The AKARI/IRC mid-infrared all-sky survey

By D. Ishihara, T. Onaka, H. Kataza, A. Salama, C. Alfageme, A. Cassatella, N. Cox, P. Garcı́a-Lario, C. Stephenson, Marvin L. Cohen and 49 more. 2010

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Context. AKARI is the first Japanese astronomical satellite dedicated to infrared astronomy. One of the main purposes of AKARI is the all-sky survey performed with six infrared bands between 9 μ m and 200 μ m during the period from 2006 May 6 to 2007 August 28. In this paper, we present the mid-infrared part (9 μ m and 18 μ m bands) of the survey carried out with one of the on-board instruments, the infrared camera (IRC). Aims. We present unprecedented observational results of the 9 μ m and 18 μ m AKARI all-sky survey and detail the operation and data processing leading to the point source detection and measurements. Methods. The raw data are processed to produce small images for every scan, and the point sources candidates are derived above the 5 σ noise level per single scan. The celestial coordinates and fluxes of the events are determined statistically and the reliability of their detections is secured through multiple detections of the same source within milli-seconds, hours, and months from each other. Results. The sky coverage is more than 90% for both bands. A total of 877 091 sources (851 189 for 9 μ m, 195 893 for 18 μ m) are confirmed and included in the current release of the point source catalog. The detection limit for point sources is 50 mJy and 90 mJy for the 9 μ m and 18 μ m bands, respectively. The position accuracy is estimated to be better than 2 '' . Uncertainties in the in-flight absolute flux calibration are estimated to be 3% for the 9 μ m band and 4% for the 18 μ m band. The coordinates and fluxes of detected sources in this survey are also compared with those of the IRAS survey and are found to be statistically consistent.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/9afd5a7537c0686fc1787a0b7d2bbb399b2daef7

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Citations in the corpus

GOODS–Herschel: an infrared main sequence for star-forming galaxies (2011, background): “1.0, Ishihara et al. 2010) reaching a detection limit of 50 mJy (5σ) with a uniform distribution over the whole sky and closer than∼450 Mpc (z<0.1).”
The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, background): “PDS 415 is detected as an infrared source in the AKARI catalog (Ishihara et al. 2010) but CD-23 12840 is not detected.”
THE SPITZER–WISE SURVEY OF THE ECLIPTIC POLES (2011, background): “…the basis for defining the zero magnitude for the Infrared Space Observatory (ISO; Schaeidt et al. 1996; Cohen et al. 1996; Schulz et al. 2002), MSX (Cohen et al. 1992; Cohen et al. 1999), Spitzer (Cohen et al. 2003), and AKARI (Tanabe et al. 2008; Ishihara et al. 2010) infrared space telescopes.”
THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE (2010, methodology): “The AKARI mission (Murakami et al. 2007) used an ingeneous technique to survey the mid-IR sky at 9 & 18 µm with sensitivities of 50 & 100 mJy (Ishihara et al. 2010) with better angular resolution than IRAS.”
Asteroid Catalog Using AKARI: AKARI/IRC Mid-Infrared Asteroid Survey (2011, methodology): “The 5 detection limits at the S9W and L18W bands are 50 and 90 mJy, respectively, and the spatial resolution of the IRC in the All-Sky Survey mode was 1000 per pixel (Ishihara et al. 2010).”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “…al. 2010; Rebull et al. 2010), theWide-field Infrared Survey Explorer (WISE) all-sky catalog (Wright et al. 2010), the AKARI point source catalogs (Ishihara et al. 2010), and the Infrared Astronomical Satellite (IRAS) point source catalog (Beichman et al. 1988), with some additional ground- and…”
Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, methodology): “The 1-σ region of the model includes the γb uncertainty of AKARI at 15 μm (4%, Ishihara et al. 2010), PACS at 110 μm (about 10%, Berta et al. 2010), and LABOCA at 850 μm (8.5%, Weiß et al. 2009).”