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

Matsuura, M.; Barlow, M. J.; Zijlstra, A. A.; Whitelock, P. A.; Cioni, M. R. L.; Groenewegen, M. A. T.; Volk, Kevin; Kemper, F.; Kodama, Tadayuki; Lagadec, E.; Meixner, Margaret; Sloan, G. C.; Srinivasan, S.

doi:10.1111/j.1365-2966.2009.14743.x

Cited by 205 publications

(290 citation statements)

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“…Carbon stars show a band attributed to SiC at 11.3 μm, in addition to amorphous carbon dust, which has continuous emission without a characteristic feature in the infrared and which dominates dust mass and infrared excess in carbon stars (Groenewegen et al 1995). Carbon stars with a higher mass-loss rate become red, owing to amorphous carbon dust (Matsuura et al 2009). The SiC feature falls in the S 9W-band (see Fig.…”

Section: (S9w -L18w) Vs (J -L18w)mentioning

confidence: 99%

AKARI's infrared view on nearby stars

Ita

Matsuura

Ishihara

et al. 2010

A&A

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Context. The AKARI, a Japanese infrared space mission, has performed an All-Sky Survey in six infrared-bands from 9 to 180 μm with higher spatial resolutions and better sensitivities than IRAS. Aims. We investigate the mid-infrared (9 and 18 μm) point source catalog (PSC) obtained with the infrared camera (IRC) onboard AKARI, in order to understand the infrared nature of the known objects and to identify previously unknown objects. Methods. Color-color diagrams and a color-magnitude diagram were plotted with the AKARI-IRC PSC and other available all-sky survey catalogs. We combined the Hipparcos astrometric catalog and the 2MASS all-sky survey catalog with the AKARI-IRC PSC. We furthermore searched literature and SIMBAD astronomical database for object types, spectral types, and luminosity classes. We identified the locations of representative stars and objects on the color−magnitude and color−color diagram schemes. The properties of unclassified sources can be inferred from their locations on these diagrams. Results. We found that the (B − V) vs. (V − S 9W) color−color diagram is useful for identifying the stars with infrared excess emerged from circumstellar envelopes or disks. Be stars with infrared excess are separated well from other types of stars in this diagram. Whereas (J − L18W) vs. (S 9W − L18W) diagram is a powerful tool for classifying several object types. Carbon-rich asymptotic giant branch (AGB) stars and OH/IR stars form distinct sequences in this color−color diagram. Young stellar objects (YSOs), pre-main sequence (PMS) stars, post-AGB stars, and planetary nebulae (PNe) have the largest mid-infrared color excess and can be identified in the infrared catalog. Finally, we plot the L18W vs. (S 9W − L18W) color−magnitude diagram, using the AKARI data together with Hipparcos parallaxes. This diagram can be used to identify low-mass YSOs and AGB stars. We found that this diagram is comparable to the [24] vs. ([8.0] − [24]) diagram of Large Magellanic Cloud sources using the Spitzer Space Telescope data. Our understanding of Galactic objects will be used to interpret color-magnitude diagram of stellar populations in the nearby galaxies that Spitzer Space Telescope observed. Conclusions. Our study of the AKARI color−color and color−magnitude diagrams will be used to explore properties of unknown objects in the future. In addition, our analysis highlights a future key project to understand stellar evolution with a circumstellar envelope, once the forthcoming astronometrical data with GAIA are available.

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Section: (S9w -L18w) Vs (J -L18w)mentioning

confidence: 99%

AKARI's infrared view on nearby stars

Ita

Matsuura

Ishihara

et al. 2010

A&A

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“…The astronomical evidence for the synthesis of dust in AGBs is brought by the identification of typical dust features in the spectral energy distribution (SED) of AGB stars, including the 9.7 µm and 18 µm features of silicates in oxygen-rich AGBs and the 11.3 µm feature ascribed to silicon carbide grains in carbon stars. Recent surveys with the Herschel space telescope of the Magellanic Clouds have questioned the primacy of AGBs as galactic dust providers at lower metallicity than that of the Milky Way (Matsuura et al 2009;Boyer et al 2012). However, owing to their large number in stellar populations, AGB stars remain important dust producers in the local and high redshift universe.…”

Section: Introductionmentioning

confidence: 99%

Dust formation in the oxygen-rich AGB star IK Tauri

Gobrecht

Cherchneff

Sarangi

et al. 2015

A&A

185

289

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Aims. We model the synthesis of molecules and dust in the inner wind of the oxygen-rich Mira-type star IK Tau by considering the effects of periodic shocks induced by the stellar pulsation on the gas and by following the non-equilibrium chemistry in the shocked gas layers between 1 R and 10 R . We consider a very complete set of molecules and dust clusters, and combine the nucleation phase of dust formation with the condensation of these clusters into dust grains. We also test the impact of increasing the local gas density. Our derived molecular abundances and dust properties are compared to the most recent observational data. Methods. A semi-analytical formalism based on parameterised fluid equations is used to describe the gas density, velocity, and temperature in the inner wind. The chemistry is described by using a chemical kinetic network of reactions and the condensation mechanism is described by a Brownian formalism. A set of stiff, ordinary, coupled differential equations is solved, and molecular abundances, dust cluster abundances, grain size distributions and dust masses are derived. Results. The shocks drive an active non-equilibrium chemistry in the dust formation zone of IK Tau where the collision destruction of CO in the post-shock gas triggers the formation of C-bearing species such as HCN and CS. Most of the modelled molecular abundances agree well with the latest values derived from Herschel data, except for SO 2 and NH 3 , whose formation may not occur in the inner wind. Clusters of alumina, Al 2 O 3 , are produced within 2 R and lead to a population of alumina grains close to the stellar surface. Clusters of silicates (Mg 2 SiO 4 ) form at larger radii (r > 3 R ), where their nucleation is triggered by the formation of HSiO and H 2 SiO. They efficiently condense and reach their final grain size distribution between ∼6 R and 8 R with a major population of medium size grains peaking at ∼200 Å. This two dust-shell configuration agrees with recent interferometric observations. The derived dust-to-gas mass ratio for IK Tau is in the range 1-6 × 10 −3 and agrees with values derived from observations of O-rich Mira-type stars. Conclusions. Our results confirm the importance of periodic shocks in chemically shaping the inner wind of AGB stars and providing gas conditions conducive to the efficient synthesis of molecules and dust by non-equilibrium processes. They indicate that the wind acceleration will possibly develop in the radius range 4-8 R in IK Tau.

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“…For example, Matsuura et al (2009) and Matsuura, Woods & Owen (2013) showed that enrichment of the ISM by AGB stars in the LMC and SMC fails to explain the total dust and PAH abundance in these galaxies. PAH destruction in the ISM is apparently so effective (Micelotta, Jones & Tielens 2010a) that they do not survive the travel from parent stars to H ii complexes where they are observed.…”

Section: Introductionmentioning

confidence: 99%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of SAO RAS are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 /F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 /F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii]λ5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii]λ5007/Hβ and metallicity. In separate metallicity bins, the F 8 /F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low metallicity complexes and negative for high metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatisation, photodestruction, shattering and sputtering of very small grains, the net F 8 /F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.

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

Cited by 205 publications

References 181 publications

AKARI's infrared view on nearby stars

AKARI's infrared view on nearby stars

Dust formation in the oxygen-rich AGB star IK Tauri

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

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