Infrared Camera (IRC) Deep Survey in the Performance-Verification Phase

Wada, Takehiko; Oyabu, Shinki; Ita, Yoshifusa; Matsuhara, Hideo; Pearson, Chris; Onaka, Takashi; Ohyama, Youichi; Usui, Fumihiko; Fujishiro, Naofumi; Ishihara, Daisuke; Kataza, Hirokazu; Kim, Woojung; Matsumoto, Toshio; Murakami, Hiroshi; Sakon, Itsuki; Tanabé, Toshihiko; Takagi, Toshinobu; Uemizu, Kazunori; Ueno, Munetaka; Watarai, Hitoshi

doi:10.1093/pasj/59.sp2.s515

Cited by 24 publications

(4 citation statements)

References 35 publications

(39 reference statements)

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“…for the NIR bands and about 0.6 -0.8 mag for the MIR bands (except for L24 which has a relatively larger difference of 1.0 mag.) Wada et al (2007) also found a similar trend in the differences between the 5σ detection limits and 50% completeness limits for the NEP-Deep data. By comparing a single exposure and stacked image of ten exposures, they found that the 50% limits do not improve much for the NIR bands, while the improvements for the MIR bands are close to the square-root of the exposure time.…”

Section: Detection Limits and Completenesssupporting

confidence: 68%

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The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

Kim

Lee

Matsuhara

et al. 2012

A&A

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We present a photometric catalog of infrared (IR) sources based on the North Ecliptic Pole Wide field (NEP-Wide) survey of AKARI, which is an infrared space telescope launched by Japan. The NEP-Wide survey covered 5.4 deg 2 area, a nearly circular shape centered on the NEP, using nine photometric filter-bands from 2−25 μm of the Infrared Camera (IRC). Extensive efforts were made to reduce possible false objects due to cosmic ray hits, multiplexer bleeding phenomena around bright sources, and other artifacts. The number of detected sources varied depending on the filter band: with about 109 000 sources being cataloged in the near-infrared (NIR) bands at 2−5 μm, about 20 000 sources in the shorter parts of the mid-infrard (MIR) bands between 7−11 μm, and about 16 000 sources in the longer parts of the MIR band, with ∼4000 sources at 24 μm. The estimated 5σ detection limits are approximately 21 mag (mag) in the 2−5 μm bands, 19.5−19 mag in the 7−11 μm, and 18.8−18.5 mag in the 15−24 μm bands in the AB magnitude scale. The completenesses for those bands were evaluated as a function of magnitude: the 50% completeness limits are about 19.8 mag at 3 μm, 18.6 mag at 9 μm, and 18 mag at 18 μm band, respectively. To construct a reliable source catalog, all of the detected sources were examined by matching them with those in other wavelength data, including optical and ground-based NIR bands. The final band-merged catalog contains about 114 800 sources detected in the IRC filter bands. The properties of the sources are presented in terms of the distributions in various color-color diagrams.

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Section: Detection Limits and Completenesssupporting

confidence: 68%

“…On the basis of these results, they concluded that the NIR bands are affected by the source confusion. In fact, the improvement in the 50% limit between one pointing and ten pointing observations is only a factor of 1.15 (Wada et al 2007) for the N3 band, implying that the source confusion could be significant.…”

Section: Detection Limits and Completenessmentioning

confidence: 99%

The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

Kim

Lee

Matsuhara

et al. 2012

A&A

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“…The earliest surveys were by the Infrared Space Observatory (ISO; Elbaz et al 1999;Gruppioni et al 2002;Rodighiero et al 2004) at 15 μm. Larger and deeper surveys came from Akari/IRC at 15 μm and the Spitzer/IRS peakup imager at 16 μm (Wada et al 2007;Burgarella et al 2009;Pearson et al 2010;Teplitz et al 2011). The present study uses photometric catalogs from the latter two surveys.…”

Section: The 16 μM Selected Samplementioning

confidence: 99%

A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions

Huang

Dai

Willner

et al. 2021

ApJ

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We describe a complete, flux-density-limited sample of galaxies at redshift 0.8 < z < 1.3 selected at 16 μm. At the selection wavelength near 8 μm rest, the observed emission comes from both dust heated by intense star formation and active galactic nuclei (AGNs). Fitting the spectral energy distributions (SEDs) of the sample galaxies to local-galaxy templates reveals that more than half the galaxies have SEDs dominated by star formation. About one-sixth of the galaxy SEDs are dominated by an AGN, and nearly all of the rest of the SEDs are composite. Comparison with X-ray and far-infrared observations shows that combinations of luminosities at rest-frame 4.5 and 8 μm give good measures of both AGN luminosity and star formation rate. The sample galaxies mostly follow the established star-forming main sequence for z = 1 galaxies, but of the galaxies more than 0.5 dex above that main sequence, more than half have AGN-type SEDs. Similarly, the most luminous AGNs tend to have higher star formation rates than the main-sequence value. Galaxies with stellar masses >1011 M ⊙ are unlikely to host an AGN. About 1% of the sample galaxies show an SED with dust emission typical of neither star formation nor an AGN.

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“…We used the NEP deep survey data at two wavelength bands, 2.4 and 3.2 µm. Only a portion (∼30%) of the NEP deep survey area is selected to produce a reliable mosaicked image (the top panel of Figure 1) since some parts of the survey data are affected by the earthshine (Wada et al 2007) and a planetary nebula.…”

Section: Introductionmentioning

confidence: 99%

Akari Observations of the Fluctuations of the Near-Infrared Background Ii

Seo¹,

Lee²,

Matsumoto³

et al. 2017

Publications of The Korean Astronomical Society

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We report a spatial fluctuation analysis of the sky brightness in the near-infrared from observations towards the north ecliptic pole (NEP) by AKARI at 2.4 and 3.2 µm. As a follow up study of our previous work on the Monitor field of AKARI, we used NEP deep survey data, which covered a circular area of about 0.4 square degrees, in order to extend fluctuation analysis at angular scales up to 1000 . After pre-processing, additional correction procedures were done to correct time varying components and instrumental effects such as MUXbleed. To remove resolved objects, we applied 2σ clipping and point spread function (PSF) subtraction. We finally obtained mosaicked images which can be used for the study of various diffuse emissions in the near-infrared sky and found that there are spatial structures in the mosaicked images using a power spectrum analysis.

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Infrared Camera (IRC) Deep Survey in the Performance-Verification Phase

Cited by 24 publications

References 35 publications

The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions

Akari Observations of the Fluctuations of the Near-Infrared Background Ii

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