scholarly journals T A U M O K—Multi-Object Spectroscopy with the Tautenburg Schmidt Telescope

1995 ◽  
Vol 148 ◽  
pp. 52-52
Author(s):  
S. Marx ◽  
H. Lehmann ◽  
M. Pluto ◽  
R. Ziener
Keyword(s):  
Focal Plane ◽  
Ccd Camera ◽  
Entrance Slit ◽  
Pixel Size ◽  
Schmidt Telescope ◽  
Max Planck ◽  
Background Light ◽  
Convex Lens ◽  
Chip Size ◽  
Calar Alto

A multi-object camera for the Tautenburg Schmidt Telescope (134/200/400) was developed and constructed in cooperation with the Max-Planck-Institut für Astronomie in Heidelberg and the Thüringer Landesstemwarte Tautenburg. The experience with the “Spaltspinne” for the 3.5 m Telescope of the Calar Alto Observatory (Pitz 1993) was the foundation of TAUMOK. The technical concept was given by Pitz et al. (1993).Thirty six rods controlled by a processor can be moved in an area with a diameter of 16 cm. This area covers a field of 2.3° in the focal plane which is flattened by a plano-convex lens. Each of 34 rods carry two fibres with diameters of 100/µm with one fibre for the object and another for the background light. The fibres have a length of 7 m and their opposite faces form the entrance slit of a spectrograph. At present, reciprocal dispersions of 3.4, 10, 20 and 40 nm/mm can be realized. A CCD camera with a chip-size of 1152 × 770 pixels (pixel size 22.5/µm) is used as detector. Two of the 36 rods are equipped with image bundles for telescope guiding.

scholarly journals The Schmidt Telescope on Calar Alto

1984 ◽  
Vol 78 ◽  
pp. 203-206
Author(s):  
K. Birkle
Keyword(s):  
National Commission ◽  
Schmidt Telescope ◽  
Max Planck ◽  
Large Telescopes ◽  
Calar Alto

During the last ten years the Max-Planck-Institut fur Astronomie (MPIA) has installed four large telescopes at its observatory on Calar Alto, Spain, which is operated jointly with the Spanish National Commission for Astronomy as the German-Spanish Astronomical Center. Figure 1 shows the domes of the 1.2 m, 2.2 m, and 3.5 m telescopes of Ritchey-Chrétien type and the dome of the Schmidt Telescope. They all are Zeiss telescopes, the former three coming from Oberkochen, the latter one from Jena.

scholarly journals TAUMOK - a Multi-Object Spectrograph for the Tautenburg Schmidt Telescope

1995 ◽  
Vol 149 ◽  
pp. 219-220 ◽  
Author(s):  
H. Lehmann ◽  
R. Ziener ◽  
M. Ball ◽  
E. Pitz
Keyword(s):  
Test Phase ◽  
Wide Field ◽  
Schmidt Telescope ◽  
Max Planck ◽  
Site Specific ◽  
Joint Project ◽  
Ground Plate ◽  
The Mean ◽  
Calar Alto ◽  
Central Obscuration

TAUMOK is a joint project of the Max Planck Institut für Astronomie Heidelberg and the Thüringer Landessternwarte Tautenburg. It is based on the concept of the “Spaltspinne” (Pitz 1993) now in operation at the Calar Alto Observatory. A first describtion of the technical concept was given by Pitz et al. (1993). TAUMOK was built at the MPIA Heidelberg in collaboration with astronomers and technicians from Tautenburg. It is now in the test phase and will have its first operation at the Tautenburg telescope in the middle of this year.The use of a Schmidt telescope gives a very wide field for multi-object spectroscopy (TAUMOK will cover a field of 2.3°) but it also requires a series of special considerations. So, some of the details of the original “Spaltspinne” were modified to meet the site specific peculiarities. The size of the ground plate was minimized and yields a central obscuration of only 60 cm in diameter. The curved field of the Schmidt focus (deviation of up to ±400 µm from the mean focal plane) is flattened by a field lens - a solution alternative to the guiding of the fiber supporting rods on a sphere.

scholarly journals The Schmidt Telescope at Calar Alto Observatory

1994 ◽  
Vol 161 ◽  
pp. 46-48
Author(s):  
K. Birkle ◽  
H. Belleman ◽  
H. Elsässer
Keyword(s):  
Image Quality ◽  
Focal Length ◽  
Mechanical Instability ◽  
Schmidt Telescope ◽  
Max Planck ◽  
Excellent Performance ◽  
Telescope Optics ◽  
Calar Alto

The Schmidt telescope at Calar Alto Observatory, Spain, was installed there in 1980 by the Max-Planck-Institut für Astronomie, Heidelberg, and has been operated since then by this institute; originally it had been operational at the Hamburg Observatory since 1955. The corrector plate and mirror have 80 cm and 120 cm diameter respectively; focal length is 240 cm. A field 5.5 deg by 5.5 deg is photographed on 24 cm by 24 cm curved plates. Two objective prisms of 1.7 deg and 4.0 deg refractive angle are available (Heckmann 1955; Birkle 1984). Thousands of direct and spectral plates have been taken, mainly for the Hamburg Quasar Survey (Engels et al. 1988). Other observing programs referred e.g. to astrometry of comets, giving support to ESA's Giotto space encounters with comets Halley and Grigg-Skjellerup (Roeser et al. 1986; Morley 1992). Gradually, however, the number of plates increased showing image quality which did not correspond to the excellent performance of the telescope optics. Several technical improvements have therefore been installed to remove some obvious mechanical instability.

Observational Data and Orbits of the Asteroids Discovered at the Baldone Observatory in 2008–2013

2015 ◽  
Vol 24 (3) ◽  
Author(s):  
K. Černis ◽  
I. Wlodarczyk ◽  
I. Eglitis
Keyword(s):  
Observational Data ◽  
Ccd Camera ◽  
Minor Planet ◽  
Orbital Elements ◽  
Main Belt ◽  
Schmidt Telescope ◽  
Ccd Observations ◽  
Near Earth Objects ◽  
Asteroids And Comets

AbstractThe paper presents statistics of the asteroids observed and discovered at the Baldone Observatory, Latvia, in 2008–2013 within the project for astrometric observations of the near-Earth objects (NEOs), the main belt asteroids and comets. CCD observations of the asteroids were obtained with the 0.80/1.20 m, f/3 Schmidt telescope and a ST-10XME 15 × 10 mm CCD camera. In the Minor Planet Circulars and the Minor Planet Electronic Circulars (2008–2013) we published 3511 astrometric positions of 826 asteroids. Among them, 43 asteroids were newly discovered at Baldone. For 36 of these asteroids the precise orbits are calculated. Because of short observational arc and small number of observations, a few asteroids have low-precision orbits and their tracks have been lost. For seven objects with poorly known orbits we present their ephemerides for 2015–2016. The orbits and the evolution of orbital elements of two asteroids, (428694) 2008 OS9 from the Apollo group and the Centaur (330836) Orius (2009 HW77), are recalculated including new observations obtained after 2011.

scholarly journals An Automatic Approach for Selecting New HA Emission-Line Galaxies

1994 ◽  
Vol 161 ◽  
pp. 611-614
Author(s):  
O. Alonso ◽  
J. Zamorano ◽  
M. Rego ◽  
J. Gallego ◽  
A.G. Vitores
Keyword(s):  
Emission Line ◽  
Selection Criterion ◽  
Schmidt Telescope ◽  
Objective Prism ◽  
Emission Line Galaxies ◽  
Calar Alto ◽  
Observational Procedure

The most unambiguous way to discover new emission-line galaxies (ELGs) is directly by the presence of their lines, using objective-prism plates of adequate resolution. The first survey using this technique was developed by Smith in 1975 with the 0.6 m CTIO Curtis Schmidt Telescope. The Universidad Complutense de Madrid (UCM) is carrying out a survey of ELGs with the Schmidt Telescope at Calar Alto (Almería, Spain) using the presence of Ha in emission in IIIa-F prism plates as selection criterion. The observational procedure and results are described in Rego et al. 1989; Zamorano et al. 1990; Zamorano et al. 1993.

scholarly journals M.A.M.A. Project: A New Measuring Machine in Paris

1984 ◽  
Vol 78 ◽  
pp. 165-167 ◽  
Author(s):  
Jean Guibert ◽  
Pierre Charvin ◽  
Patrick Stoclet
Keyword(s):  
Data Acquisition ◽  
Linear Array ◽  
Transmitted Light ◽  
Array Processor ◽  
Pixel Size ◽  
Schmidt Telescope ◽  
Control Data ◽  
On Line ◽  
Measuring Machine ◽  
Under Construction

SummaryA new photographic measuring machine is under construction at Paris Observatory. The amount of transmitted light is measured by a linear array of 1024 photodiodes. Carriage control, data acquisition and on line processing are performed by microprocessors,a S.E.L. 32/27 computer, and an AP 120-B Array Processor. It is expected that a Schmidt telescope plate of size 360 mm square will be scanned in about one hour with pixel size of ten microns.

scholarly journals A Four Star Photometer

1993 ◽  
Vol 136 ◽  
pp. 179-186
Author(s):  
J.C. Valtier ◽  
J.M. Le Contel ◽  
P. Antonelli ◽  
P. Michel ◽  
J.P. Sareyan
Keyword(s):  
Real Time ◽  
Focal Plane ◽  
Ccd Camera ◽  
Simultaneous Acquisition ◽  
Comparison Stars

AbstractA new photometer is presently being developed at the O.C.A. Observatory. It consists of four arms and a CCD camera situated in the focal plane of the telescope. Each arm can move in both directions and support a diaphragm and a liquid optic guide that directs the light to a photomultiplier. The simultaneous acquisition of the four signals enables to obtain magnitude differences between the objects in real time. A typical use of this photometer is to observe at the same time one or two variables, comparison stars and the sky background.

scholarly journals MOCAM: A 4k × 4k CCD Mosaic for the Canada-France-Hawaii Telescope Prime Focus

1995 ◽  
Vol 167 ◽  
pp. 213-220
Author(s):  
J. C. Cuillandre ◽  
Y. Melliers ◽  
R. Murowinski ◽  
D. Crampton ◽  
G. Luppino ◽  
...  
Keyword(s):  
Focal Plane ◽  
San Diego ◽  
Ccd Camera ◽  
Astronomical Observatory ◽  
Wide Field ◽  
On Line ◽  
Readout Noise ◽  
The University ◽  
Filter Wheel ◽  
Better Than

MOCAM is a wide field CCD camera, currently nearing completion, which will be offered to the Canada-France-Hawaii Telescope (CFHT) user community in 1995. The project is a collaboration between the CFHT, the Dominion Astronomical Observatory (DAO, Canada), the Institut des Sciences de l'Univers (INSU, France), Laboratoire d'Astrophysique de Toulouse (LAT, France) and the University of Hawaii (UH). In the interests of producing a reliable and effective camera in the shortest time, it was decided to use existing technologies rather than innovative ones. Two-edge buttable 2048 × 2048 15 μm pixel CCDs were obtained from the LORAL aerospace foundry, based on a mask designed by J. Geary at Smithsonian Astrophysical Observatory (SAO). They are mounted in a dewar designed by G. Luppino (UH); the focal plane mounting keeps the mosaic flat to within two pixels and the CCDs are aligned to within two pixels. A mechanical interface designed and fabricated by the DAO holds a 150 mm shutter and a filter wheel which has a positioning repeatability better than five μm.The four CCDs are operated in parallel by a San Diego GenIII controller adapted by LAT. The mosaic is read out in seven minutes and a single 33 Mb FITS file is generated to enable convenient on-line preprocessing. The user will control the system through a single CFHT Pegasus environment session. The camera field is 14′ × 14′ with a 0.″2 pixel sampling and the readout noise is less than seven electrons. The scientific goals of the initiators of the project are studies of distant clusters, deep galaxy counts and quasars surveys.

Measurement on roughness of optical surface by focal plane CCD camera

1998 ◽  
Author(s):  
Jianbai Li ◽  
Xiaoyun Li ◽  
Aihan Ying ◽  
Anqing Zao ◽  
Xiaolin Zhang
Keyword(s):  
Focal Plane ◽  
Ccd Camera ◽  
Optical Surface

scholarly journals Observations of QSOs and related objects with EFOSC, the ESO faint object spectrograph and camera

1986 ◽  
Vol 119 ◽  
pp. 57-58
Author(s):  
S. D'Odorico ◽  
S. Cristiani ◽  
R.G. Clowes ◽  
C.J. Keable
Keyword(s):  
Focal Plane ◽  
Optical Design ◽  
Pixel Size ◽  
Direct Imaging ◽  
Operating Modes ◽  
Multiple Object ◽  
Faint Object ◽  
Collimated Beam ◽  
Faint Object Spectrograph ◽  
Back Illuminated

EFOSC is a standard ESO instrument operating at the Cassegrain focus of the 3.6 m telescope since April 1st, 1985. A description of its optical design and operating modes is given in Enard and Delabre (1982) and Dekker and D'Odorico (1985). Briefly, it is a focal reducer with spectroscopic capability. The collimator produces a collimated beam with a diameter of 40 mm which passes through a filter and/or grism. The f/2.5 camera focusses the beam on the detector which is at present a thinned, back-illuminated RCA CCD with 320×512 pixels. The pixel size is 30 μm which corresponds to .675″ on the sky. There are three remotely controlled wheels in the instrument: the aperture wheel in the focal plane of the telescope, with long slits of different widths, a filter and a grism wheel with 12 positions each. The instrument can be operated in four different modes: direct imaging, slit spectroscopy, grism or multiple object spectroscopy with specially made aperture plates.

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