AKARI OBSERVATION OF THE FLUCTUATION OF THE NEAR-INFRARED BACKGROUND. (2011, ApJ,742,124). T. Matsumoto 1,2 , H. J. Seo 1 , W.-S. Jeong 3 , H. M. Lee 1 , S. Matsuura 2 , H. Matsuhara 2 , S. Oyabu 2,4 , J. Pyo 3 , and T. Wada 2. 1 SNU, 2 ISAS, 3 KASI, 4 Nagoya University.
T. Matsumoto1,2, H. J. Seo1, W.-S. Jeong3, H. M. Lee1,
S. Matsuura2, H. Matsuhara2, S. Oyabu2,4, J. Pyo3, and T. Wada2
1SNU, 2ISAS, 3KASI, 4Nagoya University
Table. Parameters in this study
Item N2 N3 N4
Number of stacked images
40 39 24
Integration time (min)
29.6 28.9 17.8
Remaining pixels (%)
47.7 46.7 47.1
Limiting magnitude (AB mag)
22.9 23.2 23.8
Fig.1Smoothed images are obtained by averaging pixels within a 50 arcseconds diameter circle centered on each pixel. Black regions in mid and lower panel represent masked pixels. The diameter of each image is 10 arcminutes. Images correspond to 2.4, 3.2, and 4.1μm from left to right. The unit is nW m−2 sr−1.
Fig.2 Fluctuation spectra of mid panel in Fig.1 obtained by two-dimensional FFT. Blue solid lines represent fluctuation spectra of shot noise due to unresolved faint galaxies, which are estimated by simulation.
Fig.4 Spectrum of excess fluctuation at large scale (filled circles) is compared with the Spitzer result (squares).
Fig.3 Correlations between the near-infrared and the far-infrared (90μm).