Download - MX002: Molecular Gas in the LMC
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
• the inner LMC
• plans for 2006
Annie Hughes, UNSW 3mm workshop, November 2005
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
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
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
The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
• ridge + arc ~ 35% ridge + arc ~ 35%
of LMC molecular of LMC molecular
gasgas
The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
The Molecular Ridge
Annie Hughes, UNSW 3mm workshop, November 2005
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
XCO factor
Annie Hughes, UNSW 3mm workshop, November 2005
XCO=NH2/ICO NH2 ~R(ΔV)/R2 XCO~ΔV/(RTb)
Analysis by Jorge Pineda & Juergen
Comparison with ASTE
Annie Hughes, UNSW 3mm workshop, November 2005
Analysis by Tony and Yojhi
Comparison with ASTE
Annie Hughes, UNSW 3mm workshop, November 2005
Analysis by Tony and Yojhi
• 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
Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005
Preliminary Results
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
Finally…
Annie Hughes, UNSW 3mm workshop, November 2005
…a huge thank you to everyone involved in the Mopra upgrade!
Appendix
Annie Hughes, UNSW 3mm workshop, November 2005
A Big Mess?
Annie Hughes, PhD Progress Review, November 2005
Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005
Preliminary Results
Annie Hughes, UNSW 3mm workshop, November 2005