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306 results on '"BINARIES"'

1. The dynamics, stability and manifestation of circumbinary orbits

Author

Doolin, Samuel and Blundell, Katherine

Subjects
521.3, Physical Sciences, Physics, Astrophysics, stars, binaries, circumbinary
Abstract

I numerically investigate the dynamics of orbits in 3D circumbinary phase-space as a function of binary eccentricity and mass fraction. I find that inclined circumbinary orbits in the elliptically-restricted three-body problem display a nodal libration mechanism in the longitude of the ascending node and in the inclination to the plane of the binary. I analyse and quantify the behaviour of these orbits and investigate their stability over time. This work is the first dynamically aware analysis of the stability of circumbinary orbits across both binary mass fraction and binary eccentricity. This work also has implications for exoplanetary astronomy in the existence and determination of stable orbits around binary systems. I also present an examination of the so-called radio ruff around the microquasar SS433, which I show to precess on a timescale of approximately 550 days. The observed precession in the projected angle of the ruff on the sky may be explained if the ruff feature arises from an inclined circumbinary excretion disk. In addition, I describe a pilot study in the near-infrared waveband in search of circumbinary material around other microquasars.

Published
2012

2. Eclipses of jets and discs of X-ray binaries as a powerful tool for understanding jet physics and binary parameters.

Author

Maccarone, Thomas J, van den Eijnden, Jakob, Russell, Thomas D, and Degenaar, Nathalie

Subjects
*X-ray binaries, *BINARY black holes, *ECLIPSES, *SPECTRAL energy distribution, *PHYSICS, *STANDARD deviations, *JET engines, *LIGHT curves
Abstract

We calculate the expected effects on the spectral energy distributions and light curves in X-ray binary jets from eclipses by the donor stars. Jets will be eclipsed for all inclination angles, with just the height along the jet where the eclipse takes place being set by the orbital parameters. Typically, eclipses will lead to 5–10 per cent reductions in the jet emission over a range of a factor of few in wavelength with a periodic modulation. In ideal systems with high inclination angles, relatively even mass ratios, and modest jet speeds, the eclipses may be deeper. We discuss how eclipses can be used to measure binary system parameters, as well as the height of the bases of the jets. We also discuss how, with data sets that will likely require future facilities, more detailed tests of models of jet physics could be made by establishing deviations from the standard recipes for compact conical flat spectrum jets and by determining the ingress and egress durations of the eclipses and measuring the transverse size of the jets. We provide representative calculations of expectations for different classes of systems, demonstrating that the most promising target for showing this effect in the radio band is the longer period 'atoll'-class neutron star X-ray binaries, while in the optical and infrared bands, the best candidates are likely to be the most edge-on black hole X-ray binaries. We also discuss the effects of the outer accretion disc eclipsing the inner jet. [ABSTRACT FROM AUTHOR]

Published
2020
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3. Detection and Characterization of Exoplanet and Binary Star Systems Through Direct Imaging and Spectroscopy

Author

Lipartito, Isabel Alexandra

Subjects
Astrophysics, Physics, Astrophysics, binaries, exoplanets, high contrast imaging, instrumentation, MKIDs, open clusters
Abstract

High contrast imaging and high-resolution spectroscopy are powerful techniques to characterize multi-component astronomical systems, examples of which range from stars with planetary companions to similar-mass stellar binaries. The first part of this thesis concerns the instrumentation and science behind detecting substellar companions. We present the development of single photon-counting detectors known as Microwave Kinetic Inductance Detectors (MKIDs) for exoplanet direct imaging. Optical/Near-IR MKIDs are low noise detectors which can resolve both the energy and arrival time of individual photons, returning microsecond-accurate time-tagged photon lists. These lists allow for image processing techniques that take advantage of photon spectral and arrival time information to model and subtract the stellar background, leaving behind signal from the faint planetary companion. We discuss the commissioning and characterization of the MKID Exoplanet Camera (MEC), a 20,440 pixel MKID infrared camera that interfaces with the The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) planet finding instrument on the Subaru Telescope at Mauna Kea. MEC is the first permanently deployed near-infrared MKID instrument and is designed to operate both as an IFU, and as a focal plane wavefront sensor in a multi-kHz feedback loop with SCExAO. We present the development and construction of a second generation digital readout system for MEC. Our readout system is capable of identifying, analyzing, and recording photon detection events in real time with a time resolution of order a few microseconds.The second part of this thesis addresses the characterization of the orbital properties and stellar components of multiple star systems through high-resolution spectroscopy. We analyze stellar binaries observed with the Michigan/Magellan Fiber System (M2FS), a fiber-fed double spectrograph that was used to complete a several year-long survey of the core half-degree of open clusters NGC 2516 and NGC 2422. This survey targeted all stars identified as solar-analog photometric members. We present orbits for 24 binaries in the field of NGC 2516 (300 Myr) and 13 binaries in the field of NGC 2422 (130 Myr). Six of these systems are double-lined spectroscopic binaries (SB2s). We fit these RV variable systems with orvara, a MCMC-based fitting program that models Keplerian orbits. We use precise stellar parallaxes and proper motions from Gaia EDR3 to determine cluster membership. We impose a barycentric radial velocity prior on all cluster members; this significantly improves our orbital constraints.Two of our systems have periods between 5 and 15 days, the critical window in which tides efficiently damp orbital eccentricity. These binaries should be included in future analyses of circularization across similarly-aged clusters. We also find a relatively flat distribution of binary mass ratios, consistent with previous work. We identify a field star whose secondary has a mass in the brown dwarf range, as well as two cluster members whose RVs suggest the presence of an additional companion. Our orbital fits will help constrain the binary fraction and binary properties across stellar age and across stellar environmentThis thesis explores the detection and characterization of stellar companions at opposite ends of the companion mass range: planetary and stellar. We present technological advances ranging across the fields of instrumentation, image processing (both real-time and post-processing), and stellar system characterization.

Published
2021

4. Test of the Weak Equivalence Principle using LIGO observations of GW150914 and Fermi observations of GBM transient 150914

Author

Molin Liu, Zonghua Zhao, Xiaohe You, Jianbo Lu, and Lixin Xu

Subjects
Gravitational-waves, Black hole physics, Gamma-ray bursts, Binaries, Physics, QC1-999
Abstract

About 0.4 s after the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a transient gravitational-wave (GW) signal GW150914, the Fermi Gamma-ray Burst Monitor (GBM) also found a weak electromagnetic transient (GBM transient 150914). Time and location coincidences favor a possible association between GW150904 and GBM transient 150914. Under this possible association, we adopt Fermi's electromagnetic (EM) localization and derive constraints on possible violations of the Weak Equivalence Principle (WEP) from the observations of two events. Our calculations are based on four comparisons: (1) The first is the comparison of the initial GWs detected at the two LIGO sites. From the different polarizations of these initial GWs, we obtain a limit on any difference in the parametrized post-Newtonian (PPN) parameter Δγ≲10−10. (2) The second is a comparison of GWs and possible EM waves. Using a traditional super-Eddington accretion model for GBM transient 150914, we again obtain an upper limit Δγ≲10−10. Compared with previous results for photons and neutrinos, our limits are five orders of magnitude stronger than those from PeV neutrinos in blazar flares, and seven orders stronger than those from MeV neutrinos in SN1987A. (3) The third is a comparison of GWs with different frequencies in the range [35 Hz, 250 Hz]. (4) The fourth is a comparison of EM waves with different energies in the range [1 keV, 10 MeV]. These last two comparisons lead to an even stronger limit, Δγ≲10−8. Our results highlight the potential of multi-messenger signals exploiting different emission channels to strengthen existing tests of the WEP.

Published
2017
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5. The New Ephemeris and Light Curve Analysis of V870 Ara by the Ground-Based and TESS Data

Author

Mark G. Blackford, Samaneh Rezaei, Mohammad Madani, Elnaz Bozorgzadeh, Amirreza Mohandes, Atila Poro, and Fatemeh Davoudi

Subjects
stars, Physics, Astronomy, Monte Carlo method, FOS: Physical sciences, Binary number, QB1-991, Astronomy and Astrophysics, Contact binary, Astrophysics, Mass ratio, Ephemeris, Light curve, eclipsing, photometric, Astrophysics - Solar and Stellar Astrophysics, individual (v870 ara), Space and Planetary Science, Observatory, techniques, binaries, Parallax, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

New CCD photometric observations and their investigation of the W UMa-type binary, V870 Ara, are presented. Light curves of the system were taken through BVI filters from the Congarinni Observatory in Australia. The new ephemeris is calculated based on seven new determined minimum times, together with the TESS data and others compiled from the literature. Photometric solutions determined by the Wilson-Devinney (W-D) code are combined with the Monte Carlo simulation to determine the adjustable parameters' uncertainties. These solutions suggest that V870 Ara is a contact binary system with a mass ratio of 0.082, a fillout factor of 96+-4 percent, and an inclination of 73.60+-0.64 degrees. The absolute parameters of V870 Ara were determined by combining the Gaia EDR3 parallax and photometric elements., Comment: 5 tables, 6 figs, accepted in the Open Astronomy Journal

Published
2021

6. Unveiling wide-orbit companions to K-type stars in Sco-Cen with Gaia EDR3

Author

Bohn, Alexander J., Ginski, Christian, Kenworthy, Matthew A., Mamajek, Eric E., Meshkat, Tiffany, Pecaut, Mark J., Reggiani, Maddalena, Seay, Christopher R., Brown, Anthony, Cugno, Gabriele, Henning, Thomas, Launhardt, Ralf, Quirrenbach, Andreas, Rickman, Emily L., and Ségransan, Damien

Subjects
Astrophysics - instrumentation and methods for astrophysics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Astrophysics - solar and stellar astrophysics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Brown dwarfs, visual, brown dwarfs, astrometry, open clusters and associations: individual: Sco-Cen, stars: individual: TYC 8252-533-1 [binaries], Astrophysics - earth and planetary astrophysics, Binaries, Stars - individual - TYC 8252-533-1, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrometry, Open clusters and associations - individual: Sco-Cen, Stars, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Orbit (control theory), Visual
Abstract

Abbreviated. We aim to identify new low-mass companions to young stars using the astrometric measurements provided by the Gaia space mission and complementary VLT/SPHERE data. We identify companion candidates from a sample of K-type, pre-main sequence stars in the Scorpius Centaurus association using the early version of the third data release of the Gaia space mission. Based on the provided positions, proper motions, and magnitudes, we identify all objects within a predefined radius whose differential proper motions are consistent with a gravitationally bound system. We derive companion masses through comparison with evolutionary tracks. For seven identified companion candidates we use additional data collected with VLT/SPHERE and VLT/NACO to assess the accuracy of the properties of the companions based on Gaia photometry alone. We identify 110 comoving companions that have a companionship likelihood of more than $95\,\%$. We identify ten especially intriguing companions that have masses in the brown dwarf regime down to $20\,M_\mathrm{Jup}$. Our high-contrast imaging data confirm both astrometry and photometric masses derived from Gaia alone. We discover a new brown dwarf companion, TYC 8252-533-1 B, with a projected separation of approximately $570\,\mathrm{au}$ from its Sun-like primary. SED modeling provides a companion mass of $52^{+17}_{-11}\,M_\mathrm{Jup}$. We show that the Gaia database can identify low-mass companions at wide separations from their host stars. For K-type Sco-Cen members Gaia can detect sub-stellar objects at projected separations larger than $300\,\mathrm{au}$ and is sensitivity limited beyond $1,000\,\mathrm{au}$ with a lower mass limit down to $20\,M_\mathrm{Jup}$. A similar analysis of other star-forming regions could significantly enlarge the sample size of such objects and test formation and evolution theories of planetary systems., Accepted for publication in A&A (31 pages, 20 figures, 12 tables)

Published
2022

7. The amplitude of the kilohertz quasi-periodic oscillations in 4U 1636-53 in the frequency-energy space

Author

Mariano Mendez, Evandro M. Ribeiro, Konstantinos Karpouzas, Guobao Zhang, Marcio G. B. de Avellar, and Astronomy

Subjects
stars, Accretion, KHZ QPO, NEUTRON-STARS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Photon energy, Parameter space, PRECESSION, X-rays: binaries, BINARIES, neutron, Radiative transfer, COHERENCE, X-RAY VARIABILITY, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Accretion (meteorology), DISKS, Astronomy and Astrophysics, accretion discs, stars: individual : 4U 1636-53, MODEL, Neutron star, Amplitude, Space and Planetary Science, DISCOVERY, Precession, Astrophysics - High Energy Astrophysical Phenomena, SOURCE STATES, Energy (signal processing)
Abstract

We present for the neutron-star low-mass X-ray binary 4U 1636–53, and for the first time for any source of kilohertz quasi-periodic oscillations (kHz QPOs), the two-dimensional behaviour of the fractional rms amplitude of the kHz QPOs in the parameter space defined by QPO frequency and photon energy. We find that the rms amplitude of the lower kHz QPO increases with energy up to $\sim \!\!12$ keV and then decreases at higher energies, while the rms amplitude of the upper kHz QPO either continues increasing or levels off at high energies. The rms amplitude of the lower kHz QPO increases and then decreases with frequency, peaking at $\sim \!\!760$ Hz, while the amplitude of the upper kHz QPO decreases with frequency, with a local maximum at around $\sim \!\!770$ Hz, and is consistent with becoming zero at the same QPO frequency, $\sim \!\!1400$ Hz, in all energy bands, thus constraining the neutron-star mass at $M_{NS} \le 1.6 \, \mathrm{M}_{\odot }$, under the assumption that this QPO reflects the Keplerian frequency at the inner edge of the accretion disc. We show that the slope of the rms energy spectrum is connected to the changing properties of the kHz QPOs in different energy bands as its frequencies change. Finally, we discuss a possible mechanism responsible for the radiative properties of the kHz QPOs and, based on a model in which the QPO arises from oscillations in a Comptonizing cloud of hot electrons, we show that the properties of the kHz QPOs can constrain the thermodynamic properties of the inner accretion flow.

Published
2019

8. Fundamental parameters and abundance analysis of the components in the SB2 system HD 60803

Author

Andrew Tkachenko, Tatiana Ryabchikova, S. Zvyagintsev, V. Tsymbal, E. Semenko, and Yu. V. Pakhomov

Subjects
Abundance (chemistry), LI-7, fundamental parameters [stars], FOS: Physical sciences, Binary number, SOFTWARE, Astronomy & Astrophysics, spectroscopic [binaries], Spectral line, BINARIES, SPECTRA, LITHIUM, CHROMOSPHERIC ACTIVITY, Solar and Stellar Astrophysics (astro-ph.SR), Physics, atmospheres [stars], Science & Technology, SPECTROSCOPY, individual: HD 60803 [stars], Significant difference, Astronomy and Astrophysics, DIFFERENCE, Condensation temperature, abundances [stars], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physical Sciences, Atomic physics, STARS
Abstract

We performed a detailed spectroscopic study of the SB2 system HD 60803 based on high-resolution spectra obtained with the different spectrographs. The analysis was done with two independent methods: a) the direct modelling of the observed binary spectrum by a sum of synthetic spectra varying a set of free parameters and minimizing a difference between the observed and theoretical spectra; b) spectrum disentangling and an independent modelling of the individual components. Being applied to binary spectra from different spectrographs both methods converge to a consistent solution for the fundamental parameters of the HD 60803 components: $T_{\rm eff}$=6055$\pm$70 K, $\log{g}$=4.08$\pm$0.12, $\zeta_{\rm RT}$=1.45$\pm$0.18 km s$^{-1}$, [M/H]=0.03$\pm$0.06 (primary), and $T_{\rm eff}$=6069$\pm$70 K, $\log{g}$=4.14$\pm$0.09, $\zeta_{\rm RT}$=1.48$\pm$0.18 km s$^{-1}$, [M/H]=0.03$\pm$0.06 (secondary). Differential abundance analysis of the components did not reveal any significant difference in their chemical composition. Besides Li both components have solar atmospheric abundances. Li abundance exceeds the solar one by $\sim$2 dex, but it agrees with Li abundance in main-sequence late F-stars. Relative-to-solar abundances in both components slightly correlate with the condensation temperature the same way as was found in the solar analogs with/without detected giant planets. The estimated age of the system is 5.5$\pm$0.5 Gyr., Comment: 10 pages, 8 figures, 4 tables, accepted in MNRAS

Published
2021

9. The EBLM project - VIII. First results for M-dwarf mass, radius, and effective temperature measurements using CHEOPS light curves

Author

David V. Martin, N. A. Walton, Isabelle Boisse, Giampaolo Piotto, Matthew P. Battley, Roberto Ragazzoni, A. Deline, Demetrio Magrin, J. Asquier, Roi Alonso, H. G. Floren, N. Miller, M. Steller, Pierre F. L. Maxted, Didier Queloz, Ignasi Ribas, Stéphane Udry, S. C. C. Barros, S. G. Sousa, C. Lovis, Kevin Heng, Manuel Guedel, G. Anglada Escudé, Sébastien Charnoz, Melissa J. Hobson, Monika Lendl, B.-O. Demory, M. I. Swayne, M. Beck, László L. Kiss, Nuno C. Santos, David Barrado, J. Cabrera, Willy Benz, Sz. Csizmadia, Thomas Beck, P. Guterman, Enric Palle, Damien Ségransan, Yann Alibert, Sergio Hoyer, G. Olofsson, Georgina Dransfield, Matthew R. Standing, Davide Gandolfi, S. Lalitha, N. Thomas, Alexis Brandeker, A. E. Simon, Wolfgang Baumjohann, Don Pollacco, C. Broeg, Guillaume Hébrard, Nascimbeni, Kunovac Hodžić, Alexis M. S. Smith, T. G. Wilson, Emma Willett, Nicola Rando, A. Bekkelien, M.-D. Busch, Ingo Walter, Van Grootel, A. Santerne, M. Fridlund, Gy. M. Szabó, David Ehrenreich, Nicolas Billot, James McCormac, K. G. Isaak, I. Pagano, Magali Deleuil, Andrea Fortier, S. Salmon, Xavier Bonfils, A. Lecavelier des Etangs, Heike Rauer, Laetitia Delrez, N. Heidari, Luca Fossati, Amaury H. M. J. Triaud, A. Collier Cameron, Melvyn B. Davies, G. Scandariato, Gisbert Peter, M. Steinberger, Luca Marafatto, D. Futyan, Roland Ottensamer, Jacques Laskar, Michaël Gillon, Anders Erikson, T. Bárczy, Olivier Demangeon, Coel Hellier, A. Bonfanti, Keele University [Keele], Instituto de Astrofísica e Ciências do Espaço (IASTRO), 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 de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)

Subjects
Fundamental Parameters, Spectroscopic, 01 natural sciences, Categorical grant, spectroscopic [Techniques], techniques: photometric, stars: low-mass, QB460, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, media_common, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Horizon (archaeology), eclipsing [Binaries], 520 Astronomy, European research, 500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften, binaries: eclipsing, 3rd-DAS, Radius, 3. Good health, Astrophysics - Solar and Stellar Astrophysics, stars: fundamental parameters, Astrophysics::Earth and Planetary Astrophysics, Meteorology, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometric, fundamental parameters [Stars], low-mass [Stars], 0103 physical sciences, media_common.cataloged_instance, Low-Mass, European union, Eclipsing, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB600, 010308 nuclear & particles physics, photometric [Techniques], Binaries, Astronomy and Astrophysics, Effective temperature, 620 Engineering, Light curve, Stars, Techniques, QC Physics, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract

The accuracy of theoretical mass, radius and effective temperature values for M-dwarf stars is an active topic of debate. Differences between observed and theoretical values have raised the possibility that current theoretical stellar structure and evolution models are inaccurate towards the low-mass end of the main sequence. To explore this issue we use the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low mass stellar companions. We use these light curves combined with the spectroscopic orbit for the solar-type companion to measure the mass, radius and effective temperature of the M-dwarf star. Here we present the analysis of three eclipsing binaries. We use the pycheops data analysis software to fit the observed transit and eclipse events of each system. Two of our systems were also observed by the TESS satellite -- we similarly analyse these light curves for comparison. We find consistent results between CHEOPS and TESS, presenting three stellar radii and two stellar effective temperature values of low-mass stellar objects. These initial results from our on-going observing programme with CHEOPS show that we can expect to have ~24 new mass, radius and effective temperature measurements for very low mass stars within the next few years., Comment: 12 pages, 8 figures, accepted for publication in MNRAS

Published
2021

10. VLTI-MATISSE chromatic aperture-synthesis imaging of η Carinae's stellar wind across the Brα line: Periastron passage observations in February 2020

Author

Th. Rivinius, C. M. P. Russell, A. Domiciano de Souza, Uwe Beckmann, Lucas Labadie, F. Allouche, P. Cruzalèbes, Sylvie Robbe-Dubois, Antoine Mérand, William C. Danchi, A. F. J. Moffat, Kenji Hamaguchi, Michael F. Corcoran, József Varga, Alexis Matter, Thomas I. Madura, Stephane Lagarde, Sebastian Wolf, Anthony Meilland, Walter Jaffe, Paul Bristow, T. R. Gull, Felix Bettonvil, D. A. Espinoza-Galeas, Jose H. Groh, J. C. Augereau, Carsten Dominik, W. J. de Wit, Markus Schöller, J. Leftley, V. Hocdé, Uwe Graser, R. van Boekel, F. Navarete, L. Klarmann, K. Ohnaka, Leonard Burtscher, Th. Henning, Karl-Heinz Hofmann, Augusto Damineli, Ian R. Stevens, C. Connot, Klaus Meisenheimer, Stefan Kraus, Patrick W. Morris, G. Yoffe, Michiel R. Hogerheijde, Romain Petrov, Ph. Berio, M. Heininger, Henrik Hartman, J. W. Isbell, Markus Wittkowski, Eric Pantin, E. Kokoulina, J. Drevon, Julien Woillez, L. B. F. M. Waters, E. Nußbaum, Dieter Schertl, Bruno Lopez, Alexander Kreplin, Gerd Weigelt, Florentin Millour, D. J. Hillier, J. Hron, M. Lehmitz, V. Gámez Rosas, J. Sanchez-Bermudez, Noel D. Richardson, C. A. Hummel, Claudia Paladini, Andrea Mehner, Farrokh Vakili, Andreas Glindemann, P. Antonelli, C. Leinert, Gérard Zins, Philippe Stee, and Low Energy Astrophysics (API, FNWI)

Subjects
Interferometric, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), individual: eta Carinae [stars], Context (language use), Outflows, Individual, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Winds, 01 natural sciences, Spectral line, outflows, Mass-Loss, general [binaries], massive [stars], Astronomi, astrofysik och kosmologi, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics and Cosmology, winds [stars], General, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), O-type star, Physics, 010308 nuclear & particles physics, Binaries, Astronomy and Astrophysics, mass-loss [stars], Radius, Stars, Techniques, interferometric [techniques], Luminous blue variable, 13. Climate action, Space and Planetary Science, Massive, Astrophysics::Earth and Planetary Astrophysics, η Carinae
Abstract

Context. Eta Carinae is a highly eccentric, massive binary system (semimajor axis ~15.5 au) with powerful stellar winds and a phase-dependent wind-wind collision (WWC) zone. The primary star, η Car A, is a luminous blue variable (LBV); the secondary, η Car B, is a Wolf-Rayet or O star with a faster but less dense wind. Aperture-synthesis imaging allows us to study the mass loss from the enigmatic LBV η Car. Understanding LBVs is a crucial step toward improving our knowledge about massive stars and their evolution. Aims. Our aim is to study the intensity distribution and kinematics of η Car’s WWC zone. Methods. Using the VLTI-MATISSE mid-infrared interferometry instrument, we perform Brα imaging of η Car’s distorted wind. Results. We present the first VLTI-MATISSE aperture-synthesis images of η Car A’s stellar windin several spectral channels distributed across the Brα 4.052 μm line (spectral resolving power R ~ 960). Our observations were performed close to periastron passage in February 2020 (orbital phase ~ 14.0022). The reconstructed iso-velocity images show the dependence of the primary stellar wind on wavelength or line-of-sight (LOS) velocity with a spatial resolution of 6 mas (~14 au). The radius of the faintest outer wind regions is ~26 mas (~60 au). At several negative LOS velocities, the primary stellar wind is less extended to the northwest than in other directions. This asymmetry is most likely caused by the WWC. Therefore, we see both the velocity field of the undisturbed primary wind and the WWC cavity. In continuum spectral channels, the primary star wind is more compact than in line channels. A fit of the observed continuum visibilities with the visibilities of a stellar wind CMFGEN model (CMFGEN is an atmosphere code developed to model the spectra of a variety of objects) provides a full width at half maximum fit diameter of the primary stellar wind of 2.84 ± 0.06 mas (6.54 ± 0.14 au). We comparethe derived intensity distributions with the CMFGEN stellar wind model and hydrodynamic WWC models.

Published
2021

12. Coherent radio emission from a population of RS Canum Venaticorum systems

Author

Joseph R. Callingham, K. C. Veken, Ph. Zarka, S. E. B. Toet, Harish Vedantham, A. Drabent, Timothy W. Shimwell, H. J. A. Röttgering, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), and Astronomy

Subjects
010504 meteorology & atmospheric sciences, Radio Continuum, Radiation mechanisms: non-thermal, Radio continuum: stars, Radiation Mechanisms, Stars: variables: general, Astrophysics, 01 natural sciences, law.invention, coronae -stars, law, Magnetic Field, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics, general -stars, Stars: coronae, Maser, 010303 astronomy & astrophysics, Chromosphere, Physics, education.field_of_study, Stars: magnetic field, Astrophysics - Solar and Stellar Astrophysics, Brightness temperature, Physics::Space Physics, Coronae, general -radio continuum, Astrophysics::High Energy Astrophysical Phenomena, Population, variables, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Instability, Acceleration, 0103 physical sciences, Binaries: general, education, General, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astronomy and Astrophysics, LOFAR, Stars, non-thermal, Space and Planetary Science, [SDU]Sciences of the Universe [physics], magnetic field -stars, binaries, starsradiation mechanisms
Abstract

Coherent radio emission from stars can be used to constrain fundamental coronal plasma parameters, such as plasma density and magnetic field strength. It is also a probe of chromospheric and magnetospheric acceleration mechanisms. Close stellar binaries, such as RS Canum Venaticorum (RS CVn) systems, are particularly interesting as their heightened level of chromospheric activity and possible direct magnetic interaction make them a unique laboratory to study coronal and magnetospheric acceleration mechanisms. RS CVn binaries are known to be radio-bright but coherent radio emission has only conclusively been detected previously in one system. Here, we present a population of 14 coherent radio emitting RS CVn systems. We identified the population in the ongoing LOFAR Two Metre Sky Survey as circularly polarised sources at 144MHz that are astrometrically associated with known RS CVn binaries. We show that the observed emission is powered by the electron cyclotron maser instability. We use numerical calculations of the maser's beaming geometry to argue that the commonly invoked 'loss-cone' maser cannot generate the necessary brightness temperature in some of our detections and that a more efficient instability, such as the shell or horseshoe maser, must be invoked. Such maser configurations are known to operate in planetary magnetospheres. We also outline two acceleration mechanisms that could produce coherent radio emission, one where the acceleration occurs in the chromosphere and one where the acceleration is due to an electrodynamic interaction between the stars. We propose radio and optical monitoring observations that can differentiate between these two mechanisms., This article consists of 14 pages, 10 normal figures and 4 gifs. The gifs themselves each consist of 32 figures. This article is to be published in Astronomy and Astrophysics, section 8. 'Stellar Atmospheres'

Published
2021

13. A new radio census of neutron star X-ray binaries

Author

M. Armas Padilla, J. van den Eijnden, Mark Reynolds, Craig O. Heinke, Thomas D. Russell, Elena Gallo, J. C. A. Miller-Jones, T. J. Maccarone, G. R. Sivakoff, Jon M. Miller, Rudy Wijnands, P. Atri, J. V. Hernández Santisteban, D. M. Russell, Arash Bahramian, Aarran W. Shaw, D. Maitra, Rich Plotkin, Nathalie Degenaar, University of St Andrews. School of Physics and Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Accretion, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Binaries, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, neutron [Stars], DAS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion (finance), Neutron star, QC Physics, Space and Planetary Science, 0103 physical sciences, QB Astronomy, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Accretion discs, QC, QB
Abstract

We report new radio observations of a sample of thirty-six neutron star (NS) X-ray binaries, more than doubling the sample in the literature observed at current-day sensitivities. These sources include thirteen weakly-magnetised ($B, Accepted for publication in MNRAS; 31 pages, 8 figures, 8 tables (including online supplementary materials)

Published
2021

14. THE ON- AND OFF-STATE GENERATIONS IN THE CASE OF THE THICK ACCRETION DISK AND UNDEFINED PRECESSION PERIOD. 3-D NUMERICAL HYDRODYNAMICAL SIMULATIONS IN ACCRETION DISK IN MICROQUASAR CYG X-1

Author

V. V. Nazarenko

Subjects
Physics, lcsh:QB1-991, Jet (fluid), Stars, Period (periodic table), Accretion disc, Radiation pressure, lcsh:Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Precession, Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars, binaries, jets, numerical - hydrodynamics methods
Abstract

In the present work we have com- puted the thick accretion disk (the accretion disk with radiation pressure) for the case of undefined precession over very long time (more than 14 precession periods). The calculations show that in this case the origin of the ON-states and OFF-states are strong irregular in time. The calculations also show that the jet’s launches are taking place very suddenly over 7 ÷ 20 minutes of the orbital time. The jet’s launches over OFF-states occurs discrete as it is observed in real microquasars.

Published
2019

15. Six new rapidly oscillating Ap stars in the Kepler long-cadence data using super-Nyquist asteroseismology

Author

Timothy R. Bedding, Daniel Luke Holdsworth, Benjamin J. Fulton, Simon J. Murphy, Daniel Huber, Margarida S. Cunha, Daniel R. Hey, D. W. Kurtz, and Andrew W. Howard

Subjects
oscillations [stars], MODELS, FOS: Physical sciences, F500, asteroseismology, Astrophysics, FREQUENCY, Rotation, SEQUENCE, 01 natural sciences, Kepler, Asteroseismology, photometric [techniques], Amplitude modulation, BINARIES, chemically peculiar [stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nyquist–Shannon sampling theorem, MODULATION, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), MISSION, Physics, ROAP STAR, 010308 nuclear & particles physics, Astronomy and Astrophysics, ROTATIONAL VELOCITIES, Cutoff frequency, PULSATION, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, DELTA-SCUTI, Astrophysics::Earth and Planetary Astrophysics, Nyquist frequency
Abstract

We perform a search for rapidly oscillating Ap stars in the Kepler long-cadence data, where true oscillations above the Nyquist limit of 283.21 {\mu}Hz can be reliably distinguished from aliases as a consequence of the barycentric time corrections applied to the Kepler data. We find evidence for rapid oscillations in six stars: KIC 6631188, KIC 7018170, KIC 10685175, KIC 11031749, KIC 11296437 and KIC 11409673, and identify each star as chemically peculiar through either pre-existing classifications or spectroscopic measurements. For each star, we identify the principal pulsation mode, and are able to observe several additional pulsation modes in KIC 7018170. We find that KIC 7018170 and KIC 11409673 both oscillate above their theoretical acoustic cutoff frequency, whilst KIC 11031749 oscillates at the cutoff frequency within uncertainty. All but KIC 11031749 exhibit strong amplitude modulation consistent with the oblique pulsator model, confirming their mode geometry and periods of rotation., Comment: 20 pages, 14 figures, accepted for publication in MNRAS

Published
2019

16. Neutrino production in Population III microquasars

Author

Matías M. Reynoso, Agustín M. Carulli, and Gustavo E. Romero

Subjects
Ciencias Astronómicas, RADIATION MECHANISMS, Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, X-RAYS, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Compact star, 01 natural sciences, purl.org/becyt/ford/1 [https], BINARIES, Pion, 0103 physical sciences, education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Muon, 010308 nuclear & particles physics, COVID-19, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Galaxy, Redshift, NON-THERMAL – NEUTRINOS, Black hole, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Neutrinos, X-rays: binaries
Abstract

Microquasars (MQs) are binary systems composed by a star feeding mass to a compact object through an accretion disk. The compact object, usually a black hole, launches oppositely directed jets which are typically observed in our galaxy through their broadband electromagnetic emission. These jets are considered potential galactic neutrino sources. MQs can also have been formed by the first generations of stars in the universe, i.e., Population III (Pop III) stars, which are considered essential contributors to the ionization processes that took place during the period of acosmic reionizationa. In the present work, we develop a model that accounts for the main particle processes occurring within Pop III MQ jets, with the aim to obtain the diffuse neutrino flux at the Earth. We define different zones within the jets of Pop III MQs where particle interactions occur, and primary particles (i.e protons and electrons) are injected. We solve a transport equation for each zone, including the relevant cooling and escape processes, which include p γ and p p interactions. Once we obtain the primary particle distributions, we compute the pion and muon distributions, as well as the neutrino output produced by their decays. Finally, we obtain the diffuse neutrino flux by integration over the redshift, the line-of-sight angle, and the MQs lifetime. We find that, for a range of parameters suitable for Pop III MQ jets, the most relevant site for neutrino production in the jets is the base of the inner conical jet. Additionally, if protons accelerated at the forward shock formed at terminal jet region can escape from the outer shell, they would produce further neutrinos via p γ interactions with the cosmic microwave background (CMB). The latter contribution to the diffuse neutrino flux turns out to be dominant in the range 10 7 GeV ≲ E ν ≲ 10 9 GeV , while the neutrinos produced in the inner jet could only account for a small fraction of the IceCube flux for E ν ∼ 10 5 GeV. The co-produced multiwavelength photon background is also computed and it is checked to be in agreement with observations., Instituto Argentino de Radioastronomía

Published
2021

17. The Census of Exoplanets in Visual Binaries: population trends from a volume-limited Gaia DR2 and literature search

Author

C. Fontanive and Daniella Carolina Bardalez Gagliuffi

Subjects
lcsh:Astronomy, Population, Brown dwarf, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, lcsh:QB1-991, Planet, multiplicity, Astrophysics::Solar and Stellar Astrophysics, education, companions, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, formation, lcsh:QC801-809, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Stars, lcsh:Geophysics. Cosmic physics, exoplanets, Astrophysics - Solar and Stellar Astrophysics, visual, Astrophysics::Earth and Planetary Astrophysics, binaries, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present an extensive search in the literature and Gaia DR2 for visual co-moving binary companions to stars hosting exoplanets and brown dwarfs within 200 pc. We found 218 planet hosts out of 938 to be part of multiple-star systems, with 10 newly discovered binaries and 2 new tertiary stellar components. This represents an overall raw multiplicity rate of 23.2$\pm$1.6% for hosts to exoplanets across all spectral types, with multi-planet systems found to have a lower duplicity frequency at the 2.2$\sigma$ level. We found that more massive hosts are more often in binary configurations, and that planet-bearing stars in multiple systems are predominantly the most massive component of stellar binaries. Investigations of multiplicity as a function of planet mass and separation revealed that giant planets with masses >0.1 MJup are more frequently seen in stellar binaries than small sub-Jovian planets with a 3.6$\sigma$ difference, a trend enhanced for the most massive (>7 MJup) short-period (0.5 AU). While stellar companion mass appears to have no impact on planet properties, binary separation seems to be an important factor in the resulting structure of planetary systems. Stellar companions on separations, Comment: Accepted for publication in Frontiers in Astronomy and Space Sciences: Exoplanets, 26 pages, 10 figures

Published
2021

18. NuSTAR monitoring of MAXI J1348−630: evidence of high density disc reflection

Author

Francesco Tombesi, John A. Tomsick, Sudip Bhattacharyya, Sudip Chakraborty, Ajay Ratheesh, Gaurava K. Jaisawal, and Keigo Fukumura

Subjects
Accretion, Astrophysics::High Energy Astrophysical Phenomena, Data analysis, FOS: Physical sciences, Binary number, High density, Astrophysics, X-rays: individual: MAXI J1348-630, Spectral line, Accretion discs, Methods: data analysis, X-rays: binaries, Consistency (statistics), X-rays, Methods, individual: MAXI J1348−630 [X-rays], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Settore FIS/05, Binaries, Astronomy and Astrophysics, Black hole, Space and Planetary Science, Reflection (physics), Outflow, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the broadband spectral analysis of all the six hard, intermediate and soft state NuSTAR observations of the recently discovered transient black hole X-ray binary MAXI J1348-630 during its first outburst in 2019. We first model the data with a combination of a multi-colour disc and a relativistic blurred reflection, and, whenever needed, a distant reflection. We find that this simple model scheme is inadequate in explaining the spectra, resulting in a very high iron abundance. We, therefore, explore the possibility of reflection from a high-density disc. We use two different sets of models to describe the high-density disc reflection: relxill-based reflection models, and reflionx-based ones. The reflionx-based high-density disc reflection models bring down the iron abundance to around the solar value, while the density is found to be $10^{20.3-21.4} \rm cm^{-3}$. We also find evidence of a high-velocity outflow in the form of $\sim$7.3 keV absorption lines. The consistency between the best-fit parameters for different epochs and the statistical significance of the corresponding model indicates the existence of high-density disc reflection in MAXI J1348-630., 15 pages, 12 figures, 5 tables; accepted for publication in MNRAS

Published
2021

19. 20 Orbits of binaries based on soar speckle observations

Author

Edgardo Costa, Manuel Andrade, Rene A. Mendez, P. P. Campo, J. Gomez, José A. Docobo, and Universidade de Santiago de Compostela. Departamento de Matemática Aplicada

Subjects
Physics, Binaries, Astronomy, Astronomy and Astrophysics, Astrometry, Stars, Techniques, Speckle pattern, High angular resolution, Space and Planetary Science, Fundamental parameters, Soar, Visual
Abstract

New observational data obtained during the 2018, 2019, and 2020 speckle runs with the 4.1-m Southern Astrophysical Research (SOAR) telescope located at Cerro Pachón (Chile) allowed us to recalculate the orbits of the visual binaries: WDS 00277-1625 (YR 1 Aa,Ab), WDS 00462-2214 (RST4155), WDS 03124-4425 (JC 8), WDS 07427-3510 (HDS 1091), WDS 10093+2020 (A2145), WDS 10116+1321 (HU 874 AB), WDS 10217-0946 (BU 25), WDS 11585-2350 (RST 3767 AB), WDS 13117-2633 (FIN 305), WDS 13305+0729 (A 1789), and WDS 16458-0046 (A1141). In addition, we present the first orbits calculated for the following binaries: WDS 07303-5657 (FIN 105), WDS 09110-1929 (I 824), WDS 12111-5302 (HU 1604), WDS 14592-4206 (HDS 2116 Aa,Ab), WDS 15157-2736 (BU 350), WDS 15493+0503 (A 1126), WDS 16402-2800 (VOU 44 AB), and WDS 18126+1224 (HDS 2570). All of them are placed below Dec. + 21° and the majority are main-sequence stars. Except in cases with giant components or close triple systems, the ANAPAR method was used in order to obtain precise dynamical parallaxes and individual masses. These parallaxes were compared with those obtained by Gaia and/or Hipparcos satellites. In the case of FIN 305, we present two different orbital solutions. Also, using the dynamical parallaxes given by these orbits, we have been able to calculate the luminosity of these systems. Said luminosities allow us to indicate an approximate age for the components of these systems, situating them within the Hertzsprung-Russell (HR) diagram. In addition, a commentary for each binary about the physical and dynamical properties of the studied binaries has been included We are very grateful for the continuous support of the Chilean Telescope Allocation Committee: http://www.das.uchile.cl/das_cntac.html under programs CN2018A-1, CN2019A-2, CN2019B-13, and CN2020A-19 and 2020B-10. This paper was supported by the ‘Xunta de Galicia’ (Spain), under the ED431B 2020/38 grant. RAM and EC acknowledge support from ANID/FONDECYT grant 1190038 SI

Published
2021

20. Search for Lensing Signatures in the Gravitational-Wave Observations from the First Half of LIGO–Virgo’s Third Observing Run

Author

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., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, 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., 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., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Are, R., Ari, 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., Bonn, 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, Iii, H. W., Bustillo, J. Calderon, 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. Casanueva, 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., Ra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chass, e-Mottin, E., Chatterjee, D., Chaturvedi, M., 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, J, R., 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., Dal Canton, T., 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., Dhur, Har, S., Diaz, M. C., Diaz-Ortiz, 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., Ezquiaga, J. M., 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., Fern, ez-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., 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, 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., Gonzalez, G., Gopakumar, A., Gosselin, M., Gouaty, R., Goyal, S., 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. 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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, Laurentis, M, Deleglise, S, Favero, V, Lillo, F, Lillo, N, Pozzo, W, Demarchi, L, Matteis, F, D'Emilio, V, Demos, N, Dent, T, Depasse, A, Pietri, R, Rosa, R, Rossi, C, Desalvo, R, 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, Ezquiaga, J, 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, Feicht, J, Fejer, M, Feng, F, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Flynn, E, Fong, H, Font, J, Fornal, B, Forsyth, P, Franke, A, Frasca, S, Frasconi, F, Frederick, C, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fronze, G, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gais, J, Galaudage, S, Gamba, R, Ganapathy, D, Ganguly, A, Gaonkar, S, 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, Giardina, K, Gibson, D, Gier, C, Giesler, M, Giri, P, Gissi, F, Glanzer, J, Gleckl, A, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonzalez, G, Gopakumar, A, Gosselin, M, Gouaty, R, Goyal, S, Grace, B, Grado, A, Granata, M, Granata, V, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, A, Gretarsson, E, Griffith, D, Griffiths, W, Griggs, H, Grignani, G, Grimaldi, A, Grimes, E, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guerrero, J, Guidi, G, Guimaraes, A, Guixe, G, Gulati, H, Guo, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Guzman, F, Haegel, L, Halim, O, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, H, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hartwig, D, Haskell, B, Hasskew, R, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heinze, J, Heinzel, J, Heitmann, H, Hellman, F, Hello, P, Helmling-Cornell, A, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Hennig, M, Vivanco, F, Heurs, M, Hild, S, Hill, P, Hines, A, Hochheim, S, Hofman, D, Hohmann, J, Holgado, A, Holland, N, Hollows, I, Holmes, Z, Holt, K, Holz, D, Hopkins, P, Hough, J, Howell, E, Hoy, C, Hoyland, D, Hreibi, A, Hsu, Y, Huang, Y, Hubner, M, Huddart, A, Huerta, E, Hughey, B, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Idzkowski, B, Iess, A, Inchauspe, H, Ingram, C, Intini, G, Isi, M, Isleif, K, Iyer, B, Jaberianhamedan, V, Jacqmin, T, Jadhav, S, James, A, Jan, A, Jani, K, Janquart, J, Janssens, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jeunon, M, Jia, W, Jiang, J, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, 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, Khadka, S, Khalili, F, Khan, I, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, 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, Kringel, V, Krishnendu, N, Krolak, A, Kuehn, G, Kuei, F, Kumar, A, Kumar, P, Kumar, R, Kuns, K, Kwang, S, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lehmann, J, Lemaitre, A, Leon, E, Leroy, N, Letendre, N, Levin, Y, Leviton, J, Li, A, Li, B, Li, J, Li, T, Li, X, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, J, Liu, K, Liu, X, Llorens-Monteagudo, M, Lo, R, Lockwood, A, Lollie, M, London, L, Longo, A, Lopez, D, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Luck, H, Lumaca, D, Lundgren, A, Macas, R, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magana-Sandoval, F, Magazzu, C, Magee, R, Maggiore, R, Majorana, E, Makarem, C, Maksimovic, I, Maliakal, S, Malik, A, Man, N, Mandic, V, Mangano, V, Mango, J, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marion, F, Mark, Z, Marka, S, Marka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, M, Martinez, V, Martinovic, K, Martynov, D, Marx, E, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Mateu-Lucena, M, Matichard, F, Matiushechkina, M, Mavalvala, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mcclincy, P, Mccormick, S, Mcculler, L, Mcghee, G, Mcguire, S, Mcisaac, C, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Mehmet, M, Mehta, A, Melatos, A, Melchor, D, Mendell, G, Menendez-Vazquez, A, Menoni, C, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merritt, J, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, P, Meylahn, F, Mhaske, A, Miani, A, Miao, H, Michaloliakos, I, Michel, C, Middleton, H, Milano, L, Miller, A, Millhouse, M, Mills, J, Milotti, E, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mir, L, Mishkin, A, Mishra, C, Mishra, T, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Mo, G, Mogushi, K, Mohapatra, S, Mohite, S, Molina, I, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moraru, D, Morawski, F, More, A, Moreno, C, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C, Mozzon, S, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E, Murray, P, Musenich, R, Nadji, S, Nagar, A, Nardecchia, I, Naticchioni, L, Nayak, B, Nayak, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nguyen, T, Nichols, S, Nissanke, S, Nocera, F, Noh, M, Norman, M, North, C, Nuttall, L, Oberling, J, O'Brien, B, O'Dell, J, Oganesyan, G, Oh, J, Oh, S, Ohme, F, Ohta, H, Okada, M, Olivetto, C, Oram, R, O'Reilly, B, Ormiston, R, Ormsby, N, Ortega, L, O'Shaughnessy, R, O'Shea, E, Ossokine, S, Osthelder, C, Ottaway, D, Overmier, H, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Panda, P, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Paolone, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patel, M, Patricelli, B, Payne, E, Pechsiri, T, Pedraza, M, Pegoraro, M, Pele, A, Penn, S, Perego, A, Pereira, A, Pereira, T, Perez, C, Perigois, C, Perreca, A, Perries, S, Petermann, J, Petterson, D, Pfeiffer, H, Pham, K, Phukon, K, Piccinni, O, Pichot, M, Piendibene, M, Piergiovanni, F, Pierini, L, Pierro, V, Pillant, G, Pilo, F, Pinard, L, Pinto, I, Piotrzkowski, B, Piotrzkowski, K, Pirello, M, Pitkin, M, Placidi, E, Plastino, W, Pluchar, C, Poggiani, R, Polini, E, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Pracchia, M, Pradier, T, Prajapati, A, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, G, Prokhorov, L, Prosposito, P, Prudenzi, L, Puecher, A, Punturo, M, Puosi, F, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Quitzow-James, R, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Rail, S, Raja, S, Rajan, C, Ramirez, K, Ramirez, T, Ramos-Buades, A, Rana, J, Rapagnani, P, Rapol, U, Ratto, B, Raymond, V, Raza, N, Razzano, M, Read, J, Rees, L, Regimbau, T, Rei, L, Reid, S, Reitze, D, Relton, P, Rettegno, P, Ricci, F, Richardson, C, Richardson, J, Richardson, L, Ricker, P, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rocha, J, Rodriguez, S, 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(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, LIGO Scientific, VIRGO, 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-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)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Etudes Scientifiques (IHES), Virgo, (Astro)-Particles Physics, Van Swinderen Institute for Particle Physics and G, Grav. waves and fundamental physics, RS: FSE Grav. waves and fundamental physics, RS: FSE MSP, Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, 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., 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., Berry, C. P. L., 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., Iii, H. W. C., 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., 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., Favero, V. D., Lillo, F. D., Lillo, N. D., Pozzo, W. D., Demarchi, L. M., Matteis, F. D., D'Emilio, V., Demos, N., Dent, T., Depasse, A., Pietri, R. D., De Rosa, R., Rossi, C. D., Desalvo, R., Simone, R. D., 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., Ezquiaga, J. M., 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., 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., Goyal, S., 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., Janquart, J., 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., Karat, S., 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., Rosa, I. L., 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. 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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., Sathyaprakash, B. S., Sauter, O., Savage, R. L., Savant, V., Sawant, D., Sawant, H. L., Sayah, S., Schaetzl, D., Scheel, M., Scheuer, J., Schindler-Tyka, A., Schmidt, P., Schnabel, R., Schneewind, M., Schofield, R. M. S., Schonbeck, A., Schulte, B. W., Schutz, B. F., Schwartz, E., Scott, J., Scott, S. M., Seglar-Arroyo, M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Seo, E. G., Sequino, V., Sergeev, A., Setyawati, Y., Shaffer, T., Shahriar, M. S., Shams, B., Sharifi, S., Sharma, A., Sharma, P., Shawhan, P., Shcheblanov, N. S., Shen, H., Shikauchi, M., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shukla, K., Shyamsundar, S., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Somala, S. N., Son, E. J., Soni, K., Soni, S., Sorazu, B., Sordini, V., Sorrentino, F., Sorrentino, N., Soulard, R., Souradeep, T., Sowell, E., Spagnuolo, V., Spencer, A. P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Steer, D. A., Steinlechner, J., Steinlechner, S., Stops, D. J., Stover, M., Strain, K. A., Strang, L. C., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudbeck, J., Sudhagar, S., Sudhir, V., Suh, H. G., Summerscales, T. Z., Sun, H., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Szewczyk, P., Tacca, M., Tait, S. C., Talbot, C., Tanasijczuk, A. J., Tanner, D. B., Tao, D., Tapia, A., San Martin, E. N. T., Tasson, J. D., Tenorio, R., Terkowski, L., Test, M., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Toland, K., Tolley, A. E., Tonelli, M., Torres-Forne, A., Torrie, C. I., E Melo, I. T., Toyra, D., Trapananti, A., Travasso, F., Traylor, G., Tringali, M. C., Tripathee, A., Troiano, L., Trovato, A., Trudeau, R. J., Tsai, D. S., Tsai, D., Tsang, K. 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., Vanosky, J., 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. Y., Watchi, J., Weaver, B., Wei, L., Weinert, M., Weinstein, A. J., Weiss, R., Weller, C. M., Wellmann, F., Wen, L., Wessels, P., Westhouse, J. W., Wette, K., Whelan, J. T., White, D. D., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, M. J., Williamson, A. R., Willis, J. L., Willke, B., Wilson, D. J., Winkler, W., Wipf, C. C., Wlodarczyk, T., Woan, G., Woehler, J., Wofford, J. K., Wong, I. C. F., Wright, M., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yang, F. W., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yeeles, D. W., Yelikar, A. B., Yeung, M. C., Ying, M., Yoon, A., Yu, H., Zadrozny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, R., Zhang, T., Zhao, C., Zhao, G., Zhao, Y., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Laurentis, M. D., Rosa, R. D., The LIGO Scientific Collaboration, The Virgo Collaboration, Arène, M., Bécsy, B., Iii, H. W. Cain, Bustillo, J. Calderón, Diaz, J. Casanueva, Cavaglià, M., Cerdá-Durán, P., Cieślar, M., Cordero-Carrión, I., Curyło, M., Canton, T. Dal, Dálya, G., D’Angelo, B., D’Antonio, S., Laurentis, M. De, Deléglise, S., Favero, V. Del, Lillo, F. De, Lillo, N. De, Pozzo, W. Del, Matteis, F. De, D’Emilio, V., Pietri, R. De, Rosa, R. De, Rossi, C. De, Simone, R. De, Díaz, M. C., D’Onofrio, L., D’Urso, D., Estellés, H., Fronzé, G. G., García-Núñez, C., García-Quirós, C., Ghosh, Abhirup., Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Sourath, González, G., Guixé, G., Gupta, Anchal, Gupta, Anuradha, Vivanco, F. Hernandez, Hübner, M. T., Kéfélian, F., Królak, A., Kumar, Rahul, Kumar, Rakesh, Rosa, I. La, Lemaître, A., Lück, H., Hernandez, I. Magaña, Magaña-Sandoval, F., Magazzù, C., Márka, S., Márka, Z., Mir, Ll. M., Mo, Geoffrey, Mukherjee, Arunava, Mukherjee, Soma, Mukherjee, Subroto, Muñiz, E. A., O’Brien, B. D., O’Dell, J., O’Reilly, B., O’Shaughnessy, R., O’Shea, E., Périgois, C., Perriès, S., Pürrer, M., Rosińska, D., Roy, Santosh, Roy, Soumen, Schönbeck, A., Südbeck, J., Szczepańczyk, M. J., San Martin, E. N. Tapia, Tiwari, Shubhanshu, Tiwari, Srishti, Torres-Forné, A., e Melo, I. Tosta, Töyrä, D., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., van der Schaaf, L., van Heijningen, J. V., Vasúth, M., Viceré, A., von Reis, E. R. G., von Wrangel, J., Weßels, P., Yu, Hang, Yu, Haocun, and Zadrożny, A.

Subjects
gravitational radiation: stochastic, IMPACT, INITIAL MASS FUNCTION, Astronomy, 01 natural sciences, General Relativity and Quantum Cosmology, COMPACT OBJECTS, Gravitational wave detectors, galaxy: redshift: high, BINARIES, Lensing, POPULATION PROPERTIES, LIGO, 010303 astronomy & astrophysics, QC, POPULATION, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/05, Physics, Astrophysical black holes, Gravitational waves, Virgo, BINARY COALESCENCE, COALESCENCE, Physics::Space Physics, Strong gravitational lensing, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy: cluster, Astrophysics - High Energy Astrophysical Phenomena, METALLICITY, Gravitational wave astronomy Gravitational wave source, Gravitational wave, BLACK-HOLE MERGERS, data analysis method, Gravitational lensing, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 1ST, STAR-FORMATION, gravitation: lens, binary: coalescence, 0103 physical sciences, gravitational waves, gravitational-wave astronomy, strong lensing, weak lensing, Weak gravitational lensing, 010308 nuclear & particles physics, gravitational radiation: background, Astronomy and Astrophysics, binary: compact, detector: sensitivity, BAYESIAN-INFERENCE, VIRGO, Space and Planetary Science, gravitational radiation: emission, COSMOLOGY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Abbott, R., et al. (LIGO and Virgo Collaboration), We search for signatures of gravitational lensing in the gravitational-wave signals from compact binary coalescences detected by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) and Advanced Virgo during O3a, the first half of their third observing run. We study: (1) the expected rate of lensing at current detector sensitivity and the implications of a non-observation of strong lensing or a stochastic gravitational-wave background on the merger-rate density at high redshift; (2) how the interpretation of individual high-mass events would change if they were found to be lensed; (3) the possibility of multiple images due to strong lensing by galaxies or galaxy clusters; and (4) possible wave-optics effects due to point-mass microlenses. Several pairs of signals in the multiple-image analysis show similar parameters and, in this sense, are nominally consistent with the strong lensing hypothesis. However, taking into account population priors, selection effects, and the prior odds against lensing, these events do not provide sufficient evidence for lensing. Overall, we find no compelling evidence for lensing in the observed gravitational-wave signals from any of these analyses., This material is based upon work supported by National Science Foundationʼs LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research for the construction and operation of the Virgo detector and the creation and support of the European Gravitational Observatory (EGO) consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India; the Department of Science and Technology, India; the Science & Engineering Research Board (SERB), India; the Ministry of Human Resource Development, India; the Spanish Agencia Estatal de Investigación; the Vicepresidència i Conselleria d’Innovació Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears; the Conselleria d’Innovació Universitats; Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, 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 Î le-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 United States Department of Energy; the Kavli Foundation; and the Gordon and Betty Moore Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provisions of the computational resources.

Published
2021

21. Investigating three Sirius-like systems with SPHERE

Author

H. M. Schmid, Arthur Vigan, T. O. B. Schmidt, Mickael Bonnefoy, M. Keppler, E. Sissa, Markus Kasper, Antonio Garufi, S. Petrus, David Mouillet, E. L. Rickman, Sebastian Daemgen, M. Cudel, Alice Zurlo, J. L. Beuzit, Janis Hagelberg, Raffaele Gratton, Roxanne Ligi, J. Melendez, Anne-Lise Maire, François Ménard, Tomas Stolker, D. Gasparri, F. Rigal, Daniel Rouan, C. Soenke, E. Cascone, Matthias Samland, Silvano Desidera, R. Galicher, Christian Ginski, Gael Chauvin, Valentina D'Orazi, M. R. Mayer, A. Potier, A-M. Lagrange, Graeme Salter, Francois Wildi, H. Le Coroller, Maud Langlois, T. A. Pacheco, Henning Avenhaus, C. Desgrange, Beth Biller, C. Lazzoni, Mariangela Bonavita, Wolfgang Brandner, Markus Janson, Markus Feldt, S. Mazevet, N. Engler, Julien Girard, C. Perrot, Dino Mesa, J. Lannier, C. Fontanive, S. Hunziker, T. Moulin, S. Peretti, Joany Andreina Manjarres Ramos, M. Lombart, Riccardo Claudi, Philippe Delorme, A. Boccaletti, University of Arizona, 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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Stockholm University, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Max Planck Institute for Radio Astronomy, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, European Southern Observatory (ESO), Universidad de Chile = University of Chile [Santiago] (UCHILE), University of Edinburgh, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Chaire IPAG 'Entreprise Inclusive' (IPAG Business School), IPAG Business School, Observatoire de Paris, Université Paris sciences et lettres (PSL), Department of Biochemistry and Molecular Biology, Mayo Clinic, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Low Energy Astrophysics (API, FNWI), 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), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Angular momentum, 530 Physics, Sirius, CD-56 7708, HD 114174, FOS: Physical sciences, Individual, Astrophysics, 01 natural sciences, Nucleosynthesis, 0103 physical sciences, Asymptotic giant branch, Solar and Stellar Astrophysics, Abundances, General, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, 520 Astronomy, Binaries, White dwarf, Astronomy and Astrophysics, HD 2133, Stars, White Dwarfs, Orbit, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Sirius-like systems are wide binaries composed of a white dwarf (WD) and a companion of a spectral type earlier than M0. The WD progenitor evolves in isolation, but its wind during the AGB phase pollutes the companion surface and transfers some angular momentum. Within SHINE survey that uses SPHERE at the VLT, we acquired images of HD2133, HD114174, and CD-567708 and combined this data with high resolution spectra of the primaries, TESS, and literature data. We performed accurate abundance analyses for the MS. We found brighter J and K magnitudes for HD114174B than obtained previously and extended the photometry down to 0.95 micron. Our new data indicate a higher temperature and then shorter cooling age (5.57+/-0.02 Gyr) and larger mass (0.75+/-0.03 Mo) for this WD than previously assumed. This solved the discrepancy previously found with the age of the MS star. The two other WDs are less massive, indicating progenitors of ~1.3 Mo and 1.5-1.8 Mo for HD2133B and CD-56 7708B, respectively. We were able to derive constraints on the orbit for HD114174 and CD-56 7708. The composition of the MS stars agrees fairly well with expectations from pollution by the AGB progenitors of the WDs: HD2133A has a small enrichment of n-capture elements, which is as expected for pollution by an AGB star with a mass 3.0 Mo. On the other hand, none of these stars show the excesses of C that are expected to go along with those of n-capture elements. This might be related to the fact that these stars are at the edges of the mass range where we expect nucleosynthesis related to thermal pulses., Accepted on Astronomy and Astrophysics. 19 pages, 15 figures

Published
2021

22. Effects of radiative losses on the relativistic jets of high-mass microquasars

Author

Alexandre Marcowith, Rolf Walder, Jean M. Favre, Mark E Dieckmann, Doris Folini, A. Charlet, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)

Subjects
Radiative cooling, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, methods: numerical, X-rays: binaries, Astronomi, astrofysik och kosmologi, Astrophysical jet, 0103 physical sciences, Radiative transfer, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Jet (fluid), 010308 nuclear & particles physics, Astronomy and Astrophysics, Observable, Plasma, radiation mechanisms: thermal, ISM: jets and outflows, Space and Planetary Science, hydrodynamics, X-rays, binaries, methods, numerical, radiation mechanisms, thermal, ISM, jets and outflows, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Relativistic quantum chemistry
Abstract

Context. Relativistic jets are ubiquitous in astrophysics. High Mass Microquasars (HMMQs) are useful labs to study such jets, as they are relatively close and evolve over observable time scales. The ambient medium into which the jet propagates is, however, far from homogeneous. Corresponding simulation studies to date consider various forms of a wind-shaped ambient medium but typically neglect radiative cooling and relativistic effects. Aims. We investigate the dynamical and structural effects of radiative losses and system parameters on relativistic jets in HMMQs, from the jet launch to its propagation over several tens of orbital separations. Methods. We use 3D relativistic hydrodynamical simulations including parameterized radiative cooling derived from relativistic thermal plasma distribution to carry out parameter studies around two fiducial cases inspired by Cygnus X-1 and Cygnus X-3. Results. Radiative losses are found to be more relevant in Cygnus X-3 than Cygnus X-1. Varying jet power, jet temperature, or the wind of the donor star tends to have a larger impact at early times, when the jet forms and instabilities initially develop, than at later times when the jet has reached a turbulent state. Conclusions. Radiative losses may be dynamically and structurally relevant at least in Cygnus X-3 case, and thus should be examined in more detail., Comment: 28 pages, 25 figures, 8 tables. Accepted for publication in A&A

Published
2022

23. Globular Clusters and Neutron Star Binaries.

Author

D'Antona, Francesca

Subjects
*GLOBULAR clusters, *STAR clusters, *NEUTRON stars, *STELLAR dynamics, *BINARY stars, *STARS, *PHYSICS
Abstract

I summarize some aspects of the research at OAR on the neutron star population in Globular clusters. In particular I discuss the evolutionary stage of the interacting millisecond pulsar binary PSR J1740-5340 in the cluster NGC 6397 and point out that the donor component can not be a recently acquired low mass star. The precise mass derived for this star helps to constrain the loss of angular momentum during the radio-ejection phase which this system is traversing. I then discuss the problem of the large number of neutron stars present in globular clusters and show that it might be due to an atypical initial mass function, which is necessary to understand the chemical anomalies shown by the low mass stars evolving today. © 2005 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2005
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24. Two Directly Imaged, Wide-orbit Giant Planets around the Young, Solar Analog TYC 8998-760-1

Author

Alexander J. Bohn, Jozua de Boer, Mark J. Pecaut, Christian Ginski, Steven Rieder, Tiffany Meshkat, Matthew A. Kenworthy, Frans Snik, Eric E. Mamajek, Christoph U. Keller, John Southworth, Maddalena Reggiani, and Low Energy Astrophysics (API, FNWI)

Subjects
Extrasolar gas giants, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Q1, T-DWARFS, 1ST, 01 natural sciences, BINARIES, Primary (astronomy), Planet, COMPANION, 0103 physical sciences, Exoplanet detection methods, RESOLVED SPECTROSCOPY, PHOTOMETRY, Astrophysics::Solar and Stellar Astrophysics, Direct imaging, Circular orbit, 010303 astronomy & astrophysics, Stellar evolution, QB600, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Science & Technology, DWARF SPECTROSCOPIC SURVEY, Solar analog, Exoplanets, Astronomy, Astronomy and Astrophysics, Mass ratio, Exoplanet, Galaxy, 2MASS, BROWN DWARF, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, DISCOVERY, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Even though tens of directly imaged companions have been discovered in the past decades, the number of directly confirmed multiplanet systems is still small. Dynamical analysis of these systems imposes important constraints on formation mechanisms of these wide-orbit companions. As part of the Young Suns Exoplanet Survey (YSES) we report the detection of a second planetary-mass companion around the 17 Myr-old, solar-type star TYC 8998-760-1 that is located in the Lower Centaurus Crux subgroup of the Scorpius-Centaurus association. The companion has a projected physical separation of 320 au and several individual photometric measurements from 1.1 to 3.8 microns constrain a companion mass of $6\pm1\,M_\mathrm{Jup}$, which is equivalent to a mass ratio of $q=0.57\pm0.10\%$ with respect to the primary. With the previously detected $14\pm3\,M_\mathrm{Jup}$ companion that is orbiting the primary at 160 au, TYC 8998-760-1 is the first directly imaged multiplanet system that is detected around a young, solar analog. We show that circular orbits are stable, but that mildly eccentric orbits for either/both components ($e > 0.1$) are chaotic on Gyr timescales, implying in-situ formation or a very specific ejection by an unseen third companion. Due to the wide separations of the companions TYC 8998-760-1 is an excellent system for spectroscopic and photometric follow-up with space-based observatories such as the James Webb Space Telescope., Accepted for publication in ApJL (12 pages, 8 figures, 2 tables)

Published
2020

25. Maximum likelihood map-making with the Laser Interferometer Space Antenna

Author

Carlo R. Contaldi, Mauro Pieroni, Nikos Karnesis, Angelo Ricciardone, Arianna I. Renzini, Giulia Cusin, Marco Peloso, Gianmassimo Tasinato, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Science and Technology Facilities Council (STFC)

Subjects
noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Maximum likelihood, satellite, FOS: Physical sciences, anisotropy, Astronomy & Astrophysics, 01 natural sciences, frequency: high, Physics, Particles & Fields, BINARIES, Optics, 0201 Astronomical and Space Sciences, 0103 physical sciences, Range (statistics), ANISOTROPIES, Sensitivity (control systems), 010306 general physics, Anisotropy, 0206 Quantum Physics, media_common, Physics, LISA, Science & Technology, 010308 nuclear & particles physics, business.industry, gravitational radiation: background, Astrophysics::Instrumentation and Methods for Astrophysics, Laser interferometer space antenna, sensitivity, Nuclear & Particles Physics, Cosmology, Sky, Physical Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, astro-ph.CO, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Intensity (heat transfer), Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Given the recent advances in gravitational-wave detection technologies, the detection and characterisation of gravitational-wave backgrounds (GWBs) with the Laser Interferometer Space Antenna (LISA) is a real possibility. To assess the abilities of the LISA satellite network to reconstruct anisotropies of different angular scales and in different directions on the sky, we develop a map-maker based on an optimal quadratic estimator. The resulting maps are maximum likelihood representations of the GWB intensity on the sky integrated over a broad range of frequencies. We test the algorithm by reconstructing known input maps with different input distributions and over different frequency ranges. We find that, in an optimal scenario of well understood noise and high frequency, high SNR signals, the maximum scales LISA may probe are $\ell_{\rm max} \lesssim 15$. The map-maker also allows to test the directional dependence of LISA noise, providing insight on the directional sky sensitivity we may expect., Corresponding author: Arianna I. Renzini, as a part of their PhD thesis. 13 pages, 9 figures

Published
2020

26. Spectroscopic patch model for massive stars using PHOEBE II and FASTWIND star

Author

Hugues Sana, Angela Kochoska, Jon O. Sundqvist, Andrej Prša, Michael Abdul-Masih, Joachim Puls, and Kyle E. Conroy

Subjects
stars, CONTACT, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, spectroscopic, 01 natural sciences, Computer Science::Digital Libraries, rotation, Spectral line, Spherical geometry, massive, ECLIPSING BINARIES, SYSTEMS, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, SPECTRA, PRESUPERNOVA EVOLUTION, close, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Physics, Science & Technology, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Radius, Surface gravity, CLOSE BINARIES, Physics::History of Physics, eclipsing, Radial velocity, Stars, LIGHT, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physical Sciences, ATMOSPHERES, binaries, techniques
Abstract

Massive stars play an important role in the mechanical and chemical evolution of galaxies. Understanding the internal processes of these stars is vital to our understanding of their evolution and eventual end products. Deformations from spherical geometry are common for massive stars; however, the tools that are currently available for the study of these systems are almost exclusively one-dimensional. We present a new spectroscopic analysis tool tailored for massive stars that deviate from spherical symmetry. This code (entitled SPAMMS) is a spectroscopic patch model that takes the three-dimensional surface geometry of the system into account to produce spectral profiles at given phases and orientations. In using the Wilson-Devinney-like code PHOEBE in combination with the non local thermodynamic equilibrium (NLTE) radiative transfer code FASTWIND, we created a three-dimensional mesh that represents the surface geometry of our system and we assigned FASTWIND emergent intensity line profiles to each mesh triangle, which take the local parameters such as temperature, surface gravity, and radius into account. These line profiles were then integrated across the visible surface, where their flux contribution and radial velocity are taken into account, thus returning a final line profile for the visible surface of the system at a given phase. We demonstrate that SPAMMS can accurately reproduce the morphology of observed spectral line profiles for overcontact systems. Additionally, we show how line profiles of rapidly-rotating single stars differ when taking rotational distortion into account, and the effects that these can have on the determined parameters. Finally, we demonstrate the code's ability to reproduce the Rossiter-Mclaughlin and Struve-Sahade effects., 10 pages, 10 figures, accepted for publication in A&A

Published
2020

27. Have hierarchical three-body mergers been detected by LIGO/Virgo?

Author

Andrew G. Sullivan, Doğa Veske, Johan Samsing, Imre Bartos, Zsuzsa Márka, Szabolcs Marka, and K. Rainer Corley

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, BINARIES, General Relativity and Quantum Cosmology, Binary black hole, Frequentist inference, Time windows, GLOBULAR-CLUSTERS, 0103 physical sciences, LIGO, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Observable, CATALOG, EVOLUTION, Black hole, ) black hole mergers [(transients], gravitational waves, Space and Planetary Science, TESTS, Astrophysics - High Energy Astrophysical Phenomena, Merge (version control), BLACK-HOLE MERGERS
Abstract

One of the proposed channels of binary black hole mergers involves dynamical interactions of three black holes. In such scenarios, it is possible that all three black holes merge in a so-called hierarchical merger chain, where two of the black holes merge first and then their remnant subsequently merges with the remaining single black hole. Depending on the dynamical environment, it is possible that both mergers will appear within the observable time window. Here we perform a search for such merger pairs in the public available LIGO and Virgo data from the O1/O2 runs. Using a frequentist p-value assignment statistics we do not find any significant merger pair candidates, the most significant being GW170809-GW151012 pair. Assuming no observed candidates in O3/O4, we derive upper limits on merger pairs to be $\sim11-110\ {\rm year^{-1}Gpc^{-3}}$, corresponding to a rate that relative to the total merger rate is $\sim 0.1-1.0$. From this we argue that both a detection and a non-detection within the next few years can be used to put useful constraints on some dynamical progenitor models., 7 pages, 4 figures

Published
2020

28. Impact of a companion and of chromospheric emission on the shape of chromosome maps for globular clusters

Author

Corinne Charbonnel, W. Chantereau, Fabrice Martins, Carmela Lardo, Julien Morin, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), University of Geneva, Liverpool John Moores University, Martins F., Morin J., Charbonnel C., Lardo C., and Chantereau W.

Subjects
catalog, stars: chromospheres, Population, main-sequence, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, multiple stellar populations, globular clusters: general, 01 natural sciences, Spectral line, Photometry (optics), evolution, 0103 physical sciences, origin, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, supermassive stars, abundance patterns, Astronomy and Astrophysics, Observable, Astrophysics - Astrophysics of Galaxies, Stars, binaries: general, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Globular cluster, uv legacy survey, Astrophysics::Earth and Planetary Astrophysics, outer-halo, binaries
Abstract

We investigate the role of binaries and chromospheric emission on HST photometry of globular clusters' stars. We quantify their respective effects on the position of stars in the chromosome map, especially among the first population. We computed atmosphere models and synthetic spectra for stars of different chemical compositions, based on isochrones produced by stellar evolution calculations with abundance variations representative of first and second populations in GCs. From this we built synthetic chromosome maps for a mixture of stars of different chemical compositions. We subsequently replaced a fraction of stars with binaries, or stars with chromospheric emission, using synthetic spectroscopy. We studied how the position of stars is affected in the chromosome map. Binaries can, in principle, explain the extension of the first population in the chromosome map. However, we find that given the binary fraction reported for GCs, the density of stars in the extended part is too small. Another difficulty of the binary explanation is that the shape of the distribution of the first population in the chromosome map is different in clusters with similar binary fractions. Additionally, we find that the contribution of chromospheric emission lines to the HST photometry is too small to have an observable impact on the shape of the chromosome map. Continuum chromospheric emission has an effect qualitatively similar to binaries. We conclude that binaries do have an impact on the morphology of the chromosome map of GCs, but they are unlikely to explain entirely the shape of the extended distribution of the first population stars. Uncertainties in the properties of continuum chromospheric emission of stars in GCs prevent any quantitative conclusion. Therefore, the origin of the extended first population remains unexplained., 11 pages, 10 figures. Accepted in Astronomy & Astrophysics

Published
2020

29. MSTAR -- a fast parallelised algorithmically regularised integrator with minimum spanning tree coordinates

Author

Antti Rantala, Pauli Pihajoki, Matias Mannerkoski, Peter H. Johansson, Thorsten Naab, Particle Physics and Astrophysics, and Department of Physics

Subjects
GALACTIC NUCLEI, Extrapolation, CODE, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Minimum spanning tree, Space (mathematics), 01 natural sciences, methods: numerical, Tree (descriptive set theory), BINARIES, SUPERMASSIVE BLACK-HOLES, SYSTEMS, 020204 information systems, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, IMPLEMENTATION, SPACE, 010303 astronomy & astrophysics, Scaling, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Discrete mathematics, Particle system, Physics, quasars: supermassive black holes, GALAXY MERGERS, Astronomy and Astrophysics, 115 Astronomy, Space science, PERTURBATIONS, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Space and Planetary Science, gravitation, Astrophysics of Galaxies (astro-ph.GA), galaxies: star clusters: general, Astrophysics::Earth and Planetary Astrophysics, Multipole expansion, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the novel algorithmically regularised integration method MSTAR for high accuracy ($|\Delta E/E| \gtrsim 10^{-14}$) integrations of N-body systems using minimum spanning tree coordinates. The two-fold parallelisation of the $\mathcal{O}(N_\mathrm{part}^2)$ force loops and the substep divisions of the extrapolation method allows for a parallel scaling up to $N_\mathrm{CPU} = 0.2 \times N_\mathrm{part}$. The efficient parallel scaling of MSTAR makes the accurate integration of much larger particle numbers possible compared to the traditional algorithmic regularisation chain (AR-CHAIN) methods, e.g. $N_\mathrm{part} = 5000$ particles on $400$ CPUs for $1$ Gyr in a few weeks of wall-clock time. We present applications of MSTAR on few particle systems, studying the Kozai mechanism and N-body systems like star clusters with up to $N_\mathrm{part} =10^4$ particles. Combined with a tree or a fast multipole based integrator the high performance of MSTAR removes a major computational bottleneck in simulations with regularised subsystems. It will enable the next generation galactic-scale simulations with up to $10^9$ stellar particles (e.g. $m_\star = 100 M_\odot$ for a $M_\star = 10^{11} M_\odot$ galaxy) including accurate collisional dynamics in the vicinity of nuclear supermassive black holes., Comment: 20 pages, 16 figures, accepted for publication in MNRAS

Published
2020

30. Full orbital solution for the binary system in the northern Galactic disk microlensing event Gaia16aye

Author

Wyrzykowski, Ł., D’Ago, G., Hanlon, L., van Heerden, H., Ihanec, N., Jovanovic, M., Kopacki, G., Martin-Carrillo, A., Marais, J., Meintjes, P., Murphy, D., Van Soelen, B., Strubble, E., Szegedi, H., Vernet, D., Vince, O., van der Westhuizen, I., Wium, D., Zhuchkov, R. Ya., Wyrzykowski, Łukasz, Mróz, P., Rybicki, K., Gromadzki, M., Kołaczkowski, Z., Zieliński, M., Zieliński, P., Britavskiy, N., Gomboc, A., Sokolovsky, K., Hodgkin, S., Abe, L., Aldi, G., AlMannaei, A., Altavilla, G., Al Qasim, A., Anupama, G., Awiphan, S., Bachelet, E., Bakış, V., Baker, S., Bartlett, S., Bendjoya, P., Benson, K., Bikmaev, I., Birenbaum, G., Blagorodnova, N., Blanco-Cuaresma, S., Boeva, S., Bonanos, A., Bozza, V., Bramich, D., Bruni, I., Burenin, R., Burgaz, U., Butterley, T., Caines, H., Caton, D., Calchi Novati, S., Carrasco, J., Cassan, A., Čepas, V., Cropper, M., Chruślińska, M., Clementini, G., Clerici, A., Conti, D., Conti, M., Cross, S., Cusano, F., Damljanovic, G., Dapergolas, A., D'ago, G, de Bruijne, J., Dennefeld, M., Dhillon, V., Dominik, M., Dziedzic, J., Erece, O., Eselevich, M., Esenoglu, H., Eyer, L., Figuera Jaimes, R., Fossey, S., Galeev, A., Grebenev, S., Gupta, A., Gutaev, A., Hallakoun, N., Hamanowicz, A., Han, C., Handzlik, B., Haislip, J., Hardy, L., Harrison, D., Hoette, V., Horne, K., Hudec, R., Hundertmark, M., Ihanec 35, N, Irtuganov, E., Itoh, R., Iwanek, P., Janulis, R., Jelínek, M., Jensen, E., Kaczmarek, Z., Katz, D., Khamitov, I., Kilic, Y., Klencki, J., Kolb, U., Kouprianov, V., Kruszyńska, K., Kurowski, S., Latev, G., Lee, C.-H., Leonini, S., Leto, G., Lewis, F., Li, Z., Liakos, A., Littlefair, S., Lu, J., Manser, C., Mao, S., Maoz, D., Maskoliūnas, M., Maund, J., Melnikov, S., Ment, K., Mikołajczyk, P., Morrell, M., Mowlavi, N., Moździerski, D., Nazarov, S., Netzel, H., Nesci, R., Ngeow, C.-C., Norton, A., Ofek, E., Pakštienė, E., Palaversa, L., Pandey, A., Paraskeva, E., PAWLAK, M., Penny, M., Penprase, B., Piascik, A., Prieto, J., Qvam, J., Ranc, C., Rebassa-Mansergas, A., Reichart, D., Reig, P., Rhodes, L., Rivet, J.-P., Rixon, G., Roberts, D., Rosi, P., Russell, D., Zanmar Sanchez, R., Scarpetta, G., Seabroke, G., Shappee, B., Schmidt, R., Shvartzvald, Y., Sitek, M., Skowron, J., Śniegowska, M., Snodgrass, C., Soares, P., Spetsieri, Z., Stankevičiūtė, A., Steele, I., Street, R., Strobl, J., Tinjaca Ramirez, L., Tomasella, L., Tsapras, Y., Villanueva, S., 56, O, Wambsganss, J., Wiersema, K., Wilson, R., Yoldas, A., Ya, R, Zhukov, D., Zdanavičius, J., Zoła, S., Zubareva, A., Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Instytut Astronomiczny Uniwersytetu Wrocławskiego, Instituto de Astrofìsica de Canarias, National Science Centre (Poland), European Commission, Ministry of Science and Higher Education (Poland), Science and Technology Facilities Council (UK), Foundation for Polish Science, Slovenian Research Agency, University of Crete, Foundation for Research and Technology, National Research Foundation of Korea, University of Leicester, European Space Agency, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Universidad de Barcelona, Agenzia Spaziale Italiana, Royal Society (UK), Ministry of Science and Technology (Taiwan), The Ohio State University, Chinese Academy of Sciences, Villum Fonden, Research Council of Lithuania, Kazan Federal University, National Aeronautics and Space Administration (US), Ministry of Education, Science and Technological Development (Serbia), W. M. Keck Foundation, Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), School of Physics, University College Dublin, Ireland, University of Pretoria [South Africa], Clinical Center of Serbia (KCS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, and Ege Üniversitesi

Subjects
Astronomy, Estels binaris, gravitational lensing: micro, techniques: photometric, binaries: general, stars: individual: Gaia16aye-L, Astrophysics, 01 natural sciences, 7. Clean energy, Gaia16aye-L, Gravitational lenses, Bulge, Fotometria astronòmica, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, QB, Physics, Gravitational lensing micro, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomical photometry, 3rd-DAS, Orbital period, Radial velocity, Orbit, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Stars: individual: Gaia16aye-L, astro-ph.SR, individual: Gaia16aye [Stars], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Gravitational lensing: micro, micro [Gravitational lensing], Double stars, 0103 physical sciences, Binaries: general, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Orbital elements, general [Binaries], photometric [Techniques], Binaries, Astronomy and Astrophysics, Light curve, Stars, QC Physics, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Techniques - photometric, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Techniques: photometric, astro-ph.IM
Abstract

Gaia16aye was a binary microlensing event discovered in the direction towards the northern Galactic disc and was one of the first microlensing events detected and alerted to by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to I = 12 mag, and it was covered in great detail with almost 25 000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution. We employed a full Keplerian binary orbit microlensing model combined with the motion of Earth and Gaia around the Sun to reproduce the complex light curve. The photometric data allowed us to solve the microlensing event entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first-ever microlensing space-parallax between the Earth and Gaia located at L2. The properties of the binary system were derived from microlensing parameters, and we found that the system is composed of two main-sequence stars with masses 0.57 +/- 0.05 M-circle dot and 0.36 +/- 0.03 M-circle dot at 780 pc, with an orbital period of 2.88 years and an eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve for the binary system. Events such as Gaia16aye indicate the potential for the microlensing method of probing the mass function of dark objects, including black holes, in directions other than that of the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations that can be made with a network of heterogeneous telescopes., Polish National Sci-ence Centre (NCN): HARMONIA NCN grant [2015/18/M/ST9/00544]; Polish National Sci-ence Centre (NCN): OPUS NCN grant [2015/17/B/ST9/03167]; Polish National Sci-ence Centre (NCN): DAINA NCN grant [2017/27/L/ST9/03221]; European CommissionEuropean CommissionEuropean Commission Joint Research Centre [312430, 730890]; Polish Ministry of Higher EducationMinistry of Science and Higher Education, Poland [3040/7.PR/2014/2, DIR/WK/2018/12]; MAESTRO NCN grant [2014/14/A/ST9/00121]; DDT programmes [SW2016b12, A34DDT3]; UK Science and Technology Facilities CouncilUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC); Foundation for Polish Science (Program START); National Science Center, PolandNational Science Centre, Poland [ETIUDA 2018/28/T/ST9/00096]; Slovenian Research AgencySlovenian Research Agency - Slovenia [P1-0031, J1-8136]; COST Action GWverseEuropean Cooperation in Science and Technology (COST) [CA16104]; National Research Foundation of KoreaNational Research Foundation of Korea [2017R1A4A1015178]; STFCUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC); European Space Agency under the NELIOTA program [4000112943]; GROWTH project - National Science Foundation [1545949]; MINECO (Spanish Ministry of Economy) [ESP2016-80079-C2-1-R, ESP2014-55996-C2-1-R, RTI2018-095076B-C21]; ICCUB (Unidad de Excelencia a Maria de Maeztu) [MDM-2014-0369]; Agenzia Spaziale Italiana (ASI)Agenzia Spaziale Italiana (ASI) [ASI I/058/10/0, ASI 2014-025-R.1.2015]; Royal Society Research GrantRoyal Society of London [RG170230]; Ministry of Science and Technology (Taiwan)Ministry of Science and Technology, Taiwan [104-2112-M-008-012MY3, 104-2923-M-008-004-MY5]; European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant [320964]; Gordon and Betty Moore FoundationGordon and Betty Moore Foundation [GBMF5490]; NSFNational Science Foundation (NSF) [AST-1515927, AST-0908816, AST-1412587]; Mt. Cuba Astronomical Foundation; Center for Cosmology and AstroParticle Physics at the Ohio State UniversityOhio State University; Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA); Villum Foundation; MINECO under the Ramon y Cajal programme [RYC-2016-20254]; MINECO [AYA2017-86274-P]; AGAUR grantAgencia de Gestio D'Ajuts Universitaris de Recerca Agaur (AGAUR) [SGR-661/2017]; Science and Technology Facilities CouncilUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC) [ST/P000541/1]; STFC consolidated grant [ST/M001296/1]; Research Council of LithuaniaResearch Council of Lithuania (LMTLT) [S-LL-19-2]; TUB.ITAKTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK); IKI; KFU; AST; National Science Fund (Bulgaria)National Science Fund of Bulgaria [DN 18/13-12.12.2017]; Institute of Astronomy via research project "Study of ICRF radio-sources and fast variable astronomical objects"; NAO Rozhen, BAS, via research project "Study of ICRF radio-sources and fast variable astronomical objects"; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011, 176004, 176021]; DFGGerman Research Foundation (DFG)European Commission [SPP 1992, WA 1074/11-1]; NCN [2016/21/B/ST9/01126]; MINECO Ramon y Cajal programme [AYA2017-86274-P, RYJ-2016-20254]; Robert Martin Ayers Sciences Fund; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA) [NNX08AR22G]; National Science FoundationNational Science Foundation (NSF) [AST-1238877]; W. M. Keck FoundationW.M. Keck Foundation; ICCUB (Unidad de Excelencia 'Maria de Maeztu') [MDM-2014-0369]; [3.6714.2017/8.9], This work relies on the results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia Multi-Lateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia.In particular we acknowledge Gaia Photomet-ric Science Alerts Team, website http://gsaweb.ast.cam.ac.uk/alerts.We thank the members of the OGLE team for discussions and support. We also would like to thank the Polish Children Fund (KFnRD) for support of an internship of their pupils in Ostrowik Observatory of the Warsaw Univ-ersity, during which some of the data were collected, in particular we thank: Robert Nowicki, Michal Por.ebski and Karol Niczyj. The work presented here has been supported by the following grants from the Polish National Sci-ence Centre (NCN): HARMONIA NCN grant 2015/18/M/ST9/00544, OPUS NCN grant 2015/17/B/ST9/03167, DAINA NCN grant 2017/27/L/ST9/03221, as well as European Commission's FP7 and H2020 OPTICON grants (312430 and 730890), Polish Ministry of Higher Education support for OPTICON FP7, 3040/7.PR/2014/2, MNiSW grant DIR/WK/2018/12. PMr and JS acknowledge support from MAESTRO NCN grant 2014/14/A/ST9/00121 to Andrzej Udal-ski. We would like to thank the following members of the AAVSO for their amazing work with collecting vast amounts of data: Teofilo Arranz, James Boardman, Stephen Brincat, Geoff Chaplin, Emery Erdelyi, Rafael Farfan, William Goff, Franklin Guenther, Kevin Hills, Jens Jacobsen, Raymond Kneip, David Lane, Fernando Limon Martinez, Gianpiero Locatelli, Andrea Mantero, Attila Madai, Peter Meadows, Otmar Nickel, Arto Oksanen, Luis Perez, Roger Pieri, Ulisse Quadri, Diego Rodriguez Perez, Frank Schorr, George Sjoberg, Andras Timar, Ray Tomlin, Tonny Vanmunster, Klaus Wenzel, Thomas Wikander. We also thank the amateur observers from around the world, in particular, Pietro Capuozzo, Leone Trascianelli, Igor Zharkov from Ardingly College and Angelo Tomassini, Karl-Ludwig Bath. We also thank Roger Pickard from the British Astronomical Association and Matthias Penselin from the German Haus der Astronomie association for their contributions. KS thanks Dr. Dmitry Chulkov and Dr. Panagiotis Gavras for the interesting discussion of stellar multiplicity. We acknowledge support of DDT programmes SW2016b12 (WHT) and A34DDT3 (TNG). The INT, TNG and WHT are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. SJF would like to thank the UCL students who assisted with the collection and checking of UCLO data for the observing campaign: Martina Aghopian, Ashleigh Arendt, Artem Barinov, Luke Barrett, Jasper Berry-Gair, Arjun Bhogal, Charles Bowesman, William Boyd, Andrei Cuceu, Michael Davies, Max Freedman, Gabriel Fu, Abirami Govindaraju, Iandeep Hothi, Clara Matthews Torres, Darius Modirrousta-Galian, Petru Neague, George Pattinson, Xiaoxi Song, and Brian Yu. P.Mr. acknowledges support from the Foundation for Polish Science (Program START) and the National Science Center, Poland (grant ETIUDA 2018/28/T/ST9/00096).; r r AC, AG and NI acknowledge the financial support from the Slovenian Research Agency (research core funding No. P1-0031 and project grant No. J1-8136)and networking support by the COST Action GWverse CA16104. Skinakas Observatory is a collaborative project of the University of Crete and the Foundation for Research and Technology-Hellas. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. KW acknowledges funding from STFC, and thanks the University of Lei-cester for the investment in instrumentation. We gratefully acknowledge financial support by the European Space Agency under the NELIOTA program, contract No. 4000112943. This work has made use of data obtained with the Kryoneri Prime Focus Instrument, developed by the European Space Agency NELIOTA project on the 1.2 m Kryoneri telescope, which is operated by IAASARS, National Observatory of Athens, Greece. The Aristarchos tele-scope is operated on Helmos Observatory by the IAASARS of the National Observatory of Athens. This work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. This work was supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R (MINECO/FEDER, UE) and ESP2014-55996-C2-1-R (MINECO/FEDER, UE) and MDM-2014-0369 of ICCUB (Unidad de Excelencia a Maria de Maeztu). This work was supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R and RTI2018-095076B-C21 (MINECO/FEDER, UE), and MDM-2014-0369 of ICCUB (Unidad de Excelencia 'Maria de Maeztu'). The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and is operated by the Institute for Space Studies of Catalonia (IEEC). Support to this study has been provided by Agenzia Spaziale Italiana (ASI) through grants ASI I/058/10/0 and ASI 2014-025-R.1.2015. KW thanks Dipali Thanki and Ray McErlean for their technical support of the scientific programme of the University of Leicester observatory. This work was supported by Royal Society Research Grant RG170230. CCN thanks the funding from Ministry of Science and Technology (Taiwan) under the contracts 104-2112-M-008-012MY3 and 104-2923-M-008-004-MY5. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WDTracer). We thank the Las Cumbres Observatory and its sta ff for its continuing support of the project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University and NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), the Villum Foundation, and George Skestos. ARM acknowledges support from the MINECO under the Ramon y Cajal programme (RYC-2016-20254) and the AYA2017-86274-P grant, and the AGAUR grant SGR-661/2017. We acknowledge support from the Science and Technology Facilities Council (TB and RWW; ST/P000541/1). K.Horne acknowledges support from STFC consolidated grant ST/M001296/1. This work was partly supported by the Research Council of Lithuania, grant No. S-LL-19-2 Authors thank to TUB.ITAK, IKI, KFU, and AST for partial supports in using RTT150 (Russian-Turkish 1.5-m telescope in Antalya).; r r This work was partially funded by the subsidy 3.6714.2017/8.9 allocated to Kazan Federal University for the state assignment in the sphere of scientific activities. This research was partially supported by contract DN 18/13-12.12.2017 with the National Science Fund (Bulgaria). Work by YS was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Uni-versities Space Research Associ-ation through a contract with NASA. GD gratefully acknowledges the obser-ving grant support from the Institute of Astronomy and NAO Rozhen, BAS, via bilateral joint research project "Study of ICRF radio-sources and fast variable astronomical objects" (PI:G.Damljanovic). This work is a part of the Projects no. 176011 "Dynamics and kinematics of celestial bodies and systems", no. 176004 "Stellar physics" and no. 176021 "Visible and invisible matter in nearby galaxies: theory and observations" supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia. YT acknowledges the support of DFG priority program SPP 1992 "Exploring the diversity of Extrasolar Planets" (WA 1074/11-1). This work of PMi, DM and ZK was supported by the NCN grant no. 2016/21/B/ST9/01126. ARM acknowledges support from the MINECO Ramon y Cajal programme RYJ-2016-20254 and grant AYA2017-86274-P and from the AGAUR grant SGR-661/2017. The work by C. R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA. The Faulkes Telescope Project is an education partner of Las Cumbres Observatory (LCO). The Faulkes Telescopes are maintained and operated by LCO. This research was made possible through the use of the AAVSO Photomet-ric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund and NSF AST-1412587. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project O ffice, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incor-porated, the National Central University of Taiwan, the Space Telescope Sci-ence Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Ins-titute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

Published
2020

31. The Milky Way's bar structural properties from gravitational waves

Author

Martijn J. C. Wilhelm, Elena D'Onghia, Elena M. Rossi, and Valeriya Korol

Subjects
Fundamental Parameters, Milky Way, Population, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Bulge, education, Astrophysics::Galaxy Astrophysics, Physics, Gravitational Waves, education.field_of_study, Spiral galaxy, Gravitational wave, Binaries, White dwarf, Structure, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, White Dwarfs, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Close
Abstract

The Laser Interferometer Space Antenna (LISA) will enable Galactic gravitational wave (GW) astronomy by individually resolving $ > 10^4$ signals from double white dwarf (DWD) binaries throughout the Milky Way. In this work we assess for the first time the potential of LISA data to map the Galactic stellar bar and spiral arms, since GWs are unaffected by stellar crowding and dust extinction unlike optical observations of the bulge region. To achieve this goal we combine a realistic population of Galactic DWDs with a high-resolution N-Body simulation a galaxy in good agreement with the Milky Way. We then model GW signals from our synthetic DWD population and reconstruct the structure of the simulated Galaxy from mock LISA observations. Our results show that while the low signal contrast between the background disc and the spiral arms hampers our ability to characterise the spiral structure, the stellar bar will instead clearly appear in the GW map of the bulge. The bar length and bar width derived from these synthetic observations are underestimated, respectively within $1\sigma$ and at a level greater than $2\sigma$, but the resulting axis ratio agrees to well within $1\sigma$, while the viewing angle is recovered to within one degree. These are competitive constraints compared to those from electromagnetic tracers, and they are obtained with a completely independent method. We therefore foresee that the synergistic use of GWs and electromagnetic tracers will be a powerful strategy to map the bar and the bulge of the Milky Way., Comment: Accepted by MNRAS, 14 pages, 11 figures, 1 table

Published
2020
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32. Binaries as precious tools for stellar evolution and asteroseismology

Author

Maceroni, Carla

Subjects
stars, Physics, Multidisciplinary, Astronomy, spectroscopic, Asteroseismology, spectroscopie, eclipsing, interiors, Stars, evolution, binaires éclipsantes, Astrophysics::Solar and Stellar Astrophysics, pulsation, Astrophysics::Earth and Planetary Astrophysics, évolution, binaries, intérieurs, Stellar evolution, Astrophysics::Galaxy Astrophysics
Abstract

Eclipsing double-lined binaries had a fundamental role in laying the foundations of stellar astro-physics and are still today an invaluable tool, as they provide an independent, purely geometrical, and accurate determination of the stellar masses and radii (often with uncertainties lower than 1%). This paper briefly reviews some important contributions to the field of stellar structure and to the more recent one of asteroseismology.

Published
2020
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33. VERITAS Detection of LS 5039 and HESS J1825-137

Author

Olivier Hervet, Dirk Pandel, Marita Krause, John L. Quinn, G. Hughes, P. T. Reynolds, Ralph Bird, Tarek M. Hassan, David Kieda, Jodi Christiansen, P. Wilcox, D. S. Hanna, K. Ragan, Wystan Benbow, I. Sadeh, A. Weinstein, M. Pohl, Anushka Udara Abeysekara, Marcos Santander, R. A. Ong, M. J. Lang, A. D. Falcone, Wei Cui, Jamie Holder, M. Kertzman, T. B. Humensky, Robert Brose, M. K. Daniel, R. R. Prado, N. Kelley-Hoskins, P. Kar, David A. Williams, Lucy Fortson, P. Kaaret, M. Nievas-Rosillo, T. J. Williamson, G. H. Sembroski, E. Pueschel, Gernot Maier, P. Moriarty, A. J. Chromey, Gordon T. Richards, E. Roache, Daniel Nieto, U.S. Department of Energy Office of Science, National Science Foundation, Smithsonian Institution, and Natural Sciences and Engineering Research Council of Canada

Subjects
individual objects, stars, Open science, HESS J1825-137, Smithsonian institution, VHE [gamma ray], FOS: Physical sciences, Library science, 01 natural sciences, Technical support, star, HESS, 0103 physical sciences, User Facility, close, individual, 010303 astronomy & astrophysics, ISM, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, gamma rays, flux, inverse scattering method, Work (electrical), binary [gamma ray], general, ddc:540, LS 5039, VERITAS, Astrophysics - High Energy Astrophysical Phenomena, binaries, statistical
Abstract

With 8 hours of observations, VERITAS confirms the detection of two very high energy gamma-ray sources. The gamma-ray binary LS 5039 is detected with a statistical significance of $8.8\sigma$. The measured flux above 1 TeV is $(2.5 \pm 0.4) \times 10^{-12} \rm \, cm^{-2} \, s^{-1}$ near inferior conjunction and $(7.8 \pm 2.8) \times 10^{-13} \rm \, cm^{-2} \, s^{-1}$ near superior conjunction. The pulsar wind nebula HESS J1825-137 is detected with a statistical significance of $6.7\sigma$ and a measured flux above 1 TeV of $(3.9 \pm 0.8) \times 10^{-12} \rm \, cm^{-2} \, s^{-1}$., Comment: 4 pages, 2 figures

Published
2020

34. The evolution of large cavities and disc eccentricity in circumbinary discs

Author

J. Calcino, Enrico Ragusa, Kieran Hirsh, Richard Alexander, Daniel J. Price, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
media_common.quotation_subject, Flow (psychology), Binary number, FOS: Physical sciences, Astrophysics, Edge (geometry), 01 natural sciences, Smoothed-particle hydrodynamics, 0103 physical sciences, Eccentricity (behavior), 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Range (particle radiation), Astronomy and Astrophysics, planet-disc interactions, accretion discs, protoplanetary discs, Orbit, Space and Planetary Science, [SDU]Sciences of the Universe [physics], hydrodynamics, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, binaries, Astrophysics - Earth and Planetary Astrophysics
Abstract

We study the mutual evolution of the orbital properties of high mass ratio, circular, co-planar binaries and their surrounding discs, using 3D Smoothed Particle Hydrodynamics simulations. We investigate the evolution of binary and disc eccentricity, cavity structure and the formation of orbiting azimuthal over-dense features in the disc. Even with circular initial conditions, all discs with mass ratios $q>0.05$ develop eccentricity. We find that disc eccentricity grows abruptly after a relatively long time-scale ($\sim 400\textrm{--}700$ binary orbits), and is associated with a very small increase in the binary eccentricity. When disc eccentricity grows, the cavity semi-major axis reaches values $a_{\rm cav}\approx 3.5\, a_{\rm bin}$. We also find that the disc eccentricity correlates linearly with the cavity size. Viscosity and orbit crossing, appear to be responsible for halting the disc eccentricity growth -- eccentricity at the cavity edge in the range $e_{\rm cav}\sim 0.05\textrm{--} 0.35$. Our analysis shows that the current theoretical framework cannot fully explain the origin of these evolutionary features when the binary is almost circular ($e_{\rm bin}\lesssim 0.01$); we speculate about alternative explanations. As previously observed, we find that the disc develops an azimuthal over-dense feature in Keplerian motion at the edge of the cavity. A low contrast over-density still co-moves with the flow after 2000 binary orbits; such an over-density can in principle cause significant dust trapping, with important consequences for protoplanetary disc observations., 20 pages, 17 figures, 1 table, accepted for publication in MNRAS

Published
2020

35. Properties of the Hyades, the eclipsing binary HD27130, and the oscillating red giant epsilon Tauri

Author

Gražina Tautvaišienė, Šarūnas Mikolaitis, Don A. VandenBerg, Gilles Otten, H. Kjeldsen, Andrea Miglio, Torben Arentoft, R. Minkevičiūtė, Jens Jessen-Hansen, Rimvydas Janulis, Karsten Brogaard, Pere L. Palle, Arnas Drazdauskas, Timothy R. White, Patrick Dorval, D. Slumstrup, V. Bagdonas, Ignas Snellen, M. Fredslund Andersen, E. Stonkutė, Alessandro Marchini, Frank Grundahl, G. J. J. Talens, E. Pakštienė, Brogaard K., Pakstiene E., Grundahl F., Mikolaitis S., Tautvaisiene G., Slumstrup D., Talens G.J.J., Vandenberg D.A., Miglio A., Arentoft T., Kjeldsen H., Janulis R., Drazdauskas A., Marchini A., Minkeviciute R., Stonkute E., Bagdonas V., Fredslund Andersen M., Jessen-Hansen J., Palle P.L., Dorval P., Snellen I.A.G., Otten G.P.P.L., White T.R., Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
oscillations [stars], Red giant, Open clusters and associations: individual: Hyade, Binaries: eclipsing, Astrophysics, 01 natural sciences, eclipsing [binaries], Astrophysics::Solar and Stellar Astrophysics, Abundances, 010303 astronomy & astrophysics, Physics, individual: E Tau [stars], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star cluster, Astrophysics - Solar and Stellar Astrophysics, Stars: individual: HD27130, Astrophysics::Earth and Planetary Astrophysics, open clusters and associations: individual: Hyades, NGC 6791, Hyades, Oscillations, Stars: abundance, stars: abundances, Stars: individual: ϵ Tau, Metallicity, MODELS, Open Clusters and Associations, Individual, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, Binary star, Stars: oscillations, individual: HD27130 [stars], SPECTRA, individual: Hyades [open clusters and associations], Eclipsing, SOLAR, Astrophysics::Galaxy Astrophysics, RADIAL-VELOCITY, stars: individual: ɛ Tau, 010308 nuclear & particles physics, Binaries, White dwarf, Astronomy and Astrophysics, Light curve, Giant star, Stars, EVOLUTION, abundances [stars], HD27130, [SDU]Sciences of the Universe [physics], Space and Planetary Science, ɛ Tau, OPEN CLUSTERS, DISTANCE, STARS, ASTEROSEISMIC MASS
Abstract

Eclipsing binary stars allow derivation of accurate and precise masses and radii. When they reside in star clusters, properties of even higher precision, along with additional information, can be extracted. Asteroseismology of solar-like oscillations offers similar possibilities for single stars. We improve the previously established properties of the Hyades eclipsing binary HD27130 and re-assess the asteroseismic properties of the giant star $\epsilon$ Tau. The physical properties of these members of the Hyades are then used to constrain the helium content and age of the cluster. New multi-colour light curves were combined with multi-epoch radial velocities to yield masses and radii of HD27130. $T_{\rm eff}$ was derived from spectroscopy and photometry, and verified using the Gaia parallax. We estimate the cluster age from re-evaluated asteroseismic properties of $\epsilon$ Tau while using HD27130 to constrain the helium content. The masses and radii, and $T_{\rm eff}$ of HD 27130 were found to be $M=1.0245\pm0.0024 M_{\odot}$, $R=0.9226\pm0.015 R_{\odot}$, $T_{\rm eff}=5650\pm50$ K for the primary, and $M=0.7426\pm0.0016 M_{\odot}$, $R=0.7388\pm0.026 R_{\odot}$, $T_{\rm eff}=4300\pm100$ K for the secondary component. Our re-evaluation of $\epsilon$ Tau suggests that the previous literature estimates are trustworthy, and that the Hipparcos parallax is more reliable than the Gaia DR2 parallax. The helium content of HD27130 and thus of the Hyades is found to be $Y=0.27$ but with significant model dependence. Correlations with the adopted metallicity results in a robust helium enrichment law with $\frac{\Delta Y}{\Delta Z}$ close to 1.2. We estimate the age of the Hyades to be 0.9 $\pm$ 0.1 (stat) $\pm$ 0.1 (sys) Gyr in slight tension with recent age estimates based on the cluster white dwarfs. (abridged), Comment: 14 pages, 8 figures, accepted for publication in Astronomy & Astrophysics

Published
2020
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36. Spectral and polarization properties of black hole accretion disc emission: including absorption effects

Author

R. Taverna, Rene W. Goosmann, Lorenzo Marra, Stefano Bianchi, Michal Dovciak, Frédéric Marin, Giorgio Matt, W. Zhang, Taverna, R, Marra, L, Bianchi, S, Dovčiak, M, Goosmann, R, Marin, F, Matt, G, Zhang, W, Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
accretion discs -polarization -stars, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Radiation, 01 natural sciences, accretion, accretion discs, polarization, stars: Abundances, stars: Black holes, X-rays: Binaries, black holes -X-rays, accretion, abundances -stars, Ionization, 0103 physical sciences, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spins, 010308 nuclear & particles physics, Scattering, Astronomy and Astrophysics, Polarization (waves), accretion discs, Accretion (astrophysics), Computational physics, Black hole, [SDU]Sciences of the Universe [physics], Space and Planetary Science, binaries, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The study of radiation emitted from black hole accretion discs represents a crucial way to understand the main physical properties of these sources, and in particular the black hole spin. Beside spectral analysis, polarimetry is becoming more and more important, motivated by the development of new techniques which will soon allow to perform measurements also in the X- and {\gamma}-rays. Photons emitted from black hole accretion discs in the soft state are indeed expected to be polarized, with an energy dependence which can provide an estimate of the black hole spin. Calculations performed so far, however, considered scattering as the only process to determine the polarization state of the emitted radiation, implicitly assuming that the temperatures involved are such that material in the disc is entirely ionized. In this work we generalize the problem by calculating the ionization structure of a surface layer of the disc with the public code CLOUDY , and then by determining the polarization properties of the emerging radiation using the Monte Carlo code STOKES . This allows us to account for absorption effects alongside scattering ones. We show that including absorption can deeply modify the polarization properties of the emerging radiation with respect to what is obtained in the pure-scattering limit. As a general rule, we find that the polarization degree is larger when absorption is more important, which occurs e.g. for low accretion rates and/or spins when the ionization of the matter in the innermost accretion disc regions is far from complete., Comment: 13 pages, 9 figures, accepted for publication in MNRAS

Published
2020

37. The mass discrepancy in intermediate- and high-mass eclipsing binaries: The need for higher convective core masses

Author

K. Pavlovski, V. Tsymbal, John Southworth, Mathias Michielsen, M. G. Pedersen, Dominic M. Bowman, Andrew Tkachenko, Cole Johnston, and Conny Aerts

Subjects
Astronomy, data analysis, CHEMICAL EVOLUTION, Astrophysics, 01 natural sciences, CRITICAL TESTS, binary stars, MACROSCOPIC INHOMOGENEITIES, Astrophysics::Solar and Stellar Astrophysics, Stellar structure, 010303 astronomy & astrophysics, Stellar evolution, Physics, Stellar atmosphere, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Physical Sciences, SOLAR ATMOSPHERE, Astrophysics::Earth and Planetary Astrophysics, stars, Stellar mass, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, MODELS, FRAUNHOFER LINES, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, spectroscopic, Asteroseismology, Computer Science::Digital Libraries, stellar structure, methods, M-CIRCLE-DOT, numerical, 0103 physical sciences, Binary star, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, Astronomy and Astrophysics, Effective temperature, CLOSE BINARIES, eclipsing, Stars, 13. Climate action, Space and Planetary Science, general, STELLAR EVOLUTION, techniques, binaries, binary stars, stellar structure, QB799
Abstract

(Abridged) Eclipsing, spectroscopic double-lined binary star systems (SB2) are excellent laboratories for calibrating theories of stellar interior structure and evolution. We aim to investigate the mass discrepancy in binary stars. We study the effect of near-core mixing on the mass of the convective core of the stars and interpret the results in the context of the mass discrepancy. Two scenarios are considered, where individual stellar components of a binary system are treated independent of each other and where they are forced to have the same age and initial chemical composition. We find that the mass discrepancy is present in our sample and that it is anti-correlated with the surface gravity of the star. No correlations are found with other fundamental and atmospheric parameters, including the stellar mass. The mass discrepancy can be partially accounted for by increasing the amount of near-core mixing in stellar evolution models. We also find that ignoring the microturbulent velocity and turbulent pressure in stellar atmosphere models of hot evolved stars results in overestimation of their effective temperature by up to 8%. Together with enhanced near-core mixing, this can almost entirely account for the 30% mass discrepancy found for the evolved primary component of V380 Cyg. We find a strong link between the mass discrepancy and the convective core mass. The mass discrepancy can be solved by considering the combined effect of extra near-core boundary mixing and consistent treatment in the spectrum analysis of hot evolved stars. Our binary modelling results in convective core masses between 17 and 35% of the stellar mass, in excellent agreement with results from gravity-mode asteroseismology of single stars. This implies larger helium core masses near the end of the main sequence than anticipated so far., 22 pages (17 pages of main text + 5 pages of appendix), 14 figures. Accepted for publication in A&A

Published
2020

38. K2 discovery of a circumsecondary disk transiting EPIC 220208795

Author

D. M. van Dam, L. van der Kamp, Matthew A. Kenworthy, G. Pojmanski, and Eric E. Mamajek

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Star (game theory), Eclipses, FOS: Physical sciences, Astrophysics, Parameter space, Astrophysics::Solar and Stellar Astrophysics, Rings, Eclipsing, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), Orbital elements, Physics, Binaries, Astronomy and Astrophysics, Radius, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Planets and satellites, Impact parameter, Eccentricity (mathematics), Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations of the star EPIC 220208795 (2MASS J01105556+0018507) reveal a single, deep and asymmetric eclipse, which we hypothesize is due to an eclipsing companion surrounded by a tilted and inclined opaque disk, similar to those seen around V928 Tau and EPIC 204376071. We aim to derive physical parameters of the disk and orbital parameters for the companion around the primary star. The modeling is carried out using a modified version of the python package pyPplusS, and optimization is done using emcee. The period analysis makes use of photometry from ground-based surveys, where we perform a period folding search for other possible eclipses by the disk. Parameters obtained by the best model fits are used to obtain the parameter space of the orbital parameters, while the most likely period obtained is used to constrain these parameters. The best model has an opaque disk with a radius of $1.14\pm0.03$ $R_{\odot}$, an impact parameter of $0.61\pm0.02$ $R_{\odot}$, an inclination of $77.01^{\circ}\pm0.03^{\circ}$, a tilt of $36.81^{\circ}\pm0.05^{\circ}$ and a transverse velocity of $77.45\pm0.05$ km s$^{-1}$. The two most likely periods are $\sim 290$ days and $\sim 236$ days, corresponding to an eccentricity of $\sim 0.7$, allowing us to make predictions for the epochs of the next eclipses. All models with tilted and inclined disks result in a minimum derived eccentricity of 0.3, which in combination with the two other known small transiting disk candidates V928 Tau and EPIC 204376071, suggest that there may be a common origin for their eccentric orbits., 13 pages, 10 figures, 10 tables, accepted for publication in Astronomy & Astrophysics. Reduced data and reduction script on GitHub at https://github.com/lizvdkamp/EPIC2202_disk

Published
2022

39. THE DEPENDENCE OF ON- AND OFF-STATE GENERATIONS IN CLASSICAL MICROQUASARS FROM THE DISK DENSITY. 3-D NUMERICAL HYDRODYNAMICAL SIMULATIONS OF THE HIGH AND LOW MASS ACCRETION RATE IN ACCRETION DISK IN MICROQUASAR CYG X-1

Author

V. V. Nazarenko

Subjects
stars, jets, Physics, lcsh:Astronomy, binary stars: jets, methods: numerical, hydrodynamics, Stars, binaries, Astrophysics, State (functional analysis), lcsh:QB1-991, Accretion rate, Astrophysics::Earth and Planetary Astrophysics, Low Mass, Astrophysics::Galaxy Astrophysics
Abstract

In the present work we have computed and have compared the on- and off- generations in low and high mass accretion rate accretion disks. The comparison shows that in the case of low mass accretion rate in disk (10−10 solar mass per year) the ON-state time interval is very short, order of 0.2 ч 0.4 of precession period; in the case of high mass accretion rate in disk (10−9 solar mass per year) the ON-state timeinterval is relatively long, order of 0.7 ч 0.9 of precession period. This shows that in the case more dense disk ON-states are relatively very long time interval because of high mass accretion rate in disk. This result is natural for classical microquasar (CYG X-1) in which the on states are corresponding high mass accretion rates. For comparison we may also write that the time intervals of OFF-states in the present calculations are order of 1.3 ч 1.5 of precession periods. The calculations also show that in OFF-states the accretion disk have the low specific viscosity and on contrary have the high specific angular momentum. In ON-states the disk have to contrary to OFF-states the high specificviscosity and low specific angular momentum. It shows that in OFF-states the disk is very rapidly rotating with low viscosity. In ON-states the situation is on contrary. Such the disk time-behaviour is true for bothlow and high mass accretion rate. The calculations also show that in ON-states the disk radius is very small, order of 0.08 of the orbital separations and on contrary in OFF-states the disk radius is relatively large, order of 0.25 of the orbital separations. The stated aboveshows that the disk is strong transformed from ON- to OFF-states., In the present work we have computed and have compared the on- and off- generations in low and high mass accretion rate accretion disks. The comparison shows that in the case of low mass accretion rate in disk (10−10 solar mass per year) the ON-state time interval is very short, order of 0.2 ч 0.4 of precession period; in the case of high mass accretion rate in disk (10−9 solar mass per year) the ON-state timeinterval is relatively long, order of 0.7 ч 0.9 of precession period. This shows that in the case more dense disk ON-states are relatively very long time interval because of high mass accretion rate in disk. This result is natural for classical microquasar (CYG X-1) in which the on-states are corresponding high mass accretion rates. For comparison we may also write that the time intervals of OFF-states in the present calculations are order of 1.3 ч 1.5 of precession periods. The calculations also show that in OFF-states the accretion disk have the low specific viscosity and on contrary have the high specific angular momentum. In ON-states the disk have to contrary to OFF-states the high specificviscosity and low specific angular momentum. It shows that in OFF-states the disk is very rapidly rotating with low viscosity. In ON-states the situation is on contrary. Such the disk time-behaviour is true for bothlow and high mass accretion rate. The calculations also show that in ON-states the disk radius is very small, order of 0.08 of the orbital separations and on contrary in OFF-states the disk radius is relatively large, order of 0.25 of the orbital separations. The stated aboveshows that the disk is strong transformed from ON- to OFF-states.

Published
2018

40. Mind the Gap

Author

Stephen Justham, Robert Farmer, S. E. de Mink, Mathieu Renzo, Pablo Marchant, and Low Energy Astrophysics (API, FNWI)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Metallicity, OPACITIES, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, BINARIES, 0103 physical sciences, STELLAR INTERIORS, REACTION-RATES, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, NUCLEOSYNTHESIS, Science & Technology, Mass distribution, METALLICITY DEPENDENCE, Astronomy and Astrophysics, THERMONUCLEAR REACTION-RATE, Redshift, WOLF-RAYET STARS, EVOLUTION, Black hole, Stars, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physical Sciences, TURBULENT CONVECTION, Astrophysics - High Energy Astrophysical Phenomena, Mass gap
Abstract

Gravitational-wave detections are now starting to probe the mass distribution of stellar-mass black holes (BHs). Robust predictions from stellar models are needed to interpret these. Theory predicts the existence of a gap in the BH mass distribution because of pair-instability supernova. The maximum BH mass below the gap is the result of pulsational mass loss. We evolve massive helium stars through their late hydrodynamical phases of evolution using the open-source MESA stellar evolution code. We find that the location of the lower edge of the mass gap at 45$M_\odot$ is remarkably robust against variations in the metallicity ($\approx 3M_\odot$), the treatment of internal mixing ($\approx 1M_\odot$), stellar wind mass loss ($\approx 4M_\odot$), making it the most robust predictions for the final stages of massive star evolution. The reason is that the onset of the instability is dictated by the near-final core mass, which in turn sets the resulting BH mass. However, varying $^{12}C\left(\alpha,\gamma\right)^{16}O$ reaction rate within its $1\sigma$ uncertainties shifts the location of the gap between $40M_\odot$ and $56M_\odot$. We provide updated analytic fits for population synthesis simulations. Our results imply that the detection of merging BHs can provide constraints on nuclear astrophysics. Furthermore, the robustness against metallicity suggests that there is a universal maximum for the location of the lower edge of the gap, which is insensitive to the formation environment and redshift for first-generation BHs. This is promising for the possibility to use the location of the gap as a "standard siren" across the Universe., Comment: 17 pages, 5 figures, 1 Table, Accepted ApJ

Published
2019

41. On the weak magnetic field of millisecond pulsars:does it decay before accretion?

Author

Thomas M. Tauris, Andreas Reisenegger, and M. Cruces

Subjects
Angular momentum, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, magnetic fields, general [pulsars], BINARIES, neutron [stars], Pulsar, Millisecond pulsar, Astrophysics::Solar and Stellar Astrophysics, NEUTRON-STAR, LOW-MASS, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), AMBIPOLAR DIFFUSION, MHD INSTABILITIES, white dwarfs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Ambipolar diffusion, White dwarf, Astronomy and Astrophysics, Accretion (astrophysics), EVOLUTION, Magnetic field, Neutron star, EQUILIBRIUM, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, WHITE-DWARF COMPANIONS, DISCOVERY, X-RAY, binaries [X-rays], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Millisecond pulsars are old, fast spinning neutron stars thought to have evolved from classical pulsars in binary systems, where the rapid rotation is caused by the accretion of matter and angular momentum from their companion. During this transition between classical and millisecond pulsars, there is a magnetic field reduction of around 4 orders of magnitude, which is not well understood. According to the standard scenario, the magnetic field is reduced as a consequence of accretion, either through ohmic dissipation or through screening by the accreted matter. We explored an alternative hypothesis in which the magnetic field is reduced through ambipolar diffusion before the accretion. This is particularly effective during the long epoch in which the pulsar has cooled, but has not yet started accreting. This makes the final magnetic field dependent on the evolution time of the companion star and thus its initial mass. We use observed binary systems to constrain the time available for the magnetic field decay based on the current pulsar companion: a helium white dwarf, a carbon-oxygen white dwarf, or another neutron star. Based on a simplified model without baryon pairing, we show that the proposed process agrees with the general distribution of observed magnetic field strengths in binaries, but is not able to explain some mildly recycled pulsars where no significant decay appears to have occurred. We discuss the possibility of other formation channels for these systems and the conditions under which the magnetic field evolution would be set by the neutron star crust rather than the core., Comment: 10 pages, 4 figures, 2 tables

Published
2019

42. Features of globular cluster’s dynamics with an intermediate-mass black hole

Author

Evgenii O. Vasiliev, M. V. Ryabova, Yuri Shchekinov, and Alena S. Gorban

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Dynamics (mechanics), Astronomy and Astrophysics, QB1-991, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, black holes, 03 medical and health sciences, 0302 clinical medicine, Star cluster, Space and Planetary Science, Intermediate-mass black hole, star clusters, 030225 pediatrics, Globular cluster, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, binaries, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

In this paper, we address the question of how a central intermediate-mass black hole (IMBH) in a globular cluster (GC) affects dynamics, core collapse, and formation of the binary population. It is shown that the central IMBH forms a binary system that affects dynamics of stars in the cluster significantly. The presence of an intermediate-mass black hole with mass ≥ 1.0-1.7%of the total stellar mass in the cluster inhibits the formation of binary stars population.

Published
2018

43. SPECTROSCOPIC MONITORING OF THE B[E] OBJECTS FSCMA AND MOCAM

Author

I. A. Usenko, A. Raj, Nadine Manset, R. I. Kokumbaeva, S. A. Khokhlov, A. V. Kusakin, A. Y. Knyazev, Anatoly S. Miroshnichenko, I. V. Reva, A. K. Kuratova, S. V. Zharikov, DGAPA/PAPIIT Project IN100614, and Ministry of Education and Science of the Republic of Kazakhstan Project No BR05236322

Subjects
Physics, Line-of-sight, Infrared, lcsh:Astronomy, Astrophysics, stars, emission-line, Be - stars, evolution, circumstellar matter, binaries, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, lcsh:QB1-991, Stars, Circumstellar dust, Astrophysics::Solar and Stellar Astrophysics, Roche lobe, Emission spectrum, Astrophysics::Earth and Planetary Astrophysics, Supergiant, Astrophysics::Galaxy Astrophysics
Abstract

Objects with the B[e] phenomenon exhibit permitted and forbidden emission lines due to the presence of circumstellar ionized gas and large infrared excesses due to processing of the stellar radiation by circumstellar dust. There are five groups of stars that show this phenomenon (pre-main-sequence Herbig Ae/Be stars, symbiotic systems, proto-planetary nebulae, some supergiant, and FS CMa type objects). The latter group is the most recently discovered and the least explored. The leading hypothesis about the group nature implies that they are mostly intermediate-mass binary sys- tems, whose circumstellar medium was created during a strong mass-transfer phase due to a Roche lobe overflow of the more massive star in the system. We have been conducting a large program of spectroscopic and photometric observations of many objects and candidates to this group. The current report is devoted to the preliminary results of our ongoing study of two objects with similar underlying early B-type stars, FS CMa (the group prototype) and MO Cam. The objects show different emission-line profiles and infrared excesses which are most likely due to different tilt angles of their non-spherical envelopes with respect to the line of sight. Variability of spectral lines is discussed here.

Published
2019

44. News on the X-ray emission from hot subdwarf stars

Author

Nicola La Palombara, Sandro Mereghetti, and ITA

Subjects
010504 meteorology & atmospheric sciences, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, QB1-991, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, x-rays, mass-loss, 01 natural sciences, neutron stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, white dwarfs, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, X-ray, White dwarf, Astronomy and Astrophysics, hot subdwarfs, Subdwarf, Neutron star, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, binaries, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In latest years, the high sensitivity of the instruments on-board the XMM-Newton and Chandra satellites allowed us to explore the properties of the X-ray emission from hot subdwarf stars. The small but growing sample of X-ray detected hot subdwarfs includes binary systems, in which the X-ray emission is due to wind accretion onto a compact companion (white dwarf or neutron star), as well as isolated sdO stars, in which X-rays are probably due to shock instabilities in the wind. X-ray observations of these low-mass stars provide information which can be useful for our understanding of the weak winds of this type of stars and can lead to the discovery of particularly interesting binary systems. Here we report the most recent results we have recently obtained in this research area., Comment: 8 pages, 3 figures. To appear in the Proceedings of the 8th Meeting on Hot Subdwarf Stars and Related Objects, 9-15 July 2017, Cracow, Poland. Eds. A. Baran, A. E. Lynas-Gray, Open Astronomy, in press

Published
2017

45. An additional pulsating mode (7.35 mHz) and pulsations timing variations of PG 1613+426

Author

Adam Moss, Riley Jordan, Marc Amaral, Terry D. Oswalt, Patrice Majewski, and Tomomi Otani

Subjects
Physics, business.industry, Astronomy, Mode (statistics), QB1-991, Astronomy and Astrophysics, Optics, subdwarfs, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, pulsations, binaries, business
Abstract

We present the detection of an additional pulsation mode (7.35 mHz) of a subdwarf B star, PG 1613+426, and periodic Observed minus Calculated (O-C) variations for two existing pulsations. PG 1613+426 is near the hot end of the sdB instability strip. One pulsation mode (6.94 mHz) was detected so far by Bonanno et al. (2002) and another pulsation mode candidate (7.05 mHz) was proposed with a confidence level above 90% by Kuassivi and Ferlet (2005). To constrain sdB star evolutional scenarios, this star was monitored in 2010, 2011, 2015, and 2017 as a part of a project for finding companions to sdB stars using the pulsation timing method. The photometric analysis of those data shows an additional 7.35 mHz pulsation mode as well as the previously detected 6.93 mHz mode. However the 7.05 mHz mode was not detected. Nightly amplitude changes of 7.35 mHz mode were observed in the 2011 data, however the 2017 data did not show nightly amplitude shifts. O-C variations were detected in both 6.93 mHz and 7.35 mHz pulsations, indicating that PG 1613+426 may have a low mass companion star. However, more observations are needed to confirm it.

Published
2017

46. Constraining Roche-Lobe Overflow Models Using the Hot-Subdwarf Wide Binary Population

Author

Joris Vos and M. Vučković

Subjects
Physics, stars, education.field_of_study, Astronomy, Population, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, QB1-991, Astrophysics, Subdwarf, Red-giant branch, Stars, Common envelope, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, subdwarfs, Roche lobe, education, binaries, Stellar evolution, rlof, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

One of the important issues regarding the final evolution of stars is the impact of binarity. A rich zoo of peculiar, evolved objects are born from the interaction between the loosely bound envelope of a giant, and the gravitational pull of a companion. However, binary interactions are not understood from first principles, and the theoretical models are subject to many assumptions. It is currently agreed upon that hot subdwarf stars can only be formed through binary interaction, either through common envelope ejection or stable Roche-lobe overflow (RLOF) near the tip of the red giant branch (RGB). These systems are therefore an ideal testing ground for binary interaction models. With our long term study of wide hot subdwarf (sdB) binaries we aim to improve our current understanding of stable RLOF on the RGB by comparing the results of binary population synthesis studies with the observed population. In this article we describe the current model and possible improvements, and which observables can be used to test different parts of the interaction model., 5 pages, 2 figures, accepted for publication in open astronomy as part of the conference proceedings for the 8th meeting on hot subdwarfs and related objects in Krakow

Published
2017

47. Observational prospects for phase transitions at LISA: Fisher matrix analysis

Author

Chloe Gowling, Mark Hindmarsh, Department of Physics, and Helsinki Institute of Physics

Subjects
Astrophysics and Astronomy, Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Parameter space, 114 Physical sciences, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, BINARIES, High Energy Physics - Phenomenology (hep-ph), Speed of sound, 0103 physical sciences, gravitational waves /sources, physics of the early universe, Sensitivity (control systems), 010303 astronomy & astrophysics, Particle Physics - Phenomenology, Physics, General Relativity and Cosmology, 010308 nuclear & particles physics, Gravitational wave, Spectral density, hep-ph, Astronomy and Astrophysics, gravitational waves / theory, Computational physics, High Energy Physics - Phenomenology, cosmological perturbation theory, astro-ph.CO, CONFUSION, Electroweak scale, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A first order phase transition at the electroweak scale would lead to the production of gravitational waves that may be observable at upcoming space-based gravitational wave (GW) detectors such as LISA (Laser Interferometer Space Antenna). As the Standard Model has no phase transition, LISA can be used to search for new physics by searching for a stochastic gravitational wave background. In this work we investigate LISA's sensitivity to the thermodynamic parameters encoded in the stochastic background produced by a phase transition, using the sound shell model to characterise the gravitational wave power spectrum, and the Fisher matrix to estimate uncertainties. We explore a parameter space with transition strengths $��< 0.5$ and phase boundary speeds $0.4 < v_\text{w} < 0.9$, for transitions nucleating at $T_{\text{N}} = 100$ GeV, with mean bubble spacings $0.1$ and $0.01$ of the Hubble length, and sound speed $c/\sqrt{3}$. We show that the power spectrum in the sound shell model can be well approximated by a four-parameter double broken power law, and find that the peak power and frequency can be measured to approximately 10% accuracy for signal-to-noise ratios (SNRs) above 20. Determinations of the underlying thermodynamic parameters are complicated by degeneracies, but in all cases the phase boundary speed will be the best constrained parameter. Turning to the principal components of the Fisher matrix, a signal-to-noise ratio above 20 produces a relative uncertainty less than 3% in the two highest-order principal components, indicating good prospects for combinations of parameters. The highest-order principal component is dominated by the wall speed. These estimates of parameter sensitivity provide a preliminary accuracy target for theoretical calculations of thermodynamic parameters., 37 pages, 11 figures

Published
2021

48. The first heavy-metal hot subdwarf composite binary SB 744

Author

Péter Németh, Alexander Bastian, Francisco Molina, and Joris Vos

Subjects
Atmospheres, Evolution, Metallicity, Population, Subdwarfs, FOS: Physical sciences, Context (language use), Helium flash, Astrophysics, SB 744 [Individual], Spectroscopic, Chemically peculiar, 23 Química, Astrophysics::Solar and Stellar Astrophysics, Abundances, education, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, education.field_of_study, Binaries, Astronomy and Astrophysics, Astrometry, Stars, Subdwarf, Radial velocity, Individual: SB 744, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract

A radial velocity follow-up of the long-period sdOB+G1V type spectroscopic binary SB 744 revealed strong lines of fluorine and lead in the optical spectrum of the sdOB star and subsolar metallicity in the G1V companion. With high-quality observations and Gaia astrometric data, we aim at measuring the chemical composition and Galactic kinematics of the system to put it in context with known populations of hot subdwarfs. Such binary systems have high potential, as they give insights into the late stages of binary evolution as well as into the mysterious formation of stripped core helium-burning stars. We have analyzed the optical spectra with homogeneous atmospheric models to derive surface parameters of the binary members from a direct wavelength space decomposition and independently measured the atmospheric properties of the cool companion. The two independent methods reached consistent results, which, amended with constraints from spectral energy distributions provided a subdwarf mass. The Gaia astrometry allowed us to derive the Galactic kinematics of the system. SB 744 turned out to be an old, Population II system, that has gone through dramatic events. The hot subdwarf star belongs to the heavy-metal subclass of sdOB stars and we report super-solar abundances of lead, based on Pb III/IV lines. The He abundance of the hot subdwarf is the lowest among the known heavy-metal sdOB stars. The presence of fluorine implies that SB 744 was once a hierarchical triple system and the inner binary has merged in the near past. As an alternative scenario, single-star evolution through late core helium flash and atmospheric mixing can also produce the observed fluorine abundances. The atmospheric metal over-abundances currently observed are perhaps the results of a combination of mixing processes during formation and radiative support., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2021

49. CONSTRAINING MODELS OF MODIFIED GRAVITY WITH THE DOUBLE PULSAR PSR J0737-3039A/B SYSTEM.

Author

IORIO, LORENZO and RUGGIERO, MATTEO LUCA

Subjects
*GRAVITATION, *FIELD theory (Physics), *PHYSICS, *PULSARS, *RADIATION sources
Abstract

In this paper we use ΔP = -1.772341 ± 13.153788 s between the phenomenologically determined orbital period Pb of the PSR J0737-3039A/B double pulsar system and the purely Keplerian period $P^{(0)}=2\pi\sqrt{a^3/G(m_{\rm A}+m_{\rm B})}$ calculated with the system's parameters, determined independently of the third Kepler law itself, in order to put constraints on some models of modified gravity (f(R), Yukawa-like fifth force, MOND). The major source of error affecting ΔP is not the one in the phenomenologically measured period (δPb = 4×10-6s), but the systematic uncertainty δP(0) in the computed Keplerian one due to the relative semimajor axis a mainly caused, in turn, by the errors in the ratio ${\mathcal R}$ of the pulsars' masses and in sin i. We get |κ| ≤ 0.8 × 10-26m-2 for the parameter that in the f(R) framework is a measure of the nonlinearity of the theory, |α| ≤ 5.5 × 10-4 for the fifth-force strength parameter (for λ ≈ a = 0.006 AU). The effects predicted by the strong-acceleration regime of MOND are far too small to be constrained with some effectiveness today and in the future as well. In view of the continuous timing of such an important system, it might happen that in the near future it will be possible to obtain somewhat tighter constraints. [ABSTRACT FROM AUTHOR]

Published
2007
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50. Eccentricity generation in hierarchical triple systems: the planetary regime.

Author

Georgakarakos, Nikolaos

Subjects
*CELESTIAL mechanics, *BINARY stars, *BINARY star orbits, *ECCENTRICS & eccentricities, *MASS (Physics), *PHYSICS
Abstract

In previous papers, we developed a technique for estimating the inner eccentricity in hierarchical triple systems, with the inner orbit being initially circular. We considered systems with well-separated components and different initial setups (e.g., coplanar and non-coplanar orbits). However, the systems we examined had comparable masses. In the present paper, the validity of some of the formulae derived previously is tested by numerically integrating the full equations of motion for systems with smaller mass ratios (from 10−3 to 103, i.e. systems with Jupiter-sized bodies). There is also discussion about HD 217107 and its planetary companions. [ABSTRACT FROM AUTHOR]

Published
2006
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