Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect

The spectral energy distribution (SED) of galaxies varies both between galaxies and within them. For instance, early-type spiral galaxies have a red bulge surrounded by a bluer star-forming disk with H II regions within. When observing redshifted galaxies, a given photometric filter probes light at...

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Autores: Papaderos, Polychronis, Östlin, Göran, Breda, I.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/330672
Acesso em linha:http://hdl.handle.net/10261/330672
Access Level:acceso abierto
Palavra-chave:Galaxies: structure
Galaxies: photometry
Galaxies: high-redshift
Galaxies: spiral
Galaxies: bulges
Galaxies: evolution
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repository_id_str
dc.title.none.fl_str_mv Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
title Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
spellingShingle Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
Papaderos, Polychronis
Galaxies: structure
Galaxies: photometry
Galaxies: high-redshift
Galaxies: spiral
Galaxies: bulges
Galaxies: evolution
title_short Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
title_full Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
title_fullStr Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
title_full_unstemmed Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
title_sort Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effect
dc.creator.none.fl_str_mv Papaderos, Polychronis
Östlin, Göran
Breda, I.
author Papaderos, Polychronis
author_facet Papaderos, Polychronis
Östlin, Göran
Breda, I.
author_role author
author2 Östlin, Göran
Breda, I.
author2_role author
author
dc.contributor.none.fl_str_mv Wenner-Gren Foundation
Fundação para a Ciência e a Tecnologia (Portugal)
Swedish Research Council
Ministerio de Ciencia, Innovación y Universidades (España)
European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxies: structure
Galaxies: photometry
Galaxies: high-redshift
Galaxies: spiral
Galaxies: bulges
Galaxies: evolution
topic Galaxies: structure
Galaxies: photometry
Galaxies: high-redshift
Galaxies: spiral
Galaxies: bulges
Galaxies: evolution
description The spectral energy distribution (SED) of galaxies varies both between galaxies and within them. For instance, early-type spiral galaxies have a red bulge surrounded by a bluer star-forming disk with H II regions within. When observing redshifted galaxies, a given photometric filter probes light at a bluer rest frame, and in relating the observed magnitudes to the rest frame of the filter, so-called k corrections are commonly applied to account for the relative dimming or brightening in addition to the pure distance effect. The amount of correction depends on the shape of the spectrum (SED), so different k corrections apply to galaxies of different spectral types. This is, however, only part of the story, since any galaxy with a spatially non-homogeneous SED will experience a spatially varying relative dimming or brightening as a function of observed wavelength. Also, the morphological appearance of galaxies will therefore change with redshift. For instance, an early spiral galaxy observed in the V band would show a prominent bulge at z = 0, whereas, if at redshift z ∼ 1, the V filter probes emission in the rest-frame near-ultraviolet where the bulge is faint and the disk relatively brighter, thus the galaxy may appear as bulgeless. One popular way of studying spatial variations in the stellar population and dust content of galaxies is the use of color maps. For star-forming galaxies that have an appreciable contribution from nebular emission (lines and continuum), an additional effect is that the shifting of strong features in or out of filters will result in a non-monotonous color evolution with redshift. Hence, unlike the effects of distance, cosmological surface brightness dimming, and gravitational lensing, which are all achromatic, the fact that most galaxies have a spatially varying SED leads to a chromatic surface brightness modulation (CMOD) with redshift. While the CMOD effects are in principle easy to grasp, they affect multicolor imaging surveys and photometric properties derived from such surveys in a complex fashion. Properties such as the bulge-to-disk ratio, Sérsic exponent, light concentration, asymmetry index and effective radius, radial color gradients, and stellar mass determinations from SED fitting will depend on the redshift, the filters employed, and the rest-frame 2D SED patterns in a galaxy and will bias results inferred on galaxy evolution across cosmic time (e.g., the evolution of the mass-size, bulge-supermassive black hole, and Tully-Fisher relation), and potentially also weak lensing, if these effects are not properly taken into account. In this article we quantify the CMOD effects for idealized galaxies built from spectral synthesis models and from galaxies with observed integral field spectroscopy, and we show that they are significant and should be taken into account in studies of resolved galaxy properties and their evolution with redshift. © The Authors 2023.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/330672
url http://hdl.handle.net/10261/330672
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
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info:eu-repo/grantAgreement/AEI//SEV-2017-0709
info:eu-repo/grantAgreement/EC/HE/101059532
http://dx.doi.org/10.1051/0004-6361/202245769
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
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dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
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spelling Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z: The chromatic surface brightness modulation (C MOD) effectPapaderos, PolychronisÖstlin, GöranBreda, I.Galaxies: structureGalaxies: photometryGalaxies: high-redshiftGalaxies: spiralGalaxies: bulgesGalaxies: evolutionThe spectral energy distribution (SED) of galaxies varies both between galaxies and within them. For instance, early-type spiral galaxies have a red bulge surrounded by a bluer star-forming disk with H II regions within. When observing redshifted galaxies, a given photometric filter probes light at a bluer rest frame, and in relating the observed magnitudes to the rest frame of the filter, so-called k corrections are commonly applied to account for the relative dimming or brightening in addition to the pure distance effect. The amount of correction depends on the shape of the spectrum (SED), so different k corrections apply to galaxies of different spectral types. This is, however, only part of the story, since any galaxy with a spatially non-homogeneous SED will experience a spatially varying relative dimming or brightening as a function of observed wavelength. Also, the morphological appearance of galaxies will therefore change with redshift. For instance, an early spiral galaxy observed in the V band would show a prominent bulge at z = 0, whereas, if at redshift z ∼ 1, the V filter probes emission in the rest-frame near-ultraviolet where the bulge is faint and the disk relatively brighter, thus the galaxy may appear as bulgeless. One popular way of studying spatial variations in the stellar population and dust content of galaxies is the use of color maps. For star-forming galaxies that have an appreciable contribution from nebular emission (lines and continuum), an additional effect is that the shifting of strong features in or out of filters will result in a non-monotonous color evolution with redshift. Hence, unlike the effects of distance, cosmological surface brightness dimming, and gravitational lensing, which are all achromatic, the fact that most galaxies have a spatially varying SED leads to a chromatic surface brightness modulation (CMOD) with redshift. While the CMOD effects are in principle easy to grasp, they affect multicolor imaging surveys and photometric properties derived from such surveys in a complex fashion. Properties such as the bulge-to-disk ratio, Sérsic exponent, light concentration, asymmetry index and effective radius, radial color gradients, and stellar mass determinations from SED fitting will depend on the redshift, the filters employed, and the rest-frame 2D SED patterns in a galaxy and will bias results inferred on galaxy evolution across cosmic time (e.g., the evolution of the mass-size, bulge-supermassive black hole, and Tully-Fisher relation), and potentially also weak lensing, if these effects are not properly taken into account. In this article we quantify the CMOD effects for idealized galaxies built from spectral synthesis models and from galaxies with observed integral field spectroscopy, and we show that they are significant and should be taken into account in studies of resolved galaxy properties and their evolution with redshift. © The Authors 2023.Polychronis Papaderos gratefully acknowledges support by the Wenner-Gren Foundation and the hospitality of the Astronomy Department at Stockholm University. He also thanks Fundação para a Ciência e a Tecnologia (FCT) for managing research funds graciously provided to Portugal by the EU. This work was supported through FCT grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and the project “Identifying the Earliest Supermassive Black Holes with ALMA (IdEaS with ALMA)” (PTDC/FIS-AST/29245/2017). Göran Östlin acknowledges support from the Swedish Research Council (VR) and the Swedish National Space Administration (SNSA). Iris Breda acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). She also acknowledges HORIZON-TMA-MSCA-2021-PF-01 postdoctoral fellowship contract 101059532 (GALYKOS). This study uses data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es), funded by the Spanish Ministry of Science under grant ICTS-2009-10, and the Centro Astronómico Hispano-Alemán. It is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). This research has made use of the Cosmology Calculator for the World Wide Web (Wright 2006) and of NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (SEV-2017-0709).Peer reviewedEDP SciencesWenner-Gren FoundationFundação para a Ciência e a Tecnologia (Portugal)Swedish Research CouncilMinisterio de Ciencia, Innovación y Universidades (España)European CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/330672reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI//SEV-2017-0709info:eu-repo/grantAgreement/EC/HE/101059532http://dx.doi.org/10.1051/0004-6361/202245769Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3306722026-05-22T06:33:51Z
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