1. 1 1 CORNISH WORKSHOP Leeds, 13 th April 2007 James Green The Methanol Multibeam Project Project MMB

2. 2 The Methanol Multibeam Project: The Team R. J. Cohen, J. L. Caswell, K. Brooks, M. G. Burton, A. Chrysostomou, P. J. Diamond, S. Ellingsen, G. A. Fuller, M. D. Gray, J. A. Green, M. G. Hoare, M. R. W. Masheder, N. McClure-Griffiths, M. Pestalozzi, C. Phillips, L. Quinn, M. Thompson, M. Voronkov, A. Walsh, D. Ward- Thompson, D. Wong- McSweeney, J. A. Yates R. J. Cohen, J. L. Caswell, K. Brooks, M. G. Burton, A. Chrysostomou, P. J. Diamond, S. Ellingsen, G. A. Fuller, M. D. Gray, J. A. Green, M. G. Hoare, M. R. W. Masheder, N. McClure-Griffiths, M. Pestalozzi, C. Phillips, L. Quinn, M. Thompson, M. Voronkov, A. Walsh, D. Ward- Thompson, D. Wong- McSweeney, J. A. Yates.

3. 3 ParticipantsParticipants

4. 4 The 6.7 GHz Methanol Maser

5. 5 Why MMB? - Previous Surveys

6. 6 MMB 7-Beam Receiver Jointly built by Jodrell Bank and ATNF.Jointly built by Jodrell Bank and ATNF. Hexagonal layout pattern of 7 equal receivers.Hexagonal layout pattern of 7 equal receivers. Capable of dual polarisation over a large bandwidth.Capable of dual polarisation over a large bandwidth. Calibration with noise injection sampled at 500Hz.Calibration with noise injection sampled at 500Hz. Jointly built by Jodrell Bank and ATNF.Jointly built by Jodrell Bank and ATNF. Hexagonal layout pattern of 7 equal receivers.Hexagonal layout pattern of 7 equal receivers. Capable of dual polarisation over a large bandwidth.Capable of dual polarisation over a large bandwidth. Calibration with noise injection sampled at 500Hz.Calibration with noise injection sampled at 500Hz.

7. 7 Survey Characteristics I 4 MHz Bandwidth (  180 km/s at 6668 MHz).4 MHz Bandwidth (  180 km/s at 6668 MHz). Assume 150km/s fully useful bandwidth, so multiple centre velocities toward Galactic centre 10km/s overlap.Assume 150km/s fully useful bandwidth, so multiple centre velocities toward Galactic centre 10km/s overlap. Doppler tracking provided by the first two local oscillators.Doppler tracking provided by the first two local oscillators. Correlator configured to provide 2048 frequency channels across each 4 MHz band, at each line frequency and each polarization.Correlator configured to provide 2048 frequency channels across each 4 MHz band, at each line frequency and each polarization. Velocity resolution 0.09 km/s at 6668 MHz.Velocity resolution 0.09 km/s at 6668 MHz. Spectra dumped every 5 seconds.Spectra dumped every 5 seconds. System noise temperatures ~20 K.System noise temperatures ~20 K. 4 MHz Bandwidth (  180 km/s at 6668 MHz).4 MHz Bandwidth (  180 km/s at 6668 MHz). Assume 150km/s fully useful bandwidth, so multiple centre velocities toward Galactic centre 10km/s overlap.Assume 150km/s fully useful bandwidth, so multiple centre velocities toward Galactic centre 10km/s overlap. Doppler tracking provided by the first two local oscillators.Doppler tracking provided by the first two local oscillators. Correlator configured to provide 2048 frequency channels across each 4 MHz band, at each line frequency and each polarization.Correlator configured to provide 2048 frequency channels across each 4 MHz band, at each line frequency and each polarization. Velocity resolution 0.09 km/s at 6668 MHz.Velocity resolution 0.09 km/s at 6668 MHz. Spectra dumped every 5 seconds.Spectra dumped every 5 seconds. System noise temperatures ~20 K.System noise temperatures ~20 K.

8. 8 Survey Characteristics II HPBW 3.2 arcmin at 6668 MHz and 3.4 arcmin at 6035 MHz.HPBW 3.2 arcmin at 6668 MHz and 3.4 arcmin at 6035 MHz. Beams spaced by 6.46 arcmin on sky.Beams spaced by 6.46 arcmin on sky. Multibeam footprint is 15arcmin across.Multibeam footprint is 15arcmin across. SPOT and MX observations to monitor variation in calibration.SPOT and MX observations to monitor variation in calibration. Blocks of 2 O in l, ±2 O in b.Blocks of 2 O in l, ±2 O in b. Continuous scanning at 0.1 O min - 1.Continuous scanning at 0.1 O min - 1. Optimal Orientation.Optimal Orientation. Beam Sensitivity consistent to ±3.5%.Beam Sensitivity consistent to ±3.5%. HPBW 3.2 arcmin at 6668 MHz and 3.4 arcmin at 6035 MHz.HPBW 3.2 arcmin at 6668 MHz and 3.4 arcmin at 6035 MHz. Beams spaced by 6.46 arcmin on sky.Beams spaced by 6.46 arcmin on sky. Multibeam footprint is 15arcmin across.Multibeam footprint is 15arcmin across. SPOT and MX observations to monitor variation in calibration.SPOT and MX observations to monitor variation in calibration. Blocks of 2 O in l, ±2 O in b.Blocks of 2 O in l, ±2 O in b. Continuous scanning at 0.1 O min - 1.Continuous scanning at 0.1 O min - 1. Optimal Orientation.Optimal Orientation. Beam Sensitivity consistent to ±3.5%.Beam Sensitivity consistent to ±3.5%.

9. 9 Results: An Example Field OBSERVATIONSLIVEDATAGRIDZILLAKVIS/RESULTS

10. 10 Survey Progress Surveyed 106 degrees galactic longitude.Surveyed 106 degrees galactic longitude. Observed 528 masers, of which 218 new.Observed 528 masers, of which 218 new. 53/100 days Parkes observing time.53/100 days Parkes observing time. Most new are weak (S peak < 4 Jy).Most new are weak (S peak < 4 Jy). Narrow linewidths (FWHM < 0.2 km/s).Narrow linewidths (FWHM < 0.2 km/s). Far-side outer Galaxy detections.Far-side outer Galaxy detections. Surveyed 106 degrees galactic longitude.Surveyed 106 degrees galactic longitude. Observed 528 masers, of which 218 new.Observed 528 masers, of which 218 new. 53/100 days Parkes observing time.53/100 days Parkes observing time. Most new are weak (S peak < 4 Jy).Most new are weak (S peak < 4 Jy). Narrow linewidths (FWHM < 0.2 km/s).Narrow linewidths (FWHM < 0.2 km/s). Far-side outer Galaxy detections.Far-side outer Galaxy detections.

11. 11 Observations - regions surveyed (180) (270)(90) (0/360)

12. 12 Observational Distribution l vs b l vs Velocity (LSR) 0

13. 13 Survey Statistics - Galactocentric distances

14. 14 Survey Statistics - Flux distribution MMB Arecibo

15. 15 Excited OH Results L.Quinn Work in progress..Work in progress..

16. 16 ATCA & MERLIN Positioning follow-up: Parkes positions accurate to ± 30 arcsec.Positioning follow-up: Parkes positions accurate to ± 30 arcsec. Capabilities to do it in both hemispheres with ATCA and MERLIN:Capabilities to do it in both hemispheres with ATCA and MERLIN: –ATCA ± 0.1 arcsec –MERLIN ± 0.01 arcsec ATCA observed and positioned all new detections.ATCA observed and positioned all new detections. MERLIN observed ~30 new in 20-30 region, positioned 25.MERLIN observed ~30 new in 20-30 region, positioned 25. Positioning follow-up: Parkes positions accurate to ± 30 arcsec.Positioning follow-up: Parkes positions accurate to ± 30 arcsec. Capabilities to do it in both hemispheres with ATCA and MERLIN:Capabilities to do it in both hemispheres with ATCA and MERLIN: –ATCA ± 0.1 arcsec –MERLIN ± 0.01 arcsec ATCA observed and positioned all new detections.ATCA observed and positioned all new detections. MERLIN observed ~30 new in 20-30 region, positioned 25.MERLIN observed ~30 new in 20-30 region, positioned 25.

17. 17 MERLIN Follow-up Examples D. Wong-McSweeney

18. 18 Pulsar Survey Piggyback Deep integrations through pointed observations conducted as part of the pulsar search program.Deep integrations through pointed observations conducted as part of the pulsar search program. No Doppler tracking.No Doppler tracking. Just Methanol 6668 MHz frequency.Just Methanol 6668 MHz frequency. Correlator configured for 8 MHz over 4096 channels for 7 beams, 2 polarizations.Correlator configured for 8 MHz over 4096 channels for 7 beams, 2 polarizations. Same spectral resolution, but over wider velocity range.Same spectral resolution, but over wider velocity range. Focused on Galactic Centre, but covering -60 < l < +45 (maximum +/- 0.5 in b).Focused on Galactic Centre, but covering -60 < l < +45 (maximum +/- 0.5 in b). Deep integrations through pointed observations conducted as part of the pulsar search program.Deep integrations through pointed observations conducted as part of the pulsar search program. No Doppler tracking.No Doppler tracking. Just Methanol 6668 MHz frequency.Just Methanol 6668 MHz frequency. Correlator configured for 8 MHz over 4096 channels for 7 beams, 2 polarizations.Correlator configured for 8 MHz over 4096 channels for 7 beams, 2 polarizations. Same spectral resolution, but over wider velocity range.Same spectral resolution, but over wider velocity range. Focused on Galactic Centre, but covering -60 < l < +45 (maximum +/- 0.5 in b).Focused on Galactic Centre, but covering -60 < l < +45 (maximum +/- 0.5 in b).

19. 19 Magellanic Clouds Slightly different technique.Slightly different technique. Pointed MX observations as well.Pointed MX observations as well. 1 new Methanol & 1 new excited OH.1 new Methanol & 1 new excited OH. Slightly different technique.Slightly different technique. Pointed MX observations as well.Pointed MX observations as well. 1 new Methanol & 1 new excited OH.1 new Methanol & 1 new excited OH.

20. 20 The Work Plan : 2007-2011 Parkes Multibeam survey till 2008.Parkes Multibeam survey till 2008. ATCA positions, snapshots and 8.4 GHz continuum.ATCA positions, snapshots and 8.4 GHz continuum. MERLIN positions and snapshots.MERLIN positions and snapshots. Distances and Galactic Distribution.Distances and Galactic Distribution. Jodrell Bank Multibeam survey 2008-2010.Jodrell Bank Multibeam survey 2008-2010. MMB catalogue of Milky Way.MMB catalogue of Milky Way. MMB survey of LMC/SMC.MMB survey of LMC/SMC. Simultaneous survey of excited OH 6035 MHz.Simultaneous survey of excited OH 6035 MHz. Methanol deep fields at Pulsar pointings.Methanol deep fields at Pulsar pointings. Parkes Multibeam survey till 2008.Parkes Multibeam survey till 2008. ATCA positions, snapshots and 8.4 GHz continuum.ATCA positions, snapshots and 8.4 GHz continuum. MERLIN positions and snapshots.MERLIN positions and snapshots. Distances and Galactic Distribution.Distances and Galactic Distribution. Jodrell Bank Multibeam survey 2008-2010.Jodrell Bank Multibeam survey 2008-2010. MMB catalogue of Milky Way.MMB catalogue of Milky Way. MMB survey of LMC/SMC.MMB survey of LMC/SMC. Simultaneous survey of excited OH 6035 MHz.Simultaneous survey of excited OH 6035 MHz. Methanol deep fields at Pulsar pointings.Methanol deep fields at Pulsar pointings.

21. 21 MMB-CORNISH Overlap

22. 22 MMB-CORNISH COINCIDENCES

23. 23 MMB-CORNISH COINCIDENCES

24. 24 MMB-CORNISH COINCIDENCES

25. 25 MMB-CORNISH COINCIDENCES 8 Jy 3 Jy 7.5 Jy 4 Jy 1.1 Jy 0.8 Jy 2.6 Jy

26. 26 ConclusionConclusion MMB first full Galactic plane survey.MMB first full Galactic plane survey. 528 detections & counting528 detections & counting MMB-CORNISH overlap looks very promising.MMB-CORNISH overlap looks very promising. MMB first full Galactic plane survey.MMB first full Galactic plane survey. 528 detections & counting528 detections & counting MMB-CORNISH overlap looks very promising.MMB-CORNISH overlap looks very promising.