H Chan, Jean Coupon, Eiichi Egami, Francois Finet, Ryuichi Fujimoto, Yuto Ichinohe, Anton T Jaelani, Chien-Hsiu Lee, Ikuyuki Mitsuishi, Anupreeta More, Surhud More, Masamune Oguri, Nobuhiro Okabe, Naomi Ota, Cristian E Rusu, Alessandro Sonnenfeld, Masayuki Tanaka, Shutaro Ueda, and Kenneth C Wong

Published
2019
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6. Exploring the hidden Universe: A novel phenomenological approach for recovering arbitrary gravitational-wave millilensing configurations

Author

Anna Liu, Isaac C F Wong, Samson H W Leong, Anupreeta More, Otto A Hannuksela, and Tjonnie G F Li

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Since the first detection of gravitational waves in 2015, gravitational-wave astronomy has emerged as a rapidly advancing field that holds great potential for studying the cosmos, from probing the properties of black holes to testing the limits of our current understanding of gravity. One important aspect of gravitational-wave astronomy is the phenomenon of gravitational lensing, where massive intervening objects can bend and magnify gravitational waves, providing a unique way to probe the distribution of matter in the universe, as well as finding applications to fundamental physics, astrophysics, and cosmology. However, current models for gravitational-wave millilensing - a specific form of lensing where small-scale astrophysical objects can split a gravitational wave signal into multiple copies - are often limited to simple isolated lenses, which is not realistic for complex lensing scenarios. In this paper, we present a novel phenomenological approach to incorporate millilensing in data analysis in a model-independent fashion. Our approach enables the recovery of arbitrary lens configurations without the need for extensive computational lens modeling, making it a more accurate and computationally efficient tool for studying the distribution of matter in the universe using gravitational-wave signals. When gravitational-wave lensing observations become possible, our method can provide a powerful tool for studying complex lens configurations, including dark matter subhalos and MACHOs., 12 pages, 8 figures

Published
2023

7. Time delay lens modelling challenge

Author

Daniel Gilman, Tommaso Treu, G. Despali, Christopher D. Fassnacht, Jonathan P. Coles, Frederic Courbin, Anupreeta More, Hyungsuk Tak, Matthew W. Auger, Hum Chand, Matteo Frigo, Philip J. Marshall, M. Millon, Dominique Sluse, A. Galan, L. Van de Vyvere, Geoff C. F. Chen, Joshua Yao-Yu Lin, Da Xu, Anowar J. Shajib, Philipp Denzel, Xuheng Ding, Ji Won Park, Simona Vegetti, Simon Birrer, Stefan Hilbert, Liliya L. R. Williams, Vivien Bonvin, Prasenjit Saha, and S. R. Kumar

Subjects
degeneracies, profiles, Point spread function, Accuracy and precision, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, Test data generation, internal structure, FOS: Physical sciences, central image, Kinematics, 01 natural sciences, Measure (mathematics), law.invention, hubble constant, law, evolution, 0103 physical sciences, early-type galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, methods: data analysis, Astrophysics - Astrophysics of Galaxies, Lens (optics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, impact, precision, constraints, Astrophysics - Instrumentation and Methods for Astrophysics, Completeness (statistics), Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In recent years, breakthroughs in methods and data have enabled gravitational time delays to emerge as a very powerful tool to measure the Hubble constant $H_0$. However, published state-of-the-art analyses require of order 1 year of expert investigator time and up to a million hours of computing time per system. Furthermore, as precision improves, it is crucial to identify and mitigate systematic uncertainties. With this time delay lens modelling challenge we aim to assess the level of precision and accuracy of the modelling techniques that are currently fast enough to handle of order 50 lenses, via the blind analysis of simulated datasets. The results in Rung 1 and Rung 2 show that methods that use only the point source positions tend to have lower precision ($10 - 20\%$) while remaining accurate. In Rung 2, the methods that exploit the full information of the imaging and kinematic datasets can recover $H_0$ within the target accuracy ($ |A| < 2\%$) and precision ($< 6\%$ per system), even in the presence of poorly known point spread function and complex source morphology. A post-unblinding analysis of Rung 3 showed the numerical precision of the ray-traced cosmological simulations to be insufficient to test lens modelling methodology at the percent level, making the results difficult to interpret. A new challenge with improved simulations is needed to make further progress in the investigation of systematic uncertainties. For completeness, we present the Rung 3 results in an appendix, and use them to discuss various approaches to mitigating against similar subtle data generation effects in future blind challenges., 23 pages, 12 figures, 6 tables, MNRAS accepted

Published
2021
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8. Ordering the confusion: A study of the impact of lens models on gravitational-wave lensing detection capabilities

Author

Justin Janquart, Anupreeta More, and Chris Van Den Broeck

Subjects
Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract

When traveling from their source to the observer, gravitational waves can get deflected by massive objects along their travel path. When the lens is massive enough and the source aligns closely with the line-of-sight to the lens, the wave undergoes strong lensing, leading to several images with the same frequency evolution. These images are separated in time, magnified, and can undergo an overall phase shift. Searches for strongly-lensed gravitational waves are already ongoing. In essence, such searches look for events originating from the same sky location and having the same detector frame parameters. However, the agreement between these quantities can also happen by chance, leading to an important confusion background. To reduce the overlap between background and foreground, one can include lensing models, enforcing the lensing parameters to also be consistent with our expectations. In principle, such models should decrease the confusion background. However, when doing realistic searches, one does not know which model is the correct one. The use of an incorrect model could lead to the non-detection of genuinely lensed events. In this work, we investigate under realistic conditions how one can identify lensed events in the unlensed background. We focus on the impact of the addition of a model for the lens density profile and investigate the effect of potential errors in the modelling. We show that it is extremely difficult to identify lensing confidently without the addition of a lens model. We also show that slight variations in the profile of the lens model are tolerable but a model with incorrect assumptions about the underlying lens population causes significant errors compared to assuming no lens model at all. We also suggest some strategies to improve the confidence in the detection of strong lensing for gravitational waves., 21 pages, 10 figures

Published
2022

9. Gravitational Lensing of Gravitational Waves: Probability of Microlensing in Galaxy-Scale Lens Population

Author

Ashish Kumar Meena, Anuj Mishra, Anupreeta More, Sukanta Bose, and Jasjeet Singh Bagla

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

With the increase in the number of observed gravitational wave (GW) signals, detecting strongly lensed GWs by galaxies has become a real possibility. Lens galaxies also contain microlenses (e.g., stars and black holes), introducing further frequency-dependent modulations in the strongly lensed GW signal within the LIGO frequency range. The multiple lensed signals in a given lens system have different underlying macro-magnifications ($|\mu|$) and are located in varied microlens densities ($\Sigma_\bullet$), leading to different levels of microlensing distortions. This work quantifies the fraction of strong lens systems affected by microlensing using realistic mock observations. We study 50 quadruply imaged systems (quads) by generating 50 realizations for each lensed signal. However, our conclusions are equally valid for lensed signals in doubly imaged systems (doubles). The lensed signals studied here have $|\mu|\sim[0.5, 10]$ and $\Sigma_\bullet\sim[10, 10^3]~{\rm M}_\odot/{\rm pc^2}$. We find that the microlensing effects are more sensitive to the macro-magnification than the underlying microlens density, even if the latter exceeds $10^3~{\rm M}_\odot/{\rm pc^2}$. The mismatch between lensed and unlensed GW signals rarely exceeds $1\%$ for nearly all binary black hole sources in the total mass range [10 M$_\odot$, 200 M$_\odot$]. This implies that microlensing is not expected to affect the detection or the parameter estimation of such signals and does not pose any further challenges in identifying the different lensed counterparts when macro-magnification is ${\leq}10$. Such a magnification cut is expected to be satisfied by ${\sim}50\%$ of the detectable pairs in quads and ${\sim}90\%$ of the doubles in the fourth observing run of the LIGO-Virgo detector network., Comment: 12 pages, 9 figures; Comments welcome

Published
2022

10. Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI). VIII. New galaxy-scale lenses from the HSC SSP

Author

Kenneth C Wong, James H H Chan, Dani C-Y Chao, Anton T Jaelani, Issha Kayo, Chien-Hsiu Lee, Anupreeta More, and Masamune Oguri

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We conduct a search for galaxy-scale strong gravitational lens systems in Data Release 4 of the Hyper Suprime-Cam Subaru Strategic Program (HSC SSP), consisting of data taken up to the S21A semester. We select 103191 luminous red galaxies from the Baryon Oscillation Spectroscopic Survey (BOSS) sample that have deep multiband imaging from the HSC SSP and use the YattaLens algorithm to automatically identify lens candidates with blue arc-like features. The candidates are visually inspected and graded based on their likelihood of being a lens. We find 8 definite lenses, 28 probable lenses, and 138 possible lenses. The new lens candidates generally have lens redshifts in the range $0.3 \lesssim z_{\mathrm{L}} \lesssim 0.9$, a key intermediate redshift range to study the evolution of galaxy structure. Follow-up spectroscopy will confirm these new lenses and measure source redshifts to enable detailed lens modeling., Comment: Accepted for publication in PASJ; 12 pages, 4 figures, 2 tables

Published
2022
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11. Erratum: Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars

Author

Santiago Avila, Carlos E. Cunha, Anupreeta More, Issha Kayo, David J. Brooks, S. Desai, Philip J. Marshall, Peter Doel, Simon Birrer, Josh Frieman, E. Suchyta, Kyler Kuehn, M. Smith, Ofer Lahav, Daniel Gruen, F. Ostrovski, G. Tarle, Matthew W. Auger, Sherry H. Suyu, E. Bertin, Juan Garcia-Bellido, T. M. C. Abbott, Veronica Motta, M. Carrasco Kind, Cristian E. Rusu, D. W. Gerdes, Christopher D. Fassnacht, J. Carretero, James H. H. Chan, E. J. Sanchez, Adriano Agnello, B. Flaugher, I. Sevilla-Noarbe, Richard G. McMahon, Flavia Sobreira, A. Carnero Rosell, Anowar J. Shajib, B. Hoyle, Marcos Lima, Jennifer L. Marshall, D. L. Hollowood, Peter Melchior, N. Kuropatkin, Frederic Courbin, G. Gutierrez, G. Meylan, M. March, M. E. C. Swanson, A. R. Walker, E. Buckley-Geer, David J. James, Tom Shanks, Timo Anguita, L. N. da Costa, Felipe Menanteau, M. A. G. Maia, J. De Vicente, Pablo Fosalba, Ramon Miquel, Tommaso Treu, Paul L. Schechter, Thomas E. Collett, J. Annis, N. D. Morgan, Marcelle Soares-Santos, S. Allam, Robert A. Gruendl, Huan Lin, C. Lemon, W. G. Hartley, Masamune Oguri, A. A. Plazas, and V. Scarpine

Subjects
Physics, QUASARES, Space and Planetary Science, Lens (geology), Astronomy, Astronomy and Astrophysics, Quasar, Sample (graphics)
Abstract

The paper ‘Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars’ was published in MNRAS, 483, 4, 5649–5671 (2019). The coordinate values of the image positions in table 4 were wrongly printed due to a clerical error. At a later stage of writing the manuscript, we have changed the zero-point definition of the lens coordinate systems, but the relative image positions were not accounted for this change of definition while printing out table 4. We provide the updated Table 4 below. This error does not impact any other results of the paper in any way, except for the table itself. We thank Collin Werner and Paul Schechter for helping us identify this error.

Published
2021
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12. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations

Author

Hiroko Niikura, Toshiki Kurita, Anupreeta More, Surhud More, Masahiro Takada, Masashi Chiba, Robert H. Lupton, Naoki Yasuda, Masamune Oguri, Sunao Sugiyama, and Takahiro Sumi

Subjects
Physics, Solar mass, 010504 meteorology & atmospheric sciences, Milky Way, Dark matter, Astronomy and Astrophysics, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, 01 natural sciences, Galactic halo, Stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

Primordial black holes (PBHs) have long been suggested as a viable candidate for the elusive dark matter. The abundance of such PBHs has been constrained using a number of astrophysical observations, except for a hitherto unexplored mass window of MPBH = [10−14, 10−9] solar masses. Here we carry out a dense-cadence, 7-hour-long observation of M31 with the Subaru Hyper Suprime-Cam (HSC) to search for microlensing of stars in M31 by PBHs lying in the halo regions of the Milky Way and M31. Given our simultaneous monitoring of tens of millions of stars in M31, if such light PBHs make up a significant fraction of dark matter, we expect to find many microlensing events. However, we identify only a single candidate event, which translates into stringent upper bounds on the abundance of PBHs in the mass range MPBH ≃ [10−11, 10−6] solar masses. The abundance of primordial black holes in the Galactic halo is constrained through their microlensing of stars in M31. Despite monitoring tens of millions of stars, only a single candidate event is found, providing stringent upper bounds on their abundance.

Published
2019
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13. Gravitational Lensing of Gravitational Waves: Effect of Microlens Population in Lensing Galaxies

Author

Jasjeet Singh Bagla, Ashish Kumar Meena, Anuj Mishra, Suvadeep Bose, and Anupreeta More

Subjects
Microlens, Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, Population, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Amplification factor, Gravitational microlensing, General Relativity and Quantum Cosmology, LIGO, Galaxy, Gravitational lens, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

With increasing sensitivities of the current ground-based gravitational-wave (GW) detectors, the prospects of detecting a strongly lensed GW signal are going to be high in the coming years. When such a signal passes through an intervening lensing galaxy or galaxy cluster, the embedded stellar-mass microlenses lead to interference patterns in the signal that may leave observable signatures. In this work, we present an extensive study of these wave effects in the LIGO/Virgo frequency band ($10$-$10^4$ Hz) due to the presence of the microlens population in galaxy-scale lenses for the first time. We consider a wide range of strong lensing (macro) magnifications and the corresponding surface microlens densities found in lensing galaxies and use them to generate realisations of the amplification factor. The methodologies for simulating amplification curves for both types of images (minima and saddle points) are also discussed. We then study how microlensing is broadly affected by the parameters like macro-magnifications, stellar densities, the initial mass function (IMF), types of images, and microlens distribution around the source. In general, with increasing macro-magnification values, the effects of microlensing become increasingly significant regardless of other parameters. Mismatch analysis between the lensed and the unlensed GW waveforms from chirping binaries suggests that, while inferring the source parameters, microlensing can not be neglected for macro-magnification $\gtrsim 15$. Furthermore, for extremely high macro-magnifications $\gtrsim 100$, the mismatch can even exceed $5\%$, which can result in both a missed detection and, consequently, a missed lensed signal., Comment: 18 pages, 13 figures. v2: Added section 5.7; updated section 5.6; typos corrected; references updated

Published
2021
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14. Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs

Author

A. Grimaldi, M. A. Barton, Samuele Cortese, Charlie Hoy, Charalampos Markakis, L. Trozzo, Albert Lazzarini, Benno Willke, A. Grado, P. Booker, C. Cahillane, Norichika Sago, J. Hennig, V. Gayathri, J. Baird, M. Jeunon, Sascha Husa, Samaya Nissanke, S. Walsh, A. Hreibi, M. J. Szczepańczyk, M. Chaturvedi, G. Venugopalan, S. R. Mohite, Alessandra Buonanno, Gabrielle Allen, H. Y. Cheung, Rana X. Adhikari, Om Sharan Salafia, F. Donovan, Edoardo Milotti, B. Lantz, M. A. Bizouard, B. K. Berger, Denis Martynov, Claudia Moreno, N. V. Krishnendu, Marco Bazzan, Satoshi Tsuchida, C. Ingram, D. A. Melchor, F. Marion, E. Goetz, Matthew Giesler, D.B. DeBra, Giuseppe Castaldi, S. G. Crowder, K. Ito, E. Lalande, M. Cannavacciuolo, E. N. Clark, Geoffrey Lovelace, L. Nguyen Quynh, J. D. E. Creighton, Lijing Shao, M. Carpinelli, J. Liu, A. Pasqualetti, R. Bajpai, F. Garufi, Archana Pai, Surendra Nadh Somala, Yoshiyuki Obuchi, C. Talbot, Carl-Johan Haster, S. Nozaki, H. Sun, V. JaberianHamedan, Tyson Littenberg, T. Washimi, T. D. Creighton, L. A. Rees, Silvia Corezzi, S. Bae, Kai-Feng Chen, F. Paoletti, Felice Sorrentino, C. L. Chan, P. Szewczyk, A. K. Prajapati, M. Patel, C. M. Mow-Lowry, Sergey P. Vyatchanin, L. Aiello, Luigi Troiano, M. Gosselin, R. Green, H. Yuzurihara, D. Hoyland, B. F. Whiting, J. Casanueva Diaz, V. M. Bedakihale, Masako Kakizaki, R. Maggiore, C. Van Den Broeck, E. Sowell, E. Coccia, M. E. Zucker, B. A. Weaver, G. Vajente, S. M. Gaebel, T. Shimoda, Y. Okutani, J. G. Rollins, A. Mhaske, H. Hansen, T. Wlodarczyk, Laura Cadonati, L. Rolland, S. T. Countryman, S. Penn, R. M. S. Schofield, K. Mogushi, H. Estelles, Y. Huang, P. A. Duverne, S. Karki, D. Moraru, A. Dmitriev, E. Floden, V. B. Adya, A. Renzini, G. L. Mansell, Y. K. Lecoeuche, G. M. Harry, L. Naticchioni, T. Shishido, Salvatore Vitale, A. Cumming, F. Di Renzo, Gianpietro Cagnoli, L.-W. Wei, S. Katsanevas, Madeline Wade, M. Tse, D. S. Tsai, D. M. Macleod, T. D. Ramirez, M. T. Hübner, Yasufumi Kojima, J. F. J. van den Brand, C. Pluchar, P. Chanial, Abhirup Ghosh, S. Sunil, M. Tacca, G. Kang, E. Capote, A. K. Mehta, N. Man, H. Pang, K. A. Strain, K. Haughian, P. Ruggi, A. Puecher, A. Mullavey, T. J. N. Nelson, Filip Morawski, P. J. Easter, G. Guixé, Xiaohui Fan, P. Leaci, Y. R. Chen, Alessandro Bertolini, J. C. Driggers, John A. Clark, Ben Farr, Fabrizio Barone, Giuseppe Intini, D. Rozza, V. Dattilo, Tejinder Kaur, Edwin J. Son, Isobel M. Romero-Shaw, T. C. Pechsiri, Umakant D. Rapol, G. S. Wallace, Stefan Hild, J. D. Jones, A. C. Baylor, L. M. DaneshgaranBajastani, R. Huxford, Surabhi Sachdev, Christopher J. Moore, V. V. Frolov, Kazuhiro Hayama, K. Venkateswara, R. Cotesta, R. Mittleman, Kentaro Komori, Soubhik Kumar Bhaumik, Yuri Levin, Akito Araya, J. Von Wrangel, T. Kajita, L. Kleybolte, S. Oshino, G. S. Davies, T. Huynh-Dinh, Hajime Sotani, A. Z. Jan, C. Makarem, Martin Hendry, Cecilio García-Quirós, Hong Wu, J.-G. Ducoin, Richard O'Shaughnessy, B. Barr, M. C. Díaz, A. Menendez-Vazquez, P. Figura, C. M. Compton, Antonios Kontos, B. L. Swinkels, Wei-Tou Ni, V. Tiwari, K. A. Thorne, Hisa-aki Shinkai, Isabel Cordero-Carrión, S. Wu, Ll. M. Mir, Junwei Cao, R. Kirchhoff, S. P. Jadhav, M. C. Heintze, Yann Bouffanais, V. Fafone, A. Pereira, J. A. Rocha, Nelson Christensen, S. A. Usman, E. G. Seo, E. K. Porter, Kendall Ackley, R. K. Nayak, A. Allocca, Marco Romanelli, Christophe Collette, C. J. Perez, B. D. O'Brien, R. P. Udall, R. C. Walet, C. Di Fronzo, T. R. Saravanan, J. Zhang, L. F. Ortega, V. P. Mitrofanov, R. Cummings, G. Koekoek, J. Betzwieser, M. Zhan, D. W. Yeeles, Antoine Heidmann, A. Brillet, G. Eddolls, A. D. Viets, D. Meacher, E. N. Tapia San Martin, K. Haris, F. Vetrano, Z. Hong, K. Kaihotsu, S. E. Dwyer, David Keitel, A. Hagiwara, L. C. Strang, R. L. Savage, Chunglee Kim, F. W. Yang, J. S. Kissel, H. Cao, Marc Favata, A. J. Weinstein, Fumihiro Uraguchi, Roger Jones, V. Villa-Ortega, David A. Williams, S. J. Cooper, N. Raza, I. W. Harry, C-Y. Lin, N. Y. Washington, N. Letendre, Nikhil Sarin, J. Heinzel, Thanh D. Nguyen, V. J. Roma, Leo Tsukada, E. Z. Hamilton, M. Matiushechkina, Nikita S. Shcheblanov, B. H. Hsieh, Y. Miyazaki, A. D. Huddart, N. Kawai, R. J. Trudeau, Anindita Ganguly, M. Diaz-Ortiz, J. Venneberg, W. Del Pozzo, P. F. Cohadon, K. E. Ramirez, H. Heitmann, D. Sawant, M. Laxen, Anchal Gupta, Kei Kotake, H. Y. Chia, E. Cuoco, N. A. Didio, E. N.Tapia San Mertin, Fabrizio Giulio Luca Pilo, F. E. Peña Arellano, A. Ueda, D. Lumaca, L. Xiao, A. P. Spencer, A. M. Farah, M. F. Carney, D. D. Brown, Chad Hanna, A. Bramley, Yue Zhao, C. Kimball, Sakae Araki, J. J. McCann, T. J. Slaven-Blair, S. ShyamSundar, C. Stachie, A. Parisi, J. Oberling, M. Pirello, Alena Ananyeva, A. Lartaux-Vollard, Suvadeep Bose, A. Depasse, A. F. Helmling-Cornell, Ajay Kumar, N. D. Ormsby, C. Whittle, Yuki Inoue, A. M. Gretarsson, C. Bradaschia, W-R. Xu, F. Carbognani, Yang Yang, Yoshiaki Himemoto, I. M. Pinto, I. La Rosa, Jean-René Cudell, C. De Rossi, Stanislav Babak, S. Sayah, H. Overmier, B. Garaventa, Nobutada Kimura, Ka Yee C. Lee, M. A. Okada, Matteo Pegoraro, Piero Rettegno, R. Gouaty, A. V. Bhandari, Z. Márka, M. Boer, Shubhanshu Tiwari, T. B. Edo, R. Gray, Masashi Ohkawa, V. Srivastava, Y. Aso, M. Fays, N. van Bakel, M. Leonardi, Osamu Miyakawa, Lior Cohen, R. Zhang, Ik Siong Heng, Geert Raaijmakers, P. Fulda, M. Mondin, K. Mason, S. Shibagaki, D. Rosińska, E. R. G. von Reis, Ray-Kuang Lee, F. Y. Khalili, Ofelia Durante, Jay D. Tasson, J. L. Willis, M. Eisenmann, Ofek Birnholtz, Sanjeev Dhurandhar, M. Merzougui, Sebastien Biscans, S. A. Nichols, A. Malik, S. Gaudio, G. Valdes, Pulak Ranjan Giri, A. Adams, I. Tosta e Melo, Deirdre Shoemaker, F. Robinet, J. K. Blackburn, Q. Chu, F. L. Linde, R. Tenorio, N. A. Holland, Yichen Huang, D. Sellers, G. R. Johns, S. Ponrathnam, Michael Williams, Moritz Mehmet, L. Terkowski, E. Cesarini, P. Kumar, A. Singha, Ken K. Y. Ng, M. Constancio, E. 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Ciani, Guenakh Mitselmakher, S. S. Eikenberry, Yuhang Zhao, B. A. Boom, A. M. Sergeev, Rosa Poggiani, B. Li, Mitsuhiro Fukushima, S. Farinon, A. Pele, Yutaro Enomoto, S. Doravari, Logan Richardson, Ping Huang, P. Raffai, G. I. McGhee, Stefano Bagnasco, Stephane Perries, Vincenzo Fiumara, K. Oh, Andrew Matas, Lucy E Clarke, S. H. Huttner, T. F. Bennett, J. Hanks, A. Chen, Andrew Melatos, M. Lorenzini, F. De Lillo, J. H. Briggs, Mark Hannam, A. Strunk, M. Llorens-Monteagudo, J-S. Tsao, N. Kijbunchoo, Sheelu Abraham, J. D. Bentley, P. A. Altin, M. Stover, P.H. Nguyen, D. Barker, Nicholas Demos, J. D. Lough, Soma Mukherjee, V. Sequino, C. J. Richardson, A. Samajdar, B. Sassolas, H. J. Bulten, D. C. Vander-Hyde, D. Griffith, C. M. Weller, Y. J. Huang, Bala R. Iyer, S. McCormick, Jian Li, Tristan Briant, Haocun Yu, L. Sun, T. Narikawa, A. M. Sintes, Chandra Kant Mishra, Joseph D. Romano, R. Bhandare, Ryo Yamazaki, Keiko Kokeyama, Mairi Sakellariadou, G. Pillant, Tenglin Li, L. Haegel, Viola Sordini, Masatake Ohashi, D. Mukherjee, B. Champion, P. Kolitsidou, B. Ratto, Nergis Mavalvala, Jerome Degallaix, M. Schneewind, C. Casentini, Naoko Ohishi, Sebastian Khan, B. C. Barish, F. De Matteis, Archisman Ghosh, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Paris-Est Marne-la-Vallée (UPEM), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut des Hautes Études Scientifiques (IHES), IHES, KAGRA, Virgo, LIGO Scientific, 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 Rennes 1 (UR1), 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 (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), 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), Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, A., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Aleman, K. M., Allen, G., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koya, Arai, Koji, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Aronson, S. M., Asada, H., Asali, Y., Ashton, G., Aso, Y., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Bals, M., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Bankar, R. S., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Bécsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Benjamin, M. G., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bhandari, A. V., Bhattacharjee, D., Bhaumik, S., Bidler, J., Bilenko, I. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., 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., Bogaert, G., Boldrini, M., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Byer, R. L., Cadonati, L., Caesar, M., Cagnoli, G., Cahillane, C., Cain, H. W., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, J., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carullo, G., Carver, T. L., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Chakravarti, K., Champion, B., Chan, C. -H., Chan, C., Chan, C. L., Chan, M., Chandra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chen, A., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. -B., Chen, Y. -R., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choate, S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y-K., Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colpi, M., Compton, C. 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., Cousins, B., Couvares, P., Covas, P. B., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cuoco, E., Curyło, M., Canton, T. Dal, Dálya, G., Dana, A., Daneshgaranbajastani, 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., Dean, R., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Del Pozzo, W., Demarchi, L. M., De Matteis, F., D’Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., De Simone, R., Dhurandhar, S., Díaz, M. C., Diaz-Ortiz, M., Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., D’Onofrio, L., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Drago, M., Driggers, J. C., Drori, Y., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., D’Urso, D., Duverne, P. -A., Dwyer, S. E., Easter, P. J., Ebersold, M., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Enomoto, Y., Errico, L., Essick, R. C., Estellés, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Farrow, N. W., 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, T. A., Fidecaro, F., Figura, P., Fiori, I., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Flynn, E., Fong, H., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Frederick, C., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fronzé, G. G., Fujii, Y., Fujikawa, Y., Fukunaga, M., Fukushima, M., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D., Gaonkar, S. G., Garaventa, B., García-Núñez, C., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Ge, G., Gemme, G., Gennai, A., George, J., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, Abhirup., Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Sourath, Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., González, G., Gopakumar, A., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Granata, V., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W., Griggs, H. L., Grignani, G., Grimaldi, A., Grimes, E., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guerrero, J. G., Guidi, G. M., Guimaraes, A. R., Guixé, G., Gulati, H. K., Guo, H. -K., Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, P., Gustafson, E. K., Gustafson, R., Guzman, F., Ha, S., Haegel, L., Hagiwara, A., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W. -B., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Hasskew, R. K., Haster, C. -J., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Vivanco, F. Hernandez, Heurs, M., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hiranuma, Y., Hirata, N., Hirose, E., Hochheim, S., Hofman, D., Hohmann, J. N., Holgado, A. M., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Z., Hopkins, P., Hough, J., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsieh, B-H., Hsu, Y., Huang, G-Z., Huang, H-Y., Huang, P., Huang, Y-C., Huang, Y. -J., Huang, Y. -W., Hübner, M. T., Huddart, A. D., Huerta, E. A., Hughey, B., Hui, D. C. Y., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Ide, S., Idzkowski, B., Iess, A., Ikenoue, B., Imam, S., Inayoshi, K., Inchauspe, H., Ingram, C., Inoue, Y., Intini, G., Ioka, K., Isi, M., Isleif, K., Ito, K., Itoh, Y., Iyer, B. R., Izumi, K., Jaberianhamedan, V., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jeon, C., Jeunon, M., Jia, W., Jiang, J., Jin, H. -B., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Jung, K., Jung, P., Junker, J., Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karat, S., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kawaguchi, K., Kawai, N., Kawasaki, T., Kéfélian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, J., Kim, K., Kim, W. S., Kim, Y. -M., Kimball, C., Kimura, N., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kita, N., Kitazawa, H., Kleybolte, L., Klimenko, S., Knee, A. M., Knowles, T. D., Knyazev, E., Koch, P., Koekoek, G., Kojima, Y., Kokeyama, K., Koley, S., Kolitsidou, P., Kolstein, M., Komori, K., Kondrashov, V., Kong, A. K. H., Kontos, A., Koper, N., Korobko, M., Kotake, K., Kovalam, M., Kozak, D. B., Kozakai, C., Kozu, R., Kringel, V., Krishnendu, N. V., Królak, A., Kuehn, G., Kuei, F., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuo, C., Kuo, H-S., Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kwak, K., Kwang, S., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lee, R., Lehmann, J., Lemaître, A., Leon, E., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Leviton, J. N., Li, A. K. Y., Li, B., Li, J., Li, K. L., Li, T. G. F., Li, X., Lin, C-Y., Lin, F-K., Lin, F-L., Lin, H. L., Lin, L. C. -C., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, G. C., Liu, J., Liu, K., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., Lollie, M. L., London, L. T., Longo, A., Lopez, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Luo, L. -W., Macas, R., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., Hernandez, I. Magaña, Magaña-Sandoval, F., Magazzù, C., Magee, R. M., Maggiore, R., Majorana, E., Makarem, C., Maksimovic, I., Maliakal, S., Malik, A., Man, N., Mandic, V., Mangano, V., Mango, J. L., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marchio, M., Marion, F., Mark, Z., 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, M., Martinez, V., Martinovic, K., Martynov, D. V., Marx, E. J., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matichard, F., Matiushechkina, M., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mcclincy, P., Mccormick, S., Mcculler, L., Mcghee, G. I., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Michimura, Y., Middleton, H., Milano, L., Miller, A. L., Millhouse, M., Mills, J. C., Milotti, E., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mio, N., Mir, Ll. M., Mishkin, A., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Mo, Geoffrey, Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina, I., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. 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Subjects
gravitational radiation: anisotropy, Physics and Astronomy (miscellaneous), gravitational radiation: stochastic, Astronomy, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Physics, Particles & Fields, Cosmology & Astrophysics, energy: flux, energy: density, gravitational radiation: energy, LIGO, QC, QB, Physics, Settore FIS/01, Spectral index, Galactic Center, Amplitude, General relativity, Sidereal time, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitational radiation: power spectrum, Gravitation, data analysis method, Anisotropic stochastic gravitational-wave background, Experimental studies of gravity, FOS: Physical sciences, O3, O2, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, Stochastic Background, Gravitational Waves, LIGO, Virgo, O1, O2, O3, O1, Gravitational waves, UPPER LIMITS, statistical analysis, 0103 physical sciences, advanced LIGO and Virgo, ddc:530, KAGRA, 010306 general physics, STFC, gravitational waves, Virgo, Gravitational Waves, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, RCUK, Galaxy, VIRGO, gravitational radiation: emission, spectrum: density, RADIATION, CROSS-CORRELATION SEARCH, Stochastic Background, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, galaxy
Abstract

We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called {\tt PyStoch} on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95\% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from $F_{\alpha, \Theta} < {\rm (0.013 - 7.6)} \times 10^{-8} {\rm erg \, cm^{-2} \, s^{-1} \, Hz^{-1}},$ and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from $\Omega_{\alpha, \Theta} < {\rm (0.57 - 9.3)} \times 10^{-9} \, {\rm sr^{-1}}$, depending on direction ($\Theta$) and spectral index ($\alpha$). These limits improve upon previous limits by factors of $2.9 - 3.5$. We also set 95\% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from $h_0 < {\rm (1.7-2.1)} \times 10^{-25},$ a factor of $\geq 2.0$ improvement compared to previous stochastic radiometer searches., Comment: 23 Pages, 9 Figures

Published
2021
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15. All-sky search in early O3 LIGO data for continuous gravitational-wave signals from unknown neutron stars in binary systems

Author

L. Kleybolte, Valérie Martinez, E. G. Seo, Susan M. Scott, E. K. Porter, Cesare Barbieri, Walter Winkler, Kopin Liu, Chad Hanna, A. Bramley, A. S. Markosyan, C. Kimball, Harald Lück, J. Oberling, M. Pirello, D. Passuello, A. Cirone, T. B. Edo, E. Knyazev, D. Verkindt, D. Ugolini, Roberto Chierici, P. Clearwater, Fiodor Sorrentino, C. Di Giorgio, J. Cao, S. C. McGuire, J. F. Read, S. Di Pace, H. Satari, J. Bidler, R. Dean, J. Calderón Bustillo, Miriam Lucio Martinez, F. Nocera, N. Letendre, Safura Sharifi, Alicia M. Sintes, M. Curyło, Nikhil Sarin, J. V. van Heijningen, E. J. Fauchon-Jones, A. Yoon, M. Lormand, J. Heinzel, Thanh D. Nguyen, E. Cuoco, D. Lumaca, M. A. Okada, K. Mason, D. J. Stops, Sanjeev Dhurandhar, J. S. H. Lee, T. Dal Canton, Felix Wellmann, J. Warner, I. Maksimovic, R. L. Ward, G. Hemming, R. Passaquieti, Laurent Pinard, F. Cleva, C. Messenger, M. P. Ross, M. Pichot, Maximiliano Isi, M. Croquette, E. M. Gretarsson, Ying Guo, D. Beniwal, Peter Fritschel, Wenxiao Wang, V. Valsan, M. Masso-Reid, Z. J. Holmes, J. Petermann, Xin Chen, R. M. Martin, Piotr Jaranowski, L. E. Sanchez, A. C. Utina, D. Hartwig, C. Rajan, Enrico Calloni, G. Traylor, S. Soni, Thomas Corbitt, L. Salconi, C. A. Costa, R. K. Choudhary, V. Boudart, W. Jia, T. Zhang, Thibaut Jacqmin, D. Lopez, Y. Drori, S. Choate, N. Leroy, S. T. Countryman, Albert Lazzarini, Geraint Pratten, H. Fair, Surabhi Sachdev, Christopher J. Moore, Q. Chu, D. Bersanetti, G. Ashton, Samuele Cortese, G. A. Prodi, Christos Karathanasis, Eric Thrane, P. Thomas, M. Arène, E. Polini, B. Bécsy, I. Molina, Des Gibson, C. Michel, R. DeSalvo, A. Viceré, V. V. Frolov, Sarah Caudill, A. Vajpeyi, T. D. Knowles, Marica Valentini, Riccardo Ciolfi, Yi Chen, Peter T. H. Pang, B. W. Schulte, Samaya Nissanke, H. Y. Cheung, M. A. Bizouard, C. H. Chan, A. W. Jones, Kentaro Komori, Soubhik Kumar Bhaumik, O. V. Palashov, Sean T. McWilliams, Charlie Hoy, P. Booker, W. Kastaun, H. Qi, B. K. Berger, B. U. Gadre, P. Dupej, Eric B. Flynn, Lili Yang, Claudia Moreno, N. V. Krishnendu, A. A. Ciobanu, J. Liu, A. Pasqualetti, Vivishek Sudhir, M. L. Lollie, F. Piergiovanni, P. J. Sutton, Lee McCuller, D. E. Cohen, Takuya Tsutsui, P. Gewecke, R. De Pietri, Rocco Romano, M. Kinley-Hanlon, M. Branchesi, Abhirup Ghosh, G. Kang, A. M. Holgado, Alena Ananyeva, C. Di Fronzo, J. Baird, M. Jeunon, B. Gateley, Aaron Buikema, L. A. Rees, Silvia Corezzi, V. Kondrashov, K. G. Arun, Rana X. Adhikari, Stanislav Babak, Peter Aufmuth, S. Sayah, A. E. Gleckl, Rajesh Kumar, M. Constancio, D. Y. T. Pong, S. Bae, M. Seglar-Arroyo, Nicolas Sanchis-Gual, J. H. Romie, Om Sharan Salafia, E. Coccia, G. Kuehn, C. C. Wipf, T. D. Abbott, F. J. Raab, Charalampos Markakis, Arunava Mukherjee, I. M. Pinto, I. La Rosa, Jean-René Cudell, Zoheyr Doctor, M. E. Zucker, B. A. Weaver, H. Vahlbruch, Gunnar Riemenschneider, J. C. Mills, K. Riles, J. Y. Vinet, H. Middleton, J. G. Rollins, E. Massera, Y. Asali, L.-W. 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Vander-Hyde, Xiuling Li, M. Caesar, V. Quetschke, H. Y. Chia, Umakant D. Rapol, G. S. Wallace, Stefan Hild, Kai Staats, L. Conti, Carl-Johan Haster, R. A. Eisenstein, A. M. Farah, M. F. Carney, C. L. Romel, A. F. Helmling-Cornell, Ajay Kumar, P. B. Covas, Aykutlu Dana, Martin M. Fejer, J. R. Smith, R. Bork, S. Ghonge, K. AultONeal, N. D. Ormsby, C. Whittle, M. Chaturvedi, A. R. Guimaraes, Hee-Suk Cho, Jishnu Suresh, V. Boschi, E. J. Son, A. Gennai, Harald P. Pfeiffer, D. L. Ferguson, Jian Li, I. Dorrington, Stephen Fairhurst, Carl Blair, I. Di Palma, A. Dmitriev, Walid Chaibi, J. Gais, Tristan Briant, Maria Luisa Chiofalo, Robert Bruntz, H. Radkins, Katerina Chatziioannou, D. J. McManus, S. D. Linker, M. Shikauchi, Archana Pai, P. Szewczyk, A. Malik, A. Brillet, A. Bozzi, L. Zhang, L. Prudenzi, T. Zelenova, F. Garufi, S. Gaudio, G. R. Johns, J. Bryant, K. Chandra, L. C. Strang, F. W. Yang, H. Vocca, L. Rolland, Surendra Nadh Somala, Riccardo Bassiri, Magnus Manske, M. van Beuzekom, M. 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J. van den Brand, S. Sunil, M. Tacca, P. G. Murray, Matthew Giesler, D. Moraru, Martin Hendry, Cecilio García-Quirós, M. C. Díaz, A. Menendez-Vazquez, N. Gohlke, Fabien Kéfélian, E. Floden, J. H. Hough, P. W. F. Forsyth, S. R. Thondapu, Gianpietro Cagnoli, J. R. Palamos, G. Baltus, P. Figura, C. M. Compton, Michele Zanolin, I. Magaña Hernandez, Antonios Kontos, Giuseppe Intini, T. J. Massinger, T. Vo, G. D. Hammond, A. Allocca, Javed Rana, P. Weßels, H. Yamamoto, F. Vetrano, Graham Woan, Robert L. Byer, Stuart Reid, F. J. Hayes, K. Soni, J. C. Driggers, A. M. Baer, A. Schönbeck, V. D'Emilio, Daniel Wysocki, I. A. O. MacMillan, Steven D. Penn, Jacob Scheuer, S. E. Dwyer, David Keitel, I. Michaloliakos, J. Betzwieser, Antoine Heidmann, N. Raza, Jonathan R. Gair, G. Pagano, Bernard F. Schutz, Li Ju, Brittany Kamai, A. Lartaux-Vollard, H. Overmier, Suvadeep Bose, B. Garaventa, R. Tenorio, N. A. Holland, D. Sellers, Carlos O. Lousto, C. V. Kalaghatgi, J. Hanson, R. Gouaty, A. V. Bhandari, Z. Márka, Jianfang Wang, Hang Yu, Riccardo Sturani, M. Merzougui, F. Kuei, L. Giacoppo, C. North, Thomas Dent, P. Corban, S. J. Cooper, Alberto Vecchio, Geoffrey Mo, James Whelan, P. Ajith, D. Schaetzl, J. M. Fishner, Will M. Farr, M. Montani, D. Sentenac, Patrick Brady, O. J. Piccinni, HyunGyu Suh, D. Davis, Nancy Aggarwal, A. Effler, E. Bonilla, K. Isleif, Kazuhiro Agatsuma, Frank Ohme, Vicky Kalogera, E. Leon, O. Halim, M. Tonelli, L. Xiao, P. Fulda, J. Smetana, D. Jariwala, I. Dave, Guoying Zhao, S. L. Nadji, R. Quitzow-James, N. N. Janthalur, B. Hughey, J. L. Willis, M. Eisenmann, Ofek Birnholtz, Monica Colpi, W. Griffiths, Eric Howell, Andrew Lundgren, W. S. Kim, M. Pracchia, S. Leavey, Hai-Ping Cheng, A. Iess, L. K. Nuttall, Veronica Granata, Yi-Ting Hsu, M. Haney, T. A. Callister, R. Macas, G. Billingsley, J. N. Hohmann, A. L. James, Jade Powell, V. Mangano, I. Belahcene, H. K. Gulati, Valeria Sipala, David H. Reitze, Rahul Kashyap, C. McIsaac, N. De Lillo, Francesco Pannarale, Soichiro Morisaki, M. Bals, A. Rocchi, Alejandro Torres-Forné, B. Goncharov, R. Birney, Aldo Ejlli, Maria Ilaria Del Principe, M. Agathos, Soumen Roy, J. Neilson, Stephane Perries, S. H. Huttner, Andrew Melatos, M. Lorenzini, J. H. Briggs, Mark Hannam, A. Strunk, N. Kijbunchoo, Sheelu Abraham, J. D. Bentley, V. Sequino, C. J. Richardson, H. J. Bulten, D. Griffith, C. M. Weller, Bala R. Iyer, S. McCormick, Haocun Yu, R. S. Bankar, M. C. Milovich-Goff, A. Mhaske, A. K. Mehta, P. J. Easter, Alessandra Corsi, D. Laghi, T. Huynh-Dinh, A. Z. Jan, Chunglee Kim, J. S. Kissel, H. Cao, Marc Favata, Roger Jones, V. J. Roma, Nikita S. Shcheblanov, A. P. Spencer, D. D. Brown, A. Depasse, N. van Bakel, J. D. Merritt, A. Masserot, K. Kawabe, E. J. Daw, Maurizio Canepa, Antonio Marquina, Eric Hennes, A. S. Ubhi, T. A. Ferreira, K. D. Giardina, S. M. Aston, K. Ueno, Michael W. Coughlin, I. Khan, L. E. Wade, J. K. Wofford, M. A. Page, Samuel Deléglise, A. Fernandez-Galiana, C. Pankow, Eric Grimes, P. M. Meyers, A. Branch, H. Masalehdan, M. Zevin, John Veitch, J. Lehmann, N. Arnaud, Vijay Varma, M. MacInnis, Rémi Soulard, P. Rapagnani, T. Mistry, Andreas Freise, Vincenzo Pierro, Paul D. Lasky, R. K. Hasskew, J. W. Westhouse, B. E. Ewing, Z. Mark, Matthew Pitkin, N. Bose, M. Granata, M. C. Tringali, Peter Graham Jones, T. Prestegard, R. Musenich, V. Spagnuolo, J. Scott, J. Lange, Sebastiano Bernuzzi, Simone Mozzon, Tania Regimbau, A. J. Tanasijczuk, K. W. Tsang, S. B. Anderson, K. M. Aleman, M. Kolstein, Zachariah B. Etienne, Gianluca Grignani, P. J. Veitch, Jennifer Watchi, D. Tsai, M. Boer, J. B. Kanner, M. Pedraza, A. Lockwood, F. Cavalier, Santosh Roy, H. Fong, G. Greco, Y. Bai, A. K. Divakarla, S. Hochheim, N. A. Robertson, J. G. Bartlett, David Jonathan Hofman, B. Nayak, Jonathan Blackman, P. Prosposito, K. Toland, Giacomo Bruno, José A. Font, N. Singh, M. Mateu-Lucena, D. P. Kapasi, J. McIver, Karsten Danzmann, Andrea H. Tapia, Javier Sánchez, E. Schwartz, A. W. Criswell, M. Punturo, Leopoldo Milano, Slawomir Gras, S. W. S. Ng, M. J. Szczepańczyk, Denis Martynov, Marco Bazzan, C. Ingram, G. Vajente, S. M. Gaebel, Alessandro Bertolini, J.-G. Ducoin, R. C. Walet, V. P. Mitrofanov, M. Diaz-Ortiz, J. Venneberg, W. Del Pozzo, P. F. Cohadon, H. Heitmann, D. Sawant, Matteo Pegoraro, Piero Rettegno, Laura Cadonati, Department of Science and Technology (India), Ministry of Human Resource Development (India), Agencia Estatal de Investigación (España), Govern de les Illes Balears, Generalitat de Catalunya, Foundation for Polish Science, European Commission, Scottish Funding Council, Hungarian Scientific Research Fund, Belgian Science Policy Office, National Research Foundation of Korea, Research Grants Council (Hong Kong), National Natural Science Foundation of China, Leverhulme Trust, Ministry of Science and Technology (Taiwan), Kavli Institute for Particle Astrophysics and Cosmology, LIGO Sci Collaboration, Virgo Collaboration, Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, A., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Aleman, K. M., Allen, G., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Aronson, S. M., Arun, K. G., Asali, Y., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Bae, S., Baer, A. M., Bagnasco, S., Bai, Y., Baird, J., Ball, M., Ballardin, G., Ballmer, S. W., Bals, M., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Bankar, R. S., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Becsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Benjamin, M. G., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bhandari, A. V., Bhattacharjee, D., Bhaumik, S., Bidler, J., Bilenko, I. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., 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., Bogaert, G., Boldrini, M., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Byer, R. L., Cadonati, L., Caesar, M., Cagnoli, G., Cahillane, C., Cain, H. W., Bustillo, J. C., Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, J., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carullo, G., Carver, T. L., Diaz, J. C., Casentini, C., Castaldi, G., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, W., Chakravarti, K., Champion, B., Chan, C. -H., Chan, C., Chan, C. L., Chandra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Chen, A., Chen, H. Y., Chen, J., Chen, X., Chen, Y., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choate, S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cieslar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colpi, M., Compton, C. M., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, 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., Cousins, B., Couvares, P., Covas, P. B., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cuoco, E., Curylo, M., Canton, T. D., Dalya, G., Dana, A., Daneshgaranbajastani, 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., Dean, R., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Del Pozzo, W., Demarchi, L. M., De Matteis, F., D'Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., De Simone, R., Dhurandhar, S., Diaz, M. C., Diaz-Ortiz, M., Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., D'Onofrio, L., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Drago, M., Driggers, J. C., Drori, Y., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., D'Urso, D., Duverne, P. -A., Dwyer, S. E., Easter, P. J., Ebersold, M., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Farrow, N. W., 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, T. A., Fidecaro, F., Figura, P., Fiori, I., Fishbach, M., Fisher, R. P., Fishner, J. M., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Flynn, E., Fong, H., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Frederick, C., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fronze, G. G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gaonkar, S. G., Garaventa, B., Garcia-Nunez, C., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Gemme, G., Gennai, A., George, J., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, A., Ghosh, S., Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., Gonzalez, G., Gopakumar, A., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Granata, V., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W., Griggs, H. L., Grignani, G., Grimaldi, A., Grimes, E., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guerrero, J. G., Guidi, G. M., Guimaraes, A. R., Guixe, G., Gulati, H. K., Guo, H. -K., Guo, Y., Gupta, A., Gupta, P., Gustafson, E. K., Gustafson, R., Guzman, F., Haegel, L., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Haskell, B., Hasskew, R. K., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Vivanco, F. H., Heurs, M., Hild, S., Hill, P., Hines, A. S., Hochheim, S., Hofman, D., Hohmann, J. N., Holgado, A. M., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hopkins, P., Hough, J., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsu, Y., Huang, Y., Hubner, M. T., Huddart, A. D., Huerta, E. A., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Intini, G., Isi, M., Isleif, K., Iyer, B. R., Jaberianhamedan, V., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jeunon, M., Jia, W., 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., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kefelian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, K., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knee, A. M., Knowles, T. D., Knyazev, E., Koch, P., Koekoek, G., Koley, S., Kolitsidou, P., Kolstein, M., Komori, K., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Kovalam, M., Kozak, D. B., Kringel, V., Krishnendu, N. V., Krolak, A., Kuehn, G., Kuei, F., Kumar, A., Kumar, P., Kumar, R., Kuns, K., Kwang, S., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lemaitre, A., Leon, E., Leroy, N., Letendre, N., Levin, Y., Leviton, J. N., Li, A. K. Y., Li, B., Li, J., Li, T. G. F., Li, X., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, J., Liu, K., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., Lollie, M. L., London, L. T., Longo, A., Lopez, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Luck, H., Lumaca, D., Lundgren, A. P., Macas, R., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., Hernandez, I. M., Magana-Sandoval, F., Magazzu, C., Magee, R. M., Maggiore, R., Majorana, E., Maksimovic, I., Maliakal, S., Malik, A., Man, N., Mandic, V., Mangano, V., Mango, J. L., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Mark, Z., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, M., Martinez, V., Martinovic, K., Martynov, D. V., Marx, E. J., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matichard, F., Matiushechkina, M., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mcclincy, P., Mccormick, S., Mcculler, L., Mcghee, G. I., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., 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., Mir, L. M., Mishkin, A., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina, I., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moraru, D., Morawski, F., More, A., Moreno, C., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Murray, P. G., Musenich, R., Nadji, S. L., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, B., Nayak, R. K., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S. W. S., Nguyen, C., Nguyen, P., Nguyen, T., Nichols, S. A., Nissanke, S., Nocera, F., Noh, M., Norman, M., North, C., Nuttall, L. K., Oberling, J., O'Brien, B. D., O'Dell, J., Oganesyan, G., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Olivetto, C., Oram, R., O'Reilly, B., Ormiston, R. G., Ormsby, N. D., Ortega, L. F., O'Shaughnessy, R., O'Shea, E., Ossokine, S., Osthelder, C., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Panda, P. K., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Paolone, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Patricelli, B., Payne, E., Pechsiri, T. C., Pedraza, M., Pegoraro, M., Pele, A., Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Perigois, C., Perreca, A., Perries, S., Petermann, J., Petterson, D., Pfeiffer, H. P., Pham, K. A., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierini, L., Pierro, V., Pillant, G., Pilo, F., Pinard, L., Pinto, I. M., Piotrzkowski, B. J., Piotrzkowski, K., Pirello, M., Pitkin, M., Placidi, E., Plastino, W., Pluchar, C., Poggiani, R., Polini, E., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Pracchia, M., Pradier, T., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Principe, M., Prodi, G. A., Prokhorov, L., Prosposito, P., Prudenzi, L., Puecher, A., Punturo, M., Puosi, F., Puppo, P., Purrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quitzow-James, R., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rail, S. X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, J., Rapagnani, P., Rapol, U. D., Ratto, B., Raymond, V., Raza, N., Razzano, M., Read, J., Rees, L. A., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Relton, P., Rettegno, P., Ricci, F., Richardson, C. J., Richardson, J. W., Richardson, L., Ricker, P. M., Riemenschneider, G., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rocha, J. A., Rodriguez, S., Rodriguez-Soto, R. D., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romero, A., Romero-Shaw, I. M., Romie, J. H., Rose, C. A., Rosinska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, S., Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sakellariadou, M., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sassolas, B., Satari, H., Sauter, O., Savage, R. 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W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tsutsui, T., Turconi, M., Ubhi, A. S., Udall, R. P., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Utina, A. C., Vahlbruch, H., Vajente, G., Vajpeyi, A., Valdes, G., Valentini, M., Valsan, V., 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., Vardaro, M., Vargas, A. F., Varma, V., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venneberg, J., Venugopalan, G., Verkindt, D., Verma, Y., Veske, D., Vetrano, F., Vicere, A., Viets, A. D., Villa-Ortega, V., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Von Reis, E. R. G., Von Wrangel, J., Vorvick, C., Vyatchanin, S. P., Wade, L. E., Wade, M., Wagner, K. J., Walet, R. C., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J. Z., Wang, W. H., Ward, R. L., Warner, J., Was, M., Washington, N. 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Chu, Q, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cieslar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colpi, M, Compton, C, 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, Cousins, B, Couvares, P, Covas, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cuoco, E, Curylo, M, Canton, T, Dalya, G, Dana, A, Daneshgaranbajastani, 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, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, Demarchi, L, De Matteis, F, D'Emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, Diaz, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D'Onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Du, Z, Ducoin, J, Dupej, P, Durante, O, D'Urso, D, Duverne, P, Dwyer, S, Easter, P, Ebersold, M, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, 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, Fair, H, Fairhurst, S, Fan, X, Farah, A, Farinon, S, Farr, B, Farr, W, Farrow, N, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, 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Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
binary: orbit, neutron star: binary, Physics and Astronomy (miscellaneous), Astronomy, binary [neutron star], Astrophysics, Gravitational Waves, LIGO (Observatory), Neutron Stars, 01 natural sciences, neutron stars, General Relativity and Quantum Cosmology, Monte Carlo: Markov chain, Physics, Particles & Fields, binary stars, binary systems, Binary Systems, LIGO, gravitational wave, QC, QB, pulsar, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Settore FIS/03, orbit [binary], General relativity, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, binary star, data analysis method, sensitivity [detector], gr-qc, frequency [modulation], Population, neutron star: spin, FOS: Physical sciences, alternative theories of gravity, Markov chain [Monte Carlo], General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, Gravitational Waves, Neutron Stars, Binary Systems, LIGO, Virgo, emission [gravitational radiation], Pulsar, binary: coalescence, 0103 physical sciences, Binary star, ddc:530, spin [neutron star], background [gravitational radiation], 010306 general physics, education, STFC, Orbital elements, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, Virgo, gravitational radiation: background, modulation: frequency, RCUK, gravitational radiation detector, detector: sensitivity, Neutron star, VIRGO, gravitational radiation: emission, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, coalescence [binary], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Rapidly spinning neutron stars are promising sources of continuous gravitational waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of the known pulsar population belongs to binary systems. Searching for unknown neutron stars in binary systems requires specialized algorithms to address unknown orbital frequency modulations. We present a search for continuous gravitational waves emitted by neutron stars in binary systems in early data from the third observing run of the Advanced LIGO and Advanced Virgo detectors using the semicoherent, GPU-accelerated, binaryskyhough pipeline. The search analyzes the most sensitive frequency band of the LIGO detectors, 50-300 Hz. Binary orbital parameters are split into four regions, comprising orbital periods of three to 45 days and projected semimajor axes of two to 40 light seconds. No detections are reported. We estimate the sensitivity of the search using simulated continuous wave signals, achieving the most sensitive results to date across the analyzed parameter space., 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, the Conselleria d’Educació i Universitat and the Direcció General de Política Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, the Barcelona Supercomputing Center—Centro Nacional de Supercomputación, Spain, the National Science Centre of Poland, and the Foundation for Polish Science (FNP), 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 French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, 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, the U.S. DOE, and the Kavli Foundation.

Published
2021
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16. Improved statistic to identify strongly lensed gravitational wave events

Author

Anupreeta More and Surhud More

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

As the number of detected gravitational wave sources increase with increasing sensitivity of the gravitational wave observatories, observing strongly lensed pair of events will become a real possibility. Lensed GW events will have very accurately measured time delays, as well as magnification ratios. If the corresponding lens system can be identified electromagnetically and the redshifts of the lens and the host galaxy can be measured, such events can be used to constrain important astrophysical parameters of the lens system. As most lensing events will have image separations that will be significantly smaller than the GW event localization uncertainties, it is important that we develop diagnostics that will aid in the robust identification of such lensed events. We define a new statistic based on the joint probability of lensing observables that can be used to discriminate lensed pair of events from the unlensed ones. To this end, we carry out simulations of lensed GW events to infer the distribution of the relative time delays, relative magnifications sub-divided by the type of lensed images. We compare this distribution to a similar one obtained for random unlensed event pairs. Our improved statistic can be used to improve the existing ranking approach adopted by the search pipelines in order to down-select event pairs for joint parameter estimates. The distributions we obtain can further be used to define more informative priors in joint parameter estimation analyses for candidate lensed events., Comment: 8 pages, 6 figures

Published
2021
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17. Survey of Gravitationally Lensed Objects in HSC Imaging (SuGOHI)

Author

Cristian Rusu, Issha Kayo, Anupreeta More, Alessandro Sonnenfeld, Naohisa Inada, John D. Silverman, Paul L. Schechter, Anton T. Jaelani, Masamune Oguri, Daichi Kondo, M. Schramm, Kenneth C. Wong, James H. H. Chan, Kaiki Taro Inoue, Timo Anguita, and Khee Gan Lee

Subjects
ii, Gravitational lensing: strong, media_common.quotation_subject, Astrophysics - astrophysics of galaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Methods: observational, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, dark energy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, search, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Quasar, space warps, cosmos, Methods observational, Galaxy, Redshift, 1st data release, x-ray, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), digital sky survey, constraints, camera
Abstract

We present spectroscopic confirmation of three new two-image gravitationally lensed quasars, compiled from existing strong lens and X-ray catalogs. Images of HSC J091843.27$-$022007.5 show a red galaxy with two blue point sources at either side, separated by 2.26 arcsec. This system has a source and a lens redshifts $z_s=0.804$ and $z_{\ell}=0.459$, respectively, as obtained by our follow-up spectroscopic data. CXCO J100201.50$+$020330.0 shows two point sources separated by 0.85 arcsec on either side of an early-type galaxy. The follow-up spectroscopic data confirm the fainter quasar has the same redshift with the brighter quasar from the SDSS fiber spectrum at $z_s=2.016$. The deflecting foreground galaxy is a typical early-type galaxy at a redshift of $z_{\ell}=0.439$. SDSS J135944.21$+$012809.8 has two point sources with quasar spectra at the same redshift $z_s=1.096$, separated by 1.05 arcsec, and fits to the HSC images confirm the presence of a galaxy between these. These discoveries demonstrate the power of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP)'s deep imaging and wide sky coverage. Combined with existing X-ray source catalogues and follow-up spectroscopy, the HSC-SSP provides us unique opportunities to find multiple-image quasars lensed by a foreground galaxy., Comment: Accepted for publication in MNRAS, 7 pages, 3 figures (add credit to Claude Cornen)

Published
2021

18. Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI) - V. Group-to-cluster scale lens search from the HSC-SSP survey

Author

Sherry H. Suyu, Issha Kayo, Alessandro Sonnenfeld, Kenneth C. Wong, Toshifumi Futamase, Cristian E. Rusu, Anton T. Jaelani, Anupreeta More, Jean Coupon, James H. H. Chan, Chien-Hsiu Lee, Masamune Oguri, Kaiki Taro Inoue, and D. C. Y. Chao

Subjects
ii, candidates, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, acs survey, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Gravitation, surveys, law, 0103 physical sciences, Cluster (physics), early-type galaxies, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, substructure, 010308 nuclear & particles physics, Group (mathematics), gravitational lensing: strong, Astronomy and Astrophysics, space warps, initial mass function, Astrophysics - Astrophysics of Galaxies, Redshift, Lens (optics), dark-matter, Space and Planetary Science, galaxies: clusters: general, kinematics, Astrophysics of Galaxies (astro-ph.GA), methods: observational, Data release, discovery
Abstract

We report the largest sample of candidate strong gravitational lenses belonging to the Survey of Gravitationally-lensed Objects in HSC Imaging for group-to-cluster scale (SuGOHI-c) systems. These candidates are compiled from the S18A data release of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) Survey. We visually inspect $\sim39,500$ galaxy clusters, selected from several catalogs, overlapping with the Wide, Deep, and UltraDeep fields, spanning the cluster redshift range $0.05, Comment: Accepted for publication in MNRAS, 19 pages, 11 figures

Published
2020

19. Discovery of an unusually compact lensed Lyman-break galaxy from the Hyper Suprime-Cam Survey

Author

Cristian E. Rusu, Kenneth C. Wong, Kaiki Taro Inoue, Masamune Oguri, Anupreeta More, Chien-Hsiu Lee, James H. H. Chan, Anton T. Jaelani, Sherry H. Suyu, Issha Kayo, and Alessandro Sonnenfeld

Subjects
Active galactic nucleus, population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Einstein radius, galaxies: high-redshift, gas, cosmic eye, emission, 0103 physical sciences, luminosity function, Absorption (logic), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, hubble, star-formation, 010308 nuclear & particles physics, Image (category theory), gravitational lensing: strong, resolution, Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, redshift z-similar-to-3, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Lyman-break galaxy, ultraviolet-spectrum
Abstract

We report the serendipitous discovery of HSC J0904$-$0102, a quadruply-lensed Lyman break galaxy (LBG) in the Survey of Gravitationally-lensed Objects in Hyper Suprime-Cam Imaging (SuGOHI). Owing to its point-like appearance, the source was thought to be a lensed active galactic nucleus. We obtained follow-up spectroscopic data with the Gemini Multi-Object Spectrographs on the Gemini South Telescope, which confirmed this to be a lens system. The deflecting foreground galaxy is a typical early-type galaxy at a high redshift of $z_{\ell} = 0.957$ with stellar velocity dispersion $\sigma_v=259\pm56$ km~s$^{-1}$. The lensed source is identified as an LBG at $z_{\rm s} = 3.403$, based on the sharp drop bluewards of Ly$\alpha$ and other absorption features. A simple lens mass model for the system, assuming a singular isothermal ellipsoid, yields an Einstein radius of $\theta_{\rm Ein} = 1. 23^{\prime\prime}$ and a total mass within the Einstein radius of $M_{\rm Ein} = (5.55\pm 0.24) \times 10^{11}M_{\odot}$ corresponding to a velocity dispersion of $\sigma_{\rm SIE}= 283\pm 3$ km~s$^{-1}$, which is in good agreement with the value derived spectroscopically. The most isolated lensed LBG image has a magnification of $\sim 6.5$. In comparison with other lensed LBGs and typical $z\sim4$ LBG populations, HSC J0904$-$0102 is unusually compact, an outlier at $>2\sigma$ confidence. Together with a previously discovered SuGOHI lens, HSC J1152$+$0047, that is similarly compact, we believe that the HSC Survey is extending LBG studies down to smaller galaxy sizes., Comment: Accepted for publication on MNRAS, 10 pages, 6 figures

Published
2020
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20. Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI)

Author

Alessandro Sonnenfeld, Aprajita Verma, Anupreeta More, Elisabeth Baeten, Christine Macmillan, Kenneth C. Wong, James H. H. Chan, Anton T. Jaelani, Chien-Hsiu Lee, Masamune Oguri, Cristian E. Rusu, Marten Veldthuis, Laura Trouille, Philip J. Marshall, Roger Hutchings, Campbell Allen, James O’ Donnell, Claude Cornen, Christopher P. Davis, Adam McMaster, Chris Lintott, Grant Miller

Published
2020
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21. STRIDES: a 3.9 per cent measurement of the Hubble constant from the strong lens system DES J0408-5354

Author

Frederic Courbin, R. L. C. Ogando, M. Costanzi, Elisabeth Krause, Anupreeta More, Marcelle Soares-Santos, I. Sevilla-Noarbe, Antonella Palmese, Daniel Thomas, E. Buckley-Geer, M. A. G. Maia, N. Kuropatkin, David J. Brooks, Matthew W. Auger, B. Flaugher, M. Millon, Keith Bechtol, F. J. Castander, L. N. da Costa, Simon Birrer, A. Roodman, J. Poh, J. Gschwend, T. M. C. Abbott, G. Gutierrez, V. Scarpine, M. Sako, Daniel Scolnic, Peter Doel, Peter Melchior, D. L. Hollowood, S. Serrano, Basilio X. Santiago, A. R. Walker, G. Tarle, Timo Anguita, E. J. Sanchez, Ramon Miquel, A. K. Romer, Christopher D. Fassnacht, D. Brout, Anowar J. Shajib, Yanxi Zhang, Thomas E. Collett, Jennifer L. Marshall, Daniel Gilman, Marcos Lima, Joshua A. Frieman, Tenglin Li, Dominique Sluse, Tommaso Treu, E. Suchyta, Niall MacCrann, Geoff C. F. Chen, August E. Evrard, D. A. Finley, F. Paz-Chinchón, J. Carretero, J. De Vicente, Chiara Spiniello, Kenneth C. Wong, S. Desai, Cristian Rusu, A. Galan, M. Carrasco Kind, Richard G. McMahon, James H. H. Chan, J. P. Dietrich, Juan Garcia-Bellido, C. Lemon, Alex Drlica-Wagner, Dragan Huterer, J. Annis, Lise Christensen, M. Smith, Daniel Gruen, D. W. Gerdes, A. A. Plazas, D. L. Burke, Robert A. Gruendl, Huan Lin, Tesla E. Jeltema, K. Honscheid, Adriano Agnello, A. Carnero Rosell, G. Meylan, David J. James, Pablo Fosalba, Salcedo Romero de Ávila, Vivien Bonvin, Michael Schubnell, National Science Foundation (US), Danish Council for Independent Research, Villum Fonden, Swiss National Science Foundation, European Commission, Ministry of Education (Taiwan), Ministry of Education, Culture, Sports, Science and Technology (Japan), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Department of Energy (US), Shajib, A. J., Birrer, S., Treu, T., Agnello, A., Buckley-Geer, E. J., Chan, J. H. H., Christensen, L., Lemon, C., Lin, H., Millon, M., Poh, J., Rusu, C. E., Sluse, D., Spiniello, C., Chen, G. C. -F., Collett, T., Courbin, F., Fassnacht, C. D., Frieman, J., Galan, A., Gilman, D., More, A., Anguita, T., Auger, M. W., Bonvin, V., Mcmahon, R., Meylan, G., Wong, K. C., Abbott, T. M. C., Annis, J., Avila, S., Bechtol, K., Brooks, D., Brout, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi Alunno Cerbolini, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Jeltema, T., Krause, E., Kuropatkin, N., Li, T. S., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Melchior, P., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Walker, A. R., Zhang, Y., McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), time delays, Cosmic microwave background, Cosmological parameters, internal structure, h-0, FOS: Physical sciences, Astrophysics, acs survey, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, strong [Gravitational lensing], 01 natural sciences, 7. Clean energy, Cosmology, law.invention, symbols.namesake, models, multi-gaussian expansion, law, 0103 physical sciences, cosmological parameters, observations [Cosmology], 010303 astronomy & astrophysics, STFC, gravitational lensing: strong, cosmology: observations, Physics, Distance scale, 010308 nuclear & particles physics, Angular diameter distance, Cosmic distance ladder, RCUK, Astronomy and Astrophysics, Quasar, density profile, elliptic galaxies, Redshift, Lens (optics), stellar-systems, Space and Planetary Science, symbols, astro-ph.CO, mass, cosmological parameter, Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Full author list: A J Shajib, S Birrer, T Treu, A Agnello, E J Buckley-Geer, J H H Chan, L Christensen, C Lemon, H Lin, M Millon, J Poh, C E Rusu, D Sluse, C Spiniello, G C-F Chen, T Collett, F Courbin, C D Fassnacht, J Frieman, A Galan, D Gilman, A More, T Anguita, M W Auger, V Bonvin, R McMahon, G Meylan, K C Wong, T M C Abbott, J Annis, S Avila, K Bechtol, D Brooks, D Brout, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, M Costanzi, L N da Costa, J De Vicente, S Desai, J P Dietrich, P Doel, A Drlica-Wagner, A E Evrard, D A Finley, B Flaugher, P Fosalba, J García-Bellido, D W Gerdes, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, D L Hollowood, K Honscheid, D Huterer, D J James, T Jeltema, E Krause, N Kuropatkin, T S Li, M Lima, N MacCrann, M A G Maia, J L Marshall, P Melchior, R Miquel, R L C Ogando, A Palmese, F Paz-Chinchón, A A Plazas, A K Romer, A Roodman, M Sako, E Sanchez, B Santiago, V Scarpine, M Schubnell, D Scolnic, S Serrano, I Sevilla-Noarbe, M Smith, M Soares-Santos, E Suchyta, G Tarle, D Thomas, A R Walker, Y Zhang, We present a blind time-delay cosmographic analysis for the lens system DES J0408-5354. This system is extraordinary for the presence of two sets of multiple images at different redshifts, which provide the opportunity to obtain more information at the cost of increased modelling complexity with respect to previously analysed systems. We perform detailed modelling of the mass distribution for this lens system using three band Hubble Space Telescope imaging. We combine the measured time delays, line-of-sight central velocity dispersion of the deflector, and statistically constrained external convergence with our lens models to estimate two cosmological distances. We measure the 'effective' time-delay distance corresponding to the redshifts of the deflector and the lensed quasar DΔ t eff=3382-115+146 Mpc and the angular diameter distance to the deflector Dd = 1711-280+376 Mpc, with covariance between the two distances. From these constraints on the cosmological distances, we infer the Hubble constant H0= 74.2-3.0+2.7 km s-1 Mpc-1 assuming a flat ΛCDM cosmology and a uniform prior for ωm as \Omega m ∼ \mathcal {U(0.05, 0.5). This measurement gives the most precise constraint on H0 to date from a single lens. Our measurement is consistent with that obtained from the previous sample of six lenses analysed by the H0 Lenses in COSMOGRAIL's Wellspring (H0LiCOW) collaboration. It is also consistent with measurements of H0 based on the local distance ladder, reinforcing the tension with the inference from early Universe probes, for example, with 2.2σ discrepancy from the cosmic microwave background measurement., TT acknowledges support by the Packard Foundation through a Packard Research fellowship and by the National Science Foundation through NSF grants AST-1714953 and AST-1906976. This project is partly funded by the Danish council for independent research under the project ‘Fundamentals of Dark Matter Structures’, DFF - 6108-00470. AA was supported by a grant from VILLUM FONDEN (project number 16599). JHHC, MM, CL, DS, FC, and AG acknowledge support from the Swiss National Science Foundation (SNSF) and by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (COSMICLENS: grant agreement No 787866). CS has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie actions grant agreement No 664931. GCFC acknowledges support from the Ministry of Education in Taiwan via Government Scholarship to Study Abroad (GSSA). CDF and GCFC acknowledge support for this work from the National Science Foundation under Grant No AST-1715611. TA acknowledges support from Proyecto FONDECYT N○ 1190335. KCW was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. This work used computational and storage services associated with the Hoffman2 Shared Cluster provided by UCLA Institute for Digital Research and Education’s Research Technology Group. This work used the Extreme Science and Engineering Discovery Environment (XSEDE) through allocation TG-AST190038, which is supported by National Science Foundation grant number ACI-1548562 (Towns et al. 2014). Specifically, this work used the Comet and Oasis system at the San Diego Supercomputer Center (SDSC), and the Bridges system, which is supported by NSF award number ACI-1445606, at the Pittsburgh Supercomputing Center (PSC, Nystrom et al. 2015). AJS thanks Smadar Naoz for providing access to additional computing nodes on the Hoffman2 Shared Cluster and Khalid Jawed for assisting with additional computational resources from the Structures–Computer Interaction Laboratory at UCLA. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Published
2020
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22. Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI). VI. Crowdsourced lens finding with Space Warps

Author

Anton T. Jaelani, James H. H. Chan, Marten Veldthuis, Alessandro Sonnenfeld, Grant Miller, Christopher P. Davis, Cristian E. Rusu, Adam McMaster, Masamune Oguri, Chien-Hsiu Lee, Campbell Allen, Christine Macmillan, Roger Hutchings, Chris Lintott, Philip J. Marshall, Kenneth C. Wong, Elisabeth Baeten, Claude Cornen, Laura Trouille, Aprajita Verma, Anupreeta More, and James O' Donnell

Subjects
Initial mass function, limit, Sample (material), dark-matter contraction, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space (commercial competition), Crowdsourcing, 01 natural sciences, law.invention, law, 0103 physical sciences, Computer vision, early-type galaxies, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, substructure, 010308 nuclear & particles physics, business.industry, gravitational lensing: strong, Astronomy and Astrophysics, initial mass function, i, Redshift, Galaxy, cd, Lens (optics), Space and Planetary Science, cfhtlens, Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysics, business, discovery
Abstract

Strong lenses are extremely useful probes of the distribution of matter on galaxy and cluster scales at cosmological distances, but are rare and difficult to find. The number of currently known lenses is on the order of 1,000. We wish to use crowdsourcing to carry out a lens search targeting massive galaxies selected from over 442 square degrees of photometric data from the Hyper Suprime-Cam (HSC) survey. We selected a sample of $\sim300,000$ galaxies with photometric redshifts in the range $0.2 < z_{phot} < 1.2$ and photometrically inferred stellar masses $\log{M_*} > 11.2$. We crowdsourced lens finding on this sample of galaxies on the Zooniverse platform, as part of the Space Warps project. The sample was complemented by a large set of simulated lenses and visually selected non-lenses, for training purposes. Nearly 6,000 citizen volunteers participated in the experiment. In parallel, we used YattaLens, an automated lens finding algorithm, to look for lenses in the same sample of galaxies. Based on a statistical analysis of classification data from the volunteers, we selected a sample of the most promising $\sim1,500$ candidates which we then visually inspected: half of them turned out to be possible (grade C) lenses or better. Including lenses found by YattaLens or serendipitously noticed in the discussion section of the Space Warps website, we were able to find 14 definite lenses, 129 probable lenses and 581 possible lenses. YattaLens found half the number of lenses discovered via crowdsourcing. Crowdsourcing is able to produce samples of lens candidates with high completeness and purity, compared to currently available automated algorithms. A hybrid approach, in which the visual inspection of samples of lens candidates pre-selected by discovery algorithms and/or coupled to machine learning is crowdsourced, will be a viable option for lens finding in the 2020s., Published version

Published
2020
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25. Lensed quasar search via time variability with the HSC transient survey

Author

Anton T. Jaelani, Tomoki Morokuma, James H. H. Chan, Anupreeta More, Sherry H. Suyu, Naoki Yasuda, D. C. Y. Chao, and Masamune Oguri

Subjects
Point spread function, Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, techniques: image processing, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, black-holes, law.invention, law, Search algorithm, Observatory, galaxies, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, cosmic evolution, Astrophysics::Galaxy Astrophysics, Physics, substructure, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational lensing: strong, space warps, Astronomy and Astrophysics, Quasar, methods: data analysis, sample, Astrophysics - Astrophysics of Galaxies, Galaxy, candidate selection, Lens (optics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), gaia, digital sky survey, Astrophysics - Instrumentation and Methods for Astrophysics, discovery, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitationally lensed quasars are useful for studying astrophysics and cosmology, and enlarging the sample size of lensed quasars is important for multiple studies. In this work, we develop a lens search algorithm for four-image (quad) lensed quasars based on their time variability. In the development of the lens search algorithm, we constructed a pipeline simulating multi-epoch images of lensed quasars in cadenced surveys, accounting for quasar variabilities, quasar hosts, lens galaxies, and the PSF variation. Applying the simulation pipeline to the Hyper Suprime-Cam (HSC) transient survey, we generated HSC-like difference images of the mock lensed quasars from Oguri & Marshall's lens catalog. We further developed a lens search algorithm that picks out variable objects as lensed quasar candidates based on their spatial extent in the difference images. We tested our lens search algorithm with the mock lensed quasars and variable objects from the HSC transient survey. Using difference images from multiple epochs, our lens search algorithm achieves a high true-positive rate (TPR) of 90.1% and a low false-positive rate (FPR) of 2.3% for the bright quads with wide separation. With a preselection of the number of blobs in the difference image, we obtain a TPR of 97.6% and a FPR of 2.6% for the bright quads with wide separation. Even when difference images are only available in one single epoch, our lens search algorithm can still detect the bright quads with wide separation at high TPR of 97.6% and low FPR of 2.4% in the optimal seeing scenario, and at TPR of $\sim94%$ and FPR of $\sim5%$ in typical scenarios. Therefore, our lens search algorithm is promising and is applicable to ongoing and upcoming cadenced surveys, particularly the HSC transient survey and the Rubin Observatory Legacy Survey of Space and Time, for finding new lensed quasar systems. [abridged], 15 pages, 11 figures

Published
2020
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26. Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI)

Author

Anton T. Jaelani, Kenneth C. Wong, Yuriko Kubota, James H. H. Chan, Cristian E. Rusu, Atsunori Yonehara, Alessandro Sonnenfeld, Sherry H. Suyu, Anupreeta More, Masamune Oguri, Chien-Hsiu Lee, and Jean Coupon

Subjects
Physics, Mass distribution, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Cosmology, Galaxy, Redshift, law.invention, Lens (optics), Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, Emission spectrum, 010303 astronomy & astrophysics
Abstract

Strong gravitationally lensed quasars provide powerful means to study galaxy evolution and cosmology. We use Chitah to hunt for new lens systems in the Hyper Suprime$-$Cam Subaru Strategic Program (HSC SSP) S16A. We present 46 lens candidates, of which 3 are previously known. Including 2 additional lenses found by YattaLens, we obtain X-shooter spectra of 6 promising candidates for lens confirmation and redshift measurements. We report new spectroscopic redshift measurements for both the lens and source galaxies in 4 lens systems. We apply the lens modeling software Glee to model our 6 X-shooter lenses uniformly. Through our analysis of the HSC images, we find that HSCJ022622$-$042522, HSCJ115252$+$004733, and HSCJ141136$-$010216 have point-like lensed images, and that the lens light distribution is well aligned with mass distribution within 6 deg. Thanks to the X-shooter spectra, we estimate fluxes on the Baldwin- Phillips-Terlevich (BPT) diagram, and find that HSCJ022622$-$042522 has a probable quasar source, based on the upper limit of the Nii flux intensity. We also measure the FWHM of Ly$\alpha$ emission of HSCJ141136$-$010216 to be $\sim$254 km/s, showing that it is a probable Lyman-$\alpha$ emitter., Comment: 13 pages, 7 figures

Published
2020
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27. A Search for Gravitationally Lensed Quasars and Quasar Pairs in Pan-STARRS1: Spectroscopy and Sources of Shear in the Diamond 2M1134$-$2103

Author

George J. Nelson, Erica Seman, Cristian E. Rusu, Christopher D. Fassnacht, Anupreeta More, Geoff C. F. Chen, and Ciprian T. Berghea

Subjects
Physics, Brightness, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Galaxy group, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Cluster (physics), 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present results of a systematic search for gravitationally lensed quasars in Pan-STARRS1. Our final sample of candidates comprises of 91 systems, not including 25 rediscovered lensed quasars and quasar pairs. In the absence of spectroscopy to verify the lensing nature of the candidates, the main sources of contaminants are likely to be quasar pairs, which we consider to be a byproduct of our work, and a smaller number of quasar$+$star associations. Amongst the independently discovered quads is 2M1134$-$2103, for which we obtained spectroscopy for the first time, finding a redshift of 2.77 for the quasar. There is evidence for microlensing in at least one image. We perform detailed mass modeling of this system using archival imaging data, and find that the unusually large shear responsible for the diamond-like configuration can be attributed mainly to a faint companion $\sim 4''$ away, and to a galaxy group/cluster $\sim 30''$ away. We also set limits of $z\sim0.5-1.5$ on the redshift of the lensing galaxy, based on its brightness, the image separation of the lensed images, and an analysis of the observed photometric flux ratios., Accepted by MNRAS. Based on feedback from the referee, the final sample of candidates is significantly different from the one in the previous submission. 15 pages + 4 pages of appendix, 7 figures, 3 tables

Published
2018

28. SDSS-IV MaNGA: the spectroscopic discovery of strongly lensed galaxies

Author

Alessandro Sonnenfeld, Anupreeta More, Brett H. Andrews, Kyle B. Westfall, Kevin Bundy, Simona Vegetti, Adam S. Bolton, Thomas E. Collett, David A. Wake, Joel R. Brownstein, Brian Cherinka, Michael S. Talbot, Anne-Marie Weijmans, Surhud More, The Leverhulme Trust, and University of St Andrews. School of Physics and Astronomy

Subjects
media_common.quotation_subject, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, strong [Gravitational lensing], 01 natural sciences, Spectral line, law.invention, Einstein radius, law, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, media_common, QB, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, general [Galaxies], DAS, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Lens (optics), Gravitational lens, QC Physics, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for 8 of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with 2 background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched ~ 1.5 million spectra, of which 3065 contained multiple high signal-to-noise background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius > 1.7", which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely., Accepted for publication in MNRAS, March 8, 2018. In press. 16 pages, 5 figures, 4 tables

Published
2018
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29. Models of gravitational lens candidates from Space Warps CFHTLS

Author

Rafael Küng, Prasenjit Saha, Lucy Oswald, Elisabeth Baeten, Julianne K. Wilcox, Jonathan P. Coles, Anupreeta More, Ignacio Ferreras, Christine Macmillan, Claude Cornen, Aprajita Verma, Phil Marshall, and University of Zurich

Subjects
Stellar mass, 530 Physics, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 10192 Physics Institute, 01 natural sciences, law.invention, Telescope, 1912 Space and Planetary Science, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, Star formation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Lens (optics), Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Halo
Abstract

We report modelling follow-up of recently-discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially-interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorised according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from ~10^11 Msun to >10^13 Msun. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above ~10^11 Msun. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW05). The two low-mass outliers are J0206-095 (SW19) and J2217+015 (SW42); if these two are indeed lenses, they probe an interesting regime of very low star-formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included., 16 pages, 10 figures, 1 table, online supplement table_1.csv contains additional detailed numbers shown in table 1 and figure 7

Published
2018

30. DES meets Gaia: discovery of strongly lensed quasars from a multiplet search

Author

David J. James, B. Flaugher, V. Scarpine, Adriano Agnello, N. D. Morgan, Karl Glazebrook, A. Carnero Rosell, T. M. C. Abbott, Veronica Motta, Matthew W. Auger, Nikolay Kuropatkin, R. H. Schindler, Michael Schubnell, Enrique Gaztanaga, E. Buckley-Geer, Shantanu Desai, E. J. Sanchez, Tommaso Treu, J. Gschwend, David Brooks, M. E. C. Swanson, Ofer Lahav, Paul L. Schechter, D. L. Burke, Marcos Lima, R. A. Bernstein, Flavia Sobreira, Timo Anguita, G. Gutierrez, I. Sevilla-Noarbe, Ricardo L. C. Ogando, Anupreeta More, E. Bertin, L. N. da Costa, A. A. Plazas, Philip J. Marshall, Brian Nord, K. Honscheid, Juan Garcia-Bellido, Alex Drlica-Wagner, Ramon Miquel, Christopher D. Fassnacht, C. B. D'Andrea, E. Suchyta, Marcelle Soares-Santos, Risa H. Wechsler, Douglas L. Tucker, Kyler Kuehn, Joshua A. Frieman, Robert A. Gruendl, M. March, J. Annis, Sherry H. Suyu, Filipe B. Abdalla, Felipe Menanteau, Gregory Tarle, Adam Amara, Carlos E. Cunha, Tim Eifler, Frederic Courbin, Takahiro Morishita, Huan Lin, K. Benoit-Lévy, K. Bechtol, K. Rojas, Georges Meylan, J. Carretero, Richard G. McMahon, M. Smith, Daniel Gruen, D. W. Gerdes, Marcio A. G. Maia, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, techniques: image processing, Astrophysics, Surveys, strong [Gravitational lensing], 01 natural sciences, law.invention, Einstein radius, surveys, law, 0103 physical sciences, image processing [Techniques], 010303 astronomy & astrophysics, Multiplet, Physics, methods: statistical, Simple lens, 010308 nuclear & particles physics, Astronomy, gravitational lensing: strong, Astronomy and Astrophysics, Quasar, Radius, Astrophysics - Astrophysics of Galaxies, Redshift, Lens (optics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery, spectroscopic confirmation and first lens models of the first two, strongly lensed quasars from a combined search in WISE and Gaia over the DES footprint. The four-image lensWGD2038-4008 (r.a.=20:38:02.65, dec.=-40:08:14.64) has source- and lens-redshifts $z_{s}=0.777 \pm 0.001$ and $z_l = 0.230 \pm 0.002$ respectively. Its deflector has effective radius $R_{\rm eff} \approx 3.4^{\prime\prime}$, stellar mass $\log(M_{\star}/M_{\odot}) = 11.64^{+0.20}_{-0.43}$, and shows extended isophotal shape variation. Simple lens models yield Einstein radii $R_{\rm E}=(1.30\pm0.04)^{\prime\prime},$ axis ratio $q=0.75\pm0.1$ (compatible with that of the starlight) and considerable shear-ellipticity degeneracies. The two-image lensWGD2021-4115 (r.a.=20:21:39.45, dec.=--41:15:57.11) has $z_{s}=1.390\pm0.001$ and $z_l = 0.335 \pm 0.002$, and Einstein radius $R_{\rm E} = (1.1\pm0.1)^{\prime\prime},$ but higher-resolution imaging is needed to accurately separate the deflector and faint quasar image. We also show high-rank candidate doubles selected this way, some of which have been independently identified with different techniques, and discuss a DES+WISE quasar multiplet selection., Comment: MNRAS subm. 21/10/2017, awaiting reviewer selection. This paper has been approved by DES Collaboration-Wide Review

Published
2018
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31. Space Warps– II. New gravitational lens candidates from the CFHTLS discovered through citizen science

Author

David Miller, Amit Kapadia, Rafael Küng, Christopher P. Davis, R. Gavazzi, Robert J. Simpson, Thomas E. Collett, Chris Lintott, Michael Parrish, Christine Macmillan, Surhud More, Arfon M. Smith, Claude Cornen, Edward Paget, Anupreeta More, Prasenjit Saha, Philip J. Marshall, Aprajita Verma, Elisabeth Baeten, Julianne K. Wilcox, Chris Snyder, and University of Zurich

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, Calibration (statistics), astro-ph.GA, Pipeline (computing), statistical [methods], ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, FOS: Physical sciences, Sample (statistics), 10192 Physics Institute, 01 natural sciences, law.invention, 1912 Space and Planetary Science, law, 0103 physical sciences, Citizen science, False positive paradox, Computer vision, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, business.industry, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Lens (optics), Gravitational lens, Space and Planetary Science, strong [gravitational lensing], Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, 3103 Astronomy and Astrophysics, Artificial intelligence, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of 29 promising (and 59 total) new lens candidates from the CFHT Legacy Survey (CFHTLS) based on about 11 million classifications performed by citizen scientists as part of the first Space Warps lens search. The goal of the blind lens search was to identify lens candidates missed by robots (the RingFinder on galaxy scales and ArcFinder on group/cluster scales) which had been previously used to mine the CFHTLS for lenses. We compare some properties of the samples detected by these algorithms to the Space Warps sample and find them to be broadly similar. The image separation distribution calculated from the Space Warps sample shows that previous constraints on the average density profile of lens galaxies are robust. SpaceWarps recovers about 65% of known lenses, while the new candidates show a richer variety compared to those found by the two robots. This detection rate could be increased to 80% by only using classifications performed by expert volunteers (albeit at the cost of a lower purity), indicating that the training and performance calibration of the citizen scientists is very important for the success of Space Warps. In this work we present the SIMCT pipeline, used for generating in situ a sample of realistic simulated lensed images. This training sample, along with the false positives identified during the search, has a legacy value for testing future lens finding algorithms. We make the pipeline and the training set publicly available., Comment: 23 pages, 12 figures, MNRAS accepted, minor to moderate changes in this version

Published
2015
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32. Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Author

Tim Eifler, A. Roodman, David J. James, Pablo Fosalba, Anupreeta More, Adriano Agnello, E. Bertin, I. Sevilla-Noarbe, Peter Melchior, J. Annis, A. Carnero Rosell, Philip J. Marshall, A. K. Romer, J. J. Thaler, Yanming Zhang, L. N. da Costa, Paul Martini, A. Fausti Neto, Ramon Miquel, Sherry H. Suyu, F. Ostrovski, M. Carrasco Kind, Matthew W. Auger, Flavia Sobreira, Robert C. Nichol, G. Meylan, Christopher D. Fassnacht, Shantanu Desai, A. A. Plazas, Frederic Courbin, David Brooks, M. E. C. Swanson, Gregory Tarle, Jennifer L. Marshall, M. March, Basilio X. Santiago, A. Benoit-Lévy, M. Banerji, K. Honscheid, Cristian E. Rusu, Juan Estrada, Ofer Lahav, B. Flaugher, C. B. D'Andrea, Risa H. Wechsler, Christopher J. Miller, Robert Connon Smith, Michael Schubnell, Nikolay Kuropatkin, Peter Doel, Kevin Reil, V. Scarpine, E. Buckley-Geer, Tommaso Treu, H. T. Diehl, F. B. Abdalla, G. Gutierrez, Alistair R. Walker, Marcelle Soares-Santos, Douglas L. Tucker, Kyler Kuehn, J. Carretero, J. P. Dietrich, Richard G. McMahon, Josh Frieman, D. A. Finley, Huan Lin, E. Suchyta, M. Sako, Marcio A. G. Maia, Paul L. Schechter, Daniel Gruen, Ricardo L. C. Ogando, Marcos Lima, D. L. Burke, D. W. Gerdes, S. Allam, T. M. C. Abbott, E. J. Sanchez, Carlos E. Cunha, Massachusetts Institute of Technology. Department of Physics, and Schechter, Paul L

Subjects
Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, astro-ph.GA, media_common.quotation_subject, statistical [methods], observational [methods], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Einstein radius, Photometry (optics), symbols.namesake, emission lines [quasars], Astrophysics::Solar and Stellar Astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, methods: statistical, biology, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, gravitational lensing: strong, Astronomy, Astronomy and Astrophysics, Quasar, biology.organism_classification, Astrophysics - Astrophysics of Galaxies, Galaxy, quasars: emission lines, Einstein Cross, Galaxias, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), strong [gravitational lensing], astro-ph.CO, symbols, methods: observational, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present spectroscopic confirmation of two new lensed quasars via data obtained at the 6.5m Magellan/Baade Telescope. The lens candidates have been selected from the Dark Energy Survey (DES) and WISE based on their multi-band photometry and extended morphology in DES images. Images of DES J0115-5244 show two blue point sources at either side of a red galaxy. Our long-slit data confirm that both point sources are images of the same quasar at $z_{s}=1.64.$ The Einstein Radius estimated from the DES images is $0.51$". DES J2200+0110 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fiber spectrum shows a quasar component at $z_{s}=2.38$ and absorption compatible with Mg II and Fe II at $z_{l}=0.799$, which we tentatively associate with the foreground lens galaxy. The long-slit Magellan spectra show that the blue components are resolved images of the same quasar. The Einstein Radius is $0.68$" corresponding to an enclosed mass of $1.6\times10^{11}\,M_{\odot}.$ Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data-mining and model-based selection that is being applied to the entire DES dataset., 7 pages, 1 figure, 2 tables, MNRAS subm. This paper includes data gathered with the 6.5m Baade Telescopes located at Las Campanas Observatory, Chile. This paper has gone through internal review by the DES collaboration, FERMILAB-PUB-15-341-AE

Published
2015
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33. Luminous red galaxies in clusters: central occupation, spatial distributions and miscentring

Author

Hanako Hoshino, Eli S. Rykoff, Anupreeta More, Alexie Leauthaud, Shun Saito, Rachel Mandelbaum, Chiaki Hikage, Benedetta Vulcani, Surhud More, Eduardo Rozo, and Claire Lackner

Subjects
Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, Dark matter, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 20399 Classical Physics not elsewhere classified, Correlation function (astronomy), Galaxy, Luminosity, Space and Planetary Science, Halo, Brightest cluster galaxy, education, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Luminous Red Galaxies (LRG) from the Sloan Digital Sky Survey are considered among the best understood samples of galaxies, and they are employed in a broad range of cosmological studies. Because they form a relatively homogeneous population, with high stellar masses and red colors, they are expected to occupy halos in a relatively simple way. In this paper, we study how LRGs occupy massive halos via direct counts in clusters and we reveal several unexpected trends suggesting that the connection between LRGs and dark matter halos may not be straightforward. Using the redMaPPer cluster catalog, we derive the central occupation of LRGs as a function richness, Ncen({\lambda}). Assuming no correlation between cluster mass and central galaxy luminosity at fixed richness, we show that clusters contain a significantly lower fraction of central LRGs than predicted from the two-point correlation function. At halo masses of 10^14.5 Msun, we find Ncen=0.73, compared to Ncen of 0.89 from correlation studies. Our central occupation function for LRGs converges to 0.95 at large halo masses. A strong anti-correlation between central luminosity and cluster mass at fixed richness is required to reconcile our results with those based on clustering studies. We also derive P_BNC, the probability that the brightest cluster member is not the central galaxy. We find P_BNC ~ 20-30% which is a factor of ~2 lower than the value found by Skibba et al. 2011. Finally, we study the radial offsets of bright non-central LRGs from cluster centers and show that bright non-central LRGs follow a different radial distribution compared to red cluster members, which follow a Navarro-Frank-White profile. This work demonstrates that even the most massive clusters do not always have an LRG at the center, and that the brightest galaxy in a cluster is not always the central galaxy., Comment: 18 pages, 9 figures, 4 tables, submitted to MNRAS, included the referee comments

Published
2015
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34. Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI). I. Automatic search for galaxy-scale strong lenses

Author

Anton T. Jaelani, Yiping Shu, Masayuki Tanaka, Adam S. Bolton, Masamune Oguri, Alessandro Sonnenfeld, Jean Coupon, Kenneth C. Wong, Yutaka Komiyama, Satoshi Miyazaki, Sherry H. Suyu, Anupreeta More, James H. H. Chan, Atsunori Yonehara, and Chien-Hsiu Lee

Subjects
Physics, Image quality, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Redshift, law.invention, Lens (optics), Photometry (optics), Boss, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Hyper Suprime-Cam Subaru Strategic Program (HSC SSP) is an excellent survey for the search for strong lenses, thanks to its area, image quality and depth. We use three different methods to look for lenses among 43,000 luminous red galaxies from the Baryon Oscillation Spectroscopic Survey (BOSS) sample with photometry from the S16A internal data release of the HSC SSP. The first method is a newly developed algorithm, named YATTALENS, which looks for arc-like features around massive galaxies and then estimates the likelihood of an object being a lens by performing a lens model fit. The second method, CHITAH, is a modeling-based algorithm originally developed to look for lensed quasars. The third method makes use of spectroscopic data to look for emission lines from objects at a different redshift from that of the main galaxy. We find 15 definite lenses, 36 highly probable lenses and 282 possible lenses. Among the three methods, YATTALENS, which was developed specifically for this problem, performs best in terms of both completeness and purity. Nevertheless five highly probable lenses were missed by YATTALENS but found by the other two methods, indicating that the three methods are highly complementary. Based on these numbers we expect to find $\sim$300 definite or probable lenses by the end of the HSC SSP., Published on PASJ. 17 pages, 8 figures. Image quality of Figures 6 and 7 has been degraded due to arXiv file size limit. Full quality versions can be found at http://member.ipmu.jp/alessandro.sonnenfeld/sugohi1_candidates.html

Published
2017
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35. Core or Cusps: The Central Dark Matter Profile of a Strong Lensing Cluster with a Bright Central Image at Redshift 1

Author

G. Gutierrez, Tim Eifler, Ramon Miquel, Daniel A. Goldstein, Thomas E. Collett, V. Scarpine, Shantanu Desai, Douglas L. Tucker, Kyler Kuehn, Mathew Smith, Xan Morice-Atkinson, Andrs A. Plazas, Chris B. D'Andrea, Alistair R. Walker, Peter Doel, D. L. Burke, David Bacon, B. Flaugher, David Brooks, David J. James, Nikolay Kuropatkin, I. Sevilla-Noarbe, E. Suchyta, Rafe Schindler, Brian Nord, Anupreeta More, Simon Birrer, Luiz N. da Costa, H. Thomas Diehl, Josh Frieman, S. Allam, Aurlien Benoit-Levy, Marcos Lima, J. Gschwend, Flavia Sobreira, Casey Papovich, Jennifer L. Marshal, Peter Melchior, E. Buckley-Geer, James Annis, K. Romer, Matias Carrasco Kind, M. March, Molly E. C. Swanson, Huan Lin, Paul Martini, Michael Schubnell, Adam Amara, Nicolas Tessore, Daniel Gruen, D. W. Gerdes, Robert C. Nichol, Francisco J. Castander, Marcio A. G. Maia, Gregory Tarle, Eli S. Rykoff, T. M. C. Abbott, Ofer Lahav, E. J. Sanchez, Tenglin Li, Steve Kuhlmann, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
galaxies: clusters: individual, Cold dark matter, Einstein ring, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], clusters: individual (SPT-CLJ2011-5228) [galaxies], Dark matter, galaxies: halos, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Physical Chemistry, Atomic, dark matter, symbols.namesake, Particle and Plasma Physics, 0103 physical sciences, Nuclear, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Mass distribution, clusters: individual [galaxies], Molecular, gravitational lensing: strong, Astronomy and Astrophysics, Radius, Redshift, halos [galaxies], Gravitational lens, Space and Planetary Science, strong [gravitational lensing], symbols, Dark energy, Biomedical Imaging, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

International audience; We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z ( )s( ) = 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is $\sim {10}^{14.2}\ {M}_{\odot }$. We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro–Frenk–White profile—with a free parameter for the inner density slope—we find that the break radius is ${270}_{-76}^{+48}$ kpc, and that the inner density falls with radius to the power −0.38 ± 0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos, dark matter-only simulations predict that the inner density should fall as ${r}^{-1}$. The tension can be alleviated if this cluster is in fact a merger, a two-halo model can also reconstruct the data, with both clumps (density varying as ${r}^{-0.8}$ and ${r}^{-1.0}$) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.

Published
2017
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36. An optically-selected cluster catalog at redshift 0.1 < z < 1.1 from the Hyper Suprime-Cam Subaru Strategic Program S16A data

Author

Anupreeta More, Hung-Yu Jian, Yutaka Komiyama, Elinor Medezinski, Lihwai Lin, Hironao Miyatake, Masayuki Tanaka, I-Non Chiu, Bau-Ching Hsieh, Surhud More, Jean Coupon, Atsushi J. Nishizawa, Masahiro Takada, Joshua S. Speagle, Sheng-Chieh Lin, Tomonori Usuda, Yuki Okura, Yen-Ting Lin, Masamune Oguri, Paul A. Price, Robert H. Lupton, Satoshi Miyazaki, Nobuhiro Okabe, Alexie Leauthaud, and Manobu M. Tanaka

Subjects
Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, High mass, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Photometric redshift
Abstract

We present an optically-selected cluster catalog from the Hyper Suprime-Cam (HSC) Subaru Strategic Program. The HSC images are sufficiently deep to detect cluster member galaxies down to $M_*\sim 10^{10.2}M_\odot$ even at $z\sim 1$, allowing a reliable cluster detection at such high redshifts. We apply the CAMIRA algorithm to the HSC Wide S16A dataset covering $\sim 232$ deg$^2$ to construct a catalog of 1921 clusters at redshift $0.115$ that roughly corresponds to $M_{\rm 200m}\gtrsim 10^{14}h^{-1}M_\odot$. We confirm good cluster photometric redshift performance, with the bias and scatter in $\Delta z/(1+z)$ being better than 0.005 and 0.01 over most of the redshift range, respectively. We compare our cluster catalog with large X-ray cluster catalogs from XXL and XMM-LSS surveys and find good correlation between richness and X-ray properties. We also study the miscentering effect from the distribution of offsets between optical and X-ray cluster centers. We confirm the high ($>0.9$) completeness and purity for high mass clusters by analyzing mock galaxy catalogs., Comment: 18 pages, 18 figures, accepted for publication in PASJ; cluster catalogs are available at http://www.slac.stanford.edu/~oguri/cluster/

Published
2017
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37. The Hyper Suprime-Cam SSP Survey: Overview and Survey Design

Author

Hiroaki Aihara, Nobuo Arimoto, Robert Armstrong, Stéphane Arnouts, Neta A Bahcall, Steven Bickerton, James Bosch, Kevin Bundy, Peter L Capak, James H H Chan, Masashi Chiba, Jean Coupon, Eiichi Egami, Motohiro Enoki, Francois Finet, Hiroki Fujimori, Seiji Fujimoto, Hisanori Furusawa, Junko Furusawa, Tomotsugu Goto, Andy Goulding, Johnny P Greco, Jenny E Greene, James E Gunn, Takashi Hamana, Yuichi Harikane, Yasuhiro Hashimoto, Takashi Hattori, Masao Hayashi, Yusuke Hayashi, Krzysztof G Hełminiak, Ryo Higuchi, Chiaki Hikage, Paul T P Ho, Bau-Ching Hsieh, Kuiyun Huang, Song Huang, Hiroyuki Ikeda, Masatoshi Imanishi, Akio K Inoue, Kazushi Iwasawa, Ikuru Iwata, Anton T Jaelani, Hung-Yu Jian, Yukiko Kamata, Hiroshi Karoji, Nobunari Kashikawa, Nobuhiko Katayama, Satoshi Kawanomoto, Issha Kayo, Jin Koda, Michitaro Koike, Takashi Kojima, Yutaka Komiyama, Akira Konno, Shintaro Koshida, Yusei Koyama, Haruka Kusakabe, Alexie Leauthaud, Chien-Hsiu Lee, Lihwai Lin, Yen-Ting Lin, Robert H Lupton, Rachel Mandelbaum, Yoshiki Matsuoka, Elinor Medezinski, Sogo Mineo, Shoken Miyama, Hironao Miyatake, Satoshi Miyazaki, Rieko Momose, Anupreeta More, Surhud More, Yuki Moritani, Takashi J Moriya, Tomoki Morokuma, Shiro Mukae, Ryoma Murata, Hitoshi Murayama, Tohru Nagao, Fumiaki Nakata, Mana Niida, Hiroko Niikura, Atsushi J Nishizawa, Yoshiyuki Obuchi, Masamune Oguri, Yukie Oishi, Nobuhiro Okabe, Sakurako Okamoto, Yuki Okura, Yoshiaki Ono, Masato Onodera, Masafusa Onoue, Ken Osato, Masami Ouchi, Paul A Price, Tae-Soo Pyo, Masao Sako, Marcin Sawicki, Takatoshi Shibuya, Kazuhiro Shimasaku, Atsushi Shimono, Masato Shirasaki, John D Silverman, Melanie Simet, Joshua Speagle, David N Spergel, Michael A Strauss, Yuma Sugahara, Naoshi Sugiyama, Yasushi Suto, Sherry H Suyu, Nao Suzuki, Philip J Tait, Masahiro Takada, Tadafumi Takata, Naoyuki Tamura, Manobu M Tanaka, Masaomi Tanaka, Masayuki Tanaka, Yoko Tanaka, Tsuyoshi Terai, Yuichi Terashima, Yoshiki Toba, Nozomu Tominaga, Jun Toshikawa, Edwin L Turner, Tomohisa Uchida, Hisakazu Uchiyama, Keiichi Umetsu, Fumihiro Uraguchi, Yuji Urata, Tomonori Usuda, Yousuke Utsumi, Shiang-Yu Wang, Wei-Hao Wang, Kenneth C Wong, Kiyoto Yabe, Yoshihiko Yamada, Hitomi Yamanoi, Naoki Yasuda, Sherry Yeh, Atsunori Yonehara, Suraphong Yuma, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universitat de Barcelona, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille ( LAM ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES )

Subjects
media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, 0103 physical sciences, 14. Life underwater, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Summit, geography.geographical_feature_category, Cosmologia, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Survey research, Galaxies, Galàxies, Cosmology, Geography, Space and Planetary Science, Sky, Magnitude (astronomy), Subaru Telescope, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of scientists from Japan, Taiwan and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg$^2$ in five broad bands ($grizy$), with a $5\,\sigma$ point-source depth of $r \approx 26$. The Deep layer covers a total of 26~deg$^2$ in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg$^2$). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey., Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the coordinates of HSC-Wide spring equatorial field in Table 5

Published
2017
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38. First Data Release of the Hyper Suprime-Cam Subaru Strategic Program

Author

Naoshi Sugiyama, Surhud More, Chiaki Hikage, Nobuo Arimoto, Shiro Mukae, Paul T. P. Ho, Chien-Hsiu Lee, Hiroaki Aihara, Hisanori Furusawa, Tomoki Morokuma, Suraphong Yuma, Masato Onodera, Nobunari Kashikawa, Masao Hayashi, Nobuhiro Okabe, Fumihiro Uraguchi, Masamune Oguri, Song Huang, Tsuyoshi Terai, Yukie Oishi, James Bosch, Yukiko Kamata, Philip J. Tait, Yoshiyuki Obuchi, Yen-Ting Lin, Haruka Kusakabe, Yoshihiko Yamada, Yoko Tanaka, Anton T. Jaelani, Anupreeta More, Masahiro Takada, S. Koshida, Rachel Mandelbaum, Masami Ouchi, Atsushi J. Nishizawa, Nobuhiko Katayama, Tomonori Usuda, Akira Konno, Kazuhiro Shimasaku, Robert Armstrong, Yoshiaki Ono, Hiroyuki Ikeda, Joshua S. Speagle, Tomotsugu Goto, Ryoma Murata, Masayuki Tanaka, Yusuke Hayashi, Yuma Sugahara, J. Furusawa, Hitomi Yamanoi, Yoshiki Matsuoka, Rieko Momose, Kuiyun Huang, Sherry Yeh, Yuji Urata, Robert H. Lupton, Michitaro Koike, Shoken Miyama, Michael A. Strauss, James E. Gunn, Shiang-Yu Wang, Krzysztof G. Hełminiak, Yuki Okura, Hisakazu Uchiyama, Melanie Simet, Yoshiki Toba, Ikuru Iwata, Lihwai Lin, Ryo Higuchi, Jean Coupon, Nao Suzuki, Hung-Yu Jian, Takashi Kojima, Hiroshi Karoji, Paul A. Price, Takatoshi Shibuya, Andy D. Goulding, Tomohisa Uchida, Hiroko Niikura, Steven J. Bickerton, Manobu Tanaka, Mana Niida, Edwin L. Turner, Yasushi Suto, Hironao Miyatake, Sogo Mineo, Yuichi Harikane, Dustin Lang, Bau-Ching Hsieh, Hitoshi Murayama, Tohru Nagao, François Finet, Alexie Leauthaud, Masashi Chiba, Fumiaki Nakata, Yousuke Utsumi, M. Onoue, Satoshi Kawanomoto, Takashi Hattori, Masatoshi Imanishi, Tadafumi Takata, Seiji Fujimoto, Yutaka Komiyama, Keiichi Umetsu, Elinor Medezinski, David N. Spergel, Tae-Soo Pyo, Naoki Yasuda, Hiroki Fujimori, and Satoshi Miyazaki

Subjects
Image quality, media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Field (computer science), Computer graphics (images), 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Pipeline (software), Astrophysics - Astrophysics of Galaxies, Object detection, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Sky, Data quality, Astrophysics of Galaxies (astro-ph.GA), Subaru Telescope, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) is a three-layered imaging survey aimed at addressing some of the most outstanding questions in astronomy today, including the nature of dark matter and dark energy. The survey has been awarded 300 nights of observing time at the Subaru Telescope and it started in March 2014. This paper presents the first public data release of HSC-SSP. This release includes data taken in the first 1.7 years of observations (61.5 nights) and each of the Wide, Deep, and UltraDeep layers covers about 108, 26, and 4 square degrees down to depths of i~26.4, ~26.5, and ~27.0 mag, respectively (5sigma for point sources). All the layers are observed in five broad bands (grizy), and the Deep and UltraDeep layers are observed in narrow bands as well. We achieve an impressive image quality of 0.6 arcsec in the i-band in the Wide layer. We show that we achieve 1-2 per cent PSF photometry (rms) both internally and externally (against Pan-STARRS1), and ~10 mas and 40 mas internal and external astrometric accuracy, respectively. Both the calibrated images and catalogs are made available to the community through dedicated user interfaces and database servers. In addition to the pipeline products, we also provide value-added products such as photometric redshifts and a collection of public spectroscopic redshifts. Detailed descriptions of all the data can be found online. The data release website is https://hsc-release.mtk.nao.ac.jp/., 34 pages, 20 figures, 7 tables, moderate revision, accepted for publication in PASJ

Published
2017

39. The DES Bright Arcs Survey: Hundreds of Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey Science Verification and Year 1 Observations

Author

Joshua A. Frieman, M. E. C. Swanson, L. N. da Costa, C. B. D'Andrea, S. E. Kuhlmann, E. Suchyta, August E. Evrard, Michael Schubnell, A. Benoit-Lévy, Kevin Reil, M. Smith, Ramon Miquel, Anupreeta More, Jennifer L. Marshall, Shantanu Desai, David J. Brooks, Alistair R. Walker, Daniel Gruen, Peter Nugent, Marcelle Soares-Santos, M. Sako, Thomas E. Collett, B. Flaugher, B. Welch, D. L. Tucker, Rafe Schindler, J. P. Dietrich, F. B. Abdalla, Erin Sheldon, S. Gaitsch, Juan Garcia-Bellido, Brian Nord, Nikolay Kuropatkin, Flavia Sobreira, Hallie Gaitsch, D. W. Gerdes, E. J. Sanchez, David J. James, D. A. Finley, J. Nightingale, Daniel Thomas, Kyler Kuehn, H. T. Diehl, E. Buckley-Geer, Tenglin Li, Yanxi Zhang, Carlos E. Cunha, J. Carretero, Alex Drlica-Wagner, A. K. Romer, M. S. S. Gill, Daniel A. Goldstein, A. Pellico, A. Fausti Neto, J. Gschwend, Marcos Lima, C. Furlanetto, Basilio X. Santiago, Ricardo L. C. Ogando, M. Carrasco Kind, E. Bertin, Robert C. Nichol, A. A. Plazas, K. A. Lindgren, D. L. Burke, A. Carnero Rosell, J. Annis, S. Allam, Robert A. Gruendl, Huan Lin, G. Gutierrez, Felipe Menanteau, C. Odden, Gregory Tarle, V. Scarpine, I. Sevilla-Noarbe, Ofer Lahav, Marcio A. G. Maia, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Strong gravitational lensing, AST-1138766, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, law.invention, Particle and Plasma Physics, law, galaxies: high-redshift, 0103 physical sciences, Nuclear, 010303 astronomy & astrophysics, Galaxy cluster, STFC, ComputingMilieux_MISCELLANEOUS, QB, Physics, 010308 nuclear & particles physics, Astronomy, Molecular, RCUK, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, Lens (optics), Gravitational lens, Space and Planetary Science, Limiting magnitude, strong [gravitational lensing], Magnitude (astronomy), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, high-redshift [galaxies], Physical Chemistry (incl. Structural)
Abstract

We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10 sigma) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have an i-band limiting magnitude for extended objects (10 sigma) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.

Published
2017
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40. Models of the strongly lensed quasar DES J0408-5354

Author

R. H. Schindler, Sherry H. Suyu, J. Carretero, Daniel A. Goldstein, Matthew W. Auger, I. Sevilla-Noarbe, J. P. Dietrich, Richard G. McMahon, Martin Crocce, Daniel Gruen, Huan Lin, Risa H. Wechsler, Juan Garcia-Bellido, David Brooks, M. E. C. Swanson, G. Gutierrez, Frederic Courbin, R. C. Smith, E. Suchyta, A. Howell, Douglas L. Tucker, Kyler Kuehn, Adriano Agnello, L. N. da Costa, Tianjun Li, A. Carnero Rosell, D. L. Burke, C. Lemon, C. B. D'Andrea, B. Flaugher, D. A. Finley, Nikolay Kuropatkin, Enrique Gaztanaga, A. A. Plazas, F. J. Castander, Paul L. Schechter, Marcio A. G. Maia, Tommaso Treu, Shantanu Desai, F. B. Abdalla, K. Honscheid, S. Allam, Robert A. Gruendl, Matthew Smith, A. Benoit-Lévy, T. M. C. Abbott, Peter Melchior, G. Meylan, N. D. Morgan, Tim Eifler, Felipe Menanteau, Flavia Sobreira, M. S. S. Gill, E. J. Sanchez, Jennifer L. Marshall, Gregory Tarle, Daniel Thomas, Vivien Bonvin, Joshua A. Frieman, Christopher S. Kochanek, M. March, Ricardo L. C. Ogando, Christopher D. Fassnacht, F. Ostrovski, Michael Schubnell, M. Carrasco Kind, Adam Amara, Alistair R. Walker, Jeffrey C. C. Chan, David J. James, Carlos E. Cunha, Anupreeta More, Pablo Fosalba, Brian Nord, Takahiro Morishita, E. Bertin, A. K. Romer, L. Buckley-Geer, Paul Martini, Philip J. Marshall, J. Gschwend, Simon Birrer, Marcos Lima, Martin Makler, Ramon Miquel, Thomas E. Collett, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], astro-ph.GA, Flux, FOS: Physical sciences, techniques: image processing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, techniques: image processig, Einstein radius, 0103 physical sciences, Chromaticity, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, STFC, catalogues, strong, methods: statistical, catalogues [gravitational lensing], QB, Physics, 010308 nuclear & particles physics, Astronomy, Velocity dispersion, RCUK, gravitational lensing: strong, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present detailed modelling of the recently discovered, quadruply lensed quasar J0408−5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ RE, G2 ≲ 0.2 arcsec and enclosed mass Mp(RE, G2) ≲ 1.0 × 10(10) M⊙. The main deflector has stellar mass log10(M⋆/M⊙) = 11.49(+0.46)(−0.32), a projected mass Mp(RE, G1) ≈ 6 × 10(11) M⊙ within its Einstein radius RE, G1 = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267–280 km s(−1). Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (ΔtAB = (135.0 ± 12.6) d, ΔtBD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408−5354 on lensed quasar finding strategies, due to its chromaticity and morphology., Monthly Notices of the Royal Astronomical Society, 472 (4), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2017
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41. A Spectroscopically Confirmed Double Source Plane Lens System in the Hyper Suprime-Cam Subaru Strategic Program

Author

Alessandro Sonnenfeld, Sherry H. Suyu, Eiichi Egami, Shuri Oyamada, Masamune Oguri, Arsha Dezuka, Yutaka Komiyama, Anupreeta More, Yousuke Utsumi, Satoshi Miyazaki, Kenneth C. Wong, Masafusa Onoue, Ryo Higuchi, and Masayuki Tanaka

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Christian ministry, Source plane, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the serendipitous discovery of HSC J142449-005322, a double source plane lens system in the Hyper Suprime-Cam Subaru Strategic Program. We dub the system Eye of Horus. The lens galaxy is a very massive early-type galaxy with stellar mass of ~7x10^11 Msun located at z_L=0.795. The system exhibits two arcs/rings with clearly different colors, including several knots. We have performed spectroscopic follow-up observations of the system with FIRE on Magellan. The outer ring is confirmed at z_S2=1.988 with multiple emission lines, while the inner arc and counterimage is confirmed at z_S1=1.302. This makes it the first double source plane system with spectroscopic redshifts of both sources. Interestingly, redshifts of two of the knots embedded in the outer ring are found to be offset by delta_z=0.002 from the other knots, suggesting that the outer ring consists of at least two distinct components in the source plane. We perform lens modeling with two independent codes and successfully reproduce the main features of the system. However, two of the lensed sources separated by ~0.7 arcsec cannot be reproduced by a smooth potential, and the addition of substructure to the lens potential is required to reproduce them. Higher-resolution imaging of the system will help decipher the origin of this lensing feature and potentially detect the substructure., 6 pages, 3 figures, accepted for publication in ApJL

Published
2016

42. Galaxy-scale gravitational lens candidates from the Hyper Suprime-Cam imaging survey and the Galaxy And Mass Assembly spectroscopic survey

Author

Bau-Ching Hsieh, Anupreeta More, Hitoshi Murayama, Sherry H. Suyu, Tsuyoshi Terai, Paul A. Price, Masamune Oguri, Jean Coupon, Atsushi J. Nishizawa, Philip J. Tait, Yousuke Utsumi, Satoshi Miyazaki, Shiang-Yu Wang, Tzihong Chiueh, Yutaka Komiyama, and James H. H. Chan

Subjects
Physics, Initial mass function, Stellar population, Stellar mass, 010308 nuclear & particles physics, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Einstein radius, Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Mass fraction, Astrophysics::Galaxy Astrophysics
Abstract

We present a list of galaxy-scale lens candidates including a highly probable interacting galaxy-scale lens in the Hyper Suprime-Cam (HSC) imaging survey. We combine HSC imaging with the blended-spectra catalog from the Galaxy And Mass Assembly (GAMA) survey to identify lens candidates, and use lens mass modeling to confirm the candidates. We find 46 matches between the HSC S14A_0b imaging data release and the GAMA catalog. Ten of them are probable lens systems according to their morphology and redshifts. There is one system with an interacting galaxy pair, HSC J084928+000949, that has a valid mass model. We predict the total mass enclosed by the Einstein radius of $\sim0.72$" ($\sim1.65$kpc) for this new expected lens system to be $\sim10^{10.59}M_{\odot}$. Using the photometry in the {\it grizy} bands of the HSC survey and stellar population synthesis modeling with a Salpeter stellar initial mass function, we estimate the stellar mass within the Einstein radius to be $\sim10^{10.46}\,M_{\odot}$. We thus find a dark matter mass fraction within the Einstein radius of $\sim25\%$. Further spectroscopy or high-resolution imaging would allow confirmation of the nature of these lens candidates. The particular system with the interacting galaxy pair, if confirmed, would provide an opportunity to study the interplay between dark matter and stars as galaxies build up through hierarchical mergers., 10 pages, 5 figures

Published
2016

43. Detection of the Splashback Radius and Halo Assembly bias of Massive Galaxy Clusters

Author

Eli S. Rykoff, David N. Spergel, Neal Dalal, Andrey V. Kravtsov, Surhud More, Rachel Mandelbaum, Anupreeta More, Masahiro Takada, Hironao Miyatake, Masamune Oguri, Eduardo Rozo, Ryoma Murata, and Benedikt Diemer

Subjects
Physics, Structure formation, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Astrophysics::Cosmology and Extragalactic Astrophysics, 20399 Classical Physics not elsewhere classified, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Satellite galaxy, Halo, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We show that the projected number density profiles of SDSS photometric galaxies around galaxy clusters displays strong evidence for the splashback radius, a sharp halo edge corresponding to the location of the first orbital apocenter of satellite galaxies after their infall. We split the clusters into two subsamples with different mean projected radial distances of their members, $\langle R_{\rm mem}\rangle$, at fixed richness and redshift, and show that the sample with smaller $\langle R_{\rm mem}\rangle$ has a smaller ratio of the splashback radius to the traditional halo boundary $R_{\rm 200m}$, than the subsample with larger $\langle R_{\rm mem}\rangle$, indicative of different mass accretion rates for the two subsamples. The same cluster samples were recently used by Miyatake et al. to show that their large-scale clustering differs despite their similar weak lensing masses, demonstrating strong evidence for halo assembly bias. We expand on this result by presenting a 6.6-$\sigma$ detection of halo assembly bias using the cluster-photometric galaxy cross-correlations. Our measured splashback radii are smaller, while the strength of the assembly bias signal is stronger, than expectations from N-body simulations based on the $\Lambda$-dominated, cold dark matter structure formation model. Dynamical friction or cluster-finding systematics such as miscentering or projection effects are not likely to be the sole source of these discrepancies., Comment: 18 pages, 13 figures. Have comments, criticisms, new ideas or new tests, please email me. For Savitzky-Golay filter for data with error covariance, see http://ascl.net/code/v/1299

Published
2016
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44. Interpreting the strongly lensed supernova iPTF16geu: time delay predictions, microlensing, and lensing rates

Author

Masamune Oguri, Sherry H. Suyu, Surhud More, Anupreeta More, and Chien-Hsiu Lee

Subjects
Physics, Time delays, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Expected value, Gravitational microlensing, 01 natural sciences, Measure (mathematics), Redshift, Luminosity, symbols.namesake, Supernova, Space and Planetary Science, 0103 physical sciences, symbols, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present predictions for time delays between multiple images of the gravitationally lensed supernova, iPTF16geu, which was recently discovered from the intermediate Palomar Transient Factory (iPTF). As the supernova is of Type Ia where the intrinsic luminosity is usually well-known, accurately measured time delays of the multiple images could provide tight constraints on the Hubble constant. According to our lens mass models constrained by the {\it Hubble Space Telescope} F814W image, we expect the maximum relative time delay to be less than a day, which is consistent with the maximum of 100 hours reported by Goobar et al. but places a stringent upper limit. Furthermore, the fluxes of most of the supernova images depart from expected values suggesting that they are affected by microlensing. The microlensing timescales are small enough that they may pose significant problems to measure the time delays reliably. Our lensing rate calculation indicates that the occurrence of a lensed SN in iPTF is likely. However, the observed total magnification of iPTF16geu is larger than expected, given its redshift. This may be a further indication of ongoing microlensing in this system., Comment: 5 pages, 3 figures, 1 table, ApjL accepted, minor but important corrections

Published
2016
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45. Survey of Gravitationally Lensed Objects in HSC Imaging (SuGOHI). II. Environments and Line-of-Sight Structure of Strong Gravitational Lens Galaxies to z ∼ 0.8

Author

Masayuki Tanaka, Alessandro Sonnenfeld, Cristian E. Rusu, Sherry H. Suyu, Anupreeta More, Anton T. Jaelani, Kenneth C. Wong, Yutaka Komiyama, James H. H. Chan, Masamune Oguri, and Chien-Hsiu Lee

Subjects
Physics, Line-of-sight, Plane (geometry), FOS: Physical sciences, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Sample (graphics), Redshift, Galaxy, law.invention, Lens (optics), Gravitational lens, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We investigate the local and line-of-sight overdensities of strong gravitational lens galaxies using wide-area multiband imaging from the Hyper Suprime-Cam Subaru Strategic Program. We present 41 new definite or probable lens candidates discovered in Data Release 2 of the survey. Using a combined sample of 87 galaxy-scale lenses out to a lens redshift of $z_{\mathrm{L}} \sim 0.8$, we compare galaxy number counts in lines of sight toward known and newly-discovered lenses in the survey to those of a control sample consisting of random lines of sight. We also compare the local overdensity of lens galaxies to a sample of "twin" galaxies that have a similar redshift and velocity dispersion to test whether lenses lie in different environments from similar non-lens galaxies. We find that lens fields contain higher number counts of galaxies compared to the control fields, but this effect arises from the local environment of the lens. Once galaxies in the lens plane are removed, the lens lines of sight are consistent with the control sample. The local environments of the lenses are overdense compared to the control sample, and are slightly overdense compared to those of the twin sample, although the significance is marginal. There is no significant evidence of the evolution of the local overdensity of lens environments with redshift., Comment: Accepted for publication in the Astrophysical Journal; 22 pages, 10 figures, 9 tables

Published
2018
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46. A new window of exploration in the mass spectrum: strong lensing by galaxy groups in the SL2S

Author

Tomás Verdugo, Jean-Paul Kneib, Jon Willis, Sherry H. Suyu, G. Soucail, Bernard Fort, Eric Jullo, C. Faure, Anupreeta More, D. Valls-Gabaud, Philip J. Marshall, Raphael Gavazzi, Mark Swinbank, Johan Richard, David Crampton, H. Tu, Veronica Motta, G. Foëx, Karun Thanjavur, Remi A. Cabanac, Marceau Limousin, Yannick Mellier, R. Pello, J.-F. Sygnet, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AUTRES, Departamento de Fisica y Astronomia [Valparaiso], Universidad de Valparaiso [Chile], Institute for Computational Cosmology (ICC), Durham University, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Département Réseaux, Sécurité et Multimédia (RSM), Université européenne de Bretagne - European University of Brittany (UEB)-Télécom Bretagne-Institut Mines-Télécom [Paris] (IMT), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Astronomy, Stanford University, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Dark-Matter, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Density Profiles, Xmm-Newton, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Environments, 01 natural sciences, Clusters, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], X-Ray-Properties, Galaxy group, Cosmic-Horseshoe, 0103 physical sciences, Group Connection, gravitational lensing: cosmology: large-scale structure of Universe, 010303 astronomy & astrophysics, Mass-to-light ratio, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, Sdss, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Redshift, Separation Gravitational Lenses, Space and Planetary Science, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics
Abstract

The existence of strong lensing systems with Einstein radii (Re) covering the full mass spectrum, from ~1-2" (produced by galaxy scale dark matter haloes) to >10" (produced by galaxy cluster scale haloes) have long been predicted. Many lenses with Re around 1-2" and above 10" have been reported but very few in between. In this article, we present a sample of 13 strong lensing systems with Re in the range 3"- 8", i.e. systems produced by galaxy group scale dark matter haloes, spanning a redshift range from 0.3 to 0.8. This opens a new window of exploration in the mass spectrum, around 10^{13}- 10^{14} M_{sun}, which is a crucial range for understanding the transition between galaxies and galaxy clusters. Our analysis is based on multi-colour CFHTLS images complemented with HST imaging and ground based spectroscopy. Large scale properties are derived from both the light distribution of the elliptical galaxies group members and weak lensing of the faint background galaxy population. On small scales, the strong lensing analysis yields Einstein radii between 2.5" and 8". On larger scales, the strong lenses coincide with the peak of the light distribution, suggesting that mass is traced by light. Most of the luminosity maps have complicated shapes, indicating that these intermediate mass structures are dynamically young. Fitting the reduced shear with a Singular Isothermal Sphere, we find sigma ~ 500 km/s and an upper limit of ~900 km/s for the whole sample. The mass to light ratio for the sample is found to be M/L_i ~ 250 (solar units, corrected for evolution), with an upper limit of 500. This can be compared to mass to light ratios of small groups (with sigma ~ 300 km/s and galaxy clusters with sigma > 1000 km/s, thus bridging the gap between these mass scales., A&A Accepted. Draft with Appendix images can be found at http://www.dark-cosmology.dk/~marceau/groups_sl2s.pdf

Published
2009
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47. Space Warps: I. Crowd-sourcing the discovery of gravitational lenses

Author

David Miller, Chris Snyder, Rafael Küng, Edward Paget, Anupreeta More, Christine Macmillan, Arfon M. Smith, Philip J. Marshall, Claude Cornen, Edwin Simpson, M. Baumer, Thomas E. Collett, Aprajita Verma, Prasenjit Saha, Amit Kapadia, Chris Lintott, Elisabeth Baeten, Julianne K. Wilcox, R. Simpson, Michael Parrish, Christopher P. Davis, and Surhud More

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, statistical [methods], FOS: Physical sciences, Crowdsourcing, 01 natural sciences, law.invention, Telescope, Set (abstract data type), Optics, law, 0103 physical sciences, Computer vision, Projection (set theory), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, Real image, Astrophysics - Astrophysics of Galaxies, Sample (graphics), Lens (optics), Gravitational lens, Space and Planetary Science, strong [gravitational lensing], Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

We describe Space Warps, a novel gravitational lens discovery service that yields samples of high purity and completeness through crowd-sourced visual inspection. Carefully produced colour composite images are displayed to volunteers via a web- based classification interface, which records their estimates of the positions of candidate lensed features. Images of simulated lenses, as well as real images which lack lenses, are inserted into the image stream at random intervals; this training set is used to give the volunteers instantaneous feedback on their performance, as well as to calibrate a model of the system that provides dynamical updates to the probability that a classified image contains a lens. Low probability systems are retired from the site periodically, concentrating the sample towards a set of lens candidates. Having divided 160 square degrees of Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) imaging into some 430,000 overlapping 82 by 82 arcsecond tiles and displaying them on the site, we were joined by around 37,000 volunteers who contributed 11 million image classifications over the course of 8 months. This Stage 1 search reduced the sample to 3381 images containing candidates; these were then refined in Stage 2 to yield a sample that we expect to be over 90% complete and 30% pure, based on our analysis of the volunteers performance on training images. We comment on the scalability of the SpaceWarps system to the wide field survey era, based on our projection that searches of 10$^5$ images could be performed by a crowd of 10$^5$ volunteers in 6 days., Comment: 21 pages, 13 figures, MNRAS accepted, minor to moderate changes in this version

Published
2015
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48. The CFHTLS-Strong Lensing Legacy Survey (SL2S): Investigating the group-scale lenses with the SARCS sample

Author

C. Alard, Jean-Paul Kneib, Veronica Motta, Marceau Limousin, Anupreeta More, Remi A. Cabanac, Surhud More, Raphael Gavazzi, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Sample (graphics), Galaxy, Redshift, law.invention, Lens (optics), Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, Luminosity function, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Strong Lensing Legacy Survey - ARCS (SARCS) sample compiled from the final T0006 data release of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) covering a total non-overlapping area of 159 sq.deg. We adopt a semi-automatic method to find gravitational arcs in the survey that makes use of an arc-finding algorithm. The candidate list is pruned by visual inspection and ranking to form the SARCS sample. This list also includes some serendipitously discovered lens candidates. The SARCS sample consists of 127 lens candidates which span arc radii~2"-18" within the unmasked area of ~ 150 sq. deg. Within the sample, 54 systems are promising lenses amongst which, we find 12 giant arcs and 2 radial arc candidates. From our sample, we detect a systematic alignment of giant arcs with the ellipticity of the baryonic component of the lens in concordance with previous studies. The lens redshift distribution corresponding to both the giant arcs and all arcs, estimated from photometric catalogs, peaks at z~0.6. Owing to the large area and depth of the CFHTLS, we find the largest lens sample probing group-scales for the first time. We compare the observed image separation distribution (ISD) of our arcs with theoretical models. A two-component density profile for the lenses which accounts for both the central galaxy and dark matter component is required by the data to explain the observed ISD. Unfortunately, current levels of uncertainties and degeneracies accommodate models both with and without adiabatic contraction. We also show the effects of changing parameters of the model that predict the ISD and that a larger lens sample might constrain relations such as the concentration-mass relation, mass-luminosity relation and slope of the luminosity function. (abridged), Comment: 21 pages, 11 figures, 3 tables ApJ accepted, some structural changes to the paper and peak of the redshift distribution changed when taken into account the photoz errors

Published
2012

49. Multi-frequency VLBI observations of the gravitational lens B2016+112

Author

Anupreeta More and Richard W. Porcas

Subjects
Lens (optics), Physics, Gravitational lens, law, Very-long-baseline interferometry, Magnification, Astrophysics, Spectral line, law.invention
Abstract

We present Global VLBI and HSA images of the gravitational lens B2016+112 at 18, 6 and 3.6 cm. Previous VLBI observations showed that images A and B (which are clearly lensed images of a single background source) and the elongated region C are each divided into components. Our new high-resolution maps reveal more components in images A and B, clearly demonstrating their expected opposite parities. According to the scenario of Koopmans et al. (2002), the arc-like region C consists of two merging, partial images (``C1-C2'') of just a small region of the same background source, seen with high lens magnification. We have determined the spectra and relative positions of the components within all four images in order to test this scenario. We find that the outer north-west components in images A and B do indeed have radio spectra similar to the components seen in C1 and C2.

Published
2007
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50. Chitah: STRONG-GRAVITATIONAL-LENS HUNTER IN IMAGING SURVEYS

Author

Tzihong Chiueh, Sherry H. Suyu, James H. H. Chan, Anupreeta More, Paul A. Price, Jean Coupon, Masamune Oguri, and Philip J. Marshall

Subjects
Physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Cosmology, law.invention, Einstein radius, Lens (optics), Telescope, Gravitational lens, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Galaxy formation and evolution
Abstract

Strong gravitationally lensed quasars provide powerful means to study galaxy evolution and cosmology. Current and upcoming imaging surveys will contain thousands of new lensed quasars, augmenting the existing sample by at least two orders of magnitude. To find such lens systems, we built a robot, CHITAH, that hunts for lensed quasars by modeling the configuration of the multiple quasar images. Specifically, given an image of an object that might be a lensed quasar, CHITAH first disentangles the light from the supposed lens galaxy and the light from the multiple quasar images based on color information. A simple rule is designed to categorize the given object as a potential four-image (quad) or two-image (double) lensed quasar system. The configuration of the identified quasar images is subsequently modeled to classify whether the object is a lensed quasar system. We test the performance of CHITAH using simulated lens systems based on the Canada-France-Hawaii Telescope Legacy Survey. For bright quads with large image separations (with Einstein radius $r_{\rm ein}>1.1"$) simulated using Gaussian point-spread functions, a high true-positive rate (TPR) of $\sim$90% and a low false-positive rate of $\sim$$3\%$ show that this is a promising approach to search for new lens systems. We obtain high TPR for lens systems with $r_{\rm ein}\gtrsim0.5"$, so the performance of CHITAH is set by the seeing. We further feed a known gravitational lens system, COSMOS 5921$+$0638, to CHITAH, and demonstrate that CHITAH is able to classify this real gravitational lens system successfully. Our newly built CHITAH is omnivorous and can hunt in any ground-based imaging surveys., 10 pages, 10 figures (accepted for publication in ApJ)

Published
2015
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