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The BIMA Survey of Embedded Cores in the Perseus Molecular Cloud Complex

The BIMA Survey of Embedded Cores in the Perseus Molecular Cloud Complex. The BIMA Embedded Cores Survey was designed to investigate various aspects of early star formation and complement the SIRTF c2d Legacy Project. Proposal approved in Fall 2000; observations completed in Spring 2002.

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The BIMA Survey of Embedded Cores in the Perseus Molecular Cloud Complex

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  1. The BIMA Survey of Embedded Cores in the Perseus Molecular Cloud Complex

  2. The BIMA Embedded Cores Survey was designed to investigate various aspects of early star formation and complement the SIRTF c2d Legacy Project. Proposal approved in Fall 2000; observations completed in Spring 2002. Survey targets: Eighteen embedded cores in the Perseus Clouds, selected from the database of NH3 cores by Jijina, Myers, & Adams 1999. Three additional cores from the survey by Looney et al. NGC 1333: IRAS2, IRAS4, IRAS8, IRAS9, L1448 IRS3 (N, C), L1448 IRS2, L1455 A1, A2, B, C, Per 4N, Per 4S, Per 5, Per 6, Per 7E, Per7W, Per9W, B1S, B5, IRAS 03282+3035 Range of luminosities: ~1L < L < ~200L Range of masses: <1M < M < ~13M

  3. The Perseus Molecular Cloud Complex + + + + + + + + + + + + + + + + + + + The Perseus Molecular Cloud Complex in 13CO (J=1- 0), from Padoan et al. 1999.

  4. Array configurations: B, C, D (angular resolutions of ~2", 6", and 14") Continuum emission and molecular line data: C18O J=1- 0 (109.8 GHz), 13CO J=1- 0 (110.2 GHz). Supplementary observations: with BIMA: N2H+ J=1- 0 (93.2 GHz), H13CO+ J=1- 0 (86.8 GHz) with FCRAO (14m antenna, resolution ~45"): C18O, N2H+

  5. Scientific Objectives for the Key Project data: Examining Envelope Structure: Power law description of mass distribution; robustness of R- 2 dependence found by Looney. Correlation of envelope structure with observed luminosity. Exploring the Extent of Molecular Depletion: Models that reproduce observed C18O line profiles require reduced abundances. Analyzing the Velocity Fields: Few published maps of velocity fields with high spatial resolution. Correlation of angular momentum distribution with stellar multiplicity (revealed by SIRTF). Tracing the Formation of Circumstellar Disks: Looney showed that disks in embedded sources cannot have more mass than the envelope distribution extrapolated to small scales. SIRTF will be sensitive to presence of hot central disks.

  6. 100% of proposed tracks have been observed with passing grades. 100% of datasets have been reduced. 100% of embedded cores have been observed in C18O and N2H+ with the FCRAO 14m antenna. With the 3 pre- Key Project objects (IRAS2, IRAS4, L1448N), the `bottleneck' was determining the optimal method for combining the BIMA and FCRAO observations. The method has now been stream- lined.

  7. Barnard5 IRS1 Colorscale: =3mm emission RMS noise in continuum: 1.4 mJy/bm Contours: C18O (J=1- 0) integrated intensity RMS noise in C18O: ~55 mJy/bm in km/s Plus symbols: 2MASS point sources

  8. NGC1333 IRAS8 NGC1333 IRAS9

  9. North of NGC1333 Per4S Per 5 Per4N

  10. L1455 A1 B A2 C

  11. L1448 IRS2 C

  12. Per9W Barnard1 S I03282 Per6

  13. Inventory NAMEIRAS PSC3mmC18O 2MASS in Pbeam IRAS2 03258+3104 2 y 49 IRAS4 03259+3105 3 y 10 IRAS8 03260+3111 1 (2?) y 36 IRAS9 03262+3114 1 y 23 L1448N 03225+3034 2 y 18 L1448C 1 y 12 L1448 IRS2 03222+3034 2 y 4 L1455A1 03245+3002 2 y 21 L1455A2 03247+3001 0 (weak?) y 25 L1455B 03249+2957 0 (weak?) y 20 L1455C 0 y 16 Per4N 03262+3123 1 y 14 Per4S 1 y 17 Per5 03267+3128 1 y 10 Per6 1 (offset?) n (offset?) 5 Per7E 0 y 2 Per7W 0 y 3 Per9W 0 y 3 B1S 03301+3057 2 y 5 B5 IRS1 03445+3242 1 y 7 I03282 03282+3035 1 y 4

  14. Observations reveal fewer continuum sources than expected. (No rich fields of embedded sources.) Uncertainties in the positions of the IRAS sources persist. These should be dispelled by SIRTF observations.

  15. NGC1333 IRAS2, IRAS4; L1448 N C18O J=1- 0 integrated intensity; BIMA + FCRAO combined; resolution ~10" NGC1333 IRAS2 NGC1333 IRAS4 L1448 N Integrated Intensity (0th moment) Map, contours = 3,6,9,10,11,12 x 0.54 Jy/bm Integrated Intensity (0th moment) Map, contours = 3,6,9,10,11,12,13,14 x 0.35 Jy/bm Integrated Intensity (0th moment) Map, contours = 3,6,8,9,10,11,12,13,14 x 0.46 Jy/bm

  16. NGC1333 IRAS2 intensity map velocity map

  17. L1448 N velocity map intensity map

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