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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
Matsuura, Shuji,Arai, Toshiaki,Bock, James J.,Cooray, Asantha,Korngut, Phillip M.,Kim, Min Gyu,Lee, Hyung Mok,Lee, Dae Hee,Levenson, Louis R.,Matsumoto, Toshio,Onishi, Yosuke,Shirahata, Mai,Tsumura, K American Astronomical Society 2017 The Astrophysical journal Vol.839 No.1
<P>The extragalactic background light (EBL) captures the total integrated emission from stars and galaxies throughout the cosmic history. The amplitude of the near-infrared EBL from space absolute photometry observations has been controversial and depends strongly on the modeling and subtraction of the zodiacal light (ZL) foreground. We report the first measurement of the diffuse background spectrum at 0.8-1.7 mu m from the CIBER experiment. The observations were obtained with an absolute spectrometer over two flights in multiple sky fields to enable the subtraction of ZL, stars, terrestrial emission, and diffuse Galactic light. After subtracting foregrounds and accounting for systematic errors, we find the nominal EBL brightness, assuming the Kelsall ZL model, is 42.7(-10.6) (+11.9) nW m(-2) sr(-1) at 1.4 mu m. We also analyzed the data using the Wright ZL model, which results in a worse statistical fit to the data and an unphysical EBL, falling below the known background light from galaxies at. lambda<. 1.3 mu m. Using a model-independent analysis based on the minimum EBL brightness, we find an EBL brightness of 28.7(-3.3)(+5.1) nWm(-2) s(r-1) at 1.4 mu m. While the derived EBL amplitude strongly depends on the ZL model, we find that we cannot fit the spectral data to ZL, Galactic emission, and EBL from solely integrated galactic light from galaxy counts. The results require a new diffuse component, such as an additional foreground or an excess EBL with a redder spectrum than that of ZL.</P>
<i>Spitzer</i> Observations of the North Ecliptic Pole
Nayyeri, H.,Ghotbi, N.,Cooray, A.,Bock, J.,Clements, D. L.,Im, M.,Kim, M. G.,Korngut, P.,Lanz, A.,Lee, H. M.,Lee, D. H.,Malkan, M.,Matsuhara, H.,Matsumoto, T.,Matsuura, S.,Nam, U. W.,Pearson, C.,Serje American Astronomical Society 2018 The Astrophysical journal Supplement series Vol.234 No.2
<P>We present a photometric catalog for Spitzer Space Telescope warm mission observations of the North Ecliptic Pole (NEP; centered at R.A. = 18(h)00(m)00(s), decl. = 66(d)33(m)38(s).552). The observations are conducted with IRAC in the 3.6 and 4.5 mu m bands over an area of 7.04 deg(2), reaching 1 sigma depths of 1.29 mu Jy and 0.79 mu Jy in the 3.6 mu m and 4.5 mu m bands, respectively. The photometric catalog contains 380,858 sources with 3.6 and 4.5 mu m band photometry over the full-depth NEP mosaic. Point-source completeness simulations show that the catalog is 80% complete down to 19.7 AB. The accompanying catalog can be used for constraining the physical properties of extragalactic objects, studying the AGN population, measuring the infrared colors of stellar objects, and studying the extragalactic infrared background light.</P>
On the origin of near-infrared extragalactic background light anisotropy
Zemcov, Michael,Smidt, Joseph,Arai, Toshiaki,Bock, James,Cooray, Asantha,Gong, Yan,Kim, Min Gyu,Korngut, Phillip,Lam, Anson,Lee, Dae Hee,Matsumoto, Toshio,Matsuura, Shuji,Nam, Uk Won,Roudier, Gael,Tsu American Association for the Advancement of Scienc 2014 Science Vol.346 No.6210
<P><B>A diffuse cosmic glow is not primordial</B></P><P>A cumulative map of all photons ever emitted by any star or galaxy is a highly desirable historical record of the universe's evolution. For this reason, cosmologists have sought to measure this diffuse distribution of light: the extragalactic background light. Zemcov <I>et al.</I> sent up a rocket to measure the fluctuations in this faint background and found largescale fluctuations greater than known galaxies alone should produce (see the Perspective by Moseley). Stars tidally stripped from their host galaxies are the most likely culprit, rather than unknown primordial galaxies.</P><P><I>Science</I>, this issue p. 732; see also p. 696</P><P>Extragalactic background light (EBL) anisotropy traces variations in the total production of photons over cosmic history and may contain faint, extended components missed in galaxy point-source surveys. Infrared EBL fluctuations have been attributed to primordial galaxies and black holes at the epoch of reionization (EOR) or, alternately, intrahalo light (IHL) from stars tidally stripped from their parent galaxies at low redshift. We report new EBL anisotropy measurements from a specialized sounding rocket experiment at 1.1 and 1.6 micrometers. The observed fluctuations exceed the amplitude from known galaxy populations, are inconsistent with EOR galaxies and black holes, and are largely explained by IHL emission. The measured fluctuations are associated with an EBL intensity that is comparable to the background from known galaxies measured through number counts and therefore a substantial contribution to the energy contained in photons in the cosmos.</P>
Kim, Min Gyu,Lee, Hyung Mok,Arai, Toshiaki,Bock, James,Cooray, Asantha,Jeong, Woong-Seob,Kim, Seong Jin,Korngut, Phillip,Lanz, Alicia,Lee, Dae Hee,Lee, Myung Gyoon,Matsumoto, Toshio,Matsuura, Shuji,Na American Astronomical Society 2017 The Astronomical journal Vol.153 No.2
<P>We present near-infrared (0.8-1.8 mu m) spectra of 105 bright (m(J) < 10) stars observed with the low-resolution spectrometer on the rocket-borne Cosmic Infrared Background Experiment. As our observations are performed above the Earth ' s atmosphere, our spectra are free from telluric contamination, which makes them a unique resource for near-infrared spectral calibration. Two-Micron All-Sky Survey photometry information is used to identify crossmatched stars after reduction and extraction of the spectra. We identify the spectral types of the observed stars by comparing them with spectral templates from the Infrared Telescope Facility library. All the observed spectra are consistent with late F to M stellar spectral types, and we identify various infrared absorption lines.</P>
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.