No need for spectroscopy in PMS star mass determinations

Details No need for spectroscopy in PMS star mass determinations No need for spectroscopy in PMS star mass determinations

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..175s&link_type=abstract

XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S

Astronomy and Astrophysics

Astronomy

Scientific paper

The problem of mass determinations of PMS stars requires the placement of each star on a temperature - luminosity diagram with evolutionary tracks. However, to determine the temperature one usually needs to know the spectral type obtained through spectroscopy, because the colors are affected by reddening from extinction and from the presence of a dusty circumstellar disk. We have found that the disk reddening can be represented by a vector, similar to the interstellar extinction one, and it is thus possible to de-redden both contributions from JHK photometry only. The method uses color-color and color-magnitude diagrams transformed to a space where extinction and disk reddening are the base of the diagrams. They are called reddening principal vectors RPV.
We have tested this method on T-Tauri low mass stars with masses known from dynamical methods. Of the 14 objects in the dynamical sample we were able to recover the mass (< 3 σ ) of 12 at the canonical age of 10^{6.3} yrs. If we relax the age assumption, we are able to find matching masses for all the objects, with ages that disperse from the canonical in acceptable amounts. We also tested the method on the individual components of the multiple sysytems in our dynamical sample with excellent results.
This new method to determine the mass of PMS stars from NIR photometry only, will greatly increase the amount of available data for initial mass function studies in the milky way and in other galaxies.

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