Physical parameters of Brown Dwarfs in Cha I with VOSA A. Bayo 1 , C. Rodrigo 2,3 , D. Barrado 2,4 , R. Sanchez-Janssen 1 , E. Solano 2,3 , B. Montesinos 2 , H. Bouy 2 , M. Morales-Calderon 2 , F. Allard 5 , F. Jimenez-Esteban 2,3 1 European Southern Observatory, Chile 2 Centro de Astrobiología, INTA-CSIC, Madrid, Spain 3 Spanish Virtual Observatory, Spain 4 Calar Alto Observatory, CAHA 5 CRAL, Ecole Normale Superiour, France Contact e-mail address: [email protected] The advent of new and more sensitive surveys providing photometry at many wavelength ranges and covering large sky areas (GALEX, SDSS, 2MASS, UKIDSS, AKARI, WISE) and the steady increase of available archival data from ground based observatories are pushing astronomy towards a change of paradigm where small groups, and not only large consortia, need to analyze large multi-wavelength data sets as part of their everyday work. In this context, the Virtual Observatory (VO), as a common frame to exchange not only observational data but also theoretical models, plays a very important role. This applies in particular to the field of brown dwarfs were the answers to most of the open questions (mechanism of formation, disk evolution, etc.) require the analysis of large datasets of multi-wavelength observations. We have improved our public web-based Virtual Observatory tool, VOSA, so that it estimates additional parameters (interstellar extinction), accesses new state-of –the-art collections of models, and performs more sophisticated and complete analysis of Spectral Energy Distributions. We show examples of these capabilities analyzing the Cha I population, paying special attention to the substellar population. Abstract SVO Services Getting a 3D view of Chamaeleon I By comparing the extinction estimated from SED fitting with the integrated extinction along the line of sight given by methods like the star counts A v (mag) SC Parameters of BDs in Chamaeleon I VOSA uses two methodologies: probability analysis of the estimated parameters and χ 2 minimization for a general overview of the fit. http://svo2.cab.inta-csic.es/svo/theory/vosa

Physical parameters of Brown Dwarfs in Cha I with VOSA · 1European Southern Observatory, Chile 2Centro de Astrobiología, INTA-CSIC, Madrid, Spain 3Spanish Virtual Observatory, Spain

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Page 1: Physical parameters of Brown Dwarfs in Cha I with VOSA · 1European Southern Observatory, Chile 2Centro de Astrobiología, INTA-CSIC, Madrid, Spain 3Spanish Virtual Observatory, Spain

Physical parameters of Brown Dwarfs in Cha I with VOSA A. Bayo1, C. Rodrigo2,3, D. Barrado2,4, R. Sanchez-Janssen1, E. Solano2,3, B.

Montesinos2, H. Bouy2, M. Morales-Calderon2, F. Allard5, F. Jimenez-Esteban2,3

1European Southern Observatory, Chile 2Centro de Astrobiología, INTA-CSIC, Madrid, Spain

3Spanish Virtual Observatory, Spain 4Calar Alto Observatory, CAHA

5CRAL, Ecole Normale Superiour, France

Contact e-mail address: [email protected]

The advent of new and more sensitive surveys providing photometry at many wavelength ranges and covering large sky areas (GALEX, SDSS, 2MASS, UKIDSS, AKARI, WISE) and the steady increase of available archival data from ground based observatories are pushing astronomy towards a change of paradigm where small groups, and not only large consortia, need to analyze large multi-wavelength data sets as part of their everyday work. In this context, the Virtual Observatory (VO), as a common frame to exchange not only observational data but also theoretical models, plays a very important role. This applies in particular to the field of brown dwarfs were the answers to most of the open questions (mechanism of formation, disk evolution, etc.) require the analysis of large datasets of multi-wavelength observations.

We have improved our public web-based Virtual Observatory tool, VOSA, so that it estimates additional parameters (interstellar extinction), accesses new state-of –the-art collections of models, and performs more sophisticated and complete analysis of Spectral Energy Distributions. We show examples of these capabilities analyzing the Cha I population, paying special attention to the substellar population.

Abstract

SVO Services

Getting a 3D view of Chamaeleon I

By comparing the extinction estimated from SED fitting with the integrated extinction along the line of sight given by methods like the star counts

Av (m

ag) SC

Parameters of BDs in Chamaeleon I

VOSA uses two methodologies: probability analysis of the estimated parameters and χ2 minimization for a general

overview of the fit.

http://svo2.cab.inta-csic.es/svo/theory/vosa