Vvv dr1: the first data release of the milky way bulge and southern plane from the near-infrared eso public survey vista variables in the via lactea

By R. Saito, M. Hempel, D. Minniti, P. Lucas, M. Rejkuba, I. Toledo, O. Gonzalez, J. Alonso-García, M. Irwin, E. González-Solares and 100 more. 2011

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Context. The ESO public survey VISTA variables in the V�a L�ctea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years. Aims: We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained. Methods: The observations are carried out on the 4-m VISTA telescope in the ZYJHK s filters. In addition to the multi-band imaging the variability monitoring campaign in the K s filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. Results: The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHK s filters taken in the 2010 observing season. The typical image quality is 0.9 arcsec {-1.0 arcsec}. The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHK s images in the disk area and 90% of the JHK s images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28 � 10 8 stellar sources in the bulge and 1.68 � 10 8 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63 � 10 8 stellar sources. About 10% of these are double detections because of overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHK s bands extend typically 4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for K s = 15-18 mag has rms 35-175 mas. Conclusions: The VVV Survey data products offer a unique dataset to map the stellar populations in the Galactic bulge and the adjacent plane and provide an exciting new tool for the study of the structure, content, and star-formation history of our Galaxy, as well as for investigations of the newly discovered star clusters, star-forming regions in the disk, high proper motion stars, asteroids, planetary nebulae, and other interesting objects. Based on observations taken within the ESO VISTA Public Survey VVV, Programme ID 179.B-2002.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6130a1b765e3b8512a7023cdd548d0b7da709516

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Citations in the corpus

REDDENING AND EXTINCTION TOWARD THE GALACTIC BULGE FROM OGLE-III: THE INNER MILKY WAY'S RV ∼ 2.5 EXTINCTION CURVE (2012, methodology): “3http://ogle.astrouw.edu.pl/ We also make use of data from the Two Micron All Sky Survey (2MASS, Skrutskie et al. 2006), which we calibrate on the measurements of Gonzalez et al. (2012), who used data from the VISTA Variables in The Via Lactea survey (VVV, Saito et al. 2012).”
Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution (2016, methodology): “We evaluate the incompleteness of the 2MASS survey by comparing with the deeper VVV survey where available (Saito et al. 2012), completeness corrected by Wegg & Gerhard (2013).”
A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS) (2018, background): “Surveys that have produced data used for variable star discovery and analysis include the gravitational microlensing surveys MACHO (Alcock et al. 1993) and OGLE (Udalski et al. 1994); supernova/transient surveys including the All-Sky Automated Survey (ASAS; Pojmański 1997), the All-Sky Automated Sur”
The Zwicky Transient Facility: Science Objectives (2019, methodology): “These surveys include the Optical Gravitational Lensing Experiment (OGLE; e.g. Soszyński et al. 2015), CRTS (Drake et al. 2009), PTF (Law et al. 2009), the Vista Variables in the Via Lactea (VVV; Saito et al. 2012), ASAS-SN, (Shappee et al. 2014)) and most recently ATLAS (Heinze et al. 2018).”
Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, background): “In light of these requirements, probably the best source for photometric variability information on our sample stars would be long-term monitoring photometric surveys over large areas of the Galactic bulge, such as OGLE (Udalski et al. 1997; Soszyński et al. 2013) in the optical, and VVV (Saito et ”
Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS II. The complete high resolution extinction map and implications for Galactic bulge studies (2012, background): “This corresponds to the first data release (DR1) of the survey, as described in Saito et al. (2012).”
Made-to-measure models of the Galactic box/peanut bulge: stellar and total mass in the bulge region (2015, background): “In the last decade, stellar surveys of the GB such as 2MASS (Skrutskie et al. 2006), VVV (Saito et al. 2012), OGLE (Sumi et al. 2004), BRAVA (Rich et al. 2007) and ARGOS (Freeman et al. 2013) have released unprecedented data sets which allow us to study the GB star-by-star.”
Precise time series photometry for the Kepler-2.0 mission (2014, background): “…is based on experience gained in the context of several ground-based wide-field time-series photometric surveys, namely: the Monitor project (Aigrain et al. 2007), the UKIRT WFCAM Transit Survey (WTS, Nefs et al. 2012), and the VISTA variables in the Vı́a Láctea survey (VVV, Saito et al. 2012).”
THE CATALINA SURVEYS PERIODIC VARIABLE STAR CATALOG (2014, background): “This will ultimately cover 562 square degrees in Z, Y , J , H and Ks (Saito et al. 2012).”
The structure of the Milky Way's bar outside the bulge (2015, methodology): “…we use data from (i) the United Kingdom Infrared Deep Sky Survey (UKIDSS) Galactic Plane Survey (GPS, Lucas et al. 2008), (ii) the VVV survey (Saito et al. 2012) and, (iii) to extend the study further from the galactic plane than previous studies, we augment this with 2MASS data (Skrutskie…”