First Results on Dark Matter Substructure from Astrometric Weak Lensing

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

doi:10.1103/physrevlett.125.111101

Cited by 37 publications

(29 citation statements)

References 114 publications

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“…The raw signal, δφ, is found by integrating Eqs. (19), (24), and the subtracted signal, h, is subsequently computed by Eq. (B6).…”

Section: Point-like Subhalo (Pbh)mentioning

confidence: 99%

“…Halos below the dot-dashed-black line corresponding to ρ s = ρ DM cannot make up f = 1 . Also shown in dashed-gray are projections from photometric lensing [12,32], α and µ lensing from astrometric lensing in Gaia data [18][19][20] and diffraction of BH mergers observable in aLIGO [7,56].…”

Section: B Extended Halo Mass Functionsmentioning

confidence: 99%

“…Smaller structures have instead been observed with strong lensing of quasars [13] and with fluctuations in stellar streams [14], both confirming subhalos down to about 10 7 M . 21 cm cosmology [15] for masses in the range 10 6 − 10 8 M , strong gravitational lensing [16] and stellar wakes [17] for M > 10 5 M , astrometric lensing [18][19][20] for M > 1 M , and disruption of compact stellar systems [21] for M > 5 M , have all been proposed to extend constraints on the HMF to lower masses.…”

mentioning

confidence: 99%

“…For sub-solar mass halos, microlensing of stars towards the Large Magellanic Cloud (e.g., MACHO [22], EROS [23], OGLE [24]), Andromeda (e.g. SUBARU [25,26]) or stars in the local neighborhood (from Gaia [19] and KEPLER [27]) constrains sufficiently dense halos to be a sub-dominant component of the dark matter. However, microlensing becomes ineffective in detecting subhalos below ∼ 10 −10 − 10 −11 M [26].…”

mentioning

confidence: 99%

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Observability of dark matter substructure with pulsar timing correlations

Ramani

Trickle

Zurek

2020

J. Cosmol. Astropart. Phys.

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Dark matter substructure on small scales is currently weakly constrained, and its study may shed light on the nature of the dark matter. In this work we study the gravitational effects of dark matter substructure on measured pulsar phases in pulsar timing arrays (PTAs). Due to the stability of pulse phases observed over several years, dark matter substructure around the Earth-pulsar system can imprint discernible signatures in gravitational Doppler and Shapiro delays. We compute pulsar phase correlations induced by general dark matter substructure, and project constraints for a few models such as monochromatic primordial black holes (PBHs), and Cold Dark Matter (CDM)-like NFW subhalos. This work extends our previous analysis, which focused on static or single transiting events, to a stochastic analysis of multiple transiting events. We find that stochastic correlations, in a PTA similar to the Square Kilometer Array (SKA), are uniquely powerful to constrain subhalos as light as ∼ 10 −13 M , with concentrations as low as that predicted by standard CDM.

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“…The raw signal, δφ, is found by integrating Eqs. (19), (24), and the subtracted signal, h, is subsequently computed by Eq. (B6).…”

Section: Point-like Subhalo (Pbh)mentioning

confidence: 99%

Section: B Extended Halo Mass Functionsmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Observability of dark matter substructure with pulsar timing correlations

Ramani

Trickle

Zurek

2020

J. Cosmol. Astropart. Phys.

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“…where r is the distance from the MW center, r s ¼ 18 kpc is the scale radius of the MW halo, and ρ s ¼ 0.003 M ⊙ =pc 3 is the density at that radius (i.e., we assume the same parameters as Ref. [37]). We also assume that all lenses are within 1 kpc of the Sun.…”

Section: A Statistical Formalismmentioning

confidence: 99%

Detecting dark matter subhalos with the Nancy Grace Roman Space Telescope

Pardo

Doré

2021

Phys. Rev. D

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The dark matter subhalo mass function is a promising way of distinguishing between dark matter models. While cold dark matter predicts halos down to Earth-sized masses, other dark matter models typically predict a cutoff in the subhalo mass function. Thus a definitive detection or limits on the existence of subhalos at small masses can give us insight into the nature of dark matter. If these subhalos exist in the Milky Way, they would produce weak lensing signatures, such as modified apparent positions, on background stars. These signatures would generate correlations in the apparent velocities and accelerations of these stars, which could be observable given sufficient astrometric resolution and cadence. The Nancy Grace Roman Space Telescope's exoplanet microlensing survey will be perfectly suited to measuring the acceleration signatures of these halos. Here we forward model these acceleration signatures and explore the Roman Space Telescope's future constraints on lens profiles and populations. We find that the Roman Space Telescope could place competitive bounds on point-source, Gaussian, and Navarro-Frenk-White (NFW) profile lenses that are complementary to other proposed methods. In particular, it could place 95% upper limits on the NFW concentration c 200 < 10 2.5 . We discuss possible systematic effects that could hinder these efforts but argue they should not prevent the Roman Space Telescope from placing strong limits. We also discuss further analysis methods for improving these constraints.

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