High Redshift Quasars as Probes of Early Star Formation

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High Redshift Quasars as Probes of Early Star Formation. / Dietrich, M.; Hamann, F.; Vestergaard, M.

I: Astronomical Society of the Pacific. Conference Proceedings, Bind 311, 01.06.2004, s. 403.

Publikation: Bidrag til tidsskrift › Konferenceartikel › Forskning › fagfællebedømt

Harvard

Dietrich, M, Hamann, F & Vestergaard, M 2004, 'High Redshift Quasars as Probes of Early Star Formation', Astronomical Society of the Pacific. Conference Proceedings, bind 311, s. 403.

APA

Dietrich, M., Hamann, F., & Vestergaard, M. (2004). High Redshift Quasars as Probes of Early Star Formation. Astronomical Society of the Pacific. Conference Proceedings, 311, 403.

Vancouver

Dietrich M, Hamann F, Vestergaard M. High Redshift Quasars as Probes of Early Star Formation. Astronomical Society of the Pacific. Conference Proceedings. 2004 jun. 1;311:403.

Author

Dietrich, M. ; Hamann, F. ; Vestergaard, M. / High Redshift Quasars as Probes of Early Star Formation. I: Astronomical Society of the Pacific. Conference Proceedings. 2004 ; Bind 311. s. 403.

Bibtex

@inproceedings{b7191782bda84e41b8ea7768807b08de,
title = "High Redshift Quasars as Probes of Early Star Formation",
abstract = "We present measurements of ultraviolet Fe II/Mg II emission line ratios for high redshift quasars (z ⪉ 5) in order to estimate the beginning of intense star formation in the early universe. A detailed comparison of these quasars at high redshifts to composite spectra of quasars at the same luminosity but lower redshifts indicates a lack of evolution in the Fe II/Mg II ratio and, by inference, the Fe/Mg abundance ratio. Nucleosynthesis and stellar evolution models predict that α-elements like Mg are produced by massive stars ending in type II SNe, while Fe is formed predominantly in SNe of type Ia. Guided by the resulting iron enrichment delay of ˜ 0.3 - 0.6 Gyr, we tentatively conclude that major star formation activity in the host galaxies of our high-z quasars must have started at zf ≃ 6 - 9, when the age of the universe was ˜ 0.5 Gyr (Ho = 72 km s-1 Mpc-1, ΩM = 0.3, ΩΛ = 0.7).",
author = "M. Dietrich and F. Hamann and M. Vestergaard",
year = "2004",
month = jun,
day = "1",
language = "English",
volume = "311",
pages = "403",
journal = "Astronomical Society of the Pacific. Conference Proceedings",
issn = "1050-3390",
publisher = "astronomical society of the pacific",

}

RIS

TY - GEN

T1 - High Redshift Quasars as Probes of Early Star Formation

AU - Dietrich, M.

AU - Hamann, F.

AU - Vestergaard, M.

PY - 2004/6/1

Y1 - 2004/6/1

N2 - We present measurements of ultraviolet Fe II/Mg II emission line ratios for high redshift quasars (z ⪉ 5) in order to estimate the beginning of intense star formation in the early universe. A detailed comparison of these quasars at high redshifts to composite spectra of quasars at the same luminosity but lower redshifts indicates a lack of evolution in the Fe II/Mg II ratio and, by inference, the Fe/Mg abundance ratio. Nucleosynthesis and stellar evolution models predict that α-elements like Mg are produced by massive stars ending in type II SNe, while Fe is formed predominantly in SNe of type Ia. Guided by the resulting iron enrichment delay of ˜ 0.3 - 0.6 Gyr, we tentatively conclude that major star formation activity in the host galaxies of our high-z quasars must have started at zf ≃ 6 - 9, when the age of the universe was ˜ 0.5 Gyr (Ho = 72 km s-1 Mpc-1, ΩM = 0.3, ΩΛ = 0.7).

AB - We present measurements of ultraviolet Fe II/Mg II emission line ratios for high redshift quasars (z ⪉ 5) in order to estimate the beginning of intense star formation in the early universe. A detailed comparison of these quasars at high redshifts to composite spectra of quasars at the same luminosity but lower redshifts indicates a lack of evolution in the Fe II/Mg II ratio and, by inference, the Fe/Mg abundance ratio. Nucleosynthesis and stellar evolution models predict that α-elements like Mg are produced by massive stars ending in type II SNe, while Fe is formed predominantly in SNe of type Ia. Guided by the resulting iron enrichment delay of ˜ 0.3 - 0.6 Gyr, we tentatively conclude that major star formation activity in the host galaxies of our high-z quasars must have started at zf ≃ 6 - 9, when the age of the universe was ˜ 0.5 Gyr (Ho = 72 km s-1 Mpc-1, ΩM = 0.3, ΩΛ = 0.7).

UR - http://adsabs.harvard.edu/full/2004ASPC..311..403D

M3 - Conference article

VL - 311

SP - 403

JO - Astronomical Society of the Pacific. Conference Proceedings

JF - Astronomical Society of the Pacific. Conference Proceedings

SN - 1050-3390

ER -

ID: 230144478