The VANDELS survey: a strong correlation between Ly α equivalent width and stellar metallicity at 3 ≤ z ≤ 5
The VANDELS survey: a strong correlation between Ly α equivalent width and stellar metallicity at 3 ≤ z ≤ 5
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VANDELS 调查：Ly α 当量宽度与 3 ≤ z ≤ 5 处的恒星金属丰度之间存在很强的相关性
DOI：
10.1093/mnras/staa1260
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发表时间：
2020
影响因子：
4.8
通讯作者：
A. Saxena
中科院分区：
文献类型：
--
作者：
F. Cullen;R. McLure;J. Dunlop;A. Carnall;D. McLeod;A. Shapley;R. Amorín;M. Bolzonella;M. Castellano;A. Cimatti;A. Cimatti;M. Cirasuolo;O. Cucciati;A. Fontana;F. Fontanot;B. Garilli;L. Guaita;L. Guaita;M. Jarvis;M. Jarvis;L. Pentericci;L. Pozzetti;M. Talia;M. Talia;G. Zamorani;A. Calabró;G. Cresci;J. Fynbo;N. Hathi;M. Giavalisco;A. Koekemoer;F. Mannucci;A. Saxena
We present the results of a new study investigating the relationship between observed Ly α equivalent width (Wλ(Ly α)) and the metallicity of the ionizing stellar population ( Z⋆) for a sample of 768 star-forming galaxies at 3 ≤ z ≤ 5 drawn from the VANDELS survey. Dividing our sample into quartiles of rest-frame Wλ(Ly α) across the range $-58 \,\rm {\mathring{\rm A}} \lesssim$Wλ(Ly α) $\lesssim 110 \,\rm {\mathring{\rm A}}$, we determine Z⋆ from full spectral fitting of composite far-ultraviolet spectra and find a clear anticorrelation between Wλ(Ly α) and Z⋆. Our results indicate that Z⋆ decreases by a factor ≳ 3 between the lowest Wλ(Ly α) quartile (〈Wλ(Ly α)$\rangle =-18\,\rm {\mathring{\rm A}}$) and the highest Wλ(Ly α) quartile (〈Wλ(Ly α)$\rangle =24\,\rm {\mathring{\rm A}}$). Similarly, galaxies typically defined as Lyman alpha emitters (LAEs; Wλ(Ly α) $\gt 20\,\rm {\mathring{\rm A}}$) are, on average, metal poor with respect to the non-LAE galaxy population (Wλ(Ly α) $\le 20\,\rm {\mathring{\rm A}}$) with Z⋆non-LAE ≳ 2 × Z⋆LAE. Finally, based on the best-fitting stellar models, we estimate that the increasing strength of the stellar ionizing spectrum towards lower Z⋆ is responsible for ${\simeq}15{-}25{{\ \rm per\ cent}}$ of the observed variation in Wλ(Ly α) across our sample, with the remaining contribution (${\simeq}75{-}85{{\ \rm per\ cent}}$) being due to a decrease in the H i/dust covering fractions in low- Z⋆ galaxies.
We present the results of a new study investigating the relationship between observed Ly α equivalent width (Wλ(Ly α)) and the metallicity of the ionizing stellar population ( Z⋆) for a sample of 768 star-forming galaxies at 3 ≤ z ≤ 5 drawn from the VANDELS survey. Dividing our sample into quartiles of rest-frame Wλ(Ly α) across the range $-58 \,\rm {\mathring{\rm A}} \lesssim$Wλ(Ly α) $\lesssim 110 \,\rm {\mathring{\rm A}}$, we determine Z⋆ from full spectral fitting of composite far-ultraviolet spectra and find a clear anticorrelation between Wλ(Ly α) and Z⋆. Our results indicate that Z⋆ decreases by a factor ≳ 3 between the lowest Wλ(Ly α) quartile (〈Wλ(Ly α)$\rangle =-18\,\rm {\mathring{\rm A}}$) and the highest Wλ(Ly α) quartile (〈Wλ(Ly α)$\rangle =24\,\rm {\mathring{\rm A}}$). Similarly, galaxies typically defined as Lyman alpha emitters (LAEs; Wλ(Ly α) $\gt 20\,\rm {\mathring{\rm A}}$) are, on average, metal poor with respect to the non-LAE galaxy population (Wλ(Ly α) $\le 20\,\rm {\mathring{\rm A}}$) with Z⋆non-LAE ≳ 2 × Z⋆LAE. Finally, based on the best-fitting stellar models, we estimate that the increasing strength of the stellar ionizing spectrum towards lower Z⋆ is responsible for ${\simeq}15{-}25{{\ \rm per\ cent}}$ of the observed variation in Wλ(Ly α) across our sample, with the remaining contribution (${\simeq}75{-}85{{\ \rm per\ cent}}$) being due to a decrease in the H i/dust covering fractions in low- Z⋆ galaxies.
DOI：
10.1088/0004-637x/782/1/6
发表时间：
2013-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
M. Hayes;M. Hayes;M. Hayes;G. Östlin;F. Duval;A. Sandberg;L. Guaita;J. Melinder;A. Adamo
通讯作者：
M. Hayes;M. Hayes;M. Hayes;G. Östlin;F. Duval;A. Sandberg;L. Guaita;J. Melinder;A. Adamo
影响因子：
4.8
作者：
R. McLure;L. Pentericci;A. Cimatti;J. Dunlop;D. Elbaz;A. Fontana;K. Nandra;R. Amorín;M. Bolzonella;A. Bongiorno;A. Carnall;M. Castellano;M. Cirasuolo;O. Cucciati;F. Cullen;S. D. Barros;S. Finkelstein;F. Fontanot;P. Franzetti;M. Fumana;A. Gargiulo;B. Garilli;L. Guaita;W. Hartley;A. Iovino;M. Jarvis;S. Juneau;W. Karman;D. Maccagni;F. Marchi;E. Mármol-Queraltó;E. Pompei;L. Pozzetti;M. Scodeggio;V. Sommariva;M. Talia;O. Almaini;I. Balestra;S. Bardelli;E. Bell;N. Bourne;R. Bowler;M. Brusa;F. Buitrago;K. Caputi;P. Cassata;S. Charlot;A. Citro;G. Cresci;S. Cristiani;E. Curtis-Lake;M. Dickinson;G. Fazio;H. Ferguson;F. Fiore;Maximilien Franco;J. Fynbo;A. Galametz;A. Georgakakis;M. Giavalisco;A. Grazian;N. Hathi;I. Jung;S. Kim;A. Koekemoer;Y. Khusanova;O. Fèvre;J. Lotz;F. Mannucci;D. Maltby;K. Matsuoka;D. McLeod;H. Méndez-Hernández;J. Méndez-Abreu;M. Mignoli;Michele Moresco;A. Mortlock;M. Nonino;M. Pannella;C. Papovich;P. Popesso;D. Rosario;M. Salvato;P. Santini;D. Schaerer;C. Schreiber;D. Stark;L. Tasca;R. Thomas;T. Treu;E. Vanzella;V. Wild;C. Williams;G. Zamorani;E. Zucca
通讯作者：
R. McLure;L. Pentericci;A. Cimatti;J. Dunlop;D. Elbaz;A. Fontana;K. Nandra;R. Amorín;M. Bolzonella;A. Bongiorno;A. Carnall;M. Castellano;M. Cirasuolo;O. Cucciati;F. Cullen;S. D. Barros;S. Finkelstein;F. Fontanot;P. Franzetti;M. Fumana;A. Gargiulo;B. Garilli;L. Guaita;W. Hartley;A. Iovino;M. Jarvis;S. Juneau;W. Karman;D. Maccagni;F. Marchi;E. Mármol-Queraltó;E. Pompei;L. Pozzetti;M. Scodeggio;V. Sommariva;M. Talia;O. Almaini;I. Balestra;S. Bardelli;E. Bell;N. Bourne;R. Bowler;M. Brusa;F. Buitrago;K. Caputi;P. Cassata;S. Charlot;A. Citro;G. Cresci;S. Cristiani;E. Curtis-Lake;M. Dickinson;G. Fazio;H. Ferguson;F. Fiore;Maximilien Franco;J. Fynbo;A. Galametz;A. Georgakakis;M. Giavalisco;A. Grazian;N. Hathi;I. Jung;S. Kim;A. Koekemoer;Y. Khusanova;O. Fèvre;J. Lotz;F. Mannucci;D. Maltby;K. Matsuoka;D. McLeod;H. Méndez-Hernández;J. Méndez-Abreu;M. Mignoli;Michele Moresco;A. Mortlock;M. Nonino;M. Pannella;C. Papovich;P. Popesso;D. Rosario;M. Salvato;P. Santini;D. Schaerer;C. Schreiber;D. Stark;L. Tasca;R. Thomas;T. Treu;E. Vanzella;V. Wild;C. Williams;G. Zamorani;E. Zucca