Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter
Ultralight scalars with a typical mass of the order <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−<...
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| Format: | Article |
| Language: | English |
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MDPI AG
2022-08-01
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| Series: | Universe |
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| Online Access: | https://www.mdpi.com/2218-1997/8/8/419 |
| _version_ | 1797407583245434880 |
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| author | Héctor J. de Vega Norma G. Sanchez |
| author_facet | Héctor J. de Vega Norma G. Sanchez |
| author_sort | Héctor J. de Vega |
| collection | DOAJ |
| description | Ultralight scalars with a typical mass of the order <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV and light scalars forming a Bose–Einstein condensate (BEC) exhibit a Jeans length in the kpc scale and were therefore proposed as dark matter (DM) candidates. Our treatment here is generic, independent of the particle physics model and applies to all DM BEC, in both in or out of equilibrium situations. Two observed quantities crucially constrain DM in an inescapable way: the average DM density <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub></semantics></math></inline-formula> and the phase-space density <i>Q</i>. The observed values of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub></semantics></math></inline-formula> and <i>Q</i> in galaxies today constrain both the possibility to form a BEC, and the DM mass <i>m</i>. These two constraints robustly exclude the axion DM that decouples after inflation. Moreover, the value <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV can only be obtained with a number of ultrarelativistic degrees of freedom at decoupling in the trillions, which is impossible for decoupling in the radiation dominated era. In addition, we find for the axion vacuum misalignment scenario that axions are produced strongly out of thermal equilibrium and that the axion mass in such a scenario turns to be <b>17 orders of magnitude</b> too large to reproduce the observed galactic structures. Moreover, we also consider inhomogenous gravitationally bounded BEC’s supported by the bosonic quantum pressure independently of any particular particle physics scenario. For a typical size <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>R</mi><mo>∼</mo></mrow></semantics></math></inline-formula> kpc and compact object masses <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>M</mi><mo>∼</mo><msup><mn>10</mn><mn>7</mn></msup><mspace width="0.277778em"></mspace><msub><mi>M</mi><mo>⊙</mo></msub></mrow></semantics></math></inline-formula> they remarkably lead to the same particle mass <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV as the BEC free-streaming length. However, the phase-space density for the gravitationally bounded BEC’s turns out to be more than <b>sixty orders of magnitude</b> smaller than the galaxy-observed values. We conclude that the BEC cannot be the total DM. The axion can be candidates to be only part of the DM of the universe. Besides, an axion in the mili-eV scale may be a relevant source of dark energy through the zero point cosmological quantum fluctuations. |
| first_indexed | 2024-03-09T03:44:40Z |
| format | Article |
| id | doaj.art-9c3e05fd47054043a911557367095548 |
| institution | Directory Open Access Journal |
| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-03-09T03:44:40Z |
| publishDate | 2022-08-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Universe |
| spelling | doaj.art-9c3e05fd47054043a9115573670955482023-12-03T14:36:17ZengMDPI AGUniverse2218-19972022-08-018841910.3390/universe8080419Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark MatterHéctor J. de Vega0Norma G. Sanchez1CNRS LPTHE, Sorbonne Université, Université Pierre et Marie Curie UPMC, CEDEX 05, 75005 Paris, FranceCNRS LERMA PSL-Observatoire de Paris, Sorbonne Université and The Chalonge–de Vega International School Center, 75014 Paris, FranceUltralight scalars with a typical mass of the order <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV and light scalars forming a Bose–Einstein condensate (BEC) exhibit a Jeans length in the kpc scale and were therefore proposed as dark matter (DM) candidates. Our treatment here is generic, independent of the particle physics model and applies to all DM BEC, in both in or out of equilibrium situations. Two observed quantities crucially constrain DM in an inescapable way: the average DM density <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub></semantics></math></inline-formula> and the phase-space density <i>Q</i>. The observed values of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub></semantics></math></inline-formula> and <i>Q</i> in galaxies today constrain both the possibility to form a BEC, and the DM mass <i>m</i>. These two constraints robustly exclude the axion DM that decouples after inflation. Moreover, the value <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV can only be obtained with a number of ultrarelativistic degrees of freedom at decoupling in the trillions, which is impossible for decoupling in the radiation dominated era. In addition, we find for the axion vacuum misalignment scenario that axions are produced strongly out of thermal equilibrium and that the axion mass in such a scenario turns to be <b>17 orders of magnitude</b> too large to reproduce the observed galactic structures. Moreover, we also consider inhomogenous gravitationally bounded BEC’s supported by the bosonic quantum pressure independently of any particular particle physics scenario. For a typical size <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>R</mi><mo>∼</mo></mrow></semantics></math></inline-formula> kpc and compact object masses <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>M</mi><mo>∼</mo><msup><mn>10</mn><mn>7</mn></msup><mspace width="0.277778em"></mspace><msub><mi>M</mi><mo>⊙</mo></msub></mrow></semantics></math></inline-formula> they remarkably lead to the same particle mass <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>m</mi><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>22</mn></mrow></msup></mrow></semantics></math></inline-formula> eV as the BEC free-streaming length. However, the phase-space density for the gravitationally bounded BEC’s turns out to be more than <b>sixty orders of magnitude</b> smaller than the galaxy-observed values. We conclude that the BEC cannot be the total DM. The axion can be candidates to be only part of the DM of the universe. Besides, an axion in the mili-eV scale may be a relevant source of dark energy through the zero point cosmological quantum fluctuations.https://www.mdpi.com/2218-1997/8/8/419dark matteraxionsBose-Einstein condensatephase-space densitygalaxy structuregalaxy data |
| spellingShingle | Héctor J. de Vega Norma G. Sanchez Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter Universe dark matter axions Bose-Einstein condensate phase-space density galaxy structure galaxy data |
| title | Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter |
| title_full | Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter |
| title_fullStr | Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter |
| title_full_unstemmed | Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter |
| title_short | Galaxy Phase-Space Density Data Preclude That Bose–Einstein Condensate Be the Total Dark Matter |
| title_sort | galaxy phase space density data preclude that bose einstein condensate be the total dark matter |
| topic | dark matter axions Bose-Einstein condensate phase-space density galaxy structure galaxy data |
| url | https://www.mdpi.com/2218-1997/8/8/419 |
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