Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud

Details Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud Low Mass Star Formation at Low Metallicity: Accretion Rates of Pre-Main Sequence Stars in the Large Magellanic Cloud

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9870r&link_type=abstract

HST Proposal ID #9870

Computer Science

Hst Proposal Id #9870 Stellar Populations

Scientific paper

As part of an ongoing effort to characterise the process of star formation at low metallicity, we propose to measure by means of U-band excess the current accretion rate for a homogenous sample of newly-born stars in NGC 1850, a young {5 Myr} stellar cluster in the LMC. Clearly, at this age most of the accretion has already taken place and its intensity is declining with respect to the earliest stages of formation. However, a comparison with Galactic Pre-Main Sequence stars of the same age immediately leads to assessing the relative strength of accretion when the metallicity is decreased by a factor of three. We have already analysed the images available in the archive for these fields and we have determined the basic parameters {effective temperature and luminosity} for all of the stars down to a mass of 0.9 Mo. To take the next step and determine the current accretion rate we only need WFPC2 imaging of NGC 1850 in the F336W passband. With three orbit worth of observations, we will reach m{F336W} 23 with an accuracy of 0.1 mag. In spite of their unique scientific potential, the data we apply for are relatively inexpensive to gather, as they are the last missing tile of a large dataset already available in the HST archive.

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