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Murakami, Wataru; Hosoda, Ikuhiro

doi:10.5190/tga.59.87

Cited by 66 publications

(76 citation statements)

References 1 publication

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“…A similar mass-loss rate versus colour relation has been obtained using [6.4]-[9.3] for carbon-rich AGB stars in the LMC and SMC ). Groenewegen (2006) also provide theoretical relations between mass-loss rates and infrared colours for photometry from Spitzer, Two-Micron All-Sky Survey (2MASS) (Skrutskie et al 2006) and AKARI (Murakami et al 2007;Ita et al 2008).…”

Section: Mass-loss Rates and Coloursmentioning

confidence: 99%

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Matsuura

Barlow

Zijlstra

et al. 2009

Monthly Notices of the Royal Astronomical Society

205

265

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We report on an analysis of the gas and dust budget in the interstellar medium (ISM) of the Large Magellanic Cloud (LMC). Recent observations from the Spitzer Space Telescope enable us to study the mid‐infrared dust excess of asymptotic giant branch (AGB) stars in the LMC. This is the first time we can quantitatively assess the gas and dust input from AGB stars over a complete galaxy, fully based on observations. The integrated mass‐loss rate over all intermediate and high mass‐loss rate carbon‐rich AGB candidates in the LMC is 8.5 × 10−3 M⊙ yr−1, up to 2.1 × 10−2 M⊙ yr−1. This number could be increased up to 2.7 × 10−2 M⊙ yr−1 if oxygen‐rich stars are included. This is overall consistent with theoretical expectations, considering the star formation rate (SFR) when these low‐ and intermediate‐mass stars where formed, and the initial mass functions. AGB stars are one of the most important gas sources in the LMC, with supernovae (SNe), which produces about 2–4 × 10−2 M⊙ yr−1. At the moment, the SFR exceeds the gas feedback from AGB stars and SNe in the LMC, and the current star formation depends on gas already present in the ISM. This suggests that as the gas in the ISM is exhausted, the SFR will eventually decline in the LMC, unless gas is supplied externally. Our estimates suggest ‘a missing dust‐mass problem’ in the LMC, which is similarly found in high‐z galaxies: the accumulated dust mass from AGB stars and possibly SNe over the dust lifetime (400–800 Myr) is significant less than the dust mass in the ISM. Another dust source is required, possibly related to star‐forming regions.

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Section: Mass-loss Rates and Coloursmentioning

confidence: 99%

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Matsuura

Barlow

Zijlstra

et al. 2009

Monthly Notices of the Royal Astronomical Society

205

265

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“…The catalogue contains a full range of information of the NB119-detected galaxies, including photometries in V Ri z J and NB119 bands as well as the phot-z values from Koyama et al (2007). Koyama et al (2008) observed this cluster at 15 μm (L15 filter) with the infrared camera (IRC) onboard the AKARI satellite (Murakami et al 2007;Onaka et al 2007). The FoVs of our MIR observations are shown with dashed line squares in Fig.…”

Section: Photometric Cataloguementioning

confidence: 99%

Panoramic Hα and mid-infrared mapping of star formation in a cluster

Koyama¹,

Kodama²,

Shimasaku³

et al. 2010

Monthly Notices of the Royal Astronomical Society

100

137

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We present the first wide‐field Hα imaging survey around the distant cluster RXJ1716.4+6708 at z= 0.81 with a narrow‐band filter on MOIRCS/Subaru, which reveals the star formation activities down to a star formation rate (SFR) of ∼1 M⊙ yr−1 without extinction correction. Combining with a wide‐field mid‐infrared (MIR) imaging survey with the AKARI satellite, we compare in detail the unobscured and obscured star formation activities in the cluster. We find that both Hα emitters and MIR galaxies avoid the cluster central region and their spatial distribution is quite similar. Most of the Hα emitters show blue colours, but we find some Hα emitters on the red sequence. The MIR galaxies tend to be systematically redder than the Hα emitters probably due to heavy dust extinction. Interestingly, the red Hα emitters and the red MIR galaxies (i.e. dusty red galaxies) are most commonly seen in the medium‐density environment such as cluster outskirts, groups and filaments, where optical colours of galaxies change. We investigate the amount of hidden star formation by calculating a ratio, SFR(IR)/SFR(Hα), and find that AHα exceeds ∼3 in extreme cases for actively star‐forming galaxies with SFR(IR) ≳20 M⊙ yr−1. It is notable that most of such very dusty galaxies with AHα≳ 3 are also located in the medium‐density environment. These findings suggest that dusty star formation is triggered in the infall region of the cluster, implying a probable link between galaxy transition and dusty star formation. We finally calculate the cluster total SFR and find that the cluster total SFR based on Hα alone can be underestimated more than a factor of ∼2 even after 1‐mag extinction correction. We suggest that the mass‐normalized cluster SFR rapidly declines since z∼ 1 following ∝ (1 +z)6, although the uncertainty is still large.

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“…Akari is a space-based telescope operating across the entire IR band, from 2.4 to 160 μm (Murakami et al 2007). The satellite was launched and is operated by the Japan Aerospace Exploration Agency (JAXA).…”

Section: Akari Datamentioning

confidence: 99%

The initial conditions of isolated star formation - IX.Akarimapping of an externally heated pre-stellar core

Nutter

Stamatellos

Ward-Thompson

2009

Monthly Notices of the Royal Astronomical Society

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We present observations of L1155 and L1148 in the Cepheus molecular cloud, taken using the Far Infrared Surveyor (FIS) instrument on the Akari satellite. We compare these data to submillimetre data taken using the Submillimetre Common‐User Bolometer Array (SCUBA) camera on the James Clerk Maxwell Telescope, and far‐infrared data taken with the imaging photo‐polarimeter (ISOPHOT) camera on board the Infrared Space Observatory (ISO) satellite. The Akari data cover a similar spectral window and are consistent with the ISO data. All of the data show a relation between the position of the peak of emission and the wavelength for the core of L1155. We interpret this as a temperature gradient. We fit modified blackbody curves to the spectral energy distributions at two positions in the core and see that the central core in L1155 (L1155C) is approximately 2° warmer at one edge than it is in the centre. We consider a number of possible heating sources and conclude that the A6V star BD+67 1263 is the most likely candidate. This star is at a distance of 0.7 pc from the front of L1155C in the plane of the sky. We carry out radiative transfer modelling of the L1155C core including the effects from the nearby star. We find that we can generate a good fit to the observed data at all wavelengths, and demonstrate that the different morphologies of the core at different wavelengths can be explained by the observed 2° temperature gradient. The L1148 core exhibits a similar morphology to that of L1155C, and the data are also consistent with a temperature gradient across the core. In this case, the most likely heating source is the star BD197053. Our findings illustrate very clearly that the apparent observed morphology of a pre‐stellar core can be highly dependent on the wavelength of the observation, and that temperature gradients must be taken into account before converting images into column density distributions. This is important to note when interpreting Akari and Spitzer data and will also be significant for Herschel data.

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Untitled

Cited by 66 publications

References 1 publication

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Panoramic Hα and mid-infrared mapping of star formation in a cluster

The initial conditions of isolated star formation - IX.Akarimapping of an externally heated pre-stellar core

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