The Red MSX Source Survey

1
The Red MSX Source Survey
Melvin Hoare University of Leeds

• RMS Team
• Stuart Lumsden, Rene Oudmaijer, James Urquhart,
  Ant Busfield, Tamara King, Andrew Clarke (Leeds)
• Toby Moore, James Allsopp (Liverpool JMU)
• Cormac Purcell, Michael Burton (UNSW)
• Zhibo Jiang (PMO)

2
Outline

• Introduction
• The need for large systematic samples
• The RMS Survey
• Galaxy-wide survey for massive YSOs
• Progress and Initial Results
• Conclusions
• Next generation galactic plane surveys

3
Massive Young Stellar Objects

• Luminous (gt104 L), embedded IR source
• Bipolar outflow
• Often has masers
• Compact, ionised wind
• IR emission lines from wind (and disc?)
• Well known examples number in the tens

GL 2591 JHK
4
Evolutionary Outline

• Hot Core à YSO à UCHII à OB Star
• SED
• Sub-mm à Mid-IR à Near-IR à Visual
• Masers
• CH3OH à H2O à OH
• Radio
• No radio à Weak Radio à Strong Radio

5
Surveys for MYSOs

• Too obscured in near-IR
• Radio continuum too weak
• No single maser transition always present
• Molecular cores do not necessarily contain YSOs
• Need to use IR where bulk of energy emerges
• IRAS-based searches suffer from confusion

6
The MSX Galactic Plane Survey

• 8, 12, 14 and 21mm, 18² resolution, blt5o
• Colour-select together with 2MASS data
• Delivers 2000 candidates

W75 N Region
7
Massive YSOs
C stars
UCHII regions
OH/IR stars
PN
8
Multi-wavelength Ground-based Follow-up Campaign

• Identify and eliminate confusing sources
• Generate sample of UCHII regions
• Begin characterisation of the genuine massive YSOs

9
Radio Continuum

• Identify UCHIIs and PN
• 5 GHz, 1² resolution at VLA ATCA
• 2000 objects observed - complete

Compact H II Region
Massive YSO candidate
10
Mid-IR

• Identify UCHIIs and MYSOs in close proximity
• 10mm, 0.8² resolution at UKIRT and ESO 3.6m, 470
  objects observed GLIMPSE

11
Millimetre lines

• Identify nearby low-L YSOs, evolved stars
• 13CO at Mopra, Onsala, JCMT, PMO GRS
• 1900 targets observed
• Resolving distance ambiguities with H I
• See poster 21 by Busfield

12
Near-IR

• Identify remaining evolved stars
• K-band imaging at UKIRT ANU 2.3m 2MASS
• 400 targets observed
• HK band spectroscopy at UKIRT
• 120 targets observed

13
(No Transcript)
14
Example

• L 5 x 104 L, d 11 kpc
• Radio quiet (lt 1 mJy)

15
GLIMPSE
Triggered by SNR? (Slane et al. 1999)
2MASS
16
Statistical Studies

• Luminosity function of MYSOs and UCHIIs (RG,
  environment)
• Lifetime of MYSO phase (L)
• Clustering of MYSOs and UCHIIs
• Triggering by UCHIIs, OB stars, SNRs
• RMS is wide, shallow counterpart the narrower and
  deeper GLIMPSE survey

17
Conclusions

• The RMS survey will deliver 500 massive YSOs
  over the whole galaxy
• Allow the systematic investigations of e.g.
• Infall/outflow with ALMA/CARMA
• Accretion/winds with VLT(I), Gemini, MROI
• Jets/equatorial winds with e-MERLIN/EVLA
• Sample will be available at www.ast.leeds.ac.uk/RM
  S

18
Next Generation Plane Surveys

• Deeper and higher spatial resolution
• Complete wavelength coverage
• Common areas
• Matched sensitivities and resolutions
• GLIMPSE is the starting point

19
(No Transcript)
20
H II region MYSO