1. LISA spectrograph Long slit Intermediate resolution Spectrograph for Astronomy Performances and application Christian Buil Active Spectroscopy in Astronomy Essen – 7 May 2011 1Essen - 7 May 2011

2. Spectrograph resolution categories ( R  ) High resolution Lhires R = 16000 eShel R = 11000 Medium resolution (or intermediate) LISA R = 500 to 1000 Low resolution Star Analyser R = 100 to 200 2Essen - 7 May 2011

3. Spectral resolution (R) and luminosity (L) : a complementary effort R x L = constant Planetary nebulae NGC 2392 – 15 x 30 seconds Faint object spectroscopy The example of Star Analyser : very low resolution, very high luminosity 3 Essen - 7 May 2011

4. But do not mystake luminosity and detectivity ! Faint object spectroscopy One limitation of slitless spectroscopy : sky background pollution The symbiotic star V1016 Cyg Another limitation of SA : optical aberration Chromatic coma : a source of detectivity degradation (bad capacity to concentrate energy) Grism improvement 4 Essen - 7 May 2011

5. Faint object spectroscopy The importance of an entrance slit Large slit Narrow slit The sky background level if proportionnal to the slit wide The backgroung photon noise is proportionnal to the square root of slit wide 5 Essen - 7 May 2011

6. The LISA concept (1/2) -Ajustable entrance slit by step (from 15 microns to 100 microns) (capacity to optimise spectral resolution to a specific target) -Fast input beam : up to f/5 input i.e. high luminosity spectrograph (reduce potential guidance problem because shorter focal length, capture of faint surface objet like galaxies, comets, … -Optimized spectral dispersion to modern camera (2 A / pixel sampling on a popular KAF8300 CCD ship) -Balance between power resolution capacity and scientific interest (R = 500 to 1000 typically) – Sodium doublet is just separated with a 23 microns slit Mg I,2,3 Na DA, D2 Halpha 2D spectrum of moon surface 6 Essen - 7 May 2011

7. -Wide spectral range in one shot : 3950 A – 7200 A (+ IR option) -Integrated calibration system (neon lamp + tungsten lamp) : easy to use and standard pipeline processing. Possibility to fully automatize acquisition. -Compact and moderate weigth : adaptable on small refractor and refractor. -Low cost : large diffusion if possible! The LISA concept (2/2) 7 Essen - 7 May 2011

8. Optical design Internal grandissement G = 0,603 For example: if the telescope focal / diameter ratio is 6, the final F/D is 6 x 0,603 = 3,6 (LISA is equivalent to a focal reducer). Essen - 7 May 20118

9. Mechanical design 9 Essen - 7 May 2011

10. Mechanical design Calibration unit Ajustable grating angle 10 Essen - 7 May 2011

11. Pointing and guidance system High reflectivity slit Very constant edge High quality slit image on the guidance camera (here M104 galaxy with a Watec 120N) 11 Essen - 7 May 2011

12. LISA on a Celestron 11 telescope 12 Essen - 7 May 2011

13. Calibration module (spectral calibration and flat-field) Electromagnetic system – 12 V power – Remote operation possible Essen - 7 May 2011 13

14. Interfaces Optimal input focal ratio f/5 to f/7 A fast Newton telescope is ideal (achromatism) For SC Telescope : focal reducer (here a Baader Alan Gee - final ratio f/6.8) Fast adaptation for CCD camera and DSRL 14 Essen - 7 May 2011

15. 15 Example of setup with Atik CCD cameras Atik 314L for spectra acquistion (1390 x 1040 x 6.45 µm pixel size) Readout noise : 4.5 e-, Camera gain : 0.250 e-/ADU, typical quantum efficiency @ 656 nm : 55% Atik Titan for pointing and guiding functions (faint object identification capability + rudimentary photometry measure on the targets) Low cost solution for LISA, low mass on the telescope, high performances

16. Amovible entrance slit High precision chromium serigraphy Slit 23 microns – R = 1100 W = 2,5 arcsec on C11 f/6.8 Slit 50 microns – R = 600 W = 5.4 arcsec on C11 f/6.8 15 – 19 – 23 – 32 microns (option 50 – 75 – 100 microns + 19 microns hole) 16 Essen - 7 May 2011

17. Automatised processing Rlhires application 17 Essen - 7 May 2011

18. Automatic spectral calibration by using observed type A, B or G star spectra and internal neon lamp spectrum Fit dispersion law with a 3 e order polynomial function (typical RMS error : 0.3 to 0.4 A) 18 Essen - 7 May 2011

19. Many tools available : computation of heliocentric velocity, H2O removal, atmopsheric transmission, spectra database, …. French/english interface 19 Essen - 7 May 2011

20. Slit 23 µm R = 1100 Slit 50 µm R = 600 Slit 100 µm R = 290 D = 12.8 cm F/D = 8 12.513.113.4 D = 28 cm F/D = 6.8 13.614.615.0 D = 35 cm F/D = 6.8 13.914.915.4 D = 50 cm F/D = 6.0 14.415.516.2 D = 100 cm F/D = 6.0 15.216.317.2 Slit 23 µm R = 1100 Slit 50 µm R = 600 Slit 100 µm R = 290 D = 12.8 cm F/D = 8 13.113.613.9 D = 28 cm F/D = 6.8 14.515.215.6 D = 35 cm F/D = 6.8 14.815.616.1 D = 50 cm F/D = 6.0 15.316.316.9 D = 100 cm F/D = 6.0 16.117.318.2 Integration time : 1 hour (6 x 600 sec) Signal to noise ratio = 10 (@ Halpha) Type A0V star – Seeing = 3 arcsec CCD KAF-8300 (Binning 1 x1) Limit magnitude Altitude 0 m - SuburbanAltitude 3000 m – Dark sky 20 Essen - 7 May 2011

21. Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12.8 cm F/D = 8 13.714.0 D = 28 cm F/D = 6.8 15.415.8 D = 35 cm F/D = 6.8 15.816.2 D = 50 cm F/D = 6.0 16.417.0 D = 100 cm F/D = 6.0 17.418.3 Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12.8 cm F/D = 8 14.214.5 D = 28 cm F/D = 6.8 15.816.2 D = 35 cm F/D = 6.8 16.216.7 D = 50 cm F/D = 6.0 16.917.5 D = 100 cm F/D = 6.0 17.818.7 Integration time : 1 hour (6 x 600 sec) Signal to noise ratio = 10 (@ Halpha) Type A0V star – Seeing = 3 arcsec Altitude 3000 m – Dark sky Limit magnitude (function of detector type) CCD KAF-8300 (Binning 2 x2)CCD KAF-3200 (Binning 2 x2) 3 hours integration (18 x 600 sec) – Slit 50 µm – D = 28 cm F/D = 6.8 M = 16.1 (KAF-8300) M = 16.5 (KAF-3200) M = 16.6 (ICX424AL) 21 Essen - 7 May 2011 Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12.8 cm F/D = 8 14.314.7 D = 28 cm F/D = 6.8 16.016.3 D = 35 cm F/D = 6.8 16.416.8 D = 50 cm F/D = 6.0 17.117.6 D = 100 cm F/D = 6.0 18.119.0 CCD ICX285AL (Binning 2 x2)

22. Observation with LISA spectrograph 22 Essen - 7 May 2011

23. Star Analyser Typical aspect of LISA 2D spectra Symbiotic star V1016 Cyg 2D spectrum before sky removal (23 µm slit) 2D spectrum after sky substraction 23 Essen - 7 May 2011

24. Symbiotic star V1016 Cyg (V = 11.2) : lines identification 24 Essen - 7 May 2011

25. First step : observation of normal stars (1/2) 25 Essen - 7 May 2011

26. First step : observation of normal stars (2/2) 26 Essen - 7 May 2011

27. Survey of know Be Star + and detection of new Be star Beta Lyrae (Shelyak) – 15 x 30 s Rapid scan of B and A star for Halpha emission signature (5-10 minutes exposure) (list of nearly 1000 stars – magnitude < 10) 27 Essen - 7 May 2011

28. Faint Be stars observation (BeSS) V = 6.09 – 9 x 120 sV = 4.74 – 8 x 60 s V = 8.62 – 6 x 300 s (new BeSS entry) V = 8.63 – 7 x 300 s (new BeSS entry) 28Essen - 7 May 2011

29. Survey of cataclysmic (novae like) SS Cyg outburst (V = 8.7) – April 4.1, 2011 29Essen - 7 May 2011

30. List of cataclysmic star (François Teyssier) … 30 Essen - 7 May 2011

31. Outburst of cataclysmic V694 Mon High velocity wind – Fast evolution 31 Essen - 7 May 2011

32. V694 Mon – Visible + IR capacity of LISA spectrograph 32 Essen - 7 May 2011

33. Recurent nova T Pyxidis : day to day monitoring of profile evolution 33 Essen - 7 May 2011

34. T Pyxidis 2D spectrum 6 arcsec refraction at 12 degree elevation Paralactic angle Observation at very low angular elevation : associated problem T Pyxidis declinaison = -32 degrees Horizon 34 Essen - 7 May 2011

35. Nova Sagittarii 2011 #2 (V5588 Sgr) V = 13.2 35 Essen - 7 May 2011

36. Eruption of Herbig Ae/Be star Z CMa Vis + IR spectrum Detail of IR spectrum 36 Essen - 7 May 2011

37. MIRA star R Leo at V = 8.5 Wide band spectrum 37 Essen - 7 May 2011

38. HD 56925 in NGC 2359 nebula Wolf-Rayet star HD 56925 WR 7 – V = 11.7 38 Essen - 7 May 2011

39. R Mon in NGC 2261 nebula 3 x 600 s @ R = 1000 Messier 1 (Crab nebulae) - 5 x 600 s @ R = 600 39 Essen - 7 May 2011

40. SUPERNOVA SN 2011ae in MCG-3-30-19 40Essen - 7 May 2011

41. SUPERNOVA SN 2011by in NGC 3979 41Essen - 7 May 2011

42. 42 Messier 104 Sombrero galaxy Audela autoguiding 2D spectrum Na rest = 5892.9 A - Na observed = 5916.9 A – z = (5916.9 – 5892.9) / 5892.9 = 0.0041 (17 Mpc)

43. NGC 4151 NGC 4051 Active galaxies (Seyfert) 43 Essen - 7 May 2011

44. McDonald 2,1 m K. Thompson AJ, 395, 404,417, 1992 Quasar 3C273 Observed Halpha at 7584 A z = (7584 - 6563)/6563 = 0.155 (official z = 0.158) 44 Essen - 7 May 2011 LISA infrared version

45. Quasar Mrk 205 observation (V = 15.5) 45 Essen - 7 May 2011

46. Observed z = 0.0710 (official value z = 0.0705) Quasar Mrk 205 7 x 600 sec. – 50 µm slit 46 Essen - 7 May 2011

47. Thank you 47 Essen - 7 May 2011