The Dusty AGB Star RS CrB: First Mid-Infrared Interferometric Observations with the Keck Telescopes

Mennesson, Bertrand; Koresko, C.; Creech‐Eakman, M. J.; Serabyn, Eugene; Colavita, M. M.; Akeson, Rachel; Appleby, E.; Bell, J.; Booth, A. J.; Crawford, S.; Dahl, W.; Fanson, James L.; Felizardo, C.; Garcia, J.; Gathright, J.; Herstein, J.; Hovland, E.; Hrynevych, M.; Johansson, Erik M. J.; Mignant, D. Le; Ligon, R.; Millan-Gabet, R.; Moore, James D.; Neyman, C.; Palmer, Dean L.; Panteleeva, T.; Paine, Chris; Ragland, Sam; Reder, Leonard J.; Rudeen, A.; Saloga, T.; Shao, Michael; Smythe, R.; Summers, K.; Swain, Mark R.; Tsubota, K.; Tyau, C.; Vasisht, Gautam; Wizinowich, Peter; Woillez, J.

doi:10.1086/498864

Cited by 5 publications

(3 citation statements)

References 31 publications

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“…The observations were carried out between October 31 st and November 4 th 2004 with the Mid-Infrared Interferometric Instrument (MIDI) at ESO's Very Large Telescope Interferometer (VLTI) on Paranal/Chile. Together with the Keck Interferometer Nuller that recently started to produce first scientific results (Mennesson et al 2005), MIDI is currently worldwide the only instrument able to conduct spectrally resolved interferometric observations in the mid-infrared (Leinert et al 2004). For the observations MIDI was used in high-sens mode using the NaCl prism as dispersive element yielding a spectral resolution of 30.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

FU Orionis: The MIDI VLTI Perspective

Quanz

Henning

Bouwman

et al. 2006

ApJ

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We present the first mid-infrared interferometric measurements of FU Orionis. We clearly resolve structures that are best explained with an optically thick accretion disk. A simple accretion disk model fits the observed SED and visibilities reasonably well and does not require the presence of any additional structure such as a dusty envelope. The inclination and also the position angle of the disk can be constrained from the multibaseline interferometric observations. Our disk model is in general agreement with most published near-infrared interferometric measurements. From the shape and strength of the 8-13 m spectrum, the dust composition of the accretion disk is derived for the first time. We conclude that most dust particles are amorphous and already much larger than those typically observed in the ISM. Although the high accretion rate of the system provides both high temperatures out to large radii and an effective transport mechanism to distribute crystalline grains, we do not see any evidence for crystalline silicates in either the total spectrum or the correlated flux spectra from the inner disk regions. Possible reasons for this nondetection are mentioned. All results are discussed in context with other high spatial resolution observations of FU Ori and other FU Ori objects. We also address the question whether FU Ori is in a younger evolutionary stage than a classical T Tauri star.

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Section: Observations and Data Reductionmentioning

confidence: 99%

FU Orionis: The MIDI VLTI Perspective

Quanz

Henning

Bouwman

et al. 2006

ApJ

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“…The KIN observations allowed a non-ambiguous determination of the dust shell spatial scale and relative flux contribution. Using a simple spherically symmetric model, in which a geometrically thin shell surrounds the stellar photosphere, we found that ~30% to ~70% of the overall mid-infrared flux -depending on the wavelengthoriginated from 7-8 stellar radii (Mennesson et al 2005 4 ). We also found that the shell opacity profile derived from the observations showed a broad peak around 11 µm (τ~=0.06), characteristic of Mg-rich silicate dust particles, and consistent with the observed IRAS spectrum.…”

Section: Evolved Stars With Known Dust: Rs Crb and Tu Taumentioning

confidence: 98%

Keck Interferometer Nuller science highlights

Mennesson¹,

Millan-Gabet

Colavita

et al. 2012

Optical and Infrared Interferometry III

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We report here on some of the major astronomical observations obtained by the Keck Interferometer Nuller (KIN), the high dynamic range instrument recombining the Keck Telescopes at wavelengths of 8 to 13 microns. A few science targets were observed during the commissioning phase (2004)(2005)(2006)(2007). These early observations aimed at demonstrating the KIN's ability to spatially resolve and characterize circumstellar dust emission around a variety of targets, ranging from evolved stars to young debris disks. Science operations started then in 2008 with the more demanding KIN exozodi key science programs, augmented by observations of YSOs and hot debris disks between 2009 and 2011. The last KIN observations were gathered in 2011B, and the interpretation of some of the results depicted here is still preliminary (exo-zodi survey) or pending (complicated behavior observed in YSOs). We discuss in particular the initial results of the KIN's exo-zodi observations, which targeted a total of 40 nearby main sequence single stars. We look for trends in this sample, searching for possible correlations between the measured KIN excesses and basic stellar properties such as spectral type or the presence of dust inferred from separate observations.

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“…Following laboratory development and testing, the addition to KI of the hardware to implement the nuller mode began in earnest in June 2004, and first 10 um measurements were performed later that year. 21 The first null measurements took place in early 2005, with first stabilized nulls in mid 2005. Shared risk observations began in Oct. 2005 in parallel with continued nuller development.…”

Section: Nuller Updatementioning

confidence: 99%

Keck Interferometer nuller update

et al. 2008

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The Keck Interferometer combines the two 10 m Keck telescopes as a long baseline interferometer, funded by NASA, as a joint development among the Jet Propulsion Laboratory, the W. M. Keck Observatory, and the Michelson Science Center. Since 2004, it has offered an Hand K-band fringe visibility mode through the Keck TAC process. Recently this mode has been upgraded with the addition of a grism for higher spectral resolution. The 10 um nulling mode, for which first nulling data were collected in 2005, completed the bulk of its engineering development in 2007. At the end of 2007, three teams were chosen in response to a nuller key science call to perform a survey of nearby stars for exozodiacal dust. This key science observation program began in Feb. 2008. Under NSF funding, Keck Observatory is leading development of ASTRA, a project to add dual-star capability for high sensitivity observations and dual-star astrometry. We review recent activity at the Keck Interferometer, with an emphasis on the nuller development.

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The Dusty AGB Star RS CrB: First Mid-Infrared Interferometric Observations with the Keck Telescopes

Cited by 5 publications

References 31 publications

FU Orionis: The MIDI VLTI Perspective

FU Orionis: The MIDI VLTI Perspective

Keck Interferometer Nuller science highlights

Keck Interferometer nuller update

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