S. Kellner
Max Planck Society
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Featured researches published by S. Kellner.
Astrophysical Journal Supplement Series | 2007
Beth A. Biller; Laird M. Close; Elena Masciadri; Eric L. Nielsen; Rainer Lenzen; Wolfgang Brandner; Donald W. McCarthy; Markus Hartung; S. Kellner; Eric E. Mamajek; Thomas Henning; Douglas L. Miller; Matthew A. Kenworthy; Craig Kulesa
Wepresent theresultsof asurveyof 45young(P250Myr), close(P50pc) starswiththeSimultaneous Differential Imager (SDI) implemented at the VLT and the MMT for the direct detection of extrasolar planets. As part of the survey, we observed 54 objects, consisting of 45 close, young stars; two more distant ( 2 � which behaved consistently like a real object. From our survey null result,we can rule out (with 93% confidence) a model planet population where N(a) / constant out to a distance of 45 AU.
Proceedings of SPIE | 2008
F. Eisenhauer; G. Perrin; Wolfgang Brandner; C. Straubmeier; A. Richichi; S. Gillessen; J.-P. Berger; Stefan Hippler; A. Eckart; M. Schöller; S. Rabien; F. Cassaing; Rainer Lenzen; M. Thiel; Y. Clénet; J. Ramos; S. Kellner; Pierre Fedou; Harald Baumeister; R. Hofmann; Eric Gendron; Armin Boehm; H. Bartko; X. Haubois; R. Klein; K. Dodds-Eden; K. Houairi; Felix Hormuth; A. Gräter; L. Jocou
We present the second-generation VLTI instrument GRAVITY, which currently is in the preliminary design phase. GRAVITY is specifically designed to observe highly relativistic motions of matter close to the event horizon of Sgr A*, the massive black hole at center of the Milky Way. We have identified the key design features needed to achieve this goal and present the resulting instrument concept. It includes an integrated optics, 4-telescope, dual feed beam combiner operated in a cryogenic vessel; near infrared wavefront sensing adaptive optics; fringe tracking on secondary sources within the field of view of the VLTI and a novel metrology concept. Simulations show that the planned design matches the scientific needs; in particular that 10µas astrometry is feasible for a source with a magnitude of K=15 like Sgr A*, given the availability of suitable phase reference sources.
Proceedings of SPIE | 2010
S. Gillessen; F. Eisenhauer; G. Perrin; Wolfgang Brandner; C. Straubmeier; K. Perraut; A. Amorim; M. Schöller; Constanza Araujo-Hauck; H. Bartko; Harald Baumeister; Jean-Philippe Berger; Pedro Carvas; F. Cassaing; F. Chapron; E. Choquet; Y. Clénet; C. Collin; A. Eckart; Pierre Fedou; Sebastian Fischer; Eric Gendron; R. Genzel; Philippe B. Gitton; F. Gonte; A. Gräter; P. Haguenauer; M. Haug; X. Haubois; T. Henning
GRAVITY is an adaptive optics assisted Beam Combiner for the second generation VLTI instrumentation. The instrument will provide high-precision narrow-angle astrometry and phase-referenced interferometric imaging in the astronomical K-band for faint objects. We describe the wide range of science that will be tackled with this instrument, highlighting the unique capabilities of the VLTI in combination with GRAVITY. The most prominent goal is to observe highly relativistic motions of matter close to the event horizon of Sgr A*, the massive black hole at center of the Milky Way. We present the preliminary design that fulfils the requirements that follow from the key science drivers: It includes an integrated optics, 4-telescope, dual feed beam combiner operated in a cryogenic vessel; near-infrared wavefrontsensing adaptive optics; fringe-tracking on secondary sources within the field of view of the VLTI and a novel metrology concept. Simulations show that 10 μas astrometry within few minutes is feasible for a source with a magnitude of mK = 15 like Sgr A*, given the availability of suitable phase reference sources (mK = 10). Using the same setup, imaging of mK = 18 stellar sources in the interferometric field of view is possible, assuming a full night of observations and the corresponding UV coverage of the VLTI.
The Astrophysical Journal | 2006
Beth A. Biller; Markus Kasper; Laird M. Close; Wolfgang Brandner; S. Kellner
This paper was accidentally submitted twice to astro-ph. This version has been withdrawn -- please see astro-ph/0601440 instead.
Proceedings of SPIE | 2006
D. Bonaccini Calia; Eric Allaert; J. L. Alvarez; C. Araujo Hauck; Gerardo Avila; Eduardo Bendek; Bernard Buzzoni; Mauro Comin; Martin J. Cullum; R. Davies; Martin Dimmler; I. Guidolin; W. Hackenberg; Stefan Hippler; S. Kellner; A. van Kesteren; Franz Koch; U. Neumann; T. Ott; Dan Popovic; Fernando Pedichini; Marco Quattri; J. Quentin; S. Rabien; Armin Silber; Mario Tapia
Two teams of scientists and engineers at Max Planck Institut fuer Extraterrestrische Physik and at the European Southern Observatory have joined forces to design, build and install the Laser Guide Star Facility for the VLT. The Laser Guide Star Facility has now been completed and installed on the VLT Yepun telescope at Cerro Paranal. In this paper we report on the first light and first results from the Commissioning of the LGSF.
arXiv: Astrophysics | 2005
G. Kanbach; A. Slowikowska; S. Kellner; H. Steinle
The Crab nebula and its pulsar have been observed for about 3 hours with the high‐speed photo‐polarimeter OPTIMA in January 2002 at the Calar Alto 3.5 m telescope. The Crab pulsar intensity and polarization are determined at all phases of rotation with higher statistical accuracy than ever. Therefore, we were able to separate the so‐called ‘off‐pulse’ phase emission (with an intensity of about 1.2% compared to the main peak, assumed to be present at all phases) from the pulsed emission and show the ‘net’ polarization of the pulsed structures. Recent theoretical results indicate that the measured optical polarization of the Crab pulsar is similar to expectations from a two‐pole caustic emission model or a striped pulsar wind model.
Astronomical Telescopes and Instrumentation | 2003
Domenico Bonaccini; Eric Allaert; C. Araujo; Enzo Brunetto; Bernard Buzzoni; Mauro Comin; Martin J. Cullum; R. Davies; C. Dichirico; Philippe Dierickx; Martin Dimmler; Michel Duchateau; C. Egedal; W. Hackenberg; Stefan Hippler; S. Kellner; A. van Kesteren; Franz Koch; U. Neumann; T. Ott; Marco Quattri; J. Quentin; S. Rabien; Roberto Tamai; Mario Tapia; M. Tarenghi
We report on the ongoing VLT Laser Guide Star Facility project, which will allow the ESO UT4 telescope to produce an artificial reference star for the Adaptive Optics systems NAOS-CONICA and SINFONI. A custom developed dye laser producing >10W CW at 589nm is installed on-board of the UT4 telescope, then relayed by means of a single mode optical fiber behind the secondary mirror, where a 500mm diameter lightweight, f/1 launch telescope is projecting the laser beam at 90 km altitude. We described the design tradeoffs and provide some details of the chosen subsystems. This paper is an update including subsystems results, to be read together with our previous paper on LGSF design description.
arXiv: Astrophysics | 2005
Beth A. Biller; Laird M. Close; Rainer Lenzen; Wolfgang Brandner; Donald W. McCarthy; Eric L. Nielsen; S. Kellner; Markus Hartung
We discuss the instrumental and data reduction techniques used to suppress speckle noise with the Simultaneous Differential Imager (SDI) implemented at the VLT and the MMT. SDI uses a quad filter to take images simultaneously at 3 wavelengths surrounding the 1.62
Proceedings of SPIE | 2014
N. Blind; F. Eisenhauer; M. Haug; S. Gillessen; Magdalena Lippa; L. Burtscher; Oliver Hans; F. Haussmann; S. Huber; A. Janssen; S. Kellner; Y. Kok; T. Ott; O. Pfuhl; E. Sturm; J. Weber; E. Wieprecht; A. Amorim; Wolfgang Brandner; G. Perrin; K. Perraut; C. Straubmeier
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Proceedings of SPIE | 2010
O. Pfuhl; F. Eisenhauer; M. Haug; M. Thiel; S. Kellner; A. Amorim; Wolfgang Brandner; Jean-Philippe Berger; Karine Rousselet-Perraut; G. Perrin; C. Straubmeier; S. Gillessen; H. Bartko; A. Gräter
m methane bandhead found in the spectrum of cool brown dwarfs and gas giants. By performing a difference of images in these filters, speckle noise from the primary can be significantly attenuated, resulting in photon noise limited data. Non-trivial data reduction tools are necessary to pipeline the simultaneous differential imaging. Here we discuss a custom algorithm implemented in IDL to perform this reduction. The script performs basic data reduction tasks but also precisely aligns images taken in each of the filters using a custom shift and subtract routine. In our survey of nearby young stars at the VLT and MMT (see Biller et al. , this conference), we achieved H band contrasts >25000 (5