Pulsar Timing Probes of Primordial Black Holes and Subhalos

Article
Report number	arXiv:1901.04490
Title	Pulsar Timing Probes of Primordial Black Holes and Subhalos
Author(s)	Dror, Jeff A. (LBL, Berkeley ; UC, Berkeley) ; Ramani, Harikrishnan (LBL, Berkeley ; UC, Berkeley) ; Trickle, Tanner (LBL, Berkeley ; UC, Berkeley) ; Zurek, Kathryn M. (CERN ; LBL, Berkeley ; UC, Berkeley)
Publication	2019-07-13
Imprint	2019-01-14
Number of pages	18
Note	18 pages, 6 figures
In:	Phys. Rev. D 100 (2019) 023003
DOI	10.1103/PhysRevD.100.023003
Subject category	hep-ph ; Particle Physics - Phenomenology ; astro-ph.HE ; Astrophysics and Astronomy ; astro-ph.CO ; Astrophysics and Astronomy
Abstract	Pulsars act as accurate clocks, sensitive to gravitational redshift and acceleration induced by transiting clumps of matter. We study the sensitivity of pulsar timing arrays (PTAs) to single transiting compact objects, focusing on primordial black holes and compact subhalos in the mass range from $10^{-12} M _{\odot}$ to well above $100 M_\odot$. We find that the Square Kilometer Array can constrain such objects to be a subdominant component of the dark matter over this entire mass range, with sensitivity to a dark matter sub-component reaching the sub-percent level over significant parts of this range. We also find that PTAs offer an opportunity to probe substantially less dense objects than lensing because of the large effective radius over which such objects can be observed, and we quantify the subhalo concentration parameters which can be constrained.
Copyright/License	Publication: © 2019-2024 authors preprint: (License: arXiv nonexclusive-distrib 1.0)

$Sensitivity distance (as defined in the text) as a function of the compact object mass $M$ for PTA Doppler and Shapiro searches, as as well as supernova and stellar lensing. The red curves in the left and right panels are the mass enclosed functions, $ r _{ {\rm enc}} $, for the NFW and UCMH-like profiles (defined in the text) respectively for three different concentration parameters $c$, and two different viral masses, $M_\text{vir} = 10^{-7} \, M_\odot, \, 10^{-1} \, M_\odot$. Where these red curves intersect the sensitivity distance curves corresponds to the effective subhalo enclosed mass, $M^*$, to which the various searches are sensitive. See text for more details.$ $Sensitivity distance (as defined in the text) as a function of the compact object mass $M$ for PTA Doppler and Shapiro searches, as as well as supernova and stellar lensing. The red curves in the left and right panels are the mass enclosed functions, $ r _{ {\rm enc}} $, for the NFW and UCMH-like profiles (defined in the text) respectively for three different concentration parameters $c$, and two different viral masses, $M_\text{vir} = 10^{-7} \, M_\odot, \, 10^{-1} \, M_\odot$. Where these red curves intersect the sensitivity distance curves corresponds to the effective subhalo enclosed mass, $M^*$, to which the various searches are sensitive. See text for more details.$ $Comparison of the reach of pulsar timing data in scenario SC3 ({\color{c2} {\bf red}}) to lensing ({\color{gray} {\bf gray}}) experiments, for NFW halos of different concentration parameters, $c$. With concentration parameters below $10^8$, PTA searches rapidly become more sensitive than lensing searches. The PTA constraints are cut-off when $ r_{ {\rm enc}} $ never crosses the sensitivity radius for any $ M $. For the concentration parameters chosen, this only occurs for the Doppler dynamic search leading to a sharp rise in the constraints at $M _{ {\rm vir}} = 10^{-9}~M_\odot$ for $ c = 100$.$ Show more plots

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