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123 results on '"Astrophysics - Cosmology and Nongalactic Astrophysics"'

1. Cosmology of Sub-MeV Dark Matter Freeze-In

Author

Tongyan Lin, Cora Dvorkin, and Katelin Schutz

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Milky Way, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Quasar, Observable, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, Standard Model, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 13. Climate action, 0103 physical sciences, 010306 general physics, Reionization, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dark matter (DM) could be a relic of freeze-in through a light mediator, where the DM is produced by extremely feeble, IR-dominated processes in the thermal Standard Model plasma. In the simplest viable models with the DM mass below the MeV scale, the DM has a small effective electric charge and is born with a nonthermal phase-space distribution. This DM candidate would cause observable departures from standard cosmological evolution. In this work, we combine data from the cosmic microwave background (CMB), Lyman-$\alpha$ forest, quasar lensing, stellar streams, and Milky Way satellite abundances to set a lower limit on freeze-in DM masses up to $\sim 20\,$keV, with the exact constraint depending on whether the DM thermalizes in its own sector. We perform forecasts for the CMB-S4 experiment, the Hydrogen Epoch of Reionization Array, and the Vera Rubin Observatory, finding that freeze-in DM masses up to $\sim 80\,$keV can be explored. These cosmological probes are highly complementary with proposed direct-detection efforts to search for this DM candidate., Comment: 5+17 pages, 3+9 figures

Published
2021

2. GW190521 from the Merger of Ultradwarf Galaxies

Author

Antonella Palmese and Christopher J. Conselice

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Redshift, General Relativity and Quantum Cosmology, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, Production (computer science), Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Stellar evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Dwarf galaxy
Abstract

We present an alternative formation scenario for the gravitational wave event GW190521, that can be explained as the merger of central black holes from two ultra-dwarf galaxies of stellar mass $\sim 10^5-10^6 ~M_\odot$, which had themselves previously undergone a merger. The GW190521 components' masses of $85^{+21}_{-14}M_\odot$ and $66^{+17}_{-18}M_\odot$ challenge standard stellar evolution models, as they fall in the so-called mass gap. We demonstrate that the merger history of ultra-dwarf galaxies at high redshifts ($1\lesssim z \lesssim 2$) matches well the LIGO/Virgo inferred merger rate for black holes within the mass range of the GW190521 components, resulting in a likely time delay of $\lesssim 4$ Gyr considering the redshift of this event. We further demonstrate that the predicted time-scales are consistent with expectations for central black hole mergers, although with large uncertainties due to the lack of high-resolution simulations in low-mass dwarf galaxies. Our findings show that this black hole production and merging channel is viable and extremely interesting as a new way to explore galaxies' black hole seeds and galaxy formation. We recommend this scenario be investigated in detail with simulations and observations., 8 pages, 4 figures

Published
2021

3. Large Anisotropies of the Stochastic Gravitational Wave Background from Cosmic Domain Walls

Author

Rong-Gen Cai, Jing Liu, and Zong-Kuan Guo

Subjects
Inflation (cosmology), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Gravitational wave, FOS: Physical sciences, General Physics and Astronomy, Spectral density, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Scale invariance, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Scalar field, Quantum fluctuation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the stochastic gravitational wave background (SGWB) from cosmic domain walls (DWs) caused by quantum fluctuations of a light scalar field $\phi$ during inflation. Perturbations of $\phi$ remain almost constant after leaving the Hubble horizon. The probabilities of the two domains depend on the averaged value of $\phi$ at each large scale region, leading to large scale perturbations of DW energy density and large anisotropies in the SGWB. We find that the angular power spectrum is scale-invariant and at least of the order of $10^{-2}$, which is expected to be detected by future gravitational-wave (GW) detectors. Since we have not detected primordial GWs yet, anisotropies of the SGWB could help us to verify the rationality of inflation and determine the energy scale of inflation., Comment: 6 pages, 2 figures

Published
2021

4. Low Mass Black Holes from Dark Core Collapse

Author

Anupam Ray, Basudeb Dasgupta, and Ranjan Laha

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Stellar evolution, Chandrasekhar limit, Particle Physics - Phenomenology, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, General Relativity and Cosmology, Gravitational wave, hep-ph, Redshift, Black hole, High Energy Physics - Phenomenology, astro-ph.CO, Production (computer science), Astrophysics - High Energy Astrophysical Phenomena, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Unusual masses of black holes being discovered by gravitational wave experiments pose fundamental questions about the origin of these black holes. Black holes with masses smaller than the Chandrasekhar limit $\approx1.4\,M_\odot$ are essentially impossible to produce through stellar evolution. We propose a new channel for production of low mass black holes: stellar objects catastrophically accrete non-annihilating dark matter, and the small dark core subsequently collapses, eating up the host star and transmuting it into a black hole. The wide range of allowed dark matter masses allows a smaller effective Chandrasekhar limit, and thus smaller mass black holes. We point out several avenues to test our proposal, focusing on the redshift dependence of the merger rate. We show that redshift dependence of the merger rate can be used as a probe of the transmuted origin of low mass black holes., v2: 8 pages, 2 figures, Minor changes (Fig. 2 updated, text improved), Conclusions unchanged. Matches version published in Physical Review Letters

Published
2021

5. Test for the Origin of Solar Mass Black Holes

Author

Alexander Kusenko, George M. Fuller, and Volodymyr Takhistov

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Population, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, education, Stellar evolution, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Solar mass, education.field_of_study, Mass distribution, High Energy Physics - Phenomenology, Neutron star, Production (computer science), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Solar-mass black holes with masses in the range of $\sim 1-2.5 M_{\odot}$ are not expected from conventional stellar evolution, but can be produced naturally via neutron star (NS) implosions induced by capture of small primordial black holes (PBHs) or from accumulation of some varieties of particle dark matter. We argue that a unique signature of such "transmuted" solar-mass BHs is that their mass distribution would follow that of the NSs. This would be distinct from the mass function of black holes in the solar-mass range predicted either by conventional stellar evolution or early Universe PBH production. We propose that analysis of the solar-mass BH population mass distribution in a narrow mass window of $\sim 1-2.5\,{\rm M}_\odot$ can provide a simple yet powerful test of the origin of these BHs. Recent LIGO/VIRGO gravitational wave (GW) observations of the binary merger events GW190425 and GW190814 are consistent with a BH mass in the range $\sim 1.5-2.6~M_{\odot}$. Though these results have fueled speculation on dark matter-transmuted solar-mass BHs, we demonstrate that it is unlikely that the origin of these particular events stems from NS implosions. Data from upcoming GW observations will be able to distinguish between solar-mass BHs and NSs with high confidence. This capability will facilitate and enhance the efficacy of our proposed test., Comment: 6 pages, 1 figure, 1 table

Published
2021

6. Deep Search for Decaying Dark Matter with XMM-Newton Blank-Sky Observations

Author

Yujin Park, Benjamin R. Safdi, Marius Kongsore, Kyle Cranmer, Nicholas L. Rodd, Joshua W. Foster, and Christopher Dessert

Subjects
Sterile neutrino, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Continuum (design consultancy), Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, 01 natural sciences, Standard Model, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Galactic Center, High Energy Physics - Phenomenology, 13. Climate action, Sky, High Energy Physics::Experiment, Halo, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Sterile neutrinos with masses in the keV range are well-motivated extensions to the Standard Model that could explain the observed neutrino masses while also making up the dark matter (DM) of the Universe. If sterile neutrinos are DM then they may slowly decay into active neutrinos and photons, giving rise to the possibility of their detection through narrow spectral features in astrophysical X-ray data sets. In this work, we perform the most sensitive search to date for this and other decaying DM scenarios across the mass range from 5 to 16 keV using archival XMM-Newton data. We reduce 547 Ms of data from both the MOS and PN instruments using observations taken across the full sky and then use this data to search for evidence of DM decay in the ambient halo of the Milky Way. We determine the instrumental and astrophysical baselines with data taken far away from the Galactic Center, and use Gaussian Process modeling to capture additional continuum background contributions. No evidence is found for unassociated X-ray lines, leading us to produce the strongest constraints to date on decaying DM in this mass range., 8+29 pages, 3+31 figures, Supplementary Data at https://github.com/bsafdi/XMM_BSO_DATA ; v2 additional cross-checks, expanded discussion

Published
2021

7. Cosmic String Interpretation of NANOGrav Pulsar Timing Data

Author

John Ellis and Marek Lewicki

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, String (physics), General Relativity and Quantum Cosmology, Gravitational wave background, High Energy Physics - Phenomenology (hep-ph), Pulsar, 0103 physical sciences, 010306 general physics, Particle Physics - Phenomenology, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, Supermassive black hole, COSMIC cancer database, Einstein Telescope, General Relativity and Cosmology, hep-th, Astrophysics::Instrumentation and Methods for Astrophysics, hep-ph, LIGO, Cosmic string, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), 13. Climate action, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Pulsar timing data used to provide upper limits on a possible stochastic gravitational wave background (SGWB). However, the NANOGrav Collaboration has recently reported strong evidence for a stochastic common-spectrum process, which we interpret as a SGWB in the framework of cosmic strings. The possible NANOGrav signal would correspond to a string tension $G\mu \in (4 \times 10^{-11}, 10^{-10}) $ at the 68% confidence level, with a different frequency dependence from supermassive black hole mergers. The SGWB produced by cosmic strings with such values of $G\mu$ would be beyond the reach of LIGO, but could be measured by other planned and proposed detectors such as SKA, LISA, TianQin, AION-1km, AEDGE, Einstein Telescope and Cosmic Explorer., Comment: matches version published in PRL

Published
2021

8. Primordial Black Holes from Long-Range Scalar Forces and Scalar Radiative Cooling

Author

Marcos M. Flores and Alexander Kusenko

Subjects
Physics, Radiative cooling, Gravitational wave, Scalar (mathematics), Dark matter, Yukawa potential, General Physics and Astronomy, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, LIGO, High Energy Physics - Phenomenology, General Relativity and Quantum Cosmology, symbols.namesake, 0103 physical sciences, symbols, 010306 general physics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract

We describe a new scenario for the formation of primordial black holes (PBHs). In the early Universe, the long-range forces mediated by the scalar fields can lead to formation of halos of heavy particles even during the radiation-dominated era. The same interactions result in the emission of scalar radiation from the motion and close encounters of particles in such halos. Radiative cooling due the scalar radiation allows the halos to collapse to black holes. We illustrate this scenario on a simple model with fermions interacting via the Yukawa forces. The abundance and the mass function of PBHs are suitable to account for all dark matter, or for some gravitational wave events detected by LIGO. The model relates the mass of the dark-sector particles to the masses and abundance of dark matter PBHs in a way that can explain why the dark matter and the ordinary matter have similar mass densities. The model also predicts a small contribution to the number of effective light degrees of freedom, which can help reconcile different measurements of the Hubble constant.

Published
2021

9. Constraining the Lensing of Binary Black Holes from Their Stochastic Background

Author

Matteo Bianconi, Christopher J. Moore, Geraint Pratten, Patricia Schmidt, Alberto Vecchio, Riccardo Buscicchio, Buscicchio, R, Moore, C, Pratten, G, Schmidt, P, Bianconi, M, and Vecchio, A

Subjects
Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational waves, gravitational-wave astronomy, black-hole binarie, Gravitational wave, Population, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Redshift, Gravitational lens, Binary black hole, 0103 physical sciences, Sensitivity (control systems), Connection (algebraic framework), 010306 general physics, education, Astrophysics - Cosmology and Nongalactic Astrophysics, Background radiation
Abstract

Gravitational waves (GWs) are subject to gravitational lensing in the same way as electromagnetic radiation. However, to date, no unequivocal observation of a lensed GW transient has been reported. Independently, GW observatories continue to search for the stochastic GW signal which is produced by many transient events at high redshift. We exploit a surprising connection between the lensing of individual transients and limits to the background radiation produced by the unresolved population of binary back hole mergers: we show that it constrains the fraction of individually resolvable lensed binary black holes to less than $\sim 4\times 10^{-5}$ at present sensitivity. We clarify the interpretation of existing, low redshift GW observations (obtained assuming no lensing) in terms of their apparent lensed redshifts and masses and explore constraints from GW observatories at future sensitivity. Based on our results, recent claims of observations of lensed events are statistically disfavoured., Comment: 9 pages, 6 figures, includes Supplemental material, published in Physical Review Letters

Published
2020

10. First Results on Dark Matter Substructure from Astrometric Weak Lensing

Author

Anna-Maria Taki, Ken Van Tilburg, Neal Weiner, and Cristina Mondino

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Proper motion, Primordial fluctuations, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Baryon, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Substructure, Astrophysics::Earth and Planetary Astrophysics, Sensitivity (control systems), 010306 general physics, Parallax, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Low-mass structures of dark matter (DM) are expected to be entirely devoid of light-emitting regions and baryons. Precisely because of this lack of baryonic feedback, small-scale substructures of the Milky Way are a relatively pristine testing ground for discovering aspects of DM microphysics and primordial fluctuations on subgalactic scales. In this work, we report results from the first search for Galactic DM subhalos with time-domain astrometric weak gravitational lensing. The analysis is based on a matched-filter template of local lensing corrections to the proper motion of stars in the Magellanic Clouds. We describe a data analysis pipeline detailing sample selection, background subtraction, and handling outliers and other systematics. For tentative candidate lenses, we identify a signature based on an anomalous parallax template that can unequivocally confirm the presence of a DM lens, opening up prospects for robust discovery potential with full time-series data. We present our constraints on substructure fraction $f_l \lesssim 5$ at 90% CL (and $f_l \lesssim 2$ at 50% CL) for compact lenses with radii $r_l < 1\,\mathrm{pc}$, with best sensitivity reached for lens masses $M_l$ around $10^7$-$10^8\,M_\odot$. Parametric improvements are expected with future astrometric data sets; by end of mission, $Gaia$ could reach $f_l \lesssim 10^{-3}$ for these massive point-like objects, and be sensitive to lighter and/or more extended subhalos for $\mathcal{O}(1)$ substructure fractions., 9 pages, 11 figures

Published
2020

11. Hidden Cores of Active Galactic Nuclei as the Origin of Medium-Energy Neutrinos: Critical Tests with the MeV Gamma-Ray Connection

Author

Kohta Murase, Shigeo S. Kimura, and Peter Mészáros

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, Flux, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, COSMIC cancer database, Gamma ray, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, KM3NeT, Astrophysics of Galaxies (astro-ph.GA), Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Mysteries about the origin of high-energy cosmic neutrinos have deepened by the recent IceCube measurement of a large diffuse flux in the 10-100 TeV range. Based on the standard disk-corona picture of active galactic nuclei (AGN), we present a phenomenological model enabling us to systematically calculate the spectral sequence of multimessenger emission from the AGN coronae. We show that protons in the coronal plasma can be stochastically accelerated up to PeV energies by plasma turbulence, and find that the model explains the large diffuse flux of medium-energy neutrinos if the cosmic rays carry only a few percent of the thermal energy. We find that the Bethe-Heitler process plays a crucial role in connecting these neutrinos and cascaded MeV gamma rays, and point out that the gamma-ray flux can even be enhanced by the reacceleration of secondary pairs. Critical tests of the model are given by its prediction that a significant fraction of the MeV gamma-ray background correlates with about 10 TeV neutrinos, and nearby Seyfert galaxies including NGC 1068 are promising targets for IceCube, KM3Net, IceCube-Gen2, and future MeV gamma-ray telescopes., 7+6 pages, 4+6 figures, 0+2 tables, version to appear in PRL (submitted on Apr/08/2019), with clarifications and extended descriptions (including discussion on NGC 1068). Conclusions unchanged

Published
2020

12. Spurious Point Source Signals in the Galactic Center Excess

Author

Rebecca K. Leane and Tracy R. Slatyer

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Artifact (error), education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, media_common.quotation_subject, Galactic Center, Population, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Asymmetry, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Region of interest, Point (geometry), Astrophysics - High Energy Astrophysical Phenomena, Spurious relationship, education, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

We re-examine evidence that the Galactic Center Excess (GCE) originates primarily from point sources (PSs). We show that in our region of interest, non-Poissonian template fitting (NPTF) evidence for GCE PSs is an artifact of unmodeled north-south asymmetry of the GCE. This asymmetry is strongly favored by the fit (although it is unclear if this is physical), and when it is allowed, the preference for PSs becomes insignificant. We reproduce this behavior in simulations, including detailed properties of the spurious PS population. We conclude that NTPF evidence for GCE PSs is highly susceptible to certain systematic errors, and should not at present be taken to robustly disfavor a dominantly smooth GCE., Comment: 6+6 pages, 3+3 figures, published in PRL. See also companion PRD paper arXiv:2002.12371

Published
2020

13. Rapid Bound State Formation of Dark Matter in the Early Universe

Author

Tobias Binder, Kyohei Mukaida, Kalliopi Petraki, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, Dark matter, FOS: Physical sciences, General Physics and Astronomy, mass [dark matter], Astrophysics, Gravitation and Astrophysics, 01 natural sciences, thermal, decoupling, dark matter: coupling, formation [bound state], coupling [dark matter], High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Thermal, Bound state, ddc:530, freeze-out, mediation, 010306 general physics, plasma, dark matter: formation, Physics, relic density, Sommerfeld enhancement, electroweak interaction, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Scattering, dark matter: mass, photon, scattering, Electroweak interaction, temperature, Decoupling (cosmology), Plasma, formation [dark matter], bound state: formation, High Energy Physics - Phenomenology, force: long-range, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], long-range [force], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The thermal decoupling description of dark matter (DM) and co-annihilating partners is reconsidered. If DM is realized at around the TeV-mass region or above, even the heaviest electroweak force carriers could act as long-range forces, leading to the existence of meta-stable DM bound states. The formation and subsequent decay of the latter further deplete the relic density during the freeze-out process on top of the Sommerfeld enhancement, allowing for larger DM masses. While so far the bound-state formation was described via the emission of an on-shell mediator ($W^{\pm}$, $Z$, $H$, $g$, photon or exotic), we point out that this particular process does not have to be the dominant scattering-bound state conversion channel in general. If the mediator is coupled in a direct way to any relativistic species present in the Early Universe, the bound-state formation can efficiently occur through particle scattering, where a mediator is exchanged virtually. To demonstrate that such a virtually stimulated conversion process can dominate the on-shell emission even for all temperatures, we analyze a simplified model where DM is coupled to only one relativistic species in the primordial plasma through an electroweak-scale mediator. We find that the bound-state formation cross section via particle scattering can exceed the on-shell emission by up to several orders of magnitude., 9 pages, 2 figures

Published
2020

14. Early Dark Energy from Massive Neutrinos as a Natural Resolution of the Hubble Tension

Author

Mark Trodden and Jeremy Sakstein

Subjects
Physics, High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Tension (physics), Scalar (mathematics), General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Neutrino decoupling, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Coincidence, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), 0103 physical sciences, Dark energy, Neutrino, 010306 general physics, Energy (signal processing), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Hubble tension can be significantly eased if there is an early component of dark energy that becomes active around the time of matter-radiation equality. Early dark energy models suffer from a coincidence problem -- the physics of matter-radiation equality and early dark energy are completely disconnected, so some degree of fine-tuning is needed in order for them to occur nearly simultaneously. In this paper we propose a natural explanation for this coincidence. If the early dark energy scalar couples to neutrinos then it receives a large injection of energy around the time that neutrinos become non-relativistic. This is precisely when their temperature is of order their mass, which, coincidentally, occurs around the time of matter-radiation equality. Neutrino decoupling therefore provides a natural trigger for early dark energy by displacing the field from its minimum just before matter-radiation equality. We discuss various theoretical aspects of this proposal, potential observational signatures, and future directions for its study., Comment: Accepted for publication, structural changes but conclusions unchanged

Published
2020

15. Exploring Primordial Black Holes from the Multiverse with Optical Telescopes

Author

Edoardo Vitagliano, Misao Sasaki, Volodymyr Takhistov, Masahiro Takada, Sunao Sugiyama, and Alexander Kusenko

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, Dark matter, General Physics and Astronomy, FOS: Physical sciences, Primordial black hole, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, 010306 general physics, education, Physics, Inflation (cosmology), Supermassive black hole, education.field_of_study, LIGO, High Energy Physics - Theory (hep-th), 13. Climate action, Event (particle physics), False vacuum, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Primordial black holes (PBHs) are a viable candidate for dark matter if the PBH masses are in the currently unconstrained "sublunar" mass range. We revisit the possibility that PBHs were produced by nucleation of false vacuum bubbles during inflation. We show that this scenario can produce a population of PBHs that simultaneously accounts for all dark matter, explains the candidate event in Subaru Hyper Suprime-Cam (HSC) data, and contains both heavy black holes as observed by LIGO and very heavy seeds of supermassive black holes. We demonstrate with numerical studies that future observations of HSC, as well as other optical surveys, such as LSST, will be able to provide a definitive test for this generic PBH formation mechanism if it is the dominant source of dark matter., 7 pages, 3 figures; v2: published version

Published
2020

16. Neutrino and Positron Constraints on Spinning Primordial Black Hole Dark Matter

Author

Basudeb Dasgupta, Anupam Ray, and Ranjan Laha

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Positron, 0103 physical sciences, 010306 general physics, Particle Physics - Phenomenology, Line (formation), Spin-½, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, General Relativity and Cosmology, hep-th, Galactic Center, hep-ph, High Energy Physics - Phenomenology, Supernova, High Energy Physics - Theory (hep-th), astro-ph.CO, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Primordial black holes can have substantial spin -- a fundamental property that has a strong effect on its evaporation rate. We conduct a comprehensive study of the detectability of primordial black holes with non-negligible spin, via the searches for the neutrinos and positrons in the MeV energy range. Diffuse supernova neutrino background searches and observation of the 511 keV gamma-ray line from positrons in the Galactic center set competitive constraints. Spinning primordial black holes are probed up to a slightly higher mass range compared to non-spinning ones. Our constraint using neutrinos is slightly weaker than that due to the diffuse gamma-ray background, but complementary and robust. Our positron constraints are typically weaker in the lower mass range and stronger in the higher mass range for the spinning primordial black holes compared to the non-spinning ones. They are generally stronger than those derived from the diffuse gamma-ray measurements for primordial black holes having masses greater than a few $\times \, 10^{16}$g., Comment: v2: 8 pages, 5 figures. Results unchanged. Published in Physical Review Letters

Published
2019

17. Cosmic Expansion History from Line-Intensity Mapping

Author

Ely D. Kovetz, Patrick C. Breysse, and José Luis Bernal

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, Dark matter, Cosmic distance ladder, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Universe, Metric expansion of space, 0103 physical sciences, Dark energy, 010306 general physics, Reionization, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

Line-intensity mapping (LIM) of emission form star-forming galaxies can be used to measure the baryon acoustic oscillation (BAO) scale as far back as the epoch of reionization. This provides a standard cosmic ruler to constrain the expansion rate of the Universe at redshifts which cannot be directly probed otherwise. In light of growing tension between measurements of the current expansion rate using the local distance ladder and those inferred from the cosmic microwave background, extending the constraints on the expansion history to bridge between the late and early Universe is of paramount importance. Using a newly derived methodology to robustly extract cosmological information from LIM, which minimizes the inherent degeneracy with unknown astrophysics, we show that present and future experiments can gradually improve the measurement precision of the expansion rate history, ultimately reaching percent-level constraints on the BAO scale. Specifically, we provide detailed forecasts for the SPHEREx satellite, which will target the H$\alpha$ and Lyman-$\alpha$ lines, and for the ground-based COMAP instrument---as well as a future stage-3 experiment---that will target the CO rotational lines. Besides weighing in on the so-called Hubble tension, reliable LIM cosmic rulers can enable wide-ranging tests of dark matter, dark energy and modified gravity., Comment: 7 pages; 3 figures

Published
2019

18. Lighting the Dark: Evolution of the Postinflationary Universe

Author

Richard Easther, Nathan Musoke, and Shaun Hotchkiss

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitation, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Long period, 0103 physical sciences, 010306 general physics, media_common, Physics, Spectral density, Inflaton, 85A40, Universe, High Energy Physics - Phenomenology, Nonlinear system, High Energy Physics - Theory (hep-th), Homogeneous, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In simple inflationary cosmological scenarios the near-exponential growth can be followed by a long period in which the Universe is dominated by the oscillating inflaton condensate. The condensate is initially almost homogeneous, but perturbations grow gravitationally, eventually fragmenting the condensate if it is not disrupted more quickly by resonance or prompt reheating. We show that the gravitational fragmentation of the condensate is well-described by the Schr\"odinger-Poisson equations and use numerical solutions to show that large overdensities form quickly after the onset of nonlinearity. This is the first exploration of this phase of nonlinear dynamics in the very early universe, which can affect the detailed form of the inflationary power spectrum and the dark matter fraction when the dark sector is directly coupled to the inflaton., Comment: 4 pages, 3 figures (v2 added refs)

Published
2019

19. Primordial Black Holes as a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 keV γ-Ray Line

Author

Ranjan Laha

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, Particle Physics - Phenomenology, Line (formation), astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, General Relativity and Cosmology, hep-th, Galactic Center, Gamma ray, hep-ph, Galaxy, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Low Mass, Particle Physics - Theory, Energy (signal processing), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We derive the strongest constraint on the fraction of dark matter that can be composed of low mass primordial black holes by using the observation of the Galactic Center 511 keV gamma-ray line. Primordial black holes of masses $\lesssim$ 10$^{15}$ kg will evaporate to produce $e^\pm$ pairs. The positrons will lose energy in the Galactic Center, become non-relativistic, and then annihilate with the ambient electrons. We derive robust and conservative bounds by assuming that the rate of positron injection via primordial black hole evaporation is less than what is required to explain the SPI/ INTEGRAL observation of the Galactic Center 511 keV gamma-ray line. Depending on the primordial black hole mass function and other astrophysical uncertainties, these constraints are the most stringent in the literature and show that primordial black holes contribute to less than 1\% of the dark matter density. Our technique also probes part of the mass range which was completely unconstrained by previous studies., v2: 8 pages, 2 figures. Published in Physical Review Letters

Published
2019

20. First Star-Forming Structures in Fuzzy Cosmic Filaments

Author

Victor H. Robles, Mark Vogelsberger, Anastasia Fialkov, Philip Mocz, Fernando Becerra, Lars Hernquist, Sownak Bose, Pierre-Henri Chavanis, Mustafa A. Amin, Jesús Zavala, Lachlan Lancaster, Federico Marinacci, Michael Boylan-Kolchin, Mocz P., Fialkov A., Vogelsberger M., Becerra F., Amin M.A., Bose S., Boylan-Kolchin M., Chavanis P.-H., Hernquist L., Lancaster L., Marinacci F., Robles V.H., Zavala J., Physique Statistique des Systèmes Complexes (LPT) (PhyStat), Laboratoire de Physique Théorique (LPT), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse)

Subjects
Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Evolution of the Universe, Cosmology, General Relativity and Quantum Cosmology, Gravitation, Cosmology & Astrophysics, 0103 physical sciences, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QC, Boson, Physics, 16. Peace & justice, Astrophysics - Astrophysics of Galaxies, Galaxy, Baryon, Stars, Astrophysics of Galaxies (astro-ph.GA), Matter wave, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Formation & evolution of stars & galaxie, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In hierarchical models of structure formation, the first galaxies form in low-mass dark matter potential wells, probing the behavior of dark matter on kiloparsec (kpc) scales. Even though these objects are below the detection threshold of current telescopes, future missions will open an observational window into this emergent world. In this Letter we investigate how the first galaxies are assembled in a `fuzzy' dark matter (FDM) cosmology where dark matter is an ultralight $\sim 10^{-22}$~eV boson and the primordial stars are expected to form along dense dark matter filaments. Using a first-of-its-kind cosmological hydrodynamical simulation, we explore the interplay between baryonic physics and unique wavelike features inherent to FDM. In our simulation, the dark matter filaments show coherent interference patterns on the boson de Broglie scale and develop cylindrical soliton-like cores which are unstable under gravity and collapse into kpc-scale spherical solitons. Features of the dark matter distribution are largely unaffected by the baryonic feedback. On the contrary, the distributions of gas and stars, which do form along the entire filament, exhibit central cores imprinted by dark matter -- a smoking gun signature of FDM., Comment: 6 pages, 2 figures, accepted to Phys. Rev. Lett

Published
2019

21. Probing Dark Matter Using Precision Measurements of Stellar Accelerations

Author

David F. Phillips, Aakash Ravi, Nicholas Langellier, Malte Buschmann, Ronald L. Walsworth, and Benjamin R. Safdi

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Milky Way, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Radial velocity, High Energy Physics - Phenomenology, Stars, Gravitational potential, High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Content (measure theory), 010306 general physics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dark matter comprises the bulk of the matter in the universe but its particle nature and cosmological origin remain mysterious. Knowledge of the dark matter density distribution in the Milky Way Galaxy is crucial to both our understanding of the standard cosmological model and for grounding direct and indirect searches for the particles comprising dark matter. Current measurements of Galactic dark matter content rely on model assumptions to infer the forces acting upon stars from the distribution of observed velocities. Here, we propose to apply the precision radial velocity method, optimized in recent years for exoplanet astronomy, to measure the change in the velocity of stars over time, thereby providing a direct probe of the local gravitational potential in the Galaxy. Using numerical simulations, we develop a realistic strategy to observe the differential accelerations of stars in our Galactic neighborhood with next-generation telescopes, at the level of $10^{-8}$ cm/s$^{2}$. Our simulations show that detecting accelerations at this level with an ensemble of $10^{3}$ stars requires the effect of stellar noise on radial velocity measurements to be reduced to $, 6 pages, 4 figures, Supplemental Material included as ancillary file

Published
2019

22. Black-Hole Remnants from Black-Hole-Neutron-Star Mergers

Author

Sebastiano Bernuzzi, Nicola Giacobbo, Michela Mapelli, Francesco Pannarale, and Francesco Zappa

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Neutron stars, black holes, mergers and acquisitions, Binary black hole, 0103 physical sciences, Binary system, 010306 general physics, education, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Gravitational wave, Black hole, Stars, Neutron star, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Dimensionless quantity
Abstract

Observations of gravitational waves and their electromagnetic counterparts may soon uncover the existence of coalescing compact binary systems formed by a stellar-mass black hole and a neutron star. These mergers result in a remnant black hole, possibly surrounded by an accretion disk. The mass and spin of the remnant black hole depend on the properties of the coalescing binary. We construct a map from the binary components to the remnant black hole using a sample of numerical-relativity simulations of different mass ratios $q$, (anti)aligned dimensionless spins of the black hole ${a}_{\mathrm{BH}}$, and several neutron star equations of state. Given the binary total mass, the mass and spin of the remnant black hole can therefore be determined from the three parameters $(q,{a}_{\mathrm{BH}},\mathrm{\ensuremath{\Lambda}})$, where $\mathrm{\ensuremath{\Lambda}}$ is the tidal deformability of the neutron star. Our models also incorporate the binary black hole and test-mass limit cases and we discuss a simple extension for generic black-hole spins. We combine the remnant characterization with recent population synthesis simulations for various metallicities of the progenitor stars that generated the binary system. We predict that black-hole--neutron-star mergers produce a population of remnant black holes with masses distributed around $7\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ and $9\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$. For isotropic spin distributions, nonmassive accretion disks are favored: no bright electromagnetic counterparts are expected in such mergers.

Published
2019

23. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

Author

Eric H. Neilsen, Martin Crocce, A. Carnero Rosell, J. Carretero, Tamara M. Davis, Martin Becker, J. P. Dietrich, J. Gschwend, Richard G. McMahon, J. DeRose, L. F. Secco, D. J. Brout, Darren L. DePoy, W. G. Hartley, F. J. Castander, Richard G. Kron, P. Andersen, Lluís Galbany, A. Roodman, Tommaso Giannantonio, C. Davis, Gary Bernstein, Daniel Gruen, S. A. Uddin, Ofer Lahav, J. Lasker, Elisabeth Krause, J. Muir, Enrique Gaztanaga, N. E. Sommer, Rob Sharp, D. L. Hollowood, Risa H. Wechsler, D. W. Gerdes, A. G. Kim, V. Scarpine, S. Serrano, Richard Kessler, A. Campos, Eli S. Rykoff, Erin Sheldon, David Brooks, D. L. Burke, Geraint F. Lewis, David Goldstein, Carlos Solans Sanchez, Bonnie Zhang, Alex Drlica-Wagner, Marcos Lima, I. Sevilla-Noarbe, H. T. Diehl, P. Martini, M. Gatti, David Bacon, J. Calcino, David J. James, Joseph J. Mohr, J. Prat, Samuel Hinton, Bruce A. Bassett, J. P. Marriner, M. Carrasco Kind, Eric J. Baxter, G. Gutierrez, Dragan Huterer, Niall MacCrann, M. H.L.S. Wang, Bhuvnesh Jain, B. Flaugher, F. Andrade-Oliveira, Alistair R. Walker, Robert C. Nichol, Joe Zuntz, S. Kent, Pablo Fosalba, S. Allam, Ryan J. Foley, Robert A. Gruendl, Anais Möller, N. Kokron, E. Bertin, R. Cawthon, Ramon Miquel, Ashley J. Ross, Juan Estrada, M. S. Schubnell, P. Doel, Marcelle Soares-Santos, J. Annis, H. Camacho, Will J. Percival, N. Weaverdyck, A. Porredon, Karl Glazebrook, Enrique Fernández, Juan Garcia-Bellido, P. Challis, Huan Lin, Daniela Carollo, Jennifer L. Marshall, Brad E. Tucker, K. Honscheid, Brian Yanny, Shantanu Desai, N. Kuropatkin, E. Kasai, Rafe Schindler, Mathew Smith, A. Alarcon, M. Childress, C. Lidman, Felipe Menanteau, Daniel Scolnic, Gregory Tarle, L. N. da Costa, Tesla E. Jeltema, August E. Evrard, E. Swann, K. C. Chan, J. De Vicente, P. Lemos, Daniel Thomas, Brian Nord, Flavia Sobreira, Michael Troxel, Joshua A. Frieman, M. March, M. E. C. Swanson, Matt J. Jarvis, Kyler Kuehn, P. Vielzeuf, Yanxi Zhang, Tim Eifler, Keith Bechtol, Antonella Palmese, Rogerio Rosenfeld, M. A. G. Maia, J. K. Hoormann, Ricardo L. C. Ogando, Ben Hoyle, A. A. Plazas, A. K. Romer, C. B. D'Andrea, Edward Macaulay, Jack Elvin-Poole, S. Samuroff, R. C. Thomas, Eric Morganson, Jacobo Asorey, Yen-Chen Pan, Peter Melchior, N. Banik, Jonathan Blazek, Tenglin Li, Sarah Bridle, Scott Dodelson, Santiago Avila, Chihway Chang, Carlos E. Cunha, Jochen Weller, T. M. C. Abbott, Hiranya V. Peiris, E. J. Sanchez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Optical Astronomy Observatory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, University of Queensland, Dark Cosmology Centre, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, Korea Astronomy and Space Science Institute, University of Portsmouth, African Institute for Mathematical Sciences, South African Astronomical Observatory, University of Pennsylvania, LSST, University of Wisconsin-Madison, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, University College London, Stanford University, SLAC National Accelerator Laboratory, Universidade de São Paulo (USP), Carnegie Mellon University, Medioambientales y Tecnológicas (CIEMAT), Astrophysical Observatory of Turin, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Harvard-Smithsonian Center for Astrophysics, University of Chicago, University of Southampton, Observatório Nacional, Texas A and M University, 382 Via Pueblo Mall, IIT Hyderabad, Excellence Cluster Universe, Ludwig-Maximilians-Universität, Steward Observatory, California Institute of Technology, University of Michigan, Santa Cruz Institute for Particle Physics, University of Pittsburgh, Universidad Autonoma de Madrid, University of Cambridge, Ludwig-Maximilians Universität München, Swinburne University of Technology, ETH Zurich, Max Planck Institute for Extraterrestrial Physics, University of Namibia, Lawrence Berkeley National Laboratory, Macquarie University, University of Sydney, Australian National University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), National Astronomical Observatory of Japan, Academia Sinica, University of Waterloo, Perimeter Institute for Theoretical Physics, University of Sussex, Brookhaven National Laboratory, Physics Department, Universidade Estadual de Campinas (UNICAMP), Duke University, Observatories of the Carnegie Institution for Science, University of Edinburgh, Natl Opt Astron Observ, IEEC, CSIC, Fermilab Natl Accelerator Lab, Univ Queensland, Univ Copenhagen, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, Korea Astron & Space Sci Inst, Univ Portsmouth, African Inst Math Sci, South African Astron Observ, Univ Penn, Univ Wisconsin, Argonne Natl Lab, CNRS, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, UCL, Stanford Univ, SLAC Natl Accelerator Lab, Carnegie Mellon Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Astrophys Observ Turin, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Harvard Smithsonian Ctr Astrophys, Univ Chicago, Univ Southampton, Observ Nacl, Texas A&M Univ, Ludwig Maximilians Univ Munchen, Steward Observ, CALTECH, Univ Michigan, Santa Cruz Inst Particle Phys, Univ Pittsburgh, Univ Autonoma Madrid, Univ Cambridge, Swinburne Univ Technol, Swiss Fed Inst Technol, Max Planck Inst Extraterr Phys, Univ Namibia, Lawrence Berkeley Natl Lab, Macquarie Univ, Univ Sydney, Australian Natl Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, ARC Ctr Excellence All Sky Astrophys CAASTRO, Natl Astron Observ Japan, Acad Sinica, Univ Waterloo, Perimeter Inst Theoret Phys, Univ Sussex, Brookhaven Natl Lab, Brandeis Univ, Duke Univ, Observ Carnegie Inst Sci, and Univ Edinburgh

Subjects
bao, Cosmology and Nongalactic Astrophysics (astro-ph.CO), MATÉRIA ESCURA, media_common.quotation_subject, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, des, Gravitation and Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, supernova, galaxies, 0103 physical sciences, redshift distributions, 010306 general physics, QC, STFC, Weak gravitational lensing, media_common, Physics, Equation of state (cosmology), RCUK, Shape of the universe, Universe, 13. Climate action, astro-ph.CO, Dark energy, baryon acoustic-oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically--confirmed Type Ia supernova lightcurves; the baryon acoustic oscillation feature; weak gravitational lensing; and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, $w$, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding $w=-0.80^{+0.09}_{-0.11}$. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of $\Omega_b=0.069^{+0.009}_{-0.012}$ that is independent of early Universe measurements. These results demonstrate the potential power of large multi-probe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade., Comment: 8 pages, 2 figures; v3 matches version accepted by PRL

Published
2019

24. Strong Constraints on Fuzzy Dark Matter from Ultrafaint Dwarf Galaxy Eridanus II

Author

Jens C. Niemeyer and David J. E. Marsh

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Milky Way, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Gravitation, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Star cluster, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Bosonic field, Matter wave, Eridanus, 010306 general physics, Dwarf galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The fuzzy dark matter (FDM) model treats DM as a bosonic field with astrophysically large de Broglie wavelength. A striking feature of this model is $\mathcal{O}(1)$ fluctuations in the dark matter density on time scales which are shorter than the gravitational timescale. Including for the first time the effect of core oscillations, we demonstrate how such fluctuations lead to heating of star clusters, and thus an increase in their size over time. From the survival of the old star cluster in Eridanus II we infer $m_a\gtrsim 0.6\rightarrow 1\times 10^{-19}\text{ eV}$ within modelling uncertainty if FDM is to compose all of the DM, and derive constraints on the FDM fraction at lower masses. The subhalo mass function in the Milky Way implies $m_a\gtrsim 0.8\times 10^{-21}\text{ eV}$ to successfully form Eridanus II. The window between $10^{-21}\text{ eV}\lesssim m_a\lesssim 10^{-20}\text{ eV}$ is affected by narrow band resonances, and the limited applicability of the diffusion approximation. Some of this window may be consistent with observations of Eridanus II and more detailed investigations are required., 6 pages, 2 figures; v2 comments and clarifications added, matches version accepted for publication in PRL

Published
2019

25. Joining Bits and Pieces of Reionization History

Author

Hazra, Dhiraj Kumar, Paoletti, Daniela, Finelli, Fabio, Smoot, George F., AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Paris Centre for Cosmological Physics (PCCP), Université Paris Diderot - Paris 7 (UPD7), ITA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, General Physics and Astronomy, Cosmic variance, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitation and Astrophysics, 01 natural sciences, CMB cold spot, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, symbols.namesake, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, symbols, Planck, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Reionization, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Cosmic Microwave Background temperature and polarization anisotropies from Planck have estimated a lower value of the optical depth to reionization ($\tau$) compared to WMAP. A significant period in the reionization history would then fall within $6, Comment: V1: 7 pages, 4 figures and 1 table; V2: Updated to Planck 2018 and recent astrophysical data

Published
2019

26. Unique Fingerprints of Alternatives to Inflation in the Primordial Power Spectrum

Author

Abraham Loeb, Zhong-Zhi Xianyu, and Xingang Chen

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Non-Gaussianity, 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, Quantum fluctuation, Scale factor (cosmology), media_common, Physics, Inflation (cosmology), Spectral density, Function (mathematics), Universe, Ekpyrotic universe, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Massive fields in the primordial universe function as standard clocks and imprint clock signals in the density perturbations that directly record the scale factor of the primordial universe as a function of time, a(t). A measurement of such signals would identify the specific scenario of the primordial universe in a model-independent fashion. In this Letter, we introduce a new mechanism through which quantum fluctuations of massive fields function as standard clocks. The clock signals appear as scale-dependent oscillatory signals in the power spectrum of alternative scenarios to inflation., 8 pages; v3, LSS forecast added and other minor revisions. A slightly shortened version will appear in PRL

Published
2019

27. Voyager 1 e± Further Constrain Primordial Black Holes as Dark Matter

Author

Marco Cirelli, Mathieu Boudaud, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
electron, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, Cosmic ray, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Electron, Astrophysics, Gravitation and Astrophysics, 01 natural sciences, mass spectrum, High Energy Physics - Phenomenology (hep-ph), magnetic field: solar, 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Mass distribution, radiation: Hawking, Galaxy, High Energy Physics - Phenomenology, gravitation, cosmic radiation, positron, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Heliosphere, Astrophysics - Cosmology and Nongalactic Astrophysics, Hawking radiation
Abstract

Primordial Black Holes (PBHs) with a mass $M \lesssim {10^{17}}$g are expected to inject sub-GeV electrons and positrons in the Galaxy via Hawking radiation. These cosmic rays are shielded by the solar magnetic field for Earth-bound detectors, but not for Voyager-1, which is now beyond the heliopause. We use its data to constrain the fraction of PBHs to the dark matter in the Galaxy, finding that PBHs with $M, v2: small comments and references added, gamma-ray limits corrected in Fig. 2, matches journal version

Published
2019

28. Unresolved Gamma-Ray Sky through its Angular Power Spectrum

Author

Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., ORIENTI, Monica, Orlando, E., Palatiello, M., Paliya, V. S., PERSIC, Massimo, Paneque, D., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, O., Reimer, A., Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Thayer, J. B., Torres, D. F., Tibaldo, L., Troja, E., Venters, T. M., Vianello, G., Wood, K., Yassine, M., Zaharijas, G., Ammazzalorso, S., Fornengo, N., Regis, M., Bregeon, J., Fermi-LAT Collaboration, Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., CARAVEO, PATRIZIA, Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Costantin, D., Cuoco, A., Cutini, S., D'AMMANDO, FILIPPO, de la Torre Luque, P., de Palma, F., Desai, A., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Fana Dirirsa, F., Favuzzi, C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., GIROLETTI, MARCELLO, Green, D., Grenier, I. A., Guillemot, L., Guiriec, S., Horan, D., Jóhannesson, G., Kuss, M., Larsson, S., Latronico, L., Li, J., Liodakis, I., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Mereu, I., Michelson, P. F., Mitthumsiri, W., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), ITA, Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Costantin, D., Cuoco, A., Cutini, S., D'Ammando, F., de la Torre Luque, P., de Palma, F., Desai, A., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Fana Dirirsa, F., Favuzzi, C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guillemot, L., Guiriec, S., Horan, D., Jóhannesson, G., Kuss, M., Larsson, S., Latronico, L., Li, J., Liodakis, I., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Mereu, I., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Thayer, J. B., Tibaldo, L., Torres, D. F., Troja, E., Venters, T. M., Vianello, G., Wood, K., Yassine, M., Zaharijas, G., Ammazzalorso, S., Fornengo, N., Regis, M., and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
noise, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gamma ray: background, High-energy astronomy, High-energy Astrophysics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Gravitation and Astrophysics, 01 natural sciences, GLAST, law.invention, Telescope, Physics and Astronomy (all), High Energy Physics - Phenomenology (hep-ph), law, 0103 physical sciences, ddc:530, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, 010308 nuclear & particles physics, fluctuation, photon, Physics and Astronomy, Spectral density, sensitivity, High Energy Physics - Phenomenology, Amplitude, Sky, [SDU]Sciences of the Universe [physics], power spectrum: angular dependence, energy spectrum: anisotropy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The gamma-ray sky has been observed with unprecedented accuracy in the last decade by the Fermi large area telescope (LAT), allowing us to resolve and understand the high-energy Universe. The nature of the remaining unresolved emission (unresolved gamma-ray background, UGRB) below the LAT source detection threshold can be uncovered by characterizing the amplitude and angular scale of the UGRB fluctuation field. This work presents a measurement of the UGRB autocorrelation angular power spectrum based on eight years of Fermi LAT Pass 8 data products. The analysis is designed to be robust against contamination from resolved sources and noise systematics. The sensitivity to subthreshold sources is greatly enhanced with respect to previous measurements. We find evidence (with $\sim$3.7$\sigma$ significance) that the scenario in which two classes of sources contribute to the UGRB signal is favored over a single class. A double power law with exponential cutoff can explain the anisotropy energy spectrum well, with photon indices of the two populations being 2.55 $\pm$ 0.23 and 1.86 $\pm$ 0.15., Comment: 8 + 12 (SOM) pages, Contact author: Michela Negro (michela.negro@to.infn.it). (Typos in Tab. VII in previous versions)

Published
2018

29. Limits on Stellar-Mass Compact Objects as Dark Matter from Gravitational Lensing of Type Ia Supernovae

Author

Miguel Zumalacárregui, Uroš Seljak, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, MACHO, halo, General Physics and Astronomy, Primordial black hole, Astrophysics, 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, Mathematical Sciences, Einstein radius, High Energy Physics - Phenomenology (hep-ph), Engineering, Astrophysics::Solar and Stellar Astrophysics, LIGO, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, hep-ph, High Energy Physics - Phenomenology, finite size, non-Gaussianity, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, black hole: primordial, signature, Astrophysics - Cosmology and Nongalactic Astrophysics, General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, gr-qc, media_common.quotation_subject, Dark matter, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), supernova: luminosity, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitation and Astrophysics, gravitation: lens, 0103 physical sciences, structure, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Gravitational wave, Universe, Gravitational lens, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The nature of dark matter (DM) remains unknown despite very precise knowledge of its abundance in the universe. An alternative to new elementary particles postulates DM as made of macroscopic compact halo objects (MACHO) such as black holes formed in the very early universe. Stellar-mass primordial black holes (PBHs) are subject to less robust constraints than other mass ranges and might be connected to gravitational-wave signals detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO). New methods are therefore necessary to constrain the viability of compact objects as a DM candidate. Here we report bounds on the abundance of compact objects from gravitational lensing of type Ia supernovae (SNe). Current SNe datasets constrain compact objects to represent less than 35.2% (Joint Lightcurve Analisis) and 37.2% (Union 2.1) of the total matter content in the universe, at 95% confidence-level. The results are valid for masses larger than $\sim 0.01M_\odot$ (solar-masses), limited by the size SNe relative to the lens Einstein radius. We demonstrate the mass range of the constraints by computing magnification probabilities for realistic SNe sizes and different values of the PBH mass. Our bounds are sensitive to the total abundance of compact objects with $M \lesssim 0.01M_\odot$ and complementary to other observational tests. These results are robust against cosmological parameters, outlier rejection, correlated noise and selection bias. PBHs and other MACHOs are therefore ruled out as the dominant form of DM for objects associated to LIGO gravitational wave detections. These bounds constrain early-universe models that predict stellar-mass PBH production and strengthen the case for lighter forms of DM, including new elementary particles., 16 pages, 9 figures. Discussion on finite SNe size and outliers expanded. Version accepted for publication in PRL

Published
2018

30. 21-cm Fluctuations from Charged Dark Matter

Author

Abraham Loeb, Julian B. Muñoz, and Cora Dvorkin

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, 010308 nuclear & particles physics, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Observable, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Baryon, High Energy Physics - Phenomenology, Stars, High Energy Physics - Phenomenology (hep-ph), Amplitude, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Adiabatic process, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Reionization, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The epoch of the formation of the first stars, known as the cosmic dawn, has emerged as a new arena in the search for dark matter. In particular, the first claimed 21-cm detection exhibits a deeper global absorption feature than expected, which could be caused by a low baryonic temperature, and has been interpreted as a sign for electromagnetic interactions between baryons and dark matter. This hypothesis has a striking prediction: large temperature anisotropies sourced by the velocity-dependent cooling of the baryons. However, in order to remain consistent with the rest of cosmological observations, only part of the dark matter is allowed to be charged, and thus interactive. Here we compute, for the first time, the 21-cm fluctuations caused by a charged subcomponent of the dark matter, including both the pre- and post-recombination evolution of all fluids. We find that, for the same parameters that can explain the anomalous 21-cm absorption signal, any percent-level fraction of charged dark matter would source novel 21-cm fluctuations with a unique acoustic spectrum, and with an amplitude above any other known effects. These fluctuations are uncorrelated with the usual adiabatic anisotropies, and would be observable at high significance with interferometers such as LOFAR and HERA, thus providing a novel probe of dark matter at cosmic dawn., Comment: 6 pages, 4 figures. Updated to match PRL accepted version

Published
2018

31. Predictions for the Sky-Averaged Depth of the 21 cm Absorption Signal at High Redshift in Cosmologies with and without Nonbaryonic Cold Dark Matter

Author

Stacy S. McGaugh

Subjects
Physics, Gravity (chemistry), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, media_common.quotation_subject, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Universe, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Path length, Sky, 0103 physical sciences, 010306 general physics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

We consider the 21cm absorption signal expected at high redshift in cosmologies with and without non-baryonic cold dark matter. The expansion of the early universe decelerates strongly with dark matter, but approximately coasts without it. This results in a different path length across the epochs when absorption is expected, with the consequence that the absorption is predicted to be a factor of $\sim 2$ greater without dark matter than with it. Observation of such a signal would motivate consideration of extended theories of gravity in lieu of dark matter., Comment: Accepted for publication in Phys. Rev. Letters. 9 pages (4 of which are bibliography), 1 figure. Model data available at http://astroweb.case.edu/ssm/models/

Published
2018

32. Severely Constraining Dark-Matter Interpretations of the 21-cm Anomaly

Author

Asher Berlin, Samuel D. McDermott, Gordan Krnjaic, and Dan Hooper

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, media_common.quotation_subject, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, 01 natural sciences, Electric charge, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gauge boson, 010308 nuclear & particles physics, Astrophysics - Astrophysics of Galaxies, Universe, Redshift, Hidden sector, High Energy Physics - Phenomenology, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The EDGES Collaboration has recently reported the detection of a stronger-than-expected absorption feature in the global 21-cm spectrum, centered at a frequency corresponding to a redshift of z ~ 17. This observation has been interpreted as evidence that the gas was cooled during this era as a result of scattering with dark matter. In this study, we explore this possibility, applying constraints from the cosmic microwave background, light element abundances, Supernova 1987A, and a variety of laboratory experiments. After taking these constraints into account, we find that the vast majority of the parameter space capable of generating the observed 21-cm signal is ruled out. The only range of models that remains viable is that in which a small fraction, ~ 0.3-2%, of the dark matter consists of particles with a mass of ~ 10-80 MeV and which couple to the photon through a small electric charge, epsilon ~ 10^{-6}-10^{-4}. Furthermore, in order to avoid being overproduced in the early universe, such models must be supplemented with an additional depletion mechanism, such as annihilations through a L_{\mu}-L_{\tau} gauge boson or annihilations to a pair of rapidly decaying hidden sector scalars., Comment: 7 pgs, 3

Published
2018

33. Dark Matter Equation of State through Cosmic History

Author

Michael Kopp, S. Ilić, Constantinos Skordis, and Daniel B. Thomas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Equation of state (cosmology), Cosmic microwave background, Dark matter, Cosmic background radiation, FOS: Physical sciences, General Physics and Astronomy, Inverse, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Omega, Redshift, Baryon, 13. Climate action, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Cold Dark Matter (CDM) is a crucial constituent of the current concordance cosmological model. Having a vanishing equation of state (EoS), its energy density scales with the inverse cosmic volume and is thus uniquely described by a single number, its present abundance. We test the inverse cosmic volume law for Dark Matter (DM) by allowing its EoS to vary independently in eight redshift bins in the range $z=10^5$ and $z=0$. We use the latest measurements of the Cosmic Microwave Background radiation from the Planck satellite and supplement them with Baryon Acoustic Oscillation (BAO) data from the 6dF and SDSS-III BOSS surveys, and with the Hubble Space Telescope (HST) key project data. We find no evidence for nonzero EoS in any of the eight redshift bins. With Planck data alone, the DM abundance is most strongly constrained around matter-radiation equality $\omega^{\rm eq}_g = 0.1193^{+0.0036}_{-0.0035}$ (95% c.l.), whereas its present day value is more weakly constrained $\omega^{(0)}_g = 0.16^{+0.12}_{-0.10}$ (95% c.l.). Adding BAO or HST data does not significantly change the $\omega^{\rm eq}_g$ constraint, while $\omega^{(0)}_g$ tightens to $0.160^{+0.069}_{-0.065} $ (95% c.l.) and $0.124^{+0.081}_{-0.067}$ (95% c.l.) respectively. Our results constrain for the first time the level of "coldness" required of the DM across various cosmological epochs and show that the DM abundance is strictly positive at all times., Comment: 6 pages, 4 figures, changed color scheme for figures

Published
2018

34. Primordial Anisotropies in the Gravitational Wave Background from Cosmological Phase Transitions

Author

Yuhsin Tsai, Raman Sundrum, Anson Hook, and Michael Geller

Subjects
Inflation (cosmology), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, Primordial fluctuations, media_common.quotation_subject, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, General Physics and Astronomy, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Universe, Gravitational wave background, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

Phase transitions in the early universe can readily create an observable stochastic gravitational wave background. We show that such a background necessarily contains anisotropies analogous to those of the cosmic microwave background (CMB) of photons, and that these too may be within reach of proposed gravitational wave detectors. Correlations within the gravitational wave anisotropies and their cross-correlations with the CMB can provide new insights into the mechanism underlying primordial fluctuations, such as multi-field inflation, as well as reveal the existence of non-standard ``hidden sectors" of particle physics in earlier eras., Comment: 6 pages, 2 figures, match the published PRL version

Published
2018

35. Measuring the Hubble Constant with Neutron Star Black Hole Mergers

Author

Hsin-Yu Chen and Salvatore Vitale

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Orbital plane, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, 010303 astronomy & astrophysics, Luminosity distance, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Mass ratio, Galaxy, LIGO, Redshift, Black hole, Neutron star, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The detection of GW170817 and the identification of its host galaxy have allowed for the first standard-siren measurement of the Hubble constant, with an uncertainty of $\sim 14\%$. As more detections of binary neutron stars with redshift measurement are made, the uncertainty will shrink. The dominating factors will be the number of joint detections and the uncertainty on the luminosity distance of each event. Neutron star black hole mergers are also promising sources for advanced LIGO and Virgo. If the black hole spin induces precession of the orbital plane, the degeneracy between luminosity distance and the orbital inclination is broken, leading to a much better distance measurement. In addition neutron star black hole sources are observable to larger distances, owing to their higher mass. Neutron star black holes could also emit electromagnetic radiation: depending on the black hole spin and on the mass ratio, the neutron star can be tidally disrupted resulting in electromagnetic emission. We quantify the distance uncertainty for a wide range of black hole mass, spin and orientations and find that the 1-$\sigma$ statistical uncertainty can be up to a factor of $\sim 10$ better than for a non-spinning binary neutron star merger with the same signal-to-noise ratio. The better distance measurement, the larger gravitational-wave detectable volume, and the potentially bright electromagnetic emission, imply that spinning black hole neutron star binaries can be the optimal standard siren sources as long as their astrophysical rate is larger than $O(10)$ Gpc$^{-3}$yr$^{-1}$, a value allowed by current astrophysical constraints., Comment: Updated a few leftovers from working version, typos. Closely matches version published in PRL - post-proofs

Published
2018

36. Self-Heating Dark Matter via Semiannihilation

Author

Ayuki Kamada, Toyokazu Sekiguchi, Hee Jung Kim, and Hyungjin Kim

Subjects
Elastic scattering, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Structure formation, 010308 nuclear & particles physics, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Kinetic energy, 01 natural sciences, Redshift, Standard Model, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Particle, Halo, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The freeze-out of dark matter (DM) depends on the evolution of the DM temperature. The DM temperature does not have to follow the standard model one, when the elastic scattering is not sufficient to maintain the kinetic equilibrium. We study the temperature evolution of the semi-annihilating DM, where a pair of the DM particles annihilate into one DM particle and another particle coupled to the standard model sector. We find that the kinetic equilibrium is maintained solely via semi-annihilation until the last stage of the freeze-out. After the freeze-out, semi-annihilation converts the mass deficit to the kinetic energy of DM, which leads to non-trivial evolution of the DM temperature. We argue that the DM temperature redshifts like radiation as long as the DM self-interaction is efficient. We dub this novel temperature evolution as self-heating. Notably, the structure formation is suppressed at subgalactic scales like keV-scale warm DM but with GeV-scale self-heating DM if the self-heating lasts roughly until the matter-radiation equality. The long duration of the self-heating requires the large self-scattering cross section, which in turn flattens the DM density profile in inner halos. Consequently, self-heating DM can be a unified solution to apparent failures of cold DM to reproduce the observed subgalactic scale structure of the Universe., 6 pages, 4 figures. v2: discussed improved, matches published version

Published
2018

37. Bounds on Dark-Matter Annihilations from 21-cm Data

Author

Paolo Panci, Guido D'Amico, and Alessandro Strumia

Subjects
Physics, Astrophysics and Astronomy, Range (particle radiation), Annihilation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Dark matter, General Physics and Astronomy, FOS: Physical sciences, hep-ph, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Physics and Astronomy (all), High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Intergalactic medium, 0103 physical sciences, astro-ph.CO, 010306 general physics, Absorption (electromagnetic radiation), Particle Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The observation of an absorption feature in the 21 cm spectrum at redshift $z\approx 17$ implies bounds on Dark Matter annihilations for a broad range of masses, given that significant heating of the intergalactic medium would have erased such feature. The resulting bounds on the DM annihilation cross sections are comparable to the strongest ones from all other observables., 8 pages. v2: improved treatment of energy deposition

Published
2018
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38. Maximum Redshift of Gravitational Wave Merger Events

Author

Savvas M. Koushiappas and Abraham Loeb

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, General Physics and Astronomy, Astronomy, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Redshift, 0103 physical sciences, Probability distribution, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics - Cosmology and Nongalactic Astrophysics, Gravitational redshift
Abstract

Future generation of gravitational wave detectors will have the sensitivity to detect gravitational wave events at redshifts far beyond any detectable electromagnetic sources. We show that if the observed event rate is greater than one event per year at redshifts z > 40, then the probability distribution of primordial density fluctuations must be significantly non-Gaussian or the events originate from primordial black holes. The nature of the excess events can be determined from the redshift distribution of the merger rate., 5 pages, 3 figures, Replaced with version accepted for publication in Physical Review Letters

Published
2017

39. Fourth Exception in the Calculation of Relic Abundances

Author

Duccio Pappadopulo, Joshua T. Ruderman, and R. T. D’Agnolo

Subjects
Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Hot dark matter, Dark matter, Scalar field dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Baryonic dark matter, 0103 physical sciences, Mixed dark matter, Warm dark matter, 010306 general physics, Light dark matter, Dark fluid, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We propose that the dark matter abundance is set by the decoupling of inelastic scattering instead of annihilations. This coscattering mechanism is generically realized if dark matter scatters against states of comparable mass from the thermal bath. Coscattering points to dark matter that is exponentially lighter than the weak scale and has a suppressed annihilation rate, avoiding stringent constraints from indirect detection. Dark matter upscatters into states whose late decays can lead to observable distortions to the blackbody spectrum of the cosmic microwave background., Comment: 8 pages, 6 figures. V3: figure added

Published
2017

40. Primordial Black Holes and r -Process Nucleosynthesis

Author

Alexander Kusenko, Volodymyr Takhistov, and George M. Fuller

Subjects
General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Compact star, 01 natural sciences, Mathematical Sciences, High Energy Physics - Phenomenology (hep-ph), Engineering, Nucleosynthesis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, 010308 nuclear & particles physics, Center (category theory), Astronomy, hep-ph, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, Neutron star, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, astro-ph.CO, r-process, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We show that some or all of the inventory of $r$-process nucleosynthesis can be produced in interactions of primordial black holes (PBHs) with neutron stars (NSs) if PBHs with masses ${10}^{-14}\,{\rm M}_\odot < {\rm M}_{\rm PBH} < {10}^{-8}\,{\rm M}_\odot$ make up a few percent or more of the dark matter. A PBH captured by a neutron star (NS) sinks to the center of the NS and consumes it from the inside. When this occurs in a rotating millisecond-period NS, the resulting spin-up ejects $\sim 0.1-0.5\,{\rm M}_{\odot}$ of relatively cold neutron-rich material. This ejection process and the accompanying decompression and decay of nuclear matter can produce electromagnetic transients, such as a kilonova-type afterglow and fast radio bursts. These transients are not accompanied by significant gravitational radiation or neutrinos, allowing such events to be differentiated from compact object mergers occurring within the distance sensitivity limits of gravitational wave observatories. The PBH-NS destruction scenario is consistent with pulsar and NS statistics, the dark matter content and spatial distributions in the Galaxy and Ultra Faint Dwarfs (UFD), as well as with the $r$-process content and evolution histories in these sites. Ejected matter is heated by beta decay, which leads to emission of positrons in an amount consistent with the observed 511-keV line from the Galactic Center., 6 pages + 3 page supplement, 3 figures; matches published version

Published
2017

41. Gravitational Waves from Oscillons with Cuspy Potentials

Author

Zong-Kuan Guo, Gary Shiu, Rong-Gen Cai, and Jing Liu

Subjects
Physics, Inflation (cosmology), Cusp (singularity), High Energy Physics - Theory, Oscillon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Inflaton, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), 0103 physical sciences, 010306 general physics, Characteristic energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the production of gravitational waves during oscillations of the inflaton around the minimum of a cuspy potential after inflation. We find that a cusp in the potential can trigger copious oscillon formation, which sources a characteristic energy spectrum of gravitational waves with double peaks. The discovery of such a double-peak spectrum could test the underlying inflationary physics., Comment: 5 pages,4 figures Accepted for publication in Phys. Rev. Lett

Published
2017

42. Probing Primordial Black Hole Dark Matter with Gravitational Waves

Author

Ely D. Kovetz

Subjects
High Energy Physics - Theory, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Hot dark matter, Dark matter, Scalar field dark matter, FOS: Physical sciences, General Physics and Astronomy, Astronomy, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Theory (hep-th), 0103 physical sciences, Mixed dark matter, Warm dark matter, 010306 general physics, Light dark matter, Dark fluid, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Primordial black holes (PBHs) have long been suggested as a candidate for making up some or all of the dark matter in the Universe. Most of the theoretically possible mass range for PBH dark matter has been ruled out with various null observations of expected signatures of their interaction with standard astrophysical objects. However, current constraints are significantly less robust in the 20 M_sun < M_PBH < 100 M_sun mass window, which has received much attention recently, following the detection of merging black holes with estimated masses of ~30 M_sun by LIGO and the suggestion that these could be black holes formed in the early Universe. We consider the potential of advanced LIGO (aLIGO) operating at design sensitivity to probe this mass range by looking for peaks in the mass spectrum of detected events. To quantify the background, which is due to black holes that are formed from dying stars, we model the shape of the stellar-black-hole mass function and calibrate its amplitude to match the O1 results. Adopting very conservative assumptions about the PBH and stellar-black-hole merger rates, we show that ~5 years of aLIGO data can be used to detect a contribution of >20 M_sun PBHs to dark matter down to f_PBH99.9% confidence level. Combined with other probes that already suggest tension with f_PBH=1, the obtainable independent limits from aLIGO will thus enable a firm test of the scenario that PBHs make up all of dark matter., 5 pages, 2 figures; expanded discussion of uncertainties; matches publication in PRL

Published
2017

43. Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Author

John A. Clark, Ben Farr, A. L. Stuver, W. S. Kim, B. C. Stephens, Christophe Collette, Ho-Gyu Lee, J. P. Zendri, C. J. Perez, Adam A. Miller, S. Appert, Soumi De, N. Gehrels, Marek Szczepanczyk, A. Giazotto, C. Bradaschia, P. Oppermann, Ik Siong Heng, P. Shawhan, I. Ferrante, P. Charlton, Kejia Lee, Yongjung Kim, Peter Weßels, Zifan Zhou, I. A. Bilenko, David J. Ottaway, P. Astone, Larne Pekowsky, C. F. Da Silva Costa, W. Z. Korth, David Jones, Marco Cavaglia, A. W. Heptonstall, Vivien Raymond, Peter R. Saulson, L. Cerboni Baiardi, Terry G. McRae, L. G. Prokhorov, A. Paoli, Michael L. Gorodetsky, T. Westphal, Ryan Lynch, Alejandro Bohé, K. Mason, E. C. Ferreira, Sanjeev Dhurandhar, Denis Martynov, Marco Bazzan, W. Parker, V. Dolique, Simon Stevenson, A. K. Lenon, Archisman Ghosh, Hartmut Grote, Xavier Siemens, W. A. Campbell, R. C. Devine, S. Penn, L. Pinard, Federico Ferrini, K. Venkateswara, D. Ugolini, V. Kondrashov, S. L. Danilishin, Arunava Mukherjee, D. Rosińska, E. J. Fauchon-Jones, M. Lormand, Yuri Levin, G. Losurdo, David H. Shoemaker, S. Karki, T. J. Cullen, G. Vajente, L. Trozzo, Albert Lazzarini, T. B. Edo, D. Verkindt, A. Viceré, Y. Minenkov, Patrice Hello, Robert Stone, A. Di Virgilio, A. R. Williamson, M. Prijatelj, B. D. Lackey, Neil J. Cornish, S. M. Gaebel, Yi Chen, J. Warner, H. Rew, K. S. Karvinen, H. Wittel, Sascha Husa, G. Venugopalan, Meng Wang, Albrecht Rüdiger, Xing-Jiang Zhu, D.B. DeBra, S. G. Schwalbe, M. Phelps, R. Passaquieti, Alexander H. Nitz, D. Schuette, C. Rajan, B. Day, Jochen Schmidt, M. T. Hartman, M. Pichot, A. S. Biscoveanu, B. J. J. Slagmolen, F. Paoletti, S. Ascenzi, J. M. Newport, T. Theeg, Maximiliano Isi, G. L. Mansell, Kipp Cannon, M. Steinke, Samaya Nissanke, Lionel Martellini, M. E. N. Normandin, G. D. Meadors, X. Guo, Mauro Tonelli, K. Siellez, G. A. Prodi, R. DeSalvo, Sung-Po Chao, R. Tso, P. J. Sutton, K. A. Thorne, Riccardo Bassiri, H. J. Bulten, F. J. Raab, C. C. Buchanan, Magnus Manske, Alessandro Bertolini, T. Etzel, I. Dorrington, E. Maros, J. H. Romie, Patrick M. Koch, V. Dattilo, P. Popolizio, Koji Arai, R. Douglas, S. Ghonge, Tejinder Kaur, Edwin J. Son, D. Passuello, O. V. Palashov, Sean T. McWilliams, F. Piergiovanni, Chang-Hwan Lee, J. J. Hacker, E. J. Sanchez, R. De Rosa, Piotr Jaranowski, Peter Fritschel, D. H. Reitze, C. S. Unnikrishnan, P. J. Veitch, F. Mezzani, Archana Pai, S. Márka, N. Mukund, L. R. Cominsky, M. Masso-Reid, Tomasz Bulik, Laleh Sadeghian, V. P. Mitrofanov, Roy Williams, Mairi Sakellariadou, G. Pillant, R. Gustafson, M. Davier, P. Kumar, Kenneth A. Strain, Jimin George, M. Sieniawska, B. R. Hall, Richard J. Oram, M. C. Tringali, Collin D. Capano, J. Birch, I. Nardecchia, Jordan Camp, Hyun Lee, J. Page, J. Calderón Bustillo, Lloyd Paul Aiello, B. C. Pant, Gregory Ashton, S. Mastrogiovanni, Samuele Cortese, R. K. Lanza, J. L. Willis, Stefan Hild, Y. Ma, E. Coccia, Fabio Marchesoni, M. E. Zucker, C. Graef, B. A. Weaver, N. Letendre, François Bondu, B. O'Reilly, W. Del Pozzo, P. F. Cohadon, G. Wu, S. Raja, H. Heitmann, Bala R. Iyer, S. McCormick, P. Ruggi, Tenglin Li, C. Aulbert, R. Cavalieri, I. Kowalska, J. McIver, Adam A. Libson, A. Mullavey, T. J. N. Nelson, P. Puppo, A. W. Muir, Howard Pan, Aaron Buikema, J. G. Rollins, P. A. Altin, C. C. Wipf, E. J. King, S. E. Strigin, M. Turconi, L.-W. Wei, Carlos Cepeda, Alvin J. K. Chua, Robert J. McCarthy, A. K. Srivastava, A. E. Pace, A. Grado, T. Sadecki, Eric Oelker, T. Denker, S. Grunewald, E. G. Thomas, A. Basti, S. B. Coughlin, Peter Aufmuth, N. Indik, C. Messenger, Marie-Anne Bizouard, Christopher P. L. Berry, A. D. Silva, M. J. Cowart, F. Jiménez-Forteza, Sourav Ghosh, Imre Bartos, J. Zweizig, G. Wang, V. Malvezzi, T. Dal Canton, S. Qiu, Linqing Wen, Jessica Steinlechner, A. Neunzert, T. Chmiel, M. Heurs, W. D. Vousden, Ryan N. Lang, Jiayi Qin, A. Singer, S. G. Crowder, M. Razzano, L. Matone, Kris Ryan, E. A. Quintero, E. L. Merilh, Z. Frei, László Á. Gergely, E. A. Huerta, A. Pele, S. Mitra, Sebastian Steinlechner, Xiaohui Fan, Richard O'Shaughnessy, B. Barr, A. Staley, Laura Sampson, V. Sequino, S. Caride, D. Tao, D. C. Vander-Hyde, Z. Tornasi, Nergis Mavalvala, E. O. Lebigot, E. Rhoades, S. Schlassa, Jerome Degallaix, J.-D. Fournier, Philip F. Hopkins, S. Jawahar, R. Goetz, Tarun Souradeep, C. Casentini, F. Marion, N. Leroy, Carl-Johan Haster, L. Rolland, Rana X. Adhikari, J-Y. Vinet, M. Lorenzini, B. Klein, Reed Essick, R. Everett, Anne E. B. Nielsen, Haocun Yu, James Healy, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, S. Kandhasamy, M. Rakhmanov, Tristan Briant, B. Sorazu, V. Re, M. Kasprzack, E. A. Houston, I. Di Palma, P. Brockill, M. Vardaro, Sebastian Khan, I. Fiori, G. Vedovato, Matthew Evans, D. B. Kozak, Fabrizio Barone, M. Mohan, T. D. Creighton, Enrico Calloni, G. Traylor, Thomas Corbitt, C. Vorvick, L. Salconi, C. A. Costa, M. Boer, J. B. Kanner, G. Debreczeni, T. Di Girolamo, N. Man, F. Garufi, L. Sun, H. Fong, N. M. Brown, K. Haughian, P. J. King, Michael Pürrer, E. Schmidt, R. Inta, E. Schreiber, B. Machenschalk, F. Donovan, S. Klimenko, M. J. Yap, D. Bersanetti, F. Martelli, Serena Vinciguerra, R. Pedurand, Benno Willke, C. Palomba, Aaron Viets, H. Fehrmann, Martin M. Fejer, J. R. Smith, R. Bork, Vuk Mandic, A. Kutynia, T. T. Nguyen, W. Katzman, F. Robinet, M. van Beuzekom, M. K. Gupta, M. S. Shahriar, Andrea Chincarini, A. K. Zadrożny, A. Avila-Alvarez, K. Gill, C. Cahillane, Joey Shapiro Key, J. R. Sanders, D. Talukder, Laura Cadonati, G. Kang, A. Pal-Singh, C. C. Yancey, Walter Winkler, J. Hennig, A. S. Markosyan, V. Gayathri, David A. Williams, I. W. Harry, R. Kennedy, Benjamin William Allen, Karan Jani, Abhirup Ghosh, Karsten Danzmann, S. Walsh, Miriam Cabero, E. Coughlin, W. G. Anderson, M. Neri, J. A. Giaime, Matthew Abernathy, Geoffrey Lovelace, Hsiao-Wen Chen, Tyson Littenberg, Alessandra Buonanno, Hua Wang, R. Metzdorff, G. Cella, Giacomo Ciani, M. Punturo, D. Huet, S. H. Huttner, Slawomir Gras, B. P. Abbott, J.-M. Isac, T. Z. Summerscales, E. K. Gustafson, S. Kaufer, Rainer Weiss, Chandra Kant Mishra, Harald Lück, L. Kleybolte, R. Bhandare, L. van der Schaaf, S. A. Pai, Cody Messick, N. Mazumder, F. Ricci, G. Mendell, R. W. P. Drever, S. Vass, S. Babak, M. Bejger, F. Cleva, Leopoldo Milano, A. Perreca, M. Cho, Susan M. Scott, Andrew Melatos, A. Masserot, R. Kirchhoff, B. L. Pearlstone, L. Rei, Gijs Nelemans, W. W. Johnson, E. A. Muñiz, C. Krämer, Robinjeet Singh, R. Coyne, Fabrice Matichard, D. Fiorucci, A. R. Wade, M. Yvert, T. D. Abbott, O. Puncken, V. Fafone, Britton D. Smith, A. L. Lombardi, P. T. Baker, A. C. Green, R. Mittleman, G. Kuehn, C. M. Mow-Lowry, Sergey P. Vyatchanin, M. Fays, Mark Hannam, Kendall Ackley, Y. Wang, David Blair, Zoheyr Doctor, M. Nery, Ettore Majorana, R. L. Savage, M. Gosselin, G. Gaur, S. C. McGuire, J. F. Read, A. S. Bell, S. Di Pace, Daniele Trifirò, C. R. Billman, Chad Hanna, J. Oberling, M. Laxen, Fausto Acernese, F. Magaña-Sandoval, J. Trinastic, A. Glaefke, A. Di Lieto, N. Kijbunchoo, E. E. Cowan, J. D. Romano, B. F. Whiting, E. D. Hall, P. Ehrens, Jolien D. E. Creighton, T. Isogai, Madeline Wade, J. Casanueva Diaz, P. Leaci, A. Colla, F. Y. Khalili, Nelson Christensen, L. Naticchioni, Salvatore Vitale, S. J. Chamberlin, D. Nolting, A. Mytidis, Swetha Bhagwat, William Yam, L. Wallace, Mi Zhang, P. Schale, C. Gray, G. H. Ogin, A. Królak, T. J. Shaffer, C. Van Den Broeck, M. Vasúth, M. Mantovani, Jonathan Cripe, K. V. Tokmakov, V. Germain, R. Frey, Duncan Meacher, M. Bitossi, G. Bergmann, Sylvia J. Zhu, S. Brunett, I. Maksimovic, D. V. Voss, R. L. Ward, M. Ducrot, Rebecca Fisher, A. L. Urban, M. Was, Kazuhiro Agatsuma, B. Shapiro, J. Eichholz, K. Holt, F. Nocera, J. C. Barayoga, Richard J. Abbott, H. Vocca, Eugeniy E. Mikhailov, C. Zhao, Alicia M. Sintes, T. Zhang, D. Barker, K. Wette, A. Bisht, G. Hemming, S. Koley, John J. Oh, Thibaut Jacqmin, C. I. Torrie, N. Straniero, D. R. Ingram, M. Korobko, F. Frasconi, Chunglee Kim, V. Sandberg, M. Saleem, M. Oliver, Douglas Davis, H. Fair, A. F. Brooks, Andrea Taracchini, B. U. Gadre, G. P. Newton, M. Fyffe, Sebastien Biscans, G. McIntyre, J. V. van Heijningen, Gabriela Gonzalez, S. M. Koehlenbeck, A. Cumming, Rory Smith, C. Adams, R. M. Blair, D. Sigg, S. W. Ballmer, D. Pascucci, D. C. Coyne, Eric Thrane, Q. Chu, D. M. Shoemaker, K. Izumi, C. Michel, E. Genin, R. Flaminio, Sarah Caudill, J.-P. Coulon, Leo Singer, R. Quitzow-James, R. Day, V. B. Adya, O. Bock, T. Hardwick, D. Steinmeyer, S. Privitera, F. Travasso, F. Baldaccini, T. Prestegard, Michelle E. Walker, G. Moreno, Jong H. Chow, J. Liu, A. Pasqualetti, J. W. W. Pratt, J. S. Kissel, M. J. Hart, Odylio D. Aguiar, D. S. Rabeling, M. Di Giovanni, K. E. Gushwa, A. Effler, H. Qi, M. Branchesi, J. C. Batch, G. Gemme, M. Drago, L. Sammut, Lionel London, V. Loriette, D. M. Macleod, Gregory M. Harry, B. L. Swinkels, V. Tiwari, László Gondán, M. Poe, Rocco Romano, Guenakh Mitselmakher, J. R. Leong, Francesco Salemi, B. A. Boom, A. M. Sergeev, C. Affeldt, A. Gennai, Rahul Kumar, Harald P. Pfeiffer, A. Sheperd, M. Ast, O. E. S. Sauter, Catherine M. McGrath, John D. Scott, J. K. Blackburn, A. Sawadsky, E. Chassande-Mottin, R. A. Mercer, Sheila Rowan, J. Woehler, A. Ain, E. M. Fries, M. Rizzo, V. Predoi, I. W. Martin, David E. McClelland, R. Taylor, Shubhanshu Tiwari, Steven Reyes, S. D'Antonio, S. Chung, Debnandini Mukherjee, S. T. Countryman, Jinsook Kim, Andrew Matas, Surabhi Sachdev, Christopher J. Moore, V. V. Frolov, M. C. Araya, C. Lazzaro, Patricia Schmidt, V. Brisson, R. T. DeRosa, C. Buy, G. Bogaert, S. Doravari, Todd Adams, B. Mours, A. Moggi, J. Ming, E. Cesarini, Innocenzo M. Pinto, K. G. Arun, A. Singhal, A. Chiummo, G. Stratta, Jesper Munch, P. Bacon, Daniel E. Holz, Achamveedu Gopakumar, M. De Laurentis, Luca Gammaitoni, A. L. Miller, Alena Ananyeva, Benoit Sassolas, M. H. Wimmer, B. Patricelli, D. S. Wu, Margaret Millhouse, M. K. M. Bader, A. Brillet, Heinz-Bernd Eggenstein, Christopher M. Biwer, M. C. Heintze, S. Frasca, S. G. Gaonkar, F. Carbognani, L. Conti, M. Constancio, Duncan A. Brown, Haixing Miao, Stephen Fairhurst, Carl Blair, E. Katsavounidis, K. L. Dooley, Lisa Barsotti, H. Radkins, A. Bozzi, C. Baune, Anirban Dasgupta, M. Brinkmann, J. P. Henry, John Worden, P. Couvares, David Coward, Sheon Chua, R. Bonnand, Jan Harms, A. S. Sengupta, Satyanarayan Ray Pitambar Mohapatra, Viswanath Bavigadda, Evan Goetz, D. Buskulic, E. Cuoco, A. Gupta, S. Meshkov, Seog Oh, S. A. Usman, Roman Schnabel, J. E. Brau, A. A. van Veggel, Efim A. Khazanov, G. Ballardin, D. J. McManus, R. Robie, F. Clara, J. S. Areeda, P. Fulda, Andreas Freise, Vincenzo Pierro, Paul D. Lasky, Evan Ochsner, A. J. Weinstein, Matthew Pitkin, S. E. Barclay, Ofek Birnholtz, M. Granata, V. Boschi, R. J. G. Jonker, Alberto Vecchio, Minchuan Zhou, J. Devenson, Will M. Farr, Eric Howell, M. Landry, M. Montani, Nancy Aggarwal, Zahoor Ali Khan, D. Mendoza-Gandara, S. Leavey, Hai-Ping Cheng, L. Di Fiore, M. Barsuglia, T. M. Evans, L. K. Nuttall, Jon M. Miller, I. Dave, M. Fletcher, B. Hughey, P. B. Covas, G. Billingsley, S. Macfoy, M. C. Edwards, C. Whittle, B. B. Miller, S. Mirshekari, A. Grant, S. E. Gossan, Felice Sorrentino, G. Greco, D. Moraru, Graham Woan, L. E. Wade, Samuel Deléglise, Gianpietro Cagnoli, Robert L. Byer, Stuart Reid, G. Valdes, A. Samajdar, L. Zhang, C. Pankow, Jacob Scheuer, P. M. Meyers, Barry C. Barish, P. Thomas, Paul J. Groot, M. Zevin, L. Zangrando, A. Allocca, Bernard F. Schutz, John Veitch, Li Ju, J. Lehmann, F. Vetrano, Daniel A. Shaddock, Y. Bouffanais, C. V. Kalaghatgi, J. Hanson, N. Arnaud, Maggie Tse, Vijay Varma, K. Napier, T. Tippens, Guido Mueller, M. MacInnis, M. Dovale Álvarez, S. E. Dwyer, David Keitel, P. Rapagnani, J. M. Gonzalez Castro, Hang Yu, B. D. Cheeseboro, G. Cerretani, S. J. Cooper, A. Lartaux-Vollard, Suvadeep Bose, T. Huynh-Dinh, M. Thomas, Christian Beer, Vladimir B. Braginsky, H. Vahlbruch, S. R. Morriss, D. Barta, R. Gouaty, Z. Márka, M. Merzougui, B. Lantz, H. Cao, D. J. Vine, K. Riles, H. Middleton, A. Fernández Galiana, Marc Favata, I. Belahcene, Roger Jones, V. J. Roma, Francesco Pannarale, M. Weinert, H. A. G. Gabbard, F. Fidecaro, G. M. Guidi, A. P. Spencer, D. D. Brown, A. Rocchi, C. Cocchieri, R. Birney, N. van Bakel, R. M. S. Schofield, V. Kringel, H. N. Isa, Benjamin J. Owen, J. F. J. van den Brand, M. Belgin, D. Tuyenbayev, S. Sunil, M. Tacca, K. Kawabe, Maria Ilaria Del Principe, Martin Hendry, S. M. Aston, Michael W. Coughlin, I. Khan, M. Agathos, M. C. Díaz, Antonios Kontos, Junwei Cao, L. Kuo, H. Yamamoto, E. Capocasa, J. L. Wright, Alessandra Corsi, J. C. Driggers, A. Schönbeck, J. E. Lord, E. J. Daw, Maurizio Canepa, J. Prasad, Steven Bloemen, Paolo Addesso, K. D. Giardina, Jonathan R. Gair, J. S. Lange, L. M. Perri, N. A. Lockerbie, N. A. Robertson, J. G. Bartlett, Blake Moore, Márton Tápai, David Jonathan Hofman, Liam Cunningham, A. Noack, Jonathan Blackman, K. Toland, Thomas Dent, Vladimir Dergachev, J. Junker, Y. Setyawati, Tania Regimbau, M. M. Hanke, James Whelan, P. Ajith, S. B. Anderson, David B. Tanner, Zachariah B. Etienne, Jennifer Watchi, T. P. Downes, M. Pedraza, M. Chan, Maria Alessandra Papa, F. Cavalier, P. G. Murray, B. K. Berger, Fabien Kéfélian, J. H. Hough, J. R. Palamos, Michele Zanolin, T. J. Massinger, T. Vo, G. D. Hammond, D. B. Kelley, Zhihui Du, S. S. Eikenberry, Yanxi Zhang, Rosa Poggiani, T. A. Callister, M. Haney, H. S. Cho, Jade Powell, V. Mangano, V. Frey, S. Farinon, Yi-Ming Hu, P. Raffai, O. J. Piccinni, J. Hanks, Gavin Davies, C. Tomlinson, J. D. Lough, Soma Mukherjee, H. R. Paris, Frank Ohme, Vicky Kalogera, A. Post, M. Leonardi, S. J. Kimbrell, S. S. Forsyth, Aviral Singh, Andrew Lundgren, M. Factourovich, J. Betzwieser, Antoine Heidmann, D. Töyrä, H. Overmier, J. E. Broida, D. Sellers, J. Meidam, Riccardo Sturani, D. Hoak, D. Sentenac, Patrick Brady, (Astro)-Particles Physics, Abbott, B. P, Abbott, R, Abbott, T. D, Abernathy, M. R, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, B, Allocca, A, Altin, P. A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arnaud, N, Arun, K. G, Ascenzi, S, Ashton, G, Ast, M, Aston, S. M, Astone, P, Aufmuth, P, Aulbert, C, Avila Alvarez, A, Babak, S, Bacon, P, Bader, M. K. M, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Batch, J. C, Baune, C, Bavigadda, V, Bazzan, M, Beer, C, Bejger, M, Belahcene, I, Belgin, M, Bell, A. S, Berger, B. K, Bergmann, G, Berry, C. P. 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D, Capocasa, E, Carbognani, F, Caride, S, Casanueva Diaz, J, Casentini, C, Caudill, S, Cavaglià, M, Cavalier, F, Cavalieri, R, Cella, G, Cepeda, C. B, Cerboni Baiardi, L, Cerretani, G, Cesarini, E, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chassande Mottin, E, Cheeseboro, B. D, Chen, H. Y, Chen, Y, Cheng, H. P, Chincarini, A, Chiummo, A, Chmiel, T, Cho, H. S, Cho, M, Chow, J. H, Christensen, N, Chu, Q, Chua, A. J. K, Chua, S, Chung, S, Ciani, G, Clara, F, Clark, J. A, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P. F, Colla, A, Collette, C. G, Cominsky, L, Constancio, M, Conti, L, Cooper, S. J, Corbitt, T. R, Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Coughlin, E, Coughlin, M. W, Coughlin, S. B, Coulon, J. P, Countryman, S. T, Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Danilishin, S. L, D'Antonio, S, Danzmann, K, Dasgupta, A, Da Silva Costa, C. F, Dattilo, V, Dave, I, Davier, M, Davies, G. S, Davis, D, Daw, E. J, Day, B, Day, R, De, S, Debra, D, Debreczeni, G, Degallaix, J, DE LAURENTIS, Martina, Deléglise, S, Del Pozzo, W, Denker, T, Dent, T, Dergachev, V, DE ROSA, Rosario, Derosa, R. T, Desalvo, R, Devenson, J, Devine, R. C, Dhurandhar, S, Díaz, M. C, Di Fiore, L, Di Giovanni, M, DI GIROLAMO, Tristano, Di Lieto, A, Di Pace, S, Di Palma, I, Di Virgilio, A, Doctor, Z, Dolique, V, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I, Douglas, R, Dovale Álvarez, M, Downes, T. P, Drago, M, Drever, R. W. P, Driggers, J. C, Du, Z, Ducrot, M, Dwyer, S. E, Edo, T. B, Edwards, M. C, Effler, A, Eggenstein, H. B, Ehrens, P, Eichholz, J, Eikenberry, S. S, Essick, R. C, Etienne, Z, Etzel, T, Evans, M, Evans, T. M, Everett, R, Factourovich, M, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon Jones, E. J, Favata, M, Fays, M, Fehrmann, H, Fejer, M. M, Fernández Galiana, A, Ferrante, I, Ferreira, E. C, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, R. P, Flaminio, R, Fletcher, M, Fong, H, Forsyth, S. S, Fournier, J. D, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fries, E. M, Fritschel, P, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Gaonkar, S. G, Garufi, Fabio, Gaur, G, Gayathri, V, Gehrels, N, Gemme, G, Genin, E, Gennai, A, George, J, Gergely, L, Germain, V, Ghonge, S, Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S, Giaime, J. A, Giardina, K. D, Giazotto, A, Gill, K, Glaefke, A, Goetz, E, Goetz, R, Gondan, L, González, G, Gonzalez Castro, J. M, Gopakumar, A, Gorodetsky, M. L, Gossan, S. E, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Gray, C, Greco, G, Green, A. C, Groot, P, Grote, H, Grunewald, S, Guidi, G. M, Guo, X, Gupta, A, Gupta, M. K, Gushwa, K. E, Gustafson, E. K, Gustafson, R, Hacker, J. J, Hall, B. R, Hall, E. D, Hammond, G, Haney, M, Hanke, M. M, Hanks, J, Hanna, C, Hannam, M. D, Hanson, J, Hardwick, T, Harms, J, Harry, G. M, Harry, I. W, Hart, M. J, Hartman, M. T, Haster, C. J, Haughian, K, Healy, J, Heidmann, A, Heintze, M. C, Heitmann, H, Hello, P, Hemming, G, Hendry, M, Heng, I. S, Hennig, J, Henry, J, Heptonstall, A. W, Heurs, M, Hild, S, Hoak, D, Hofman, D, Holt, K, Holz, D. E, Hopkins, P, Hough, J, Houston, E. A, Howell, E. J, Hu, Y. M, Huerta, E. A, Huet, D, Hughey, B, Husa, S, Huttner, S. H, Huynh Dinh, T, Indik, N, Ingram, D. R, Inta, R, Isa, H. N, Isac, J. M, Isi, M, Isogai, T, Iyer, B. R, Izumi, K, Jacqmin, T, Jani, K, Jaranowski, P, Jawahar, S, Jiménez Forteza, F, Johnson, W. W, Jones, D. I, Jones, R, Jonker, R. J. G, Ju, L, Junker, J, Kalaghatgi, C. V, Kalogera, V, Kandhasamy, S, Kang, G, Kanner, J. B, Karki, S, Karvinen, K. 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Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. .s., Urban, A. .l., Usman, S. .a., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., van den Brand, J. .f. .j., Van Den Broeck, C., Vander Hyde, D. .c., van der Schaaf, L., van Heijningen, J. .v., van Veggel, A. .a., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. .j., Venkateswara, K., Venugopalan, G., Verkindt, D., VETRANO, FLAVIO, VICERE', ANDREA, Viets, A. .d., Vinciguerra, S., Vine, D. .j., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D. .v., Vousden, W. .d., Vyatchanin, S. .p., Wade, A. .r., Wade, L. .e., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, Y., Ward, R. .l., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. .j., Weiss, R., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. .t., Whiting, B. .f., Whittle, C., Williams, D., Williams, R. .d., Williamson, A. .r., Willis, J. .l., Willke, B., Wimmer, M. .h., Winkler, W., Wipf, C. .c., Wittel, H., Woan, G., Woehler, J., Worden, J., Wright, J. .l., Wu, D. .s., Wu, G., Yam, W., Yamamoto, H., Yancey, C. .c., Yap, M. .j., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. .j., Zhu, X. .j., Zucker, M. .e., Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Science and Engineering Research Board, Royal Society, Fundação de Amparo à Pesquisa do Estado de São Paulo, Australian Research Council, Országos Tudományos Kutatási Alapprogramok, Narodowe Centrum Nauki, Centre National de la Recherche Scientifique, Max-Planck-Gesellschaft, National Science Foundation, Leverhulme Trust, Ministry of Science and Technology of the People’s Republic of China, Conselleria d’Economia i Competitivitat and Conselleria d’Educació, Russian Foundation for Basic Research, Cultura i Universitats of the Govern de les Illes Balears, Lyon Institute of Origins, Brazilian Ministry of Science, Technology, and Innovation, Ministry of Human Resource Development, Kavli Foundation, Scottish Universities Physics Alliance, Research Corporation for Science Advancement, Istituto Nazionale di Fisica Nucleare, National Research Foundation of Korea, Nederlandse Organisatie voor Wetenschappelijk Onderzoek, Canadian Institute for Advanced Research, Natural Sciences and Engineering Research Council of Canada, Science and Technology Facilities Council, Ontario Ministry of Economic Development and Innovation, Ministerio de Economía y Competitividad, Scottish Funding Council, European Commission, Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Gravitational-wave observatory, Astronomy, STRING COSMOLOGY, General Physics and Astronomy, Gravitational waves, stochastic background, LIGO, O1, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, Energy density, INFLATION, COMPACT BINARY COALESCENCES, PHASE-TRANSITIONS, PLANCK 2015, RADIATION, POPULATION, RATES, LIGO, QC, QB, Data display, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Stochastic systems, Energy density spectrum, Black holes, Gravitational effects, Gravitational-wave signals, stochastic background, Upper limits, gravitational waves, astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Laser interferometer gravitational-wave observatories, Astrophysics - High Energy Astrophysical Phenomena, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, Population, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Gravity waves, O1, Gravitational waves, LIGO detectors, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Physics and Astronomy (all), Binary black hole, 0103 physical sciences, GW151226, ddc:530, 010306 general physics, education, STFC, Inflation (cosmology), Interferometers, 010308 nuclear & particles physics, RCUK, Stochastic background, Flocculation, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Physical Review, 530 Physik, Stars, Physics and Astronomy, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, Laser interferometry
Abstract

A wide variety of astrophysical and cosmological sources are expected to contribute to a stochastic gravitational-wave background. Following the observations of GW150914 and GW151226, the rate and mass of coalescing binary black holes appear to be greater than many previous expectations. As a result, the stochastic background from unresolved compact binary coalescences is expected to be particularly loud. We perform a search for the isotropic stochastic gravitational-wave background using data from Advanced LIGO's first observing run. The data display no evidence of a stochastic gravitational-wave signal. We constrain the dimensionless energy density of gravitational waves to be $\Omega_0, Comment: 13 pages, 6 figures

Published
2017

44. Ultralight Dark Matter Resonates with Binary Pulsars

Author

Sergey Sibiryakov, Diego Blas, and Diana López Nacir

Subjects
Astrophysics and Astronomy, astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, Scalar field dark matter, General Physics and Astronomy, Binary number, Perturbation (astronomy), FOS: Physical sciences, Astrophysics, 7. Clean energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), Gravitational field, Pulsar, 0103 physical sciences, 010306 general physics, Particle Physics - Phenomenology, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, hep-th, hep-ph, Orbital period, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Scalar field, Particle Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We consider the scenario where dark matter (DM) is represented by an ultra-light classical scalar field performing coherent periodic oscillations. We point out that such DM perturbs the dynamics of binary systems either through its gravitational field or via direct coupling to ordinary matter. This perturbation gets resonantly amplified if the frequency of DM oscillations is close to a (half-)integer multiple of the orbital frequency of the system and leads to a secular variation of the orbital period. We suggest to use binary pulsars as probes of this scenario and estimate their sensitivity. While the current accuracy of observations is not yet sufficient to probe the purely gravitational effect of DM, it already yields constraints on direct coupling that are competitive with other bounds. The sensitivity will increase with the upcoming radio observatories such as Square Kilometer Array., 6 pages, 3 figures; references added. v3: Typo corrected. Extra clarifications on bounds on quadratic coupling

Published
2017

45. γ-ray Constraints on Decaying Dark Matter and Implications for IceCube

Author

Benjamin R. Safdi, Nicholas L. Rodd, Yotam Soreq, Kohta Murase, and Timothy Cohen

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Cosmic background radiation, General Physics and Astronomy, Flux, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Galaxy, Hidden sector, High Energy Physics - Phenomenology, 13. Climate action, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

Utilizing the Fermi measurement of the gamma-ray spectrum toward the Galactic Center, we derive some of the strongest constraints to date on the dark matter (DM) lifetime in the mass range from hundreds of MeV to above an EeV. Our profile-likelihood based analysis relies on 413 weeks of Fermi Pass 8 data from 200 MeV to 2 TeV, along with up-to-date models for diffuse gamma-ray emission within the Milky Way. We model Galactic and extragalactic DM decay and include contributions to the DM-induced gamma-ray flux resulting from both primary emission and inverse-Compton scattering of primary electrons and positrons. For the extragalactic flux, we also calculate the spectrum associated with cascades of high-energy gamma-rays scattering off of the cosmic background radiation. We argue that a decaying DM interpretation for the 10 TeV-1 PeV neutrino flux observed by IceCube is disfavored by our constraints. Our results also challenge a decaying DM explanation of the AMS-02 positron flux. We interpret the results in terms of individual final states and in the context of simplified scenarios such as a hidden-sector glueball model., Comment: Updated to correct an issue in Fig. S12, 9+19 pages, 2+14 figures, Supplementary Data available at https://dspace.mit.edu/handle/1721.1/105550

Published
2017

46. Kinematic Sunyaev-Zel’dovich Effect with Projected Fields: A Novel Probe of the Baryon Distribution with Planck, WMAP, and WISE Data

Author

David N. Spergel, Jia Liu, Simone Ferraro, Nick Battaglia, and J. Colin Hill

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, 010308 nuclear & particles physics, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Sunyaev–Zel'dovich effect, 7. Clean energy, 01 natural sciences, CMB cold spot, Galaxy, Cosmology, Redshift, 13. Climate action, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The kinematic Sunyaev-Zel'dovich (kSZ) effect --- the Doppler boosting of cosmic microwave background (CMB) photons due to Compton-scattering off free electrons with non-zero bulk velocity --- probes the abundance and distribution of baryons in the Universe. All kSZ measurements to date have explicitly required spectroscopic redshifts. Here, we implement a novel estimator for the kSZ -- large-scale structure cross-correlation based on projected fields: it does not require redshift estimates for individual objects, allowing kSZ measurements from large-scale imaging surveys. We apply this estimator to cleaned CMB temperature maps constructed from Planck and Wilkinson Microwave Anisotropy Probe data and a galaxy sample from the Wide-field Infrared Survey Explorer (WISE). We measure the kSZ effect at 3.8-4.5$\sigma$ significance, depending on the use of additional WISE galaxy bias constraints. We verify that our measurements are robust to possible dust emission from the WISE galaxies. Assuming the standard $\Lambda$CDM cosmology, we directly constrain $( {f_{b}}/{0.158} ) ( {f_{\rm free}}/{1.0} ) = 1.48 \pm 0.19$ (statistical error only) at redshift $z \approx 0.4$, where $f_{b}$ is the fraction of matter in baryonic form and $f_{\rm free}$ is the free electron fraction. This is the tightest kSZ-derived constraint reported to date on these parameters. The consistency between the $f_{b}$ value found here and the values inferred from analyses of the primordial CMB and Big Bang nucleosynthesis verifies that baryons approximately trace the dark matter distribution down to $\sim$Mpc scales. While our projected-field estimator is already competitive with other kSZ approaches when applied to current datasets (because we are able to use the full-sky WISE photometric survey), it will yield enormous signal-to-noise when applied to upcoming high-resolution, multi-frequency CMB surveys., Comment: 5 pages + references, 2 figures; v2: matches PRL accepted version, results unchanged

Published
2016

47. Demonstration of Cosmic Microwave Background Delensing Using the Cosmic Infrared Background

Author

Anthony Challinor, Patricia Larsen, Daisy Mak, Blake D. Sherwin, Challinor, Anthony [0000-0003-3479-7823], and Apollo - University of Cambridge Repository

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Strong gravitational lensing, General Physics and Astronomy, Astronomy, Spectral density, FOS: Physical sciences, Planck temperature, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Amplitude, Gravitational lens, Cosmic infrared background, 0103 physical sciences, symbols, astro-ph.CO, Planck, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Delensing is an increasingly important technique to reverse the gravitational lensing of the cosmic microwave background (CMB) and thus reveal primordial signals the lensing may obscure. We present a first demonstration of delensing on Planck temperature maps using the cosmic infrared background (CIB). Reversing the lensing deflections in Planck CMB temperature maps using a linear combination of the 545 and 857GHz maps as a lensing tracer, we find that the lensing effects in the temperature power spectrum are reduced in a manner consistent with theoretical expectations. In particular, the characteristic sharpening of the acoustic peaks of the temperature power spectrum resulting from successful delensing is detected at a significance of 16$\rm{\sigma}$, with an amplitude of $A_{\rm{delens}} = 1.12 \pm 0.07$ relative to the expected value of unity. This first demonstration on data of CIB delensing, and of delensing techniques in general, is significant because lensing removal will soon be essential for achieving high-precision constraints on inflationary B-mode polarization., Comment: 6 pages, 5 figures, accepted for publication in PRL

Published
2016

48. Codecaying Dark Matter

Author

Jeff A. Dror, Wee Hao Ng, and Eric Kuflik

Subjects
Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Hot dark matter, Dark matter, Scalar field dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Baryonic dark matter, 0103 physical sciences, Mixed dark matter, Warm dark matter, 010306 general physics, Light dark matter, Dark fluid, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We propose a new mechanism for thermal dark matter freezeout, termed Co-Decaying Dark Matter. Multi-component dark sectors with degenerate particles and out-of-equilibrium decays can co-decay to obtain the observed relic density. The dark matter density is exponentially depleted through the decay of nearly degenerate particles, rather than from Boltzmann suppression. The relic abundance is set by the dark matter annihilation cross-section, which is predicted to be boosted, and the decay rate of the dark sector particles. The mechanism is viable in a broad range of dark matter parameter space, with a robust prediction of an enhanced indirect detection signal. Finally, we present a simple model that realizes co-decaying dark matter., 6 pages, 3 figures; matches version on PRL with updated references

Published
2016

49. How Isotropic is the Universe?

Author

Stephen M. Feeney, Hiranya V. Peiris, Daniela Saadeh, Andrew Pontzen, and Jason D. McEwen

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Isotropy, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Universe, 0103 physical sciences, Anisotropy, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

A fundamental assumption in the standard model of cosmology is that the Universe is isotropic on large scales. Breaking this assumption leads to a set of solutions to Einstein's field equations, known as Bianchi cosmologies, only a subset of which have ever been tested against data. For the first time, we consider all degrees of freedom in these solutions to conduct a general test of isotropy using cosmic microwave background temperature and polarization data from Planck. For the vector mode (associated with vorticity), we obtain a limit on the anisotropic expansion of $(\sigma_V/H)_0 < 4.7 \times 10^{-11}$ (95% CI), which is an order of magnitude tighter than previous Planck results that used CMB temperature only. We also place upper limits on other modes of anisotropic expansion, with the weakest limit arising from the regular tensor mode, $(\sigma_{T,\rm reg}/H)_0, Comment: 6 pages, 1 figure, v2: replaced with version accepted by PRL

Published
2016

50. Did LIGO Detect Dark Matter?

Author

Yacine Ali-Haïmoud, Adam G. Riess, Alvise Raccanelli, Ely D. Kovetz, Ilias Cholis, Marc Kamionkowski, Simeon Bird, and Julian B. Muñoz

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Scalar field dark matter, FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Gravitational wave background, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, Light dark matter, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Hot dark matter, Astronomy, LIGO, Dark matter halo, High Energy Physics - Phenomenology, 13. Climate action, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We consider the possibility that the black-hole (BH) binary detected by LIGO may be a signature of dark matter. Interestingly enough, there remains a window for masses $20\,M_\odot \lesssim M_{\rm bh} \lesssim 100\, M_\odot$ where primordial black holes (PBHs) may constitute the dark matter. If two BHs in a galactic halo pass sufficiently close, they radiate enough energy in gravitational waves to become gravitationally bound. The bound BHs will rapidly spiral inward due to emission of gravitational radiation and ultimately merge. Uncertainties in the rate for such events arise from our imprecise knowledge of the phase-space structure of galactic halos on the smallest scales. Still, reasonable estimates span a range that overlaps the $2-53$ Gpc$^{-3}$ yr$^{-1}$ rate estimated from GW150914, thus raising the possibility that LIGO has detected PBH dark matter. PBH mergers are likely to be distributed spatially more like dark matter than luminous matter and have no optical nor neutrino counterparts. They may be distinguished from mergers of BHs from more traditional astrophysical sources through the observed mass spectrum, their high ellipticities, or their stochastic gravitational wave background. Next generation experiments will be invaluable in performing these tests., Comment: 5 pages, 2 figures, updated to match version published in PRL

Published
2016

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