1. nigel douglas university of groningen nigel douglas university of groningen measuring kinematics in elliptical galaxies measuring kinematics in elliptical galaxies

2. (spiral) galaxy dynamics neutral gas (stars, H II regions) Braun 2002

3. rotation curve decomposition RotCurve (cwru.edu)

4. early-type galaxy dynamics stellar spectroscopy Statler et al 99

5. IFU (integral field unit) Oosterloo priv comm

6. discrete tracers of kinematics globular clusters satellites PNe stars globular clusters satellites PNe stars

7. stellar streams Ibata et al. 2004

8. PNe easy to detect easy to measure radial velocity linewidth  21 km/s ubiquitous at  2.5  20 per 10 9 L B e.g. 750 for NGC 3379

9. PNe v stars by assumption PNe follow stars how true is this? PNe age and population synthesis

10. techniques for acquiring PNe radial velocities: imaging+spectroscopy perot-fabry slitless spectroscopy

11. imaging + spectroscopy ngc 5128 Hui, Ford, Ciardullo, Jacoby 1993 Hui, Ford, Freeman, Dopita 1995 Peng, Ford, Freeman 2004

12. fabry-perot ngc 3384 Tremblay, Merritt, Wiilliams 1995 68 PNe

13. slitless spectroscopy: the PN spectrum

14. Slitless spectroscopy(1) trials at AAT 1995 slitless spectroscopy NGC 5128

15. Slitless spectroscopy(2) cf Hui et al 1995 24 PNe compared cf Hui et al 1995 24 PNe compared

16. Slitless spectroscopy(3) Fehrenbach 1947 Douglas & Taylor 1999 Fehrenbach 1947 Douglas & Taylor 1999

17. CDI at WHT: M94 modified ISIS 1997-2001 NGC 7457 NGC 5866 Douglas et al. 2000

18. M B = -19.8 D = 10.5 Mpc UT1 + FORS1 1999/2000 14 hrs: 535 PN to 3 R eff CDI at VLT: NGC 4697 Méndez et al. 2001

19. Bibliography: PNe velocities with slitless spectroscopy CDI (rotating spectrograph): Douglas & Taylor 1999 Douglas, Gerssen et al 2000 CDI (mirror and grism): Méndez, Riffeser et al 2001 PN.S(simultaneous CDI): Douglas, Arnaboldi et al 2002 Romanowsky, Douglas et al 2003 CDI (rotating spectrograph): Douglas & Taylor 1999 Douglas, Gerssen et al 2000 CDI (mirror and grism): Méndez, Riffeser et al 2001 PN.S(simultaneous CDI): Douglas, Arnaboldi et al 2002 Romanowsky, Douglas et al 2003

20. PN.S design

21. PN.S grating

22. PN.S mask

24. instrument efficiency = 72%  total system efficiency = 33% three 36 Å [O III] filters ( -1400.. +3400 km/s) field of view = 11.4’ x 10.3’ dispersion 1.29 pxl/Å built by prime optics, RSAA, ASTRON Douglas et al 2002

25. sample data 5’ x 2’ field in M31 (H. Merrett et al.)

26. pn.spectrograph project pn.s team: n. douglas, n. napolitano (groningen) k. kuijken (leiden) a. romanowsky, m. merrifield, h. merrett (nottingham) m. arnaboldi (turin) m. capaccioli (naples) k. freeman (rsaa) o. gerhard (basel ) pn.s team: n. douglas, n. napolitano (groningen) k. kuijken (leiden) a. romanowsky, m. merrifield, h. merrett (nottingham) m. arnaboldi (turin) m. capaccioli (naples) k. freeman (rsaa) o. gerhard (basel )

27. sample of 12 bright, round E galaxies: B  12.5, E2 or rounder, v < 1300 km/s 100 - 400 PNe per galaxy, to 5-15 R eff ~ 8 hours to reach m 5007 = 28.0 PN.S programme

28. WHT+PN.S: March 2002 3 hrs : 197 PN velocities to 7 R eff,  v = 20 km/s E1, M B = -20.0 D = 11 Mpc NGC 3379

29. Surface brightness profiles PNe stars (Capaccioli et al. 1990)

30. NGC 3379: Dispersion profile isotropic constant-M/L Hernquist model 110 PNe Isotropic singular isothermal halo 197 PNe long-slit data (Statler & Smecker- Hane 1999) 29 PNe (Ciardullo, Jacoby & Dejonghe 1993) Sluis et al. also confirmed with ~60 PNe

31. “Science three” dispersion profiles isotropic constant-M/L Hernquist model Romanowsky et al. 2003 (refs for long-slit: Bender et al 1994) Romanowsky et al. 2003 (refs for long-slit: Bender et al 1994)

32. - single wavelength: poor discrimination utilises 0.1% of spectrum + undispersed H-alpha camera PN.S limitations

33. M-CDI: masked counter-dispersed imaging past narrow band surveys at D > 10 Mpc: poor returns in follow-up spectroscopy apply counter-dispersed imaging (don’t need good astrometry) but utilise all information

34. Ciardullo et al. 1998 UT2+FORS2/MXU: 28-30 Apr 2001 MCDI 1400B VPH grism 6 fields @ 1 hr each: 200 PN velocities to 5 R eff,  v =15 km/s PNe in M87

35. NGC3377 future developments:

36. NGC3377 future developments: wavelength tagging detectors

37. NGC3377 future developments: spectrum of an entire galaxy

38. NGC3377 future developments: non-radial velocities