1. The Maryland-Magellan Tunable Filter S. Veilleux (U. Maryland) http://www.astro.umd.edu/~veilleux/mmtf Magellan = Arizona, Carnegie, Harvard, Michigan, MIT + Chile

2. PLAN  General principles  Prototype: TTF (Taurus Tunable Filter)  Description  Science  MMTF  Description  Commissioning  Science  Outlook

3. Optical Fabry-Perot Interferometer Etalon: two parallel flat semi- transparent mirrors separated by a fixed distance L This system acts as a narrow- band filter, producing concentric rings at each wavelength m = 2  L cos  2 mono ~ 2 / (N m) (N = finesse) (m = few – 150)

4. Etalon

5. Fabry-Perot Techniques  The etalon is scanned over a range of spacings to build up a spectral data cube over a narrow spectral interval (~ 50 – 100 Å).  Produces complete kinematic maps of line-emitting region: 10,000 – 100,000 spectra !  Sensitivity: ~ 10 -17 erg s -1 cm -2 arcsec -2 (  m ~ few cm -6 pc ~ few R) 3D Spectral Imaging x y L

6. Search for Starburst-Driven Winds Star-forming disk has [N II] 6583/H  < 1 Shocked wind material has [N II] 6583/H  > 1 (SV & Rupke 2002) [N II] 6583/H  H  6563 [N II] 6583 [N II] / H  1 kpc DiskWind NGC 1482 TTF Imaging

7. 5 kpc “Zone of Influence” of Winds in Local Starbursts Warm ionized gas from superwinds has been detected out to ~ 10 – 30+ kpc from the nucleus [bounded by sensitivity of instrument] NGC 1482: H  + [N II] + X-rays 12 kpc wind disk 10 kpc [NII]/H  NGC 1482 (SV, et al. 2003)

8. “Zone of Influence” of AGN–driven Winds AGN-driven winds clear out path for ionizing radiation  “ionization cones” on large scale (Optical: SV et al. 2003; HI: Brinks 2003; X-ray: Young, Wilson, & Shopbell 2001) NGC 1068 log(H  ) + HI 21-cm 10 kpc N N log([O III]) + X-rays 10 kpc

9. The Maryland-Magellan Tunable Filter S. Veilleux (U. Maryland) June 2006: First light! NGC 4945 Hα http://www.astro.umd.edu/~veilleux/mmtf

10. Maryland-Magellan Tunable Filter ( )  PI: S. Veilleux (U. Maryland)  Co-PIs: J. Bland-Hawthorn (USyd), A. Dressler (OCIW), M. Rauch (OCIW), & S. Vogel (U. Maryland)  Co-Is: B. Bigelow (OCIW / U. Michigan), M. McDonald (Maryland), D. Rupke (Maryland), P. Shopbell (Caltech), B. Sutin (OCIW/Skewray), I. Thompson (OCIW), B. Weiner (Arizona), & R. Weymann (OCIW)  Additional Technical Support (OCIW): A. Bagish, C. Birk, T. Hare, D. Osip, F. Perez, A. Uomoto  Funding Agency: NSF/ATI (instrument), NSF/EXC (science) Tunable filter for IMACS on the Baade 6.5m telescope with wavelength coverage ~ 5000 – 9200+ Å, bandwidth ~ 6 – 20 Å, and FOV ~ 27

11. Resolution versus FOV R FOV 10 5 10 6 100 1000 MMTF Others

12. MMTF: Schedule  August 15, 2003: NSF/ATI Award notification

14. Shipment: End-Result of Attempt #1

15. MMTF: Schedule  August 15, 2003: NSF/ATI Award notification  June 2006: Commissioning & first light  Semester 07A: PI instrument  Semester 09A: Facility instrument

16. MMTF: Description  Host instrument: IMACS FOV: 27 DIQ: ~ 0.4 – 0.7  CCD: 8 x SITe ST-002A 2048 x 4096 x 15  m pixels  Low-order Fabry-Perot etalon: Etalon: IC Optical Systems ET- 150-FS-100, 150 mm, /100 Finesse: ~ 30 (effective) Broad-band coating: ~ 5000 – 9200+ Å Bandwidth: ~ 6 – 20 Å Monochromatic FOV: ≤ 12' @ 6600 Å  Electronic controller: T-stabilized & remote-controlled  Order-blocking filters (R ~ 30)

17. MMTF: Description  Host instrument: IMACS FOV: 27 DIQ: ~ 0.4 – 0.7  NEW CCD: 8 x E2V 2048 x 4096 x 15  m pixels  Low-order Fabry-Perot etalon: Etalon: IC Optical Systems ET- 150-FS-100, 150 mm, /100 Finesse: ~ 30 (effective) Broad-band coating: ~ 5000 – 9200+ Å Bandwidth: ~ 6 – 20 Å Monochromatic FOV: ≤ 12' @ 6600 Å  Electronic controller: T-stabilized & remote-controlled  Order-blocking filters (R ~ 30)

18. New CCD

20. Etalon ET-150

23. MMTF: Observing Modes  Mode #1: stare mode fixed-gap narrow-band imaging over whole FOV  Mode #2: gap scanning mode low-resolution data cube  Mode #3: charge shuffling & frequency switching mode The charges on each CCD are shuffled up and down at the same rate that the etalon plates are scanned between two / three discrete gap positions FOV ~ 2 x 4.5 x 27 ~ 250 Need two telescope nods of  4.5 for contiguous FOV Mode #2Mode #3

24. Commissioning (June 2006)

25. Successful Commissioning (June 2006) !

26. MMTF Science Commissioning & March ‘07 Emission-line study of galactic nebulae Deep multi-line imaging of nearby galaxies Survey of emission-line galaxies in clusters & superclusters at intermediate redshifts Survey of emission-line galaxies in the field at high redshifts Search for damped Lyα galaxies along l.o.s to high- redshift QSOs

27. MMTF Commissioning  900-sec Hα “snapshot”  Full Moon! NGC 4945 ┼ N E

28. MMTF Commissioning  900-sec Hα “snapshot”  Full Moon! Cen A ┼ N E

29. MMTF Commissioning Cen A  900-sec [N II] λ6583 “snapshot”  Full Moon! ┼ E N N

30. MMTF Commissioning Cen A jet  900-sec “snapshot” of jet in Hα  Full Moon! ← 145” → ← 170” → 60’’ = 1 kpc ┼ E N

31. Cen A  FUV GALEX + R-band → Jet-induced star formation  Recently: Deep emission line maps to compare with GALEX data N ┼ E (Cackett et al.)

32. MMTF Commissioning  NGC 1313 –SB(s)d –z = 0.0016 –[N II] / Hα = 0.1 → 0.7 HαHα [N II] [N II]/Hα 0 1 ← 280” → (Weiner et al.) [Veilleux et al. 1999] ┼ N E ← 780” →

33. Emission-Line Imaging of Nearby Galaxies  NGC 5713 –SAB(rs)bc pec –z = 0.0063 –SINGS galaxy –10 + 20 min –[N II] / Hα = 0.3 → 0.7 10 HαHα[N II] [N II]/Hα ← 140” → (Weiner et al.) ┼ N E ← 300” →

34. MMTF Science  Surveys of emission-line galaxies (& nebulae) at low- and high-z in the field, cluster, supercluster environments 5-σ sensitivity (2” aperture): ~ 1 x 10 -17 erg s -1 cm -2 in 1 hr @ 6600 Å 0 0.5 1.0 1.5 2.0 10 Mo/yr 1 Mo/yr 10 Mo/yr 1 Mo/yr 0.1 Mo/yr 10 Mo/yr Galaxy 1 Mo/yr LMC 0.1 Mo/yr SMC –18 –16 –14 –12 [O II] Ly 

35. Cooling Flow Clusters  object (McDonald et al.)

36. Cooling Flow Clusters  object (McDonald et al.)

37. Supercluster @ z = 0.73 in the COSMOS Field  object (Scoville et al. 2007)

38. “Tomography” of z = 0.73 Supercluster in the COSMOS Field ~15 minutes / slice x 14 slices (Veilleux et al.)

39. “Tomography” of Galaxy Clusters  RCS 1450+0840 –[O II] λ3727 –z = 0.765 –15 minutes / slice x 10 slices (Dressler et al.)

40. Damped Lyα Galaxies  DLA: –z = 4.38 → λ = 6543.8 Å –FWHM ~ 9 Å –Factor 5x reduction in QSO light –No 3-σ detection within 1 ” ~2 x 10 -18 erg s -1 cm -2 SFR < 0.6 M sun / yr (~LMC) 56 kpc  QSO 1202-0725: –z = 4.7 (Rauch & Becker)

41. Search for Lyα Galaxies at z = 5.7  COSMOS Field –λ = 8200 Å filter –3-sigma, 1” aperture: ~ 5 x 10 -18 erg s -1 cm -2 –Filter out of focus in austral winter! →Wait for new CCD on f/2 camera (Martin, Dressler et al.) ← ~ 180” →

42. MMTF: Science  Emission-line imaging of galactic nebulae  Deep multi-line imaging of nearby galaxies  Survey of emission-line galaxies & nebulae at low- and high-redshifts in the field, cluster and supercluster environments PI Instrument: 9 programs, 16 nights http://www.astro.umd.edu/~veilleux/mmtf 5-σ sensitivity (2” aperture): ~ 1 x 10 -17 erg s -1 cm -2 in 1 hr @ 6600 Å

43. http://www.astro.umd.edu/~veilleux/mmtf

48. MMTF Proposals & collaborations welcome!