Bayesian hierarchical modelling of the M*–SFR relation from 1 ≲ z ≲ 6 in ASTRODEEP

L. Sandles; E. Curtis-Lake; S. Charlot; J. Chevallard; R. Maiolino

doi:10.1093/mnras/stac1999

Bayesian hierarchical modelling of the M*–SFR relation from 1 ≲ z ≲ 6 in ASTRODEEP

L. Sandles
, E. Curtis-Lake
, S. Charlot
, J. Chevallard
, R. Maiolino

Research output: Contribution to journal › Article › peer-review

16 Citations (Scopus)

18 Downloads (Pure)

Abstract

The Hubble Frontier Fields represent the opportunity to probe the high-redshift evolution of the main sequence of star-forming galaxies to lower masses than possible in blank fields thanks to foreground lensing of massive galaxy clusters. We use the BEAGLE SED-fitting code to derive stellar masses, $\mathrm{M_{\star}}=\log(M/\mathrm{M_{\odot}})$, SFRs, $\Psi=\log(\psi/\mathrm{M_{\odot}}\,\mathrm{yr}^{-1})$ and redshifts from galaxies within the ASTRODEEP catalogue. We fit a fully Bayesian hierarchical model of the main sequence over $1.253$, measurements of the main sequence to low masses and high redshifts still strongly depend on priors employed in SED fitting (as well as other fitting assumptions). Future data-sets with JWST should improve this.

Original language	English
Pages (from-to)	2951-2969
Journal	Monthly Notices of the Royal Astronomical Society (MNRAS)
Volume	515
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stac1999
Publication status	Published - 31 Jul 2022

Keywords

astro-ph.GA

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10.1093/mnras/stac1999Licence: CC BY

stac1999
© The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 2.82 MBLicence: CC BY

Cite this

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title = "Bayesian hierarchical modelling of the M*–SFR relation from 1 ≲ z ≲ 6 in ASTRODEEP",

abstract = " The Hubble Frontier Fields represent the opportunity to probe the high-redshift evolution of the main sequence of star-forming galaxies to lower masses than possible in blank fields thanks to foreground lensing of massive galaxy clusters. We use the BEAGLE SED-fitting code to derive stellar masses, \$\textbackslash{}mathrm\{M\_\{\textbackslash{}star\}\}=\textbackslash{}log(M/\textbackslash{}mathrm\{M\_\{\textbackslash{}odot\}\})\$, SFRs, \$\textbackslash{}Psi=\textbackslash{}log(\textbackslash{}psi/\textbackslash{}mathrm\{M\_\{\textbackslash{}odot\}\}\textbackslash{},\textbackslash{}mathrm\{yr\}\textasciicircum{}\{-1\})\$ and redshifts from galaxies within the ASTRODEEP catalogue. We fit a fully Bayesian hierarchical model of the main sequence over \$1.253\$, measurements of the main sequence to low masses and high redshifts still strongly depend on priors employed in SED fitting (as well as other fitting assumptions). Future data-sets with JWST should improve this. ",

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author = "L. Sandles and E. Curtis-Lake and S. Charlot and J. Chevallard and R. Maiolino",

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AU - Sandles, L.

AU - Curtis-Lake, E.

AU - Charlot, S.

AU - Chevallard, J.

AU - Maiolino, R.

N1 - © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

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AB - The Hubble Frontier Fields represent the opportunity to probe the high-redshift evolution of the main sequence of star-forming galaxies to lower masses than possible in blank fields thanks to foreground lensing of massive galaxy clusters. We use the BEAGLE SED-fitting code to derive stellar masses, $\mathrm{M_{\star}}=\log(M/\mathrm{M_{\odot}})$, SFRs, $\Psi=\log(\psi/\mathrm{M_{\odot}}\,\mathrm{yr}^{-1})$ and redshifts from galaxies within the ASTRODEEP catalogue. We fit a fully Bayesian hierarchical model of the main sequence over $1.253$, measurements of the main sequence to low masses and high redshifts still strongly depend on priors employed in SED fitting (as well as other fitting assumptions). Future data-sets with JWST should improve this.

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ER -

Bayesian hierarchical modelling of the M*–SFR relation from 1 ≲ z ≲ 6 in ASTRODEEP

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