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THE <i>COSMIC INFRARED BACKGROUND EXPERIMENT</i> ( <i>CIBER</i> ): THE LOW RESOLUTION SPECTROMETER
Tsumura, K.,Arai, T.,Battle, J.,Bock, J.,Brown, S.,Cooray, A.,Hristov, V.,Keating, B.,Kim, M. G.,Lee, D. H.,Levenson, L. R.,Lykke, K.,Mason, P.,Matsumoto, T.,Matsuura, S.,Murata, K.,Nam, U. W.,Renbarg IOP Publishing 2013 The Astrophysical journal Supplement series Vol.207 No.2
THE <i>COSMIC INFRARED BACKGROUND EXPERIMENT</i> ( <i>CIBER</i> ): THE NARROW-BAND SPECTROMETER
Korngut, P. M.,Renbarger, T.,Arai, T.,Battle, J.,Bock, J.,Brown, S. W.,Cooray, A.,Hristov, V.,Keating, B.,Kim, M. G.,Lanz, A.,Lee, D. H.,Levenson, L. R.,Lykke, K. R.,Mason, P.,Matsumoto, T.,Matsuura, IOP Publishing 2013 The Astrophysical journal, Supplement series Vol.207 No.2
Observation of the Cosmic Near-Infrared Background with the CIBER rocket
MinGyu Kim,T. Matsumoto,Hyung Mok Lee,T. Arai,J. Battle,J. Bock,S. Brown,A. Cooray,V. Hristov,B. Keating,P. Korngut,Dae-Hee Lee,L. R. Levenson,K. Lykke,P. Mason,S. Matsuura,U. W. Nam,T. Renbarger,A. S 한국천문학회 2012 天文學會報 Vol.37 No.1
Identification and spectral analysis of the CIBER/LRS detected stars
김민규,이형목,이대희,남욱원,정웅섭,Kim, MinGyu,Matsumoto, T.,Lee, Hyung Mok,Arai, T.,Battle, J.,Bock, J.,Brown, S.,Cooray, A.,Hristov, V.,Keating, B.,Korngut, P.,Lee, Dae-Hee,Levenson, L.R.,Lykke, K.,Mason, P.,Matsu 한국천문학회 2012 天文學會報 Vol.37 No.2
CIBER (Cosmic Infrared Background ExpeRiment) is a sounding-rocket borne experiment which is designed to find the evidence of the First stars (Pop.III stars) in the universe. They are expected to be formed between the recombination era at z ~ 1100 and the most distant quasar (z ~ 8). They have never been directly detected due to its faintness so far, but can be observed as a background radiation at around $1{\mu}m$ which is called the Cosmic Near-Infrared Background (CNB). The CIBER is successfully launched on July 10, 2010 at White Sands Missile Range, New Mexico, USA. It consists of three kinds of instruments. One of them is a LRS (Low Resolution Spectrometer) which is a refractive telescope of 5.5 cm aperture with spectral resolution of 20 ~ 30 and wavelength coverage of 0.7 to $2.0{\mu}m$ to measure the spectrum of the CNB. Since LRS detects not only CNB but also stellar components, we can study their spectral features with the broad band advantage especially at around $1{\mu}m$ which is difficult at ground observations because of the atmospheric absorption by water vapor. I identified around 300 stars from observed six fields. If we can classify their spectral types with SED fitting, we can study their physical conditions of the stellar atmosphere as well as making a stellar catalogue of continuous stellar spectrum.