Modelling of mid-infrared interferometric signature of hot exozodiacal dust emission

Kirchschlager, Florian; Wolf, S.; Brunngräber, Robert; Matter, A.; Krivov, A. V.; Labdon, Aaron

doi:10.1093/mnras/stx2515

Cited by 10 publications

(9 citation statements)

References 26 publications

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“…In particular, the visibility deficits of both circumstellar emission models (disc ring and Gaussian) compared to the pure stellar photosphere are similar. The main difference is the oscillations occurring for the disc model which are caused by the limited extension of the disc ring and which have been noticed also in the studies of Absil et al (2009) and Kirchschlager et al (2018). In summary, we conclude that the disc model is in line with the interferometric data.…”

Section: O D E L L I N G O F D U S T P Ro P E Rt I E Ssupporting

confidence: 74%

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First L band detection of hot exozodiacal dust with VLTI/MATISSE

Kirchschlager

Wolf

Matter

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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For the first time we observed the emission of hot exozodiacal dust in L band. We used the new instrument MATISSE at the Very Large Telescope Interferometer to detect the hot dust around κ Tuc with a significance of 3σ to 6σ at wavelengths between 3.37 and 3.85 μm and a dust-to-star flux ratio of 5 to $7\,\mathrm{\%}$. We modelled the spectral energy distribution based on the new L band data alone and in combination with H band data published previously. In all cases we find 0.58 μm grains of amorphous carbon to fit the κ Tuc observations the best, however, also nanometre or micrometre grains and other carbons or silicates reproduce the observations well. Since the H band data revealed a temporal variability, while our L band data were taken at a different epoch, we combine them in different ways. Depending on the approach, the best fits are obtained for a narrow dust ring at a stellar distance in the 0.1 to 0.29 au range and thus with a temperature between 940 and 1430 K. Within the 1σ uncertainty dust location and temperature are confined to 0.032 − 1.18 au and 600 − 2000 K.

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Section: O D E L L I N G O F D U S T P Ro P E Rt I E Ssupporting

confidence: 74%

“…With a spatial resolution of a few mas and operating in L, M, and N band, MATISSE offers critical capabilities for the study of hot exozodis. In particular, MATISSE will be able to confine the dust properties of hot exozodis (Ertel et al 2018a;Kirchschlager et al 2018).…”

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confidence: 99%

First L band detection of hot exozodiacal dust with VLTI/MATISSE

Kirchschlager

Wolf

Matter

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…In particular, the visibility deficits of both circumstellar emission models (disc ring and Gaussian) compared to the pure stellar photosphere are similar. The main difference are the oscillations occurring for the disc model which are caused by the limited extension of the disc ring and which have been noticed also in the studies of Absil et al (2009) and Kirchschlager et al (2018). In summary, we conclude that the disc model is in line with the interferometric data.…”

Section: Modelling Of Dust Propertiessupporting

confidence: 74%

First L band detection of hot exozodiacal dust with VLTI/MATISSE

Kirchschlager,

Ertel,

Wolf

et al. 2020

Preprint

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For the first time we observed the emission of hot exozodiacal dust in L band. We used the new instrument MATISSE at the Very Large Telescope Interferometer to detect the hot dust around κ Tuc with a significance of 3σ to 6σ at wavelengths between 3.37 and 3.85 µm and a dust-to-star flux ratio of 5 to 7 %. We modelled the spectral energy distribution based on the new L band data alone and in combination with H band data published previously. In all cases we find 0.58 µm grains of amorphous carbon to fit the κ Tuc observations the best, however, also nanometre or micrometre grains and other carbons or silicates reproduce the observations well. Since the H band data revealed a temporal variability, while our L band data were taken at a different epoch, we combine them in different ways. Depending on the approach, the best fits are obtained for a narrow dust ring at a stellar distance in the 0.1 to 0.29 au range and thus with a temperature between 940 and 1430 K. Within the 1σ uncertainty dust location and temperature are confined to 0.032 − 1.18 au and 600 − 2000 K.

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“…It may also allow for the detection of such systems around Sun-like stars. The detailed study of the detected systems with the LBTI (Ertel et al 2018c) and current and future instruments on the Very Large Telescope Interferometer (Ertel et al 2018a;Kirchschlager et al 2018;Defrère et al 2018) may also allow us to determine the origin of the dust in these individual cases and the connection between the HZ dust and hotter dust even closer to the stars, thus helping to understand the origins and dynamics of the various dust species in the HZs of the stars and closer in.…”

Section: A Consistent Picture From the Present And Absent Trendsmentioning

confidence: 99%

The HOSTS Survey for Exozodiacal Dust: Observational Results from the Complete Survey

Ertel

Defrère

Hinz

et al. 2020

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The Large Binocular Telescope Interferometer (LBTI) enables nulling interferometric observations across the N band (8 to 13 µm) to suppress a star's bright light and probe for faint circumstellar emission. We present and statistically analyze the results from the LBTI/HOSTS (Hunt for Observable Signatures of Terrestrial Systems) survey for exozodiacal dust. By comparing our measurements to model predictions based on the Solar zodiacal dust in the N band, we estimate a 1 σ median sensitivity of 23 zodis for early type stars and 48 zodis for Sun-like stars, where 1 zodi is the surface density of habitable zone (HZ) dust in the Solar system. Of the 38 stars observed, 10 show significant excess. A clear correlation of our detections with the presence of cold dust in the systems was found, but none with the stellar spectral type or age. The majority of Sun-like stars have relatively low HZ dust levels (best-fit median: 3 zodis, 1 σ upper limit: 9 zodis, 95% confidence: 27 zodis based on our N band measurements), while ∼20% are significantly more dusty. The Solar system's HZ dust content is consistent with being typical. Our median HZ dust level would not be a major limitation to the direct imaging search for Earth-like exoplanets, but more precise constraints are still required, in particular

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Modelling of mid-infrared interferometric signature of hot exozodiacal dust emission

Cited by 10 publications

References 26 publications

First L band detection of hot exozodiacal dust with VLTI/MATISSE

First L band detection of hot exozodiacal dust with VLTI/MATISSE

First L band detection of hot exozodiacal dust with VLTI/MATISSE

The HOSTS Survey for Exozodiacal Dust: Observational Results from the Complete Survey

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