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      "affiliations": [
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          "country": "Italy", 
          "value": "Scuola Superiore Meridionale, Largo San Marcellino 10, Naples, 80138, Italy", 
          "organization": "Scuola Superiore Meridionale"
        }, 
        {
          "country": "Italy", 
          "value": "Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cinthia, Naples, 80126, Italy", 
          "organization": "Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cinthia"
        }
      ], 
      "surname": "D\u2019Agostino", 
      "email": "rocco.dagostino@unina.it", 
      "full_name": "D\u2019Agostino, Rocco", 
      "given_names": "Rocco"
    }, 
    {
      "affiliations": [
        {
          "country": "Macedonia", 
          "value": "Physics Department, State University of Tetovo, Ilinden Street nn, Tetovo, 1200, North Macedonia", 
          "organization": "State University of Tetovo"
        }
      ], 
      "surname": "Jusufi", 
      "email": "kimet.jusufi@unite.edu.mk", 
      "full_name": "Jusufi, Kimet", 
      "given_names": "Kimet"
    }, 
    {
      "affiliations": [
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          "country": "Italy", 
          "value": "Scuola Superiore Meridionale, Largo San Marcellino 10, Naples, 80138, Italy", 
          "organization": "Scuola Superiore Meridionale"
        }, 
        {
          "country": "Italy", 
          "value": "Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cinthia, Naples, 80126, Italy", 
          "organization": "Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cinthia"
        }, 
        {
          "country": "Italy", 
          "value": "Dipartimento di Fisica \u201cE. Pancini\u201d, Universit\u00e0 di Napoli \u201cFederico II\u201d, Via Cintia, Naples, 80126, Italy", 
          "organization": "Universit\u00e0 di Napoli \u201cFederico II\u201d"
        }
      ], 
      "surname": "Capozziello", 
      "email": "capozziello@unina.it", 
      "full_name": "Capozziello, Salvatore", 
      "given_names": "Salvatore"
    }
  ], 
  "titles": [
    {
      "source": "Springer", 
      "title": "Testing Yukawa cosmology at the Milky Way and M31 galactic scales"
    }
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      "value": "10.1140/epjc/s10052-024-12741-6"
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      "journal_title": "European Physical Journal C", 
      "material": "article", 
      "journal_volume": "84", 
      "artid": "s10052-024-12741-6", 
      "year": 2024, 
      "page_start": "1", 
      "journal_issue": "4"
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      "url": "https://creativecommons.org/licenses//by/4.0", 
      "license": "CC-BY-4.0"
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  "copyright": [
    {
      "holder": "The Author(s)", 
      "year": "2024"
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  "control_number": "84610", 
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  "abstracts": [
    {
      "source": "Springer", 
      "value": "We address the galaxy rotation curves through the Yukawa gravitational potential emerging as a correction of the Newtonian potential in extended theories of gravity. On the one hand, we consider the contribution of the galactic bulge, galactic disk, and the dark matter halo of the Navarro\u2013Frenk\u2013White profile, in the framework of the standard  $$\\Lambda $$  <math> <mi>\u039b</mi> </math>  CDM model. On the other hand, we use modified Yukawa gravity to show that the rotational velocity of galaxies can be addressed successfully without the need for dark matter. In Yukawa gravity, we recover MOND and show that dark matter might be seen as an apparent effect due to the modification of the law of gravitation in terms of two parameters: the coupling constant  $$\\alpha $$  <math> <mi>\u03b1</mi> </math>   and the characteristic length  $$\\lambda $$  <math> <mi>\u03bb</mi> </math>  . We thus test our theoretical scenario using the Milky Way and M31 rotation velocity curves. In particular, we place observational constraints on the free parameters of Yukawa cosmology through the Monte Carlo method and then compare our results with the predictions of the  $$\\Lambda $$  <math> <mi>\u039b</mi> </math>  CDM paradigm by making use of Bayesian information criteria. Specifically, we find that  $$\\lambda $$  <math> <mi>\u03bb</mi> </math>   is constrained to be of the order of kpc, while cosmological data suggest  $$\\lambda $$  <math> <mi>\u03bb</mi> </math>   of the order of Gpc. To explain this discrepancy, we argue that there is a fundamental limitation in measuring  $$\\lambda $$  <math> <mi>\u03bb</mi> </math>   due to the role of quantum mechanics on cosmological scales."
    }
  ], 
  "imprints": [
    {
      "date": "2024-04-11", 
      "publisher": "Springer"
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}