TAIPAN fibre feed and spectrograph: engineering overview · TAIPAN will conduct a stellar and galaxy survey of the So uthern sky. The TAIPAN positioner is being developed as a prototype

TAIPAN Fibre Feed and Spectrograph: Engineering Overview Nicholas F. Staszak*, Jon Lawrence, Ross Zhelem, Robert Content, Vladimir Churilov, Scott Case,

Rebecca Brown, Andrew M. Hopkins, Kyler Kuehn, Naveen Pai, Urs Klauser, Vijay Nichani, Lew Waller

Australian Astronomical Observatory, 105 Delhi Rd., North Ryde, NSW 2113, Australia.

ABSTRACT TAIPAN will conduct a stellar and galaxy survey of the Southern sky. The TAIPAN positioner is being developed as a prototype for the MANIFEST instrument on the GMT. The TAIPAN Spectrograph is an AAO designed all-refractive 2-arm design that delivers a spectral resolution of R>2000 over the wavelength range 370-870 nm. It is fed by a custom fibre cable from the TAIPAN Starbugs positioner. The design for TAIPAN incorporates 150 optical fibres (with an upgrade path to 300). Presented is an engineering overview of the UKST Fibre Cable design used to support Starbugs, the custom slit design, and the overall design and build plan for the TAIPAN Spectrograph. Keywords: spectrographs, Starbugs, MANIFEST, TAIPAN, UKST, GMT

1. INTRODUCTION TAIPAN, currently nearing completion, is a multi-object parallel-positioning fibre-optic spectrograph designed for the UK Schmidt Telescope at Siding Spring Observatory in northern New South Wales, Australia. The instrument will be used to perform galaxy and stellar surveys across the whole Southern hemisphere sky, over a 5 year period. An AAO designed fibre optic cable is used to transmit light from each of the 150 Starbug Robots (with an upgrade path to 300) to a custom designed slit as input to the TAIPAN Spectrograph. The TAIPAN Fibre cable is designed to minimize path length to the spectrograph for maximum throughput while incorporating the AAO’s best practices for minimizing focal ratio degradation within a fibre run. Presented is a discussion of the detailed design considerations of the fibre cable and slit design. The TAIPAN Spectrograph completely replaces the UKST 6DF spectrograph that was used for the RAVE survey and is part of the complete TAIPAN Instrument package being delivered to the UKST in 2016. The TAIPAN Spectrograph is an AAO designed all-refractive 2-arm design. It delivers a spectral resolution of R>2000 over the wavelength range of 370-870 nm. It contains completely custom optics and mechanical components starting with a 300 fibre slit assembly. The 300 fibre slit feeds a 5 element f/2.41 collimator assembly with one aspheric surface. The collimator optics reside within individual lens cells that provide tip, tilt, and x, y alignment adjustment. Alignment is accomplished on the AAO lens centering station. The beam from the collimator is split into two bands with the blue arm covering 370 to 592 nm and the red arm covering 580 to 870 nm. Two volume phase holographic (VPH) gratings are provided by Kaiser Optical Systems. The beam splitter and VPH grating assemblies reside in kinematically mounted holder assemblies for alignment and the ability to accurately remove and replace from the spectrograph. Custom camera barrels and lenses feed semi-custom Spectral Instruments 1100s Dewar Detectors. The red and blue cameras are F1.5, each a five element design with three aspheric surfaces. The optical subassemblies interface to a monolithic spectrograph structure. All optics in the TAIPAN Spectrograph have been manufactured by Optimax. An overview of the overall opto-mechanical design and assembly of the TAIPAN spectrograph will be presented. *[email protected]: phone 61-2-9372-4857: www.aao.gov.au

Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II, edited by Ramón Navarro, James H. Burge, Proc. of SPIE Vol. 9912, 991223

© 2016 SPIE · CCC code: 0277-786X/16/$18 · doi: 10.1117/12.2233796

Proc. of SPIE Vol. 9912 991223-1

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fibre, P1. This i

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R COUPLIN

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ence measuremwith terminated is leg 1 in Figu

the LEMO conntire assembly. ss of the conne

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%. When gel w

taken with Ceto standard teleonnectors rely

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igure 12 below

test.

ment of input d and polished ure 12. This is c

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was added to th

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the fibre s and the onditions

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In this setup,This LED waeffectively cprojected oncontributes toFigure 14.

gnment. The

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ment that woulddeposited on th

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n 530nm. allows an nnulus is This blur below in

Proc. of SPIE Vol. 9912 991223-10


Five separate connections were tested using this method to determine the broadening in this setup with an average result of 1.46°. These numbers are well within the tolerance of 2° and give a further 0.5° margin for the final completed science cable.

7. SPECTROGRAPH OPTICAL DESIGN The TAIPAN spectrograph is a 2 arm design with a 300 fibre input slit. The fibre near field is reimaged by the spectrograph optics onto the CCD detector, while the fibre far field forms the pupil which is projected by the spectrograph collimator onto the VPH gratings, dispersing the beam into the cameras. The design operates with two semi-custom Spectral Instrument Dewar detectors. The red and blue spectrograph cameras provide demagnification of the fibre slit and are therefore a more challenging design when compared to the collimator. Each camera images the spectra on a 2k x 2k E2V detector. The average resolution is approximately 2350. The wavelength range is from 370 nm to 870 nm with the dichroic cut-off at 590 nm and a common region to both cameras from 580 nm to 592 nm. The cut-off wavelength and the overlapping region were chosen based on science requirements and to minimize the overlap region. This in turn maximizes the resolution of the spectrograph for the same spectral length in each pixel. In order to produce quality spectra with a reduced number of optical elements, the TAIPAN spectrograph relies upon aspheric surfaces in both the collimator and camera. The fibre core size is 50 µm which corresponds to 3.3" on the sky. A design choice had to be made between two competing designs, one design using mirrors, the other a fully transmissive design. It was decided to use the latter based on specific advantages. Modern antireflection coatings are very efficient over a large wavelength range and different incident angles. While there are now better reflection coatings for mirrors than in the past, the large operational wavelength range starting at 370 nm remains a challenge. Also, the surface form error of a mirror creates far larger aberrations and scattered light than a lens surface of the same error. For a given root mean square (RMS) surface form error or surface roughness, the Optical Path Difference (OPD) RMS will be 2 RMS after reflection by a mirror. It will be (n-1) RMS after refraction by a lens surface with n the refractive index. The OPD is 0.43885 RMS for a CaF2 glass surface at the standard Nd wavelength of 587.6 nm. Light would have to pass 21 CaF2 surfaces to have about the same OPD RMS than after a single mirror reflection. A mirror is then equivalent to 21 CaF2 lens surfaces in that respect. Other advantages are that it avoids any diffractive and light blocking obstruction in the beam and the need for highly off-axis aspheres in the collimator, which would be required in a reflective design. Finally, the detector Dewar assembly can be made very small, when compared to the Dewar of a Schmidt camera design which would be required when using mirrors. The entire detector Dewar assembly can be decoupled from the rest of the spectrograph and placed in a mount for position adjustments and focus travel. An important disadvantage of transmissive systems is glass absorption at UV wavelengths. This was very significantly reduced in the present design by incorporating UV transmission as an important factor at every step of the design through choice of glasses. Total glass absorption from slit to detector starting at 370 nm is only 9%, reducing to 3.3% at 400 nm, and continuing to drop at longer wavelengths. The input of each fibre receives a beam with a focal ratio of about 2.5 from the UKST telescope, which is relatively fast. The collimator design had to be somewhat faster to accommodate focal ratio degradation in the fibres and tolerances due to fibre pointing error. Two designs were studied, the first with bare fibres as the spectrograph input slit, and a competing design in which a microlens array was added at the end of the fibres. The purpose of the microlens array was to increase the focal ratio of the beam entering the collimator. A microlens array would have permitted the collimator design to reduce to one lens (Figure 15). A disadvantage of this configuration is that the slit must be curved. The bare fibre slit input is geometrically straight and mated to a plano-concave, low cost, fused-silica lens. This is a relatively simple configuration. Another disadvantage of the microlens slit input is that microlens tolerances degrade the beam mostly through pupil defocus and angular errors in the beam direction. This is equivalent to a large FRD. The large tolerances are due to the fast telescope focal ratio. Using a microlens array with an Integral Field Unit (IFU) allows spectra to be packed very tightly thereby reconstituting a pseudo-slit without empty space between the images of each fibre. In Multi-Object Spectroscopy (MOS), where each fibre observes a different object, it is necessary to have gaps between spectra to avoid cross-contamination. The advantage of having more spectra with a microlens array is therefore not an option with the TAIPAN Spectrograph design. The final design choice was to use the bare fibre slit input with an additional four lenses in the collimator. The final collimator design is f/2.41 based on the combination of telescope focal

Proc. of SPIE Vol. 9912 991223-11


001 (V1) Date: 00160.2857

2/01/2016

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Proc. of SPIE Vol. 9912 991223-12


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Proc. of SPIE Vol. 9912 991223-13


SLIT / Light

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Proc. of SPIE Vol. 9912 991223-14


I

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Proc. of SPIE Vol. 9912 991223-15


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Proc. of SPIE Vol. 9912 991223-16


1

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Proc. of SPIE Vol. 9912 991223-18


Interferomete

Interferome

Collimator

dlimator R

-rVeturn flat

uvera (Blue/Red

Corrector lens

9.1 Optical The testing operformance individually corrected by 28) over thecollimator ascameras.

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Figure 28.

e performed, inluded. The colltegrated with t

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Figure 29

the spectrograpd cameras are he spectrograpo-aligned to le

ment process ice target, and

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encompasses aet. The collimnterferometric necessary for elens, with zer

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Optical test setu

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ph is based upbuilt as suba

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ms. In this all real design sectimera barrels w

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he same time, ed using the imbre cable is illuf the test spect

at system certified

at is fully s (Figure n of the and red

m splitter flattener window

corrected the focal

efractive ion. The with the

re of the pe, is the e camera m splitter nal stage, is of the the field

mage of a uminated trum and

Proc. of SPIE Vol. 9912 991223-19


10. SUMMARY TAIPAN is a spectroscopic instrument that incorporates a fibre positioning system, an optical spectrograph, and a fibre cable linking the positioner with the spectrograph slit. This paper has described the spectrograph, which is a novel all-refractive 2-arm design delivering a spectral resolution of R>2000 over the wavelength range 370-870 nm, and the fibre cable, which has been designed to maximize throughput and minimize focal degradation. All three aspects of the TAIPAN instrument will be installed at the UKST towards the end of 2016 and will commence science observations in 2017.

REFERENCES

[1] ‘The UK Schmidt Telescope’, (accessed 24 May 2016). [2] Kyler Kuehn, Jon Lawrence, David M. Brown, Scott Case, Matthew Colless, Robert Content, Luke Gers, James

Gilbert, Michael Goodwin, Andrew M. Hopkins, Michael Ireland, Nuria P. F. Lorente, Rolf Muller, Vijay Nichani, Azizi Rakman, Samuel N. Richards, Will Saunders, Nick F. Staszak, Julia Tims, Lewis G. Waller. “TAIPAN: Optical Spectroscopy with Starbugs,” Proc. SPIE 9147, 914710, (2014).

[3] Johnson, S., et al., R. Taylor, R., Bailes, M., Bartel, N., Baugh, C., Bietenholz, M., Blake, C., Braun, R., Brown, J., Chatterjee, S., Darling, J., Deller, A., Dodson, R., Edwards, P., Ekers, R., Ellingsen, S., Feain, I., Gaensler, B., Haverkorn, M., Hobbs, G., Hopkins, A., Jackson, C., James, C., Joncas, G., Kaspi, V., Kilborn, V., Koribalski, B., Kothes, R., Landecker, T., Lenc, A., Lovell, J., Macquart, J.-P., Manchester, R., Matthews, D., McClure-Griffiths, N., Norris, R., Pen, U.-L., Phillips, C., Power, C., Protheroe, R., Sadler, E., Schmidt, B., Stairs, I., Staveley-Smith, L., Stil, J., Tingay, S., Tzioumis, A., Walker, M., Wall, J., Wolleben, M.,“Science with ASKAP, the Australian square-kilometre-array pathfinder,” Experimental Astronomy, Volume 22, Issue 3, pp.151-273 (2008).

[4] Ricker, G.,“Transiting Exoplanet Survey Satellite (TESS),” Proc. SPIE 9143, 914320 (2014). [5] Nicholas F. Staszak, Jon Lawrence, David M. Brown, Rebecca Brown, Ross Zhelem, Michael Goodwin, Kyler

Kuehn, Nuria P. F. Lorente, Vijay Nichani, Lew Waller, Scott Case, Robert Content, Andrew M. Hopkins, Urs Klauser, Naveen Pai, Rolf Mueller, Slavko Mali, Minh V. Vuong. “TAIPAN Instrument Fibre Positioner and Starbug Robots: Engineering Overview” Proc. SPIE 9916, in press (2016).

[6] Thorlabs Furcation Tube photograph, viewed 5 June 2016, < http://www.thorlabs.hk/newgrouppage9.cfm?objectgroup_id=312>.

[7] Robert E. Parks, William P. Kuhn, "Optical alignment using the Point Source Microscope", Proceedings of SPIE Vol. 5877, 58770B (2005)

[8] Robert E. Parks, "Versatile autostigmatic microscope", Proceedings of SPIE Vol. 6289, 62890J (2006)

Proc. of SPIE Vol. 9912 991223-20


Documents

TAIPAN fibre feed and spectrograph: engineering overview · TAIPAN will conduct a stellar and galaxy survey of the So uthern sky. The TAIPAN positioner is being developed as a prototype