Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies
We analyze the star-forming and structural properties of 45 massive (log(M/M_) > 10) compact star-forming galaxies (SFGs) at 2 < z < 3 to explore whether they are progenitors of compact quiescent galaxies at z ∼ 2. The optical/NIR and far-IR Spitzer/Herschel colors indicate that most compac...
| Autor: | |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2014 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/33907 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/33907 |
| Access Level: | acceso abierto |
| Palabra clave: | 52 Star-forming galaxies Active galactic nuclei Hubble-space-telescope Ultra-deep-field Lyman-break galaxies Digital sky survey Goods-south field Greater-Than 1 Spectral energy-distribution Stellar population synthesis. Astrofísica |
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Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxiesPérez González, Pablo Guillermo52Star-forming galaxiesActive galactic nucleiHubble-space-telescopeUltra-deep-fieldLyman-break galaxiesDigital sky surveyGoods-south fieldGreater-Than 1Spectral energy-distributionStellar population synthesis.AstrofísicaWe analyze the star-forming and structural properties of 45 massive (log(M/M_) > 10) compact star-forming galaxies (SFGs) at 2 < z < 3 to explore whether they are progenitors of compact quiescent galaxies at z ∼ 2. The optical/NIR and far-IR Spitzer/Herschel colors indicate that most compact SFGs are heavily obscured. Nearly half (47%) host an X-ray-bright active galactic nucleus (AGN). In contrast, only about 10% of other massive galaxies at that time host AGNs. Compact SFGs have centrally concentrated light profiles and spheroidal morphologies similar to quiescent galaxies and are thus strikingly different from other SFGs, which typically are disk-like and sometimes clumpy or irregular.Most compact SFGs lie either within the star formation rate (SFR)–mass main sequence (65%) or below it (30%), on the expected evolutionary path toward quiescent galaxies. These results show conclusively that galaxies become more compact before they lose their gas and dust, quenching star formation. Using extensive HST photometry from CANDELS and grism spectroscopy from the 3D-HST survey, we model their stellar populations with either exponentially declining (τ ) star formation histories (SFHs) or physically motivated SFHs drawn from semianalytic models (SAMs). SAMs predict longer formation timescales and older ages ∼2 Gyr, which are nearly twice as old as the estimates of the τ models. Both models yield good spectral energy distribution fits, indicating that the systematic uncertainty in the age due to degeneracies in the SFH is of that order of magnitude. However, SAM SFHs better match the observed slope and zero point of the SFR–mass main sequence. Contrary to expectations, some low-mass compact SFGs (log(M/M_) = 10–10.6) have younger ages but lower specific SFRs than that of more massive galaxies, suggesting that the low-mass galaxies reach the red sequence faster. If the progenitors of compact SFGs are extended SFGs, state-of-the-art SAMs show that mergers and disk instabilities (DIs) are both able to shrink galaxies, but DIs are more frequent (60% versus 40%) and form more concentrated galaxies. We confirm this result via high-resolution hydrodynamic simulations.IOP PublishingUniversidad Complutense de Madrid20142014-08-1020142014-08-10journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/33907reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/339072026-06-02T12:44:21Z |
| dc.title.none.fl_str_mv |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| title |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| spellingShingle |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies Pérez González, Pablo Guillermo 52 Star-forming galaxies Active galactic nuclei Hubble-space-telescope Ultra-deep-field Lyman-break galaxies Digital sky survey Goods-south field Greater-Than 1 Spectral energy-distribution Stellar population synthesis. Astrofísica |
| title_short |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| title_full |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| title_fullStr |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| title_full_unstemmed |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| title_sort |
Candels+3D-HST: compact SFGs at z ∼ 2-3, the progenitors of the first quiescent galaxies |
| dc.creator.none.fl_str_mv |
Pérez González, Pablo Guillermo |
| author |
Pérez González, Pablo Guillermo |
| author_facet |
Pérez González, Pablo Guillermo |
| author_role |
author |
| dc.contributor.none.fl_str_mv |
Universidad Complutense de Madrid |
| dc.subject.none.fl_str_mv |
52 Star-forming galaxies Active galactic nuclei Hubble-space-telescope Ultra-deep-field Lyman-break galaxies Digital sky survey Goods-south field Greater-Than 1 Spectral energy-distribution Stellar population synthesis. Astrofísica |
| topic |
52 Star-forming galaxies Active galactic nuclei Hubble-space-telescope Ultra-deep-field Lyman-break galaxies Digital sky survey Goods-south field Greater-Than 1 Spectral energy-distribution Stellar population synthesis. Astrofísica |
| description |
We analyze the star-forming and structural properties of 45 massive (log(M/M_) > 10) compact star-forming galaxies (SFGs) at 2 < z < 3 to explore whether they are progenitors of compact quiescent galaxies at z ∼ 2. The optical/NIR and far-IR Spitzer/Herschel colors indicate that most compact SFGs are heavily obscured. Nearly half (47%) host an X-ray-bright active galactic nucleus (AGN). In contrast, only about 10% of other massive galaxies at that time host AGNs. Compact SFGs have centrally concentrated light profiles and spheroidal morphologies similar to quiescent galaxies and are thus strikingly different from other SFGs, which typically are disk-like and sometimes clumpy or irregular.Most compact SFGs lie either within the star formation rate (SFR)–mass main sequence (65%) or below it (30%), on the expected evolutionary path toward quiescent galaxies. These results show conclusively that galaxies become more compact before they lose their gas and dust, quenching star formation. Using extensive HST photometry from CANDELS and grism spectroscopy from the 3D-HST survey, we model their stellar populations with either exponentially declining (τ ) star formation histories (SFHs) or physically motivated SFHs drawn from semianalytic models (SAMs). SAMs predict longer formation timescales and older ages ∼2 Gyr, which are nearly twice as old as the estimates of the τ models. Both models yield good spectral energy distribution fits, indicating that the systematic uncertainty in the age due to degeneracies in the SFH is of that order of magnitude. However, SAM SFHs better match the observed slope and zero point of the SFR–mass main sequence. Contrary to expectations, some low-mass compact SFGs (log(M/M_) = 10–10.6) have younger ages but lower specific SFRs than that of more massive galaxies, suggesting that the low-mass galaxies reach the red sequence faster. If the progenitors of compact SFGs are extended SFGs, state-of-the-art SAMs show that mergers and disk instabilities (DIs) are both able to shrink galaxies, but DIs are more frequent (60% versus 40%) and form more concentrated galaxies. We confirm this result via high-resolution hydrodynamic simulations. |
| publishDate |
2014 |
| dc.date.none.fl_str_mv |
2014 2014-08-10 2014 2014-08-10 |
| dc.type.none.fl_str_mv |
journal article http://purl.org/coar/resource_type/c_6501 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
| format |
article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/20.500.14352/33907 |
| url |
https://hdl.handle.net/20.500.14352/33907 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| dc.rights.openaire.fl_str_mv |
info:eu-repo/semantics/openAccess |
| rights_invalid_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| eu_rights_str_mv |
openAccess |
| dc.format.none.fl_str_mv |
application/pdf |
| dc.publisher.none.fl_str_mv |
IOP Publishing |
| publisher.none.fl_str_mv |
IOP Publishing |
| dc.source.none.fl_str_mv |
reponame:Docta Complutense instname:Universidad Complutense de Madrid (UCM) |
| instname_str |
Universidad Complutense de Madrid (UCM) |
| reponame_str |
Docta Complutense |
| collection |
Docta Complutense |
| repository.name.fl_str_mv |
|
| repository.mail.fl_str_mv |
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1869425165451919360 |
| score |
15.300724 |