Calibration of the AKARI Far-Infrared Imaging Fourier-Transform Spectrometer

Murakami, Noriko; Kawada, Manabu; Takahashi, H.; Okada, Yoko; Yasuda, Akiko; Ootsubo, Takafumi; Kaneda, Hidehiro; Matsuo, Hiroshi; Baluteau, J. P.; Davis-Imhof, Peter; Gom, Brad; Naylor, David; Zavagno, A.; Yamamura, I.; Matsuura, Shuji; Shirahata, Mai; Doi, Yasuo; Shibai, Hiroshi

doi:10.1093/pasj/62.5.1155

Cited by 9 publications

(7 citation statements)

References 33 publications

(16 reference statements)

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“…The [OIII] 88µm intensity map taken by the MIPS covers the center of 30 Dor (rectangle in figure 1), partially overlapped with our map at the north edge. The MIPS measurement shows values about three times larger than ours, but both are roughly consistent by considering large uncertainties of our absolute line intensity calibration (Murakami et al 2010). Owing to our clear detection outside the Spitzer observing area, we reveal the widely extended structure of the highly-ionized region.…”

Section: [Oiii] Intensity Mapsupporting

confidence: 90%

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Widely Extended [O III] 88μm Line Emission around the 30 Doradus Region Revealed with AKARI FIS-FTS

Kawada

Takahashi

Yasuda

et al. 2011

Publications of the Astronomical Society of Japan

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We present the distribution map of the far-infrared [OIII] 88µm line emission around the 30 Doradus (30 Dor) region in the Large Magellanic Cloud obtained with the Fourier Transform Spectrometer of the Far-Infrared Surveyor onboard AKARI. The map reveals that the [OIII] emission is widely distributed by more than 10 ′ around the super star cluster R136, implying that the 30 Dor region is affluent with interstellar radiation field hard enough to ionize O 2+ . The observed [OIII] line intensities are as high as (1 − 2) × 10 −6 W m −2 sr −1 on the peripheral regions 4 ′ − 5 ′ away from the center of 30 Dor, which requires gas densities of 60 − 100 cm −3 . However the observed size of the distribution of the [OIII] emission is too large to be explained by massive stars in the 30 Dor region enshrouded by clouds with the constant gas density of 10 2 cm −3 . Therefore the surrounding structure is likely to be highly clumpy. We also find a global correlation between the [OIII] and the far-infrared continuum emission, suggesting that the gas and dust are well mixed in the highly-ionized region where the dust survives in clumpy dense clouds shielded from the energetic photons.

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Section: [Oiii] Intensity Mapsupporting

confidence: 90%

“…In the final step of the pipeline, raw spectra are converted to sky spectra by correcting for instrumental factors. Details of the calibration scheme of FIS-FTS and the accuracy are described in Murakami et al (2010).…”

Section: Data Reductionmentioning

confidence: 99%

Widely Extended [O III] 88μm Line Emission around the 30 Doradus Region Revealed with AKARI FIS-FTS

Kawada

Takahashi

Yasuda

et al. 2011

Publications of the Astronomical Society of Japan

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“…Its primary mission was to survey the entire sky in near-, mid-, and far-infrared, from 1.7 µm to 180 µm, through its 68.5 cm aperture telescope and with two kinds of instruments: the Far-Infrared Surveyor (FIS) for far-infrared observations and the InfraRed Camera (IRC) for near and mid-infrared observations. The calibration of the AKARI Far-Infrared Imaging Fourier Transform Spectrometer (FIS-FTS) has been described by Murakami et al (2010). It is based on bright astronomical sources, such as stars, asteroids and planets.…”

Section: Visible and Near- Mid- And Far-infrared Instrumentsmentioning

confidence: 99%

Spectroradiometry with space telescopes

Pauluhn

Huber

Smith

et al. 2015

Astron Astrophys Rev

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Radiometry, i.e. measuring the power of electromagnetic radiationhitherto often referred to as "photometry"-is of fundamental importance in astronomy. We provide an overview of how to achieve a valid laboratory calibration of space telescopes and discuss ways to reliably extend this calibration to the spectroscopic telescope's performance in space. A lot of effort has been, and still is going into radiometric "calibration" of telescopes once they are in space; these methods use celestial primary and transfer standards and are based in part on stellar models. The history of the calibration of the Hubble Space Telescope serves as a platform to review these methods. However, we insist that a true calibration of spectroscopic space telescopes must directly be based on and traceable to laboratory standards, and thus be independent of the observations. This has recently become a well-supported aim, following the discovery of the acceleration of the cosmic expansion by use of type-Ia supernovae, and has led to plans for launching calibration rockets for the visible and infrared spectral range. This is timely, too, because an adequate exploitation of data from present space missions, such as Gaia, and from many current astronomical projects like Euclid and WFIRST demands higher radiometric accuracy than is generally available today. A survey of the calibration of instruments observing from the X-ray to the infrared spectral domains that include instrument-or mission-specific estimates of radiometric accuracies rounds off this review.

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“…2c). Since some local spectra show unrealistically steep continuum slopes at wavenumbers smaller than 64 cm −1 (>156 μm), probably due to the calibration errors around the cuton wavenumber of the detector responsivity that varies among the array pixels (Murakami et al 2010), we additionally mask the spectral region at <65 cm −1 . We fit all the local spectra with the two dust modified blackbody components adopted in the above fitting, plus the [OIII] and [NII] emission lines, the OH absorption line, and the excess component.…”

Section: Spectra Of Various Local Areasmentioning

confidence: 99%

Properties of dust at the Galactic center probed by AKARI far-infrared spectral mapping

Kaneda

Yasuda

Onaka

et al. 2012

A&A

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Aims. We investigate the properties of interstellar dust in the Galactic center region toward the Arches and Quintuplet clusters. Methods. With the Fourier Transform Spectrometer of the AKARI/Far-Infrared Surveyor, we performed the far-infrared (60-140 cm −1 ) spectral mapping of an area of about 10 × 10 that includes both clusters to obtain a low-resolution (R = 1.2 cm −1 ) spectrum at every spatial bin of 30 × 30 . Results. We derive the spatial variations in the dust continuum emission at different wavenumbers, which are compared with those of the [OIII] 88 μm (113 cm −1 ) emission and the OH 119 μm (84 cm −1 ) absorption. The spectral fitting shows that two modified blackbody components with temperatures of ∼20 K and ∼50 K can reproduce most of the continuum spectra. For some spectra, however, we find that there is a significant excess on top of a modified blackbody continuum around 80-90 cm −1 (110-130 μm). Conclusions. The warmer dust component is spatially correlated with the [OIII] emission and hence likely to be associated with the highly-ionized gas locally heated by intense radiation from the two clusters. The excess emission probably represents a dust feature, which is found to be spatially correlated with the OH absorption and a CO cloud. We find that a dust model including micron-sized graphite grains can quite closely reproduce the observed spectrum with the dust feature.

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Calibration of the AKARI Far-Infrared Imaging Fourier-Transform Spectrometer

Cited by 9 publications

References 33 publications

Widely Extended [O III] 88μm Line Emission around the 30 Doradus Region Revealed with AKARI FIS-FTS

Widely Extended [O III] 88μm Line Emission around the 30 Doradus Region Revealed with AKARI FIS-FTS

Spectroradiometry with space telescopes

Properties of dust at the Galactic center probed by AKARI far-infrared spectral mapping

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