LISA spectrograph Long slit Intermediate resolution Spectrograph for

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

Spectrograph resolution categories ( R = l/dl ) Lhires R = 16000 Medium resolution (or intermediate) Low resolution Essen - 7 May 2011 High resolution e. Shel R = 11000 LISA R = 500 to 1000 Star Analyser R = 100 to 200 2

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

Faint object spectroscopy But do not mystake luminosity and detectivity ! One limitation of slitless spectroscopy : sky background pollution The symbiotic star V 1016 Cyg Another limitation of SA : optical aberration Chromatic coma : a source of detectivity degradation (bad capacity to concentrate energy) Grism improvement Essen - 7 May 2011 4

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 Essen - 7 May 2011 5

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 KAF 8300 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 2 D spectrum of moon surface Mg I, 2, 3 Essen - 7 May 2011 Na DA, D 2 Halpha 6

The LISA concept (2/2) - 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! Essen - 7 May 2011 7

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 2011 8

Mechanical design Essen - 7 May 2011 9

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

Pointing and guidance system High reflectivity slit Very constant edge Essen - 7 May 2011 High quality slit image on the guidance camera (here M 104 galaxy with a Watec 120 N) 11

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

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

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) Essen - 7 May 2011 Fast adaptation for CCD camera and DSRL 14

Example of setup with Atik CCD cameras Atik 314 L 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 Essen - 7 May 2011 15

Amovible entrance slit High precision chromium serigraphy 15 – 19 – 23 – 32 microns (option 50 – 75 – 100 microns + 19 microns hole) Slit 23 microns – R = 1100 W = 2, 5 arcsec on C 11 f/6. 8 Essen - 7 May 2011 Slit 50 microns – R = 600 W = 5. 4 arcsec on C 11 f/6. 8 16

Automatised processing Rlhires application Essen - 7 May 2011 17

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) Essen - 7 May 2011 18

Many tools available : computation of heliocentric velocity, H 2 O removal, atmopsheric transmission, spectra database, …. French/english interface Essen - 7 May 2011 19

Limit magnitude Integration time : 1 hour (6 x 600 sec) Signal to noise ratio = 10 (@ Halpha) Type A 0 V star – Seeing = 3 arcsec CCD KAF-8300 (Binning 1 x 1) Altitude 0 m - Suburban Altitude 3000 m – Dark sky Slit 23 µm R = 1100 Slit 50 µm R = 600 Slit 100 µm R = 290 D = 12. 8 cm F/D = 8 12. 5 13. 1 13. 4 D = 28 cm F/D = 6. 8 13. 6 14. 6 D = 35 cm F/D = 6. 8 13. 9 D = 50 cm F/D = 6. 0 D = 100 cm F/D = 6. 0 Essen - 7 May 2011 Slit 23 µm R = 1100 Slit 50 µm R = 600 Slit 100 µm R = 290 D = 12. 8 cm F/D = 8 13. 1 13. 6 13. 9 15. 0 D = 28 cm F/D = 6. 8 14. 5 15. 2 15. 6 14. 9 15. 4 D = 35 cm F/D = 6. 8 14. 8 15. 6 16. 1 14. 4 15. 5 16. 2 D = 50 cm F/D = 6. 0 15. 3 16. 9 15. 2 16. 3 17. 2 D = 100 cm F/D = 6. 0 16. 1 17. 3 18. 2 20

Limit magnitude (function of detector type) Integration time : 1 hour (6 x 600 sec) Signal to noise ratio = 10 (@ Halpha) Type A 0 V star – Seeing = 3 arcsec Altitude 3000 m – Dark sky CCD KAF-8300 (Binning 2 x 2) CCD KAF-3200 (Binning 2 x 2) Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12. 8 cm F/D = 8 14. 2 14. 5 15. 8 D = 28 cm F/D = 6. 8 15. 8 16. 2 D = 35 cm F/D = 6. 8 D = 50 cm F/D = 6. 0 16. 4 17. 0 D = 100 cm F/D = 6. 0 17. 4 18. 3 Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12. 8 cm F/D = 8 13. 7 14. 0 D = 28 cm F/D = 6. 8 15. 4 D = 35 cm F/D = 6. 8 Slit 50 µm R = 600 Slit 100 µm R = 280 D = 12. 8 cm F/D = 8 14. 3 14. 7 16. 2 D = 28 cm F/D = 6. 8 16. 0 16. 3 16. 2 16. 7 D = 35 cm F/D = 6. 8 16. 4 16. 8 D = 50 cm F/D = 6. 0 16. 9 17. 5 D = 50 cm F/D = 6. 0 17. 1 17. 6 D = 100 cm F/D = 6. 0 17. 8 18. 7 D = 100 cm F/D = 6. 0 18. 1 19. 0 3 hours integration (18 x 600 sec) – Slit 50 µm – D = 28 cm F/D = 6. 8 Essen - 7 May 2011 CCD ICX 285 AL (Binning 2 x 2) M = 16. 1 (KAF-8300) M = 16. 5 (KAF-3200) M = 16. 6 (ICX 424 AL) 21

Observation with LISA spectrograph Essen - 7 May 2011 22

Typical aspect of LISA 2 D spectra Symbiotic star V 1016 Cyg Star Analyser 2 D spectrum before sky removal (23 µm slit) 2 D spectrum after sky substraction Essen - 7 May 2011 23

Symbiotic star V 1016 Cyg (V = 11. 2) : lines identification Essen - 7 May 2011 24

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

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

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) Essen - 7 May 2011 27

Faint Be stars observation (Be. SS) V = 6. 09 – 9 x 120 s Essen - 7 May 2011 V = 8. 62 – 6 x 300 s (new Be. SS entry) V = 4. 74 – 8 x 60 s V = 8. 63 – 7 x 300 s (new Be. SS entry) 28

Survey of cataclysmic (novae like) SS Cyg outburst (V = 8. 7) – April 4. 1, 2011 Essen - 7 May 2011 29

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

Outburst of cataclysmic V 694 Mon High velocity wind – Fast evolution Essen - 7 May 2011 31

V 694 Mon – Visible + IR capacity of LISA spectrograph Essen - 7 May 2011 32

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

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

Nova Sagittarii 2011 #2 (V 5588 Sgr) V = 13. 2 Essen - 7 May 2011 35

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

MIRA star R Leo at V = 8. 5 Wide band spectrum Essen - 7 May 2011 37

Wolf-Rayet star HD 56925 WR 7 – V = 11. 7 HD 56925 in NGC 2359 nebula Essen - 7 May 2011 38

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

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

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

Messier 104 Sombrero galaxy Audela autoguiding 2 D spectrum Na rest = 5892. 9 A - Na observed = 5916. 9 A – z = (5916. 9 – 5892. 9) / 5892. 9 = 0. 0041 (17 Mpc) Essen - 7 May 2011 42

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

Quasar 3 C 273 LISA infrared version Observed Halpha at 7584 A z = (7584 - 6563)/6563 = 0. 155 (official z = 0. 158) Mc. Donald 2, 1 m K. Thompson AJ, 395, 404, 417, 1992 Essen - 7 May 2011 44

Quasar Mrk 205 observation (V = 15. 5) Essen - 7 May 2011 45

Quasar Mrk 205 7 x 600 sec. – 50 µm slit Observed z = 0. 0710 (official value z = 0. 0705) Essen - 7 May 2011 46

Thank you Essen - 7 May 2011 47