The CPMDS catalogue of common proper motion double stars in the Bordeaux Carte du Ciel zone

Gavras, P.; Sinachopoulos, D.; Campion, J.-F. Le; Ducourant, C.

doi:10.1051/0004-6361/200913369

Cited by 4 publications

(1 citation statement)

References 15 publications

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“…To check if the computation of these parameters on the reconstructed images had discriminatory capabilities for different galaxy classes, we simulated Gaia observations on a set of 2640 galaxies. This simulation was performed using Gaia's pixel-level simulator, the Gaia Instrument and Basic Image Simulator, or GIBIS, version 7 (Babusiaux et al 2009), with MAGIL, which is the MAnager of Gaia Image Library (Gavras et al 2010).…”

Section: P5mentioning

confidence: 99%

Pushing the limits of theGaiaspace mission by analyzing galaxy morphology

Krone-Martins

Ducourant

Teixeira

et al. 2013

A&A

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Context. The ESA Gaia mission, to be launched during 2013, will observe billions of objects, among which many galaxies, during its 5 yr scanning of the sky. This will provide a large space-based dataset with unprecedented spatial resolution. Aims. Because of its natural Galactic and astrometric priority, Gaia's observational strategy was optimized for point sources. Nonetheless, it is expected that ∼10 6 sources will be extragalactic, and a large portion of them will be angularly small galaxies. Although the mission was designed for point sources, an analysis of the raw data will allow the recovery of morphology of those objects at a ∼0.2 level. This may constitute a unique all-sky survey of such galaxies. We describe the conceptual design of the method adopted for the morphological analysis of these objects as well as first results obtained from data simulations of low-resolution highly binned data. Methods. First, the raw Gaia 1D observations are used to reconstruct a 2D image of the object -this image is known to contain artifacts and reconstruction signatures. Then, parameters characteristic of the reconstructed image are measured, and used for a purely morphological classification. Finally, based on the classification, a light profile is selected (pure-disk, disk+bulge, pure bulge, point source+disk, etc.) and fitted to all Gaia 1D observations simultaneously in a global process using forward modeling. Results. Using simulations of Gaia observations from official Gaia Data Processing and Analysis Consortium tools, we were able to obtain the preliminary classification of the simulated objects at the ∼83% level for two classes (ellipticals, spirals/irregulars) or at the ∼79%, ∼56%, and ∼74% levels for three classes (E, S, and I). The morphological parameters of simulated object light profiles are recovered with errors at the following levels: −9 ± 36% for the bulge radius, 11 ± 53% for the bulge intensity, 1 ± 4% for the disk radius, and −1 ± 7% for the disk intensity. From these results, we conclude that it is possible to push the limits of the Gaia space mission by analysing galaxy morphology.

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Section: P5mentioning

confidence: 99%

Pushing the limits of theGaiaspace mission by analyzing galaxy morphology

Krone-Martins

Ducourant

Teixeira

et al. 2013

A&A

Self Cite

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TheGaia-ESO Survey: double-, triple-, and quadruple-line spectroscopic binary candidates

Merle

Eck

Jorissen

et al. 2017

A&A

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Context. The Gaia-ESO Survey (GES) is a large spectroscopic survey that provides a unique opportunity to study the distribution of spectroscopic multiple systems among different populations of the Galaxy. Aims. Our aim is to detect binarity/multiplicity for stars targeted by the GES from the analysis of the cross-correlation functions (CCFs) of the GES spectra with spectral templates. Methods. We developed a method based on the computation of the CCF successive derivatives to detect multiple peaks and determine their radial velocities, even when the peaks are strongly blended. The parameters of the detection of extrema (doe) code have been optimized for each GES GIRAFFE and UVES setup to maximize detection. The doe code therefore allows to automatically detect multiple line spectroscopic binaries (SBn, n ≥ 2). Results. We apply this method on the fourth GES internal data release and detect 354 SBn candidates (342 SB2, 11 SB3, and even one SB4), including only nine SBs known in the literature. This implies that about 98% of these SBn candidates are new because of their faint visual magnitude that can reach V = 19. Visual inspection of the SBn candidate spectra reveals that the most probable candidates have indeed a composite spectrum. Among the SB2 candidates, an orbital solution could be computed for two previously unknown binaries: CNAME 06404608+0949173 (known as V642 Mon) in NGC 2264 and CNAME 19013257-0027338 in Berkeley 81 (Be 81). A detailed analysis of the unique SB4 (four peaks in the CCF) reveals that CNAME 08414659-5303449 (HD 74438) in the open cluster IC 2391 is a physically bound stellar quadruple system. The SB candidates belonging to stellar clusters are reviewed in detail to discard false detections. We suggest that atmospheric parameters should not be used for these system components; SB-specific pipelines should be used instead. Conclusions. Our implementation of an automatic detection of spectroscopic binaries within the GES has allowed the efficient discovery of many new multiple systems. With the detection of the SB1 candidates that will be the subject of a forthcoming paper, the study of the statistical and physical properties of the spectroscopic multiple systems will soon be possible for the entire GES sample.

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Chlorine-bearing molecules in molecular absorbers at intermediate redshifts

Wallström

Müller

Roueff

et al. 2019

A&A

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We use observations of chlorine-bearing species in molecular absorbers at intermediate redshifts to investigate chemical properties and 35 Cl/ 37 Cl isotopic ratios in the absorbing sightlines. Chloronium (H2Cl + ) is detected along three independent lines of sight in the z=0.89 and z=0.68 molecular absorbers located in front of the lensed quasars PKS 1830−211 and B 0218+357, respectively. Hydrogen chloride (HCl) was observed only toward PKS 1830−211, and is found to behave differently from H2Cl + . It is detected in one line of sight with an abundance ratio [H2Cl + ]/[HCl] ∼ 1, but remains undetected in the other, more diffuse, line of sight, with a ratio [H2Cl + ]/[HCl] > 17. The absorption profiles of these two chlorine-bearing species are compared to other species and discussed in terms of the physical properties of the absorbing gas. Our findings are consistent with the picture emerging from chemical models where different species trace gas with different molecular hydrogen fraction. The 35 Cl/ 37 Cl isotopic ratios are measured in the different lines of sight and are discussed in terms of stellar nucleosynthesis.

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The CPMDS catalogue of common proper motion double stars in the Bordeaux Carte du Ciel zone

Cited by 4 publications

References 15 publications

Pushing the limits of theGaiaspace mission by analyzing galaxy morphology

Pushing the limits of theGaiaspace mission by analyzing galaxy morphology

TheGaia-ESO Survey: double-, triple-, and quadruple-line spectroscopic binary candidates

Chlorine-bearing molecules in molecular absorbers at intermediate redshifts

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