FeII/MgII Emission Line Ratio in High Redshift Quasars

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

FeII/MgII Emission Line Ratio in High Redshift Quasars. / Dietrich, M.; Hamann, F.; Appenzeller, I.; Vestergaard, Marianne.

In: Astrophysical Journal, Vol. 596, No. 2, 817, 27.06.2003.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Dietrich, M, Hamann, F, Appenzeller, I & Vestergaard, M 2003, 'FeII/MgII Emission Line Ratio in High Redshift Quasars', Astrophysical Journal, vol. 596, no. 2, 817. https://doi.org/10.1086/378045

APA

Dietrich, M., Hamann, F., Appenzeller, I., & Vestergaard, M. (2003). FeII/MgII Emission Line Ratio in High Redshift Quasars. Astrophysical Journal, 596(2), [817]. https://doi.org/10.1086/378045

Vancouver

Dietrich M, Hamann F, Appenzeller I, Vestergaard M. FeII/MgII Emission Line Ratio in High Redshift Quasars. Astrophysical Journal. 2003 Jun 27;596(2). 817. https://doi.org/10.1086/378045

Author

Dietrich, M. ; Hamann, F. ; Appenzeller, I. ; Vestergaard, Marianne. / FeII/MgII Emission Line Ratio in High Redshift Quasars. In: Astrophysical Journal. 2003 ; Vol. 596, No. 2.

Bibtex

@article{c4420e8ac79349208a85770e8d2c4afe,
title = "FeII/MgII Emission Line Ratio in High Redshift Quasars",
abstract = "We present results of the analysis of near infrared spectroscopic observations of 6 high-redshift quasars (z > 4), emphasizing the measurement of the ultraviolet FeII/MgII emission line strength in order to estimate the beginning of intense star formation in the early universe. To investigate the evolution of the FeII/MgII ratio over a wider range in cosmic time, we measured this ratio for composite quasar spectra which cover a redshift range of 0 4 quasars must have started already at an epoch corresponding to z_f = 6 to 9, when the age of the universe was ~0.5 Gyr (H_o = 72 km/s/Mpc, Omega_M = 0.3, Omega_Lambda = 0.7). This epoch corresponds well to the re-ionization era of the universe.",
keywords = "astro-ph",
author = "M. Dietrich and F. Hamann and I. Appenzeller and Marianne Vestergaard",
year = "2003",
month = jun,
day = "27",
doi = "10.1086/378045",
language = "English",
volume = "596",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",
number = "2",

}

RIS

TY - JOUR

T1 - FeII/MgII Emission Line Ratio in High Redshift Quasars

AU - Dietrich, M.

AU - Hamann, F.

AU - Appenzeller, I.

AU - Vestergaard, Marianne

PY - 2003/6/27

Y1 - 2003/6/27

N2 - We present results of the analysis of near infrared spectroscopic observations of 6 high-redshift quasars (z > 4), emphasizing the measurement of the ultraviolet FeII/MgII emission line strength in order to estimate the beginning of intense star formation in the early universe. To investigate the evolution of the FeII/MgII ratio over a wider range in cosmic time, we measured this ratio for composite quasar spectra which cover a redshift range of 0 4 quasars must have started already at an epoch corresponding to z_f = 6 to 9, when the age of the universe was ~0.5 Gyr (H_o = 72 km/s/Mpc, Omega_M = 0.3, Omega_Lambda = 0.7). This epoch corresponds well to the re-ionization era of the universe.

AB - We present results of the analysis of near infrared spectroscopic observations of 6 high-redshift quasars (z > 4), emphasizing the measurement of the ultraviolet FeII/MgII emission line strength in order to estimate the beginning of intense star formation in the early universe. To investigate the evolution of the FeII/MgII ratio over a wider range in cosmic time, we measured this ratio for composite quasar spectra which cover a redshift range of 0 4 quasars must have started already at an epoch corresponding to z_f = 6 to 9, when the age of the universe was ~0.5 Gyr (H_o = 72 km/s/Mpc, Omega_M = 0.3, Omega_Lambda = 0.7). This epoch corresponds well to the re-ionization era of the universe.

KW - astro-ph

U2 - 10.1086/378045

DO - 10.1086/378045

M3 - Journal article

VL - 596

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 817

ER -

ID: 123370693