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Preparatory works for the calibration of SPICA Mid-infrared Instrument (SMI) are reported. We focus on three calibration items, flux, wavelength, and geometrical distortion, and discuss requirements, strategies, and candidates of celestial objects to be used for the calibration. Information of previous and ongoing space infrared astronomical missions is compiled as a reference. We confirm that the standard stars for the flux calibration used in other missions are also applicable for SMI. We investigate objects for wavelength calibration, and conclude that both planetary nebulae and Be stars are needed. In addition, we discuss possible use of molecular lines in red-giant stars for the high-resolution mode. Globular clusters are only the objects that provide a sufficient number of position references for the correction of the geometrical distortion, but further investigation is needed to establish the correction method. The total amount of the observing time for the calibration of SPICA/SMI well fits the allocation plan of the observing time. Information and consideration made so far shall also be useful for future space infrared astronomical missions., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA2130034000, レポート番号: JAXA-RR-21-007E

本ドキュメントは、2006年2月22日に打ち上げられ、全天サーベイおよび、多数の指向観測を実施し、2011年11月24日にすべての運用を終了した赤外線天文衛星「あかり」のアーカイブデータ(高次処理データ: カタログ、イメージ、スペクトル)を天文学の研究者に紹介することを目的としています。, This document aims to introduce the archival data (mainly highly processed data such as catalogue, images, and spectra) taken by the AKARI infrared astronomy satellite, primarily for professional astronomers who are not necessarily familiar with AKARI. AKARI was launched on February 22, 2006, carried out numerous pointing observations as well as all sky surveys, and completed all the operations on November 24, 2011., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1930007000, レポート番号: JAXA-RM-19-003

本ドキュメントは、2006年2月22日に打ち上げられ、全天サーベイおよび、多数の指向観測を実施し、2011年11月24日にすべての運用を終了した赤外線天文衛星「あかり」のアーカイブデータ(高次処理データ: カタログ、イメージ、スペクトル)を天文学の研究者に紹介することを目的としています。, This document aims to introduce the archival data (mainly highly processed data such as catalogue, images, and spectra) taken by the AKARI infrared astronomy satellite, primarily for professional astronomers who are not necessarily familiar with AKARI. AKARI was launched on February 22, 2006, carried out numerous pointing observations as well as all sky surveys, and completed all the operations on November 24, 2011., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1930008000, レポート番号: JAXA-RM-19-004E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1830021000, レポート番号: JAXA-SP-18-006E

本ドキュメントは, 2006年2月22日に打ち上げられ, 全天サーベイおよび, 多数の指向観測を実施し, 2011年11月24日にすべての運用を終了した赤外線天文衛星「あかり」のアーカイブデータ（高次処理データ: カタログ, イメージ, スペクトル）を天文学の研究者に紹介することを目的としています., This document aims to introduce the archival data (mainly highly processed data such as catalogue, images, and spectra) taken by the AKARI infrared astronomy satellite, primarily for professional astronomers who are not necessarily familiar with AKARI. AKARI was launched on February 22, 2006, carried out numerous pointing observations as well as all sky surveys, and completed all the operations on November 24, 2011., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1830017000, レポート番号: JAXA-RM-18-009E

本ドキュメントは, 2006年2月22日に打ち上げられ, 全天サーベイおよび, 多数の指向観測を実施し, 2011年11月24日にすべての運用を終了した赤外線天文衛星「あかり」のアーカイブデータ（高次処理データ: カタログ, イメージ, スペクトル）を天文学の研究者に紹介することを目的としています., This document aims to introduce the archival data (mainly highly processed data such as catalogue, images, and spectra) taken by the AKARI infrared astronomy satellite, primarily for professional astronomers who are not necessarily familiar with AKARI. AKARI was launched on February 22, 2006, carried out numerous pointing observations as well as all sky surveys, and completed all the operations on November 24, 2011., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1830016000, レポート番号: JAXA-RM-18-007

第21回宇宙科学シンポジウム (2021年1月6日-7日. オンライン開催), 21st Space Science Symposium (January 6-7, 2021. Online Meeting), 資料番号: SA6000163019, レポート番号: S5-001

第20回宇宙科学シンポジウム (2020年1月8日-9日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 20th Space Science Symposium (January 8-9, 2020. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000152016, レポート番号: S4-007

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027000, レポート番号: JAXA-SP-17-010E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We overview the AKARI mission and current status of the data processing and archiving activity. AKARI was launched in February 2006, and started observation from May 2006. Operation under cryogenic temperature lasted until August 2007 (Phase 1 and 2), where the All-Sky Survey in six wavelength bands in the mid- and far-infrared as well as over 5000 pointed observations were carried out. Another 12,000 observations using the near-infrared channel of the IRC were made in the warm phase (Phase 3) from June 2008 to February 2010. The AKARI satellite was switched-off in November 2011. Since April 2013, AKARI data processing and analysis team has been working in collaboration with universities to process as much as AKARI data to 'science ready' state and archive them for future scientific analysis. New data products since the last AKARI conference are briefly explained., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026001, レポート番号: JAXA-SP-17-009E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, AKARI is the first Japanese satellite mission dedicated to the infrared astronomy. AKARI was launched in February 2006 and carried out an all-sky survey as well as twenty thousands of pointed observations from near- to far-IR wavelengths over four-years mission. AKARI operation was terminated in November, 2011. The All-Sky far- and mid-IR Point Source Catalogues, Asteroid catalogue, as well as point source catalogues from the Large Magellanic Cloud and the North Ecliptic Pole region have been published. Science targets of AKARI range from the solar system objects to cosmology. Science highlights from the AKARI data are briefly summarized. The AKARI project has been reconfigured in April 2013 to focus on data reduction and archiving. Revision of far-IR All-Sky Survey point source catalogue, mid- and far-IR faint source catalogues, All-Sky image maps are planned to be produced. Imaging and spectroscopic data taken in the pointed observation mode will also be archived as ''science-ready'' data products AKARI data and our experience through the mission are a legacy to promote the SPICA mission., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027094, レポート番号: JAXA-SP-17-010E

形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026000, レポート番号: JAXA-SP-17-009E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We introduce a general-purpose surface brightness correction method for compact extended sources imaged in the slow-scan pointed-observation mode of the Far-Infrared Surveyor (FIS) aboard the AKARI infrared astronomical satellite. Our method recovers correct surface brightness maps by rescaling archived raw FIS maps using the surface-brightness-dependent inverse FIS response function. The flux of a target source is then automatically corrected for as the simple sum of surface brightnesses within the adopted target perimeter (i.e., standard contour photometry). This correction method is contrasted with the previous aperture photometry method for point sources, which directly corrects for the target flux with a flux-dependent scaling law. The new surface brightness correction method is applicable to objects of any shape from unresolved point sources to resolved extended objects, as long as the target is not deemed diffuse, i.e., the total extent of the target source does not exceed much more than a single FIS scan width of about 10 min. The new correction method takes advantage of the well-defined shape (i.e., the scale-invariance) of the point spread function, which enables us to adopt a power-law FIS response function. We analyze the point source photometric calibrator data using the FIS AKARI Slow-Scan Tool and constrain the parameters of the adopted power-law FIS response function. We conclude that the photometric accuracy of the new correction method is better than 10% error based on comparisons with the expected fluxes of the photometric calibrators, and that resulting fluxes without the present correction method can lead to differences more than a factor of two., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026053, レポート番号: JAXA-SP-17-009E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, Two far-infrared point source catalogues from the AKARI All-Sky Survey are presented. The FIS Bright Source Catalogue ver.2 was released in April 2016 and publically available from the ISAS archive. It is the revised version of the initial release in March 2010, and have improvements in number of detections, completeness and reliability, and accuracy. The FIS Faint Source Catalogue is under evaluation and will be available in public soon. The catalogue contains fainter sources in the high-visibility region (high ecliptic-latitude regions). Two catalogues are expected to be used widely in future astronomical researches as standard data., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026038, レポート番号: JAXA-SP-17-009E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We present details of a point source catalogue using all the reference images for spectroscopic observations of AKARI/IRC-S9W (Yamagishi et al. in this volume). The catalogue includes about 42,000 sources, for which we performed PSF fitting with two-dimensional Gaussian and cross-identifications with 2MASS and WISE PSCs. About 80% of the sources in the catalogue are found in the other PSCs. Thanks to the deeper sensitivity and higher spatial resolution than WISE, we find 8400 sources and provide 9 micrometers flux for 8500 objects not detected in WISE W3. The procedure of this work can be applied to all the pointed imaging data of IRC, which shall detect a few tens thousands MIR sources and be helpful to understand the SED of many objects such as YSO., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026044, レポート番号: JAXA-SP-17-009E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We compare the all-sky AKARI/Far-Infrared Surveyor (FIS) Bright Source Catalogue (BSC) Version 2 with the Herschel/ Photodetector Array Camera and Spectrometer (PACS) Point Source Catalogue (PSC), in order to investigate condition for correct matching. We define a ''fake''-match rate based on the AKARI-Herschel flux ratio and study the dependence of this rate on the source density of the region (Ndens), AKARI-Herschel separation (D), Galactic latitude (absolute value of b), and the AKARI flux. We find that the 'fake'-match rate depends on Ndens, D, and absolute value of b and not strongly on the AKARI flux where the sources with smaller Ndens and D and larger absolute value of b result in lower ''fake''-match rate. In our analysis, if we limit the AKARI sources with FQUAL= 3, Ndens = 0 and absolute value of b greater than 30 degrees, and adopt a searching radius of less than 10 arcsec, the source is likely to be matched with an appropriate counterpart in a catalogue of astronomical data whose position accuracy is better than that of the AKARI catalogue., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026039, レポート番号: JAXA-SP-17-009E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We present the current status of the AKARI slitless spectroscopic catalogue, which is produced as a part of the AKARI data archive activities. AKARI has capability of slitless spectroscopy in the NIR and MIR wavelengths for a 10' × 10' area. The data reduction is, however, very difficult due to a confusion of nearby sources after dispersion. In order to solve the problem, we first make a point source list in each FOV from the reference image, and evaluate overlaps between the spectra based on their positions and fluxes. As a trial, we applied the procedure to the Phase 2 MIR-S data (5-3 micrometers). As a result of processing all reference images of 884 spectroscopic observations, 42,000 point sources (at lambda = 9 micrometers) are extracted with a detection limit of 0.3 mJy. Based on the source list, we identified the non-overlapped sources and extracted their spectra. We obtained MIR spectra of 880 objects including main sequence stars, AGB stars, galaxies, and AGNs. The dataset is valuable as an unbiased spectral sample in the MIR. The point source and spectroscopic catalogues will be publicly released in the near future., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026002, レポート番号: JAXA-SP-17-009E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, We present the preliminary results of the flux calibration for extended sources observed with the Far-Infrared Surveyor (FIS) onboard the AKARI satellite. The circumstellar shells of evolved stars (particularly of AGB and post-AGB stars) retain the fossil record of their mass loss in the form of dust/gas density distributions and these shells have the potential to verify/constrain many theoretical aspects of stellar evolution and mass loss. Hence, it is critical to have an accurate surface brightness and flux calibration. The FIS has four photometric bands between 50-180 μm with two types of Ge:Ga array detectors. The Ge:Ga array is long known to have a slow transient response and FIS has already been characterized for point sources. To calibrate for extended sources, we used a method in which photometry is done in a contour aperture of the 3σ detection threshold above the background to encompass more than the PSF core. We show that the revised slow transient corrections for the short wavelength band have a similar functional form as for the point source corrections, whereas for the long wavelength band two distinct functional forms dependent on the source brightness., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027055, レポート番号: JAXA-SP-17-010E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We present the relation between stellar mass and star formation rate (SFR) of a sample of infrared (IR)-bright dust-obscured galaxies (DOGs) that are defined by (i - brackets 22 brackets)(sub AB) greater than 7.0 and flux density at 22 micrometers greater than 3.8 mJy. Combining the Sloan Digital Sky Survey (SDSS), TwoMicron All Sky Survey (TWOMASS), Wide-field Infrared Survey Explorer (WISE), Infrared Astronomical Satellite (IRAS), and AKARI catalogs, we selected 7 IR-bright DOG at Z(sub spec) is greater than 0 and less than 1. We estimated their stellar mass and SFR based on a spectral energy distribution fitting technique, and compared them with main sequence of star-forming galaxies at z is greater than 0 and less than 2 and local ULIRGs. As a result, we found that most of IR-bright DOGs lie significantly above the main sequence of star-forming galaxies at similar redshifts. We conclude that the majority of IRAS- and/or AKARI-detected IR-bright DOGs are starburst galaxies., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026029, レポート番号: JAXA-SP-17-009E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, AKARI carried out an all-sky survey with two onboard instruments; the Infrared Camera (IRC) and the Far-Infrared Surveyor (FIS). The first version of the catalogues, the FIS Bright Source Catalogue (FIS-BSC) and the IRC Point Source Catalogue (IRC-PSC) were released publicly in March 2010. The AKARI All-Sky catalogues are superior to the previous all-sky infrared catalogues by IRAS significantly in spatial resolution, sensitivity, and wavelength coverage. We present the specifications of the AKARI catalogues and their characteristics by comparing with other infrared source catalogues. We continue efforts to improve the AKARI catalogues in reliability and completeness as well as accuracy of flux and position measurements. FIS Faint Source Catalogue, which provides fainter sources than the BSC at the high-visibility regions, is also planned to be produced. We report the current status of improvement works and prospects for the future., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027095, レポート番号: JAXA-SP-17-010E

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, Here we briefly overview the latest data reduction toolkit and reduced images with it that are already available online. AKARI performed approximately 4000 pointed observations over 16 months in Phases 1 and 2, when the telescope and instruments were cooled by liquid helium. Observation targets include solar system objects, Galactic objects, local galaxies, and galaxies at cosmological distances. We describe major updates on calibration processes of near- and mid-infrared images taken by the InfraRed Camera, which has nine photometric filters covering 2-27 micrometers continuously. The latest toolkit has been applied to data from each pointed observation to generate calibrated and stacked images. About 90% of the stacked images have a position accuracy better than 1.5 arcsec. Uncertainties in aperture photometry estimated from a typical standard sky deviation of stacked images are a factor of approximately 2-4 smaller than those of AllWISE at similar wavelengths. This work has already been published as Egusa et al. (2016)., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026042, レポート番号: JAXA-SP-17-009E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, Results of infrared photometries and dust shell modeling of a peculiar object WISE J180956.27-330500.2 are presented. The object has shown a significant time variation of its SED in the last 30 years. The variation is understood as a formation and expansion of massive dust shell since late 1990’s. The object was suspected to be a red star in the optical wavelengths before the mass ejection, which allows us to hypothesize that the object is possibly the first example of the AGB star just experiencing an episodic mass loss after a thermal pulse. Observation of this object with SPICA after some 10 years from now will bring us an important clue to understand the stellar evolution and mass loss, as well as the chemistry in the thick circumstellar envelopes., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027058, レポート番号: JAXA-SP-17-010E

第19回宇宙科学シンポジウム (2019年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 19th Space Science Symposium (January 9-10, 2019. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000144188, レポート番号: P-153

第19回宇宙科学シンポジウム (2019年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 19th Space Science Symposium (January 9-10, 2019. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000144043, レポート番号: P-008

第19回宇宙科学シンポジウム (2019年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 19th Space Science Symposium (January 9-10, 2019. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000144047, レポート番号: P-012

We performed a far-IR imaging survey of the circumstellar dust shells of 144 evolved stars as a mission programme of the AKARI infrared astronomical satellite using the Far-Infrared Surveyor (FIS) instrument. With this survey, we deliver far-IR surface brightness distributions of roughly 10' x 40' or 10' x 20' areas of the sky around the target evolved stars in the four FIS bands at 65, 90, 140, and 160 microns. Our objectives are to characterize the far-IR surface brightness distributions of the cold dust component in the circumstellar dust shells, from which we derive the amount of cold dust grains as low as 20 K and empirically establish the history of the early mass loss history. In this first installment of the series, we introduce the project and its aims, describe the observations, data reduction, and surface brightness correction process, and present the entire data set along with the results of integrated photometry measurements (i.e., the central source and circumstellar dust shell altogether). We find that (1) far-IR emission is detected from all but one object at the spatial resolution about 30" - 50" in the corresponding bands, (2) roughly 60 - 70 % of the target sources show some extension, (3) previously unresolved nearby objects in the far-IR are now resolved around 28 target sources, (4) the results of photometry measurements are reasonable with respect to the entries in the AKARI/FIS Bright Source Catalogue, despite the fact that the targets are assumed to be point-sources when catalogue flux densities were computed, and (5) an IR two-color diagram would place the target sources in a roughly linear distribution that may correlate with the age of the circumstellar dust shell and can potentially be used to identify which targets are more extended than others., To be published in PASJ AKARI Special Issue: 25 pages, 5 figures, 5 tables (and 28 supplementary figures available only in PASJ on-line)

Our understanding of protoplanetary disks has greatly improved over the last decade due to a wealth of data from new facilities. Unbiased dust surveys with Spitzer leave us with good constraints on the dust dispersal timescale of small grains in the terrestrial planet forming region. In the ALMA era, this can be confronted for the first time also with evolutionary timescales of mm grains in the outer disk. Gas surveys in the context of the existing multi-wavelength dust surveys will be a key in large statistical studies of disk gas evolution. Unbiased gas surveys are limited to ALMA CO submm surveys, where the quantitative interpretation is still debated. Herschel gas surveys have been largely biased, but brackets O I brackets 63 micrometers surveys and also accretion tracers agree qualitatively with the evolutionary timescale of small grains in the inner disk. Recent advances achieved by means of consistent multi-wavelength studies of gas AND dust in planet forming disks reveal the subtleties of the quantitative interpretation of gas surveys. Observational methods to determine disk masses e.g., from CO submm lines require the knowledge of the dust properties in the disk. Understanding not only the gas evolution, but also its chemical composition will provide crucial input for planet formation models. Kinetic chemical results give profoundly different answers than thermodynamic equilibrium in terms of the C/O ratios as well as the water ice/rock ratios. Again, dust has a key impact on the chemical evolution and composition of the gas. Grain growth for example affects freeze-out processes and strongly increases the cosmic ray induced UV field.

第18回宇宙科学シンポジウム (2018年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 18th Space Science Symposium (January 9-10, 2018. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000118061, レポート番号: P-027

著者人数: 20名, Accepted: 2016-12-10, 資料番号: SA1160343000

第17回宇宙科学シンポジウム (2017年1月5日-6日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 17th Space Science Symposium (January 5-6, 2017. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 11名, 資料番号: SA6000060138, レポート番号: P-096

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, Ultra- and Hyper-luminous IR galaxies (L(sub IR) greater than 10(exp 12) solar luminosity for ULIRGs and L(sub IR) greater than 10(exp 13) solar luminosity for HyLIRGs) are populations of galaxies with strong IR dust emission, which is associated with a powerful AGN activity. Currently, identifications of ULIRGs and HyLIRGs are dominated by broad-line QSOs, but existence of FIR with an extremely faint optical counterpart suggests that there are significant number of obscured QSOs among the FIR sources. Utilizing the unique sample of bright FIR sources in a wide survey field from AKARI FIS Bright Source Catalogue, we look for luminous type-2 QSOs at z in the order of 0.5-1 by identifying FIR sources with extremely large FIR to optical flux ratio. In order to reveal the nature of the optically-faint FIR sources and to kick-off a systematic search for type-2 QSOs at intermediate redshifts, we observed 8 AKARI 90 micrometers FIR sources with a faint optical counterpart (i greater than 20 mag) using FOCAS on the Subaru telescope. They are identified with emission line galaxies at z = 0.3-0.6. Through optical-MIR-FIR SED fitting, their integrated IR luminosity are estimated to be 10(exp 12-12.5) solar luminosity. The identification of these ULIRGs at intermediate redshifts confirms the effectiveness of our selection method. One of these objects shows broad brackets O III brackets 5007 angstroms (FWHM of 2200 km s(exp -1) with blue shift of 2300 km s(exp -1)) and brackets O II brackets 3726 angstroms emission lines (FWHM of 1100 km s(exp -1)). The co-existence of extreme outflow and high SFR (in the order of 1000 solar mass yr(exp -1)) suggest the galaxy evolves into its most active stage when both of the AGN and star formation activities reach the peak period., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026068, レポート番号: JAXA-SP-17-009E

著者人数: 21名, Accepted: 2012-07-09, 資料番号: SA1004295000

平成27年度宇宙科学情報解析シンポジウム（2016年2月12日. 宇宙航空研究開発機構宇宙科学研究所（JAXA)(ISAS)）, 相模原市, 神奈川県, Space Science Informatics Symposium FY2015 (February 12, 2016. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000093016

We present a general surface brightness correction method for compact extended sources imaged in the slow-scan pointed observation mode of the Far-Infrared Surveyor (FIS) aboard the AKARI Infrared Astronomical Satellite. Our method recovers correct surface brightness distribution maps by re-scaling archived raw FIS maps using the surface-brightness-dependent inverse FIS response function. The flux of a target source is then automatically corrected for as the simple sum of surface brightnesses within the adopted contour encircling the perimeter of the target (i.e., contour photometry). This correction method is contrasted to the previous aperture photometry method for point sources, which directly corrects for the target flux with a flux-dependent scaling law. The new surface brightness correction scheme is applicable to objects of any shape from unresolved point sources to resolved extended objects, as long as the target is not deemed diffuse, i.e., the total extent of the target source does not exceed too much more than a single FIS scan width of 10 arcmin. The new correction method takes advantage of the well-defined shape (i.e., the scale invariance) of the point-spread function, which enables us to adopt a power-law FIS response function. We analyze the point-source photometric calibrator data using the FIS AKARI Slow-scan Tool (FAST) and constrained the parameters of the adopted power-law FIS response function. We conclude that the photometric accuracy of the new correction method is better than 10% error based on comparisons with the expected fluxes of the photometric calibrators and that resulting fluxes without the present correction method can lead up to 230% overestimates or down to 50% underestimates., Comment: accepted for publication in PASJ

第16回宇宙科学シンポジウム (2016年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 16th Space Science Symposium (January 6-7, 2016. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 35名, 資料番号: SA6000046078, レポート番号: P-079

第16回宇宙科学シンポジウム (2016年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 16th Space Science Symposium (January 6-7, 2016. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000046002, レポート番号: P-002

第16回宇宙科学シンポジウム (2016年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 16th Space Science Symposium (January 6-7, 2016. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 16名, 資料番号: SA6000046220, レポート番号: P-221

第16回宇宙科学シンポジウム (2016年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 16th Space Science Symposium (January 6-7, 2016. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000046003, レポート番号: P-003

Accepted: 2012-08-04, 資料番号: SA1004472000

第15回宇宙科学シンポジウム (2015年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 15th Space Science Symposium (January 6-7, 2015. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 16名, 資料番号: SA6000034306, レポート番号: P-307

第15回宇宙科学シンポジウム (2015年1月6日-7日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 15th Space Science Symposium (January 6-7, 2015. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 11名, 資料番号: SA6000034084, レポート番号: P-084

平成18年度宇宙科学情報解析センターシンポジウム（2006年11月28日. 宇宙航空研究開発機構宇宙科学研究本部(JAXA)(ISAS)）, 相模原市, 神奈川県, 2006 PLAIN Center Symposium (Space Science Informatics Symposium FY2006) (November 28, 2006. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000108010

We present ESO/VLT spectra in the 2.9--4.1 micron range for a large sample of infrared stars in the Large Magellanic Cloud (LMC), selected on the basis of MSX and 2MASS colours to be extremely dust-enshrouded AGB star candidates. Out of 30 targets, 28 are positively identified as carbon stars, significantly adding to the known population of optically invisible carbon stars in the LMC. We also present spectra for six IR-bright stars in or near three clusters in the LMC, identifying four of them as carbon stars and two as oxygen-rich supergiants. We analyse the molecular bands of C2H2 at 3.1 and 3.8 micron, HCN at 3.57 micron, and sharp absorption features in the 3.70--3.78 micron region that we attribute to C2H2. There is evidence for a generally high abundance of C2H2 in LMC carbon stars, suggestive of high carbon-to-oxygen abundance ratios at the low metallicity in the LMC. The low initial metallicity is also likely to have resulted in less abundant HCN and CS. The sample of IR carbon stars exhibits a range in C2H2:HCN abundance ratio. We do not find strong correlations between the properties of the molecular atmosphere and circumstellar dust envelope, but the observed differences in the strengths and shapes of the absorption bands can be explained by differences in excitation temperature. High mass-loss rates and strong pulsation would then be seen to be associated with a large scale height of the molecular atmosphere., Comment: Accepted for publication in Astronomy and Astrophysics. 20 pages. Figure 11 is degraded for posting on astro-ph

The dependence of stellar molecular bands on the metallicity is studied using infrared L-band spectra of AGB stars (both carbon-rich and oxygen-rich) and M-type supergiants in the Large and Small Magellanic Clouds (LMC and SMC) and in the Sagittarius Dwarf Spheroidal Galaxy. The spectra cover SiO bands for oxygen-rich stars, and acetylene (C2H2), CH and HCN bands for carbon-rich AGB stars. The equivalent width of acetylene is found to be high even at low metallicity. The high C2H2 abundance can be explained with a high carbon-to-oxygen (C/O) ratio for lower metallicity carbon stars. In contrast, the HCN equivalent width is low: fewer than half of the extra-galactic carbon stars show the 3.5micron HCN band, and only a few LMC stars show high HCN equivalent width. HCN abundances are limited by both nitrogen and carbon elemental abundances. The amount of synthesized nitrogen depends on the initial mass, and stars with high luminosity (i.e. high initial mass) could have a high HCN abundance. CH bands are found in both the extra-galactic and Galactic carbon stars. None of the oxygen-rich LMC stars show SiO bands, except one possible detection in a low quality spectrum. The limits on the equivalent widths of the SiO bands are below the expectation of up to 30angstrom for LMC metallicity. Several possible explanations are discussed. The observations imply that LMC and SMC carbon stars could reach mass-loss rates as high as their Galactic counterparts, because there are more carbon atoms available and more carbonaceous dust can be formed. On the other hand, the lack of SiO suggests less dust and lower mass-loss rates in low-metallicity oxygen-rich stars. The effect on the ISM dust enrichment is discussed., accepted for A&A

Accepted: 2004-03-10, 資料番号: SA1003382000

Accepted: 2003-03-11, 資料番号: SA1003351000

太陽などの恒星の進化の終末期は、星からの質量放出によって大きく影響される。一方、進化末期の星は、質量放出を通じて星間空間に新しく合成された元素を供給し、銀河や宇宙の進化に貢献する。これら質量放出星は赤外線で非常に明るく、赤外線天文学が始まって以来の対象である。SPICAはこのような天体についても、これまでとは質的に異なる情報をもたらし、研究を大きく進める可能性を持つ。SPICAに期待される進化末期天体の観測と、それによって得られるであろう成果について議論する。, 資料番号: AA0045441045

資料番号: AA0045916013

Accepted: 2002-04-11, 資料番号: SA1003888000

Accepted: 2002-10-21, 資料番号: SA1003886000