Annual Report 2011 Max Planck Institute for Astronomy

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72 IV. Instrumental Developments and Projects Credit: Morganson et al., arXiv:1109.6241 Flux [10 –21 W / (m 2 nm)] 0.9 0.6 0.3 0 0.9 0.6 0.3 0 0.9 0.6 0.3 0 MMT spectrum CAHA spectrum PS1 total efficiency 700 i z y 800 900 1000 Observed Wavelength [nm] Fig. IV.1.2: The spectra of the first PS1 high-redshift quasar obtained by MMT and Calar Alto as well as the PS1 iP1, zP1, yP1 filter curves. These data will fill the V 10–15 mag gap between the Hipparcos photometry of bright stars, the deep photometry of PS1 and SDSS. This range is crucial for the detailed study of the closest cool stars and is only available with large uncertainties from the plate surveys. Other surveys of interest to us are the Medium Deep Survey, which monitors daily up to four pointings, and cover 70 square degrees, and the PanPlanets survey dedicated to the search over transiting exoplanets, particularly around M-type dwarfs. Published results cover the Solar system and near- Earth asteroids up to the most distant quasars, with a z 6.0 quasar discovered at MPIA. As the first deep, wide, high-accuracy optical survey, PS1 is a unique resource for the community. Prior to its full data release expected 2015, it has established Memoranda of Understanding with several large projects with other wavelength coverage or spectral resolutions, which greatly benefit from the PS1 catalogue. High-schools in Heidelberg and world-wide have access to the images to search for asteroids, and have successfully done so. Early Results obtained at MPIA MPIA has concentrated its efforts in four main areas: very-low mass stars and brown dwarfs of the solar neighbourhood, exoplanets, the structure of the Milky Way, and Quasars. Our search for cool brown dwarfs of the solar neighbourhood firstly involved cross-matching with 2MASS and selecting red y-J candidates. As SDSS before, PS1 has the right wavelength sensitivity to detect the early T-type dwarfs. Over 40 new T-type dwarfs have been discovered (Deacon et al., 2011, AJ 142, 77). A crossmatch with WISE is underway. Proper motions based on 2MASS and PS1 data also revealed new brown dwarf companions to Hipparcos stars (Deacon et al., arXiv:1109.6319), providing new benchmark objects to calibrate the brown dwarf models. We take advantage of the wide sky coverage of PS1 to study the nearby 625-Myr-old Hyades cluster. We can select cluster candidates to large cluster radii (30 pc) to study the cluster evaporation, especially close to the stellar/brown dwarf boundary (Goldman et al., submitted to A&A). We confirm previous indications of mass segregation with a larger significance and the lack of low-mass members at the cluster centre. The PS1 survey also offers an unprecedented look at the structure of our Galaxy, with deep, uniform optical data in five bands covering the whole Galactic plane in addition to the Northern Galactic Cap. The MPIA leads the PS1 science collaboration’s study of the Galaxy. Our research in this area includes: a search for new dwarf galaxies, the characterisation of the structure of the Monoceros stream, and mapping the Galaxy’ dust. Regarding our quasar work, we first use the deep z– and y–band imaging to select for optical dropout highredshift candidates. We found the first PS1 high-redshift quasar (Morganson et al., arXiv:1109.6241: The First High-redshift Quasar from Pan-StarrS) at redshift 6 (see Figure IV.1.2); the prospect to discover z 7 QSOs is promising. B. Goldman, E. Bañados, N. Deacon, T. Henning, N. Martin, E. Morganson, H.-W. Rix, B. Venemans, F. Walter In collaboration with partner institutes of the PS1 Science Consortium,in particular the Institute for Astronomy of the University of Hawaii; as well as the ZAH of the University of Heidelberg through the SFB 881 “The Milky Way”
IV.2 argoS: Laser guided Ground Layer Adaptive Optics for the LBT argoS, the Advanced Rayleigh Ground layer adaptive Optics System for the LBT goals on the improvement of the image quality for both Luci instruments by a factor of 2–3 in full width half maximum, which increases the spectroscopic efficiency by a factor of 4–9. All this will be provided for the full 4 arcmin field of view of both Luci instruments and their multi-object capability by the means of 6 green Rayleigh laser guide stars. As argoS only corrects for the turbulence in the lower atmosphere (the so called ground layer) the full diffraction limit will not be reached. However, from the beginning argoS incooperated an on-axis diffraction limited upgrade with a Sodium laser into the design. MPIA is one of the three bigger partners in the argos consortium. In this role MPIA is responsible for the overall software and control, the calibration unit and the procurement of the dichroics, which separate the laser light to the wavefront sensor. Fig. IV.2.1: The swing arms in their shipping containment starting the long way from MPIA to the LBT at Mt. Graham, Arizona. In the last year the swing arm, which holds the calibration unit, was assembled at MPIA and shipped to the LBT. The swing arm is built out of carbon fiber, a new material, which will be also very important for building new large scale telescopes to light weight their structure. In August the swing arm was then installed at the telescope. The green laser light of the artificial guide stars has to be directed to the wavefront sensor. While the infrared light, used for science, should still reach the Luci instruments. This is done by the means of a so called dichroic, which transmits light of certain wavelengths, in our case the near infrared, and reflects light of other wavelengths, in our case the green light of the laser guide star. Such dichroics are often used in optical instruments but the size and shape, which was needed for argos was much bigger and more challenging as usual. During this year, the two dichroics needed for the right and left side of argos have been delivered to MPIA. They have been tested for transmission and reflection. The result of the measurements shows that they comply with all specifications and even surpass some of them. With this positive result one of the most critical components of argos are ready in time. At the end of next Credit: W. Gässler 73
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Contents Preface ..................
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6 I. General Credit: MPIA / AMQ I.
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8 I. General lows us to understand
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10 I. General Credit: CAHA I.2 Obse
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12 I. General in December 2009, the
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14 I. General Credit: eSo/l. calça
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16 I. General Point source sensitiv
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18 I. General I.3 National and Inte
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20 I. General Credit for both figur
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Page 26 and 27: 24 II. Highlights II. Highlights II
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Page 86 and 87: 84 V. People and Events times a yea
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Page 96 and 97: 94 V.3 Honors and Awards Ernst Patz
Page 98 and 99: 96 V. People and Events Andreas Sch
Page 100 and 101: 98 Staff Schultz (since 8.9.), Scor
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124 Publications formation efficien
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126 Publications Erroz Ferrer: Gran
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128 Publications Hansen, S. H., A.
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130 Publications L. Michaud, G. Mon
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132 Publications Notices of the Roy
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134 Publications Riechers, D. A., F
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136 Publications Hayano, T. Henning
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140 Publications Dzyurkevich, N., N
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142 Publications Mordasini, C., Y.
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144 Publications Astrophysics of Pl
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Annual Report 2011 Max Planck Institute for Astronomy

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