The Third Us Naval Observatory CCD Astrograph Catalog (Ucac3)

Zacharias, N.; Finch, Charlie T.; Girard, T. M.; Hambly, N. C.; Wycoff, G. L.; Zacharias, M. I.; Castillo, Danilo J.; Corbin, T. E.; DiVittorio, Michael; Dutta, Somnath; Gaume, R. A.; Gauss, S.; Germain, M. E.; Hall, David; Hartkopf, William I.; Hsu, Danley C.; Holdenried, E. R.; Макаров, В. В.; Martines, Marcos Roberto; Mason, Brian D.; Monet, D.; Rafferty, T. J.; Rhodes, Alan; Siemers, T.; Smith, D.; Tilleman, T.; Urban, S. E.; Wieder, G.; Winter, Lars; Young, André

doi:10.1088/0004-6256/139/6/2184

Cited by 334 publications

(163 citation statements)

References 10 publications

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“…5 ± 3.5. These results are in agreement with those derived by T2014 (PA=17 Zacharias et al 2010) when including the ∼0″ .1 astrometric uncertainty from our ALMA Cycle 0 observations and the 0″ .06 uncertainty from our input coordinates (2MASS catalog, Cutri et al 2003). We corrected for this offset in our analysis of the disk.…”

Section: Disk Orientationsupporting

confidence: 91%

GAS INSIDE THE 97 AU CAVITY AROUND THE TRANSITION DISK Sz 91

Cánovas

Schreiber

Cáceres

et al. 2015

ApJ

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We present ALMA (Cycle 0) band6 and band3 observations of the transition disk Sz 91. The disk inclination and position angle are determined to be i=49• . 5 and the dusty and gaseous disk are detected up to ∼220 and ∼400 AU from the star, respectively. Most importantly, our continuum observations indicate that the cavity size in the millimeter-sized dust distribution must be ∼97 AU in radius, the largest cavity observed around a T Tauri star. Our data clearly confirmthe presence of CO 12 (2-1) well inside the dust cavity. Based on these observational constraints we developed a disk model that simultaneously accounts for the CO 12 and continuum observations (i.e., gaseous and dusty disk). According to our model, most of the millimeter emission comes from a ring located between 97 and 140 AU. We also find that the dust cavity is divided into an innermost region largely depleted of dust particles ranging from the dust sublimation radius up to 85 AU, and a second, moderately dust-depleted region, extending from 85 to 97 AU. The extremely large size of the dust cavity, the presence of gas and small dust particles within the cavity, and the accretion rate of Sz 91 are consistent with the formation of multiple (giant) planets.

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Section: Disk Orientationsupporting

confidence: 91%

GAS INSIDE THE 97 AU CAVITY AROUND THE TRANSITION DISK Sz 91

Cánovas

Schreiber

Cáceres

et al. 2015

ApJ

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“…4.2) and published proper motion (UCAC3, Zacharias et al 2010) agrees well with the velocity of the young disc population of the Galaxy (see Moór et al 2006, Fig. 1.…”

Section: Age Estimates Of the Systemsupporting

confidence: 83%

Young solar type active stars: the TYC 2627-638-1 system

Oláh

Korhonen²,

Vida

et al. 2010

A&A

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We present BV(RI) C and JHK s photometry and low-and high-resolution spectroscopy of the 11th mag G-type star TYC 2627-638-1. Our investigation reveals that the target is separated into two young, early-G-type main-sequence (or late pre-main-sequence) stars, which are most probably bound and form a wide binary system. A substellar body orbits the brighter component as implied by radial velocity variations. The brighter component possibly also has a faint, later type stellar companion.Both components of the wide binary have clear emission cores in the Ca ii H&K lines and filled-in Hα absorption, indicating that both stars are chromospherically active. Our photometric time series reveals clear but only a few hundredths of a magnitude amplitude rotational modulation, which is most likely due to cool starspots. Two distinct periods, near 3.5 and 3.7 days, are found in the brightness variations. Photometry obtained separately of the two components of the wide binary show that these periodicities belong to the brighter star. The fainter component shows a much slower light variation of about 0.3 mag. amplitude. In addition, long-term changes in the brightness of both stars are seen. The spectral energy distribution shows a strong near-infrared excess in the fainter component of the wide binary.

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“…All stars are matched with the UCAC3 catalog (Zacharias et al 2010) in order to assign equatorial coordinates and to adjust instrumental magnitudes to a standard magnitude system. The astrometric calibration achieves an average residual of 0.23 arcsec.…”

Section: Observations and Data Reductionmentioning

confidence: 99%