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PROCESSING OF INTERSTELLAR MEDIUM AS DIVULGED BY AKARI
TAKASHI ONAKA,TAMAMI I. MORI,RYOU OHSAWA,ITSUKI SAKON,AARON C. BELL,MARK HAMMONDS,TAKASHI SHIMONISHI,DAISUKE ISHIHARA,HIDEHIRO KANEDA,YOKO OKADA,MASAHIRO TANAKA 한국천문학회 2017 天文學論叢 Vol.32 No.1
A wide spectral coverage from near-infrared (NIR) to far-infrared (FIR) of {\it AKARI} both for imaging and spectroscopy enablesus to efficiently study the emission from gas and dust in the interstellar medium (ISM). In particular, the Infrared Camera(IRC) onboard {\it AKARI}offers a unique opportunity to carry out sensitive spectroscopy in the NIR (2--5\,$\mu$m) for the first time from a spaceborn telescope. This spectral range contains a number of important dust bands and gas lines, such as the aromatic and aliphatic emissionbands at 3.3 and 3.4--3.5\,$\mu$m, H$_2$O and CO$_2$ ices at 3.0 and 4.3\,$\mu$m, CO, H$_2$, and \ion{H}{I} gas emission lines. In this paper we concentrate on the aromatic and aliphatic emission and ice absorption features. The balance between dust supply and destruction suggests significant dust processing takingplace as well as dust formation in the ISM. Detailed analysis of the aromatic and aliphatic bands of {\it AKARI} observations for a number of\ion{H}{ii} regions and \ion{H}{ii} region-like objectssuggests processing of carbonaceous dust in the ISM. The ice formation process canalso be studied with IRC NIR spectroscopy efficiently. In this review, dust processing in the ISM divulged by recentanalysis of {\it AKARI} data is discussed.
ICE ABSORPTION FEATURES IN NIR SPECTRA OF GALACTIC OBJECTS
TAMAMI I. MORI,TAKASHI ONAKA,ITSUKI SAKON,RYOU OHSAWA,HIDEHIRO KANEDA,MITSUYOSHI YAMAGISHI,YOKO OKADA,MASAHIRO TANAKA,TAKASHI SHIMONISHI 한국천문학회 2017 天文學論叢 Vol.32 No.1
We present results of AKARI/IRC near-infrared (NIR) slit-spectroscopy (2.5--5.0\,$\mu$m, $R \sim 100$) of Galactic sources,focusing on ice absorption features. We investigate the abundance of H$_2$O and CO$_2$ ices and other ice species (CO and XCN ices)along lines of sight towards Galactic \ion{H}{ii} regions, massive YSOs, and infrared diffuse sources. Even among those different kinds of astronomical objects,the abundance ratio of CO$_2$ to H$_2$O ices does not vary significantly,suggesting that the pathway to CO$_2$ ice formation driven by UV irradiation is not effectiveat least among the present targets.
SPECTRAL EVOLUTION OF NOVAE IN THE NEAR-INFRARED BASED ON AKARI OBSERVATIONS
ITSUKI SAKON,TAKASHI ONAKA,Fumihiko Usui,SAYAKA SHIMAMOTO,RYOU OHSAWA,Takehiko Wada,Hideo Matsuhara,AKIRA ARAI 한국천문학회 2017 天文學論叢 Vol.32 No.1
We have carried out the near-infrared spectroscopic observations of recent classical novae (e.g., V2468Cyg, V1280Sco) within a few years from the outburst with AKARI as a part of AKARI Open Time Observing Program for Phase 3-II "Spectral Evolution of Novae in the Near-Infrared based on AKARI Observations (Proposal ID: SENNA)". The homogeneous datasets of near-infrared spectra from 2.5 $\mu$m to 5 $\mu$m with AKARI/IRC collected in this program are useful to infer the physical conditions of the shell formed by the ejected materials, to examine the chemical properties of the ejecta gas, and to examine the properties of dust formed in the nova ejecta.
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.
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.
miniTAO/ANIR Paα SURVEY OF LOCAL LIRGs
Tateuchi, Ken,Motohara, Kentaro,Konishi, Masahiro,Takahashi, Hidenori,Kato, Natsuko,Uchimoto, Yuka K.,Toshikawa, Koji,Ohsawa, Ryou,Kitagawa, Yutaro,Yoshii, Yuzuru,Doi, Mamoru,Kohno, Kotaro,Kawara, Kim The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
ANIR (Atacama Near InfraRed camera) is a near infrared camera for the University of Tokyo Atacama 1m telescope, installed at the summit of Co. Chajnantor (5,640 m altitude) in northern Chile. The high altitude and extremely low water vapor (PWV = 0.5 mm) of the site enable us to perform observation of hydrogen $Pa{\alpha}$ emission line at $1.8751{\mu}m$. Since its first light observation in June 2009, we have been carrying out a $Pa{\alpha}$ narrow-band imaging survey of nearby luminous infrared galaxies (LIRGs), and have obtained $Pa{\alpha}$ for 38 nearby LIRGs listed in AKARI/FIS-PSC at the velocity of recession between 2,800 km/s and 8,100 km/s. LIRGs are affected by a large amount of dust extinction ($A_V$~ 3 mag), produced by their active star formation activities. Because $Pa{\alpha}$ is the strongest hydrogen recombination line in the infrared wavelength ranges, it is a good and direct tracer of dust-enshrouded star forming regions, and enables us to probe the star formation activities in LIRGs. We find that LIRGs have two star-forming modes. The origin of the two modes probably come from differences between merging stage and/or star-forming process.