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N-body Simulations of Large-Scale Structure in the Generalized Cubic Covariant Galileon Model

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arxiv 2608.06499 v1 pith:Y7VPZAFR submitted 2026-08-06 astro-ph.CO

Luís Atayde , Noemi Frusciante , Baojiu Li This is my paper · ORCID
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abstract

We present the first N-body simulations of structure formation in the Generalized Cubic Covariant Galileon (GCCG) model. This theory extends the cubic covariant Galileon through power-law kinetic and cubic derivative interactions and admits tracker solutions leading to late-time cosmic acceleration. Previous studies of GCCG have mostly focused on the background, linear perturbations, or semi-analytic nonlinear prescriptions. Here we implement the nonlinear scalar-field equation in the ECOSMOG adaptive-mesh refinement code, allowing us to follow the coupled evolution of matter clustering and Vainshtein screening in the fully nonlinear regime. We quantify the impact of GCCG on the nonlinear matter power spectrum and compare the simulation results with predictions from the halo-model reaction approach. For the parameter choices considered, the GCCG model enhances the matter power spectrum relative to the corresponding QCDM cosmology, with the effect increasing towards low redshift and reaching approximately $7\%$ at $z=0$ in the transition to the nonlinear regime. At smaller scales, the enhancement decreases as a consequence of Vainshtein screening. We find that the reaction framework captures the qualitative behaviour of the simulations, while residual differences appear on deeply nonlinear scales. We also analyse the abundance of dark matter haloes, finding an enhancement relative to QCDM that becomes more pronounced towards lower redshift and in the high-mass tail. These simulations provide the first nonlinear calibration of structure formation in GCCG and establish the range of validity of efficient semi-analytical predictions for applications to forthcoming large-scale-structure surveys.

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Works this paper leans on

64 extracted references · 4 canonical work pages

  1. [1]

    A. G. Riesset al.(Supernova Search Team), Astron. J. 116, 1009 (1998), arXiv:astro-ph/9805201

    arXiv 1998

  2. [2]

    Perlmutteret al.(Supernova Cosmology Project), As- trophys

    S. Perlmutteret al.(Supernova Cosmology Project), As- trophys. J.517, 565 (1999), arXiv:astro-ph/9812133

    arXiv 1999

  3. [3]

    Aghanimet al.(Planck), Astron

    N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]

    arXiv 2020

  4. [4]

    D. J. Eisensteinet al.(SDSS), Astrophys. J.633, 560 (2005), arXiv:astro-ph/0501171

    arXiv 2005

  5. [5]

    Alamet al.(BOSS), Mon

    S. Alamet al.(BOSS), Mon. Not. Roy. Astron. Soc.470, 2617 (2017), arXiv:1607.03155 [astro-ph.CO]

    arXiv 2017

  6. [6]

    Di Valentinoet al., Astropart

    E. Di Valentinoet al., Astropart. Phys.131, 102605 (2021), arXiv:2008.11284 [astro-ph.CO]

    arXiv 2021

  7. [7]

    Weinberg, Rev

    S. Weinberg, Rev. Mod. Phys.61, 1 (1989)

    1989

  8. [8]

    S. M. Carroll, Living Rev. Rel.4, 1 (2001), arXiv:astro- ph/0004075

    arXiv 2001

Show all 64 references
  1. [9]

    Akramiet al.(CANTATA),Modified Gravity and Cos- mology

    Y. Akramiet al.(CANTATA),Modified Gravity and Cos- mology. An Update by the CANTATA Network, edited by E. N. Saridakis, R. Lazkoz, V. Salzano, P. Vargas Moniz, S. Capozziello, J. Beltr´ an Jim´ enez, M. De Laurentis, and G. J. Olmo (Springer, 2021) arXiv:2105.12582 [gr-qc]

    2021 arXiv

  2. [10]

    A. G. Adameet al.(DESI), JCAP04, 012 (2025), arXiv:2404.03000 [astro-ph.CO]

    2025 arXiv

  3. [11]

    A. G. Adameet al.(DESI), JCAP01, 124 (2025), arXiv:2404.03001 [astro-ph.CO]

    2025 arXiv

  4. [12]

    Guet al.(DESI), (2025), arXiv:2504.06118 [astro- ph.CO]

    G. Guet al.(DESI), (2025), arXiv:2504.06118 [astro- ph.CO]

    2025

  5. [13]

    Abdul Karimet al.(DESI), (2025), arXiv:2503.14738 [astro-ph.CO]

    M. Abdul Karimet al.(DESI), (2025), arXiv:2503.14738 [astro-ph.CO]

    2025 arXiv

  6. [14]

    T. M. C. Abbottet al.(DES), (2026), arXiv:2605.27221 [astro-ph.CO]

    2026 arXiv

  7. [15]

    G. Ye, M. Martinelli, B. Hu, and A. Silvestri, Phys. Rev. Lett.134, 181002 (2025), arXiv:2407.15832 [astro- ph.CO]

    2025 arXiv

  8. [16]

    W. J. Wolf, C. Garc ´ ıa-Garc ´ ıa, T. Anton, and P. G. Fer- reira, (2025), arXiv:2504.07679 [astro-ph.CO]

    2025 arXiv

  9. [17]

    W. J. Wolf, P. G. Ferreira, and C. Garc ´ ıa-Garc ´ ıa, Phys. Rev. D111, L041303 (2025), arXiv:2409.17019 [astro- ph.CO]

    2025 arXiv

  10. [18]

    G. W. Horndeski, Int. J. Theor. Phys.10, 363 (1974)

    1974

  11. [19]

    Deffayet, X

    C. Deffayet, X. Gao, D. A. Steer, and G. Zahariade, Phys. Rev. D84, 064039 (2011), arXiv:1103.3260 [hep- th]

    2011 arXiv

  12. [20]

    Kobayashi, M

    T. Kobayashi, M. Yamaguchi, and J. Yokoyama, Prog. Theor. Phys.126, 511 (2011), arXiv:1105.5723 [hep-th]

    2011 arXiv

  13. [21]

    Ostrogradsky, Mem

    M. Ostrogradsky, Mem. Acad. St. Petersbourg6, 385 (1850)

  14. [22]

    R. P. Woodard, Scholarpedia10, 32243 (2015), arXiv:1506.02210 [hep-th]

    2015 arXiv

  15. [23]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]

    2017 arXiv

  16. [24]

    De Felice and S

    A. De Felice and S. Tsujikawa, JCAP1202, 007 (2012), arXiv:1110.3878 [gr-qc]

    2012 arXiv

  17. [25]

    Frusciante, S

    N. Frusciante, S. Peirone, L. Atayde, and A. De Fe- lice, Phys. Rev. D101, 064001 (2020), arXiv:1912.07586 [astro-ph.CO]

    2020 arXiv

  18. [26]

    Giacomello, A

    F. Giacomello, A. De Felice, and S. Ansoldi, JCAP03, 038 (2019), arXiv:1811.10885 [astro-ph.CO]

    2019 arXiv

  19. [27]

    J. A. Kable, G. Benevento, N. Frusciante, A. De Fe- lice, and S. Tsujikawa, JCAP09, 002 (2022), arXiv:2111.10432 [astro-ph.CO]

    2022 arXiv

  20. [28]

    A. I. Vainshtein, Phys. Lett. B39, 393 (1972)

    1972

  21. [29]

    Joyce, B

    A. Joyce, B. Jain, J. Khoury, and M. Trodden, Phys. Rept.568, 1 (2015), arXiv:1407.0059 [astro-ph.CO]

    2015 arXiv

  22. [30]

    against fullN-body simulations [34] in the limit in which the GCCG model resembles the original Cubic Covariant Galileon model [35], achieving∼5% accuracy across a wide range of scales and redshifts, and used to forecast percent-level constraints on the extra GCCG pa- rameters...

  23. [31]

    Atayde, N

    L. Atayde, N. Frusciante, B. Bose, S. Casas, and B. Li, Phys. Rev. D110, 024082 (2024), arXiv:2404.11471 [astro-ph.CO]

    2024 arXiv

  24. [32]

    Cataneo, L

    M. Cataneo, L. Lombriser, C. Heymans, A. Mead, A. Barreira, S. Bose, and B. Li, Mon. Not. Roy. Astron. Soc.488, 2121 (2019), arXiv:1812.05594 [astro-ph.CO]

    2019 arXiv

  25. [33]

    B. Bose, M. Cataneo, T. Tr¨ oster, Q. Xia, C. Heymans, and L. Lombriser, Mon. Not. Roy. Astron. Soc.498, 4650 (2020), arXiv:2005.12184 [astro-ph.CO]

    2020 arXiv

  26. [34]

    B. Bose, B. S. Wright, M. Cataneo, A. Pourtsidou, C. Giocoli, L. Lombriser, I. G. McCarthy, M. Baldi, S. Pfeifer, and Q. Xia., Mon. Not. Roy. Astron. Soc. 508, 2479 (2021), arXiv:2105.12114 [astro-ph.CO]

    2021 arXiv

  27. [35]

    Barreira, B

    A. Barreira, B. Li, W. A. Hellwing, C. M. Baugh, and S. Pascoli, JCAP10, 027 (2013), arXiv:1306.3219 [astro- ph.CO]

    2013 arXiv

  28. [36]

    Deffayet, G

    C. Deffayet, G. Esposito-Farese, and A. Vikman, Phys. Rev.D79, 084003 (2009), arXiv:0901.1314 [hep-th]

    2009 arXiv

  29. [37]

    Boseet al., Mon

    B. Boseet al., Mon. Not. Roy. Astron. Soc.536, 664 (2024), arXiv:2406.13667 [astro-ph.CO]

    2024 arXiv

  30. [38]

    Li, G.-B

    B. Li, G.-B. Zhao, R. Teyssier, and K. Koyama, JCAP 01, 051 (2012), arXiv:1110.1379 [astro-ph.CO]

    2012 arXiv

  31. [39]

    Puchwein, M

    E. Puchwein, M. Baldi, and V. Springel, Mon. Not. Roy. Astron. Soc.436, 348 (2013), arXiv:1305.2418 [astro- 12 ph.CO]

    2013 arXiv

  32. [40]

    Llinares, D

    C. Llinares, D. F. Mota, and H. A. Winther, Astron. Astrophys.562, A78 (2014), arXiv:1307.6748 [astro- ph.CO]

    2014 arXiv

  33. [41]

    Schmidt, Phys

    F. Schmidt, Phys. Rev. D80, 123003 (2009), arXiv:0910.0235 [astro-ph.CO]

    2009 arXiv

  34. [42]

    Schmidt, Phys

    F. Schmidt, Phys. Rev. D80, 043001 (2009), arXiv:0905.0858 [astro-ph.CO]

    2009 arXiv

  35. [43]

    Li, G.-B

    B. Li, G.-B. Zhao, and K. Koyama, JCAP05, 023 (2013), arXiv:1303.0008 [astro-ph.CO]

    2013 arXiv

  36. [44]

    Hassani and L

    F. Hassani and L. Lombriser, Mon. Not. Roy. Astron. Soc.497, 1885 (2020), arXiv:2003.05927 [astro-ph.CO]

    2020 arXiv

  37. [45]

    Nouri-Zonoz, F

    A. Nouri-Zonoz, F. Hassani, E. Bellini, and M. Kunz, (2025), arXiv:2511.04676 [astro-ph.CO]

    2025

  38. [46]

    Ganjooet al., (2026), arXiv:2604.15434 [astro- ph.CO]

    H. Ganjooet al., (2026), arXiv:2604.15434 [astro- ph.CO]

    2026 arXiv

  39. [47]

    N. O. Woodcock, S. Bose, Y. Gao, and B. Li, (2026), arXiv:2607.24940 [astro-ph.CO]

    2026 arXiv

  40. [48]

    Deffayet, O

    C. Deffayet, O. Pujolas, I. Sawicki, and A. Vikman, JCAP1010, 026 (2010), arXiv:1008.0048 [hep-th]

    2010 arXiv

  41. [49]

    Kobayashi, M

    T. Kobayashi, M. Yamaguchi, and J. Yokoyama, Phys. Rev. Lett.105, 231302 (2010), arXiv:1008.0603 [hep-th]

    2010 arXiv

  42. [50]

    Barreira, B

    A. Barreira, B. Li, C. M. Baugh, and S. Pascoli, JCAP 1311, 056 (2013), arXiv:1308.3699 [astro-ph.CO]

    2013 arXiv

  43. [51]

    Barreira, B

    A. Barreira, B. Li, C. M. Baugh, and S. Pascoli, jcap8, 059 (2014), arXiv:1406.0485

    2014 arXiv

  44. [52]

    J. Renk, M. Zumalacarregui, F. Montanari, and A. Bar- reira, JCAP1710, 020 (2017), arXiv:1707.02263 [astro- ph.CO]

    2017 arXiv

  45. [53]

    I. S. Albuquerque, N. Frusciante, F. Pace, and C. Schimd, Phys. Rev. D109, 023535 (2024), arXiv:2401.04096 [astro-ph.CO]

    2024 arXiv

  46. [54]

    Bellini and I

    E. Bellini and I. Sawicki, arXiv:1404.3713 [astro-ph, physics:gr-qc] (2014), arXiv: 1404.3713

    2014 arXiv

  47. [55]

    Teyssier, Astron

    R. Teyssier, Astron. Astrophys.385, 337 (2002), arXiv:astro-ph/0111367

    2002 arXiv

  48. [56]

    Davis, B

    A.-C. Davis, B. Li, D. F. Mota, and H. A. Winther, Astrophys. J.748, 61 (2012), arXiv:1108.3081 [astro- ph.CO]

    2012 arXiv

  49. [57]

    Brax, A.-C

    P. Brax, A.-C. Davis, B. Li, H. A. Winther, and G.- B. Zhao, JCAP04, 029 (2013), arXiv:1303.0007 [astro- ph.CO]

    2013 arXiv

  50. [58]

    P. Brax, C. van de Bruck, A.-C. Davis, B. Li, and D. J. Shaw, Phys. Rev. D83, 104026 (2011), arXiv:1102.3692 [astro-ph.CO]

    2011 arXiv

  51. [59]

    Becker, C

    C. Becker, C. Arnold, B. Li, and L. Heisenberg, JCAP 10, 055 (2020), arXiv:2007.03042 [astro-ph.CO]

    2020 arXiv

  52. [60]

    Crocce, S

    M. Crocce, S. Pueblas, and R. Scoccimarro, Mon. Not. Roy. Astron. Soc.373, 369 (2006), arXiv:astro- ph/0606505

    2006

  53. [61]

    Springel, Mon

    V. Springel, Mon. Not. Roy. Astron. Soc.364, 1105 (2005), arXiv:astro-ph/0505010

    2005 arXiv

  54. [62]

    POWMES: Measuring the Power Spectrum in an N-body Simulation,

    S. Colombi and D. Novikov, “POWMES: Measuring the Power Spectrum in an N-body Simulation,” Astro- physics Source Code Library, record ascl:1110.017 (2011), ascl:1110.017

    2011

  55. [63]

    P. S. Behroozi, R. H. Wechsler, and H.-Y. Wu, Astro- phys. J.762, 109 (2013), arXiv:1110.4372 [astro-ph.CO]

    2013 arXiv

  56. [64]

    pynbody: N-Body/SPH analysis for python,

    A. Pontzen, R. Roˇ skar, G. Stinson, and R. Woods, “pynbody: N-Body/SPH analysis for python,” Astro- physics Source Code Library, record ascl:1305.002 (2013), ascl:1305.002

    2013

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