Gaia photometry for white dwarfs

Context. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint on...

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Autores: Carrasco Martínez, José Manuel, Catalán, S., Jordi i Nebot, Carme, Tremblay, P.-E., Napiwotzki, R., Luri Carrascoso, Xavier, Robin, A. C., Kowalski, P. M.
Formato: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2014
País:España
Recursos:Universidad de Barcelona
Repositorio:Dipòsit Digital de la UB
OAI Identifier:oai:diposit.ub.edu:2445/53544
Acesso em linha:https://hdl.handle.net/2445/53544
Access Level:acceso abierto
Palavra-chave:Evolució estel·lar
Fotometria astronòmica
Galàxies
Estels nans
Stellar evolution
Astronomical photometry
Galaxies
Dwarf stars
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spelling Gaia photometry for white dwarfsCarrasco Martínez, José ManuelCatalán, S.Jordi i Nebot, CarmeTremblay, P.-E.Napiwotzki, R.Luri Carrascoso, XavierRobin, A. C.Kowalski, P. M.Evolució estel·larFotometria astronòmicaGalàxiesEstels nansStellar evolutionAstronomical photometryGalaxiesDwarf starsContext. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint only the nearby (~ 20 pc) sample is reasonably complete. The Gaia space mission will drastically increase the sample of known white dwarfs through its 5-6 years survey of the whole sky up to magnitude V = 20-25. Aims. We provide a characterisation of Gaia photometry for white dwarfs to better prepare for the analysis of the scientific output of the mission. Transformations between some of the most common photometric systems and Gaia passbands are derived. We also give estimates of the number of white dwarfs of the different galactic populations that will be observed. Methods. Using synthetic spectral energy distributions and the most recent Gaia transmission curves, we computed colours of three different types of white dwarfs (pure hydrogen, pure helium, and mixed composition with H/He = 0.1). With these colours we derived transformations to other common photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbers of white dwarfs predicted to be observed by Gaia. Results. We provide relationships and colour-colour diagrams among different photometric systems to allow the prediction and/or study of the Gaia white dwarf colours. We also include estimates of the number of sources expected in every galactic population and with a maximum parallax error. Gaia will increase the sample of known white dwarfs tenfold to about 200 000. Gaia will be able to observe thousands of very cool white dwarfs for the first time, which will greatly improve our understanding of these stars and early phases of star formation in our Galaxy.Springer Verlag2014info:eu-repo/semantics/articleinfo:eu-repo/semantics/acceptedVersionapplication/pdfhttps://hdl.handle.net/2445/53544Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Dipòsit Digital de la UBinstname:Universidad de BarcelonaInglésVersió postprint del document publicat a: http://dx.doi.org/10.1051/0004-6361/201220596Astronomy and Astrophysics, 2014, vol. 565, num. A11, p. 1-16http://dx.doi.org/10.1051/0004-6361/201220596info:eu-repo/grantAgreement/EC/FP7/237718(c) Springer Verlag, 2014info:eu-repo/semantics/openAccessoai:diposit.ub.edu:2445/535442026-05-27T06:46:51Z
dc.title.none.fl_str_mv Gaia photometry for white dwarfs
title Gaia photometry for white dwarfs
spellingShingle Gaia photometry for white dwarfs
Carrasco Martínez, José Manuel
Evolució estel·lar
Fotometria astronòmica
Galàxies
Estels nans
Stellar evolution
Astronomical photometry
Galaxies
Dwarf stars
title_short Gaia photometry for white dwarfs
title_full Gaia photometry for white dwarfs
title_fullStr Gaia photometry for white dwarfs
title_full_unstemmed Gaia photometry for white dwarfs
title_sort Gaia photometry for white dwarfs
dc.creator.none.fl_str_mv Carrasco Martínez, José Manuel
Catalán, S.
Jordi i Nebot, Carme
Tremblay, P.-E.
Napiwotzki, R.
Luri Carrascoso, Xavier
Robin, A. C.
Kowalski, P. M.
author Carrasco Martínez, José Manuel
author_facet Carrasco Martínez, José Manuel
Catalán, S.
Jordi i Nebot, Carme
Tremblay, P.-E.
Napiwotzki, R.
Luri Carrascoso, Xavier
Robin, A. C.
Kowalski, P. M.
author_role author
author2 Catalán, S.
Jordi i Nebot, Carme
Tremblay, P.-E.
Napiwotzki, R.
Luri Carrascoso, Xavier
Robin, A. C.
Kowalski, P. M.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Evolució estel·lar
Fotometria astronòmica
Galàxies
Estels nans
Stellar evolution
Astronomical photometry
Galaxies
Dwarf stars
topic Evolució estel·lar
Fotometria astronòmica
Galàxies
Estels nans
Stellar evolution
Astronomical photometry
Galaxies
Dwarf stars
description Context. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint only the nearby (~ 20 pc) sample is reasonably complete. The Gaia space mission will drastically increase the sample of known white dwarfs through its 5-6 years survey of the whole sky up to magnitude V = 20-25. Aims. We provide a characterisation of Gaia photometry for white dwarfs to better prepare for the analysis of the scientific output of the mission. Transformations between some of the most common photometric systems and Gaia passbands are derived. We also give estimates of the number of white dwarfs of the different galactic populations that will be observed. Methods. Using synthetic spectral energy distributions and the most recent Gaia transmission curves, we computed colours of three different types of white dwarfs (pure hydrogen, pure helium, and mixed composition with H/He = 0.1). With these colours we derived transformations to other common photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbers of white dwarfs predicted to be observed by Gaia. Results. We provide relationships and colour-colour diagrams among different photometric systems to allow the prediction and/or study of the Gaia white dwarf colours. We also include estimates of the number of sources expected in every galactic population and with a maximum parallax error. Gaia will increase the sample of known white dwarfs tenfold to about 200 000. Gaia will be able to observe thousands of very cool white dwarfs for the first time, which will greatly improve our understanding of these stars and early phases of star formation in our Galaxy.
publishDate 2014
dc.date.none.fl_str_mv 2014
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/53544
url https://hdl.handle.net/2445/53544
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Versió postprint del document publicat a: http://dx.doi.org/10.1051/0004-6361/201220596
Astronomy and Astrophysics, 2014, vol. 565, num. A11, p. 1-16
http://dx.doi.org/10.1051/0004-6361/201220596
info:eu-repo/grantAgreement/EC/FP7/237718
dc.rights.none.fl_str_mv (c) Springer Verlag, 2014
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) Springer Verlag, 2014
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Springer Verlag
publisher.none.fl_str_mv Springer Verlag
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Dipòsit Digital de la UB
instname:Universidad de Barcelona
instname_str Universidad de Barcelona
reponame_str Dipòsit Digital de la UB
collection Dipòsit Digital de la UB
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,301603

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