Ely D. Kovetz

Ben-Gurion University of the Negev

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Marc Kamionkowski

Johns Hopkins University

Julián B. Muñoz

The University of Texas at Austin

Patrick C. Breysse

New York University

Yacine Ali-Haïmoud

New York University

Tzu‐Ching Chang

China Medical University

Cora Dvorkin

Harvard University

José Luis Bernal

Instituto de Física de Cantabria

Marcelo A. Alvarez

Lawrence Berkeley National Laboratory

Emmanuel Schaan

Kavli Institute for Particle Astrophysics and Cosmology

Sara M. Simon

Fermi National Accelerator Laboratory

Cooperative Institutions

Centre National de la Recherche Scientifique

208

University of California, Berkeley

186

California Institute of Technology

164

University of Chicago

148

Kavli Institute for Particle Astrophysics and Cosmology

146

Fermi National Accelerator Laboratory

126

Lawrence Berkeley National Laboratory

121

Princeton University

120

Stanford University

109

Center for Astrophysics Harvard & Smithsonian

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Probing ultralight scalar, vector and tensor dark matter with pulsar timing arrays

Physics Letters B (2024)

Caner Ünal F. Urban Ely D. Kovetz

Pulsar timing arrays (PTAs) are sensitive to oscillations in the gravitational potential along the line-of-sight due to ultralight particle pressure. We calculate the probing power of PTAs for ultralight bosons across all frequencies, from those larger than the inverse observation time to those smaller than the inverse distance to the pulsar. We show that since the signal amplitude grows comparably to the degradation in PTA sensitivity at frequencies smaller than inverse observation time, the discovery potential can be extended towards lower masses by over three decades, maintaining high precision. We demonstrate that, in the mass range 10−26−10−23 eV, existing 15-year PTA data can robustly detect or rule out an ultralight component down to O(1−10)% of the total dark matter. Non-detection, together with other bounds in different mass ranges, will imply that ultralight scalar/axion can comprise at most 1−10% of dark matter in the 10−30−10−17 eV range. With 30 years of observation, current PTAs can extend the reach down to 0.1−1%, while next-generation PTAs such as SKA can attain the 0.01−0.1% precision. We generalize and derive predictions for ultralight spin-1 vector (i.e. dark photon) and spin-2 tensor dark components.

10.1016/j.physletb.2024.138830

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Citations (3)

Outliers in the LIGO black hole mass function from coagulation in dense clusters

Monthly Notices of the Royal Astronomical Society (2021)

Jordan Flitter Julián B. Muñoz Ely D. Kovetz

The advanced LIGO O3a run catalog has been recently published, and it includes several events with unexpected mass properties, including mergers with individual masses in the lower and upper mass gaps, as well as mergers with unusually small mass ratios between the binary components. Here we entertain the possibility that these outliers are the outcome of hierarchical mergers of black holes or neutron stars in the dense environments of globular clusters. We use the coagulation equation to study the evolution of the black hole mass function within a typical cluster. Our prescription allows us to monitor how various global quantities change with time, such as the total mass and number of compact objects in the cluster, its overall merger rate, and the probability to form intermediate-mass black holes via a runaway process. By accounting for the LIGO observational bias, we predict the merger event distributions with respect to various variables such as the individual masses M1 and M2, their ratio q, and redshift z, and we compare our predictions with the published O3a data. We study how these distributions depend on the merger-rate and ejections parameters and produce forecasts for the (tight) constraints that can be placed on our model parameters using the future dataset of the O5 run. Finally, we also consider the presence of a static channel with no coagulation producing merger events alongside the dynamic channel, finding that the two can be distinguished based solely on the merger mass distribution with future O5 data.

Black hole (networking)

Mass ratio

Mass segregation

10.1093/mnras/stab2203

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Citations (8)

Astro2020 science white paper inflation and dark energy from spectroscopy at z > 2

Simone Ferraro Michael Wilson Muntazir Abidi David Alonso Behzad Ansarinejad

White (mutation)

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Mapping large-scale-structure evolution over cosmic times

Experimental Astronomy (2021)

Marta B. Silva Ely D. Kovetz Garrett K. Keating Azadeh Moradinezhad Dizgah M. Béthermin

Abstract This paper outlines the science case for line-intensity mapping with a space-borne instrument targeting the sub-millimeter (microwaves) to the far-infrared (FIR) wavelength range. Our goal is to observe and characterize the large-scale structure in the Universe from present times to the high redshift Epoch of Reionization. This is essential to constrain the cosmology of our Universe and form a better understanding of various mechanisms that drive galaxy formation and evolution. The proposed frequency range would make it possible to probe important metal cooling lines such as [CII] up to very high redshift as well as a large number of rotational lines of the CO molecule. These can be used to trace molecular gas and dust evolution and constrain the buildup in both the cosmic star formation rate density and the cosmic infrared background (CIB). Moreover, surveys at the highest frequencies will detect FIR lines which are used as diagnostics of galaxies and AGN. Tomography of these lines over a wide redshift range will enable invaluable measurements of the cosmic expansion history at epochs inaccessible to other methods, competitive constraints on the parameters of the standard model of cosmology, and numerous tests of dark matter, dark energy, modified gravity and inflation. To reach these goals, large-scale structure must be mapped over a wide range in frequency to trace its time evolution and the surveyed area needs to be very large to beat cosmic variance. Only a space-borne mission can properly meet these requirements.

Cosmic variance

Structure formation

Baryon Acoustic Oscillations

10.1007/s10686-021-09755-3

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Direct millicharged dark matter cannot explain the EDGES signal

Physical review. D/Physical review. D. (2019)

Cyril Creque-Sarbinowski Lingyuan Ji Ely D. Kovetz Marc Kamionkowski

Heat transfer between baryons and millicharged dark matter has been invoked as a possible explanation for the anomalous 21-cm absorption signal seen by EDGES. Prior work has shown that the solution requires that millicharged particles make up only a fraction $({m}_{\ensuremath{\chi}}/\mathrm{MeV})0.0115%\ensuremath{\lesssim}f\ensuremath{\lesssim}0.4%$ of the dark matter and that their mass ${m}_{\ensuremath{\chi}}$ and charge ${q}_{\ensuremath{\chi}}$ have values $0.1\ensuremath{\lesssim}({m}_{\ensuremath{\chi}}/\mathrm{MeV})\ensuremath{\lesssim}10$ and ${10}^{\ensuremath{-}6}\ensuremath{\lesssim}({q}_{\ensuremath{\chi}}/e)\ensuremath{\lesssim}{10}^{\ensuremath{-}4}$. Here we show that such particles come into chemical equilibrium before recombination, and so are subject to a constraint on the effective number ${N}_{\mathrm{eff}}$ of relativistic degrees of freedom, which we update using Planck 2018 data. We moreover determine the precise relic abundance $f$ that results for a given mass ${m}_{\ensuremath{\chi}}$ and charge ${q}_{\ensuremath{\chi}}$ and incorporate this abundance into the constraints on the millicharged-dark-matter solution to the EDGES signal. With these two results, the solution is ruled out if the relic abundance is set by freeze-out.

10.1103/physrevd.100.023528

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Citations (44)

Searching for Signals of Merging Primordial Black Hole Binaries

Bulletin of the American Physical Society (2017)

Ilias Cholis Yacine Ali-Haïmoud Simeon Bird Marc Kamionkowski Ely D. Kovetz

Primordial black hole

Black hole (networking)

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Microwave spectro-polarimetry of matter and radiation across space and time

Experimental Astronomy (2021)

Jacques Delabrouille Maximilian H. Abitbol Nabila Aghanim Yacine Ali-Haïmoud David Alonso

Abstract This paper discusses the science case for a sensitive spectro-polarimetric survey of the microwave sky. Such a survey would provide a tomographic and dynamic census of the three-dimensional distribution of hot gas, velocity flows, early metals, dust, and mass distribution in the entire Hubble volume, exploit CMB temperature and polarisation anisotropies down to fundamental limits, and track energy injection and absorption into the radiation background across cosmic times by measuring spectral distortions of the CMB blackbody emission. In addition to its exceptional capability for cosmology and fundamental physics, such a survey would provide an unprecedented view of microwave emissions at sub-arcminute to few-arcminute angular resolution in hundreds of frequency channels, a data set that would be of immense legacy value for many branches of astrophysics. We propose that this survey be carried out with a large space mission featuring a broad-band polarised imager and a moderate resolution spectro-imager at the focus of a 3.5 m aperture telescope actively cooled to about 8K, complemented with absolutely-calibrated Fourier Transform Spectrometer modules observing at degree-scale angular resolution in the 10–2000 GHz frequency range. We propose two observing modes: a survey mode to map the entire sky as well as a few selected wide fields, and an observatory mode for deeper observations of regions of specific interest.

Black-body radiation

10.1007/s10686-021-09721-z

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Citations (37)

Closing the window on fuzzy dark matter with the 21-cm signal

Physical review. D/Physical review. D. (2022)

Jordan Flitter Ely D. Kovetz

Fuzzy dark matter (FDM) is a well motivated candidate for dark matter (DM) as its tiny mass and large de-Broglie wavelength suppress small-scale matter fluctuations, thereby solving some of the small-scale discrepancies in $\Lambda$CDM. Although it has been ruled out as the single component of DM by several observables, there is still a region in the FDM parameter space (the "FDM window", $10^{-25}\,\mathrm{eV}\lesssim m_\mathrm{FDM}\lesssim10^{-23}\,\mathrm{eV}$) where FDM is allowed to comprise a large portion of the total DM. In this work, for the first time, we study the signature of FDM (comprised of ultra-light axions) in fractions less than unity on the 21cm signal and its detectability by 21cm interferometers such as HERA, taking into account the degeneracy with both astrophysical and cosmological parameters, using a new pipeline that combines modified versions of the CAMB and 21cmFAST codes. Our forecasts imply that HERA in its design performance will be sensitive to FDM fractions as small as 1% in the FDM window, and improve over existing bounds for other masses by up to an order of magnitude.

Matter wave

Cold dark matter

SIGNAL (programming language)

10.1103/physrevd.106.063504

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Citations (30)

Snowmass 2021 CMB-S4 White Paper

arXiv (Cornell University) (2022)

Kevork N. Abazajian Arwa Abdulghafour Graeme E. Addison Peter Adshead Zeeshan Ahmed

This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan.

White paper

White (mutation)

10.48550/arxiv.2203.08024

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Citations (10)

Power spectrum and non-Gaussianities in anisotropic inflation

Journal of Cosmology and Astroparticle Physics (2014)

Anindya Dey Ely D. Kovetz Sònia Paban

We study the planar regime of curvature perturbations for single field inflationary models in an axially symmetric Bianchi I background. In a theory with standard scalar field action, the power spectrum for such modes has a pole as the planarity parameter goes to zero. We show that constraints from back reaction lead to a strong lower bound on the planarity parameter for high-momentum planar modes and use this bound to calculate the signal-to-noise ratio of the anisotropic power spectrum in the CMB, which in turn places an upper bound on the Hubble scale during inflation allowed in our model. We find that non-Gaussianities for these planar modes are enhanced for the flattened triangle and the squeezed triangle configurations, but show that the estimated values of the fNL parameters remain well below the experimental bounds from the CMB for generic planar modes (other, more promising signatures are also discussed). For a standard action, fNL from the squeezed configuration turns out to be larger compared to that from the flattened triangle configuration in the planar regime. However, in a theory with higher derivative operators, non-Gaussianities from the flattened triangle can become larger than the squeezed configuration in a certain limit of the planarity parameter.

Planarity testing

Slow roll

10.1088/1475-7516/2014/06/025

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Citations (7)