The initial<i>Gaia</i>source list

Smart, R. L.; Nicastro, L.

doi:10.1051/0004-6361/201424241

Cited by 50 publications

(41 citation statements)

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“…Of the 1141 million sources in the secondary astrometric data set 685 million are in common with the Initial Gaia Source List (IGSL, Smart & Nicastro 2014) and 456 million are new sources . The IGSL formed the starting point for the process of assigning Gaia observations to sources (Fabricius et al 2016).…”

Section: Overview Of the Contents Of Gaia Dr1mentioning

confidence: 99%

“…The vast majority of these pairs are created during the cross-match stage, when observations (focal plane transits) get grouped together and assigned to sources (see Fabricius et al 2016). The main underlying cause is sources appearing twice in the IGSL, which was evident from the many close pairs occurring along photographic survey plate boundaries (the IGSL is based to a large extent on photographic surveys, Smart & Nicastro 2014). A large fraction of these pairs are likely to be two instances of the same physical source (i.e.…”

Section: Gaia Dr1 Validation and Source Filteringmentioning

confidence: 99%

See 1 more Smart Citation

GaiaData Release 1

Brown¹,

Vallenari²,

Prusti³

et al. 2016

A&A

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1,739

272

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Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. Aims. A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. Methods. The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue. Results. Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the Hipparcos and Tycho-2 catalogues -a realisation of the Tycho-Gaia Astrometric Solution (TGAS) -and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of ∼3000 Cepheid and RR Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yr −1 for the proper motions. A systematic component of ∼0.3 mas should be added to the parallax uncertainties. For the subset of ∼94 000 Hipparcos stars in the primary data set, the proper motions are much more precise at about 0.06 mas yr −1 . For the secondary astrometric data set, the typical uncertainty of the positions is ∼10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to ∼0.03 mag over the magnitude range 5 to 20.7. Conclusions. Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data.

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Section: Overview Of the Contents Of Gaia Dr1mentioning

confidence: 99%

Section: Gaia Dr1 Validation and Source Filteringmentioning

confidence: 99%

GaiaData Release 1

Brown¹,

Vallenari²,

Prusti³

et al. 2016

A&A

Self Cite

1,739

272

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“…For the astrometric calibration, THELI uses Scamp (Bertin & Arnouts 1996). Source catalogs (mostly stars) were extracted from the images and matched against the Initial Gaia Source List (IGSL, Smart & Nicastro 2014) in the J2000 ICRF reference frame. Images were distortion-corrected using a thirdorder polynomial description, and registered with respect to each other with a typical precision of 1/20th pixel.…”

Section: Gemini Observations and Data Reductionmentioning

confidence: 99%

Gemini Follow-up of Two Massive H i Clouds Discovered with the Australian Square Kilometer Array Pathfinder

Madrid

Lee-Waddell

Serra

et al. 2018

ApJL

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Using the Gemini Multi Object Spectrograph (GMOS) we search for optical counterparts of two massive (∼ 10 9 M ⊙ ) neutral hydrogen clouds near the spiral galaxy IC 5270, located in the outskirts of the IC 1459 group. These two H i clouds were recently discovered using the Australian Square Kilometer Array Pathfinder (ASKAP). Two low surface brightness optical counterparts to one of these H i clouds are identified in the new Gemini data that reaches down to magnitudes of ∼27.5 mag in the g-band. The observed H i mass to light ratio derived with these new data, M H I /L g = 242, is among the highest reported to date. We are also able to rule out that the two H i clouds are dwarf companions of IC 5270. Tidal interactions and ram pressure stripping are plausible explanations for the physical origin of these two clouds.

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“…This utilized adapted V magnitudes of 12.76 and 17.1 for the two stellar images, the bolometric luminosities for the four M stars given in Table 5, the bolometric magnitude of the 'B-N' image inferred from Table 2, and appropriate bolometric corrections for the M stars in question. (f) From UCAC4 (Zacharias et al 2013);Smart & Nicastro (2014);Huber et al (2015).…”

Section: Notes (A)mentioning

confidence: 99%

EPIC 220204960: A Quadruple Star System Containing Two Strongly Interacting Eclipsing Binaries

Rappaport

Vanderburg

Borkovits

et al. 2017

Mon. Not. R. Astron. Soc.

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We present a strongly interacting quadruple system associated with the K2 target EPIC 220204960. The K2 target itself is a K p = 12.7 magnitude star at T eff 6100 K which we designate as "B-N" (blue northerly image). The host of the quadruple system, however, is a K p 17 magnitude star with a composite M-star spectrum, which we designate as "R-S" (red southerly image). With a 3.2 separation and similar radial velocities and photometric distances, 'B-N' is likely physically associated with 'R-S', making this a quintuple system, but that is incidental to our main claim of a strongly interacting quadruple system in 'R-S'. The two binaries in 'R-S' have orbital periods of 13.27 d and 14.41 d, respectively, and each has an inclination angle of 89• . From our analysis of radial velocity measurements, and of the photometric lightcurve, we conclude that all four stars are very similar with masses close to 0.4 M . Both of the binaries exhibit significant ETVs where those of the primary and secondary eclipses 'diverge' by 0.05 days over the course of the 80-day observations. Via a systematic set of numerical simulations of quadruple systems consisting of two interacting binaries, we conclude that the outer orbital period is very likely to be between 300 and 500 days. If sufficient time is devoted to RV studies of this faint target, the outer orbit should be measurable within a year.

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The initialGaiasource list

Cited by 50 publications

References 12 publications

GaiaData Release 1

GaiaData Release 1

Gemini Follow-up of Two Massive H i Clouds Discovered with the Australian Square Kilometer Array Pathfinder

EPIC 220204960: A Quadruple Star System Containing Two Strongly Interacting Eclipsing Binaries

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