The IRTS (Infrared Telescope in Space) Mission

Murakami, Hiroshi; Freund, Minoru M.; Ganga, K.; Guo, Hao; Hirao, T.; Hiromoto, Norihisa; Kawada, Manabu; Lange, A. E.; Makiuti, S.; Matsuhara, Hideo; Matsumoto, Toshio; Matsuura, Shuji; Murakami, Masahide; Nakagawa, Takao; Narita, Masanao; Noda, Minoru; Okuda, H.; Okumura, Ko; Onaka, Takashi; Roellig, Thomas L.; Sato, S.; Shibai, Hiroshi; Smith, Beverly J.; Tanabé, Toshihiko; Tanaka, M.; Watabe, Toyoki; Yamamura, I.; Yuen, Lunming

doi:10.1093/pasj/48.5.l41

Cited by 75 publications

(26 citation statements)

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“…Thronson et al 1987;Claussen et al 1987;Jura & Kleinmann 1990;Noguchi et al 2004). For example, Le Bertre et al (2003) investigated the spectra of 689 AGB stars acquired in the four radial directions (l = −10 • , 50 • , 130 • , and 170 • ) with the Near-InfraRed Spectrometer (NIRS; Noda et al 1996) on-board the InfraRed Telescope in Space (IRTS; Murakami et al 1996), and found that O-rich AGB stars outnumber C-rich ones in the inner Galaxy (<8 kpc), whereas the situation is the reverse in the outer Galaxy. However, most past studies surveyed limited regions of the solar neighborhood because of their sensitivity constraints.…”

Section: Introductionmentioning

confidence: 99%

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Ishihara

Kaneda

Onaka

et al. 2011

A&A

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Context. The environmental conditions for asympotic giant branch (AGB) stars to reach the carbon-rich (C-rich) phase are important to understand the evolutionary process of AGB stars. The difference between the spatial distributions of C-rich and oxygen-rich (O-rich) AGB stars is essential for the study of the Galactic structure and the chemical evolution of the interstellar medium. Aims. We quantitatively investigate the spatial distributions of C-rich and O-rich AGB stars in our Galaxy. We discuss the difference between them and its origin. Methods. We classify a large number of AGB stars newly detected by the AKARI mid-infrared all-sky survey. In the color-color diagrams, we define their occupation zones based on the locations of known objects. We then obtain the spatial distributions of C-rich and O-rich AGB stars, assuming that they have the same luminosity for a given mass-loss rate. Results. We find that O-rich AGB stars are concentrated toward the Galactic center and that the density decreases with Galactocentric distance, whereas C-rich AGB stars show a relatively uniform distribution within about 8 kpc of Sun. Conclusions. Our result confirms the trends reported in previous studies and extends them to a Galactic scale. We discuss the relations between our result, the Galactic metallicity gradient, and the chemical evolution of the ISM in our Galaxy.

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Section: Introductionmentioning

confidence: 99%

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Ishihara

Kaneda

Onaka

et al. 2011

A&A

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“…These bands, also called Aromatic Infrared Bands (AIBs), have now been observed in many places where interstellar or circumstellar matter is submitted to UV irradiation, in our Galaxy as well as in external galaxies. Many observations were performed by the recent IR space missions, in particular the Infrared Space Observatory (ISO; Kessler et al 1996) and the Infrared Telescope in Space (IRTS; Murakami et al 1996).…”

Section: Introductionmentioning

confidence: 99%

Spectroscopy of polycyclic aromatic hydrocarbons and very small grains in photodissociation regions

Rapacioli¹,

Joblin²,

Boissel

2004

A&A

239

294

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Abstract.We have coupled a singular value decomposition method with a Monte Carlo search algorithm to analyse the midinfrared ISOCAM spectral maps of photodissociation regions (PDRs) in NGC 7023 and ρ Oph-SR3.Three different spectra and their associated spatial distribution were extracted from this analysis. It is shown that they can be associated with polycyclic aromatic hydrocarbons (PAHs) in their cationic and neutral forms and a third population of carbonaceous very small grains (VSGs). The method allows for the first time (i) to separate the contribution of neutral PAHs to the interstellar emission spectrum from that of cationic PAHs; (ii) to show that the 7.8 µm component of the "7.7 µm" broad feature is carried by VSGs, whereas the 7.6 µm component is due to PAHs; and (iii) to give evidence that free-flying PAHs are produced in PDRs by photoevaporation of VSGs. It is proposed that these carbonaceous VSGs are indeed PAH clusters. We derived a minimal size of 400 carbon atoms per cluster and estimated a UV absorption power of the order of 10 −24 W C −1 for their dissociation.

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“…The IRTS has a primary mirror 15 cm in diameter, cooled with liquid helium, and succeeded in the survey observation for about one month until all the helium was consumed (Murakami et al 1996). The FarInfrared Line Mapper (FILM) is one of the focal plane instruments of the IRTS (Shibai et al 1994).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Diffuse far-infrared [$\ion{C}{ii}$] line emission from high Galactic latitude

Makiuti

Shibai

Okuda

et al. 2002

A&A

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• ) of the Galactic plane are systematically larger than those on the northern side (b > 0 • ). We infer from this difference that there is a displacement of the Sun with respect to the center of interstellar medium from which the [C ii] line comes. When an exponential distribution is assumed for the [C ii] emitting gas, it is expected that the Sun is located at the distance of about 17% of the scale height above the center of the gas. This is consistent with the previously reported displacement of the Sun from the Galactic plane.

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The IRTS (Infrared Telescope in Space) Mission

Cited by 75 publications

References 0 publications

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Spectroscopy of polycyclic aromatic hydrocarbons and very small grains in photodissociation regions

Diffuse far-infrared [$\ion{C}{ii}$] line emission from high Galactic latitude

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