VISTA: status and performance

Emerson, J. P.; Sutherland, William J.

doi:10.1117/12.857105

Cited by 85 publications

(76 citation statements)

References 31 publications

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“…The VMC data analysed in this study refer to observations acquired with the Visible and Infrared Survey Telescope for Astronomy (VISTA; Emerson & Sutherland 2010). The data were reduced onto the VISTA photometric system, which is close to the Vegamag system, with the VISTA Data Flow System pipeline v1.3 (VDFS; Irwin et al 2004) and extracted from the VISTA Science Archive (VSA; Cross et al 2012).…”

Section: Observations and Data Selectionmentioning

confidence: 99%

The VMC survey

Cioni

Bekki

Girardi

et al. 2016

A&A

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Aims. In this study we use multi-epoch near-infrared observations from the VISTA survey of the Magellanic Cloud system (VMC) to measure the proper motions of different stellar populations in a tile of 1.5 deg 2 in size in the direction of the Galactic globular cluster 47 Tuc. We obtain the proper motion of the cluster itself, of the Small Magellanic Cloud (SMC), and of the field Milky Way stars. Methods. Stars of the three main stellar components are selected according to their spatial distributions and their distributions in colour−magnitude diagrams. Their average coordinate displacement is computed from the difference between multiple K s -band observations for stars as faint as K s = 19 mag. Proper motions are derived from the slope of the best-fitting line among ten VMC epochs over a time baseline of ∼1 yr. Background galaxies are used to calibrate the absolute astrometric reference frame. Results. The resulting absolute proper motion of 47 Tuc is (μ α cos(δ), μ δ ) = (+7.26 ± 0.03, −1.25 ± 0.03) mas yr −1 . This measurement refers to about 35 000 sources distributed between 10 and 60 from the cluster centre. For the SMC we obtain (μ α cos(δ), μ δ ) = (+1.16 ± 0.07, −0.81 ± 0.07) mas yr −1 from about 5250 red clump and red giant branch stars. The absolute proper motion of the Milky Way population in the line of sight (l = 305.9, b = −44.9) of this VISTA tile is (μ α cos(δ), μ δ ) = (+10.22 ± 0.14, −1.27 ± 0.12) mas yr −1 and has been calculated from about 4000 sources. Systematic uncertainties associated with the astrometric reference system are 0.18 mas yr −1 . Thanks to the proper motion we detect 47 Tuc stars beyond its tidal radius.

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Section: Observations and Data Selectionmentioning

confidence: 99%

The VMC survey

Cioni

Bekki

Girardi

et al. 2016

A&A

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“…Finally, the telluric correction was applied using the fire_xtellcor_ld, a clone of the xtellcor program from SpexTool (Cushing et al 2004;Vacca et al 2003) 2.3 VISTA/VIRCAM The VVV survey (Minniti et al 2010;Saito et al 2012;Hempel et al 2014) is one of the six ESO public surveys carried out with the 4.1m Visual and Infrared Survey Telescope for Astronomy (VISTA) telescope and VIR-CAM camera at cerro Paranal Chile (Dalton et al 2006;Emerson & Sutherland 2010). It has sixteen 2048x2048 pixels chips with a pixel scale of 0.34 ′′ .…”

Section: Magellan/firementioning

confidence: 99%

Spectrophotometric characterization of high proper motion sources fromWISE

Beamín

Ivanov

Minniti

et al. 2015

Mon. Not. R. Astron. Soc.

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The census of the solar neighborhood is almost complete for stars and becoming more complete in the brown dwarf regime. Spectroscopic, photometric and kinematic characterization of nearby objects helps us to understand the local mass function, the binary fraction, and provides new targets for sensitive planet searches. We aim to derive spectral types and spectro-photometric distances of a sample of new high proper motion sources found with the WISE satellite, and obtain parallaxes for those objects that fall within the area observed by the Vista Variables in the Vía Láctea survey (VVV). We used low resolution spectroscopy and template fitting to derive spectral types, multiwavelength photometry to characterize the companion candidates and obtain photometric distances. Multi-epoch imaging from the VVV survey was used to measure the parallaxes and proper motions for three sources. We confirm a new T2 brown dwarf within ∼15 pc. We derived optical spectral types for twenty four sources, mostly M dwarfs within 50 pc. We addressed the wide binary nature of sixteen objects found by the WISE mission and previously known high proper motion sources. Six of these are probably members of wide binaries, two of those are new, and present evidence against the physical binary nature of two candidate binary stars found in the literature, and eight that we selected as possible binary systems. We discuss a likely microlensing event produced by a nearby low mass star and a galaxy, that is to occur in the following five years.

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“…The near-IR data analysed in this study were obtained with the Visual and Infrared Survey Telescope for Astronomy (VISTA; Emerson & Sutherland 2010) for the VMC survey and include observations acquired until the end of September 2011. The data were reduced onto the VISTA photometric system (Vegamag = 0) with the VISTA Data Flow System (VDFS) pipeline v1.1 (Irwin et al 2004) and extracted from the VISTA Science Archive 1 (VSA).…”

Section: Vmc Datamentioning

confidence: 99%

The VMC Survey

Cioni¹,

Kamath²,

Rubele³

et al. 2012

A&A

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Context. The number and spatial distribution of confirmed quasi-stellar objects (QSOs) behind the Magellanic system is limited. This undermines their use as astrometric reference objects for different types of studies. Aims. We have searched for criteria to identify candidate QSOs using observations from the VISTA survey of the Magellanic Clouds system (VMC) that provides photometry in the Y JK s bands and 12 epochs in the K s band. Methods. The (Y − J) versus (J − K s ) diagram has been used to distinguish QSO candidates from Milky Way stars and stars of the Magellanic Clouds. Then, the slope of variation in the K s band has been used to identify a sample of high confidence candidates. These criteria were developed based on the properties of 117 known QSOs presently observed by the VMC survey. Results. VMC Y JK s magnitudes and K s light-curves of known QSOs behind the Magellanic system are presented. About 75% of them show a slope of variation in K s > 10 −4 mag/day and the shape of the light-curve is in general irregular and without any clear periodicity. The number of QSO candidates found in tiles including the south ecliptic pole and the 30 Doradus regions is 22 and 26, respectively, with a ∼20% contamination by young stellar objects, planetary nebulae, stars and normal galaxies. Conclusions. By extrapolating the number of QSO candidates to the entire VMC survey area we expect to find about 1200 QSOs behind the LMC, 400 behind the SMC, 200 behind the Bridge and 30 behind the Stream areas, but not all will be suitable for astrometry. Further, the K s band light-curves can help support investigations of the mechanism responsible for the variations.

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VISTA: status and performance

Cited by 85 publications

References 31 publications

The VMC survey

The VMC survey

Spectrophotometric characterization of high proper motion sources fromWISE

The VMC Survey

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