Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Why only take 2 interferograms? Why not take 2* N ? The birth of the TAURUS concept Note: A single interferogram only contains (1/ N ) th of in spatial information Scanning the FP across a full FSR is a natural way to: Recover ALL of the spatial information Resolve the fundamental ambiguity in the individual interferograms Scanning can be achieved in 3 ways: a)Changing  : - by tilting the FP or by moving the image across the fringes as in photographic interferograms (to partially resolve ambiguity) b)Changing  : - by changing the pressure of a gas in the FP gap as in 0 th dimensional scanning with eg: propane c)Scanning d: - by changing the physical gap between the plates very difficult since need to maintain parallelism to /2 N, at least TAURUS = QI etalons + IPCS … c1980

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Queensgate Instruments (ET70)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ CS100 controller FP etalons Queensgate Instruments (Capacitance Micrometry) Capacitors X-bridge Y-bridge Z-bridge (+ stonehenge) Piezo transducers (3) Construction Super-flat /200 base Centre piece (optical contact) Top plate Scanning d over 1*FSR m  (m-1) ; d  d + ( /2)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Alec Boksenberg and the Image Photon Counting System (IPCS) Imperial College, London  QI etalons + CS100 University College, London  IPCS TAURUS  16 Mbyte datacubes } Perfect synthesis …

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ How big a field? From before, Jacquinot central spot given by: R  = 2  or: R ~ 8  2 / 2 ~ 8  2 (d/D T ) 2 /  J 2, where  J is the angle on the sky. However, given an array detector, we can work off-axis: So, how far? Answer: Until the rings get narrower than  ~2 pixels (the seeing disk) Now, from the Airy Function we obtain: d  /d = -1/ 0.sin(  ) The full TAURUS field,  F is then:  F = 2  2 (d/D T ) 2 / R   F /  J ~ 20, typically or ~400 in 

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ TAURUS Datacube Recalling the phase delay equ n : m = 2  l.cos  For small values of  : goes as [1 – (  2 /2)] where   tan -1 [(y-y 0 ]/[x-x 0 ]) and (x 0,y 0 ) = centre of FP fringes  (x 1,y 1 ) is shifted in z-dir n w.r.t. (x 0,y 0 ) and this -shift is thus ~parabolic in  It is also periodic in “m”. We thus refer to this shift as a “Phase-correction” So the surface of constant is a “Nested Parabola” Cut through a “Nested Parabola and you get a set of rings and these rings are the FP fringes.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Wavelength Calibration (converting z to ) As shown, surfaces of constant, as seen in an (x,z)-slice are defined by a set of nested parabolæ, equally spaced in z. Any (x,y)-slice within the cube cuts through these nested paraboloids to give the familiar FP fringes (rings). Now -calibration requires transforming z  where: l (z) = l (0) + az a is a constant of proportionality. Constructive interference on axis (x 0,y 0 ) gives: az 0 = m 0 /2  - l (0) but an off-axis (x,y) point transmits the same 0 at (z 0 + p xy ) where: ap xy = l (z 0 ).(sec  xy – 1)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Phase Correction The 2D phase-map, p(x,y), can be defined such that: p(x,y) = m  z 0 (sec  – 1) The phase-map, p(x,y), can be obtained from a -calibration data-cube by illuminating the FP with a diffuse monochromatic source of wavelength,. at (x 2,y 2 ) z at (x 1,y 1 ) z I 0 (z) I 0 ( ) Phase corrected zz Note: Phase-map is discontinuous at each  z

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ The Phase-Map The phase-map is so called since it can be used to transform the raw TAURUS cube, with its strange multi-paraboloidal iso-wavelength contours into a well- tempered data cube where all (x,y)-slices are now at constant wavelengths. The process is called phase-correction since it represents a periodic function of period,  z. ie: If the z-value (z’) of a phase-shifted pixel exceeds the z-dimensions of the data-cube, then the spectra is simply folded back by one FSR to (z’ -  z). It will be noted that the phase-map (as defined previously) is independent of and hence in principle any calibration wavelength, cal, can be used to phase- correct an observation data-cube at an arbitary obs, remembering that:   2 &  z = /2 But also, the phase-map can be expressed in -space as:  xy = 0 (1 - cos  ) and hence is also independent of gap, l, and thus applicable to all FPs at all.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Order (m) and gap ( l ) determination The periodicity of the FP interference fringes makes -calibration non-trivial. The paraboloidal mapping from z  doesn’t exactly help, either! Nevertheless, using 2 calibration wavelengths: Say: 1 and 2, peak on-axis at z 1 and z 2 The trick is to find m1 (and hence m2), the order of interference. From m we can infer the gap, l, and hence obtain a -calibration where: az 0 = m 0 /2  - l (0) Then: zz z2 – z1 1 2 m1m1 2  ( 1  2 ) m2  m1m2  m1 = If m 1 can be estimated (from manufacturers specs or absolute capacitance measures) then we can search for a solution where m 2 is an integer. This can be an iterative process with several wavelength pairs. Clearly the further 1 and 2 are apart, the more accuracy is achieved.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Wavelength Calibration If m 1 can be estimated (from manufacturers specs or absolute capacitance measures) then we can search for a solution where m 2 is an integer. This can be an iterative process with several wavelength pairs. Clearly the further 1 and 2 are apart, the more accuracy is achieved. Once the interference order, m 1, for a known wavelength, 1, has been identified then wavelength calibration is given by: { } (z  z 0 ) m0z0m0z0 + 1 = 0

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ FP P in collimated beam Interference fringes formed at infinity: Sky and FP fringes are con-focal Detector sees FP fringes superimposed on sky image FPIF

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ FP I in image plane Interference fringes formed at infinity: Sky and FP fringes are not con-focal Detector sees FP plates superimposed on sky image ie: No FP fringes seen on detector FP is not perfectly centred on image plane (out of focus) to avoid detector seeing dust particles on plates. FPIF

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ FP (or Interference Filter) in image plane The FP still acts as a periodic monochromator but the angles into the FP (or IF) must not exceed the Jacquinot criteria, which states that: 2 < 8  2 / R (or R  = 2  ) At f/8: = 2.tan -1 (1/16) ~7.2º, so R < 500 At f/16: = 2.tan-1(1/32) ~3.6º, so R < 2,000 Note: the FoV is determined not by the width of the fringes but by the diameter of the FP. Also, an IF is simply a solid FP (  ~2.1) with very narrow gap.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Data-cube science

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ FP observations of NGC 7793 on the 3.6m. Top left: DSS Blue Band image. Top right: Spitzer infrared array camera (IRAC) 3.6μm image. Middle left: Hα monochromatic image. Middle right: Hα velocity field. Bottom: position-velocity (PV) diagram.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ FP observations of NGC 7793 on the 36cm. Top left: DSS Blue Band image. Top right: Spitzer IRAC 3.6μm image. Middle left: Hα monochromatic image. Middle right: Hα velocity field. Bottom: PV diagram.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ ADHOC screen shot (Henri)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ ADHOC screen shot (Henri)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Imaging Fourier Transform Spectrographs (IFTS) FTS = Michelson Interferometer: IFTS = Imaging IFTS over solid angle, . Beam-splitter produces 2 arms; Light recombined to form interference fringes on detector; One arm is adjustable to give path length variations; Detected intensity is determined by the path difference,  x, between the 2 arms.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ IFTS theory (simple version) Given that frequency, = 1/ (unit units of “c”): Phase difference between two mirrors = 2  x So recorded intensity, I, is given by: I xx 2 (, ) 1 2 = [1 + cos(2  x)] Now, if we vary x in the range:   x/2  , continuously then:   -- I (x) = B ( ).(1 + cos2  x).d   -- B ( ) = I (x).(1 + cos2  x).dx and These represent Fourier Transform pairs. Spectrum B ( ) is obtained from the cosine transformation of the Interferogram I (x)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ IFTS reality (simple version) At x = 0: the IFTS operates simply as an imager; White light fringes – all wavelengths behave the same At all other x-values, a subset of wavelengths constructively/dsitructively interfere For a particular, the intensity varies sinusoidally according to the simple relationship: I ) 1 2 ( = [1 + cos(2  x)] In reality, of course, x goes from 0   x max which limits the spectral resolving power to: R 0 =  = 2  x max eg: if  x max = 100mm and = 500nm then: R 0 

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ IFTS in practice Since we are talking here about an imaging FTS then what is it’s imaging FoV? Circular symmetry of the IFTS is identical to the FP and hence: 2  l.cos  = m And also: R  >> 2  limited only by the wavelength variation, , across a pixel: However, in anaolgy to the FP  Phase-correction is required in order to accommodate path difference variations over the image surface.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Pros & Cons of an IFTS Advantages: Arbitary wavelength resolution to the R limit set by  x max ; A large 2D field of view; A very clean sinc function, instrumental profile cf: the FP’s Airy Function A finesse N = 2  /  which can have values higher than 10 3 Disadvantages: Sequential scanning – like the FP. However, the effective integration time of each interferogram image can be monitored through a separate complementary channel, if required; Very accurate control of scanned phase delay is required Especially problematic in the optical At all times, the detector sees the full spectrum and hence each interferogram receives integrated noise from the source and the sky This compensates for the fact that all wavelengths are observed simultaneously which is why there is no SNR advantage over an FP; Also sky lines produce even more noise, all the time.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Michelson Interfermeter (N = 2 interference ; n >>1)

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Hybrid and Exotic Systems Examples of this are: Integral Field Units (IFUs). These can use either: Lenslets Fibres Lenslets + Fibres Mirror Slicers FP & IFTS are classical 3D imaging spectrographs ie: Sequential detection of images to create 3D datat cubes: FP = Wavelength scanning IFTS = Phase delay scanning There are, however, techniques which use a 2D area detector to sample 2D spatial information with spectral information, symultaneously. These we refer to as: Hybrid Systems

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Integral Field Spectroscopy Extended (diffuse) object with lots of spectra Use “contiguous” 2D array of fibres or ‘mirror slicer’ to obtain a spectrum at each point in an image SIFS Tiger MPI’s 3D

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Lenslet array (example) Used in SPIRAL (AAT) VIMOS (VLT) Eucalyptus (OPD) LIMO (glass) Pitch = 1mm Some manufacturers use plastic lenses. Pitches down to ~50  m

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Tiger (Courtes, Marseille) Technique reimages telescope focal plane onto a micro-lens array Feeds a classical, focal reducer, grism spectrograph Micro-lens array: Dissects image into a 2D array of small regions in the focal surface Forms multiple images of the telescope pupil which are imaged through the grism spectrograph. This gives a spectrum for each small region of the image (or lenslet) Without the grism, each telescope pupil image would be recorded as a grid of points on the detector in the image plane The grism acts to disperse the light from each section of the image independently So, why don’t the spectra all overlap?

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Tiger (in practice) Enlarger Lenslet arrayCollimator Grism Camera Detector

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Avoiding overlap The grism is angled (slightly) so that the spectra can be extended in the -direction Each pupil image is small enough so there’s no overlap orthogonal to the dispersion direction -direction Represents a neat/clever optical trick

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Tiger constraints The number and length of the Tiger spectra is constrained by a combination of: detector format micro-lens format spectral resolution spectral range Nevertheless a very effective and practical solution can be obtained Tiger (on CFHT) SAURON (on WHT) OSIRIS(on Keck) True 3D spectroscopy – does NOT use time-domain as the 3 rd axis (like FP & IFTS) – very limited FoV, as a result

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Tiger Results (SAURON – WHT)