Search

Your search keyword '"Brand, K"' showing total 1,727 results
Start Over Author "Brand, K"
1,727 results on '"Brand, K"'

1. Rapid Variability of Mrk 421 During Extreme Flaring as Seen Through the Eyes of XMM-Newton

Author

Gokus, A., Wilms, J., Kadler, M., Dorner, D., Nowak, M. A., Kreikenbohm, A., Leiter, K., Bretz, T., Schleicher, B., Markowitz, A. G., Pottschmidt, K., Mannheim, K., Kreykenbohm, I., Langejahn, M., McBride, F., Beuchert, T., Dauser, T., Kreter, M., Abhir, J., Baack, D., Balbo, M., Biland, A., Brand, K., Buss, J., Eisenberger, L., Elsaesser, D., Guenther, P., Hildebrand, D., Linhoff, M., Paravac, A., Rhode, W., Sliusar, V., Hasan, S., and Walter, R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

By studying the variability of blazars across the electromagnetic spectrum, it is possible to resolve the underlying processes responsible for rapid flux increases, so-called flares. We report on an extremely bright X-ray flare in the high-peaked BL Lacertae object Mrk 421 that occurred simultaneously with enhanced $\gamma$-ray activity detected at very high energies (VHE) by FACT on 2019 June 9. We triggered an observation with XMM-Newton, which observed the source quasi-continuously for 25 hours. We find that the source was in the brightest state ever observed using XMM-Newton, reaching a flux of $2.8\times10^{-9}$ erg cm$^{-2}$ s$^{-1}$ over an energy range of 0.3 - 10 keV. We perform a spectral and timing analysis to reveal the mechanisms of particle acceleration and to search for the shortest source-intrinsic time scales. Mrk 421 exhibits the typical harder-when-brighter behaviour throughout the observation and shows a clock-wise hysteresis pattern, which indicates that the cooling dominates over the acceleration process. While the X-ray emission in different sub-bands is highly correlated, we can exclude large time lags as the computed zDCFs are consistent with a zero lag. We find rapid variability on time scales of 1 ks for the 0.3 - 10 keV band and down to 300s in the hard X-ray band (4 - 10 keV). Taking these time scales into account, we discuss different models to explain the observed X-ray flare, and find that a plasmoid-dominated magnetic reconnection process is able to describe our observation best., Comment: 13 pages, 7 figures, accepted for publication in MNRAS

Published
2024

3. Rapid variability of Markarian 421 during extreme flaring as seen through the eyes of XMM–Newton

Author

Gokus, A, primary, Wilms, J, additional, Kadler, M, additional, Dorner, D, additional, Nowak, M A, additional, Kreikenbohm, A, additional, Leiter, K, additional, Bretz, T, additional, Schleicher, B, additional, Markowitz, A G, additional, Pottschmidt, K, additional, Mannheim, K, additional, Kreykenbohm, I, additional, Langejahn, M, additional, McBride, F, additional, Beuchert, T, additional, Dauser, T, additional, Kreter, M, additional, Abhir, J, additional, Baack, D, additional, Balbo, M, additional, Biland, A, additional, Brand, K, additional, Buss, J, additional, Eisenberger, L, additional, Elsaesser, D, additional, Günther, P, additional, Hildebrand, D, additional, Linhoff, M, additional, Paravac, A, additional, Rhode, W, additional, Sliusar, V, additional, Hasan, S, additional, and Walter, R, additional

Published
2024
Full Text
View/download PDF

4. Activation of GSK3 Prevents Termination of TNF-Induced Signaling

Author

Welz B, Bikker R, Hoffmeister L, Diekmann M, Christmann M, Brand K, and Huber R

Subjects
tnf, gsk3, pkc, staurosporine, il-8, nf-κb, termination of tnf-induced signaling, termination of inflammation, Pathology, RB1-214, Therapeutics. Pharmacology, RM1-950
Abstract

Bastian Welz,* Rolf Bikker,* Leonie Hoffmeister, Mareike Diekmann, Martin Christmann, Korbinian Brand,* René Huber* Institute of Clinical Chemistry, Hannover Medical School, Hannover, 30625, Germany*These authors contributed equally to this workCorrespondence: Korbinian BrandInstitute of Clinical Chemistry, Hannover Medical School, Carl-Neuberg Str. 1, Hannover, 30625, GermanyTel +49 511 532 6614Fax +49 511 532 8614Email brand.korbinian@mh-hannover.deBackground: Termination of TNF-induced signaling plays a key role in the resolution of inflammation with dysregulations leading to severe pathophysiological conditions (sepsis, chronic inflammatory disease, cancer). Since a recent phospho-proteome analysis in human monocytes suggested GSK3 as a relevant kinase during signal termination, we aimed at further elucidating its role in this context.Materials and Methods: For the analyses, THP-1 monocytic cells and primary human monocytes were used. Staurosporine (Stauro) was applied to activate GSK3 by inhibiting kinases that mediate inhibitory GSK3α/β-Ser21/9 phosphorylation (eg, PKC). For GSK3 inhibition, Kenpaulone (Ken) was used. GSK3- and PKC-siRNAs were applied for knockdown experiments. Protein expression and phosphorylation were assessed by Western blot or ELISA and mRNA expression by qPCR. NF-κB activation was addressed using reporter gene assays.Results: Constitutive GSK3β and PKCβ expression and GSK3α/β-Ser21/9 and PKCα/βII-Thr638/641 phosphorylation were not altered during TNF long-term incubation. Stauro-induced GSK3 activation (demonstrated by Bcl3 reduction) prevented termination of TNF-induced signaling as reflected by strongly elevated IL-8 expression (used as an indicator) following TNF long-term incubation. A similar increase was observed in TNF short-term-exposed cells, and this effect was inhibited by Ken. PKCα/β-knockdown modestly increased, whereas GSK3α/β-knockdown inhibited TNF-induced IL-8 expression. TNF-dependent activation of two NF-κB-dependent indicator plasmids was enhanced by Stauro, demonstrating transcriptional effects. A TNF-induced increase in p65-Ser536 phosphorylation was further enhanced by Stauro, whereas IκBα proteolysis and IKKα/β-Ser176/180 phosphorylation were not affected. Moreover, PKCβ-knockdown reduced levels of Bcl3. A20 and IκBα mRNA, both coding for signaling inhibitors, were dramatically less affected under our conditions when compared to IL-8, suggesting differential transcriptional effects.Conclusion: Our results suggest that GSK3 activation is involved in preventing the termination of TNF-induced signaling. Our data demonstrate that activation of GSK3 – either pathophysiologically or pharmacologically induced – may destroy the finely balanced condition necessary for the termination of inflammation-associated signaling.Keywords: TNF, GSK3, PKC, staurosporine, IL-8, NF-κB, termination of TNF-induced signaling, termination of inflammation

Published
2021

6. Mid-Infrared Variability from the Spitzer Deep, Wide-Field Survey

Author

Kozlowski, Szymon, Kochanek, Christopher S., Stern, Daniel, Ashby, Matthew L. N., Assef, Roberto J., Bock, J. J., Borys, C., Brand, K., Brodwin, M., Brown, M. J. I., Cool, R., Cooray, A., Croft, S., Dey, Arjun, Eisenhardt, P. R., Gonzalez, A., Gorjian, V., Griffith, R., Grogin, N., Ivison, R., Jacob, J., Jannuzi, B. T., Mainzer, A., Moustakas, L., Rottgering, H., Seymour, N., Smith, H. A., Stanford, S. A., Stauffer, J. R., Sullivan, I. S., van Breugel, W., Willner, S. P., and Wright, E. L.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We use the multi-epoch, mid-infrared Spitzer Deep, Wide-Field Survey to investigate the variability of 474,179 objects in 8.1 deg^2 of the NDWFS Bootes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 micron bands. We find that 1.1% of the studied sample meet our standard selection criteria for being classed as a variable source. We require that the 3.6 and 4.5 micron light-curves are strongly correlated (r>0.8) and that their joint variance exceeds that for all sources with the same magnitude by 2 sigma. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBootes survey, radio catalogs, 24 micron-selected AGN candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects. Most of the stellar, galaxy and unclassified sources are false positives. For our standard selection criteria, 11-12% of the mid-IR counterparts to X-ray sources, 24 micron-selected AGN candidates and spectroscopically identified AGNs show variability. Mid-IR AGN variability can be well described by a single power-law structure function with a power-law index of 0.5 at both 3.6 and 4.5 microns, and an amplitude of 0.1 mag on rest-frame time scales of 2 years. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities. (Abridged), Comment: preprint 38 pages, 10 figures, full catalogs available from http://data.spitzer.caltech.edu/popular/sdwfs/20100503_enhanced/catalogs/

Published
2010
Full Text
View/download PDF

7. The Spitzer Deep, Wide-Field Survey

Author

Ashby, M. L. N., Stern, D., Brodwin, M., Griffith, R., Eisenhardt, P., Kozlowski, S., Kochanek, C. S., Bock, J. J., Borys, C., Brand, K., Brown, M. J. I., Cool, R., Cooray, A., Croft, S., Dey, A., Eisenstein, D., Gonzalez, A. H., Gorjian, V., Grogin, N. A., Ivison, R. J., Jacob, J., Jannuzi, B. T., Mainzer, A., Moustakas, L. A., Rottgering, H. J. A., Seymour, N., Smith, H. A., Stanford, S. A., Stauffer, J. R., Sullivan, I., van Breugel, W., Willner, S. P., and Wright, E. L.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of ten square degrees in the Bootes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Cycle four Spitzer Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit -- for the first time -- the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z~3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS datasets will thus be especially useful for characterizing galaxy evolution beyond z~1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly-released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 x 10e5 distinct sources detected to the average 5-sigma, 4" diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 micron, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 min integration time of the SDWFS IRAC imaging, more than 50% of isolated FIRST radio sources and more than 80% of on-axis XBootes sources are detected out to 8.0 micron. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class., Comment: 71 pages, 18 figures, accepted for publication in the Astrophysical Journal

Published
2009
Full Text
View/download PDF

8. Spitzer 24 um Excesses for Bright Galactic Stars in Bootes and First Look Survey Fields

Author

Hovhannisyan, L. R., Mickaelian, A. M., Weedman, D. W., Floc'h, E. Le, Houck, J. R., Soifer, B. T., Brand, K., Dey, A., and Jannuzi, B. T.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Optically bright Galactic stars (V < 13 mag) having fv(24 um) > 1 mJy are identified in Spitzer mid-infrared surveys within 8.2 square degrees for the Bootes field of the NOAO Deep Wide-Field Survey and within 5.5 square degrees for the First Look Survey (FLS). 128 stars are identified in Bootes and 140 in the FLS, and their photometry is given. (K-[24]) colors are determined using K magnitudes from the 2MASS survey for all stars in order to search for excess 24 um luminosity compared to that arising from the stellar photosphere. Of the combined sample of 268 stars, 141 are of spectral types F, G, or K, and 17 of these 141 stars have 24 um excesses with (K-[24]) > 0.2 mag. Using limits on absolute magnitude derived from proper motions, at least 8 of the FGK stars with excesses are main sequence stars, and estimates derived from the distribution of apparent magnitudes indicate that all 17 are main sequence stars. These estimates lead to the conclusion that between 9% and 17% of the main sequence FGK field stars in these samples have 24 um infrared excesses. This result is statistically similar to the fraction of stars with debris disks found among previous Spitzer targeted observations of much brighter, main sequence field stars., Comment: Accepted for publication in The Astronomical Journal

Published
2009
Full Text
View/download PDF

9. High Redshift Dust Obscured Galaxies, A Morphology-SED Connection Revealed by Keck Adaptive Optics

Author

Melbourne, J., Bussman, S., Brand, K., Desai, V., Armus, L., Dey, Arjun, Jannuzi, B. T., Houck, J. R., Matthews, K., and Soifer, B. T.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

A simple optical to mid-IR color selection, R-[24] > 14, i.e. f_nu(24) / f_nu(R) > 1000, identifies highly dust obscured galaxies (DOGs) with typical redshifts of z~2 +/- 0.5. Extreme mid-IR luminosities (L_{IR} > 10^{12-14}) suggest that DOGs are powered by a combination of AGN and star formation, possibly driven by mergers. In an effort to compare their photometric properties with their rest frame optical morphologies, we obtained high spatial resolution (0.05 -0.1") Keck Adaptive Optics (AO) K'-band images of 15 DOGs. The images reveal a wide range of morphologies, including: small exponential disks (8 of 15), small ellipticals (4 of 15), and unresolved sources (2 of 15). One particularly diffuse source could not be classified because of low signal to noise ratio. We find a statistically significant correlation between galaxy concentration and mid-IR luminosity, with the most luminous DOGs exhibiting higher concentration and smaller physical size. DOGs with high concentration also tend to have spectral energy distributions (SEDs) suggestive of AGN activity. Thus central AGN light may be biasing the morphologies of the more luminous DOGs to higher concentration. Conversely, more diffuse DOGs tend to show an SED shape suggestive of star formation. Two of fifteen in the sample show multiple resolved components with separations of ~1 kpc, circumstantial evidence for ongoing mergers., Comment: 14 pages, 10 figures, Accepted for publication in the Astronomical Journal

Published
2009
Full Text
View/download PDF

10. HST Morphologies of z~2 Dust Obscured Galaxies I: Power-law Sources

Author

Bussmann, R. S., Dey, Arjun, Lotz, J., Armus, L., Brand, K., Brown, M. J. I., Desai, V., Eisenhardt, P., Higdon, J., Higdon, S., Jannuzi, B. T., Floc'h, E. Le, Melbourne, J., Soifer, B. T., and Weedman, D.

Subjects
Astrophysics
Abstract

We present high spatial resolution optical and near-infrared imaging obtained using the ACS, WFPC2 and NICMOS cameras aboard the Hubble Space Telescope of 31 24um--bright z~2 Dust Obscured Galaxies (DOGs) identified in the Bootes Field of the NOAO Deep Wide-Field Survey. Although this subset of DOGs have mid-IR spectral energy distributions dominated by a power-law component suggestive of an AGN, all but one of the galaxies are spatially extended and not dominated by an unresolved component at rest-frame UV or optical wavelengths. The observed V-H and I-H colors of the extended components are 0.2-3 magnitudes redder than normal star-forming galaxies. All but 1 have axial ratios >0.3, making it unlikely that DOGs are composed of an edge-on star-forming disk. We model the spatially extended component of the surface brightness distributions of the DOGs with a Sersic profile and find effective radii of 1-6 kpc. This sample of DOGs is smaller than most sub-millimeter galaxies (SMGs), but larger than quiescent high-redshift galaxies. Non-parametric measures (Gini and M20) of DOG morphologies suggest that these galaxies are more dynamically relaxed than local ULIRGs. We estimate lower limits to the stellar masses of DOGs based on the rest-frame optical photometry and find that these range from ~10^(9-11) M_sun. If major mergers are the progenitors of DOGs, then these observations suggest that DOGs may represent a post-merger evolutionary stage., Comment: 23 pages, 9 figures, 6 tables, accepted to ApJ; lower limits on stellar mass revised upwards by factor of (1+z)

Published
2008
Full Text
View/download PDF

11. Morphologies of High Redshift, Dust Obscured Galaxies from Keck Laser Guide Star Adaptive Optics

Author

Melbourne, J., Desai, V., Armus, Lee, Dey, Arjun, Brand, K., Thompson, D., Soifer, B. T., Matthews, K., Jannuzi, B. T., and Houck, J. R.

Subjects
Astrophysics
Abstract

Spitzer MIPS images in the Bootes field of the NOAO Deep Wide-Field Survey have revealed a class of extremely dust obscured galaxy (DOG) at z~2. The DOGs are defined by very red optical to mid-IR (observed-frame) colors, R - [24 um] > 14 mag, i.e. f_v (24 um) / f_v (R) > 1000. They are Ultra-Luminous Infrared Galaxies with L_8-1000 um > 10^12 -10^14 L_sun, but typically have very faint optical (rest-frame UV) fluxes. We imaged three DOGs with the Keck Laser Guide Star Adaptive Optics (LGSAO) system, obtaining ~0.06'' resolution in the K'-band. One system was dominated by a point source, while the other two were clearly resolved. Of the resolved sources, one can be modeled as a exponential disk system. The other is consistent with a de Vaucouleurs profile typical of elliptical galaxies. The non-parametric measures of their concentration and asymmetry, show the DOGs to be both compact and smooth. The AO images rule out double nuclei with separations of greater than 0.1'' (< 1 kpc at z=2), making it unlikely that ongoing major mergers (mass ratios of 1/3 and greater) are triggering the high IR luminosities. By contrast, high resolution images of z~2 SCUBA sources tend to show multiple components and a higher degree of asymmetry. We compare near-IR morphologies of the DOGs with a set of z=1 luminous infrared galaxies (LIRGs; L_IR ~ 10^11 L_sun) imaged with Keck LGSAO by the Center for Adaptive Optics Treasury Survey. The DOGs in our sample have significantly smaller effective radii, ~1/4 the size of the z=1 LIRGs, and tend towards higher concentrations. The small sizes and high concentrations may help explain the globally obscured rest-frame blue-to-UV emission of the DOGs., Comment: 9 pages, 7 figures, 2 tables, accepted for publication in the Astronomical Journal

Published
2008
Full Text
View/download PDF

12. The Mid-Infrared Properties of X-ray Sources

Author

Gorjian, V., Brodwin, M., Kochanek, C. S., Murray, S., Stern, D., Brand, K., Eisenhardt, P. R., Ashby, M. L. N., Barmby, P., Brown, M. J. I., Dey, A., Forman, W., Jannuzi, B. T., Jones, C., Kenter, A. T., Pahre, M. A., Shields, J. C., Werner, M. W., and Willner, S. P.

Subjects
Astrophysics
Abstract

We combine the results of the Spitzer IRAC Shallow Survey and the Chandra XBootes Survey of the 8.5 square degrees Bootes field of the NOAO Deep Wide- Field Survey to produce the largest comparison of mid-IR and X-ray sources to date. The comparison is limited to sources with X-ray fluxes >8x10-15 erg cm-2s-1 in the 0.5-7.0 keV range and mid-IR sources with 3.6 um fluxes brighter than 18.4 mag (12.3 uJy). In this most sensitive IRAC band, 85% of the 3086 X-ray sources have mid-IR counterparts at an 80% confidence level based on a Bayesian matching technique. Only 2.5% of the sample have no IRAC counterpart at all based on visual inspection. Even for a smaller but a significantly deeper Chandra survey in the same field, the IRAC Shallow Survey recovers most of the X-ray sources. A majority (65%) of the Chandra sources detected in all four IRAC bands occupy a well-defined region of IRAC [3.6] - [4.5] vs [5.8] - [8.0] color-color space. These X-ray sources are likely infrared luminous, unobscured type I AGN with little mid-infrared flux contributed by the AGN host galaxy. Of the remaining Chandra sources, most are lower luminosity type I and type II AGN whose mid-IR emission is dominated by the host galaxy, while approximately 5% are either Galactic stars or very local galaxies., Comment: Accepted for publication in ApJ

Published
2008
Full Text
View/download PDF

13. A large population of mid-infrared selected, obscured active galaxies in the Bootes field

Author

Hickox, R. C., Jones, C., Forman, W. R., Murray, S. S., Brodwin, M., Brown, M. J. I., Eisenhardt, P. R., Stern, D., Kochanek, C. S., Eisenstein, D., Cool, R. J., Jannuzi, B. T., Dey, A., Brand, K., Gorjian, V., and Caldwell, N.

Subjects
Astrophysics
Abstract

We identify a population of 640 obscured and 839 unobscured AGNs at redshifts 0.7~80%. The observed numbers of IRAGNs are comparable to predictions from previous X-ray, optical, and IR luminosity functions, for the given redshifts and IRAC flux limits. We observe a bimodal distribution in R-[4.5] color, suggesting that luminous IR-selected AGNs have either low or significant dust extinction, which may have implications for models of AGN obscuration., Comment: 23 emulateapj pages, 24 figures, 4 tables, v2: minor changes match version to appear in ApJ

Published
2007
Full Text
View/download PDF

14. Optical Line Diagnostics of z~2 Optically Faint ULIRGs in the Spitzer Bootes Survey

Author

Brand, K., Dey, A., Desai, V., Soifer, B. T., Bian, C., Armus, L., Brown, M. J. I., Floc'h, E. Le, Higdon, S. J., Houck, J. R., Jannuzi, B. T., and Weedman, D. W.

Subjects
Astrophysics
Abstract

We present near-infrared spectroscopic observations for a sample of ten optically faint luminous infrared galaxies (R-[24]> 14) using Keck NIRSPEC and Gemini NIRI. The sample is selected from a 24 micron Spitzer MIPS imaging survey of the NDWFS Bootes field. We measure accurate redshifts in the range 1.31900 km/s) Halpha or Hbeta emission lines; the remaining three are type II AGN. Given their large mid-IR luminosities and faint optical magnitudes, we might expect these sources to be heavily extincted quasars, and therefore only visible as type II AGN. The visibility of broad lines in 70% of the sources suggests that it is unlikely that these AGN are being viewed through the mid-plane of a dusty torus. For four of the sources we constrain the Halpha/Hbeta Balmer decrement and estimate the extinction to the emission line region to be large for both type I and type II AGN, with A_Halpha > 2.4-5 mag. Since the narrow-line region is also extincted and the UV continuum emission from the host galaxies is extremely faint, this suggests that much of the obscuration is contributed by dust on large (~kpc) scales within the host galaxies. These sources may be examples of "host-obscured" AGN which could have space densities comparable or greater to that of optically luminous type I AGN with similar bolometric luminosities., Comment: 13 pages, ApJ accepted

Published
2007
Full Text
View/download PDF

15. Mid-Infrared Selection of Brown Dwarfs and High-Redshift Quasars

Author

Stern, D., Kirkpatrick, J. D., Allen, L., Bian, C., Blain, A., Brand, K., Brodwin, M., Brown, M. J. I., Cool, R., Desai, V., Dey, A., Eisenhardt, P., Gonzalez, A., Jannuzi, B. T., Menendez-Delmestre, K., Smith, H. A., Soifer, B. T., Tiede, G. P., and Wright, E.

Subjects
Astrophysics
Abstract

We discuss color selection of rare objects in a wide-field, multiband survey spanning from the optical to the mid-infrared. Simple color criteria simultaneously identify and distinguish two of the most sought after astrophysical sources: the coolest brown dwarfs and the most distant quasars. We present spectroscopically-confirmed examples of each class identified in the IRAC Shallow Survey of the Bootes field of the NOAO Deep Wide-Field Survey. ISS J142950.9+333012 is a T4.5 brown dwarf at a distance of approximately 42 pc, and ISS J142738.5+331242 is a radio-loud quasar at redshift z=6.12. Our selection criteria identify a total of four candidates over 8 square degrees of the Bootes field. The other two candidates are both confirmed 5.5

Published
2006
Full Text
View/download PDF

16. Photometric Redshifts in the IRAC Shallow Survey

Author

Brodwin, M., Brown, M. J. I., Ashby, M. L. N., Bian, C., Brand, K., Dey, A., Eisenhardt, P. R., Eisenstein, D. J., Gonzalez, A. H., Huang, J. -S., Jannuzi, B. T., Kochanek, C. S., McKenzie, E., Pahre, M. A., Smith, H. A., Soifer, B. T., Stanford, S. A., Stern, D., and Elston, R. J.

Subjects
Astrophysics
Abstract

Accurate photometric redshifts are calculated for nearly 200,000 galaxies to a 4.5 micron flux limit of ~13 uJy in the 8.5 deg^2 Spitzer/IRAC Shallow survey. Using a hybrid photometric redshift algorithm incorporating both neural-net and template-fitting techniques, calibrated with over 15,000 spectroscopic redshifts, a redshift accuracy of \sigma = 0.06(1+z) is achieved for 95% of galaxies at 01) galaxy clusters. We present one such spectroscopically confirmed cluster at =1.24, ISCS J1434.5+3427. Finally, we present a measurement of the 4.5 micron-selected galaxy redshift distribution., Comment: 14 pages, 9 Figures, 5 Tables. ApJ in press. For a version with full-resolution figures, please see http://www.astro.utoronto.ca/~brodwin/papers/0607450.pdf

Published
2006
Full Text
View/download PDF

17. The AGN Contribution to the Mid-IR Emission of Luminous Infrared Galaxies

Author

Brand, K., Dey, A., Weedman, D., Desai, V., Floc'h, E. Le, Jannuzi, B. T., Soifer, B. T., Brown, M. J. I., Eisenhardt, P., Gorjian, V., Papovich, C., Smith, H. A., Willner, S. P., and Cool, R. J.

Subjects
Astrophysics
Abstract

We determine the contribution of AGN to the mid-IR emission of luminous infrared galaxies (LIRGs) at z>0.6 by measuring the mid-IR dust continuum slope of 20,039 mid-IR sources. The 24 micron sources are selected from a Spitzer/MIPS survey of the NOAO Deep Wide-Field Survey Bo\"otes field and have corresponding 8 micron data from the IRAC Shallow Survey. There is a clear bimodal distribution in the 24 micron to 8 micron flux ratio. The X-ray detected sources fall within the peak corresponding to a flat spectrum in nufnu, implying that it is populated by AGN-dominated LIRGs, whereas the peak corresponding to a higher 24 micron to 8 micron flux ratio is likely due to LIRGs whose infrared emission is powered by starbursts. The 24 micron emission is increasingly dominated by AGN at higher 24 micron flux densities (f_24): the AGN fraction of the z>0.6 sources increases from ~9% at f_24 ~ 0.35 mJy to 74+/-20% at f_24 ~ 3 mJy in good agreement with model predictions. Deep 24 micron, small area surveys, like GOODS, will be strongly dominated by starburst galaxies. AGN are responsible for ~ 3-7% of the total 24 micron background., Comment: 6 pages, accepted for publication in ApJ

Published
2006
Full Text
View/download PDF

18. IRS spectra of two ultraluminous infrared galaxies at z=1.3

Author

Desai, V., Armus, L., Soifer, B. T., Weedman, D. W., Higdon, S., Bian, C., Borys, C., Spoon, H. W. W., Charmandaris, V., Brand, K., Brown, M. J. I., Dey, A., Higdon, J., Houck, J., Jannuzi, B. T., Floc'h, E. Le, Ashby, M. L. N., and Smith, H. A.

Subjects
Astrophysics
Abstract

We present low-resolution (64 < R < 124) mid-infrared (8--38 micron) Spitzer/IRS spectra of two z~1.3 ultraluminous infrared galaxies (LFIR~10^13) discovered in a Spitzer/MIPS survey of the Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). MIPS J142824.0+352619 is a bright 160 micron source with a large infrared-to-optical flux density ratio and a possible lensing amplification of <~10. The 6.2, 7.7, 11.3, and 12.8 micron PAH emission bands in its IRS spectrum indicate a redshift of z~1.3. The large equivalent width of the 6.2 micron PAH feature indicates that at least 50% of the mid-infrared energy is generated in a starburst, an interpretation that is supported by a large [NeII]/[NeIII] ratio and a low upper limit on the X-ray luminosity. SST24 J142827.19+354127.71 has the brightest 24 micron flux (10.55 mJy) among optically faint (R > 20) galaxies in the NDWFS. Its mid-infrared spectrum lacks emission features, but the broad 9.7 micron silicate absorption band places this source at z~1.3. Given this redshift, SST24 J142827.19+354127.71 has among the largest rest-frame 5 micron luminosities known. The similarity of its SED to those of known AGN-dominated ULIRGs and its lack of either PAH features or large amounts of cool dust indicate that the powerful mid-infrared emission is dominated by an active nucleus rather than a starburst. Our results illustrate the power of the IRS in identifying massive galaxies in the ``redshift desert'' and in discerning their power sources. Because they are bright, MIPS J142824.0+352619 (pending future observations to constrain its lensing amplification) and SST24 J142827.19+354127.71 are useful z>1 templates of a high luminosity starburst and AGN, respectively., Comment: 9 pages, 4 figures; accepted for publication in ApJ; several small clarifications have been made

Published
2005
Full Text
View/download PDF

19. The Nuclear Accretion History of Red Galaxies

Author

Brand, K., NDWFS, the, and teams, XBoötes

Subjects
Astrophysics
Abstract

We use an X-ray stacking technique to investigate the evolution of the mean X-ray luminosity of ~21,000 red galaxies at 0.3 < z < 0.9 as a function of their stellar mass and redshift. The red galaxies are selected from the 9.3 deg^2 Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). The mean X-ray luminosity is an order of magnitude larger than we would expect from stellar sources alone and therefore must be primarily due to AGN emission. The X-ray luminosities (L_x ~ 10^41 ergs/s) imply that these must be sources with relatively low accretion rates and/or accretion efficiencies onto their central super-massive black hole (SMBH). The mean X-ray luminosity increases significantly as a function of optical luminosity and stellar mass, implying that more massive galaxies have higher nuclear accretion rates than lower mass galaxies. We calculate that the mean X-ray luminosity evolves as (1+z)^3.3+/-1.5. This suggests a global decline in the mean AGN activity of normal early-type galaxies from z~1 to the present. If accreting at typical AGN efficiencies, SMBHs within red galaxies accreted an insignificant proportion of their mass in this time., Comment: To appear in the proceedings for the Vth Marseille International Cosmology Conference: The Fabulous Destiny of Galaxies: Bridging Past and Present (5 pages)

Published
2005

20. MIPS J142824.0+352619: A Hyperluminous Starburst Galaxy at z=1.325

Author

Borys, C., Blain, A. W., Dey, A., Floc'h, E. Le, Jannuzi, B. T., Barnard, V., Bian, C., Brodwin, M., Men'endez-Delmestre, K., Thompson, D., Brand, K., Brown, M. J. I., Dowell, C. D., Eisenhardt, P., Farrah, D., Frayer, D. T., Higdon, J., Higdon, S., Phillips, T., Soifer, B. T., Stern, D., and Weedman, D.

Subjects
Astrophysics
Abstract

Using the SHARC-II camera at the Caltech Submillimeter Observatory to obtain 350 micron images of sources detected with the MIPS instrument on Spitzer, we have discovered a remarkable object at z=1.325+/-0.002 with an apparent Far-Infrared luminosity of 3.2(+/-0.7) x 10^13 Lsun. Unlike other z>1 sources of comparable luminosity selected from mid-IR surveys, MIPS J142824.0+352619 lacks any trace of AGN activity, and is likely a luminous analog of galaxies selected locally by IRAS, or at high redshift in the submillimeter. This source appears to be lensed by a foreground elliptical galaxy at z=1.034, although the amplification is likely modest (~10). We argue that the contribution to the observed optical/Near-IR emission from the foreground galaxy is small, and hence are able to present the rest-frame UV through radio Spectral Energy Distribution of this galaxy. Due to its unusually high luminosity, MIPS J142824.0+352619 presents a unique chance to study a high redshift dusty starburst galaxy in great detail., Comment: 6 pages, 3 figures, accepted for publication in ApJ

Published
2005
Full Text
View/download PDF

21. Discovery of a Large ~200 kpc Gaseous Nebula at z=2.7 with the Spitzer Space Telescope

Author

Dey, A., Bian, C., Soifer, B. T., Brand, K., Brown, M. J. I., Chaffee, F. H., LeFloc'h, E., Hill, G., Houck, J. R., Jannuzi, B. T., Rieke, M., Weedman, D., Brodwin, M., and Eisenhardt, P.

Subjects
Astrophysics
Abstract

We report the discovery of a very large, spatially extended Ly alpha -emitting nebula at z=2.656 associated with a luminous mid-infrared source. The bright mid-infrared source (F(24um)=0.86 mJy) was first detected in observations made using the Spitzer Space Telescope. Existing broad-band imaging data from the NOAO Deep Wide-Field Survey revealed the mid-infrared source to be associated with a diffuse, spatially extended, optical counterpart in the Bw band. Spectroscopy and further imaging of this target reveals that the optical source is an almost purely line-emitting nebula with little, if any, detectable diffuse continuum emission. The Lya nebula has a luminosity of L[Lya] ~ 1.7e44 erg/s and an extent of at least 20 arcsec (160 kpc). Its central ~8 arcsec shows an ordered, monotonic velocity profile; interpreted as rotation, this region encloses a mass M = 6e12 Msun. Several sources lie within the nebula. The central region of the nebula shows narrow (~365 km/s) emission lines of CIV and HeII. The mid-infrared source is a compact object lying within the nebula, but offset from the center by a projected distance of ~2.5 arcsec (20 kpc), and likely to be an enshrouded AGN. A young star-forming galaxy lies near the northern end of the nebula. We suggest that the nebula is a site of recent multiple galaxy and AGN formation, with the spatial distribution of galaxies within the nebula perhaps tracking the formation history of the system., Comment: 37 pages (includes 11 figures). Accepted to ApJ

Published
2005
Full Text
View/download PDF

22. Current-induced conductance switching in epitaxial La0.7Sr0.3MnO3/SrTiO3 multilayers

Author

Doerr, K., Mueller, K. -H., Walter, T., Sahana, M., Eckert, D., Nenkov, K., Schultz, L., Brand, K., and Lehmann, M.

Subjects
Condensed Matter - Strongly Correlated Electrons
Abstract

We report on the non-linear in-plane electrical transport in coherently grown [La0.7Sr0.3MnO3/SrTiO3] multilayers with ultrathin (< 3 nm) single layers. Current-induced switching of the conductance, with low conductance at larger currents, is demonstrated. The conductance switching is modified under a magnetic field, resulting in an extremely large magnetoresistance of negative, or in a special case even positive, sign. Our results suggest a percolative nature of transport where a large local current density gives rise to a spin-polarizing and a thermal effect of current., Comment: 10 pages, 6 figures

Published
2000

23. Mid-infrared variability from the spitzer deep wide-field survey

Author

Kozłowski, S, Kochanek, CS, Stern, D, Ashby, MLN, Assef, RJ, Bock, JJ, Borys, C, Brand, K, Brodwin, M, Brown, MJI, Cool, R, Cooray, A, Croft, S, Dey, A, Eisenhardt, PR, Gonzalez, A, Gorjian, V, Griffith, R, Grogin, N, Ivison, R, Jacob, J, Jannuzi, BT, Mainzer, A, Moustakas, L, Röttgering, H, Seymour, N, Smith, HA, Stanford, SA, Stauffer, JR, Sullivan, IS, Van Breugel, W, Willner, SP, and Wright, EL

Subjects
cosmology: observations, galaxies: active, infrared: galaxies, quasars: general, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We use the multi-epoch, mid-infrared Spitzer Deep Wide-Field Survey to investigate the variability of objects in 8.1 deg2 of the NOAO Deep Wide Field Survey Boötes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 μm bands. Out of 474, 179 analyzed sources, 1.1% meet our standard variability selection criteria that the two light curves are strongly correlated (r>0.8) and that their joint variance (σ12) exceeds that for all sources with the same magnitude by 2σ. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBoötes survey, radio catalogs, 24 μm selected active galactic nucleus (AGN) candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects, although most of the stellar, galaxy, and unclassified sources are false positives. For our standard selection criteria, 11%-12% of the mid-IR counterparts to X-ray sources, 24 μm AGN candidates, and spectroscopically identified AGNs show variability. The exact fractions depend on both the search depth and the selection criteria. For example, 12% of the 1131 known z>1 AGNs in the field and 14%-17% of the known AGNs with well-measured fluxes in all four Infrared Array Camera bands meet our standard selection criteria. The mid-IR AGN variability can be well described by a single power-law structure function with an index of γ ≈ 0.5 at both 3.6 and 4.5 μm, and an amplitude of S 0 ≃ 0.1 mag on rest-frame timescales of 2 yr. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities. © 2010. The American Astronomical Society. All rights reserved.

Published
2010

24. THE SPITZER DEEP, WIDE-FIELD SURVEY

Author

Ashby, MLN, Stern, D, Brodwin, M, Griffith, R, Eisenhardt, P, Kozłowski, S, Kochanek, CS, Bock, JJ, Borys, C, Brand, K, Brown, MJI, Cool, R, Cooray, A, Croft, S, Dey, A, Eisenstein, D, Gonzalez, AH, Gorjian, V, Grogin, NA, Ivison, RJ, Jacob, J, Jannuzi, BT, Mainzer, A, Moustakas, LA, Röttgering, HJA, Seymour, N, Smith, HA, Stanford, SA, Stauffer, JR, Sullivan, I, van Breugel, W, Willner, SP, and Wright, EL

Subjects
infrared: galaxies, infrared: stars, surveys, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg2 in the Boötes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit - for the first time - the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ∼ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ∼ 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 × 105 distinct sources detected to the average 5σ, 4″-diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0μm, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, >50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and >80% of on-axis XBoötes sources are detected out to 8.0μm. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class. © 2009. The American Astronomical Society. All rights reserved.

Published
2009

25. Mapping crustal structure across southern Australia using seismic ambient noise tomography.

Author

O'Donnell, J.P., Agrawal, S., Eakin, C.M., Thiel, S., Brand, K., Gorbatov, A., and Goleby, B.

Abstract

[Display omitted] • The AusArray SA and Lake Eyre Basin arrays expand seismic coverage in South Australia. • We develop a shear wave model of southern Australia crustal structure to 20 km depth. • We interpret variations in uppermost to mid crustal seismic structure. The rocks of southern Australia record over three billion years of Earth's evolution, but the basement geology is veiled by sediment. Geophysical data are needed to unveil the geology. The 2018–2022 Lake Eyre Basin and 2020–2022 AusArray SA seismic arrays expand seismic coverage in South Australia. In conjunction with permanent and preceding temporary arrays, we extracted Rayleigh wave dispersion data from ambient noise recordings at a total of 501 seismic stations spanning the transition from Precambrian to Phanerozoic Australia. These data were used to develop Rayleigh wave phase velocity maps of southern Australia at periods 3–20 s, and in turn, a shear wave velocity model to 20 km depth. At upper-crustal depths, low velocity structure tracks Phanerozoic sedimentary accumulations. The Moyston Fault, regarded as the boundary between the Delamerian and Lachlan Orogens, has an intermittent expression in the shear velocity model: it has no obvious expression at depths shallower than ∼ 10 km, but in the mid-crust is marked by a velocity contrast in southern Victoria and a velocity contrast tracing the southern edge of the Darling Basin in western New South Wales. An arcuate velocity contrast characterising the western edge of deep, sediment-filled troughs of the Darling Basin is a candidate for the transition from Precambrian to Phanerozoic crust. Fluid derived from neotectonic metamorphic devolatilization and/or remnant hydrated mantle is our preferred hypothesis for explaining seismicity and coincident seismic and conductivity anomalies in the mid-to-lower crust beneath the Ikara–Flinders Ranges. Our model suggests that the Olympic Dam and Carrapateena IOCG deposits reside above the margin of a mid-crustal low seismic velocity zone. We surmise that this might reflect past metalliferous fluid movement associated with the Olympic Cu-Au Province, akin to low reflectivity and low resistivity zones evident in 2D reflection seismic and magnetotelluric profiles, respectively. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

26. Lack of S100A9 aggravates pneumococcal pneumonia in mice

Author

Ostermann, L, primary, Katsarou, K, additional, Maus, R, additional, Christmann, M, additional, Neumann, K, additional, Brand, K, additional, Seeliger, B, additional, Bühling, F, additional, Viemann, D, additional, Welte, T, additional, and Maus, U A, additional

Published
2022
Full Text
View/download PDF

30. Metformin in pregnancy and risk of adverse long-term outcomes:a register-based cohort study

Author

Brand, K. M. (Kerstin M G), Saarelainen, L. (Laura), Sonajalg, J. (Jaak), Boutmy, E. (Emmanuelle), Foch, C. (Caroline), Vääräsmäki, M. (Marja), Morin-Papunen, L. (Laure), Schlachter, J. (Judith), C. S. (CLUE Study Group), Hakkarainen, K. M. (Katja M), Korhonen, P. (Pasi), Brand, K. M. (Kerstin M G), Saarelainen, L. (Laura), Sonajalg, J. (Jaak), Boutmy, E. (Emmanuelle), Foch, C. (Caroline), Vääräsmäki, M. (Marja), Morin-Papunen, L. (Laure), Schlachter, J. (Judith), C. S. (CLUE Study Group), Hakkarainen, K. M. (Katja M), and Korhonen, P. (Pasi)

Abstract

Introduction: This study aimed to investigate if maternal pregnancy exposure to metformin is associated with increased risk of long-term and short-term adverse outcomes in the child. Research design and methods: This register-based cohort study from Finland included singleton children born 2004–2016 with maternal pregnancy exposure to metformin or insulin (excluding maternal type 1 diabetes): metformin only (n=3967), insulin only (n=5273) and combination treatment (metformin and insulin; n=889). The primary outcomes were long-term offspring obesity, hypoglycemia, hyperglycemia, diabetes, hypertension, polycystic ovary syndrome, and challenges in motor–social development. In a sensitivity analysis, the primary outcomes were investigated only among children with maternal gestational diabetes. Secondary outcomes were adverse outcomes at birth. Analyses were conducted using inverse- probability of treatment weighting (IPTW), with insulin as reference. Results: Exposure to metformin or combination treatment versus insulin was not associated with increased risk of long-term outcomes in the main or sensitivity analyses. Among the secondary outcomes, increased risk of small for gestational age (SGA) was observed for metformin (IPTW-weighted OR 1.65, 95% CI 1.16 to 2.34); increased risk of large for gestational age, preterm birth and hypoglycemia was observed for combination treatment. No increased risk was observed for neonatal mortality, hyperglycemia, or major congenital anomalies. Conclusions: This study found no increased long-term risk associated with pregnancy exposure to metformin (alone or in combination with insulin), compared with insulin. The increased risk of SGA associated with metformin versus insulin suggests caution in pregnancies with at-risk fetal undernutrition. The increased risks of adverse outcomes at birth associated with combination treatment may reflect confounding by indication or severity., CLUE Study Group Members of the CLUE Study Group are Minna Vehkala (Global Database Studies, IQVIA), Robyn Thorén (Global Database Studies, IQVIA), Henrik Svanström (Global Database Studies, IQVIA).

Published
2022

44. Search for charginos, neutralinos and gravitinos at LEP

Author

Abreu, P., Adam, W., Adye, T., Ajinenko, I., Alekseev, G. D., Alemany, R., Allport, P. P., Almehed, S., Amaldi, U., Amato, S., Andersson, P., Andreazza, A., Antilogus, P., Apel, W -D., Arnoud, Y., Åsman, B., Augustin, J -E., Augustinus, A., Baillon, P., Bambade, P., Barbi, M., Bardin, D. Y., Barker, G., Baroncelli, A., Barring, O., Bates, M. J., Battaglia, M., Baubillier, M., Baudot, J., Becks, K -H., Begalli, M., Beilliere, P., Belokopytov, Yu., Belous, K., Benvenuti, A. C., Berat, C., Berggren, M., Bertini, D., Bertrand, D., Besancon, M., Bianchi, F., Bigi, M., Bilenky, M. S., Billoir, P., Bizouard, M -A., Bloch, D., Blume, M., Bonesini, M., Bonivento, W., Boonekamp, M., Booth, P. S. L., Borgland, A. W., Borisov, G., Bosio, C., Botner, O., Boudinov, E., Bouquet, B., Bourdarios, C., Bowcock, T. J. V., Bozzo, M., Branchini, P., Brand, K. D., Brenke, T., Brenner, R. A., Brown, R. C. A., Bruckman, P., Brunet, J -M., Bugge, L., Buran, T., Burgsmueller, T., Buschmann, P., Cabrera, S., Caccia, M., Calvi, M., Camacho Rozas, A. J., Camporesi, T., Canale, V., Canepa, M., Carena, F., Carroll, L., Caso, C., Castillo Gimenez, M. V., Cattai, A., Cavallo, F. R., Chabaud, V., Chapkin, M., Charpentier, Ph., Chaussard, L., Checchia, P., Chelkov, G. A., Chen, M., Chierici, R., Chhapnikov, P., Chochula, P., Chorowicz, V., Chudoba, J., Cindro, V., Collins, P., Colomer, M., Contri, R., Cortina, E., Cosme, G., Cossutti, F., Cowell, J -H., Crawley, H. B., Crennell, D., Crosetti, G., Cuevas Maestro, J., Czellar, S., Dahm, J., Dalmagne, B., Damgaard, G., Dauncey, P. D., Davenport, M., Da Silva, W., Deghorain, A., Della Ricca, G., Delpierre, P., Demaria, N., De Angelis, A., De Boer, W., De Brabandere, S., De Clercq, C., De La Vaissiere, C., De Lotto, B., De Min, A., De Paula, L., Dijkstra, H., Di Ciaccio, L., Di Diodato, A., Djannati, A., Dolbeau, J., Doroba, K., Dracos, M., Drees, J., Drees, K. -A., Dris, M., Durand, J -D., Edsall, D., Ehret, R., Eigen, G., Ekelof, T., Ekspong, G., Elsing, M., Engel, J -P., Erzen, B., Espirito Santo, M., Falk, E., Fanourakis, G., Fassouliotis, D., Feindt, M., Fenyuk, A., Ferrari, P., Ferrer, A., Fichet, S., Filippas, T. A., Firestone, A., Fischer, P. -A., Foeth, H., Fokitis, E., Fontanelli, F., Formenti, F., Franek, B., Frodesen, A. G., Fruhwirth, R., Fulda-Quenzer, F., Fuster, J., Galloni, A., Gamba, D., Gandelman, M., Garcia, C., Garcia, J., Gaspar, C., Gasparini, U., Gavillet, Ph., Gazis, E. N., Gele, D., Gerber, J -P., Gokieli, R., Golob, B., Goncalves, P., Gopal, G., Gorn, L., Gorski, M., Gouz, Yu., Gracco, V., Graziani, E., Green, C., Grefrath, A., Gris, P., Grosdidier, G., Grzelak, K., Gumenyuk, S., Gunther, M., Guy, J., Hahn, F., Hahn, S., Hajduk, Z., Hallgren, A., Hamacher, K., Harris, F. J., Hedberg, V., Henriques, R., Hernandez, J. J., Herquet, P., Herr, H., Hessing, T. L., Heuser, J. -M., Higon, E., Holmgren, S -O., Holt, P. J., Holthuizen, D., Hoorelbeke, S., Houlden, M., Hrubec, J., Huet, K., Hultqvist, K., Jackson, J. N., Jacobsson, R., Jalocha, P., Janik, R., Jarlskog, Ch., Jarlskog, G., Jarry, P., Jean-Mariels, B., Johansson, E. K., Jonsson, L., Jonsson, P., Joram, C., Juillot, P., Kaiser, M., Kapusta, F., Karafasoulis, K., Karvelas, E., Katsanevas, S., Katsoufis, E. C., Keranen, R., Khokhlov, Yu., Khomenko, B. A., Khovanski, N. N., King, B., Kjaer, N. J., Klapp, O., Klein, H., Kluit, P., Knoblauch, D., Kokkinias, P., Koratzinos, M., Korcyl, K., Kostioukhine, V., Kourkoumelis, C., Kouznetsov, O., Krammer, M., Kreuter, C., Kronkvist, I., Krstic, J., Krumstein, Z., Krupinski, W., Kubinec, P., Kucewicz, W., Kurvinen, K., Lacasta, C., Laktineh, I., Lamsa, J. W., Lanceri, L., Lane, D. W., Langefeld, P., Lapin, V., Laugier, J -P., Lauhakangas, R., Leder, G., Ledroit, F., Lefebure, V., Legan, C. K., Leisos, A., Leitner, R., Lemonne, J., Lenzen, G., Lepeltier, V., Lesiak, T., Lethuillier, M., Libby, J., Liko, D., Lipniacka, A., Lippi, I., Loerstad, B., Loken, J. G., Lopez, J. M., Loukas, D., Lutz, P., Lyons, L., MacNaughton, J., Maehlum, G., Mahon, J. R., Maio, A., Malmgren, T. G. M., Malychev, V., Mandl, F., Marco, J., Marco, R., Marechal, B., Margoni, M., Marin, J -C., Mariotti, C., Markou, A., Martinez-Rivero, C., Martinez-Vidal, F., Marti i Garcia, S., Masik, J., Matorras, F., Matteuzzi, C., Matthiae, G., Mazzucato, M., Mc Cubbin, M., Mc Kay, R., Mc Nulty, R., Mc Pherson, G., Medbo, J., Meroni, C., Meyer, S., Meyer, W. T., Michelotto, M., Migliore, E., Mirabito, L., Mjoernmark, U., Moa, T., Moeller, R., Moenig, K., Monge, M. R., Morettini, P., Mueller, H., Muenich, K., Mulders, M., Mundim, L. M., Murray, W. J., Muryn, B., Myatt, G., Myklebust, T., Naraghi, F., Navarria, F. L., Navas, S., Nawrocki, K., Negri, P., Nemecek, S., Neumann, W., Neumeister, N., Nicolaidou, R., Nielsen, B. S., Nieuwenhuizen, M., Nikolaenko, V., Nikolenko, M., Niss, P., Nomerotski, A., Normand, A., Nygren, A., Oberschulte-Beckmann, W., Obraztsov, V., Olshevski, A. G., Onofre, A., Orava, R., Orazi, G., Ortuno, S., Osterberg, K., Ouraou, A., Paganini, P., Paganoni, M., Paiano, S., Pain, R., Palka, H., Papadopoulou, Th. D., Papageorgiou, K., Pape, L., Parkes, C., Parodi, F., Parzefall, U., Passeri, A., Pegoraro, M., Peralta, L., Pernegger, H., Pernicka, M., Perrotta, A., Petridou, C., Petrolini, A., Phillips, H. T., Piana, G., Pierre, F., Pimenta, M., Piotto, E., Podobnik, T., Podobrin, O., Pol, M. E., Polok, G., Poropat, P., Pozdniakov, V., Privitera, P., Pukhaeva, N., Pullia, A., Radojicic, D., Ragazzi, S., Rahmani, H., Ratoff, P. N., Read, A. L., Reale, M., Rebecchi, P., Redaelli, N. G., Regler, M., Reid, D., Reinhardt, R., Renton, R. B., Resvanis, L. K., Richard, F., Ridky, J., Rinaudo, G., Rohne, O., Romero, A., Ronchese, P., Roos, L., Rosenberg, E. I., Rosinsky, P., Roudeau, P., Rovelli, T., Ruhlmann-Kleider, V., Ruiz, A., Rybicki, K., Saarikko, H., Sacquin, Y., Sadovsky, A., Sajot, G., Salt, J., Sannino, M., Schneider, H., Schwickerath, U., Schyns, M. A. E., Sciolla, G., Scuri, F., Seager, P., Sedykh, Y., Segar, A. M., Seitz, A., Sekulin, R., Serbelloni, L., Shellard, R. C., Sheridan, A., Siegrist, P., Silvestre, R., Simonetto, F., Sisakian, A. N., Skaali, T. B., Smadja, G., Smirnov, N., Smirnova, O., Smith, G. R., Sokolov, A., Sosnowski, R., Souza-Santos, D., Spassov, T., Spiriti, E., Sponholz, P., Squarcial, S., Stampfer, D., Stanescu, C., Stanic, S., Stapnes, S., Stavitski, I., Stevenson, K., Stocchi, A., Strauss, J., Strub, R., Stugu, B., Szczekowski, M., Szeptycka, M., Tabarelli, T., Tavernet, J. P., Tegenfeldt, F., Terranova, F., Thomas, J., Tilquin, A., Timmermans, J., Tkatchev, L. G., Todorov, T., Todorova, T., Toet, D. Z., Tomaradze, A., Tome, B., Tonazzo, A., Tortora, L., Transtromer, G., Treille, D., Tristram, G., Trombini, A., Troncon, C., Tsirou, A., Turluer, M -L., Tyapkin, I. A., Tyndel, M., Tzamarias, S., Ueberschaer, B., Ullaland, O., Uvarov, V., Valenti, G., Vallazza, E., Vander Velde, C., Van Apeldoorn, G. W., Van Damlo, P., Van Doninck, W. K., Van Eldik, J., Van Lysebetten, A., Vassilopoulos, N., Vegni, G., Ventura, L., Venus, W., Verbeure, F., Verlato, M., Vertogradov, L. S., Vilanova, D., Vincent, P., Vitale, L., Vlasov, E., Vodopyanov, A. S., Vrba, V., Wahlen, H., Walck, C., Waldner, F., Weiser, C., Wetherell, A. M., Wicke, D., Wickens, J. H., Wielers, M., Wilkinson, G. R., Williams, W. S. C., Winter, M., Witek, M., Wlodek, T., Yi, J., Yip, K., Yushchenko, O., Zach, F., Zaitsev, A., Zalewska, A., Zalewski, P., Zavrtanik, D., Zevgolatakos, E., Zimin, N. I., Zucchelli, G. C., Zumerle, G., and DELPHI Collaboration

Published
1998
Full Text
View/download PDF

46. Determination of |Vcb| from the semileptonic decay B0 → D*−ℓ+ ν

Author

Abreu, P., Adam, W., Adye, T., Agasi, E., Ajinenko, I., Aleksan, R., Alekseev, G. D., Alemany, R., Allport, P. P., Almehed, S., Amaldi, U., Amato, S., Andreazza, A., Andrieux, M. L., Antilogus, P., Apel, W-D., Arnoud, Y., Åsman, B., Augustin, J-E., Augustinus, A., Baillon, P., Bambade, P., Barao, F., Barate, R., Barbi, M., Barbiellini, G., Bardin, D. Y., Baroncelli, A., Barring, O., Barrio, J. A., Bartl, W., Bates, M. J., Battaglia, M., Baubillier, M., Baudot, J., Becks, K-H., Begalli, M., Beilliere, P., Belokopytov, Yu., Benvenuti, A. C., Berggren, M., Bertrand, D., Bianchi, F., Bigi, M., Bilenky, M. S., Billoir, P., Bloch, D., Blume, M., Blyth, S., Bolognese, T., Bonesini, M., Bonivento, W., Booth, P. S. L., Borisov, G., Bosio, C., Bosworth, S., Botner, O., Boudinov, E., Bouquet, B., Bourdarios, C., Bowcock, T. J. V., Bozzo, M., Branchini, P., Brand, K. D., Brenke, T., Brenner, R. A., Bricman, C., Brillault, L., Brown, R. C. A., Bruckman, P., Brunet, J-M., Bugge, L., Buran, T., Burgsmueller, T., Buschmann, P., Buys, A., Cabrera, S., Caccia, M., Calvi, M., Camacho Rozas, A. J., Camporesi, T., Canale, V., Canepa, M., Cankocak, K., Cao, F., Carena, F., Carroll, L., Caso, C., Castillo Gimenez, M. V., Cattai, A., Cavallo, F. R., Cerrito, L., Chabaud, V., Chapkin, M., Charpentier, Ph., Chaussard, L., Chauveau, J., Checchia, P., Chelkov, G. A., Chen, M., Chierici, R., Chliapnikov, P., Chochula, P., Chorowicz, V., Chudoba, J., Cindro, V., Collins, P., Contreras, J. L., Contri, R., Cortina, E., Cosme, G., Cossutti, F., Crawley, H. B., Crennell, D., Crosetti, G., Maestro, J. Cuevas, Czellar, S., Dahl-Jensen, E., Dahm, J., Dalmagne, B., Dam, M., Damgaard, G., Dauncey, P. D., Davenport, M., Da Silva, W., Defoix, C., Deghorain, A., Della Ricca, G., Delpierre, P., Demaria, N., De Angelis, A., De Boer, W., De Brabandere, S., De Clercq, C., De La Vaissiere, C., De Lotto, B., De Min, A., De Paula, L., De Saint-Jean, C., Dijkstra, H., Di Ciaccio, L., Djama, F., Dolbeau, J., Donszelmann, M., Doroba, K., Dracos, M., Drees, J., Drees, K. A., Dris, M., Dufour, Y., Edsall, D., Ehret, R., Eigen, G., Ekelof, T., Ekspong, G., Elsing, M., Engel, J-P., Ershaidat, N., Erzen, B., Santo, M. Espirito, Falk, E., Fassouliotis, D., Feindt, M., Fenyuk, A., Ferrer, A., Filippas, T. A., Firestone, A., Fischer, P. A., Foeth, H., Fokitis, E., Fontanelli, F., Formenti, F., Franek, B., Frenkiel, P., Fries, D. C., Frodesen, A. G., Fruhwirth, R., Fulda-Quenzer, F., Fuster, J., Galloni, A., Gamba, D., Gandelman, M., Garcia, C., Garcia, J., Gaspar, C., Gasparini, U., Gavillet, Ph., Gazis, E. N., Gele, D., Gerber, J-P., Gibbs, M., Gokieli, R., Golob, B., Gopal, G., Gorn, L., Gorski, M., Gouz, Yu., Gracco, V., Graziani, E., Grosdidier, G., Grzelak, K., Gumenyuk, S., Gunnarsson, P., Gunther, M., Guy, J., Hahn, F., Hahn, S., Hajduk, Z., Hallgren, A., Hamacher, K., Hao, W., Harris, F. J., Hedberg, V., Henriques, R., Hernandez, J. J., Herquet, P., Herr, H., Hessing, T. L., Higon, E., Hilke, H. J., Hill, T. S., Holmgren, S-O., Holt, P. J., Holthuizen, D., Hoorelbeke, S., Houlden, M., Hrubec, J., Huet, K., Hultqvist, K., Jackson, J. N., Jacobsson, R., Jalocha, P., Janik, R., Jarlskog, Ch., Jarlskog, G., Jarry, P., Jean-Marie, B., Johansson, E. K., Jonsson, L., Jonsson, P., Joram, C., Juillot, P., Kaiser, M., Kapusta, F., Karafasoulis, K., Karlsson, M., Karvelas, E., Katsanevas, S., Katsoufis, E. C., Keranen, R., Khokhlov, Yu., Khomenko, B. A., Khovanski, N. N., King, B., Kjaer, N. J., Klein, H., Klovning, A., Kluit, P., Koene, B., Kokkinias, P., Koratzinos, M., Korcyl, K., Kourkoumelis, C., Kouznetsov, O., Kramer, P. H., Krammer, M., Kreuter, C., Kronkvist, I., Krumstein, Z., Krupinski, W., Kubinec, P., Kucewicz, W., Kurvinen, K., Lacasta, C., Laktineh, I., Lamblot, S., Lamsa, J. W., Lanceri, L., Lane, D. W., Langefeld, P., Last, I., Laugier, J-P., Lauhakangas, R., Leder, G., Ledroit, F., Lefebure, V., Legan, C. K., Leitner, R., Lemoigne, Y., Lemonne, J., Lenzen, G., Lepeltier, V., Lesiak, T., Liko, D., Lindner, R., Lipniacka, A., Lippi, I., Loerstad, B., Loken, J. G., Lopez, J. M., Loukas, D., Lutz, P., Lyons, L., Maehlum, G., Maio, A., Malychev, V., Mandl, F., Marco, J., Marco, R., Marechal, B., Margoni, M., Marin, J-C., Mariotti, C., Markou, A., Maron, T., Martinez-Rivero, C., Martinez-Vidal, F., Marti i Garcia, S., Masik, J., Matorras, F., Matteuzzi, C., Matthiae, G., Mazzucato, M., Mc Cubbin, M., Mc Kay, R., Mc Nulty, R., Medbo, J., Merk, M., Meroni, C., Meyer, S., Meyer, W. T., Michelotto, M., Migliore, E., Mirabito, L., Mitaroff, W. A., Mjoernmark, U., Moa, T., Moeller, R., Moenig, K., Monge, M. R., Morettini, P., Mueller, H., Mundim, L. M., Murray, W. J., Muryn, B., Myatt, G., Naraghi, F., Navarria, F. L., Navas, S., Nawrocki, K., Negri, P., Nemecek, S., Neumann, W., Neumeister, N., Nicolaidou, R., Nielsen, B. S., Nieuwenhuizen, M., Nikolaenko, V., Niss, P., Nomerotski, A., Normand, A., Novak, M., Oberschulte-Beckmann, W., Obraztsov, V., Olshevski, A. G., Onofre, A., Orava, R., Osterberg, K., Ouraou, A., Paganini, P., Paganoni, M., Pages, P., Palka, H., Papadopoulou, Th. D., Papageorgiou, K., Pape, L., Parkes, C., Parodi, F., Passeri, A., Pegoraro, M., Peralta, L., Pernegger, H., Pernicka, M., Perrotta, A., Petridou, C., Petrolini, A., Petrovyck, M., Phillips, H. T., Piana, G., Pierre, F., Pimenta, M., Pindo, M., Plaszczynski, S., Podobrin, O., Pol, M. E., Polok, G., Poropat, P., Pozdniakov, V., Prest, M., Privitera, P., Pukhaeva, N., Pullia, A., Radojicic, D., Ragazzi, S., Rahmani, H., Ratoff, P. N., Read, A. L., Reale, M., Rebecchi, P., Redaelli, N. G., Regler, M., Reid, D., Renton, P. B., Resvanis, L. K., Richard, F., Richardson, J., Ridky, J., Rinaudo, G., Ripp, I., Romero, A., Roncagliolo, I., Ronchese, P., Roos, L., Rosenberg, E. I., Rosso, E., Roudeau, P., Rovelli, T., Ruckstuhl, W., Ruhlmann-Kleider, V., Ruiz, A., Rybicki, K., Saarikko, H., Sacquin, Y., Sadovsky, A., Sajot, G., Salt, J., Sanchez, J., Sannino, M., Schimmelpfennig, M., Schneider, H., Schwickerath, U., Schyns, M. A. E., Sciolla, G., Scuri, F., Seager, P., Sedykh, Y., Segar, A. M., Seitz, A., Sekulin, R., Shellard, R. C., Siccama, I., Siegrist, P., Simonetti, S., Simonetto, F., Sisakian, A. N., Sitar, B., Skaali, T. B., Smadja, G., Smirnov, N., Smirnova, O., Smith, G. R., Solovianov, O., Sosnowski, R., Souza-Santos, D., Spassov, T., Spiriti, E., Sponholz, P., Squarcia, S., Stanescu, C., Stapnes, S., Stavitski, I., Stichelbaut, F., Stocchi, A., Strauss, J., Strub, R., Stugu, B., Szczekowski, M., Szeptycka, M., Tabarelli, T., Tavernet, J. P., Tchikilev, O., Tilquin, A., Timmermans, J., Tkatchev, L. G., Todorov, T., Toet, D. Z., Tomaradze, A., Tonazzo, A., Tortora, L., Transtromer, G., Treille, D., Trischuk, W., Tristram, G., Trombini, A., Troncon, C., Tsirou, A., Turluer, M-L., Tyapkin, I. A., Tyndel, M., Tzamarias, S., Ueberschaer, B., Ullaland, O., Uvarov, V., Valenti, G., Vallazza, E., Vander Velde, C., Van Apeldoorn, G. W., Van Dam, P., Van Doninck, W. K., Van Eldik, J., Vassilopoulos, N., Vegni, G., Ventura, L., Venus, W., Verbeure, F., Verlato, M., Vertogradov, L. S., Vilanova, D., Vincent, P., Vitale, L., Vlasov, E., Vodopyanov, A. S., Vrba, V., Wahlen, H., Walck, C., Weierstall, M., Weilhammer, P., Weiser, C., Wetherell, A. M., Wicke, D., Wickens, J. H., Wielers, M., Wilkinson, G. R., Williams, W. S. C., Winter, M., Witek, M., Woschnagg, K., Yip, K., Yushchenko, O., Zach, F., Zaitsev, A., Zalewska, A., Zalewski, P., Zavrtanik, D., Zevgolatakos, E., Zimin, N. I., Zito, M., Zontar, D., Zuberi, R., Zucchelli, G. C., Zumerle, G., and DELPHI Collaboration

Published
1996
Full Text
View/download PDF

47. Determination of the average lifetime ofb-baryons

Author

Abreu, P., Adam, W., Adye, T., Agasi, E., Ajinenko, I., Aleksan, R., Alekseev, G. D., Alemany, R., Allport, P. P., Almehed, S., Amaldi, U., Amato, S., Andreazza, A., Andrieux, M. L., Antilogus, P., Apel, W-D., Arnoud, Y., Asman, B., Augustin, J-E., Augustinus, A., Baillon, P., Bambade, P., Barao, F., Barate, R., Barbi, M., Bardin, D. Y., Baroncelli, A., Barring, O., Barrio, J. A., Bartl, W., Bates, M. J., Battaglia, M., Baubillier, M., Baudot, J., Becks, K-H., Begalli, M., Beilliere, P., Belokopytov, Yu., Belous, K., Benvenuti, A. C., Berggren, M., Bertrand, D., Bianchi, F., Bigi, M., Bilenky, M. S., Billoir, P., Bloch, D., Blume, M., Blyth, S., Bolognese, T., Bonesini, M., Bonivento, W., Booth, P. S. L., Borisov, G., Bosio, C., Bosworth, S., Botner, O., Boudinov, E., Bouquet, B., Bourdarios, C., Bowcock, T. J. V., Bozzo, M., Branchini, P., Brand, K. D., Brenke, T., Brenner, R. A., Bricman, C., Brillault, L., Brown, R. C. A., Bruckman, P., Brunet, J-M., Bugge, L., Buran, T., Burgsmueller, T., Buschmann, P., Buys, A., Cabrera, S., Caccia, M., Calvi, M., Camacho Rozas, A. J., Camporesi, T., Canale, V., Canepa, M., Cankocak, K., Cao, F., Carena, F., Carroll, L., Caso, C., Castillo Gimenez, M. V., Cattai, A., Cavallo, F. R., Cerrito, L., Chabaud, V., Chapkin, M., Charpentier, Ph., Chaussard, L., Chauveau, J., Checchia, P., Chelkov, G. A., Chen, M., Chierici, R., Chliapnikov, P., Chochula, P., Chorowicz, V., Chudoba, J., Cindro, V., Collins, P., Contreras, J. L., Contri, R., Cortina, E., Cosme, G., Cossutti, F., Crawley, H. B., Crennell, D., Crosetti, G., Maestro, J. Cuevas, Czellar, S., Dahl-Jensen, E., Dahm, J., Dalmagne, B., Dam, M., Damgaard, G., Dauncey, P. D., Davenport, M., Da Silva, W., Defoix, C., Deghorain, A., Della Ricca, G., Delpierre, P., Demaria, N., De Angelis, A., De Boer, W., De Brabandere, S., De Clercq, C., De La Vaissiere, C., De Lotto, B., De Min, A., De Paula, L., De Saint-Jean, C., Dijkstra, H., Di Ciaccio, L., Djama, F., Dolbeau, J., Donszelmann, M., Doroba, K., Dracos, M., Drees, J., Drees, K. A., Dris, M., Dufour, Y., Edsall, D., Ehret, R., Eigen, G., Ekelof, T., Ekspong, G., Elsing, M., Engel, J-P., Ershaidat, N., Erzen, B., Falk, E., Fassouliotis, D., Feindt, M., Ferrer, A., Filippas, T. A., Firestone, A., Fischer, P. A., Foeth, H., Fokitis, E., Fontanelli, F., Formenti, F., Franek, B., Frenkiel, P., Fries, D. C., Frodesen, A. G., Fruhwirth, R., Fulda-Quenzer, F., Fuster, J., Galloni, A., Gamba, D., Gandelman, M., Garcia, C., Garcia, J., Gaspar, C., Gasparini, U., Gavillet, Ph., Gazis, E. N., Gele, D., Gerber, J-P., Gerdyukov, L., Gibbs, M., Gokieli, R., Golob, B., Gopal, G., Gorn, L., Gorski, M., Gouz, Yu., Gracco, V., Graziani, E., Grosdidier, G., Grzelak, K., Gumenyuk, S., Gunnarsson, P., Gunther, M., Guy, J., Hahn, F., Hahn, S., Hajduk, Z., Hallgren, A., Hamacher, K., Hao, W., Harris, F. J., Hedberg, V., Henriques, R., Hernandez, J. J., Herquet, P., Herr, H., Hessing, T. L., Higon, E., Hilke, H. J., Hill, T. S., Holmgren, S-O., Holt, P. J., Holthuizen, D., Hoorelbeke, S., Houlden, M., Hrubec, J., Huet, K., Hultqvist, K., Jackson, J. N., Jacobsson, R., Jalocha, P., Janik, R., Jarlskog, Ch., Jarlskog, G., Jarry, P., Jean-Marie, B., Johansson, E. K., Jonsson, L., Jonsson, P., Joram, C., Juillot, P., Kaiser, M., Kapusta, F., Karafasoulis, K., Karlsson, M., Karvelas, E., Katsanevas, S., Katsoufis, E. C., Keranen, R., Khokhlov, Yu., Khomenko, B. A., Khovanski, N. N., King, B., Kjaer, N. J., Klein, H., Klovning, A., Kluit, P., Koene, B., Kokkinias, P., Koratzinos, M., Korcyl, K., Kourkoumelis, C., Kouznetsov, O., Kramer, P. H., Krammer, M., Kreuter, C., Kronkvist, I., Krumstein, Z., Krupinski, W., Kubinec, P., Kucewicz, W., Kurvinen, K., Lacasta, C., Laktineh, I., Lamblot, S., Lamsa, J. W., Lanceri, L., Lane, D. W., Langefeld, P., Last, I., Laugier, J-P., Lauhakangas, R., Leder, G., Ledroit, F., Lefebure, V., Legan, C. K., Leitner, R., Lemoigne, Y., Lemonne, J., Lenzen, G., Lepeltier, V., Lesiak, T., Liko, D., Lindner, R., Lipniacka, A., Lippi, I., Loerstad, B., Loken, J. G., Lopez, J. M., Loukas, D., Lutz, P., Lyons, L., MacNaughton, J., Maehlum, G., Maio, A., Malychev, V., Mandl, F., Marco, J., Marco, R., Marechal, B., Margoni, M., Marin, J-C., Mariotti, C., Markou, A., Maron, T., Martinez-Rivero, C., Martinez-Vidal, F., Marti i Garcia, S., Masik, J., Matorras, F., Matteuzzi, C., Matthiae, G., Mazzucato, M., Mc Cubbin, M, Mc Kay, R., Mc Nulty, R., Medbo, J., Merk, M., Meroni, C., Meyer, S., Meyer, W. T., Michelotto, M., Migliore, E., Mirabito, L., Mitaroff, W. A., Mjoernmark, U., Moa, T., Moeller, R., Moenig, K., Monge, M. R., Morettini, P., Mueller, H., Mundim, L. M., Murray, W. J., Muryn, B., Myatt, G., Naraghi, F., Navarria, F. L., Navas, S., Nawrocki, K., Negri, P., Nemecek, S., Neumann, W., Neumeister, N., Nicolaidou, R., Nielsen, B. S., Nieuwenhuizen, M., Nikolaenko, V., Niss, P., Nomerotski, A., Normand, A., Oberschulte-Beckmann, W., Obraztsov, V., Olshevski, A. G., Onofre, A., Orava, R., Osterberg, K., Ouraou, A., Paganini, P., Paganoni, M., Pages, P., Palka, H., Papadopoulou, Th. D., Papageorgiou, K., Pape, L., Parkes, C., Parodi, F., Passeri, A., Pegoraro, M., Peralta, L., Pernegger, H., Perrotta, A., Petridou, C., Petrolini, A., Petrovyck, M., Phillips, H. T., Piana, G., Pierre, F., Pimenta, M., Pindo, M., Plaszczynski, S., Podobrin, O., Pol, M. E., Polok, G., Poropat, P., Pozdniakov, V., Prest, M., Privitera, P., Pukhaeva, N., Pullia, A., Radojicic, D., Ragazzi, S., Rahmani, H., Ratoff, P. N., Read, A. L., Reale, M., Rebecchi, P., Redaelli, N. G., Regler, M., Reid, D., Renton, P. B., Resvanis, L. K., Richard, F., Richardson, J., Ridky, J., Rinaudo, G., Ripp, I., Romero, A., Roncagliolo, I., Ronchese, P., Roos, L., Rosenberg, E. I., Rosso, E., Roudeau, P., Rovelli, T., Ruckstuhl, W., Ruhlmann-Kleider, V., Ruiz, A., Rybicki, K., Saarikko, H., Sacquin, Y., Sadovsky, A., Sajot, G., Salt, J., Sanchez, J., Sannino, M., Schimmelpfennig, M., Schneider, H., Schwickerath, U., Schyns, M. A. E., Sciolla, G., Scuri, F., Seager, P., Sedykh, Y., Segar, A. M., Seitz, A., Sekulin, R., Shellard, R. C., Siccama, I., Siegrist, P., Simonetti, S., Simonetto, F., Sisakian, A. N., Sitar, B., Skaali, T. B., Smadja, G., Smirnov, N., Smirnova, O., Smith, G. R., Solovianov, O., Sosnowski, R., Souza-Santos, D., Spassov, T., Spiriti, E., Sponholz, P., Squarcia, S., Stanescu, C., Stapnes, S., Stavitski, I., Stichelbaut, F., Stocchi, A., Strauss, J., Strub, R., Stugu, B., Szczekowski, M., Szeptycka, M., Tabarelli, T., Tavernet, J. P., Tchikilev, O., Tilquin, A., Timmermans, J., Tkatchev, L. G., Todorov, T., Toet, D. Z., Tomaradze, A., Tome, B., Tonazzo, A., Tortora, L., Transtromer, G., Treille, D., Trischuk, W., Tristram, G., Trombini, A., Troncon, C., Tsirou, A., Turluer, M-L., Tyapkin, I. A., Tyndel, M., Tzamarias, S., Ueberschaer, B., Ullaland, O., Uvarov, V., Valenti, G., Vallazza, E., Vander Velde, C., Van Apeldoorn, G. W., Van Dam, P., Van Doninck, W. K., Van Eldik, J., Vassilopoulos, N., Vegni, G., Ventura, L., Venus, W., Verbeure, F., Verlato, M., Vertogradov, L. S., Vilanova, D., Vincent, P., Vitale, L., Vlasov, E., Vodopyanov, A. S., Vrba, V., Wahlen, H., Walck, C., Waldner, F., Weierstall, M., Weilhammer, P., Weiser, C., Wetherell, A. M., Wicke, D., Wickens, J. H., Wielers, M., Wilkinson, G. R., Williams, W. S. C., Winter, M., Witek, M., Woschnagg, K., Yip, K., Yushchenko, O., Zach, F., Zaitsev, A., Zalewska, A., Zalewski, P., Zavrtanik, D., Zevgolatakos, E., Zimin, N. I., Zito, M., Zontar, D., Zuberi, R., Zucchelli, G. C., Zumerle, G., and DELPHI Collaboration

Published
1996
Full Text
View/download PDF

48. Study of rareb decays with the DELPHI detector at LEP

Author

Adam, W., Adye, T., Agasi, E., Ajinenko, I., Aleksan, R., Alekseev, G. D., Alemany, R., Allport, P. P., Almehed, S., Amaldi, U., Amato, S., Andreazza, A., Andrieux, M. L., Antilogus, P., Apel, W-D., Arnoud, Y., Åsman, B., Augustin, J-E., Augustinus, A., Baillon, P., Bambade, P., Barao, F., Barate, R., Barbi, M., Bardin, D. Y., Baroncelli, A., Barring, O., Barrio, J. A., Bartl, W., Bates, M. J., Battaglia, M., Baubillier, M., Baudot, J., Becks, K. -H., Begalli, M., Beilliere, P., Belokopytov, Yu., Benvenuti, A. C., Berggren, M., Bertini, D., Bertrand, D., Bianchi, F., Bigi, M., Bilenky, M. S., Billoir, P., Bloch, D., Blume, M., Bolognese, T., Bonesini, M., Bonivento, W., Booth, P. S. L., Borisov, G., Bosio, C., Botner, O., Boudinov, E., Bouquet, B., Bourdarios, C., Bowcock, T. J. V., Bozzo, M., Branchini, P., Brand, K. D., Brenke, T., Brenner, R. A., Bricman, C., Brown, R. C. A., Bruckman, P., Brunet, J-M., Bugge, L., Buran, T., Burgsmueller, T., Buschmann, P., Buys, A., Cabrera, S., Caccia, M., Calvi, M., Camacho Rozas, A. J., Camporesi, T., Canale, V., Canepa, M., Cankocak, K., Cao, F., Carena, F., Carroll, L., Caso, C., Castillo Gimenez, M. V., Cattai, A., Cavallo, F. R., Chabaud, V., Charpentier, Ph., Chaussard, L., Chauveau, J., Checchia, P., Chelkov, G. A., Chen, M., Chierici, R., Chliapnikov, P., Chochula, P., Chorowicz, V., Chudoba, J., Cindro, V., Collins, P., Contreras, J. L., Contri, R., Cortina, E., Cosme, G., Cossutti, F., Crawley, H. B., Crennell, D., Crosetti, G., Maestro, J.Cuevas, Czellar, S., Dahl-Jensen, E., Dahm, J., Dalmagne, B., Dam, M., Damgaard, G., Dauncey, P. D., Davenport, M., Da Silva, W., Defoix, C., Deghorain, A., Della Ricca, G., Delpierre, P., Demaria, N., De Angelis, A., De Boer, W., De Brabandere, S., De Clercq, C., De La Vaissiere, C., De Lotto, B., De Min, A., De Paula, L., De Saint-Jean, C., Dijkstra, H., Di Ciaccio, L., Djama, F., Dolbeau, J., Donszelmann, M., Doroba, K., Dracos, M., Drees, J., Drees, K. -A., Dris, M., Durand, J-D., Edsall, D., Ehret, R., Eigen, G., Ekelof, T., Ekspong, G., Elsing, M., Engel, J-P., Erzen, B., Santo, M.Espirito, Falk, E., Fassouliotis, D., Feindt, M., Fenyuk, A., Ferrer, A., Fichet, S., Filippas, T. A., Firestone, A., Fischer, P. -A., Foeth, H., Fokitis, E., Fontanelli, F., Formenti, F., Franek, B., Frenkiel, P., Fries, D. C., Frodesen, A. G., Fruhwirth, R., Fulda-Quenzer, F., Fuster, J., Galloni, A., Gamba, D., Gandelman, M., Garcia, C., Garcia, J., Gaspar, C., Gasparini, U., Gavillet, Ph., Gazis, E. N., Gele, D., Gerber, J-P., Gibbs, M., Gokieli, R., Golob, B., Gopal, G., Gorn, L., Gorski, M., Gouz, Yu., Gracco, V., Graziani, E., Grosdidier, G., Grzelak, K., Gumenyuk, S., Gunnarsson, P., Gunther, M., Guy, J., Hahn, F., Hahn, S., Hajduk, Z., Hallgren, A., Hamacher, K., Hao, W., Harris, F. J., Hedberg, V., Henriques, R., Hernandez, J. J., Herquet, P., Herr, H., Hessing, T. L., Higon, E., Hilke, H. J., Hill, T. S., Holmgren, S-O., Holt, P. J., Holthuizen, D., Hoorelbeke, S., Houlden, M., Hrubec, J., Huet, K., Hultqvist, K., Jackson, J. N., Jacobsson, R., Jalocha, P., Janik, R., Jarlskog, Ch., Jarlskog, G., Jarry, P., Jean-Marie, B., Johansson, E. K., Jonsson, L., Jonsson, P., Joram, C., Juillot, P., Kaiser, M., Kapusta, F., Karafasoulis, K., Karlsson, M., Karvelas, E., Katsanevas, S., Katsoufis, E. C., Keranen, R., Khokhlov, Yu., Khomenko, B. A., Khovanski, N. N., King, B., Kjaer, N. J., Klein, H., Klovning, A., Kluit, P., Koene, B., Kokkinias, P., Koratzinos, M., Korcyl, K., Kourkoumelis, C., Kouznetsov, O., Kramer, P. -H., Krammer, M., Kreuter, C., Kronkvist, I., Krumstein, Z., Krupinski, W., Kubinec, P., Kucewicz, W., Kurvinen, K., Lacasta, C., Laktineh, I., Lamblot, S., Lamsa, J. W., Lanceri, L., Lane, D. W., Langefeld, P., Last, I., Laugier, J-P., Lauhakangas, R., Leder, G., Ledroit, F., Lefebure, V., Legan, C. K., Leitner, R., Lemoigne, Y., Lemonne, J., Lenzen, G., Lepeltier, V., Lesiak, T., Libby, J., Liko, D., Lindner, R., Lipniacka, A., Lippi, I., Loerstad, B., Loken, J. G., Lopez, J. M., Loukas, D., Lutz, P., Lyons, L., MacNaughton, J., Maehlum, G., Maio, A., Malychev, V., Marco, J., Marco, R., Marechal, B., Margoni, M., Marin, J-C., Mariotti, C., Markou, A., Maron, T., Martinez-Rivero, C., Martinez-Vidal, F., Marti i Garcia, S., Masik, J., Matorras, F., Matteuzzi, C., Matthiae, G., Mazzucato, M., Cubbin, M. Mc, Kay, R. Mc, Nulty, R. Mc, Medbo, J., Merk, M., Meroni, C., Meyer, S., Meyer, W. T., Miagkov, A., Michelotto, M., Migliore, E., Mirabito, L., Mitaroff, W. A., Mjoernmark, U., Moa, T., Moeller, R., Moenig, K., Monge, M. R., Morettini, P., Mueller, H., Mundim, L. M., Murray, W. J., Muryn, B., Myatt, G., Naraghi, F., Navarria, F. L., Navas, S., Nawrocki, K., Negri, P., Neumann, W., Neumeister, N., Nicolaidou, R., Nielsen, B. S., Nieuwenhuizen, M., Nikolaenko, V., Niss, P., Nomerotski, A., Normand, A., Novak, M., Oberschulte-Beckmann, W., Obraztsov, V., Olshevski, A. G., Onofre, A., Orava, R., Osterberg, K., Ouraou, A., Paganini, P., Paganoni, M., Pages, P., Palka, H., Papadopoulou, Th. D., Papageorgiou, K., Pape, L., Parkes, C., Parodi, F., Passeri, A., Pegoraro, M., Peralta, L., Pernegger, H., Pernicka, M., Perrotta, A., Petridou, C., Petrolini, A., Petrovyck, M., Phillips, H. T., Piana, G., Pierre, F., Pimenta, M., Pindo, M., Plaszczynski, S., Podobrin, O., Pol, M. E., Polok, G., Poropat, P., Pozdniakov, V., Prest, M., Privitera, P., Pukhaeva, N., Pullia, A., Radojicic, D., Ragazzi, S., Rahmani, H., Rames, J., Ratoff, P. N., Read, A. L., Reale, M., Rebecchi, P., Redaelli, N. G., Regler, M., Reid, D., Renton, P. B., Resvanis, L. K., Richard, F., Richardson, J., Ridky, J., Rinaudo, G., Ripp, I., Romero, A., Roncagliolo, I., Ronchese, P., Roos, L., Rosenberg, E. I., Rosso, E., Roudeau, P., Rovelli, T., Ruckstuhl, W., Ruhlmann-Kleider, V., Ruiz, A., Rybicki, K., Saarikko, H., Sacquin, Y., Sadovsky, A., Sahr, O., Sajot, G., Salt, J., Sanchez, J., Sannino, M., Schimmelpfennig, M., Schneider, H., Schwickerath, U., Schyns, M. A. E., Sciolla, G., Scuri, F., Seager, P., Sedykh, Y., Segar, A. M., Seitz, A., Sekulin, R., Shellard, R. C., Siccama, I., Siegrist, P., Simonetti, S., Simonetto, F., Sisakian, A. N., Sitar, B., Skaali, T. B., Smadja, G., Smirnov, N., Smirnova, O., Smith, G. R., Sokolov, A., Solovianov, O., Sosnowski, R., Souza-Santos, D., Spassov, T., Spiriti, E., Sponholz, P., Squarcia, S., Stanescu, C., Stapnes, S., Stavitski, I., Stevenson, K., Stichelbaut, F., Stocchi, A., Strauss, J., Strub, R., Stugu, B., Szczekowski, M., Szeptycka, M., Tabarelli, T., Tavernet, J. P., Tchikilev, O., Thomas, J., Tilquin, A., Timmermans, J., Tkatchev, L. G., Todorov, T., Todorova, S., Toet, D. Z., Tomaradze, A., Tome, B., Tonazzo, A., Tortora, L., Transtromer, G., Treille, D., Trischuk, W., Tristram, G., Trombini, A., Troncon, C., Tsirou, A., Turluer, M-L., Tyapkin, I. A., Tyndel, M., Tzamarias, S., Ueberschaer, B., Ullaland, O., Uvarov, V., Valenti, G., Vallazza, E., Velde, C. Vander, Van Apeldoorn, G. W., Van Dam, P., Van Doninck, W. K., Van Eldik, J., Vassilopoulos, N., Vegni, G., Ventura, L., Venus, W., Verbeure, F., Verlato, M., Vertogradov, L. S., Vilanova, D., Vincent, P., Vitale, L., Vlasov, E., Vodopyanov, A. S., Vrba, V., Wahlen, H., Walck, C., Waldner, F., Weierstall, M., Weilhammer, P., Weiser, C., Wetherell, A. M., Wicke, D., Wickens, J. H., Wielers, M., Wilkinson, G. R., Williams, W. S. C., Winter, M., Witek, M., Woschnagg, K., Yip, K., Yushchenko, O., Zach, F., Zaitsev, A., Zalewska, A., Zalewski, P., Zavrtanik, D., Zevgolatakos, E., Zimin, N. I., Zito, M., Zontar, D., Zucchelli, G. C., Zumerle, G., and DELPHI Collaboration

Published
1996
Full Text
View/download PDF

49. Search for high massγγ resonances in $$q\bar q\gamma \gamma $$ at LEP Iat LEP I

Author

Abreu, P., Adam, W., Adye, T., Agasi, E., Ajinenko, I., Aleksan, R., Alekseev, G. D., Alemany, R., Allport, P. P., Almehed, S., Amaldi, U., Amato, S., Andreazza, A., Andrieux, M. L., Antilogus, P., Apel, W-D., Arnoud, Y., Åsman, B., Augustin, J-E., Augustinus, A., Baillon, P., Bambade, P., Barao, F., Barate, R., Barbi, M., Bardin, D. Y., Baroncelli, A., Barring, O., Barrio, J. A., Bartl, W., Bates, M. J., Battaglia, M., Baubillier, M., Baudot, J., Becks, K-H., Begalli, M., Beilliere, P., Belokopytov, Yu., Benvenuti, A. C., Berggren, M., Bertini, D., Bertrand, D., Bianchi, F., Bigi, M., Bilenky, M. S., Billoir, P., Bloch, D., Blume, M., Bolognese, T., Bonesini, M., Bonivento, W., Booth, P. S. L., Borisov, G., Bosio, C., Botner, O., Boudinov, E., Bouquet, B., Bourdarios, C., Bowcock, T. J. V., Bozzo, M., Branchini, P., Brand, K. D., Brenke, T., Brenner, R. A., Bricman, C., Brown, R. C. A., Bruckman, P., Brunet, J-M., Bugge, L., Buran, T., Burgsmueller, T., Buschmann, P., Buys, A., Cabrera, S., Caccia, M., Calvi, M., Camacho Rozas, A. J., Camporesi, T., Canale, V., Canepa, M., Cankocak, K., Cao, F., Carena, F., Carroll, L., Caso, C., Castillo Gimenez, M. V., Cattai, A., Cavallo, F. R., Chabaud, V., Charpentier, Ph., Chaussard, L., Checchia, P., Chelkov, G. A., Chen, M., Chierici, R., Chliapnikov, P., Chochula, P., Chorowicz, V., Chudoba, J., Cindro, V., Collins, P., Contreras, J. L., Contri, R., Cortina, E., Cosme, G., Cossutti, F., Crawley, H. B., Crennell, D., Crosetti, G., Maestro, J.Cuevas, Czellar, S., Dahl-Jensen, E., Dahm, J., Dalmagne, B., Dam, M., Damgaard, G., Dauncey, P. D., Davenport, M., Silva, W.Da, Defoix, C., Deghorain, A., Ricca, G.Della, Delpierre, P., Demaria, N., De Angelis, A., De Boer, W., De Brabandere, S., De Clercq, C., De La Vaissiere, C., De Lotto, B., De Min, A., De Paula, L., De Saint-Jean, C., Dijkstra, H., Di Ciaccio, L., Djama, F., Dolbeau, J., Donszelmann, M., Doroba, K., Dracos, M., Drees, J., Drees, K. -A., Dris, M., Durand, J-D., Edsall, D., Ehret, R., Eigen, G., Ekelof, T., Ekspong, G., Elsing, M., Engel, J-P., Erzen, B., Santo, M.Espirito, Falk, E., Fassouliotis, D., Feindt, M., Fenyuk, A., Ferrer, A., Fichet, S., Filippas, T. A., Firestone, A., Fischer, P. -A., Foeth, H., Fokitis, E., Fontanelli, F., Formenti, F., Franek, B., Frenkiel, P., Fries, D. C., Frodesen, A. G., Fruhwirth, R., Fulda-Quenzer, F., Fuster, J., Galloni, A., Gamba, D., Gandelman, M., Garcia, C., Garcia, J., Gaspar, C., Gasparini, U., Gavillet, Ph., Gazis, E. N., Gele, D., Gerber, J-P., Gibbs, M., Gokieli, R., Golob, B., Gopal, G., Gorn, L., Gorski, M., Gouz, Yu., Gracco, V., Graziani, E., Grosdidier, G., Grzelak, K., Gumenyuk, S., Gunnarsson, P., Gunther, M., Guy, J., Hahn, F., Hahn, S., Hallgren, A., Hamacher, K., Hao, W., Harris, F. J., Hedberg, V., Henriques, R., Hernandez, J. J., Herquet, P., Herr, H., Hessing, T. L., Higon, E., Hilke, H. J., Hill, T. S., Holmgren, S-O., Holt, P. J., Holthuizen, D., Hoorelbeke, S., Houlden, M., Hrubec, J., Huet, K., Hultqvist, K., Jackson, J. N., Jacobsson, R., Jalocha, P., Janik, R., Jarlskog, Ch., Jarlskog, G., Jarry, P., Jean-Marie, B., Johansson, E. K., Jonsson, L., Jonsson, P., Joram, C., Juillot, P., Kaiser, M., Kapusta, F., Karafasoulis, K., Karlsson, M., Karvelas, E., Katsanevas, S., Katsoufis, E. C., Keranen, R., Khokhlov, Yu., Khomenko, B. A., Khovanski, N. N., King, B., Kjaer, N. J., Klein, H., Klovning, A., Kluit, P., Koene, B., Kokkinias, P., Koratzinos, M., Korcyl, K., Kourkoumelis, C., Kouznetsov, O., Kramer, P. -H., Krammer, M., Kreuter, C., Kronkvist, I., Krumstein, Z., Krupinski, W., Kubinec, P., Kucewicz, W., Kurvinen, K., Lacasta, C., Laktineh, I., Lamsa, J. W., Lanceri, L., Lane, D. W., Langefeld, P., Last, I., Laugier, J-P., Lauhakangas, R., Leder, G., Ledroit, F., Lefebure, V., Legan, C. K., Leitner, R., Lemoigne, Y., Lemonne, J., Lenzen, G., Lepeltier, V., Lesiak, T., Libby, J., Liko, D., Lindner, R., Lipniacka, A., Lippi, I., Loerstad, B., Loken, J. G., Lopez, J. M., Loukas, D., Lutz, P., Lyons, L., MacNaughton, J., Maehlum, G., Maio, A., Malmgren, T. G. M., Malychev, V., Mandl, F., Marco, J., Marco, R., Marechal, B., Margoni, M., Marin, J-C., Mariotti, C., Markou, A., Maron, T., Martinez-Rivero, C., Martinez-Vidal, F., Marti i Garcia, S., Masik, J., Matorras, F., Matteuzzi, C., Matthiae, G., Mazzucato, M., Cubbin, M.Mc, Kay, R.Mc, Nulty, R.Mc, Medbo, J., Merk, M., Meroni, C., Meyer, S., Meyer, W. T., Miagkov, A., Michelotto, M., Migliore, E., Mirabito, L., Mitaroff, W. A., Mjoernmark, U., Moa, T., Moeller, R., Moenig, K., Monge, M. R., Morettini, P., Mueller, H., Mundim, L. M., Murray, W. J., Muryn, B., Myatt, G., Naraghi, F., Navarria, F. L., Navas, S., Nawrocki, K., Negri, P., Neumann, W., Neumeister, N., Nicolaidou, R., Nielsen, B. S., Nieuwenhuizen, M., Nikolaenko, V., Niss, P., Nomerotski, A., Normand, A., Novak, M., Oberschulte-Beckmann, W., Obraztsov, V., Olshevski, A. G., Onofre, A., Orava, R., Osterberg, K., Ouraou, A., Paganini, P., Paganoni, M., Pages, P., Pain, R., Palka, H., Papadopoulou, Th. D., Papageorgiou, K., Pape, L., Parkes, C., Parodi, F., Passeri, A., Pegoraro, M., Peralta, L., Pernicka, M., Perrotta, A., Petridou, C., Petrolini, A., Petrovyck, M., Phillips, H. T., Piana, G., Pierre, F., Pimenta, M., Plaszczynski, S., Podobrin, O., Pol, M. E., Polok, G., Poropat, P., Pozdniakov, V., Prest, M., Privitera, P., Pukhaeva, N., Pullia, A., Radojicic, D., Ragazzi, S., Rahmani, H., Ratoff, P. N., Read, A. L., Reale, M., Rebecchi, P., Redaelli, N. G., Regler, M., Reid, D., Renton, P. B., Resvanis, L. K., Richard, F., Richardson, J., Ridky, J., Rinaudo, G., Ripp, I., Romero, A., Roncagliolo, I., Ronchese, P., Roos, L., Rosenberg, E. I., Rosso, E., Roudeau, P., Rovelli, T., Ruckstuhl, W., Ruhlmann-Kleider, V., Ruiz, A., Saarikko, H., Sacquin, Y., Sadovsky, A., Sahr, O., Sajot, G., Salt, J., Sanchez, J., Sannino, M., Schimmelpfennig, M., Schneider, H., Schwickerath, U., Schyns, M. A. E., Sciolla, G., Scuri, F., Seager, P., Sedykh, Y., Segar, A. M., Seitz, A., Sekulin, R., Serbelloni, L., Shellard, R. C., Siccama, I., Siegrist, P., Simonetti, S., Simonetto, F., Sisakian, A. N., Sitar, B., Skaali, T. B., Smadja, G., Smirnov, N., Smirnova, O., Smith, G. R., Solovianov, O., Sosnowski, R., Souza-Santos, D., Spassov, T., Spiriti, E., Sponholz, P., Squarcia, S., Stanescu, C., Stapnes, S., Stavitski, I., Stevenson, K., Stichelbaut, F., Stocchi, A., Strauss, J., Strub, R., Stugu, B., Szczekowski, M., Szeptycka, M., Tabarelli, T., Tavernet, J. P., Tchikilev, O., Thomas, J., Tilquin, A., Timmermans, J., Tkatchev, L. G., Todorov, T., Todorova, S., Toet, D. Z., Tomaradze, A., Tonazzo, A., Tortora, L., Transtromer, G., Treille, D., Trischuk, W., Tristram, G., Trombini, A., Troncon, C., Tsirou, A., Turluer, M. -L., Tyapkin, I. A., Tyndel, M., Tzamarias, S., Ueberschaer, B., Ullaland, O., Uvarov, V., Valenti, G., Vallazza, E., Velde, C.Vander, Van Apeldoorn, G. W., Van Dam, P., Van Eldik, J., Vassilopoulos, N., Vegni, G., Ventura, L., Venus, W., Verbeure, F., Verlato, M., Vertogradov, L. S., Vilanova, D., Vincent, P., Vitale, L., Vlasov, E., Vodopyanov, A. S., Vrba, V., Wahlen, H., Walck, C., Waldner, F., Weierstall, M., Weilhammer, P., Weiser, C., Wetherell, A. M., Wicke, D., Wickens, J. H., Wielers, M., Wilkinson, G. R., Williams, W. S. C., Winter, M., Witek, M., Woschnagg, K., Yip, K., Yushchenko, O., Zach, F., Zaitsev, A., Zalewska, A., Zalewski, P., Zavrtanik, D., Zevgolatakos, E., Zimin, N. I., Zito, M., Zontar, D., Zucchelli, G. C., Zumerle, G., and DELPHI Collaboration

Published
1996
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results