TY - JOUR
T1 - Infrared spectroscopy of the gravitationally lensed quasar B1422+231
T2 - Mg II λ2798 and Fe II emission from the broad-line gas at z = 3.62
AU - Kawara, Kimiaki
AU - Murayama, Takashi
AU - Taniguchi, Yoshiaki
AU - Arimoto, Nobuo
N1 - Funding Information:
1The Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara-shi, Kanagawa 229, Japan. 2 Present address: ISO Science Operations Centre, Astrophysics Division of ESA, Villafranca, 28080 Madrid, Spain; kkawara@iso.vilspa.esa.es. 3Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation. 4 Astronomical Institute, Tohoku University, Aoba, Sendai, 980-77, Japan; murayama@astroa.astr.tohoku.ac.jp, tani@astroa.astr.tohoku.ac.jp. 5Royal Greenwich Observatory, Madingly Road, Cambridge CB3 0EZ, England, UK. 6Institute of Astronomy, University of Tokyo, 2-21-1, Osawa, Mitaka, Tokyo 181, Japan; arimoto@mtk.ioa.s.u-tokyo.ac.jp.
Funding Information:
Astronomy Observatories. This work was financially supported in part by Grant-in-Aids for the Scientific Research (Nos. 06640349, 07222206, and 0704405) of the Japanese Ministry of Education, Culture, Sport, and Science, and by the Founda- tion for Promotion of Astronomy, Japan. Y. T. would like to thank K. Tritton, R. Terlevich, E. Terlevich, and I. Salamanca for their warm hospitality at the Royal Greenwich Observatory.
PY - 1996
Y1 - 1996
N2 - The rest-frame UV-optical (2000-5300 Å) spectrum of the gravitationally lensed flat-spectrum radio-loud quasar B1422+231 system at z = 3.62 is presented. The spectrum is similar to the Large Bright Quasar Survey (LBQS) composite spectrum (Francis et al.), which indicates no significant UV-optical spectral evolution in some quasars at 0 < z < 3.6. The Fe n(UV + optical)/Mg II λ2798 flux ratio is 12.2 ±3.9, which is comparable to 8.9 for the LBQS composite spectrum of quasars at z = 1-2 analyzed in this work, and 7.8 ±2.6 for quasars at z = 0.15-0.63 analyzed by Wills, Netzer, & Wills. It is concluded that the majority of stars in the host galaxy of B1422+231 have formed much earlier (∼1.5 Gyr) than z = 3.6. The first detection of [O II] λ5007 in a quasar beyond z = 3 is also reported.
AB - The rest-frame UV-optical (2000-5300 Å) spectrum of the gravitationally lensed flat-spectrum radio-loud quasar B1422+231 system at z = 3.62 is presented. The spectrum is similar to the Large Bright Quasar Survey (LBQS) composite spectrum (Francis et al.), which indicates no significant UV-optical spectral evolution in some quasars at 0 < z < 3.6. The Fe n(UV + optical)/Mg II λ2798 flux ratio is 12.2 ±3.9, which is comparable to 8.9 for the LBQS composite spectrum of quasars at z = 1-2 analyzed in this work, and 7.8 ±2.6 for quasars at z = 0.15-0.63 analyzed by Wills, Netzer, & Wills. It is concluded that the majority of stars in the host galaxy of B1422+231 have formed much earlier (∼1.5 Gyr) than z = 3.6. The first detection of [O II] λ5007 in a quasar beyond z = 3 is also reported.
KW - Cosmology: observations
KW - Galaxies: evolution
KW - Galaxies: formation
KW - Gravitational lensing
KW - Quasars: emission lines
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U2 - 10.1086/310315
DO - 10.1086/310315
M3 - Article
AN - SCOPUS:15444362625
SN - 0004-637X
VL - 470
SP - L85-L88
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 PART II
ER -