3rd SONG Workshop – 1 April 2010 Prelude: The MUSICOS Before the SONG James E. Neff College of Charleston I.MUSICOS: The Consortium II.The MUSICOS Campaigns III.Results and Lessons Learned IV.Implications for SONG

3rd SONG Workshop – 1 April 2010 Formation of MUSICOS ( MUlti-SIte COntinuous Spectroscopy) Experience with arranging international observing campaigns in support of IUE mission –photometry generally successful, but –spectroscopy from multiple sites never was 1st MUSICOS Workshop (June Meudon) –Concluded that advancement in several scientific areas could be advanced by... –global coverage with 2-m telescopes –spectroscopy with R > 30,000

3rd SONG Workshop – 1 April 2010 There were enough telescopes, but not enough spectrographs, so... –design and build bench-mounted, fiber-coupled spectrograph(s) that could be easily and cheaply duplicated –locate them in critical sites (Hawaii & China)

3rd SONG Workshop – 1 April 2010 The scientific areas identified were... –magnetic activity (surface structure and flares) –stellar winds –stellar oscillations But any phenomenon variable on timescales ~1/2 to several days had been poorly explored Initially, use existing “ISIS” spectrographs and transport them to these two sites for campaigns –begin construction of MUSICOS spectrographs

3rd SONG Workshop – 1 April 2010 First Campaign: MUSICOS 89 Combine 3 scientific programs, 3 nights each... –Non-Radial Pulsations of Be Star [Hubert] –Corotating Interaction Regions of Ae Star [Catala] –Doppler Imaging and Flares of RS CVn Star [Foing] Main Network: –Xinglong 2.2m with ISIS s/g –U. Hawaii 2.2 m with ISISbis s/g –McMath-Pierce 1.5m Telescope with stellar s/g –OHP 1.52m with Aurelie s/g Supporting Network: IUE, Crimea, CFHT, ESO/CAT, Lick, photometry from many sites

3rd SONG Workshop – 1 April % duty cycle for 2 programs, <50% for other 2 nd MUSICOS Workshop March 1990 in Meudon –discussed lessons learned –discussed data reduction issues –re-assigned scientific responsibilities –selected programs for next MUSICOS campaign 3 principal scientific papers with all participants as co-authors (2-part author list) Reduced data available to entire consortium for more detailed analysis papers with subset of authors contributing directly to that work

3rd SONG Workshop – 1 April 2010 The MUSICOS 92 CAMPAIGN 3 programs, 4 nights each, in succession –Pulsations of  2 Tau [Kennelly & Walker] –Winds/Chromsophere of AB Aur [Bohm & Catala] –Imaging Magnetic Activity of HR 1099 [Neff & Simon] Main Network: –Xinglong 2.2m with ISIS s/g –U. Hawaii 2.2 m with MUSICOS s/g (7 nights) –McMath-Pierce 1.5m telescope with stellar s/g –Penn State 1.6m telescope with fiber-fed echelle s/g –WHT 4.2m telescope with Utrecht echelle s/g (4 nights) –OHP 1.52m with Aurelie s/g Supporting Network: IUE, KPNO 2.1m, Penn State, ESO, AAT, Lowell SSS, VLA, photometry and radio: many sites

3rd SONG Workshop – 1 April 2010 Line profile variations (left) Window functions (right) Xinglong, OHP, WHT, NSO Kennelly et al (A&A 313, 571) note different sampling, resolution, S/N

3rd SONG Workshop – 1 April 2010 Radial velocity variations of  2 Tau during MUSICOS 92 campaign (Kenelly et al.)

3rd SONG Workshop – 1 April 2010 Evolution of MUSICOS Campaigns – programs, 13 nights, 3 southern sites – programs, 17 nights, 5 primary sites – Programs, 24 nights, 8 primary sites –began interleaving programs that did not require strictly continuous observations Workshops –3rd: May 1993 at ESTEC –4th: June 1994 in Beijing –5th: September 1995 in St. Andrews –6th: 1997 in Garching –7th: June 2000 at ESTEC

3rd SONG Workshop – 1 April 2010 Summary of Results 5 successful campaigns, 19 scientific programs –duty cycles typically 80% –always enough observations to produce something new from each program/campaign, though not always what was anticipated ~20 primary and many secondary papers –initially primary papers had same main title –but this broke down eventually, so it’s hard to tell exactly how many papers were produced or how frequently they were cited

3rd SONG Workshop – 1 April Pulsations –48 Per,  2 Tau,  Dor, V480 Tau,  Per,  Ori –Be,  Sct, O7.5 III, early F, supergiant w/ NS –radial velocity and profile variations –multiple periods 2.Doppler Imaging, Flares, Activity –HR 1099 (3X), EI Eri, AB Dor, SU Aur, AB Aur –but these provide only a “snapshot” of the morphology; it varies from year to year, but on what intermediate timescales? 3.Winds and Circumstellar Environment –AB Aur,  Per,  Ori,  Ori,  Ori

3rd SONG Workshop – 1 April 2010 Implications for SONG Yes, it is possible, with a heroic effort, to obtain continuous high-resolution spectroscopy with existing sites. Capability severely limited by –Inhomogeneity of instruments –Complexity of data analysis –Coordination of large number of partners –“A chain is only as strong as its weakest link” Existing instruments CAN NOT satisfy the requirements that drive SONG

3rd SONG Workshop – 1 April 2010 But the SONG network optimized for precision radial velocity variations CAN enable many other scientific programs –most Doppler Imaging candidates are bright enough –there has been virtually no probing of intermediate timescales corresponding to starspot evolution The conclusion of everyone involved with MUSICOS was that we need: a global, centrally-managed network of homogeneous automated spectroscopic telescopes. In a word: SONG