Multi-wavelength imaging of circumstellar disks in the Orion Nebula

Details Multi-wavelength imaging of circumstellar disks in the Orion Nebula Multi-wavelength imaging of circumstellar disks in the Orion Nebula

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7367m&link_type=abstract

HST Proposal ID #7367

Computer Science

Hst Proposal Id #7367 Young Stars And Circumstellar Material

Scientific paper

We will use STIS and NICMOS to obtain multi-wavelength images of a sample of circumstellar disks seen as silhouettes against the bright emission-line background of the Orion Nebula. These new data will greatly complement our pending Cycle 6 WFPC2 study, where the disks will be observed at 6565 Angstroms {H Alpha}. In Cycle 7, we will make use of the newly available instruments to obtain images for all disks at 3727 Angstroms {[OII]} and 5007 Angstroms {[OIII]} using STIS, and at 1.876 microns {Pa Alpha} using NICMOS for two of the disks. The combined Cycle 6 and 7 data will provide unprecedented spatial resolution imaging of the disks {at [OII], 20 AU, compared to disk sizes 50-1000 AU diameter}, across an extended wavelength range, allowing us expand our sensitivity to disk surface density by an order of magnitude. Therefore, we will be able to examine the radial structure of the disks in great detail, and over a wide spatial extent. Results from our Cycle 4 WFPC2 imaging program indicate that the disks are truncated at their outer edges: the new data will allow us to examine this truncation and the inner disk radial profile in much greater detail, and therefore provide strong observational constraints on the putative truncation mechanism. We will also obtain deep near-IR continuum images of the edge-on disk Orion 114-426 in order to detect the central star directly, or at least place a much stronger lower limit on the line-of-sight extinction towards it, and thus also on the total disk mass. Finally, long-slit spectroscopy of the reflection nebula in the edge-on disk Orion 114-426 will be obtained in order to indirectly spectrally type the hidden central star.

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