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LISA spectrograph Long slit Intermediate
resolution Spectrograph for Astronomy Performances
and application
Christian Buil
Active Spectroscopy in Astronomy Essen 7 May
2011
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Spectrograph resolution categories ( R l/dl )
Lhires R 16000
eShel R 11000
High resolution
Medium resolution (or intermediate)
LISA R 500 to 1000
Star Analyser R 100 to 200
Low resolution
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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
Planetary nebulae NGC 2392 15 x 30 seconds
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Faint object spectroscopy
But do not mystake luminosity and detectivity !
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
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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
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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

2D spectrum of moon surface
Na DA, D2
Mg I,2,3
Halpha
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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.

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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).
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Mechanical design
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Mechanical design
Ajustable grating angle
Calibration unit
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Pointing and guidance system
High quality slit image on the guidance
camera (here M104 galaxy with a Watec 120N)
High reflectivity slit Very constant edge
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LISA on a Celestron 11 telescope
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Calibration module (spectral calibration and
flat-field)
Electromagnetic system 12 V power Remote
operation possible
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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
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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 _at_ 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
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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 C11
f/6.8
Slit 50 microns R 600 W 5.4 arcsec on C11
f/6.8
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Automatised processing Rlhires application
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Automatic spectral calibration by using observed
type A, B or G star spectra and internal neon
lamp spectrum
Fit dispersion law with a 3e order polynomial
function (typical RMS error 0.3 to 0.4 A)
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Many tools available computation of
heliocentric velocity, H2O removal, atmopsheric
transmission, spectra database, .
French/english interface
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Limit magnitude
Integration time 1 hour (6 x 600 sec)Signal to
noise ratio 10 (_at_ Halpha)Type A0V star
Seeing 3 arcsec CCD KAF-8300 (Binning 1 x1)
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 15.0
D 35 cm F/D 6.8 13.9 14.9 15.4
D 50 cm F/D 6.0 14.4 15.5 16.2
D 100 cm F/D 6.0 15.2 16.3 17.2
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
D 28 cm F/D 6.8 14.5 15.2 15.6
D 35 cm F/D 6.8 14.8 15.6 16.1
D 50 cm F/D 6.0 15.3 16.3 16.9
D 100 cm F/D 6.0 16.1 17.3 18.2
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Limit magnitude (function of detector type)
Integration time 1 hour (6 x 600 sec)Signal to
noise ratio 10 (_at_ Halpha)Type A0V star
Seeing 3 arcsec Altitude 3000 m Dark sky
CCD KAF-8300 (Binning 2 x2)
CCD KAF-3200 (Binning 2 x2)
CCD ICX285AL (Binning 2 x2)
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 15.8
D 35 cm F/D 6.8 15.8 16.2
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 14.2 14.5
D 28 cm F/D 6.8 15.8 16.2
D 35 cm F/D 6.8 16.2 16.7
D 50 cm F/D 6.0 16.9 17.5
D 100 cm F/D 6.0 17.8 18.7
Slit 50 µm R 600 Slit 100 µm R 280
D 12.8 cm F/D 8 14.3 14.7
D 28 cm F/D 6.8 16.0 16.3
D 35 cm F/D 6.8 16.4 16.8
D 50 cm F/D 6.0 17.1 17.6
D 100 cm F/D 6.0 18.1 19.0
M 16.1 (KAF-8300) M 16.5 (KAF-3200)M 16.6
(ICX424AL)
3 hours integration (18 x 600 sec) Slit 50 µm
D 28 cm F/D 6.8
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Observation with LISA spectrograph
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Typical aspect of LISA 2D spectra Symbiotic star
V1016 Cyg
Star Analyser
2D spectrum before sky removal (23 µm slit)
2D spectrum after sky substraction
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Symbiotic star V1016 Cyg (V 11.2) lines
identification
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First step observation of normal stars (1/2)
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First step observation of normal stars (2/2)
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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 lt 10)
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Faint Be stars observation (BeSS)
V 6.09 9 x 120 s
V 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)
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Survey of cataclysmic (novae like)
SS Cyg outburst (V 8.7) April 4.1, 2011
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List of cataclysmic star (François Teyssier)

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Outburst of cataclysmic V694 Mon High velocity
wind Fast evolution
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V694 Mon Visible IR capacity of LISA
spectrograph
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Recurent nova T Pyxidis day to day monitoring
of profile evolution
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Observation at very low angular elevation
associated problem T Pyxidis declinaison -32
degrees
T Pyxidis 2D spectrum
6 arcsec refraction at 12 degree elevation
Paralactic angle
Horizon
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Nova Sagittarii 2011 2 (V5588 Sgr) V 13.2
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Eruption of Herbig Ae/Be star Z CMa
Vis IR spectrum
Detail of IR spectrum
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MIRA star R Leo at V 8.5
Wide band spectrum
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Wolf-Rayet star HD 56925 WR 7 V 11.7
HD 56925 in NGC 2359 nebula
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Messier 1 (Crab nebulae) - 5 x 600 s _at_ R 600
R Mon in NGC 2261 nebula 3 x 600 s _at_ R 1000
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SUPERNOVA SN 2011ae in MCG-3-30-19
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SUPERNOVA SN 2011by in NGC 3979
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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)
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Active galaxies (Seyfert)
NGC 4151
NGC 4051
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Quasar 3C273
LISA infrared version
Observed Halpha at 7584 A z (7584 - 6563)/6563
0.155 (official z 0.158)
McDonald 2,1 m K. Thompson AJ, 395, 404,417, 1992
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Quasar Mrk 205 observation (V 15.5)
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Quasar Mrk 205 7 x 600 sec. 50 µm slit
Observed z 0.0710 (official value z 0.0705)
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Thank you