Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images

Autores
Martin, G.; Bazkiaei, A.E.; Spavone, M.; Iodice, E.; Mihos, J.C.; Montes, M.; Benavides Blanco, Jose Antonio; Brough, S.; Carlin, J.L.; Collins, C.A.; Duc, P.A.; Gómez, F.A.; Galaz, G.; Hernández Toledo, H.M.; Jackson, R.A.; Kaviraj, S.; Knapen, J.H.; Martínez-Lombilla, C.; Mcgee, S.; O'ryan, D.; Prole, D.J.; Rich, R.M.; Román, J.; Shah, E.A.; Starkenburg, T.K.; Watkins, A.E.; Zaritsky, D.; Pichon, C.; Armus, L.; Bianconi, M.; Buitrago, F.; Busá, I.; Davis, F.; Demarco, R.; Desmons, A.; Garciá, P.; Graham, A.W.; Holwerda, B.; Hon, D.S.-H.; Khalid, A.; Klehammer, J.; Klutse, D.Y.; Lazar, I.; Nair, P.; Noakes-Kettel, E.A.; Rutkowski, M.; Saha, K.; Sahu, N.; Sola, E.; Vázquez Mata, J.A.; Vera-Casanova, A.; Yoon, I.
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilizing automated techniques and human visual classification in conjunction with realistic mock images produced using the NewHorizon cosmological simulation, we investigate the nature, frequency, and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-yr depth of the Legacy Survey of Space and Time (30-31 mag arcsec-2), falling to 60 per cent assuming a shallower final depth of 29.5 mag arcsec-2. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M* ∼1011.5 M⊙). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterization of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimized, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z < 0.2).
Fil: Martin, G.. University of Arizona; Estados Unidos. Korea Astronomy And Space Science Institute; China
Fil: Bazkiaei, A.E.. Macquarie University; Australia. The Australian Research Council Centre Of Excellence For All Sky Astrophysics In 3 Dimensions; Australia
Fil: Spavone, M.. Istituto Nazionale di Astrofisica; Italia
Fil: Iodice, E.. Istituto Nazionale di Astrofisica; Italia
Fil: Mihos, J.C.. Case Western Reserve University; Estados Unidos
Fil: Montes, M.. Space Telescope Science Institute; Estados Unidos
Fil: Benavides Blanco, Jose Antonio. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Brough, S.. Unsw Sydney; Australia
Fil: Carlin, J.L.. Rubin Observatory Project Office; Estados Unidos
Fil: Collins, C.A.. Liverpool John Moores University; Reino Unido
Fil: Duc, P.A.. Centre National de la Recherche Scientifique; Francia
Fil: Gómez, F.A.. Universidad de La Serena; Chile
Fil: Galaz, G.. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; Chile
Fil: Hernández Toledo, H.M.. Universidad Nacional Autónoma de México; México
Fil: Jackson, R.A.. Yonsei University; Corea del Sur
Fil: Kaviraj, S.. University Of Hertfordshire; Reino Unido
Fil: Knapen, J.H.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Martínez-Lombilla, C.. Unsw Sydney; Australia
Fil: Mcgee, S.. The University Of Birmingham (tub);
Fil: O'ryan, D.. Lancaster University; Reino Unido
Fil: Prole, D.J.. Macquarie University; Australia
Fil: Rich, R.M.. University of California at Los Angeles; Estados Unidos
Fil: Román, J.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Shah, E.A.. University of California at Davis; Estados Unidos
Fil: Starkenburg, T.K.. Northwestern University; Estados Unidos
Fil: Watkins, A.E.. University Of Hertfordshire; Reino Unido
Fil: Zaritsky, D.. University of Arizona; Estados Unidos
Fil: Pichon, C.. Korea Institute For Advanced Study; China. Université Pierre et Marie Curie; Francia. University of Edinburgh; Reino Unido
Fil: Armus, L.. Infrared Processing & Estados Unidos
Fil: Bianconi, M.. The University Of Birmingham (tub);
Fil: Buitrago, F.. Universidade de Lisboa; Portugal. Universidad de Valladolid; España
Fil: Busá, I.. Osservatorio Astrofisico Di Catania; Italia
Fil: Davis, F.. University Of Hertfordshire; Reino Unido
Fil: Demarco, R.. Universidad de Concepci Ón; Chile
Fil: Desmons, A.. Unsw Sydney; Australia
Fil: Garciá, P.. Universidad Internacional de Valencia; España
Fil: Graham, A.W.. Swinburne University Of Technology; Australia
Fil: Holwerda, B.. University of Louisville; Estados Unidos
Fil: Hon, D.S.-H.. Swinburne University Of Technology; Australia
Fil: Khalid, A.. Unsw Sydney; Australia
Fil: Klehammer, J.. Centre National de la Recherche Scientifique; Francia
Fil: Klutse, D.Y.. Astrophysics Resear Ch Centre; Reino Unido
Fil: Lazar, I.. University Of Hertfordshire; Reino Unido
Fil: Nair, P.. The University Of Alabama; Estados Unidos
Fil: Noakes-Kettel, E.A.. University Of Hertfordshire; Reino Unido
Fil: Rutkowski, M.. Minnesota State University; Estados Unidos
Fil: Saha, K.. Inter-university Centre For Astronomy And Astrophysics India; India
Fil: Sahu, N.. Swinburne University Of Technology; Australia
Fil: Sola, E.. Centre National de la Recherche Scientifique; Francia
Fil: Vázquez Mata, J.A.. Universidad Nacional Autónoma de México; México
Fil: Vera-Casanova, A.. Istituto Nazionale di Astrofisica; Italia
Fil: Yoon, I.. National Radio Astronomy Observatory; Estados Unidos
Materia
GALAXIES: INTERACTIONS
GALAXIES: STRUCTURE
METHODS: NUMERICAL
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/202956
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/202956
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock imagesMartin, G.Bazkiaei, A.E.Spavone, M.Iodice, E.Mihos, J.C.Montes, M.Benavides Blanco, Jose AntonioBrough, S.Carlin, J.L.Collins, C.A.Duc, P.A.Gómez, F.A.Galaz, G.Hernández Toledo, H.M.Jackson, R.A.Kaviraj, S.Knapen, J.H.Martínez-Lombilla, C.Mcgee, S.O'ryan, D.Prole, D.J.Rich, R.M.Román, J.Shah, E.A.Starkenburg, T.K.Watkins, A.E.Zaritsky, D.Pichon, C.Armus, L.Bianconi, M.Buitrago, F.Busá, I.Davis, F.Demarco, R.Desmons, A.Garciá, P.Graham, A.W.Holwerda, B.Hon, D.S.-H.Khalid, A.Klehammer, J.Klutse, D.Y.Lazar, I.Nair, P.Noakes-Kettel, E.A.Rutkowski, M.Saha, K.Sahu, N.Sola, E.Vázquez Mata, J.A.Vera-Casanova, A.Yoon, I.GALAXIES: INTERACTIONSGALAXIES: STRUCTUREMETHODS: NUMERICALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilizing automated techniques and human visual classification in conjunction with realistic mock images produced using the NewHorizon cosmological simulation, we investigate the nature, frequency, and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-yr depth of the Legacy Survey of Space and Time (30-31 mag arcsec-2), falling to 60 per cent assuming a shallower final depth of 29.5 mag arcsec-2. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M* ∼1011.5 M⊙). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterization of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimized, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z < 0.2).Fil: Martin, G.. University of Arizona; Estados Unidos. Korea Astronomy And Space Science Institute; ChinaFil: Bazkiaei, A.E.. Macquarie University; Australia. The Australian Research Council Centre Of Excellence For All Sky Astrophysics In 3 Dimensions; AustraliaFil: Spavone, M.. Istituto Nazionale di Astrofisica; ItaliaFil: Iodice, E.. Istituto Nazionale di Astrofisica; ItaliaFil: Mihos, J.C.. Case Western Reserve University; Estados UnidosFil: Montes, M.. Space Telescope Science Institute; Estados UnidosFil: Benavides Blanco, Jose Antonio. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Brough, S.. Unsw Sydney; AustraliaFil: Carlin, J.L.. Rubin Observatory Project Office; Estados UnidosFil: Collins, C.A.. Liverpool John Moores University; Reino UnidoFil: Duc, P.A.. Centre National de la Recherche Scientifique; FranciaFil: Gómez, F.A.. Universidad de La Serena; ChileFil: Galaz, G.. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; ChileFil: Hernández Toledo, H.M.. Universidad Nacional Autónoma de México; MéxicoFil: Jackson, R.A.. Yonsei University; Corea del SurFil: Kaviraj, S.. University Of Hertfordshire; Reino UnidoFil: Knapen, J.H.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; EspañaFil: Martínez-Lombilla, C.. Unsw Sydney; AustraliaFil: Mcgee, S.. The University Of Birmingham (tub);Fil: O'ryan, D.. Lancaster University; Reino UnidoFil: Prole, D.J.. Macquarie University; AustraliaFil: Rich, R.M.. University of California at Los Angeles; Estados UnidosFil: Román, J.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; EspañaFil: Shah, E.A.. University of California at Davis; Estados UnidosFil: Starkenburg, T.K.. Northwestern University; Estados UnidosFil: Watkins, A.E.. University Of Hertfordshire; Reino UnidoFil: Zaritsky, D.. University of Arizona; Estados UnidosFil: Pichon, C.. Korea Institute For Advanced Study; China. Université Pierre et Marie Curie; Francia. University of Edinburgh; Reino UnidoFil: Armus, L.. Infrared Processing &amp; Estados UnidosFil: Bianconi, M.. The University Of Birmingham (tub);Fil: Buitrago, F.. Universidade de Lisboa; Portugal. Universidad de Valladolid; EspañaFil: Busá, I.. Osservatorio Astrofisico Di Catania; ItaliaFil: Davis, F.. University Of Hertfordshire; Reino UnidoFil: Demarco, R.. Universidad de Concepci Ón; ChileFil: Desmons, A.. Unsw Sydney; AustraliaFil: Garciá, P.. Universidad Internacional de Valencia; EspañaFil: Graham, A.W.. Swinburne University Of Technology; AustraliaFil: Holwerda, B.. University of Louisville; Estados UnidosFil: Hon, D.S.-H.. Swinburne University Of Technology; AustraliaFil: Khalid, A.. Unsw Sydney; AustraliaFil: Klehammer, J.. Centre National de la Recherche Scientifique; FranciaFil: Klutse, D.Y.. Astrophysics Resear Ch Centre; Reino UnidoFil: Lazar, I.. University Of Hertfordshire; Reino UnidoFil: Nair, P.. The University Of Alabama; Estados UnidosFil: Noakes-Kettel, E.A.. University Of Hertfordshire; Reino UnidoFil: Rutkowski, M.. Minnesota State University; Estados UnidosFil: Saha, K.. Inter-university Centre For Astronomy And Astrophysics India; IndiaFil: Sahu, N.. Swinburne University Of Technology; AustraliaFil: Sola, E.. Centre National de la Recherche Scientifique; FranciaFil: Vázquez Mata, J.A.. Universidad Nacional Autónoma de México; MéxicoFil: Vera-Casanova, A.. Istituto Nazionale di Astrofisica; ItaliaFil: Yoon, I.. National Radio Astronomy Observatory; Estados UnidosOxford University Press2022-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/202956Martin, G.; Bazkiaei, A.E.; Spavone, M.; Iodice, E.; Mihos, J.C.; et al.; Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 513; 1; 6-2022; 1459-14870035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac1003info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/513/1/1459/6566363info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2203.07675info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:13:30Zoai:ri.conicet.gov.ar:11336/202956instacron: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:34982025-09-29 10:13:30.582CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
title Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
spellingShingle Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
Martin, G.
GALAXIES: INTERACTIONS
GALAXIES: STRUCTURE
METHODS: NUMERICAL
title_short Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
title_full Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
title_fullStr Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
title_full_unstemmed Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
title_sort Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images
dc.creator.none.fl_str_mv Martin, G.
Bazkiaei, A.E.
Spavone, M.
Iodice, E.
Mihos, J.C.
Montes, M.
Benavides Blanco, Jose Antonio
Brough, S.
Carlin, J.L.
Collins, C.A.
Duc, P.A.
Gómez, F.A.
Galaz, G.
Hernández Toledo, H.M.
Jackson, R.A.
Kaviraj, S.
Knapen, J.H.
Martínez-Lombilla, C.
Mcgee, S.
O'ryan, D.
Prole, D.J.
Rich, R.M.
Román, J.
Shah, E.A.
Starkenburg, T.K.
Watkins, A.E.
Zaritsky, D.
Pichon, C.
Armus, L.
Bianconi, M.
Buitrago, F.
Busá, I.
Davis, F.
Demarco, R.
Desmons, A.
Garciá, P.
Graham, A.W.
Holwerda, B.
Hon, D.S.-H.
Khalid, A.
Klehammer, J.
Klutse, D.Y.
Lazar, I.
Nair, P.
Noakes-Kettel, E.A.
Rutkowski, M.
Saha, K.
Sahu, N.
Sola, E.
Vázquez Mata, J.A.
Vera-Casanova, A.
Yoon, I.
author Martin, G.
author_facet Martin, G.
Bazkiaei, A.E.
Spavone, M.
Iodice, E.
Mihos, J.C.
Montes, M.
Benavides Blanco, Jose Antonio
Brough, S.
Carlin, J.L.
Collins, C.A.
Duc, P.A.
Gómez, F.A.
Galaz, G.
Hernández Toledo, H.M.
Jackson, R.A.
Kaviraj, S.
Knapen, J.H.
Martínez-Lombilla, C.
Mcgee, S.
O'ryan, D.
Prole, D.J.
Rich, R.M.
Román, J.
Shah, E.A.
Starkenburg, T.K.
Watkins, A.E.
Zaritsky, D.
Pichon, C.
Armus, L.
Bianconi, M.
Buitrago, F.
Busá, I.
Davis, F.
Demarco, R.
Desmons, A.
Garciá, P.
Graham, A.W.
Holwerda, B.
Hon, D.S.-H.
Khalid, A.
Klehammer, J.
Klutse, D.Y.
Lazar, I.
Nair, P.
Noakes-Kettel, E.A.
Rutkowski, M.
Saha, K.
Sahu, N.
Sola, E.
Vázquez Mata, J.A.
Vera-Casanova, A.
Yoon, I.
author_role author
author2 Bazkiaei, A.E.
Spavone, M.
Iodice, E.
Mihos, J.C.
Montes, M.
Benavides Blanco, Jose Antonio
Brough, S.
Carlin, J.L.
Collins, C.A.
Duc, P.A.
Gómez, F.A.
Galaz, G.
Hernández Toledo, H.M.
Jackson, R.A.
Kaviraj, S.
Knapen, J.H.
Martínez-Lombilla, C.
Mcgee, S.
O'ryan, D.
Prole, D.J.
Rich, R.M.
Román, J.
Shah, E.A.
Starkenburg, T.K.
Watkins, A.E.
Zaritsky, D.
Pichon, C.
Armus, L.
Bianconi, M.
Buitrago, F.
Busá, I.
Davis, F.
Demarco, R.
Desmons, A.
Garciá, P.
Graham, A.W.
Holwerda, B.
Hon, D.S.-H.
Khalid, A.
Klehammer, J.
Klutse, D.Y.
Lazar, I.
Nair, P.
Noakes-Kettel, E.A.
Rutkowski, M.
Saha, K.
Sahu, N.
Sola, E.
Vázquez Mata, J.A.
Vera-Casanova, A.
Yoon, I.
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
author
author
author
author
author
author
author
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author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: INTERACTIONS
GALAXIES: STRUCTURE
METHODS: NUMERICAL
topic GALAXIES: INTERACTIONS
GALAXIES: STRUCTURE
METHODS: NUMERICAL
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilizing automated techniques and human visual classification in conjunction with realistic mock images produced using the NewHorizon cosmological simulation, we investigate the nature, frequency, and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-yr depth of the Legacy Survey of Space and Time (30-31 mag arcsec-2), falling to 60 per cent assuming a shallower final depth of 29.5 mag arcsec-2. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M* ∼1011.5 M⊙). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterization of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimized, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z < 0.2).
Fil: Martin, G.. University of Arizona; Estados Unidos. Korea Astronomy And Space Science Institute; China
Fil: Bazkiaei, A.E.. Macquarie University; Australia. The Australian Research Council Centre Of Excellence For All Sky Astrophysics In 3 Dimensions; Australia
Fil: Spavone, M.. Istituto Nazionale di Astrofisica; Italia
Fil: Iodice, E.. Istituto Nazionale di Astrofisica; Italia
Fil: Mihos, J.C.. Case Western Reserve University; Estados Unidos
Fil: Montes, M.. Space Telescope Science Institute; Estados Unidos
Fil: Benavides Blanco, Jose Antonio. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Brough, S.. Unsw Sydney; Australia
Fil: Carlin, J.L.. Rubin Observatory Project Office; Estados Unidos
Fil: Collins, C.A.. Liverpool John Moores University; Reino Unido
Fil: Duc, P.A.. Centre National de la Recherche Scientifique; Francia
Fil: Gómez, F.A.. Universidad de La Serena; Chile
Fil: Galaz, G.. Universidad Católica de Chile; Chile. Pontificia Universidad Católica de Chile; Chile
Fil: Hernández Toledo, H.M.. Universidad Nacional Autónoma de México; México
Fil: Jackson, R.A.. Yonsei University; Corea del Sur
Fil: Kaviraj, S.. University Of Hertfordshire; Reino Unido
Fil: Knapen, J.H.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Martínez-Lombilla, C.. Unsw Sydney; Australia
Fil: Mcgee, S.. The University Of Birmingham (tub);
Fil: O'ryan, D.. Lancaster University; Reino Unido
Fil: Prole, D.J.. Macquarie University; Australia
Fil: Rich, R.M.. University of California at Los Angeles; Estados Unidos
Fil: Román, J.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Shah, E.A.. University of California at Davis; Estados Unidos
Fil: Starkenburg, T.K.. Northwestern University; Estados Unidos
Fil: Watkins, A.E.. University Of Hertfordshire; Reino Unido
Fil: Zaritsky, D.. University of Arizona; Estados Unidos
Fil: Pichon, C.. Korea Institute For Advanced Study; China. Université Pierre et Marie Curie; Francia. University of Edinburgh; Reino Unido
Fil: Armus, L.. Infrared Processing &amp; Estados Unidos
Fil: Bianconi, M.. The University Of Birmingham (tub);
Fil: Buitrago, F.. Universidade de Lisboa; Portugal. Universidad de Valladolid; España
Fil: Busá, I.. Osservatorio Astrofisico Di Catania; Italia
Fil: Davis, F.. University Of Hertfordshire; Reino Unido
Fil: Demarco, R.. Universidad de Concepci Ón; Chile
Fil: Desmons, A.. Unsw Sydney; Australia
Fil: Garciá, P.. Universidad Internacional de Valencia; España
Fil: Graham, A.W.. Swinburne University Of Technology; Australia
Fil: Holwerda, B.. University of Louisville; Estados Unidos
Fil: Hon, D.S.-H.. Swinburne University Of Technology; Australia
Fil: Khalid, A.. Unsw Sydney; Australia
Fil: Klehammer, J.. Centre National de la Recherche Scientifique; Francia
Fil: Klutse, D.Y.. Astrophysics Resear Ch Centre; Reino Unido
Fil: Lazar, I.. University Of Hertfordshire; Reino Unido
Fil: Nair, P.. The University Of Alabama; Estados Unidos
Fil: Noakes-Kettel, E.A.. University Of Hertfordshire; Reino Unido
Fil: Rutkowski, M.. Minnesota State University; Estados Unidos
Fil: Saha, K.. Inter-university Centre For Astronomy And Astrophysics India; India
Fil: Sahu, N.. Swinburne University Of Technology; Australia
Fil: Sola, E.. Centre National de la Recherche Scientifique; Francia
Fil: Vázquez Mata, J.A.. Universidad Nacional Autónoma de México; México
Fil: Vera-Casanova, A.. Istituto Nazionale di Astrofisica; Italia
Fil: Yoon, I.. National Radio Astronomy Observatory; Estados Unidos
description Tidal features in the outskirts of galaxies yield unique information about their past interactions and are a key prediction of the hierarchical structure formation paradigm. The Vera C. Rubin Observatory is poised to deliver deep observations for potentially millions of objects with visible tidal features, but the inference of galaxy interaction histories from such features is not straightforward. Utilizing automated techniques and human visual classification in conjunction with realistic mock images produced using the NewHorizon cosmological simulation, we investigate the nature, frequency, and visibility of tidal features and debris across a range of environments and stellar masses. In our simulated sample, around 80 per cent of the flux in the tidal features around Milky Way or greater mass galaxies is detected at the 10-yr depth of the Legacy Survey of Space and Time (30-31 mag arcsec-2), falling to 60 per cent assuming a shallower final depth of 29.5 mag arcsec-2. The fraction of total flux found in tidal features increases towards higher masses, rising to 10 per cent for the most massive objects in our sample (M* ∼1011.5 M⊙). When observed at sufficient depth, such objects frequently exhibit many distinct tidal features with complex shapes. The interpretation and characterization of such features varies significantly with image depth and object orientation, introducing significant biases in their classification. Assuming the data reduction pipeline is properly optimized, we expect the Rubin Observatory to be capable of recovering much of the flux found in the outskirts of Milky Way mass galaxies, even at intermediate redshifts (z < 0.2).
publishDate 2022
dc.date.none.fl_str_mv 2022-06
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/202956
Martin, G.; Bazkiaei, A.E.; Spavone, M.; Iodice, E.; Mihos, J.C.; et al.; Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 513; 1; 6-2022; 1459-1487
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/202956
identifier_str_mv Martin, G.; Bazkiaei, A.E.; Spavone, M.; Iodice, E.; Mihos, J.C.; et al.; Preparing for low surface brightness science with the Vera C. Rubin Observatory: Characterization of tidal features from mock images; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 513; 1; 6-2022; 1459-1487
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac1003
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/513/1/1459/6566363
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2203.07675
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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