With the aim of understanding the coevolution of star formation rate (SFR), stellar mass (M*), and oxygen abundance (O/H) in galaxies up to redshift z ≃ 3.7, we have compiled the largest available data set for studying Metallicity Evolution and Galaxy Assembly (MEGA); it comprises ~1000 galaxies with a common O/H calibration and spans almost two orders of magnitude in metallicity, a factor of ~106 in SFR, and a factor of ~105 in stellar mass. From a principal component analysis, we find that the three-dimensional parameter space reduces to a Fundamental Plane in metallicity (FPZ) given by 12 + log(O/H) = -0.14 log (SFR) + 0.37 log(M*) + 4.82. The mean O/H FPZ residuals are small (0.16 dex) and consistent with trends found in smaller galaxy samples with more limited ranges in M*, SFR, and O/H. Importantly, the FPZ is found to be approximately redshift invariant within the uncertainties. In a companion paper, these results are interpreted with an updated version of the model presented by Dayal, Ferrara & Dunlop.

Coevolution of metallicity and star formation in galaxies to z sime 3.7 - I. A Fundamental Plane

FERRARA, ANDREA
2016

Abstract

With the aim of understanding the coevolution of star formation rate (SFR), stellar mass (M*), and oxygen abundance (O/H) in galaxies up to redshift z ≃ 3.7, we have compiled the largest available data set for studying Metallicity Evolution and Galaxy Assembly (MEGA); it comprises ~1000 galaxies with a common O/H calibration and spans almost two orders of magnitude in metallicity, a factor of ~106 in SFR, and a factor of ~105 in stellar mass. From a principal component analysis, we find that the three-dimensional parameter space reduces to a Fundamental Plane in metallicity (FPZ) given by 12 + log(O/H) = -0.14 log (SFR) + 0.37 log(M*) + 4.82. The mean O/H FPZ residuals are small (0.16 dex) and consistent with trends found in smaller galaxy samples with more limited ranges in M*, SFR, and O/H. Importantly, the FPZ is found to be approximately redshift invariant within the uncertainties. In a companion paper, these results are interpreted with an updated version of the model presented by Dayal, Ferrara & Dunlop.
Settore FIS/05 - Astronomia e Astrofisica
galaxies: abundances, galaxies: evolution, galaxies: high-redshift, galaxies: star formation
File in questo prodotto:
File Dimensione Formato  
stw1993.pdf

Accesso chiuso

Tipologia: Published version
Licenza: Non pubblico
Dimensione 3.05 MB
Formato Adobe PDF
3.05 MB Adobe PDF   Visualizza/Apri   Richiedi una copia
11384_64698.pdf

accesso aperto

Tipologia: Accepted version (post-print)
Licenza: Creative commons
Dimensione 1.02 MB
Formato Adobe PDF
1.02 MB Adobe PDF Visualizza/Apri

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11384/64698
Citazioni
  • ???jsp.display-item.citation.pmc??? ND
  • Scopus 51
  • ???jsp.display-item.citation.isi??? 51
social impact