The Far-Infrared Surveyor (FIS) for AKARI

By M. Kawada, H. Baba, P. Barthel, D. Clements, Marvin L. Cohen, Y. Doi, E. Figuerêdo, M. Fujiwara, T. Goto, S. Hasegawa and 50 more. 2007

203 citations recorded by the source corpus.

The Far-Infrared Surveyor (FIS) is one of two focal-plane instruments on the AKARI satellite. FIS has four photometric bands at 65, 90, 140, and 160 mu m, and uses two kinds of array detectors. The FIS arrays and optics are designed to sweep the sky with high spatial resolution and redundancy. The actual scan width is more than eight arcminutes, and the pixel pitch matches the diffraction limit of the telescope. Derived point-spread functions (PSFs) from observations of asteroids are similar to those given by the optical model. Significant excesses, however, are clearly seen around tails of the PSFs, whose contributions are about 30% of the total power. All FIS functions are operating well in orbit, and the performance meets the laboratory characterizations, except for the two longer wavelength bands, which are not performing as well as characterized. Furthermore, the FIS has a spectroscopic capability using a Fourier transform spectrometer (FTS). Because the FTS takes advantage of the optics and detectors of the photometer, it can simultaneously make a spectral map. This paper summarizes the in-flight technical and operational performance of the FIS.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c6c9a73f77edd7719190a87d286b340c88119e53

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In Astronomy and Astrophysics

1. D. M. Alexander
2. D. Elbaz
3. E. Daddi
4. Mark Dickinson
5. D. Narayanan
6. C. Casey
7. P. Hopkins
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In Instrumentation

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2. D. M. Alexander
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7. D. Narayanan
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Citations in the corpus

• Dusty Star Forming Galaxies at High Redshift (2014, background): “Far-Infrared Surveyor [FIS], 2006–2011 The Far-Infrared Surveyor on board the 68.5 cm AKARI telescope (formerly known as the ASTRO-F satellite; Murakami et al., 2007; Kawada et al., 2007) imaged the sky at 65, 90, 140, and 160 µm.”
• A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “2 (Moshir et al. 1992) and SDSS DR7, and supplemented with data from the AKARI/Far-Infrared Surveyor (FIS; Kawada et al. 2007) All-Sky Survey Bright Source Catalogue ver 1.0 and photo-z’s from Hwang et al. (2010).”
• GOODS–Herschel: an infrared main sequence for star-forming galaxies (2011, methodology): “Far-IR measurements were supplemented with theAKARI/Far-Infrared Surveyor (FIS; Kawada et al. 2007) all-sky survey Bright Source Catalogue (BSC ver.”
• The AKARI/IRC mid-infrared all-sky survey (2010, methodology): “It has two scientific instruments, the Infrared Camera (IRC; Onaka et al., 2007) for 2–26µm and the Far-Infrared Surveyor (FIS; Kawada et al., 2007) for 50–200µm.”
• REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “…thanks to the presence of a counterpart in either the IRAS Faint Source Catalog (v2; Moshir et al. 1992) or the AKARI/Far-Infrared Surveyor (FIS; Kawada et al. 2007) all-sky survey Bright Source Kroupa (2001) and a Baldry & Glazebrook (2003) IMF are converted to the Chabrier scale by adding…”