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AKARI FAR-INFRARED ALL-SKY SURVEY MAPS
Doi, Yasuo,Komugi, Shinya,Kawada, Mitsunobu,Takita, Satoshi,Arimatsu, Ko,Ikeda, Norio,Kato, Daisuke,Kitamura, Yoshimi,Nakagawa, Takao,Ootsubo, Takafumi,Morishima, Takahiro,Hattori, Makoto,Tanaka, Masa The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
Far-infrared observations provide crucial data for the investigation and characterisation of the properties of dusty material in the Interstellar Medium (ISM), since most of its energy is emitted between ~ 100 and $200{\mu}m$. We present the first all-sky image from a sensitive all-sky survey using the Japanese AKARI satellite, in the wavelength range $50-180{\mu}m$. Covering > 99% of the sky in four photometric bands with four filters centred at $65{\mu}m$, $90{\mu}m$, $140{\mu}m$, and $160{\mu}m$ wavelengths, this achieved spatial resolutions from 1 to 2 arcmin and a detection limit of < 10 MJy $sr^{-1}$, with absolute and relative photometric accuracies of < 20%. All-sky images of the Galactic dust continuum emission enable astronomers to map the large-scale distribution of the diffuse ISM cirrus, to study its thermal dust temperature, emissivity and column density, and to measure the interaction of the Galactic radiation field and embedded objects with the surrounding ISM. In addition to the point source population of stars, protostars, star-forming regions, and galaxies, the high Galactic latitude sky is shown to be covered with a diffuse filamentary-web of dusty emission that traces the potential sites of high latitude star formation. We show that the temperature of dust particles in thermal equilibrium with the ambient interstellar radiation field can be estimated by using $90{\mu}m$, $140{\mu}m$, and $160{\mu}m$ data. The FIR AKARI full-sky maps provide a rich new data set within which astronomers can investigate the distribution of interstellar matter throughout our Galaxy, and beyond.
ADVANTAGES OF THE AKARI FIR ALL-SKY MAPS
YASUO DOI,SATOSHI TAKITA,TAKAFUMI OOTSUBO,KO ARIMATSU,MASAHIRO TANAKA,TAKAHIRO MORISHIMA,MITSUNOBU KAWADA,SHUJI MATSUURA,YOSHIMI KITAMURA,MAKOTO HATTORI,TAKAO NAKAGAWA,GLENN WHITE,NORIO IKEDA 한국천문학회 2017 天文學論叢 Vol.32 No.1
We present the {\it AKARI} far-infrared (FIR) all-sky maps and describe its characteristics, calibration accuracy and scientific capabilities. The {\it AKARI} FIR survey has covered 97\% of the whole sky in four photometric bands, which cover continuously 50--180 micron with band central wavelengths of 65, 90, 140, and 160 microns. The data have been publicly released in 2014 \citep{2015PASJ...67...50D} with improved data quality that have been achieved since the last internal data release \citep{2012PKAS...27..111D}. The accuracy of the absolute intensity is $\leq10$\% for the brighter regions. Quantitative analysis of the relative intensity accuracy and its dependence upon spatial scan numbers has been carried out. The data for the first time reveal the whole sky distribution ofinterstellar matter with arcminute-scale spatial resolutions at the peakof dust continuum emission, enabling us to investigate large-scaledistribution of interstellar medium in great detail. The filamentarystructure covering the whole sky is well traced by the all-sky maps. We describe advantages of the AKARI FIR all-sky maps for the study of interstellar matter comparing to other observational data.
FIR VIEW OF DISKS OF WEAK-LINE T TAURI STARS
SATOSHI TAKITA,YASUO DOI,KO ARIMATSU,TAKAFUMI OOTSUBO 한국천문학회 2017 天文學論叢 Vol.32 No.1
We have observed $\sim$60 Weak-line T Tauri stars (WTTSs) toward the Chamaeleon star forming region using the AKARI Far-Infrared Surveyor (FIS) All-Sky maps. We could not detect any significant emission from each source even at the most sensitive WIDE-S band. Then, we have performed stacking analysis of these WTTSs using the WIDE-S band images to improve the sensitivity. However, we could not detect any significant emission in the resultant image with a noise level of 0.05~MJy~sr$^{-1}$, or 3 mJy for a point source. The three-sigma upper limit of 9~mJy leads to the disk dust mass of 0.01~M$_{\oplus}$. This result suggests that the disks around Chamaeleon WTTSs are already evolved to debris disks.
A First Look at BISTRO Observations of the <i>ρ</i> Oph-A core
Kwon, Jungmi,Doi, Yasuo,Tamura, Motohide,Matsumura, Masafumi,Pattle, Kate,Berry, David,Sadavoy, Sarah,Matthews, Brenda C.,Ward-Thompson, Derek,Hasegawa, Tetsuo,Furuya, Ray S.,Pon, Andy,Francesco, Jame American Astronomical Society 2018 The Astrophysical Journal Vol.859 No.1
SMALL-SCALE STRUCTURE OF THE ZODIACAL DUST CLOUD OBSERVED IN FAR-INFRARED WITH AKARI
TAKAFUMI OOTSUBO,YASUO DOI,SATOSHI TAKITA,SHUJI MATSUURA,MITSUNOBU KAWADA,TAKAO NAKAGAWA,KO AROMATSU,MASAHIRO TANAKA,TORU KONDO,DAISUKE ISHIHARA,Fumihiko Usui,MAKOTO HATTORI 한국천문학회 2017 天文學論叢 Vol.32 No.1
The zodiacal light emission is the thermal emission from the interplanetary dust and the dominant diffuse radiation in the mid- to far-infrared wavelength region. Even in the far-infrared, the contribution of the zodiacal emission is not negligible at the region near the ecliptic plane. The AKARI far-infrared all-sky survey covered 97\% of the whole sky in four photometric bands with band central wavelengths of 65, 90, 140, and 160~$\mu$m. AKARI detected the small-scale structure of the zodiacal dust cloud, such as the asteroidal dust bands and the circumsolar ring, in far-infrared wavelength region. Although the most part of the zodiacal light structure in the AKARI far-infrared all-sky image can be well reproduced with the DIRBE zodiacal light model, there are discrepancies in the small-scale structures. In particular, the intensity and the ecliptic latitude of the peak position of the asteroidal dust bands cannot be reproduced precisely with the DIRBE models. The AKARI observational data during more than one year has advantages over the 10-month DIRBE data in modeling the full-sky zodiacal dust cloud. The resulting small-scale zodiacal light structure template has been used to subtract the zodiacal light from the AKARI all-sky maps.
THE FILAMENTARY WEB OF STAR FORMATION
White, Glenn J.,Doi, Yasuo,Komugi, Shinya,Kawada, Mitsunobu,Takita, Satoshi,Arimatsu, Ko,Ikeda, Norio,Kato, Daisuke,Kitamura, Yoshimi,Nakagawa, Takao,Ootsubo, Takafumi,Morishima, Takahiro,Hattori, Mak The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
Following the first Public Release of the AKARI Point Source catalogues, we have worked on the production of a new far-infrared All-Sky Diffuse mapping product. In this paper we report first results from the All Sky diffuse maps that will shortly be released to the community, based on analysis of data from the Far Infrared Surveyor ($65{\mu}m-160{\mu}m$) instrument. These data are likely to have a strong impact on studies of extended structures, and the diffuse ISM.
FOREGROUND OF GAMMA-RAY BURSTS (GRBS) FROM AKARI FIS DATA
L. Viktor Toth,YASUO DOI,SAROLTA ZAHORECZ,Marton Agas,LAJOS G. BALAZS,Adrienn Forro,Istvan I. Racz 한국천문학회 2017 天文學論叢 Vol.32 No.1
A significant number of the parameters of a gamma-ray burst (GRB) and its host galaxy are calculated from the afterglow. There are various methods obtaining extinction values for the necessary correction for galactic foreground. These are: galaxy counts, from HI 21 cm surveys, from spectroscopic measurements and colors of nearby Galactic stars, or using extinction maps calculated from infrared surveys towards the GRB. We demonstrate that \textit{AKARI} Far-Infrared Surveyor sky surface brightness maps are useful uncovering the fine structure of the galactic foreground of GRBs. Galactic cirrus structures of a number of GRBs are calculated with a 2 arcminute resolution, and the results are compared to that of other methods.
Little Leaguer’s Shoulder Can Cause Severe Three-Dimensional Humeral Deformity
Yuji Hosokawa,Teruhisa Mihata,Yasuo Itami,Masashi Neo,Munekazu Doi 대한정형외과학회 2017 Clinics in Orthopedic Surgery Vol.9 No.4
We analyzed three-dimensional (3D) humeral deformity (valgus–varus, flexion–extension, and rotational deformation) after little leaguer’s shoulder using 3D computed tomography in a 15-year-old male baseball player. Humeral retroversion was increased by 27.1° on the dominant side compared with the nondominant side. Compared with the nondominant shaft, the dominant humeral shaft was deformed in the varus direction (9.4°), resulting in a decreased neck–shaft angle (dominant side, 127.5°; nondominant side, 135.1°), and it was also deformed in the extension direction (21.0°). This case demonstrates that little leaguer’s shoulder can cause markedly greater humeral retroversion than has been reported previously and can result in varus and extension deformation of the humerus. These findings suggest that humeral deformity in overhead throwing athletes may not always solely reflect adaptation to throwing.
AARON C. BELL,TAKASHI ONAKA,YASUO DOI,ITSUKI SAKON,Fumihiko Usui,DAISUKE ISHIHARA,HIDEHIRO KANEDA,MARTIN GIARD,RONIN WU,RYOU OHSAWA,TAMAMI MORI-ITO,MARK HAMMONDS,이호규,Itsuki Sakon 한국천문학회 2017 天文學論叢 Vol.32 No.1
Our understanding of dust emission, interaction, and evolution, is evolving. In recent years, electric dipole emission by spinning dust has been suggested to explain the anomalous microwave excess (AME), appearing between 10 and 90 Ghz. The observed frequencies suggest that spinning grains should be on the order of 10nm in size, hinting at polycyclic aromatic hydrocarbon molecules (PAHs). We present data from the AKARI/Infrared Camera (IRC) due to its high sensitivity to the PAH bands. By inspecting the IRC data for a few AME regions, we find a preliminary indication that regions well-fitted by a spinning-dust model have a higher 9~$\mu$m than 18~$\mu$m intensity vs. non-spinning-dust regions. Ongoing efforts to improve the analysis by using DustEM and including data from the AKARI Far Infrared Surveyor (FIS), IRAS, and Planck High Frequency Instrument (HFI) are described.
INFRARED OBSERVATIONS OF DUST AROUND HELIUM NOVA V445 PUPPIS
SAYAKA SHIMAMOTO,ITSUKI SAKON,TAKASHI ONAKA,Fumihiko Usui,TAKAFUMI OOTSUBO,YASUO DOI,RYOU OHSAWA,DAISUKE ISHIHARA 한국천문학회 2017 天文學論叢 Vol.32 No.1
We detected bright mid- to far-infrared emission from the helium nova V445 Puppis in the AKARI all-sky survey data taken in 2006. Assuming an optically thin condition, we decomposed the spectral energy distribution (SED) of V445 Puppis in October 2006 by model fitting and found that the SED can be explained by a combination of cold amorphous carbon (125~K and the mass of $4.5^{+6.6}_{-2.7}\times 10^{-4} ~{\rm M}_{\odot}$) and warm amorphous carbon (250~K and the mass of $1.8^{+1.0}_{-0.5}\times 10^{-5} ~{\rm M}_{\odot}$). Assuming that the former is pre-existing dust formed in the past nova outbursts and the latter is newly formed dust in December 2000's nova wind, this result suggests that the amount of dust formed around V445 Puppis in a single outburst is larger than $10^{-5} ~{\rm M}_{\odot}$, which is larger than those in any other classical novae ever reported.