•Millimetre Astronomy Legacy Team • 90 GHz survey MALT 90 James Jackson (Boston University) Kate Brooks, Jill Rathborne (ATNF), Jonathan Foster (Boston U), Gary Fuller (Manchester), Friedrich Wyrowski (MPIfR), and 38 others…. Great Barriers Townsville 2010
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Millimetre Astronomy Legacy Team 90 GHz survey MALT 90 James Jackson (Boston University) Kate Brooks, Jill Rathborne (ATNF), Jonathan Foster (Boston U),
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•Millimetre Astronomy Legacy Team
• 90 GHz survey
MALT 90
James Jackson (Boston University)
Kate Brooks, Jill Rathborne (ATNF), Jonathan Foster (Boston U), Gary Fuller (Manchester), Friedrich Wyrowski
(MPIfR), and 38 others….Great Barriers Townsville 2010
High-mass star formation: dense cores
Giant Molecular
Cloud
OH Masers
CH3OH + H2O Masers
High-massStarHII Region
High-massStar
Pre-UCHII + IRUCHIIHCHII + cm
Hot Molecular Core
mm onlyStarless Core
WarmCompact mid-IR sources4.5 m “green fuzzies”
Protostellar core
ColdDark in the mid- and far-IR
Starless core
Hot Core
Hot H II region embeddedStrong, extended mid-IR emissionStrong 8 m PAH emission
Slide courtesy of Kate Brooks
Image credit: NASA/JPL-Caltech/Univ. of WisconsinBlue - 3.6m, Green - 8m, Red - 24m
1.2 degrees
0.2
degr
ees
Cores in the Nessie Nebula
Image credit: NASA/JPL-Caltech/Univ. of WisconsinBlue - 3.6m, Green - 8m, Red - 24m
Cores in the Nessie Nebula
Cold core
Image credit: NASA/JPL-Caltech/Univ. of WisconsinBlue - 3.6m, Green - 8m, Red - 24m
Cores in the Nessie Nebula
Protostellar core
Image credit: NASA/JPL-Caltech/Univ. of WisconsinBlue - 3.6m, Green - 8m, Red - 24m
Cores in the Nessie Nebula
Stellar “H II region” core
MALT 90: The Millimetre Astronomy Legacy Team 90 GHz Survey MALT 90 will image 3,000 high-mass cores
with Mopra in key 90 GHz molecular lines, e.g. N2H+, HCO+, HCN, HNC…
The survey will be complete: all high-mass star forming cores (M > 200 M) to 10 kpc.
It will provide key information for Herschel and ATLASGAL studies
MALT 90 sources will be key targets for ALMA
ALMA will be able to image any core detected in MALT 90 at 1” angular resolution with excellent signal-to-noise
MALT 90 science goal:How do high-mass star-forming cores evolve?MALT 90 will provide
Kinematic distances Column densities Molecular chemical abundances Virial masses Core kinematics A large sample of the elusive youngest cores
Why 90 GHz ? Molecular lines at ~90
GHz require high densities for their excitation (n > 105 cm-3)
These lines are therefore sensitive ONLY to dense star-forming cores.
Dense core
13CO
C18O
CS
Image credit: NASA/JPL-Caltech/Univ. of WisconsinBlue - 3.6m, Green - 8m, Red - 24m
1.2 degrees
0.2
degr
ees
All of these cores are strong molecular line emitters easily detected by Mopra
Size ~100 pc x 0.5 pc
Mopra HNC (1-0) integrated emissionFor more on Nessie see Jackson et al. 2010
ApJL
The MALT 90 strategy
A blind fully-sampled 90 GHz Galactic plane survey is impractical 90 GHz emission is relatively weak Dense cores have a small solid angle
BUT submm thermal dust emission indicates cores The ATLASGAL 870 m survey of the Galactic
plane has now identified thousands of cores. ATLASGAL sources will be imaged with Mopra in
molecular lines.
ATLASGAL 0.87 mm
Spitzer/MIPS 24 m
Mopra HNC (1-0) integrated emission
Core classification : Spitzer GLIMPSE/MIPSGAL
Pre-stellar Protostellar H II region
Blue 3.6 m Green 8 m, Red 24 m Spitzer: GlIMPLSE?MIPSGAL
The primary goal of the MALT 90 GHz Survey is to characterize star-forming cores and to study their physical and chemical evolution
MALT 90 Survey Observing Parameters16 lines
3’ x 3’ maps
Two orthogonally scanned “on-the-fly” maps for each source