mx002: molecular gas in the lmc
DESCRIPTION
MX002: Molecular Gas in the LMC. MX002 observers in 2005: Juergen Ott, Tony Wong, Erik Muller, Jorge Pineda, Min Wang, Annie Hughes. Talk Outline. the MX002 project observations in 2005 the molecular ridge near 30 Doradus: mass function, X-factor, line profiles, ASTE/Mopra - PowerPoint PPT PresentationTRANSCRIPT
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MX002: Molecular Gas in the LMC
MX002 observers in 2005:
Juergen Ott, Tony Wong, Erik Muller,
Jorge Pineda, Min Wang, Annie Hughes
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Talk Outline
• the MX002 project
• observations in 2005
• the molecular ridge near 30 Doradus:
mass function, X-factor, line profiles,
ASTE/Mopra
• the inner LMC
• plans for 2006
Annie Hughes, UNSW 3mm workshop, November 2005
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MX002 Overview
1212CO(J=1-0) survey of the Magellanic CO(J=1-0) survey of the Magellanic
System (LMC+SMC+MB)System (LMC+SMC+MB)
Scientific MotivationsScientific Motivations• Molecular cloud formation and evolutionMolecular cloud formation and evolution
• Initial stages of star formationInitial stages of star formation
• Low-Z, high-UV replicates high-z conditionsLow-Z, high-UV replicates high-z conditions
Annie Hughes, UNSW 3mm workshop, November 2005
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MX002 Overview
Why the LMC?Why the LMC?• unique opportunity for southern telescopesunique opportunity for southern telescopes
• low metallicity ~0.3Zlow metallicity ~0.3Z, emulating conditions at , emulating conditions at
high-zhigh-z
• high angular resolution + overview of high angular resolution + overview of
dynamics in whole galaxydynamics in whole galaxy
• existing HI datasetexisting HI dataset
• 30 Doradus - an exciting molecular gas 30 Doradus - an exciting molecular gas
laboratory!laboratory!
Annie Hughes, UNSW 3mm workshop, November 2005
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Observation Strategy
• OTF mapping ~120 5’x5’ fieldsOTF mapping ~120 5’x5’ fields• CO(J=1-0) (115.271 GHz)CO(J=1-0) (115.271 GHz)• mostly old correlator/RXmostly old correlator/RX• ~100 minutes per field~100 minutes per field• BW~64 MHzBW~64 MHz• ΔΔv= ~0.16 km/sv= ~0.16 km/s • RMS~0.4 KRMS~0.4 K• beam FWHM ~ 30”beam FWHM ~ 30”• Tsys @115 GHz ~600 KTsys @115 GHz ~600 K• mostly extragalactic “green-time”mostly extragalactic “green-time”
Annie Hughes, UNSW 3mm workshop, November 2005
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The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
• ridge + arc ~ 35% ridge + arc ~ 35%
of LMC molecular of LMC molecular
gasgas
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The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
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The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
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The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
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The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
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Clump Mass Spectrum
Annie Hughes, UNSW 3mm workshop, November 2005
MVIR~R(ΔV)2, dN/dMVIR M
α ~ 1.5 α ~ 1.6
Analysis by Jorge Pineda & Juergen
MW α = 1.6-1.8, NANTEN LMC α = 1.9
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XCO factor
Annie Hughes, UNSW 3mm workshop, November 2005
XCO=NH2/ICO NH2 ~R(ΔV)/R2 XCO~ΔV/(RTb)
Analysis by Jorge Pineda & Juergen
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Comparison with ASTE
Annie Hughes, UNSW 3mm workshop, November 2005
Analysis by Tony and Yojhi
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Comparison with ASTE
Annie Hughes, UNSW 3mm workshop, November 2005
Analysis by Tony and Yojhi
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• central R~1.2 kpc
• relationship
between atomic
and molecular gas,
focusing on
pressure and
dynamics
• includes star-
forming and non-SF
clouds
Inner LMC Survey
Annie Hughes, UNSW 3mm workshop, November 2005
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Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005
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Preliminary Results
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Plans for 2006+
Annie Hughes, UNSW 3mm workshop, November 2005
• molecular ridge mapping is complete
• continue inner LMC mapping
• Mopra follow-up 3mm multi-line survey
of ridge clouds to investigate physical
parameters as function of the UV
radiation field
• ATCA follow-up of ridge clouds
• NANTEN2/ASTE/APEX
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Finally…
Annie Hughes, UNSW 3mm workshop, November 2005
…a huge thank you to everyone involved in the Mopra upgrade!
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Appendix
Annie Hughes, UNSW 3mm workshop, November 2005
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A Big Mess?
Annie Hughes, PhD Progress Review, November 2005
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Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005
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Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005