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Virgo Horoscope Today: March 22, 2024 | Vogue India | Horoscope

Virgo

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VIRGO AND HER NEIGHBORS

Virgo was recently selected to join the Summer ’17 , and we are launching our first product later this month. With this in mind, I thought it would be beneficial to explain a bit about what we are working on and why we are so excited to be working on it. NYC Techstars accelerator program Virgo provides a cloud-based video recording platform for colonoscopies. The system is incredibly user friendly, especially compared to the medical hardware and software to which physicians are accustomed. Before Virgo, gastroenterologists had to carry around unsecure DVDs and external hard drives just to record their procedures. As a result, the vast majority of colonoscopies went unrecorded, with perhaps only a few still images saved per case. Virgo helps doctors stay organized and use this video content for research, training, quality improvement, and patient education. You may ask why we chose to solve this problem, and every company has an origin story. For us, it was a convergence of serendipity, curiosity, strangers, and friends that led to the formation of Virgo. I was 13 years old when my dad bought an iMac with iMovie and a digital camcorder. It took about a week for my friends and me to start making home movies. We parodied Mission Impossible and Scream, made a music video for Michael Jackson’s , and created a stop motion video of Teenage Mutant Ninja Turtle action figures breakdancing. I spent hours editing those movies instead of studying. Beat It Those hours paid off, and I eventually became a product manager for a medical device company. For every new product launch, I would observe surgeries and help doctors learn to use the new equipment. I always tried to capture and edit video from the cases. The video footage we captured became our best asset. We turned surgical footage into sales tools, marketing pieces, and educational clips for both patients and surgeons. Then, while working at a robotic surgery company, I noticed even more opportunities to capture medical video. However, the existing equipment for recording medical video is challenging to set up and records onto DVDs and external hard drives. Doctors and nurses rarely, if ever, use the equipment — they have better things to worry about. While screening colonoscopy is an effective tool for detecting pre-cancerous polyps, There is good reason to believe that the systematic video recording of colonoscopies will lead to even better medicine. We founded Virgo to make that a reality. colorectal cancer remains the third leading cause of cancer related deaths in the United States at over 50,000 per year. Video is becoming ubiquitous in society. Clearly, video is an incredible communication tool. Three hundred hours of video are uploaded to YouTube every minute. Facebook serves over 8 billion video views per day. A simple cliché explains why video is so powerful: If a picture is worth a thousand words, then a 15 minute colonoscopy video is worth 54 words (15 mins * 60 secs * 60 frames/sec * 1000 words/frame). It is estimated that there are . That’s 7.56 * 10¹⁴ words, or about 15 times more words than are contained in my favorite novel, . million 14 million colonoscopies per year in the US alone billion , by Kurt Vonnegut Slaughterhouse-Five But before Virgo, no one was writing all those words down. By recording clinical videos and writing these words down, physicians will be able to practice their craft better than ever before by reducing errors, cutting waste out of the system, and better educating patients. Magical things start happening when you record lots of video. You notice things that you hadn’t noticed before. You learn things. Other people learn things from you. We expect the same magical things to happen in medicine. We’re working with gastroenterologists at UCLA, Harvard, Penn Medical Center, UCSF, Rush University, UMASS, Indiana University, and Duke University, all of whom are excited to record their procedures. Like us, they believe systematic video recording will benefit research, training, quality of care, and patient education. Even more exciting are all the applications they haven’t thought of yet. We’re at the beginning of this journey, and we’re looking for talented software developers, hardware engineers, data scientists, and all those passionate about improving through to come join us. If this sounds like you or someone you know, please reach out. healthcare technology Sincerely, Matt Schwartz CEO & Co-Founder, Virgo matt@virgosvs.com P.S. If you know a gastroenterologist that would be interested in learning more about Virgo’s technology, be sure to forward this post to them!

Introducing Virgo

Advancing the Detection of Ultralight Vector Dark Matter through Novel Analytical Strategies

The Next Steps for Primordial Black Hole Research

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3.3 Plugging the pair instability gap with PBH? An equally powerful mass challenge for PBH arises from the pair instability gap. This is generated by the catastrophic core collapse of massive stars that results from pair-instability SNe, and predicts a deficit of astrophysical BH between ∼ 50 M⊙ and ∼ 120 M⊙. The full LIGO-Virgo O3 data set reveals a definitive decline in merger rates above ∼ 40 M⊙ [55] but with several candidates filling this gap at high credibility [56]. Could PBH populate the pair instability gap? A smoking gun signature would be a feature in the BH mass spectrum, most likely indicative of a new formation mechanism. 3.4 PBH eccentricity Even though PBH binaries are formed with large eccentricity at high redshift, they have enough time to circularize before the GW signal can enter the observation band of current and future detectors. This implies that an observation of a non-zero eccentricity e would rule out the interpretation as a primordial binary formed in the early Universe, while it may still be compatible with a PBH binary formed in the late-time universe [57, 58]. 3.5 PBH spin The PBHs form in the early universe through the standard scenario of the collapse of large overdensities inherit a characteristic mass-spin correlations induced by accretion effects [7]. Using this criterion for determining the possible primordial nature of individual GW events would require reducing uncertainties on the accretion model and studied at the population level [59]. Fig. 3 presents a flowchart from Ref. [47] one might follow to assess the primordial nature of a binary merger based on measurements of the redshift z, eccentricity e, tidal deformability Λ, component masses m, and dimensionless spins χ. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3.3 Plugging the pair instability gap with PBH? An equally powerful mass challenge for PBH arises from the pair instability gap. This is generated by the catastrophic core collapse of massive stars that results from pair-instability SNe, and predicts a deficit of astrophysical BH between ∼ 50 M⊙ and ∼ 120 M⊙. The full LIGO-Virgo O3 data set reveals a definitive decline in merger rates above ∼ 40 M⊙ [55] but with several candidates filling this gap at high credibility [56]. Could PBH populate the pair instability gap? A smoking gun signature would be a feature in the BH mass spectrum, most likely indicative of a new formation mechanism. 3.4 PBH eccentricity Even though PBH binaries are formed with large eccentricity at high redshift, they have enough time to circularize before the GW signal can enter the observation band of current and future detectors. This implies that an observation of a non-zero eccentricity e would rule out the interpretation as a primordial binary formed in the early Universe, while it may still be compatible with a PBH binary formed in the late-time universe [57, 58]. 3.5 PBH spin The PBHs form in the early universe through the standard scenario of the collapse of large overdensities inherit a characteristic mass-spin correlations induced by accretion effects [7]. Using this criterion for determining the possible primordial nature of individual GW events would require reducing uncertainties on the accretion model and studied at the population level [59]. Fig. 3 presents a flowchart from Ref. [47] one might follow to assess the primordial nature of a binary merger based on measurements of the redshift z, eccentricity e, tidal deformability Λ, component masses m, and dimensionless spins χ. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

Cab the Pair Instability Gap Be Plugged With Primordial Black Holes?

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3 The PBH Roadmap Future experiments abound, ranging from approved projects to imminently enter the detailed design phase, to provide significantly enhanced constraints on PBH scenarios, including terrestrial laser interferometers (Einstein Telescope, Cosmic Explorer)[25], and space laser interferometers (LISA, DECIGO [26], TianQin and Taiji [27]), to atomic interferometers on the ground with demonstrators under construction and extensions planned to km scales (AION MAGIS, MAGIA, MIGA, ELGA, ZAIGA), as well as in space (AEDGE) [28], and designs for lunar interferometer/seismometer arrays (LGWA, GLOC)[29]. The science goals focus on bridging frequency gaps in the LIGO/VIRGO/KAGRA frequency range that has so far led to hundreds of detections of BH mergers in the (10 − 100)M⊙ range by going both to higher and lower frequencies. The new science that can be explored ranges from the masses and equation of state of neutron stars as well as multimessage signals from core collapse supernovae to kpc distances (kHz to Hz range) to SMBH and IMBH detections and BH inspiralling (Hz to mHz, and eventually µHz). One would ultimately approach the pulsar timing array sensitivities (NANOGrav, SKA) at nanohertz frequencies to enable exploration of first order very early universe phase transitions, and presence of loop decays in a network of cosmic strings [30]. We next address various “smoking-gun” signatures that may identify PBHs, notably including high redshift mergers and sub-solar mass PBHs. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3 The PBH Roadmap Future experiments abound, ranging from approved projects to imminently enter the detailed design phase, to provide significantly enhanced constraints on PBH scenarios, including terrestrial laser interferometers (Einstein Telescope, Cosmic Explorer)[25], and space laser interferometers (LISA, DECIGO [26], TianQin and Taiji [27]), to atomic interferometers on the ground with demonstrators under construction and extensions planned to km scales (AION MAGIS, MAGIA, MIGA, ELGA, ZAIGA), as well as in space (AEDGE) [28], and designs for lunar interferometer/seismometer arrays (LGWA, GLOC)[29]. The science goals focus on bridging frequency gaps in the LIGO/VIRGO/KAGRA frequency range that has so far led to hundreds of detections of BH mergers in the (10 − 100)M⊙ range by going both to higher and lower frequencies. The new science that can be explored ranges from the masses and equation of state of neutron stars as well as multimessage signals from core collapse supernovae to kpc distances (kHz to Hz range) to SMBH and IMBH detections and BH inspiralling (Hz to mHz, and eventually µHz). One would ultimately approach the pulsar timing array sensitivities (NANOGrav, SKA) at nanohertz frequencies to enable exploration of first order very early universe phase transitions, and presence of loop decays in a network of cosmic strings [30]. We next address various “smoking-gun” signatures that may identify PBHs, notably including high redshift mergers and sub-solar mass PBHs. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

The Primordial Black Hole Roadmap

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 2.2 What is the effect of PBH clustering? Another open issue worth mentioning is the clustering of PBHs. It may significantly affect the merger rates of coalescing binaries and, consequently, the gravitational wave signal measured by the LIGO/Virgo collaboration and by future experiments. Indeed, even if isolated PBH binaries are not significantly affected by encounters with a third PBH, PBH binaries residing in PBH clusters might suffer such interactions, thus modifying the expected merger rate. If PBHs cluster or not is therefore an important question to address. A significant PBH clustering might also modify constraints arising from microlensing observations and from the cosmic microwave background. Clustering might also be relevant in determining PBH spins. While the gravitational collapse of a spherical over density during radiation domination generates nearly spinless PBHs [6], they may acquire a large spin in the presence of accretion [7]. Indeed, if PBHs cluster they can more easily merge to form binaries at late times, so that the resulting PBH coming from such merger will have a non-zero value even when no accretion is present. PBHs, even if rare, are potentially important for seeding galaxy and even quasar formation at very high redshift [11]. These would be intermediate mass PBHs that enhanced local growth by gravitational instability of cold dark matter. in such a scenario, both massive galaxies and SMBH would form at epochs much earlier than in the standard model of structure formation. Moreover SMBH formation would precede or be contemporaneous with massive galaxy formation, as actually favored by recent JWST observations [12]. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 2.2 What is the effect of PBH clustering? Another open issue worth mentioning is the clustering of PBHs. It may significantly affect the merger rates of coalescing binaries and, consequently, the gravitational wave signal measured by the LIGO/Virgo collaboration and by future experiments. Indeed, even if isolated PBH binaries are not significantly affected by encounters with a third PBH, PBH binaries residing in PBH clusters might suffer such interactions, thus modifying the expected merger rate. If PBHs cluster or not is therefore an important question to address. A significant PBH clustering might also modify constraints arising from microlensing observations and from the cosmic microwave background. Clustering might also be relevant in determining PBH spins. While the gravitational collapse of a spherical over density during radiation domination generates nearly spinless PBHs [6], they may acquire a large spin in the presence of accretion [7]. Indeed, if PBHs cluster they can more easily merge to form binaries at late times, so that the resulting PBH coming from such merger will have a non-zero value even when no accretion is present. PBHs, even if rare, are potentially important for seeding galaxy and even quasar formation at very high redshift [11]. These would be intermediate mass PBHs that enhanced local growth by gravitational instability of cold dark matter. in such a scenario, both massive galaxies and SMBH would form at epochs much earlier than in the standard model of structure formation. Moreover SMBH formation would precede or be contemporaneous with massive galaxy formation, as actually favored by recent JWST observations [12]. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

What Is the Effect of PBH Clustering?

This paper is available on arxiv under CC 4.0 license. Authors: (1) Igor Yu. Potemine, Institut de Math´ematiques, Universit´e Paul Sabatier. Table of Links Abstract and Introduction 5-dimensional Einstein Equations Nested Gogberashvili Models Harmony of Transcosmic Spheres Sequence of Event Horizons Time-amalgamated Multiverses Dark Energy and Multiversal Nurseries Black Holes as Multiverses Multi-solitonic and Gyratonic Gravitational Waves Elliptic and Spiral Galaxies Cosmological Coupling Conclusion and References 12 Conclusion It turns out that nested Gogberashvili shells represent good models for multiverses inside the Hyperverse. In this paper we have restrained the Hyperverse to its local (4 + 1)- dimensional stratum. However, similar solutions exist in all dimensions d + 1 with d > 2. In fact, we can construct an infinite tower of embedded Gogberashvili multiverses of various dimensions. An alternative approach is given by Robinson-Trautman metrics describing expanding spacetimes and spherical gravitational waves. It provides us with an intriguing idea to consider supermassive astronomical black holes as expanding (2 + 1)-dimensional multiverses (with possible higher strata too). It might give new angles of view on the black hole growth, the cosmological coupling, relativistic jets and even on the classification of galaxies. References [1] V. Rubakov and M. Shaposhnikov. Extra space-time dimensions: Towards a solution to the cosmological constant problem. Physics Letters B, 125(2-3):139–143, 1983. [2] M. Gogberashvili. Our world as an expanding shell. Europhysics Letters, 7(3):396–399, 2000. [3] I. Potemine. The amalgamated structure of the Local Multiverse. Journal of High Energy Physics, Gravitation and Cosmology, 7(4):1213–1218, 2021. [4] K. Alvi. Approximate binary-black-hole metric. Physical Review D, 61(12-15), 2000. [5] J. Podolsky, R. Svarc, and H. Maeda. All solutions of Einstein’s equations in 2+1 dimensions: Λ-vacuum, pure radiation, or gyratons. Classical and Quantum Gravity, 36, 2019. [6] I. Robinson and A. Trautman. Spherical gravitational waves. Physical Review Letters, 8(4):431–432, 1960. 7] J. Podolsky and R. Svarc. Gyratons in the Robinson–Trautman and Kundt classes. Physical Review D, 99, 2019. [8] T.X. Zhang. The principles and laws of black hole universe. Journal of Modern Physics, 9(9):1838–1865, 2018. [9] Y. Bisabr. Gravitational coupling and the cosmological constant. International Journal of Modern Physics D, 27(8), 2018. [10] K. Croker, M. Zevin, D. Farrah, K. Nishimura, and G. Tarl´e. Cosmologically coupled compact objects: A single-parameter model for LIGO–Virgo mass and redshift distributions. The Astrophysical Journal Letters, 921(2), 2021.

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