Pulsar timing array constraints on spin-2 ULDM

Armaleo, Juan Manuel; Nacir, Diana Laura Lopez; Urban, Federico

doi:10.1088/1475-7516/2020/09/031

Cited by 23 publications

(26 citation statements)

References 81 publications

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“…Heuristically (µ/m) 1/2 ∼ (1/mL) where L is the characteristic size of the soliton, and M ∼ (m pl /m) 2 /L. Since in the non-relativistic regime µ/m 1, we expect the maximal values of the above quantities (40) to be bounded from above by the case µ ∼ m. Significant deviations from the above expression can be expected as one approaches this limit [12].…”

Section: A Extremally Polarized Solitonsmentioning

confidence: 97%

“…Both hedgehogs have higher energies (at a fixed particle number) compared to the ground state solitons discussed earlier, and have zero spin and orbital angular momentum. Explicitly, after fixing the particle number to be the same as the polarized solitons (N s hh = N ), we have E s=1 hh ≈ 0.33E and E s=2 hh ≈ 0.17E where E < 0 and N are given in (40). Note that ∆E = E s hh − E > 0.…”

Section: Beyond Ground-state Solitonsmentioning

confidence: 99%

“…12 More generally, many existing studies carried out for scalar dark matter, can be repeated for the case of higherspin dark matter including soliton formation mechanisms [32], halo formation [31], dynamical friction [33], generation of gravitational waves [34], time delays caused in pulsar timing arrays by time-dependent pressures and energy densities [35], black-hole superradiance and 'gravitational atoms' [36], transient vortices [37] etc. Some of these have already been extended to higher-spin fields, see for example, [38][39][40].…”

Section: A Gravitational Interactionsmentioning

confidence: 99%

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Polarized solitons in higher-spin wave dark matter

Jain,

Amin

2021

Preprint

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We first show that the effective non-relativistic theory of gravitationally interacting, massive integer-spin fields (spin-0, 1, and 2 in particular) is described by a 2s + 1 component Schrödinger-Poisson action, where s is the spin of the field. We then construct s + 1 distinct, gravitationally supported solitons in this non-relativistic theory from identically polarized plane waves. Such solitons are extremally polarized, with macroscopically large spin, but no orbital angular momentum. These s + 1 solitons form a basis set, out of which partially polarized solitons can be constructed. All such solitons are ground states, have a spherically symmetric energy density but not field configurations. We discuss how solitons in higher-spin fields can be distinguished from scalar solitons, and potential gravitational and non-gravitational probes of them.

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Section: A Extremally Polarized Solitonsmentioning

confidence: 97%

Section: Beyond Ground-state Solitonsmentioning

confidence: 99%

Section: A Gravitational Interactionsmentioning

confidence: 99%

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Polarized solitons in higher-spin wave dark matter

Jain,

Amin

2021

Preprint

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“…At leading (linear) order in α the interaction Eq. (2.2) can be absorbed into a redefinition of the metric g ij → g ij + αM ij M P [31]. Therefore, the effect of spin-2 ULDM on the detector can be equivalently described by the gravitational effect of an oscillating metric perturbation h ij given by…”

Section: The Shape and Strength Of The Signalmentioning

confidence: 99%

Searching for spin-2 ULDM with gravitational waves interferometers

Armaleo,

Nacir,

Urban

2020

Preprint

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The detection of gravitational waves from merging binaries has ushered in the era of gravitational wave interferometer astronomy. Besides these strong, transient, calamitous events, much weaker signals can be detected if the oscillations are nearly monochromatic and "continuous", that is, coherent over a long time. In this work we show that ultra-light dark matter of spin two, owing to its universal coupling α to Standard Model fields, generates a signal that is akin to but distinct from a continuous gravitational wave. We show that this signal could be detected with current and planned gravitational wave interferometers. In the event of a null detection, current facilities could constrain the coupling to be below α ∼ 10 −7 for frequencies of tens of Hz, corresponding to dark matter masses around the 10 −13 eV mark. Future facilities could further lower these upper limits and extend them to smaller masses down to 10 −18 eV. These limits would be the most stringent bounds on the spin-2 Yukawa fifth force strength, parametrised by α, in the frequency ranges accessible by gravitational wave interferometers. The implementation of this type of searches for gravitational wave interferometers would therefore further our grasp of both dark matter and gravity.

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“…* * Our evolution equations(8) describe the secular evolution of the binary on timescales much longer than the orbital period. It would be interesting to extend our formalism to cover sub-orbital timescales, similar to the treatment of Desjacques et al (2020)66 for binaries perturbed by an oscillating axion field;67,68 we leave this for future work.…”

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confidence: 99%

Bridging the $μ$Hz gap in the gravitational-wave landscape with binary resonance

Blas,

Jenkins

2021

Preprint

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Gravitational-wave (GW) astronomy is transforming our understanding of the Universe by probing phenomena invisible to electromagnetic observatories. A comprehensive exploration of the GW frequency spectrum is essential to fully harness this potential. Remarkably, current methods have left the µHz frequency band almost untouched. Here we show that this µHz gap can be filled by searching for deviations in the orbits of binary systems caused by their resonant interaction with GWs. In particular, we show that laser ranging of the Moon and artificial satellites around the Earth, as well as timing of binary pulsars, may discover the first GW signals in this band, or otherwise set stringent new constraints. To illustrate the discovery potential of these binary resonance searches, we consider the GW signal from a cosmological first-order phase transition, showing that our methods will probe regions of the parameter space that are inaccessible to any other near-future GW mission. We also discuss how our methods can shed light on the possible GW signal detected by NANOGrav, either constraining its spectral properties or even giving an independent confirmation.Our results can be reproduced using the Python code gwresonance, available at this URL.

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Pulsar timing array constraints on spin-2 ULDM

Cited by 23 publications

References 81 publications

Polarized solitons in higher-spin wave dark matter

Polarized solitons in higher-spin wave dark matter

Searching for spin-2 ULDM with gravitational waves interferometers

Bridging the $μ$Hz gap in the gravitational-wave landscape with binary resonance

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