Matches in SemOpenAlex for { <https://semopenalex.org/work/W4376272336> ?p ?o ?g. }
- W4376272336 endingPage "440" @default.
- W4376272336 startingPage "428" @default.
- W4376272336 abstract "ABSTRACT A variety of observational campaigns seek to test dark matter models by measuring dark matter subhaloes at low masses. Despite their predicted lack of stars, these subhaloes may be detectable through gravitational lensing or via their gravitational perturbations on stellar streams. To set measurable expectations for subhalo populations within Lambda cold dark matter, we examine 11 Milky Way (MW)-mass haloes from the FIRE-2 baryonic simulations, quantifying the counts and orbital fluxes for subhaloes with properties relevant to stellar stream interactions: masses down to $10^{6}, text{M}_odot$, distances ≲50 kpc of the galactic centre, across z = 0 − 1 (tlookback = 0–8 Gyr). We provide fits to our results and their dependence on subhalo mass, distance, and lookback time, for use in (semi)analytical models. A typical MW-mass halo contains ≈16 subhaloes $gt 10^{7}, text{M}_odot$ (≈1 subhalo $gt 10^{8}, text{M}_odot$) within 50 kpc at z ≈ 0. We compare our results with dark matter-only versions of the same simulations: because they lack a central galaxy potential, they overpredict subhalo counts by 2–10×, more so at smaller distances. Subhalo counts around a given MW-mass galaxy declined over time, being ≈10× higher at z = 1 than at z ≈ 0. Subhaloes have nearly isotropic orbital velocity distributions at z ≈ 0. Across our simulations, we also identified 4 analogues of Large Magellanic Cloud satellite passages; these analogues enhance subhalo counts by 1.4–2.1 times, significantly increasing the expected subhalo population around the MW today. Our results imply an interaction rate of ∼5 per Gyr for a stream like GD-1, sufficient to make subhalo–stream interactions a promising method of measuring dark subhaloes." @default.
- W4376272336 created "2023-05-13" @default.
- W4376272336 creator A5041415725 @default.
- W4376272336 creator A5044296184 @default.
- W4376272336 creator A5063617691 @default.
- W4376272336 creator A5065168624 @default.
- W4376272336 creator A5089098555 @default.
- W4376272336 creator A5091350146 @default.
- W4376272336 date "2023-05-12" @default.
- W4376272336 modified "2023-10-17" @default.
- W4376272336 title "The dark side of FIRE: predicting the population of dark matter subhaloes around Milky Way-mass galaxies" @default.
- W4376272336 cites W1481345939 @default.
- W4376272336 cites W1907817908 @default.
- W4376272336 cites W1966671643 @default.
- W4376272336 cites W1976412804 @default.
- W4376272336 cites W1986805436 @default.
- W4376272336 cites W2010581546 @default.
- W4376272336 cites W2011301426 @default.
- W4376272336 cites W2033933651 @default.
- W4376272336 cites W2036024475 @default.
- W4376272336 cites W2052002005 @default.
- W4376272336 cites W2052333057 @default.
- W4376272336 cites W2088139983 @default.
- W4376272336 cites W2098776230 @default.
- W4376272336 cites W2101349161 @default.
- W4376272336 cites W2105171788 @default.
- W4376272336 cites W2135403967 @default.
- W4376272336 cites W2136626788 @default.
- W4376272336 cites W2139031955 @default.
- W4376272336 cites W2140908947 @default.
- W4376272336 cites W2216753448 @default.
- W4376272336 cites W2221167480 @default.
- W4376272336 cites W2301571137 @default.
- W4376272336 cites W2315142564 @default.
- W4376272336 cites W2359505960 @default.
- W4376272336 cites W2396703009 @default.
- W4376272336 cites W2410361993 @default.
- W4376272336 cites W2429438195 @default.
- W4376272336 cites W2510412236 @default.
- W4376272336 cites W2512489826 @default.
- W4376272336 cites W2528129257 @default.
- W4376272336 cites W2557326983 @default.
- W4376272336 cites W2564821084 @default.
- W4376272336 cites W2573445935 @default.
- W4376272336 cites W2589317285 @default.
- W4376272336 cites W2601316834 @default.
- W4376272336 cites W2691626934 @default.
- W4376272336 cites W2774653944 @default.
- W4376272336 cites W2782994775 @default.
- W4376272336 cites W2796687148 @default.
- W4376272336 cites W2797463651 @default.
- W4376272336 cites W2798663476 @default.
- W4376272336 cites W2808702599 @default.
- W4376272336 cites W2888532099 @default.
- W4376272336 cites W2904789576 @default.
- W4376272336 cites W2940527889 @default.
- W4376272336 cites W2952261829 @default.
- W4376272336 cites W2953653843 @default.
- W4376272336 cites W2963357806 @default.
- W4376272336 cites W2971437713 @default.
- W4376272336 cites W3005079263 @default.
- W4376272336 cites W3020671156 @default.
- W4376272336 cites W3034360320 @default.
- W4376272336 cites W3039537179 @default.
- W4376272336 cites W3086007137 @default.
- W4376272336 cites W3087827168 @default.
- W4376272336 cites W3092667560 @default.
- W4376272336 cites W3098069588 @default.
- W4376272336 cites W3098221464 @default.
- W4376272336 cites W3098451528 @default.
- W4376272336 cites W3098887528 @default.
- W4376272336 cites W3098976132 @default.
- W4376272336 cites W3099007478 @default.
- W4376272336 cites W3099863439 @default.
- W4376272336 cites W3099878876 @default.
- W4376272336 cites W3100140790 @default.
- W4376272336 cites W3101608901 @default.
- W4376272336 cites W3103170606 @default.
- W4376272336 cites W3104052343 @default.
- W4376272336 cites W3105420829 @default.
- W4376272336 cites W3105443865 @default.
- W4376272336 cites W3105465984 @default.
- W4376272336 cites W3106918088 @default.
- W4376272336 cites W3123752787 @default.
- W4376272336 cites W3125070545 @default.
- W4376272336 cites W3125864581 @default.
- W4376272336 cites W3190785892 @default.
- W4376272336 cites W3206680518 @default.
- W4376272336 cites W4213259675 @default.
- W4376272336 cites W4282972831 @default.
- W4376272336 cites W4283277259 @default.
- W4376272336 cites W4288079944 @default.
- W4376272336 cites W4291287649 @default.
- W4376272336 cites W4292510800 @default.
- W4376272336 cites W4307813519 @default.
- W4376272336 cites W4312047277 @default.
- W4376272336 cites W4316015667 @default.
- W4376272336 cites W4318541252 @default.