Millimeter Interferometer Mosaics of Clusters in Formation

Details Millimeter Interferometer Mosaics of Clusters in Formation Millimeter Interferometer Mosaics of Clusters in Formation

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999alma.confe..14d&link_type=abstract

Science with the Atacama Large Millimeter Array (ALMA), Associated Universities, Inc., held October 6-8, 1999 at Carnegie Instit

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Protoclusters, Clusters, Mosaic, Formation

Scientific paper

Stars form typically in clusters, in short time intervals (less than or equal to 1 Myr) and in small (less than or equal to 0.5 pc) regions of turbulent dense gas (e.g., see Lada, Strom, & Myers 1993). Millimeter interferometers can now provide wide-field, high-resolution observations of protoclusters, where objects are typically too proximate and embedded to observe by other means. Following Testi & Sargent (1998), who mosaicked the Serpens NW+SE protocluster at OVRO, we have observed mosaics of other regions with high surface densities of protostellar objects including the NGC 1333 IRAS 4 region in Perseus (at the IRAM PdBI), the rho Oph A region of Ophiuchus (at BIMA, with P. André), the L1551 IRAS 5 region in Taurus (at BIMA), and the OMC-2 region in Orion (at OVRO). Continuum mosaics at lambda = 3.2 mm were made alongside line mosaics of N2H+ (1-0), a dense gas tracer of quiescent material that avoids confusion from outflow motions. These maps will provide data on relative spacings, masses, and velocities that address key issues in cluster formation, and demonstrate a compelling future scientific programme for ALMA. Lada, E. A., Strom, K., & Myers, P. C. 1993, in "Protostars and Planets III", ed. E.H. Levy, J. Lunine, & M. S. Matthews, (University of Arizona Press: Tucson), p. 245 Testi, L., & Sargent, A. I. 1998, ApJ, 508, L91

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