The BIMA Survey of Embedded Coresin the Perseus Molecular Cloud Complex

The BIMA Embedded Cores Survey was designed toinvestigate various aspects of early star formation andcomplement 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 databaseof NH

3 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 < ~200LRange of masses: <1M < M < ~13M

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

The Perseus Molecular Cloud Complex

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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: N

2H+ J=1- 0 (93.2 GHz), H13CO+ J=1- 0 (86.8 GHz)

with FCRAO (14m antenna, resolution ~45"): C18O, N2H+

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.

100% of proposed tracks have beenobserved with passing grades.

100% of datasets have been reduced.

100% of embedded cores have beenobserved in C18O and N

2H+ with the

FCRAO 14m antenna.

With the 3 pre- Key Project objects(IRAS2, IRAS4, L1448N), the`bottleneck' was determining theoptimal method for combiningthe BIMA and FCRAO observations.The method has now been stream-lined.

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

NGC1333 IRAS9

NGC1333 IRAS8

North of NGC1333

Per 5

Per4N

Per4S

L1455

A1

A2

B

C

L1448IRS2C

Per6

Barnard1 S

I03282

Per9W

InventoryNAME IRAS PSC 3mm C18O 2MASS in PbeamIRAS2 03258+3104 2 y 49IRAS4 03259+3105 3 y 10IRAS8 03260+3111 1 (2?) y 36IRAS9 03262+3114 1 y 23L1448N 03225+3034 2 y 18L1448C 1 y 12L1448 IRS2 03222+3034 2 y 4L1455A1 03245+3002 2 y 21L1455A2 03247+3001 0 (weak?) y 25L1455B 03249+2957 0 (weak?) y 20L1455C 0 y 16Per4N 03262+3123 1 y 14Per4S 1 y 17Per5 03267+3128 1 y 10Per6 1 (offset?) n (offset?) 5Per7E 0 y 2Per7W 0 y 3Per9W 0 y 3B1S 03301+3057 2 y 5B5 IRS1 03445+3242 1 y 7I03282 03282+3035 1 y 4

Observations revealfewer continuum sourcesthan expected.(No rich fields ofembedded sources.)

Uncertainties in thepositions of the IRASsources persist. Theseshould be dispelledby SIRTF observations.

NGC1333 IRAS2, IRAS4; L1448 NC18O J=1- 0 integrated intensity;

BIMA + FCRAO combined;resolution ~10"

Integrated Intensity (0th moment) Map,contours = 3,6,8,9,10,11,12,13,14

x 0.46 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 = 3,6,9,10,11,12

x 0.54 Jy/bm

NGC1333 IRAS2 NGC1333 IRAS4 L1448 N

NGC1333 IRAS2

intensity map velocity map

L1448 N

intensity map velocity map