Revista mexicana de astronomía y astrofísica

 

Statical analysis of molecular line emission from T Tauri disk models

 

Itziar de Gregorio–Monsalvo,¹ Paola D'Alessio,² and José F. Gómez³

 

1 European Southern Observatory, Chile.
Itziar de Gregorio–Monsalvo: European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile (idegrego@eso.org).

2 Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, México.
Paola D'Alessio: Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Campus Morelia, Apartado Postal 3–72, 58090, Morelia, Michoacán, México (p.dalessio@astrosmo.unam.mx).

3 Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain.
José F. Gómez: Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, E–18080 Granada, Spain (jfg@iaa.es).

 

Received 2006 December 04
Accepted 2007 March 12

 

Resumen

En este trabajo modelamos la emisión esperada de la línea molecular C¹⁷O(J=32) en discos protoplanetarios, modificando diferentes parámetros físicos para obtener distintas características observacionales. Nuestra meta es determinar la clase de observaciones que nos permitirán extraer información sobre los parámetros físicos de los discos. Con este propósito realizamos un análisis estadístico de componentes principales y una correlación lineal múltiple en el conjunto de resultados obtenidos a partir de los modelos. Además, presentamos un estudio sobre futuras observaciones de línea molecular en discos protoplanetarios usando SMA y ALMA.

 

Abstract

In this work we model the expected emission from the molecular line C¹⁷O(J=32) in protoplanetary disks, modifying different physical parameters to obtain distinctive observational signatures. Our aim is to determine the kind of observations that will allow us to extract information about the physical parameters of disks. With this purpose we perform a statistical analysis of principal components and a multiple linear correlation on our set of results from the models. We also present prospects for future molecular line observations of protoplanetary disks using SMA and ALMA.

Key Words: ISM: molecules—Methods statical—planetary system:protoplanetary disk—radiative transfer

 

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Acknowledgement

We wish to thank the LAEFF staff for allowing the use of their personal computers to carry out the calculations of the molecular line emission models. PD acknowledges grants from Conacyt and PAPIIT, México. The model calculations were performed in the cluster at CRyA–UNAM acquired with Conacyt grants 36571–E, 47366–F, and UNAM–PAPIIT grant 110606. FG and IdG are supported by Junta de Andalucía grant FQM–1747. JFG also acknowledges partial support from grants AYA2005–08523–C03–03 of the Spanish MEC (including FEDER funds) and TIC–126 of Junta de Andalucía.

 

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