Contrast sensitivities in the <i>Gaia</i> Data Release 2

Brandeker, Alexis; Cataldi, Gianni

doi:10.1051/0004-6361/201834321

Cited by 56 publications

(47 citation statements)

References 13 publications

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“…The advantage of this approach is that the sources in the chance alignment catalog, being nearby and having precise parallaxes, are more representative of objects in the binary catalog. Unsurprisingly -since it was verified in ER18 that there are no strong trends in contrast sensitivity with apparent magnitude or source density; see also Brandeker & Cataldi (2019) -the improved constraints are fairly similar to those derived in ER18. We compare them in Figure D4.…”

Section: D2 Contrast Sensitivity For Close Pairssupporting

confidence: 66%

“…comparing the two point correlation function of chance alignments to what would be expected in the absence of crowding/blending effects (e.g. Arenou et al 2018;Brandeker & Cataldi 2019). Of course, the sensitivity to companions in a particular catalog depends on the quality cuts imposed: cuts that remove objects with somewhat contaminated photometry will lower the sensitivity.…”

Section: D2 Contrast Sensitivity For Close Pairsmentioning

confidence: 99%

See 1 more Smart Citation

Discovery of an equal-mass ‘twin’ binary population reaching 1000 + au separations

El-Badry

Rix

Tian

et al. 2019

Monthly Notices of the Royal Astronomical Society

125

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We use a homogeneous catalog of 42,000 main-sequence wide binaries identified by Gaia to measure the mass ratio distribution, p(q), of binaries with primary masses 0.1 < M 1 /M < 2.5, mass ratios 0.1 q < 1, and separations 50 < s/AU < 50, 000. A well-understood selection function allows us to constrain p(q) in 35 independent bins of primary mass and separation, with hundreds to thousands of binaries in each bin. Our investigation reveals a sharp excess of equal-mass "twin" binaries that is statistically significant out to separations of 1,000 to 10,000 AU, depending on primary mass. The excess is narrow: a steep increase in p(q) at 0.95 q < 1, with no significant excess at q 0.95. A range of tests confirm the signal is real, not a data artifact or selection effect. Combining the Gaia constraints with those from close binaries, we show that the twin excess decreases with increasing separation, but its width (q 0.95) is constant over 0.01 < a/AU < 10, 000. The wide twin population would be difficult to explain if the components of all wide binaries formed via core fragmentation, which is not expected to produce strongly correlated component masses. We conjecture that wide twins formed at closer separations (a 100 AU), likely via accretion from circumbinary disks, and were subsequently widened by dynamical interactions in their birth environments. The separation-dependence of the twin excess then constrains the efficiency of dynamical widening and disruption of binaries in young clusters. We also constrain p(q) across 0.1 q < 1. Besides changes in the twin fraction, p(q) is independent of separation at fixed primary mass over 100 s/AU < 50, 000. It is flatter than expected for random pairings from the IMF but more bottom-heavy for wide binaries than for binaries with a 100 AU.

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Section: D2 Contrast Sensitivity For Close Pairssupporting

confidence: 66%

Section: D2 Contrast Sensitivity For Close Pairsmentioning

confidence: 99%

Discovery of an equal-mass ‘twin’ binary population reaching 1000 + au separations

El-Badry

Rix

Tian

et al. 2019

Monthly Notices of the Royal Astronomical Society

125

View full text Add to dashboard Cite

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“…Ziegler et al 2018and Brandeker & Cataldi (2019) have mapped the completeness limit close to bright stars to be ∆G ∼ 6 mag at ρ = 2 , ∆G ∼ 8 mag at ρ = 3 , and ∆G ∼ 10 mag at ρ = 6 . The evolutionary models of Baraffe et al (2015) would imply corresponding physical limits of M ∼ 0.20M at ρ = 250 AU, M ∼ 0.085M at ρ = 375 AU, and M ∼ 0.050M at ρ = 750 AU.…”

Section: Limits On Additional Companionsmentioning

confidence: 99%

TESS Hunt for Young and Maturing Exoplanets (THYME). IV. Three Small Planets Orbiting a 120 Myr Old Star in the Pisces–Eridanus Stream*

Newton

Mann

Kraus

et al. 2021

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Young exoplanets can offer insight into the evolution of planetary atmospheres, compositions, and architectures. We present the discovery of the young planetary system TOI 451 (TIC 257605131, Gaia DR2 4844691297067063424). TOI 451 is a member of the 120-Myr-old Pisces-Eridanus stream (Psc-Eri). We confirm membership in the stream with its kinematics, its lithium abundance, and the rotation and UV excesses of both TOI 451 and its wide binary companion, TOI 451 B (itself likely an M dwarf binary). We identified three candidate planets transiting in the TESS data and followed up the signals with photometry from Spitzer and ground-based telescopes. The system comprises three validated planets at periods of 1.9, 9.2 and 16 days, with radii of 1.9, 3.1, and 4.1 R ⊕ , respectively. The host star is near-solar mass with V = 11.0 and H = 9.3 and displays an infrared excess indicative of a debris disk. The planets offer excellent prospects for transmission spectroscopy with HST and JWST, providing the opportunity to study planetary atmospheres that may still be in the process of evolving.

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“…The resolving power of the Gaia instrument of two sources that lie close together in the sky mainly depends on the angular separation and the magnitude difference (de Bruijne et al 2015) and is called contrast sensitivity, see Brandeker & Cataldi (2019) for a Gaia DR2 determination. In dense regions we especially lose faint sources due to this effect (Rybizki et al 2020), which directly affects our ability to resolve resolve binaries.…”

Section: Contrast Sensitivitymentioning

confidence: 99%

Gaia Early Data Release 3

Smart

Sarro

Rybizki

et al. 2021

A&A

217

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Aims. We produce a clean and well-characterised catalogue of objects within 100 pc of the Sun from the Gaia Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. Methods. Theselection of objects within 100 pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100 pc is included in the catalogue. Results. We have produced a catalogue of 331 312 objects that we estimate contains at least 92% of stars of stellar type M9 within 100 pc of the Sun. We estimate that 9% of the stars in this catalogue probably lie outside 100 pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of Gaia Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10 pc of the Sun. Conclusions. We provide the community with a large, well-characterised catalogue of objects in the solar neighbourhood. This is a primary benchmark for measuring and understanding fundamental parameters and descriptive functions in astronomy.

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Contrast sensitivities in the Gaia Data Release 2

Cited by 56 publications

References 13 publications

Discovery of an equal-mass ‘twin’ binary population reaching 1000 + au separations

Discovery of an equal-mass ‘twin’ binary population reaching 1000 + au separations

TESS Hunt for Young and Maturing Exoplanets (THYME). IV. Three Small Planets Orbiting a 120 Myr Old Star in the Pisces–Eridanus Stream*

Gaia Early Data Release 3

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