Observations of DG Tauri with the Keck Interferometer

Colavita, M. M.; Akeson, Rachel; Wizinowich, Peter; Shao, Michael; Acton, Scott T.; Beletic, James W.; Bell, J.; Berlin, Jeffrey C.; Boden, A. F.; Booth, A. J.; Boutell, R.; Chaffee, Frederic H.; Chan, Dwight; Chock, J.; Cohen, Richard W.; Crawford, S.; Creech‐Eakman, M. J.; Eychaner, Glenn; Felizardo, C.; Gathright, J.; Hardy, G.; Henderson, Heike; Herstein, J.; Heß, Michael Reinhard; Hovland, E.; Hrynevych, M.; Johnson, Richard L.; Kelley, J. H.; Kendrick, Rick; Koresko, C.; Kurpis, P.; Mignant, D. Le; Lewis, Hilton; Ligon, E. R.; Lupton, William; McBride, Dennis; Mennesson, Bertrand; Millan-Gabet, R.; Monnier, John D.; Moore, James D.; Nance, Craig E.; Neyman, C.; Niessner, Albert F.; Palmer, Dean L.; Reder, Leonard J.; Rudeen, A.; Saloga, T.; Sargent, Anneila I.; Serabyn, Eugene; Smythe, R.; Stomski, Paul J.; Summers, K.; Swain, Mark R.; Swanson, Paul N.; Thompson, R. R.; Tsubota, K.; Tumminello, A.; Belle, Gerald van; Vasisht, Gautam; Vause, J.; Walker, James M.; Wallace, J. Kent; Wehmeier, Udo J.

doi:10.1086/377704

Cited by 60 publications

(27 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In both cases, the estimates may differ by more than three standard deviations. The additional errors atop the statistical errors determined by the data processing software are 3.3±1.2 % on the square visibilities (mean and dispersion in our 20 surveyed stars), which is in line with the generally accepted value of 5% (Colavita et al 2003). However, the purely systematic term (highly correlated errors) is only 1.8 ± 0.9 %.…”

Section: Resultssupporting

confidence: 87%

“…However, complete removal does not happen. Colavita et al (2003) measured ≈ 5% systematic errors on the calibrated squared visibility amplitudes at the Keck Interferometer by observing binaries of known orbital parameters. More recently, high-precision diameter measurements using sufficiently well resolved stars with CHARA (White et al 2018;Karovicova et al 2018) were shown to significantly differ (several σ and up to 15%) from values previously obtained from under-resolved interferometric observations, leading the authors to conclude that they were plagued with undiagnosed systematics.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Towards reliable uncertainties in IR interferometry: the bootstrap for correlated statistical and systematic errors

Lachaume

Jordán

Brahm

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We propose a method to overcome the usual limitation of current data processing techniques in optical and infrared long-baseline interferometry: most reduction pipelines assume uncorrelated statistical errors and ignore systematics. We use the bootstrap method to sample the multivariate probability density function of the interferometric observables. It allows us to determine the correlations between statistical error terms and their deviation from a Gaussian distribution. In addition, we introduce systematics as an additional, highly correlated error term whose magnitude is chosen to fit the data dispersion.We have applied the method to obtain accurate measurements of stellar diameters for under-resolved stars, i.e. smaller than the angular resolution of the interferometer. We show that taking correlations and systematics has a significant impact on both the diameter estimate and its uncertainty. The robustness of our diameter determination comes at a price: we obtain 4 times larger uncertainties, of a few percent for most stars in our sample.

show abstract

Section: Resultssupporting

confidence: 87%

Section: Introductionmentioning

confidence: 99%

Towards reliable uncertainties in IR interferometry: the bootstrap for correlated statistical and systematic errors

Lachaume

Jordán

Brahm

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The early compendium of sizes showed some puzzling results for T Tauri disks, too. Some T Tauri disk sizes were quite large compared to expectations based on the central star luminosities (e.g., Colavita et al, 2003;Eisner et al, 2005). In some cases, the accretion luminosity of the infalling material is comparable to the star's luminosity and must be included in the total central luminosity.…”

Section: Size-luminosity Diagrammentioning

confidence: 87%

The Inner Regions of Protoplanetary Disks

Dullemond

Monnier

2010

Annu. Rev. Astron. Astrophys.

268

279

View full text Add to dashboard Cite

To understand how planetary systems form in the dusty disks around pre-mainsequence stars a detailed knowledge of the structure and evolution of these disks is required. While this is reasonably well understood for the regions of the disk beyond about 1 AU, the structure of these disks inward of 1 AU remains a puzzle. This is partly because it is very difficult to spatially resolve these regions with current telescopes. But it is also because the physics of this region, where the disk becomes so hot that the dust starts to evaporate, is poorly understood. With infrared interferometry it has become possible in recent years to directly spatially resolve the inner AU of protoplanetary disks, albeit in a somewhat limited way. These observations have partly confirmed current models of these regions, but also posed new questions and puzzles. Moreover, it has turned out that the numerical modeling of these regions is extremely challenging. In this review we give a rough overview of the history and recent developments in this exciting field of astrophysics.

show abstract

“…But the amount and morphology of this 'inner' material bears on how such PMS binary systems interact with and accrete material from their circumbinary reservoir, and motivates study with the highest-resolution techniques available. Here we report on observations of DQ Tau with the Keck Interferometer (KI, Colavita et al 2003). These observations partially resolve the DQ Tau system, and allow us to model the system visual orbit based on the spectroscopic orbit by M1997.…”

Section: Introductionmentioning

confidence: 91%

Interferometric Evidence for Resolved Warm Dust in the Dq Tau System

Boden

Akeson

Sargent

et al. 2009

ApJ

View full text Add to dashboard Cite

We report on near-infrared (IR) interferometric observations of the doublelined pre-main sequence (PMS) binary system DQ Tau. We model these data with a visual orbit for DQ Tau supported by the spectroscopic orbit & analysis of Mathieu et al (1997). Further, DQ Tau exhibits significant near-IR excess; modeling our data requires inclusion of near-IR light from an 'excess' source. Remarkably the excess source is resolved in our data, similar in scale to the binary itself (∼ 0.2 AU at apastron), rather than the larger circumbinary disk (∼ 0.4 AU radius). Our observations support the Mathieu et al (1997) and Carr et al. (2001) inference of significant warm material near the DQ Tau binary.

show abstract

Observations of DG Tauri with the Keck Interferometer

Cited by 60 publications

References 26 publications

Towards reliable uncertainties in IR interferometry: the bootstrap for correlated statistical and systematic errors

Towards reliable uncertainties in IR interferometry: the bootstrap for correlated statistical and systematic errors

The Inner Regions of Protoplanetary Disks

Interferometric Evidence for Resolved Warm Dust in the Dq Tau System

Contact Info

Product

Resources

About