The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters
- Autores
- Meneghetti, Massimo; Ragagnin, Antonio; Borgani, Stefano; Calura, Francesco; Despali, Giulia; Giocoli, Carlo; Granato, Gian Luigi; Grillo, Claudio; Moscardini, Lauro; Rasia, Elena; Rosati, Piero; Angora, Giuseppe; Bassini, Luigi; Bergamini, Pietro; Caminha, Gabriel B.; Granata, Giovanni; Mercurio, Amata; Metcalf, Robert Benton; Natarajan, Priyamvada; Nonino, Mario; Pignataro, Giada Venusta; Ragone Figueroa, Cinthia Judith; Vanzella, Eros; Acebron, Ana; Dolag, Klaus; Murante, Giuseppe; Taffoni, Giuliano; Tornatore, Luca; Tortorelli, Luca; Valentini, Milena
- Año de publicación
- 2022
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. An excess of galaxy galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the cold-dark-matter (CDM) cosmological model has recently been reported. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in CDM cosmology. Aims. We quantify the impact of the numerical resolution and active galactic nucleus (AGN) feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations. Methods. We analyze cluster-size halos (M200 > 5 × 1014 M ) simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Our analysis focuses on galaxies with Einstein radii in the range 000 :5 = E = 300. Results. We find that improving the mass resolution by factors of 10 and 25, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor of between 3 and 6. However, we notice that such simulations form overly massive galaxies whose contribution to the lensing cross section would be significant but that their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross sections are galaxies with smaller masses that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent from simulations. Conclusion. Based on these results, we reaffirm the tension between observations of GGSL and theoretical expectations in the framework of the ?CDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty simultaneously reproducing the stellar mass function and the internal structure of galaxies.
Fil: Meneghetti, Massimo. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Ragagnin, Antonio. Universidad de Bologna; Italia. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Borgani, Stefano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Calura, Francesco. Istituto Nazionale di Astrofisica; Italia
Fil: Despali, Giulia. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Giocoli, Carlo. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Granato, Gian Luigi. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Grillo, Claudio. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Moscardini, Lauro. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Rasia, Elena. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Rosati, Piero. Università di Ferrara; Italia
Fil: Angora, Giuseppe. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Bassini, Luigi. Universitat Zurich; Suiza
Fil: Bergamini, Pietro. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Caminha, Gabriel B.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Granata, Giovanni. Università degli Studi di Milano; Italia
Fil: Mercurio, Amata. Istituto Nazionale di Astrofisica; Italia
Fil: Metcalf, Robert Benton. Universidad de Bologna; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Natarajan, Priyamvada. University of Yale; Estados Unidos
Fil: Nonino, Mario. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Pignataro, Giada Venusta. Istituto Di Radioastronomia; Italia. Universidad de Bologna; Italia
Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Istituto Nazionale di Fisica Nucleare; Italia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Vanzella, Eros. Istituto Nazionale di Astrofisica; Italia
Fil: Acebron, Ana. Università degli Studi di Milano; Italia
Fil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Ludwig Maximilians Universitat; Alemania
Fil: Murante, Giuseppe. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Taffoni, Giuliano. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Tornatore, Luca. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Tortorelli, Luca. Ludwig Maximilians Universitat; Alemania
Fil: Valentini, Milena. Ludwig Maximilians Universitat; Alemania - Materia
-
DARK MATTER
GALAXIES: CLUSTERS: GENERAL
GRAVITATIONAL LENSING: STRONG - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/203218
Ver los metadatos del registro completo
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The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clustersMeneghetti, MassimoRagagnin, AntonioBorgani, StefanoCalura, FrancescoDespali, GiuliaGiocoli, CarloGranato, Gian LuigiGrillo, ClaudioMoscardini, LauroRasia, ElenaRosati, PieroAngora, GiuseppeBassini, LuigiBergamini, PietroCaminha, Gabriel B.Granata, GiovanniMercurio, AmataMetcalf, Robert BentonNatarajan, PriyamvadaNonino, MarioPignataro, Giada VenustaRagone Figueroa, Cinthia JudithVanzella, ErosAcebron, AnaDolag, KlausMurante, GiuseppeTaffoni, GiulianoTornatore, LucaTortorelli, LucaValentini, MilenaDARK MATTERGALAXIES: CLUSTERS: GENERALGRAVITATIONAL LENSING: STRONGhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. An excess of galaxy galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the cold-dark-matter (CDM) cosmological model has recently been reported. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in CDM cosmology. Aims. We quantify the impact of the numerical resolution and active galactic nucleus (AGN) feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations. Methods. We analyze cluster-size halos (M200 > 5 × 1014 M ) simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Our analysis focuses on galaxies with Einstein radii in the range 000 :5 = E = 300. Results. We find that improving the mass resolution by factors of 10 and 25, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor of between 3 and 6. However, we notice that such simulations form overly massive galaxies whose contribution to the lensing cross section would be significant but that their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross sections are galaxies with smaller masses that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent from simulations. Conclusion. Based on these results, we reaffirm the tension between observations of GGSL and theoretical expectations in the framework of the ?CDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty simultaneously reproducing the stellar mass function and the internal structure of galaxies.Fil: Meneghetti, Massimo. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Ragagnin, Antonio. Universidad de Bologna; Italia. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Borgani, Stefano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Calura, Francesco. Istituto Nazionale di Astrofisica; ItaliaFil: Despali, Giulia. Ruprecht Karls Universitat Heidelberg; AlemaniaFil: Giocoli, Carlo. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Granato, Gian Luigi. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Grillo, Claudio. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Moscardini, Lauro. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Rasia, Elena. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Rosati, Piero. Università di Ferrara; ItaliaFil: Angora, Giuseppe. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Bassini, Luigi. Universitat Zurich; SuizaFil: Bergamini, Pietro. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Caminha, Gabriel B.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Granata, Giovanni. Università degli Studi di Milano; ItaliaFil: Mercurio, Amata. Istituto Nazionale di Astrofisica; ItaliaFil: Metcalf, Robert Benton. Universidad de Bologna; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Natarajan, Priyamvada. University of Yale; Estados UnidosFil: Nonino, Mario. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Pignataro, Giada Venusta. Istituto Di Radioastronomia; Italia. Universidad de Bologna; ItaliaFil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Istituto Nazionale di Fisica Nucleare; Italia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Vanzella, Eros. Istituto Nazionale di Astrofisica; ItaliaFil: Acebron, Ana. Università degli Studi di Milano; ItaliaFil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Ludwig Maximilians Universitat; AlemaniaFil: Murante, Giuseppe. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Taffoni, Giuliano. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Tornatore, Luca. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Tortorelli, Luca. Ludwig Maximilians Universitat; AlemaniaFil: Valentini, Milena. Ludwig Maximilians Universitat; AlemaniaEDP Sciences2022-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/203218Meneghetti, Massimo; Ragagnin, Antonio; Borgani, Stefano; Calura, Francesco; Despali, Giulia; et al.; The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters; EDP Sciences; Astronomy and Astrophysics; 668; A188; 12-2022; 1-140004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202243779info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2022/12/aa43779-22/aa43779-22.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:26:37Zoai:ri.conicet.gov.ar:11336/203218instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:26:38.299CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| title |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| spellingShingle |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters Meneghetti, Massimo DARK MATTER GALAXIES: CLUSTERS: GENERAL GRAVITATIONAL LENSING: STRONG |
| title_short |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| title_full |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| title_fullStr |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| title_full_unstemmed |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| title_sort |
The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters |
| dc.creator.none.fl_str_mv |
Meneghetti, Massimo Ragagnin, Antonio Borgani, Stefano Calura, Francesco Despali, Giulia Giocoli, Carlo Granato, Gian Luigi Grillo, Claudio Moscardini, Lauro Rasia, Elena Rosati, Piero Angora, Giuseppe Bassini, Luigi Bergamini, Pietro Caminha, Gabriel B. Granata, Giovanni Mercurio, Amata Metcalf, Robert Benton Natarajan, Priyamvada Nonino, Mario Pignataro, Giada Venusta Ragone Figueroa, Cinthia Judith Vanzella, Eros Acebron, Ana Dolag, Klaus Murante, Giuseppe Taffoni, Giuliano Tornatore, Luca Tortorelli, Luca Valentini, Milena |
| author |
Meneghetti, Massimo |
| author_facet |
Meneghetti, Massimo Ragagnin, Antonio Borgani, Stefano Calura, Francesco Despali, Giulia Giocoli, Carlo Granato, Gian Luigi Grillo, Claudio Moscardini, Lauro Rasia, Elena Rosati, Piero Angora, Giuseppe Bassini, Luigi Bergamini, Pietro Caminha, Gabriel B. Granata, Giovanni Mercurio, Amata Metcalf, Robert Benton Natarajan, Priyamvada Nonino, Mario Pignataro, Giada Venusta Ragone Figueroa, Cinthia Judith Vanzella, Eros Acebron, Ana Dolag, Klaus Murante, Giuseppe Taffoni, Giuliano Tornatore, Luca Tortorelli, Luca Valentini, Milena |
| author_role |
author |
| author2 |
Ragagnin, Antonio Borgani, Stefano Calura, Francesco Despali, Giulia Giocoli, Carlo Granato, Gian Luigi Grillo, Claudio Moscardini, Lauro Rasia, Elena Rosati, Piero Angora, Giuseppe Bassini, Luigi Bergamini, Pietro Caminha, Gabriel B. Granata, Giovanni Mercurio, Amata Metcalf, Robert Benton Natarajan, Priyamvada Nonino, Mario Pignataro, Giada Venusta Ragone Figueroa, Cinthia Judith Vanzella, Eros Acebron, Ana Dolag, Klaus Murante, Giuseppe Taffoni, Giuliano Tornatore, Luca Tortorelli, Luca Valentini, Milena |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
DARK MATTER GALAXIES: CLUSTERS: GENERAL GRAVITATIONAL LENSING: STRONG |
| topic |
DARK MATTER GALAXIES: CLUSTERS: GENERAL GRAVITATIONAL LENSING: STRONG |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Context. An excess of galaxy galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the cold-dark-matter (CDM) cosmological model has recently been reported. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in CDM cosmology. Aims. We quantify the impact of the numerical resolution and active galactic nucleus (AGN) feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations. Methods. We analyze cluster-size halos (M200 > 5 × 1014 M ) simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Our analysis focuses on galaxies with Einstein radii in the range 000 :5 = E = 300. Results. We find that improving the mass resolution by factors of 10 and 25, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor of between 3 and 6. However, we notice that such simulations form overly massive galaxies whose contribution to the lensing cross section would be significant but that their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross sections are galaxies with smaller masses that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent from simulations. Conclusion. Based on these results, we reaffirm the tension between observations of GGSL and theoretical expectations in the framework of the ?CDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty simultaneously reproducing the stellar mass function and the internal structure of galaxies. Fil: Meneghetti, Massimo. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Ragagnin, Antonio. Universidad de Bologna; Italia. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Borgani, Stefano. Università degli Studi di Trieste; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Calura, Francesco. Istituto Nazionale di Astrofisica; Italia Fil: Despali, Giulia. Ruprecht Karls Universitat Heidelberg; Alemania Fil: Giocoli, Carlo. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Granato, Gian Luigi. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina Fil: Grillo, Claudio. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Moscardini, Lauro. Universidad de Bologna; Italia. Istituto Nazionale di Fisica Nucleare; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Rasia, Elena. Institute For Fundamental Physics Of The Universe; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Rosati, Piero. Università di Ferrara; Italia Fil: Angora, Giuseppe. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Bassini, Luigi. Universitat Zurich; Suiza Fil: Bergamini, Pietro. Università degli Studi di Milano; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Caminha, Gabriel B.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania Fil: Granata, Giovanni. Università degli Studi di Milano; Italia Fil: Mercurio, Amata. Istituto Nazionale di Astrofisica; Italia Fil: Metcalf, Robert Benton. Universidad de Bologna; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Natarajan, Priyamvada. University of Yale; Estados Unidos Fil: Nonino, Mario. Istituto Nazionale di Fisica Nucleare; Italia Fil: Pignataro, Giada Venusta. Istituto Di Radioastronomia; Italia. Universidad de Bologna; Italia Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina. Istituto Nazionale di Fisica Nucleare; Italia. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina Fil: Vanzella, Eros. Istituto Nazionale di Astrofisica; Italia Fil: Acebron, Ana. Università degli Studi di Milano; Italia Fil: Dolag, Klaus. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Ludwig Maximilians Universitat; Alemania Fil: Murante, Giuseppe. Istituto Nazionale di Fisica Nucleare; Italia Fil: Taffoni, Giuliano. Istituto Nazionale di Fisica Nucleare; Italia Fil: Tornatore, Luca. Istituto Nazionale di Fisica Nucleare; Italia Fil: Tortorelli, Luca. Ludwig Maximilians Universitat; Alemania Fil: Valentini, Milena. Ludwig Maximilians Universitat; Alemania |
| description |
Context. An excess of galaxy galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the cold-dark-matter (CDM) cosmological model has recently been reported. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in CDM cosmology. Aims. We quantify the impact of the numerical resolution and active galactic nucleus (AGN) feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations. Methods. We analyze cluster-size halos (M200 > 5 × 1014 M ) simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Our analysis focuses on galaxies with Einstein radii in the range 000 :5 = E = 300. Results. We find that improving the mass resolution by factors of 10 and 25, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor of between 3 and 6. However, we notice that such simulations form overly massive galaxies whose contribution to the lensing cross section would be significant but that their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross sections are galaxies with smaller masses that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent from simulations. Conclusion. Based on these results, we reaffirm the tension between observations of GGSL and theoretical expectations in the framework of the ?CDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty simultaneously reproducing the stellar mass function and the internal structure of galaxies. |
| publishDate |
2022 |
| dc.date.none.fl_str_mv |
2022-12 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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http://hdl.handle.net/11336/203218 Meneghetti, Massimo; Ragagnin, Antonio; Borgani, Stefano; Calura, Francesco; Despali, Giulia; et al.; The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters; EDP Sciences; Astronomy and Astrophysics; 668; A188; 12-2022; 1-14 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/203218 |
| identifier_str_mv |
Meneghetti, Massimo; Ragagnin, Antonio; Borgani, Stefano; Calura, Francesco; Despali, Giulia; et al.; The probability of galaxy- galaxy strong lensing events in hydrodynamical simulations of galaxy clusters; EDP Sciences; Astronomy and Astrophysics; 668; A188; 12-2022; 1-14 0004-6361 CONICET Digital CONICET |
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eng |
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eng |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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