The MALT90 survey of massive star forming regions Ana Duarte Cabral Sylvain Bontemps James Jackson Jill Rathborne Jonathan Foster and the MALT90 consortium MW2011 Rome 19.09.2011

Outline Context and purpose of MALT90 Current status and pilot results The first year of MALT90 Searching for outflows in massive cores: SiO

Context On the light of the large continuum submm surveys Need of a large molecular line legacy towards sites of high-mass star formation capable of: Estimate dynamical distances and understand the Galactic distribution of high-mass star forming clouds Calculate statistical properties and search for chemical and physical evolutionary changes

Survey Millimetre Astronomy Legacy Team 90 GHz (MALT90) Survey, using the 22m Mopra telescope in Australia. PI: James Jackson, Boston University Jill Rathborne, Jonathan Foster Mapping simultaneously 16 molecular transitions at 90GHz, providing a range of high-density tracers. Targeting sites of massive star formation, designed to cover several evolutionary stages, from quiescent to PDRs.

Key specifications Nb of dense cores targeted: 3,000 - Pre-stellar (mid-IR dark) 1,000 - Protostellar (24μm emission) 1,000 - HII Region (bright 8, 24μm emission) 1,000 Angular Resolution: 38’’ Size of each map: 3’ x 3’ Spectral Resolution: 0.11 km/s Sensitivity 0.2 K Survey Region +20° > l > +3° and -3° > l > -60° Dates of data collection Austral winter 2010-2014 Line Frequency (GHz) Tracer N2H+ 93.17 Density, chemically robust 13CS 92.49 Column density H41α 92.03 Ionized gas CH3CN 91.98 Hot core HC3CN 91.19 Hot core 13C34S 90.92 Column density HNC 90.66 Density, cold chemistry HC13CCN 90.59 Hot core HCO+ 89.18 Density HCN 88.63 Density HNCO 41,3 88.24 Hot core HNCO 40,4 87.93 Hot core C2H 87.32 Photo-dissociation SiO 86.85 Shock/outflow H13CO+ 86.75 Column density H13CN 86.34 Column density Line Freq (GHz) Tracer N2H+ J=1-0 93.17 Density, chemically robust 13CS J=2-1 92.49 Column density H41α 92.03 Ionized gas CH3CN 5(1)-4(1) 91.98 Hot core HC3CN J=10-9 1v6 l=1f 91.19 Hot core 13C34S J=2-1 90.92 Column density HNC J=1-0 90.66 Density, cold chemistry HC13CCN J=10-9 90.59 Hot core HCO+ J=1-0 89.18 Density HCN J=1-0 F=1-1 88.63 Density HNCO 4(1,3)-3(1,2) 88.24 Hot core HNCO 4(0,4)-3(0,3) 87.93 Hot core C2HJ=1-0 3/2-1/2 F=2-1 87.32 Photo-dissociation SiO J=2-1 v=0 86.85 Shock/outflow H13CO+ J=1-0 86.75 Column density H13CN J=1-0 F=2-1 86.34 Column density

Current Status Pilot Survey, July09 - (182 targets) - complete Survey strategy Target source list Foster et al. 2011 Year 1, June-Sept10 - (499 targets) - complete ~ 830 hours Observations from Narrabri, Sydney Data released Rathborne et al. in prep Jackson et al. in prep Year 2, May-Sept11 - (~600 targets) - ongoing ~ 900 hours Observations from Narrabri, Sydney, Bordeaux, Moscow, Florida, Boston Mapped ~450 cores so far Logs, observing schedules, source lists available via team wiki Automated data reduction pipeline

Pilot Survey Outcome Source selection using ATLASGAL (870µm) Foster et al. 2011 Source selection using ATLASGAL (870µm) Importance of mapping V.S. pointed observations Importance of spectral resolution (0.1km/s) Schuller et al. 2009

First Year Data available to everyone via the Australia Telescope Online Archive (ATOA: http://atoa.atnf.csiro.au/MALT90) For each source in each line: Raw data Processed cubes Moment maps (zeroth, first, second) Signal-to-noise maps Database of line emission characteristics Peak spectra Temp, VLSR, DV 2-d Integrated emission morphology of emission, location of peak Line ratios, extended or compact, broad line-widths, shocked gas, complex chemistry

products - kinematical distances With the VLSR we can derive a kinematical distance: Galaxy rotation models Reid et al. 2009 Clemens 1985 Extinction maps HI absorption CO clouds Needed for: - Core masses - Protostellar luminosities - Physical relation of adjacent filamentary features - Galactic structure Galactic CO emission (Dame et al. 2001) Galaxy model from Reid et al. 2009

products - Chemical evolution Chemical variations capable of indicating special phases in the core’s chemical evolution Initial collapse (CO freeze out) Dense gas freeze-out Protostar HII region High N2H+ abundance Low N2H+ abundance N2H+ HNC HCO+ HCN N2H+ HNC HCO+ HCN Lee et al. 2004

products - Chemical evolution Hot vs Cold cores

Looking for outflows The expectations Duarte-Cabral, Bontemps, et al. in prep The expectations Statistical study of outflow properties and SiO line profiles Find evolutionary changes on the outflow properties Motte et al. 2007 (0.14 km/s, rms ~ 0.03K) IR bright IR quiet Lopez-Sepulcre et al. 2011 (1.5 km/s, rms ~ 0.009K) vlsr (km/s) Lopez-Sepulcre et al. 2011

Looking for outflows The reality… 235/499 young sources The source sample: 235/499 young sources 129 protostars, 106 quiescent, 156 HII regions, 56 PDRs 30 % SiO detections: 49 % of protostars 20 % of quiescent Velocity binned to 1.3 km/s (rms~ 0.04K).

Looking for outflows Some “not-too-bad” cases

Looking for outflows Some statistics - evolutionary trends?

(ATOA: http://atoa.atnf.csiro.au/MALT90) Future Better distances and SED fittings Understand the real nature of sources and perform (more) meaningful statistics Extension to the full 2000 sources (from quiescent to protostars) Source list worth of follow up with ALMA http://malt90.bu.edu (ATOA: http://atoa.atnf.csiro.au/MALT90)