The Fiber Optical Cable and Connector System (FOCCoS), provides optical connection between 2400
positioners and a set of spectrographs by an optical fibers cable as part of Subaru PFS instrument. Each positioner
retains one fiber entrance attached at a microlens, which is responsible for the F-ratio transformation into a larger one so
that difficulties of spectrograph design are eased. The optical fibers cable will be segmented in 3 parts at long of the
way, cable A, cable B and cable C, connected by a set of multi-fibers connectors. Cable B will be permanently attached
at the Subaru telescope. The first set of multi-fibers connectors will connect the cable A to the cable C from the
spectrograph system at the Nasmith platform. The cable A, is an extension of a pseudo-slit device obtained with the
linear disposition of the extremities of the optical fibers and fixed by epoxy at a base of composite substrate. The second
set of multi-fibers connectors will connect the other extremity of cable A to the cable B, which is part of the positioner's
device structure. The optical fiber under study for this project is the Polymicro FBP120170190, which has shown very
encouraging results. The kind of test involves FRD measurements caused by stress induced by rotation and twist of the
fiber extremity, similar conditions to those produced by positioners of the PFS instrument. The multi-fibers connector
under study is produced by USCONEC Company and may connect 32 optical fibers. The tests involve throughput of
light and stability after many connections and disconnections. This paper will review the general design of the FOCCoS
subsystem, methods used to fabricate the devices involved and the tests results necessary to evaluate the total efficiency
of the set.
At least during the last ten years, the Brazilian astronomical community has been asking for an echelle spectrograph for
the 1.6 m telescope installed at Pico dos Dias Observatory (Brazópolis, MG, Brazil, OPD/MCTI/LNA). Among the
scientific cases are topics related to the chemical evolution of the Galaxy, asteroseismology, chemical composition and
chromospheric activities of solar type stars and the relations between solar analogues and terrestrial planets. During 2009
the project finally got started. The called ECHARPE spectrograph (Espectrógrafo ECHelle de Alta Resolução para o
telescópio Perkin-Elmer) is being projected to offer a spectral resolution of R ~ 50000, in the range 390-900 nm and with
a single exposition. It will be a bench spectrograph with two channels: blue and red, fed by two optical fibers (object, sky
or calibration) with aperture of 1.5 or 2.0 arcseconds. The instrument will be placed in one of the telescope pillar
ramification, in the originals installations of a Coudé spectrograph and in a specially created environment controlled
room. In this work we will present the scientific motivations, the conceptual optical design, the expected performance of
the spectrograph, and the status of its development. ECHARPE is expected to be delivered to the astronomical
community in 2014, fully prepared and optimized for remote operations.
ECHARPE spectrograph - Espectrógrafo ECHelle de Alta Resolução para o telescópio Perkin-Elmer - is being
designed at LNA - Laboratório Nacional de Astrofísica, Brazil - to be mounted on 1.60 meter telescope at Pico dos
Dias Observatory, Brazil. It will offer a spectral resolution of R ~ 50000, in the interval 390-900 nm and in a single
exposition. It will be a fiber fed, bench spectrograph with two channels: blue and red, fed by two optical fibers (object,
sky or calibration) with aperture of 1.5 or 2.0 arcseconds. This paper reports on technical characteristics of the
spectrograph mechanical design and presents a new developed mounting system for echelle grating and collimator and
relay mirrors, which allows linear and rotational adjustments in all degrees of freedom without using springs.
Claudia Rodrigues, Keith Taylor, Francisco Jablonski, Marcelo Assafin, Alex Carciofi, Deonisio Cieslinski, Joaquim E. Costa, Ruben Dominguez, Tania Dominici, Gabriel A. Franco, Damien Jones, Antonio Kanaan, René Laporte, Antonio Magalhaes, André Milone, José Neri, Antonio Pereyra, Luiz A. Reitano, Karleyne M. Silva, Cesar Strauss
We present a summary of the concept design report of a new astronomical instrument: SPARC4, Simultaneous
Polarimeter and Rapid Camera in 4 bands. SPARC4 will provide photometry and polarimetry in four optical
broad bands (griz SDSS) simultaneously. This is achieved by the use of dichroic beam splitters. The square eld
of view is around 5.6 arcmin on a side. SPARC4 time resolution is sub-second for photometry and somewhat
longer for polarimetry. This is provided by the use of fast EMCCDs. The main motivation for building SPARC4
is to explore astrophysical objects which exhibit fast temporal variability in
ux and polarization. The instrument
will be installed at the 1.6-m telescope of the Observatorio do Pico dos Dias (Brazil).
The Prime Focus Spectrograph (PFS) of the Subaru Measurement of Images and Redshifts (SuMIRe) project has been
endorsed by Japanese community as one of the main future instruments of the Subaru 8.2-meter telescope at Mauna Kea,
Hawaii. This optical/near-infrared multi-fiber spectrograph targets cosmology with galaxy surveys, Galactic archaeology,
and studies of galaxy/AGN evolution.
Taking advantage of Subaru’s wide field of view, which is further extended with the recently completed Wide Field
Corrector, PFS will enable us to carry out multi-fiber spectroscopy of 2400 targets within 1.3 degree diameter. A
microlens is attached at each fiber entrance for F-ratio transformation into a larger one so that difficulties of spectrograph design are eased. Fibers are accurately placed onto target positions by positioners, each of which consists of two stages
of piezo-electric rotary motors, through iterations by using back-illuminated fiber position measurements with a widefield
metrology camera. Fibers then carry light to a set of four identical fast-Schmidt spectrographs with three color arms
each: the wavelength ranges from 0.38 μm to 1.3 μm will be simultaneously observed with an average resolving power
of 3000.
Before and during the era of extremely large telescopes, PFS will provide the unique capability of obtaining spectra of
2400 cosmological/astrophysical targets simultaneously with an 8-10 meter class telescope. The PFS collaboration, led
by IPMU, consists of USP/LNA in Brazil, Caltech/JPL, Princeton, and JHU in USA, LAM in France, ASIAA in Taiwan,
and NAOJ/Subaru.
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