Erratum: Gamma Rays from Ultracompact Primordial Dark Matter Minihalos [Phys. Rev. Lett.<b>103</b>, 211301 (2009)]

Scott, Pat; Sivertsson, Sofia

doi:10.1103/physrevlett.105.119902

Cited by 48 publications

(120 citation statements)

References 2 publications

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“…The halo density required to power a dark star of a given mass and luminosity can be estimated using Equation (14) in Iocco et al (2008). The self-annihilation time t SA for a halo with a given dark matter density can then be obtained by, e.g., inverting Equation (6) in Scott & Sivertsson (2009). The self-annihilation times obtained in this manner are rather approximate, relying on a number of assumptions we already know to be violated in the first stars (a constant halo self-annihilation rate and the constant infall of WIMPs from a uniform, unbound dark matter halo with an assumed velocity structure).…”

Section: Stellar Structure and Evolutionmentioning

confidence: 99%

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

Zackrisson¹,

Scott²,

Rydberg³

et al. 2010

ApJ

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The first stars in the history of the universe are likely to form in the dense central regions of ∼10 5 -10 6 M cold dark matter halos at z ≈ 10-50. The annihilation of dark matter particles in these environments may lead to the formation of so-called dark stars, which are predicted to be cooler, larger, more massive, and potentially more long-lived than conventional population III stars. Here, we investigate the prospects of detecting high-redshift dark stars with the upcoming James Webb Space Telescope (JWST). We find that all dark stars with masses up to 10 3 M are intrinsically too faint to be detected by JWST at z > 6. However, by exploiting foreground galaxy clusters as gravitational telescopes do, certain varieties of cool (T eff 30,000 K) dark stars should be within reach at redshifts up to z ≈ 10. If the lifetimes of dark stars are sufficiently long, many such objects may also congregate inside the first galaxies. We demonstrate that this could give rise to peculiar features in the integrated spectra of galaxies at high redshifts, provided that dark stars make up at least ∼1% of the total stellar mass in such objects.

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Section: Stellar Structure and Evolutionmentioning

confidence: 99%

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

Zackrisson¹,

Scott²,

Rydberg³

et al. 2010

ApJ

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“…One outstanding prediction of cosmological simulations using cold dark matter particles is that the Milky Way halo should be heavily populated with thousands of smaller dark matter subhalos as a result of the hierarchical assembly process (Klypin et al 1999;Moore et al 1999;Springel et al 2008). Dark matter subhalos would include any dark matter configuration, from those hosting the largest known dwarf spheroidal galaxies in the Milky Way to the lightest predicted dark matter substructures with masses around 10 −4 M e (Ricotti & Gould 2009;Scott & Sivertsson 2009). Conceptually in this scenario, the bulk of the subhalo population is made up by small-scale dark matter substructures with limited or null star formation, which would be almost impossible to detect in existing optical surveys.…”

Section: Introductionmentioning

confidence: 99%

3fgl Demographics Outside the Galactic Plane Using Supervised Machine Learning: Pulsar and Dark Matter Subhalo Interpretations

Mirabal

Charles

Ferrara

et al. 2016

ApJ

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Nearly one-third of the sources listed in the Third Fermi Large Area Telescope (LAT) catalog (3FGL) remain unassociated. It is possible that predicted and even unanticipated gamma-ray source classes are present in these data waiting to be discovered. Taking advantage of the excellent spectral capabilities achieved by the Fermi LAT, we use machine-learning classifiers (Random Forest and XGBoost) to pinpoint potentially novel source classes in the unassociated 3FGL sample outside the Galactic plane. Here we report a total of 34 high-confidence Galactic candidates at. The currently favored standard astrophysical interpretations for these objects are pulsars or low-luminosity globular clusters hosting millisecond pulsars (MSPs). Yet these objects could also be interpreted as dark matter annihilation taking place in ultra-faint dwarf galaxies or dark matter subhalos. Unfortunately, Fermi LAT spectra are not sufficient to break degeneracies between the different scenarios. Careful visual inspection of archival optical images reveals no obvious evidence for low-luminosity globular clusters or ultra-faint dwarf galaxies inside the 95% error ellipses. If these are pulsars, this would bring the total number of MSPs at   b 5 | | to 106, down to an energy flux ≈4.0 × 10 −12 erg cm −2 s −1 between 100 MeV and 100 GeV. We find this number to be in excellent agreement with predictions from a new population synthesis of MSPs that predicts 100-126 highlatitude 3FGL MSPs depending on the choice of high-energy emission model. If, however, these are dark matter substructures, we can place upper limits on the number of Galactic subhalos surviving today and on dark matter annihilation cross sections. These limits are beginning to approach the canonical thermal relic cross section for dark matter particle masses below ∼100 GeV in the bottom quark (bb) annihilation channel.

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“…Due to their early formation, the central regions of UCMHs would have a high dark matter (DM) density. If DM is in the form of Weakly Interacting Massive Particles (WIMPs), WIMP annihilation within UCMHs may lead to an observable gamma-ray signal [6,7].…”

Section: Introductionmentioning

confidence: 99%

“…Scott & Sivertsson [7] have investigated gamma-ray emission from UCMHs formed from perturbations which * ppxaj1@nottingham.ac.uk † anne.green@nottingham.ac.uk enter the horizon at three different epochs in the early Universe: e + e − annihilation, and the QCD and electroweak (EW) phase transitions. They find that an UCMH corresponding to the e + e − annihilation epoch, which has present day mass M UCMH (z = 0) ∼ 10 2 M ⊙ , could be detected by the Fermi satellite or current Air Cherenkov telescopes (ACTs), at a distance of 100 pc.…”

Section: Introductionmentioning

confidence: 99%

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

Josan¹,

Green²

2010

Phys. Rev. D

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Ultracompact minihalos (UCMHs) are dense dark matter structures which can form from large density perturbations shortly after matter-radiation equality. If dark matter is in the form of Weakly Interacting Massive Particles (WIMPs), then UCMHs may be detected via their gamma-ray emission. We investigate how the Fermi satellite could constrain the abundance of UCMHs and place limits on the power spectrum of the primordial curvature perturbation. Detection by Fermi would put a lower limit on the UCMH halo fraction. The smallest detectable halo fraction, fUCMH > ∼ 10 −7 , is for MUCMH ∼ 10 3 M⊙. If gamma-ray emission from UCMHs is not detected, an upper limit can be placed on the halo fraction. The bound is tightest, fUCMH < ∼ 10 −5 , for MUCMH ∼ 10 5 M⊙. The resulting upper limit on the power spectrum of the primordial curvature perturbation in the event of non-detection is in the range PR < ∼ 10 −6.5 − 10 −6 on scales k ∼ 10 1 − 10 6 Mpc −1 . This is substantially tighter than the existing constraints from primordial black hole formation on these scales, however it assumes that dark matter is in the form of WIMPs and UCMHs are not disrupted during the formation of the Milky Way halo.

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Erratum: Gamma Rays from Ultracompact Primordial Dark Matter Minihalos [Phys. Rev. Lett.103, 211301 (2009)]

Cited by 48 publications

References 2 publications

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

3fgl Demographics Outside the Galactic Plane Using Supervised Machine Learning: Pulsar and Dark Matter Subhalo Interpretations

Gamma rays from ultracompact minihalos: Potential constraints on the primordial curvature perturbation

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