VOSA: virtual observatory SED analyzer

Bayo, A.; Rodrigo, C.; Barrado, D.; Solano, E.; Gutiérrez, Raúl; Morales-Calderón, M.; Allard, F.

doi:10.1051/0004-6361:200810395

Cited by 546 publications

(477 citation statements)

References 34 publications

Supporting

Mentioning

472

Contrasting

Order By: Relevance

“…We repeated their procedure by fitting the GRAMS C-rich grid of models of dust shells around red supergiant and AGB stars (Srinivasan, Sargent & Meixner 2011) to the same mid-infared photometry as Riebel et al (2012), supplemented with data from WISE (Cutri et al 2012) and DENIS (Cioni et al 2000) catalogs. Using VOSA (Bayo et al 2008) we performed a Bayesian analysis of the data. We assumed the distance of LMC d = 49.97 kpc (Pietrzyński et al 2013) and E(B-V)=0.05 (Muerset et al 1991).…”

Section: The Cool Giantmentioning

confidence: 99%

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present an analysis of multi-epoch low-resolution spectrophotometry, complemented by the light curves provided by massive photometric surveys spanning over 100 years, of the symbiotic binary LMC S63. We showed that it is an eclipsing binary with the orbital period of 1050 d . We also found evidence of outbursts in history of the white dwarf. If it was a Z-And type outburst, as is most likely, it would be a second such outburst recorded in the Magellanic Cloud symbiotic system. We confirmed that the red giant is enhanced in carbon, and estimated C/O ≃ 1.2 by fitting a model atmosphere to the SALT spectrum. We also found bi-periodic pulsations of the red giant, and demonstrated that it is similar to other carbon variables with confirmed bi-periodicity.

show abstract

Section: The Cool Giantmentioning

confidence: 99%

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…Most of the data were retrieved using the latest version of the VO SED Analyzer tool 3 (VOSA; Bayo et al 2008Bayo et al , 2013. They include ultraviolet photometry from GALEX (Bianchi & GALEX Team 2000), optical photometry (B, V and I) from the Tycho-2 and DENIS catalogues (Høg et al 2000;DENIS Consortium 2005), near-infrared photometry from 2MASS (Skrutskie et al 2006), and mid-infrared photometry from AKARI and WISE (Ishihara et al 2010;Cutri et al 2012).…”

Section: Photometrymentioning

confidence: 99%

Proper motions of young stars in Chamaeleon

Martí

Jiménez-Esteban

Bayo

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

Context. The study of the motion of the members of a given open cluster or stellar association provides key information about their formation and early evolution. The Chamaeleon cloud complex constitutes one of the closest and best studied low-mass star-forming regions in the Galaxy. Aims. We want to provide further evidence of the origin of the proposed stellar members of Chamaeleon and to identify interlopers from the foreground Cha and η Cha associations. Methods. We have compiled lists of spectroscopically confirmed members of Chamaeleon I and II, Cha and η Cha, and of background objects in the same line of sight. Using Virtual Observatory tools, we cross-match these lists with the UCAC3 catalogue to get the proper motions of the objects. In the vector point diagram, we identify the different moving groups, and use this information to study the membership of proposed candidate members of the associations from the literature. For those objects with available radial velocities, we compute their Galactic space velocities. We look for correlations between the known properties of the objects and their proper motions. Results. The members of the dark clouds exhibit clearly different proper motions from those of the foreground associations and of the background stars. The data suggest that Chamaeleon II could have different dynamical properties from Chamaeleon I. Although the two foreground clusters and η Chamaeleontis constitute two different proper motion groups, they have similar spatial motions, which are different from the spatial motion of Chamaeleon I. On the other hand, the space motions of the Chamaeleon II stars look more similar to those of the foreground clusters than to the Chamaeleon I stars, but the numbers are low. We find no correlations between the proper motions and the properties of the objects in either of the clouds. Conclusions. On the basis of proper motion, Chamaeleon I and II constitute two physical entities unrelated to the foreground and η Chamaeleontis clusters, but with the available data it is unclear to what extent the stellar populations in both clouds are physically connected to each other.

show abstract

“…Finally, the spectrum was integrated in the bandpass listed in Table 4 as described in Bayo et al (2008). We did not consider the NUV point for the reason listed previously.…”

Section: Hd 8049 B a New Nearby Wdmentioning

confidence: 99%

Astrophysical false positives in direct imaging for exoplanets: a white dwarf close to a rejuvenated star

Zurlo

Vigan

Hagelberg

et al. 2013

A&A

View full text Add to dashboard Cite

Context. As is the case for all techniques involved in the research for exoplanets, direct imaging has to take into account the probability of so-called astrophysical false positives, which are phenomena that mimic the signature of the objects we are seeking. Aims. In this work we present the case of a false positive found during a direct-imaging survey conducted with VLT/NACO. A promising exoplanet candidate was detected around the K2-type star HD 8049 in July 2010. Its contrast of ∆H = 7.05 at 1.57 arcsec allowed us to assume a 35 M Jup companion at 50 projected AU, for the nominal system age and heliocentric distance. Methods. To check whether it was gravitationally bound to the host star, as opposed to an unrelated background object, we re-observed the system one year later and concluded a high probability of a bound system. We also used radial velocity measurements of the host star, spanning a time range of ∼30 yr, to constrain the companion's mass and orbital properties, as well as to probe the host star's spectral age indicators and general spectral energy distribution. We also obtained U-band imaging with EFOSC and near-infrared spectroscopy for the companion. Results. Combining all these information we conclude that the companion of HD 8049 is a white dwarf (WD) with temperature T eff = 18 800 ± 2100 K and mass M WD = 0.56 ± 0.08 M . The significant radial velocity trend combined with the imaging data indicates that the most probable orbit has a semi-major axis of about 50 AU. The discrepancy between the age indicators speaks against a bona-fide young star. The moderately high level of chromospheric activity and fast rotation, mimicking the properties of a young star, might be induced by the exchange of mass with the progenitor of the WD. This example demonstrates some of the challenges in determining accurate age estimates and identifications of faint companions.

show abstract

VOSA: virtual observatory SED analyzer

Cited by 546 publications

References 34 publications

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Proper motions of young stars in Chamaeleon

Astrophysical false positives in direct imaging for exoplanets: a white dwarf close to a rejuvenated star

Contact Info

Product

Resources

About