Early science with the Large Millimetre Telescope: Deep LMT/AzTEC millimetre observations of ϵ Eridani and its surroundings

Chavez-Dagostino, Miguel; Bertone, E.; Miera, Fernando Cruz-Sáenz de; Marshall, J. P.; Wilson, Grant; Sánchez-Argüelles, David; Hughes, D. H.; Kennedy, Grant M.; Vega, O.; Luz, V. De la; Dent, W. R. F.; Eiroa, C.; Gómez-Ruiz, Arturo I.; Greaves, J. S.; Lizano, Susana; López-Valdivia, Ricardo; Mamajek, Eric E.; Montaña, Alfredo; Olmedo, Manuel; Rodríguez‐Montoya, Iván; Schloerb, F. Peter; Yun, Min S.; Zavala, Jorge A.; Zeballos, M.

doi:10.1093/mnras/stw1363

Cited by 38 publications

(47 citation statements)

References 53 publications

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“…We found that a central ring with a radius of ∼13 au and an outer ring peaked at 64 au with a width of ∼24 au can fit the observed radial profile relatively well (red line in Figure 5). It is reassuring that the peak position of the outer ring is found to be similar to the location found in other studies (∼64 au, Backman et al 2009;MacGregor et al 2015;Chavez-Dagostino et al 2016). However, as in the 35 μm profile analysis, this does not indicate there is only one inner excess region, but only that the inner excess emission region is extended at least to ∼13 au.…”

Section: Excess Emission At 24 M Msupporting

confidence: 88%

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The Inner 25 au Debris Distribution in the ϵ Eri System

Buizer

Rieke

et al. 2017

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Debris disk morphology is wavelength dependent due to the wide range of particle sizes and size-dependent dynamics influenced by various forces. Resolved images of nearby debris disks reveal complex disk structures that are difficult to distinguish from their spectral energy distributions. Therefore, multi-wavelength resolved images of nearby debris systems provide an essential foundation to understand the intricate interplay between collisional, gravitational, and radiative forces that govern debris disk structures. We present the Stratospheric Observatory for Infrared Astronomy (SOFIA) 35 μm resolved disk image of ò Eri, the closest debris disk around a star similar to the early Sun. Combining with the Spitzer resolved image at 24 μm and 15-38 μm excess spectrum, we examine two proposed origins of the inner debris in ò Eri: (1) in situ planetesimal belt(s) and (2) dragged-in grains from the cold outer belt. We find that the presence of in situ dust-producing planetesmial belt(s) is the most likely source of the excess emission in the inner 25 au region. Although a small amount of dragged-in grains from the cold belt could contribute to the excess emission in the inner region, the resolution of the SOFIA data is high enough to rule out the possibility that the entire inner warm excess results from dragged-in grains, but not enough to distinguish one broad inner disk from two narrow belts.

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Section: Excess Emission At 24 M Msupporting

confidence: 88%

“…The large cold ring at 64 au is confirmed in the millimeter (Lestrade & Thilliez 2015;MacGregor et al 2015). From these images, it appears that many of the clumps can be ascribed to chance alignment with background galaxies (Chavez-Dagostino et al 2016).…”

Section: Introductionmentioning

confidence: 70%

The Inner 25 au Debris Distribution in the ϵ Eri System

Buizer

Rieke

et al. 2017

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“…VLA source 6 coincides with Eridani. Finally, VLA source 11 coincides within ∼2 with millimeter source 5 in the list of Chavez-Dagostino et al (2016). the distance of Eridani) and that this comparison rules out the possibility that the radio emission is coming from a position displaced more than 0.2 AU from the star.…”

Section: Field Sources At 10 Ghzsupporting

confidence: 57%

Flat-spectrum Radio Continuum Emission Associated with ϵ Eridani

Rodrı́guez

Lizano²,

Loinard

et al. 2019

ApJ

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We present Very Large Array observations at 33.0 GHz that detect emission coincident with Eridani to within 0. 07 (0.2 AU at the distance of this star), with a positional accuracy of 0. 05. This result strongly supports the suggestion of previous authors that the quiescent centimeter emission comes from the star and not from a proposed giant exoplanet with a semi-major axis of ∼ 1. 0 (3.4 AU). The centimeter emission is remarkably flat and is consistent with optically thin free-free emission. In particular, it can be modeled as a stellar wind with a mass loss rate of the order of 6.6×10 −11 M yr −1 , which is 3,300 times the solar value, exceeding other estimates of this star's wind. However, interpretation of the emission in terms of other thermal mechanisms like coronal free-free and gyroresonance emission cannot be discarded.

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“…Assuming the two sources are physically not related, the chance of both within 4 of the star is 0.06%. The contamination from multiple background point sources is also seen around Eri (Chavez-Dagostino et al 2016). Therefore, it is possible that the sources in HD 95086 are related background galaxies, and the 0.06% probability is then a lower limit.…”

Section: Alignment Of a Background Galaxymentioning

confidence: 99%

ALMA 1.3 mm Map of the HD 95086 System

Su¹,

MacGregor²,

Booth³

et al. 2017

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Planets and minor bodies such as asteroids, Kuiper-belt objects and comets are integral components of a planetary system. Interactions among them leave clues about the formation process of a planetary system. The signature of such interactions is most prominent through observations of its debris disk at millimeter wavelengths where emission is dominated by the population of large grains that stay close to their parent bodies. Here we present ALMA 1.3 mm observations of HD 95086, a young early-type star that hosts a directly imaged giant planet b and a massive debris disk with both asteroid-and Kuiper-belt analogs. The location of the Kuiper-belt analog is resolved for the first time. The system can be depicted as a broad (∆R/R ∼0.84), inclined (30• ±3• ) ring with millimeter emission peaked at 200±6 au from the star. The 1.3 mm disk emission is consistent with a broad disk with sharp boundaries from 106±6 to 320±20 au with a surface density distribution described by a power law with an index of -0.5±0.2. Our deep ALMA map also reveals a bright source located near the edge of the ring, whose brightness at 1.3 mm and potential spectral energy distribution are consistent with it being a luminous star-forming galaxy at high redshift. We set constraints on the orbital properties of planet b assuming co-planarity with the observed disk.

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Early science with the Large Millimetre Telescope: Deep LMT/AzTEC millimetre observations of ϵ Eridani and its surroundings

Cited by 38 publications

References 53 publications

The Inner 25 au Debris Distribution in the ϵ Eri System

The Inner 25 au Debris Distribution in the ϵ Eri System

Flat-spectrum Radio Continuum Emission Associated with ϵ Eridani

ALMA 1.3 mm Map of the HD 95086 System

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