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1. The Sloan Digital Sky Survey Monitor Telescope Pipeline

Author

Tucker, D. L., Kent, S., Richmond, M. W., Annis, J., Smith, J. A., Allam, S. S., Rodgers, C. T., Stute, J. L., Adelman-McCarthy, J. K., Brinkmann, J., Doi, M., Finkbeiner, D., Fukugita, M., Goldston, J., Greenway, B., Gunn, J. E., Hendry, J. S., Hogg, D. W., Ichikawa, S. -I., Ivezic, Z., Knapp, G. R., Lampeitl, H., Lee, B. C., Lin, H., McKay, T. A., Merrelli, A., Munn, J. A., Neilsen, Jr., E. H., Newberg, H. J., Richards, G. T., Schlegel, D. J., Stoughton, C., Uomoto, A., and Yanny, B.

Subjects
Astrophysics
Abstract

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi-step process which involves data from three different telescopes: the 1.0-m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5-m Photometric Telescope (PT) at the Apache Point Observatory (APO), New Mexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5-m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single-CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0-m and the PT). We also describe transformation equations that convert photometry on the USNO-1.0m u'g'r'i'z' system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi-automated PT factory, which runs MTPIPE in the day-to-day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS-related projects, including the Southern u'g'r'i'z' Standard Star project, the u'g'r'i'z' Open Star Clusters project, and the SDSS extension (SDSS-II)., Comment: 24 pages, 16 figures (1 color), accepted for publication in Astronomische Nachrichten

Published
2006
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4. The Sloan Digital Sky Survey monitor telescope pipeline

Author

Department of Physics, University of Michigan, 500 East University, Ann Arbor, MI 48109-1120, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Dept. of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Physics Department, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623-5603, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA, Deptartment of Physics & Astronomy, Austin Peay State University, P.O. Box 4608, Clarksville, TN 37044 USA ; Los Alamos National Laboratory, ISR-4, MS D448, Los Alamos, NM 87545-0000, USA ; Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA, Institute of Astronomy, School of Science, University of Tokyo, Osawa 2-21-1, Mitaka, Tokyo 181-0015, Japan, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ; Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA, Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa, Kashiwa City, Chiba 277-8582, Japan, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; University of California at Berkeley, Depts. of Physics and Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA, National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; Department of Astronomy, University of Washington, Box 351580, Seattle WA 98195-1580 USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley CA 94720-8160, USA, Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15232, USA ; Dept. of Astronomy, 105-24, California Inst. of Tech., 1201 East California Boulevard, Pasadena, CA 91125, USA, US Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002, USA, Dept. of Physics, Appl. Phys., Astron., Rensselaer Polytech. Inst., 100 Eighth Street, Troy, NY 12180-3590, USA, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley CA 94720-8160, USA, Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA, Kent, S., Richmond, M. W., Annis, J., Smith, J. A., Allam, S. S., Rodgers, C. T., Stute, J. L., Adelman-Mc Carthy, J. K., Brinkmann, J., Doi, M., Finkbeiner, D., Fukugita, M., Goldston, J., Greenway, B., Gunn, J. E., Hendry, J. S., Hogg, D. W., Ichikawa, S. -I., Ivezić, [zcaron]., Knapp, G. R., Lampeitl, H., Lee, B. C., Lin, H., McKay, T. A., Merrelli, A., Munn, J. A., Neilsen, E. H., Newberg, H. J., Richards, G. T., Schlegel, D. J., Stoughton, C., Uomoto, A., Yanny, B., Department of Physics, University of Michigan, 500 East University, Ann Arbor, MI 48109-1120, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Dept. of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA, Physics Department, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623-5603, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA, Deptartment of Physics & Astronomy, Austin Peay State University, P.O. Box 4608, Clarksville, TN 37044 USA ; Los Alamos National Laboratory, ISR-4, MS D448, Los Alamos, NM 87545-0000, USA ; Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA, Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA, Institute of Astronomy, School of Science, University of Tokyo, Osawa 2-21-1, Mitaka, Tokyo 181-0015, Japan, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ; Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA, Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa, Kashiwa City, Chiba 277-8582, Japan, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; University of California at Berkeley, Depts. of Physics and Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA, National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; Department of Astronomy, University of Washington, Box 351580, Seattle WA 98195-1580 USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley CA 94720-8160, USA, Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15232, USA ; Dept. of Astronomy, 105-24, California Inst. of Tech., 1201 East California Boulevard, Pasadena, CA 91125, USA, US Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002, USA, Dept. of Physics, Appl. Phys., Astron., Rensselaer Polytech. Inst., 100 Eighth Street, Troy, NY 12180-3590, USA, Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ; Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley CA 94720-8160, USA, Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA, Kent, S., Richmond, M. W., Annis, J., Smith, J. A., Allam, S. S., Rodgers, C. T., Stute, J. L., Adelman-Mc Carthy, J. K., Brinkmann, J., Doi, M., Finkbeiner, D., Fukugita, M., Goldston, J., Greenway, B., Gunn, J. E., Hendry, J. S., Hogg, D. W., Ichikawa, S. -I., Ivezić, [zcaron]., Knapp, G. R., Lampeitl, H., Lee, B. C., Lin, H., McKay, T. A., Merrelli, A., Munn, J. A., Neilsen, E. H., Newberg, H. J., Richards, G. T., Schlegel, D. J., Stoughton, C., Uomoto, A., and Yanny, B.

Abstract

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi-step process which involves data from three different telescopes: the 1.0-m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5-m Photometric Telescope (PT) at the Apache Point Observatory (APO), NewMexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5-m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single-CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0-m and the PT). We also describe transformation equations that convert photometry on the USNO-1.0m u ′ g ′ r ′ i ′ z ′ system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi-automated PT factory, which runs MTPIPE in the day-to-day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS-related projects, including the Southern u ′ g ′ r ′ i ′ z ′ Standard Star project, the u ′ g ′ r ′ i ′ z ′ Open Star Clusters project, and the SDSS extension (SDSS-II). (© 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

Published
2007

11. Robust and selective nano cavities for protein separation: an interpenetrating polymer network modified hierarchically protein imprinted hydrogel.

Author

Nematollahzadeh A, Lindemann P, Sun W, Stute J, Lütkemeyer D, and Sellergren B

Subjects
Adsorption, Chromatography, High Pressure Liquid methods, Humans, Hydrogel, Polyethylene Glycol Dimethacrylate chemistry, Hydrogels chemistry, Microscopy, Electron, Scanning, Microscopy, Electron, Transmission, Porosity, Solid Phase Extraction methods, Spectroscopy, Fourier Transform Infrared, Immunoglobulin G analysis, Molecular Imprinting methods, Polymers chemistry, Serum Albumin analysis
Abstract

In the present work, we report a novel method for the reinforcement of hierarchically structured molecularly imprinted polymer (MIP) for the separation of human serum albumin (HSA) and immunoglobulin G (IgG) proteins under pressure driven flow conditions. The template proteins (HSA or IgG) were first physically adsorbed at their isoelectric point on the surface of wide pore silica particles. Thereafter, the pore system was filled with a monomer solution and polymerized to form a lightly crosslinked polyacrylamide network covering the protein template. In order to enhance the rigidity of the hydrogels, different type of crosslinkers such as ethylene glycol dimethacrylate (EGDMA), 3,4-dihydroxyphenethylamine (DA) and methylene-bis-acrylamide (MBA), at least partially interpenetrated into the initially made acrylamide base hydrogel leading to formation of an interpenetrating polymer network (IPN). Then the silica matrix was removed to leave highly porous and reinforced MIP. TGA together with FT-IR and TEM analysis supported the interpenetration of the secondary crosslinkers in the initially formed polymer matrix. The compression property of the modified hydrogels as a function of degree of swelling was in the following order: DA>EGDMA>MBA-IPN-modified hydrogel. Batch binding assay verified the capability of the IPN modified MIPs to capture the target proteins. Moreover, solid phase extraction, HPLC and SDS-PAGE revealed that the EGDMA modified MIP could selectively capture and separate the proteins from human serum or fermentation broth., (Copyright © 2014 Elsevier B.V. All rights reserved.)

Published
2014
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13. Kinetic analysis of the binding of hemopexin-like domain of gelatinase B cloned and expressed in Pichia pastoris to tissue inhibitor of metalloproteinases-1.

Author

Stute J, Pourmotabbed T, and Tschesche H

Subjects
Kinetics, Matrix Metalloproteinase 9 genetics, Matrix Metalloproteinase 9 isolation & purification, Protein Binding, Protein Structure, Tertiary, Surface Plasmon Resonance, Tissue Inhibitor of Metalloproteinase-1 genetics, Hemopexin chemistry, Matrix Metalloproteinase 9 chemistry, Matrix Metalloproteinase 9 metabolism, Pichia genetics, Tissue Inhibitor of Metalloproteinase-1 metabolism
Abstract

The gelatinases are a subgroup of the matrix metalloproteinase family. The interaction of their C-terminal hemopexin-like domain with a tissue inhibitor of metalloproteinases (TIMP) is a major part of the regulatory mechanisms of gelatinases. To investigate the interaction of the hemopexin-like domain of gelatinase B (92-Pex) and TIMP-1, we expressed the individual domain in Pichia pastoris. The active refolded domain was purified by ion exchange chromatography and gel filtration. We investigated the formation of the 92-Pex/TIMP-1 complex by surface plasmon resonance (SPR). The dissociation constant Kd was calculated to be 0.86 nM. Analogous to the complex of the hemopexin-like domain of gelatinase A and TIMP-2 (Olson, M. W. et al., 1997), the binding curves of the 92-Pex/TIMP-1 complex were best fitted with a monophasic model.

Published
2003
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14. [Andrological problems with foreign workers (author's transl)].

Author

Stute J

Subjects
Adult, Epidermolysis Bullosa genetics, Ethnicity, Female, Germany, West, Humans, Male, Pregnancy, Emigration and Immigration, Infertility, Male diagnosis
Abstract

Since 20 years more and more foreign workers are employed in the Federal Republic of Germany. In view of the innumerable so far unsolved social problems like for example housing and school problems the ambition to have many children seems to be paradox at first glance. In the home country of the men the children are in important factor of protection concerning age and illness. If these people don't succeed in getting a child of their own, they react with despair and depression. The ability of the man to guarantee the subsequent existence depends among others from the number of children he generates and this is at the same time an important way of documenting his virility. And in addition to that it may be assumed that the relations mentioned above will be enforced by religious norms.

Published
1981

15. [Diphenylcyclopropenone - a new strong contact sensitizer (author's transl)].

Author

Stute J, Hausen BM, and Schulz KH

Subjects
Adult, Animals, Cross Reactions, Dose-Response Relationship, Drug, Guinea Pigs, Humans, Male, Skin immunology, Cyclopropanes immunology, Dermatitis, Occupational immunology
Abstract

A new synthetic substance - diphenylcyclopropenone - has been proven to be responsible for contact dermatitis in three persons handling it in chemical laboratories. A student of chemistry developed a dermatitis of the hands that lasted for more than two months. Based on the case history this dermatitis was considered to be an allergic one. The sensitizing capacity of diphenylcyclopropenone was proven experimentally in guinea pigs by use of the open epicutaneous sensitization method. All 25 animals became strongly sensitive. Sensitization could also be induced by a single application of low concentrations, for example with 3% in acetone. Cross-reactions could be elicited in the sensitized animals by intermediate produts and the synthesis like alpha, alpha'-dibromdibenzylketone and the remaining procduct called "red oil". The intermediate product is a mixture of racemic d- and l-forms and a meso-form as well, whereas the "red oil" consists of polymerized carbonyl compounds, from which diphenylcyclopropenone is extracted with boiling cyclohexane. Risk of contact with the sensitizer is greatest in the last step of synthesis. Care should not only be taken while handling this new substance in chemical laboratories, but contact should also be avoided with the intermediate and end products in cases where a diphenylcyclopropenone contact allergy is present.

Published
1981

17. [Relationship between the skin test and the specific IgE (radio-allergo-sorbens test) in the diagnosis of inhalative allergies].

Author

Brückner V, Noster U, Schulz KH, and Stute J

Subjects
Asthma diagnosis, Chronic Disease, Coombs Test, Factor Analysis, Statistical, Humans, Hypersensitivity, Immediate, Methods, Rhinitis diagnosis, Rhinitis, Allergic, Seasonal diagnosis, Immunoglobulin E analysis, Respiratory Hypersensitivity diagnosis, Skin Tests
Abstract

Immediate-type reactions such as asthma, pollinosis and several forms of urticaria can be regarded as type I reactions according to Coombs and Gell. Primary these diseases are caused by the immune globulin E. As skin testing is accompanied by numerous failors, there is a real possibility in increasing the diagnostic relevance by measurement of the specific IgE in serum (Radio-Allergo-Sorbens-Test = RAST; Phadebas-RAST -- Pharmacia Uppsala). There are often found divergent results and therefore this investigation was started. 1357 RAST-results (530 patients) were compared with skin tests in order to investigate the concordance of the two test-methods. The statistical analysis is performed wit "4-square-Chi2". Very good correspondence could be calculated for the pollens of Festuca elatior, Poa pratensis, horse-epithelium and housedustmite (1 0/00O significancy). 1 0/0 significancy was found for catepithelium and 5 0/0 for Birch-pollen. The advantages and the disadventages of RAST are discussed.

Published
1977

18. [Nutritional habits and protein status of surgical patients during the preclinical phase].

Author

Bessert I and Stute J

Subjects
Blood Proteins analysis, Body Weight, Gastrectomy, Humans, Immunoglobulins analysis, Postoperative Complications, Serum Albumin analysis, Skinfold Thickness, Nutritional Physiological Phenomena, Preoperative Care
Abstract

In this study the importance of nutrition during the preoperative period has to be find out. Three methods are helpful in it: 1. anamnesis of nutrition; 2. status of the subcutaneous fat tissue by measuring the skinfolds with a Harpenden-Caliper; 3. proteinstatus. 24 patients after gastric surgery and 20 patients of a control group were investigated. There was found a loss of weight inabout half of these 24 "gastric patients" preoperatively. These special patients showed a malnutrition in their anamnesis, thin skinfolds, low serum albumin and total protein concentration and a decreased concentration of immunoglobulins. They got six times more infectious complicationes than the patients without a preoperative loss of weight. It is proposed to develop an adequate plan for preoperative and post-operative nutrition.

Published
1977

19. [Olfactometric, psychological studies in asthma patients].

Author

Stute J

Subjects
Acetone, Adaptation, Physiological, Adolescent, Adult, Asthma complications, Butyrates, Female, Humans, Hypersensitivity complications, Male, Menstruation, Middle Aged, Oils, Volatile, Personality Inventory, Plants, Medicinal, Psychoanalytic Theory, Sinusitis physiopathology, Smoking, Socioeconomic Factors, Asthma physiopathology, Smell
Published
1972

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