pith. sign in

arxiv: 2607.00840 · v1 · pith:F7Z5PMENnew · submitted 2026-07-01 · ✦ hep-ph · astro-ph.HE

Dark matter energy exchange in stars orbiting supermassive black holes

Stephan A. Meighen-Berger , R. Andrew Gustafson , Nicole F. Bell , Jayden L. Newstead , Sandra Robles , Ian M. Shoemaker This is my paper

Pith reviewed 2026-07-02 09:58 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HE
keywords dark matterenergy exchangestellar orbitssupermassive black holesdark starsscattering cross sectionsgalactic centerfreeze-in
0
0 comments X

The pith

Dark matter scattering can match the luminosity of stars orbiting close to supermassive black holes at cross sections of 10^{-36} cm² for a spiked density profile.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper calculates the average energy a star gains from scattering off dark matter particles during its orbit around the galactic center black hole. For the star S4714 on a very close orbit, this energy input equals the star's luminosity when the dark matter density is spiked and the scattering cross section is around 10^{-36} cm² for MeV to GeV dark matter masses or 5×10^{-38} cm² for lighter masses. This matters to a sympathetic reader because it shows a way stars could become dark stars through energy transfer alone, without dark matter annihilating inside them. The required cross sections fit models where dark matter is produced by freeze-in and do not violate other bounds from cosmic rays or the sun.

Core claim

Stars on tight orbits around the supermassive black hole at the Galactic Center pass through regions where the dark matter density may be strongly enhanced. For a spiked dark matter profile, the exchange reaches the stellar luminosity at σ_χp ∼ 10^{-36} cm² for MeV-GeV masses and σ_χe ∼ 5×10^{-38} cm² for sub-MeV masses, opening a new annihilation-free route toward dark-star phases. These cross sections lie within the range predicted by freeze-in scenarios and are consistent with cosmic-ray-boosted and solar-reflection dark matter constraints.

What carries the argument

The orbit-averaged DM-induced energy exchange rate computed for a star on a relativistic orbit in a spiked dark matter density profile.

If this is right

  • The energy exchange can reach the level of the star's own luminosity.
  • This occurs at cross sections compatible with freeze-in dark matter production.
  • The values remain consistent with constraints from cosmic-ray boosted dark matter and solar reflection.
  • Stars can reach dark-star phases without requiring dark matter annihilation.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the spiked profile is present, measurements of stellar energy output near galactic centers could constrain dark matter scattering cross sections.
  • The mechanism could be tested by comparing predicted and observed luminosities for other known close-orbit stars.
  • Applying this to different galactic centers might reveal similar effects if spikes form there too.

Load-bearing premise

The dark matter density near the supermassive black hole is enhanced in a spiked profile that the star's orbit samples.

What would settle it

Observation or modeling that the dark matter density profile around Sagittarius A* does not have a strong enough spike to make the energy exchange match luminosity at the stated cross sections.

Figures

Figures reproduced from arXiv: 2607.00840 by Ian M. Shoemaker, Jayden L. Newstead, Nicole F. Bell, R. Andrew Gustafson, Sandra Robles, Stephan A. Meighen-Berger.

Figure 1
Figure 1. Figure 1: FIG. 1. Schematic illustration of a star on a highly eccentric [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. DM density as a function of radius. The pink band [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Analytic orbit-averaged DM–proton energy ex [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Analytic orbit-averaged DM-induced energy exchange [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
read the original abstract

Stars on tight orbits around the supermassive black hole at the Galactic Center pass through regions where the dark matter~(DM) density may be strongly enhanced. We compute the orbit-averaged DM-induced energy exchange for S4714 as an example. It is a star on an exceptionally close and relativistic orbit around Sagittarius~A*. For a spiked dark matter profile, the exchange reaches the stellar luminosity at $\sigma_{\chi p} \sim 10^{-36}~\mathrm{cm}^2$ for MeV-GeV masses and $\sigma_{\chi e} \sim 5\times10^{-38}~\mathrm{cm}^2$ for sub-MeV masses, opening a new annihilation-free route toward dark-star phases. These cross sections lie within the range predicted by freeze-in scenarios and are consistent with cosmic-ray--boosted and solar-reflection dark matter constraints.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript computes the orbit-averaged energy exchange rate between dark matter and the star S4714 on its close, relativistic orbit around Sagittarius A*. For an assumed spiked DM density profile, the exchange equals stellar luminosity at σ_χp ∼ 10^{-36} cm² (MeV-GeV masses) and σ_χe ∼ 5×10^{-38} cm² (sub-MeV masses), framing this as an annihilation-free channel toward dark-star phases that lies inside freeze-in and cosmic-ray-boosted constraints.

Significance. If the modeling assumptions hold, the result identifies a new astrophysical signature of DM scattering near SMBHs that connects laboratory-accessible cross sections to observable stellar properties, without invoking annihilation. No machine-checked proofs or public code are reported, but the forward calculation from standard profiles and orbital data is a clear strength.

major comments (2)
  1. [DM profile modeling (abstract and profile section)] The spiked DM density profile is load-bearing for the central claim that the quoted cross sections reach L_star. Without a quantitative sensitivity study showing how the required σ values shift for a non-spiked (e.g., NFW or adiabatically contracted but non-spiked) profile at ∼10^{-3} pc, the result cannot be assessed as lying inside the freeze-in window.
  2. [Energy exchange calculation] The orbit-averaged energy-exchange formula and its numerical evaluation (including integration limits, DM velocity distribution, and relativistic corrections for S4714) are not visible in sufficient detail to verify the quoted cross-section thresholds; this prevents confirmation that the luminosity-matching values are robust.
minor comments (1)
  1. [Abstract] The abstract states the cross sections without quoting the exact spike parameters (e.g., power-law index or normalization radius) used; a one-sentence definition or reference would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We address each major comment below. Where revisions are needed to improve clarity and robustness, we will incorporate them in the revised manuscript.

read point-by-point responses

  1. Referee: [DM profile modeling (abstract and profile section)] The spiked DM density profile is load-bearing for the central claim that the quoted cross sections reach L_star. Without a quantitative sensitivity study showing how the required σ values shift for a non-spiked (e.g., NFW or adiabatically contracted but non-spiked) profile at ∼10^{-3} pc, the result cannot be assessed as lying inside the freeze-in window.

    Authors: The spiked profile is the physically motivated case for the Galactic Center due to adiabatic contraction from SMBH growth, as standard in the literature for such orbits. For non-spiked profiles the DM density drops sharply and the required cross sections would increase substantially, potentially outside the freeze-in window; our claim is therefore scoped to the spiked scenario as a possible new signature. We will add a short quantitative sensitivity paragraph (including order-of-magnitude estimates for NFW and contracted non-spiked cases at the relevant radii) to make this dependence explicit. revision: yes

  2. Referee: [Energy exchange calculation] The orbit-averaged energy-exchange formula and its numerical evaluation (including integration limits, DM velocity distribution, and relativistic corrections for S4714) are not visible in sufficient detail to verify the quoted cross-section thresholds; this prevents confirmation that the luminosity-matching values are robust.

    Authors: We agree that additional detail is required for reproducibility. The orbit average is obtained by integrating the local energy-transfer rate (using the standard DM-star scattering kinematics) along the relativistic orbit of S4714, with the DM velocity distribution taken as isotropic in the spike frame and relativistic corrections applied to the relative velocity and energy transfer. We will insert the explicit integral expression, the adopted integration limits, the form of the velocity distribution, and the treatment of relativistic effects into the methods section of the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity; forward calculation from external profile assumption

full rationale

The derivation computes orbit-averaged energy exchange rates from an input spiked DM density profile, S4714 orbital data, and scattering cross sections, then compares the result to stellar luminosity to obtain required sigma values. No equations reduce outputs to fitted inputs by construction, no self-citations are load-bearing for the central result, and the spiked profile is invoked as a modeling choice rather than derived internally. The calculation is self-contained against external benchmarks and does not exhibit any of the enumerated circular patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the unverified assumption of a spiked DM density profile near Sgr A* and standard stellar parameters for S4714; no free parameters or invented entities are explicitly introduced in the abstract.

axioms (1)
  • domain assumption Dark matter density follows a spiked profile near the supermassive black hole
    Required to reach the luminosity-matching cross sections quoted in the abstract.

pith-pipeline@v0.9.1-grok · 5699 in / 1225 out tokens · 24834 ms · 2026-07-02T09:58:03.064172+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

71 extracted references · 66 canonical work pages · 38 internal anchors

  1. [1]

    SINFONI in the Galactic Center: young stars and IR flares in the central light month

    F. Eisenhaueret al., SINFONI in the Galactic Center: Young stars and IR flares in the central light month, As- trophys. J.628, 246 (2005), arXiv:astro-ph/0502129

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  2. [2]

    On the nature of the fast moving star S2 in the Galactic Center

    F. Martins, S. Gillessen, F. Eisenhauer, R. Genzel, T. Ott, and S. Trippe, On the nature of the fast mov- ing star S2 in the Galactic Center, Astrophys. J. Lett. 672, L119 (2008), arXiv:0711.3344 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  3. [3]

    Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole

    R. Abuteret al.(GRAVITY), Detection of the gravita- tional redshift in the orbit of the star S2 near the Galactic centre massive black hole, Astron. Astrophys.615, L15 (2018), arXiv:1807.09409 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  4. [4]

    Peißker, A

    F. Peißker, A. Eckart, M. Zajaˇ cek, B. Ali, and M. Parsa, S62 and S4711: Indications of a Population of Faint Fast-moving Stars inside the S2 Orbit—S4711 on a 7.6 yr Orbit around Sgr A*, Astrophys. J.899, 50 (2020), arXiv:2008.04764 [astro-ph.GA]

    work page arXiv 2020

  5. [5]

    Dark matter annihilation at the galactic center

    P. Gondolo and J. Silk, Dark matter annihilation at the galactic center, Phys. Rev. Lett.83, 1719 (1999), arXiv:astro-ph/9906391

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  6. [6]

    G. D. Quinlan, L. Hernquist, and S. Sigurdsson, Models of Galaxies with Central Black Holes: Adiabatic Growth in Spherical Galaxies, Astrophys. J.440, 554 (1995), arXiv:astro-ph/9407005

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  7. [7]

    Dark matter distributions around massive black holes: A general relativistic analysis

    L. Sadeghian, F. Ferrer, and C. M. Will, Dark mat- ter distributions around massive black holes: A general relativistic analysis, Phys. Rev. D88, 063522 (2013), arXiv:1305.2619 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  8. [8]

    Time-Dependent Models for Dark Matter at the Galactic Center

    G. Bertone and D. Merritt, Time-dependent models for dark matter at the Galactic Center, Phys. Rev. D72, 103502 (2005), arXiv:astro-ph/0501555

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  9. [9]

    Dark Matter Dynamics and Indirect Detection

    G. Bertone and D. Merritt, Dark matter dynamics and indirect detection, Mod. Phys. Lett. A20, 1021 (2005), arXiv:astro-ph/0504422

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  10. [10]

    Balaji, D

    S. Balaji, D. Sachdeva, F. Sala, and J. Silk, Dark mat- ter spikes around Sgr A* inγ-rays, JCAP08, 063, arXiv:2303.12107 [hep-ph]

    work page arXiv

  11. [11]

    Akita, A

    K. Akita, A. Ibarra, and R. Zimmermann, Dark matter explanations for the neutrino emission from the Seyfert galaxy NGC 1068, arXiv:2507.16539 [hep-ph] (2025)

    work page arXiv 2025

  12. [12]

    Dynamical constraints on a dark matter spike at the Galactic Centre from stellar orbits

    T. Lacroix, Dynamical constraints on a dark matter spike at the Galactic Centre from stellar orbits, Astron. Astro- phys.619, A46 (2018), arXiv:1801.01308 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  13. [13]

    Abd El Dayemet al.(GRAVITY), Improving con- straints on the extended mass distribution in the Galactic center with stellar orbits, Astron

    K. Abd El Dayemet al.(GRAVITY), Improving con- straints on the extended mass distribution in the Galactic center with stellar orbits, Astron. Astrophys.692, A242 (2024), arXiv:2409.12261 [astro-ph.GA]

    work page arXiv 2024

  14. [14]

    Dark stars at the Galactic centre - the main sequence

    P. Scott, M. Fairbairn, and J. Edsjo, Dark stars at the Galactic centre - the main sequence, Mon. Not. Roy. As- tron. Soc.394, 82 (2009), arXiv:0809.1871 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  15. [15]

    I. John, R. K. Leane, and T. Linden, Dark matter scattering constraints from observations of stars sur- rounding Sgr A*, Phys. Rev. D109, 123041 (2024), arXiv:2311.16228 [astro-ph.HE]

    work page arXiv 2024

  16. [16]

    J. F. Acevedo, A. J. Reilly, and L. Santos-Olmsted, Dark Drag Around Sagittarius A* (2025), arXiv:2510.01320 [hep-ph]

    work page arXiv 2025

  17. [17]

    R. A. Gustafson, I. M. Shoemaker, and V. Takhistov, Probing Dark Matter Interactions with Stellar Motion near Sagittarius A* (2025), arXiv:2510.07387 [hep-ph]

    work page arXiv 2025

  18. [18]

    G. Elor, R. McGehee, and A. Pierce, Maximizing Di- rect Detection with Highly Interactive Particle Relic Dark Matter, Phys. Rev. Lett.130, 031803 (2023), arXiv:2112.03920 [hep-ph]

    work page arXiv 2023

  19. [19]

    P. N. Bhattiprolu, G. Elor, R. McGehee, and A. Pierce, Freezing-in hadrophilic dark matter at low reheating tem- peratures, JHEP01, 128, arXiv:2210.15653 [hep-ph]

    work page arXiv

  20. [20]

    J. F. Navarro, C. S. Frenk, and S. D. M. White, The Structure of cold dark matter halos, Astrophys. J.462, 563 (1996), arXiv:astro-ph/9508025

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  21. [21]

    PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection

    M. Cirelli, G. Corcella, A. Hektor, G. Hutsi, M. Kadastik, P. Panci, M. Raidal, F. Sala, and A. Strumia, PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection, JCAP03, 051, [Erratum: JCAP 10, E01 (2012)], arXiv:1012.4515 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  22. [22]

    O. Y. Gnedin and J. R. Primack, Dark Matter Profile in the Galactic Center, Phys. Rev. Lett.93, 061302 (2004), arXiv:astro-ph/0308385

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  23. [23]

    Made-to-Measure models of the Galactic Box/Peanut bulge: stellar and total mass in the bulge region

    M. Portail, C. Wegg, O. Gerhard, and I. Martinez- Valpuesta, Made-to-measure models of the Galactic box/peanut bulge: stellar and total mass in the bulge region, Monthly Notices of the Royal Astronomical Soci- ety448, 713 (2015), arXiv:1502.00633 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  24. [24]

    An estimate of the DM profile in the Galactic bulge region

    F. Iocco and M. Benito, An estimate of the DM profile in the Galactic bulge region, Phys. Dark Univ.15, 90 (2017), arXiv:1611.09861 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  25. [25]

    The Density of Dark Matter in the Galactic Bulge and Implications for Indirect Detection

    D. Hooper, The Density of Dark Matter in the Galac- tic Bulge and Implications for Indirect Detection, Phys. Dark Univ.15, 53 (2017), arXiv:1608.00003 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  26. [26]

    Baumgart, S

    M. Baumgart, S. Bottaro, D. Redigolo, N. L. Rodd, and T. R. Slatyer, Testing real WIMPs with CTAO, JHEP 02, 213, arXiv:2507.15937 [hep-ph]

    work page arXiv

  27. [27]

    T. K. Karydas, F. Scarcella, B. J. Kavanagh, and G. Bertone, On the survival of dark matter spikes: Stellar and compact-object perturbations (2026), arXiv:2606.13761 [astro-ph.GA]

    work page arXiv 2026

  28. [28]

    Gould, Resonant enhancements in wimp capture by the earth, Astrophys

    A. Gould, Resonant enhancements in wimp capture by the earth, Astrophys. J.321, 571 (1987)

    1987

  29. [29]

    Gould, WIMP Distribution in and Evaporation From the Sun, Astrophys

    A. Gould, WIMP Distribution in and Evaporation From the Sun, Astrophys. J.321, 560 (1987)

    1987

  30. [30]

    Modules for Experiments in Stellar Astrophysics (MESA)

    B. Paxton, L. Bildsten, A. Dotter, F. Herwig, P. Lesaffre, and F. Timmes, Modules for Experiments in Stellar As- trophysics (MESA), Astrophysical Journal Supplement Series192, 3 (2011), arXiv:1009.1622 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  31. [31]

    Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars

    B. Paxton, M. Cantiello, P. Arras, L. Bildsten, E. F. Brown, A. Dotter, C. Mankovich, M. H. Montgomery, D. Stello, F. X. Timmes, and R. Townsend, Modules for Experiments in Stellar Astrophysics (MESA): Plan- ets, Oscillations, Rotation, and Massive Stars, The As- trophysical Journal Supplement Series208, 4 (2013), arXiv:1301.0319 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  32. [32]

    Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions

    B. Paxton, P. Marchant, J. Schwab, E. B. Bauer, L. Bild- sten, M. Cantiello, L. Dessart, R. Farmer, H. Hu, N. Langer, R. H. D. Townsend, D. M. Townsley, and F. X. Timmes, Modules for Experiments in Stellar Astro- physics (MESA): Binaries, Pulsations, and Explosions, 11 The Astrophysical Journal Supplement Series220, 15 (2015), arXiv:1506.03146 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  33. [33]

    Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions

    B. Paxtonet al., Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions, Astrophys. J. Suppl.234, 34 (2018), arXiv:1710.08424 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  34. [34]

    Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

    B. Paxton, R. Smolec, J. Schwab, A. Gautschy, L. Bild- sten, M. Cantiello, A. Dotter, R. Farmer, J. A. Goldberg, A. S. Jermyn, S. M. Kanbur, P. Marchant, A. Thoul, R. H. D. Townsend, W. M. Wolf, M. Zhang, and F. X. Timmes, Modules for Experiments in Stellar As- trophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conser...

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  35. [35]

    A. S. Jermynet al.(MESA), Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convec- tion, Energy Conservation, Automatic Differentiation, and Infrastructure, Astrophys. J. Suppl.265, 15 (2023), arXiv:2208.03651 [astro-ph.SR]

    work page arXiv 2023

  36. [36]

    Aalberset al.(LZ), New Constraints on Cos- mic Ray-Boosted Dark Matter from the LUX-ZEPLIN Experiment, Phys

    J. Aalberset al.(LZ), New Constraints on Cos- mic Ray-Boosted Dark Matter from the LUX-ZEPLIN Experiment, Phys. Rev. Lett.134, 241801 (2025), arXiv:2503.18158 [hep-ex]

    work page arXiv 2025

  37. [37]

    Direct detection of dark matter—APPEC committee report*,

    J. Billardet al., Direct detection of dark matter—appec committee report*, Rept. Prog. Phys.85, 056201 (2022), arXiv:2104.07634 [hep-ex]

    work page arXiv 2022

  38. [38]

    Results on MeV-scale dark matter from a gram-scale cryogenic calorimeter operated above ground

    G. Angloheret al.(CRESST), Results on MeV-scale dark matter from a gram-scale cryogenic calorimeter op- erated above ground, Eur. Phys. J. C77, 637 (2017), arXiv:1707.06749 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  39. [39]

    Angloheret al.(CRESST), Testing spin-dependent dark matter interactions with lithium aluminate tar- gets in CRESST-III, Phys

    G. Angloheret al.(CRESST), Testing spin-dependent dark matter interactions with lithium aluminate tar- gets in CRESST-III, Phys. Rev. D106, 092008 (2022), arXiv:2207.07640 [astro-ph.CO]

    work page arXiv 2022

  40. [40]

    Aguilar-Arevaloet al.(DAMIC), Results on low-mass weakly interacting massive particles from a 11 kg-day target exposure of DAMIC at SNOLAB, Phys

    A. Aguilar-Arevaloet al.(DAMIC), Results on low-mass weakly interacting massive particles from a 11 kg-day target exposure of DAMIC at SNOLAB, Phys. Rev. Lett. 125, 241803 (2020), arXiv:2007.15622 [astro-ph.CO]

    work page arXiv 2020

  41. [41]

    Low-Mass Dark Matter Search with the DarkSide-50 Experiment

    P. Agneset al.(DarkSide), Low-Mass Dark Mat- ter Search with the DarkSide-50 Experiment, Phys. Rev. Lett.121, 081307 (2018), arXiv:1802.06994 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  42. [42]

    DarkSide-50 532-day Dark Matter Search with Low-Radioactivity Argon

    P. Agneset al.(DarkSide), DarkSide-50 532-day Dark Matter Search with Low-Radioactivity Argon, Phys. Rev. D98, 102006 (2018), arXiv:1802.07198 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  43. [43]

    Dark Matter Search Results from a One Tonne$\times$Year Exposure of XENON1T

    E. Aprileet al.(XENON), Dark Matter Search Results from a One Ton-Year Exposure of XENON1T, Phys. Rev. Lett.121, 111302 (2018), arXiv:1805.12562 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  44. [44]

    Aprileet al.(XENON), Light Dark Matter Search with Ionization Signals in XENON1T, Phys

    E. Aprileet al.(XENON), Light Dark Matter Search with Ionization Signals in XENON1T, Phys. Rev. Lett. 123, 251801 (2019), arXiv:1907.11485 [hep-ex]

    work page arXiv 2019

  45. [45]

    Sabti, J

    N. Sabti, J. Alvey, M. Escudero, M. Fairbairn, and D. Blas, Refined Bounds on MeV-scale Thermal Dark Sectors from BBN and the CMB, JCAP01, 004, arXiv:1910.01649 [hep-ph]

    work page arXiv 1910

  46. [46]

    Krnjaic and S

    G. Krnjaic and S. D. McDermott, Implications of BBN Bounds for Cosmic Ray Upscattered Dark Matter, Phys. Rev. D101, 123022 (2020), arXiv:1908.00007 [hep-ph]

    work page arXiv 2020

  47. [47]

    Sabti, J

    N. Sabti, J. Alvey, M. Escudero, M. Fairbairn, and D. Blas, Addendum: Refined bounds on MeV-scale ther- mal dark sectors from BBN and the CMB, JCAP08, A01, arXiv:2107.11232 [hep-ph]

    work page arXiv

  48. [48]

    E. O. Nadler, V. Gluscevic, K. K. Boddy, and R. H. Wechsler, Constraints on Dark Matter Microphysics from the Milky Way Satellite Population, Astrophys. J. Lett.878, 32 (2019), [Erratum: Astrophys.J.Lett. 897, L46 (2020), Erratum: Astrophys.J. 897, L46 (2020)], arXiv:1904.10000 [astro-ph.CO]

    work page arXiv 2019

  49. [49]

    H. An, H. Nie, M. Pospelov, J. Pradler, and A. Ritz, Solar reflection of dark matter, Phys. Rev. D104, 103026 (2021), arXiv:2108.10332 [hep-ph]

    work page arXiv 2021

  50. [50]

    Zhanget al.(PandaX), Search for Light Dark Matter with 259 Days of Data in PandaX-4T, Phys

    M. Zhanget al.(PandaX), Search for Light Dark Matter with 259 Days of Data in PandaX-4T, Phys. Rev. Lett. 135, 211001 (2025), arXiv:2507.11930 [hep-ex]

    work page arXiv 2025

  51. [51]

    New Constraints and Prospects for sub-GeV Dark Matter Scattering off Electrons in Xenon

    R. Essig, T. Volansky, and T.-T. Yu, New Constraints and Prospects for sub-GeV Dark Matter Scattering off Electrons in Xenon, Phys. Rev. D96, 043017 (2017), arXiv:1703.00910 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  52. [52]

    Dark matter and the first stars: a new phase of stellar evolution

    D. Spolyar, K. Freese, and P. Gondolo, Dark matter and the first stars: a new phase of stellar evolution, Phys. Rev. Lett.100, 051101 (2008), arXiv:0705.0521 [astro- ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  53. [53]

    Dark Matter capture and annihilation on the First Stars: preliminary estimates

    F. Iocco, Dark Matter Capture and Annihilation on the First Stars: Preliminary Estimates, Astrophys. J. Lett. 677, L1 (2008), arXiv:0802.0941 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  54. [54]

    I. V. Moskalenko and L. Wai, Dark matter burners: Pre- liminary estimates (2006), arXiv:astro-ph/0608535

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  55. [55]

    Dark Stars: A Review

    K. Freese, T. Rindler-Daller, D. Spolyar, and M. Valluri, Dark Stars: A Review, Rept. Prog. Phys.79, 066902 (2016), arXiv:1501.02394 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  56. [56]

    Peißker, A

    F. Peißker, A. Eckart, M. Zajaˇ cek, and S. Britzen, Obser- vation of S4716-a Star with a 4 yr Orbit around Sgr A*, Astrophys. J.933, 49 (2022), arXiv:2207.02142 [astro- ph.GA]

    work page arXiv 2022

  57. [57]

    Abuteret al.(GRAVITY), Astron

    R. Abuteret al.(GRAVITY), Mass distribution in the Galactic Center based on interferometric astrometry of multiple stellar orbits, Astron. Astrophys.657, L12 (2022), arXiv:2112.07478 [astro-ph.GA]

    work page arXiv 2022

  58. [58]

    King’s College London, King’s Computational Research, Engineering and Technology Environment (CREATE) (2026)

    2026

  59. [59]

    The Galactic Center Massive Black Hole and Nuclear Star Cluster

    R. Genzel, F. Eisenhauer, and S. Gillessen, The Galac- tic Center massive black hole and nuclear star cluster, Rev. Mod. Phys.82, 3121 (2010), arXiv:1006.0064 [astro- ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  60. [60]

    The structure of the nuclear stellar cluster of the Milky Way

    R. Schodelet al., The structure of the nuclear stellar cluster of the Milky Way (2007), arXiv:astro-ph/0703178

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  61. [61]

    The nuclear star cluster of the Milky Way

    R. Schoedel, D. Merritt, and A. Eckart, The nuclear star cluster of the Milky Way, J. Phys. Conf. Ser.131, 012044 (2008), arXiv:0810.0204 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  62. [62]

    F. K. Baganoffet al., Chandra x-ray spectroscopic imag- ing of Sgr A* and the central parsec of the Galaxy, As- trophys. J.591, 891 (2003), arXiv:astro-ph/0102151

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  63. [63]

    P. G. Mezger, W. J. Duschl, and R. Zylka, The Galactic Center: a laboratory for AGN?, Astronomy and Astro- physics Review7, 289 (1996)

    1996

  64. [64]

    Betancourt Kamenetskaia, M

    B. Betancourt Kamenetskaia, M. Fujiwara, A. Ibarra, and T. Toma, Dark matter spikes with strongly self- interacting particles, JCAP09, 074, arXiv:2506.12642 [hep-ph]

    work page arXiv

  65. [65]

    D. N. Spergel and P. J. Steinhardt, Observational ev- idence for selfinteracting cold dark matter, Phys. Rev. Lett.84, 3760 (2000), arXiv:astro-ph/9909386

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  66. [66]

    Dark Matter Halos as Particle Colliders: A Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters

    M. Kaplinghat, S. Tulin, and H.-B. Yu, Dark Matter Halos as Particle Colliders: Unified Solution to Small- Scale Structure Puzzles from Dwarfs to Clusters, Phys. 12 Rev. Lett.116, 041302 (2016), arXiv:1508.03339 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  67. [67]

    Zhang and Y

    Z.-C. Zhang and Y. Tang, Velocity distribution of dark matter in spikes around Schwarzschild black holes and effects on gravitational waves from extreme-mass- ratio inspirals, Phys. Rev. D110, 103008 (2024), arXiv:2403.18529 [astro-ph.GA]

    work page arXiv 2024

  68. [68]

    Zhang, H.-C

    Z.-C. Zhang, H.-C. Yuan, and Y. Tang, Universal den- sity and velocity distributions of dark matter around massive black holes, Phys. Rev. D112, 043025 (2025), arXiv:2503.02573 [astro-ph.GA]

    work page arXiv 2025

  69. [69]

    A. K. Drukier, K. Freese, and D. N. Spergel, Detecting Cold Dark Matter Candidates, Phys. Rev. D33, 3495 (1986)

    1986

  70. [70]

    Twelve years of spectroscopic monitoring in the Galactic Center: the closest look at S-stars near the black hole

    M. Habibi, S. Gillessen, F. Martins, F. Eisenhauer, P. M. Plewa, O. Pfuhl, E. George, J. Dexter, I. Waisberg, T. Ott, S. von Fellenberg, M. Baub¨ ock, A. Jimenez- Rosales, and R. Genzel, Twelve Years of Spectroscopic Monitoring in the Galactic Center: The Closest Look at S-stars near the Black Hole, Astrophys. J.847, 120 (2017), arXiv:1708.06353 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  71. [71]

    The GWs from the S-stars revolving around the SMBH at Sgr A*

    R.-G. Cai, T.-B. Liu, and S.-J. Wang, Gws from s- stars revolving around smbh at sgr a**, Commun. Theor. Phys.70, 735 (2018), arXiv:1808.03164 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018