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1. CAST constraints on the axion-electron coupling

Author

Barth, K., Belov, A., Beltran, B., Brauninger, H., Carmona, J. M., Collar, J. I., Dafni, T., Davenport, M., Di Lella, L., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Ribas, E. Ferrer, Fischer, H., Franz, J., Friedrich, P., Galan, J., Garcia, J. A., Geralis, T., Giomataris, I., Gninenko, S., Gomez, H., Hassinoff, M. D., Heinsius, F. H., Hoffmann, D. H. H., Irastorza, I. G., Jacoby, J., Jakovcic, K., Kang, D., Konigsmann, K., Kotthaus, R., Kousouris, K., Krcmar, M., Kuster, M., Lakic, B., Liolios, A., Ljubicic, A., Lutz, G., Luzon, G., Miller, D. W., Papaevangelou, T., Pivovaroff, M. J., Raffelt, G., Redondo, J., Riege, H., Rodriguez, A., Ruz, J., Savvidis, I., Semertzidis, Y., Stewart, L., Van Bibber, K., Vieira, J. D., Villar, J. A., Vogel, J. K., Walckiers, L., and Zioutas, K.

Subjects
Astrophysics - Solar and Stellar Astrophysics, High Energy Physics - Phenomenology
Abstract

In non-hadronic axion models, which have a tree-level axion-electron interaction, the Sun produces a strong axion flux by bremsstrahlung, Compton scattering, and axio-recombination, the "BCA processes." Based on a new calculation of this flux, including for the first time axio-recombination, we derive limits on the axion-electron Yukawa coupling g_ae and axion-photon interaction strength g_ag using the CAST phase-I data (vacuum phase). For m_a < 10 meV/c2 we find g_ag x g_ae< 8.1 x 10^-23 GeV^-1 at 95% CL. We stress that a next-generation axion helioscope such as the proposed IAXO could push this sensitivity into a range beyond stellar energy-loss limits and test the hypothesis that white-dwarf cooling is dominated by axion emission.

Published
2013
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2. Search for 14.4 keV solar axions emitted in the M1-transition of 57Fe nuclei with CAST

Author

CAST Collaboration, Andriamonje, S., Aune, S., Autiero, D., Barth, K., Belov, A., Beltrán, B., Bräuninger, H., Carmona, J. M., Cebrián, S., Collar, J. I., Dafni, T., Davenport, M., Di Lella, L., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Ferrer-Ribas, E., Fischer, H., Franz, J., Friedrich, P., Geralis, T., Giomataris, I., Gninenko, S., Gómez, H., Hasinoff, M., Heinsius, F. H., Hoffmann, D. H. H., Irastorza, I. G., Jacoby, J., Jakovčić, K., Kang, D., Königsmann, K., Kotthaus, R., Krčmar, M., Kousouris, K., Kuster, M., Lakić, B., Lasseur, C., Liolios, A., Ljubičić, A., Lutz, G., Luzón, G., Miller, D., Morales, J., Ortiz, A., Papaevangelou, T., Placci, A., Raffelt, G., Riege, H., Rodríguez, A., Ruz, J., Savvidis, I., Semertzidis, Y., Serpico, P., Stewart, L., Vieira, J., Villar, J., Vogel, J., Walckiers, L., and Zioutas, K.

Subjects
High Energy Physics - Experiment
Abstract

We have searched for 14.4 keV solar axions or more general axion-like particles (ALPs), that may be emitted in the M1 nuclear transition of 57Fe, by using the axion-to-photon conversion in the CERN Axion Solar Telescope (CAST) with evacuated magnet bores (Phase I). From the absence of excess of the monoenergetic X-rays when the magnet was pointing to the Sun, we set model-independent constraints on the coupling constants of pseudoscalar particles that couple to two photons and to a nucleon g_{a\gamma} |-1.19 g_{aN}^{0}+g_{aN}^{3}|<1.36\times 10^{-16} GeV^{-1} for m_{a}<0.03 eV at the 95% confidence level., Comment: 23 pages, 5 figures. Revised version of the paper after referee`s comments. Main changes in the Measurement and data analysis section

Published
2009
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3. Search for solar axion emission from 7Li and D(p,gamma)3He nuclear decays with the CAST gamma-ray calorimeter

Author

CAST Collaboration, Andriamonje, S., Aune, S., Autiero, D., Barth, K., Belov, A., Beltran, B., Brauninger, H., Carmona, J. M., Cebrian, S., Collar, J. I., Dafni, T., Davenport, M., Lella, L. Di., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Ribas, E. Ferrer., Fischer, H., Franz, J., Friedrich, P., Geralis, T., Giomataris, I., Gninenko, S., Gomez, H., Hasinoff, M., Heinsius, F. H., Hoffmann, D. H. H., Irastorza, I. G., Jacoby, J., Jakovcic, K., Kang, D., Konigsmann, K., Kotthaus, R., Krcmar, M., Kousouris, K., Kuster, M., Lakic, B., Lasseur, C., Liolios, A., Ljubicic, A., Lutz, G., Luzon, G., Miller, D. W., Morales, J., Ortiz, A., Papaevangelou, T., Placci, A., Raffelt, G., Riege, H., Rodriguez, A., Ruz, J., Savvidis, I., Semertzidis, Y., Serpico, P., Stewart, L., Vieira, J. D., Villar, J., Vogel, J., Walckiers, L., and Zioutas, K.

Subjects
High Energy Physics - Experiment
Abstract

We present the results of a search for a high-energy axion emission signal from 7Li (0.478 MeV) and D(p,gamma)3He (5.5 MeV) nuclear transitions using a low-background gamma-ray calorimeter during Phase I of the CAST experiment. These so-called "hadronic axions" could provide a solution to the long-standing strong-CP problem and can be emitted from the solar core from nuclear M1 transitions. This is the first such search for high-energy pseudoscalar bosons with couplings to nucleons conducted using a helioscope approach. No excess signal above background was found., Comment: 20 pages, 8 figures, final version to be published in JCAP

Published
2009
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4. The X-ray Telescope of CAST

Author

Kuster, M., Bräuninger, H., Cébrian, S., Davenport, M., Elefteriadis, C., Englhauser, J., Fischer, H., Franz, J., Friedrich, P., Hartmann, R., Heinsius, F. H., Hoffmann, D. H. H., Hoffmeister, G., Joux, J. N., Kang, D., Königsmann, K., Kotthaus, R., Papaevangelou, T., Lasseur, C., Lippitsch, A., Lutz, G., Morales, J., Rodríguez, A., Strüder, L., Vogel, J., and Zioutas, K.

Subjects
Physics - Instrumentation and Detectors, Astrophysics, High Energy Physics - Experiment
Abstract

The Cern Axion Solar Telescope (CAST) is in operation and taking data since 2003. The main objective of the CAST experiment is to search for a hypothetical pseudoscalar boson, the axion, which might be produced in the core of the sun. The basic physics process CAST is based on is the time inverted Primakoff effect, by which an axion can be converted into a detectable photon in an external electromagnetic field. The resulting X-ray photons are expected to be thermally distributed between 1 and 7 keV. The most sensitive detector system of CAST is a pn-CCD detector combined with a Wolter I type X-ray mirror system. With the X-ray telescope of CAST a background reduction of more than 2 orders off magnitude is achieved, such that for the first time the axion photon coupling constant g_agg can be probed beyond the best astrophysical constraints g_agg < 1 x 10^-10 GeV^-1., Comment: 19 pages, 25 figures and images, replaced by the revised version accepted for publication in New Journal of Physics

Published
2007
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5. The discovery of X-rays from Venus with Chandra

Author

Dennerl, K., Burwitz, V., Englhauser, J., Lisse, C., and Wolk, S.

Subjects
Astrophysics
Abstract

On January 10 and 13, 2001, Venus was observed for the first time with an X-ray astronomy satellite. The observation, performed with the ACIS-I and LETG/ACIS-S instruments on Chandra, yielded data of high spatial, spectral, and temporal resolution. Venus is clearly detected as a half-lit crescent, with considerable brightening on the sunward limb. The morphology agrees well with that expected from fluorescent scattering of solar X-rays in the planetary atmosphere. The radiation is observed at discrete energies, mainly at the O-K_alpha energy of 0.53 keV. Fluorescence radiation is also detected from C-K_alpha at 0.28 keV and, marginally, from N-K_alpha at 0.40 keV. An additional emission line is indicated at 0.29 keV, which might be the signature of the C 1s --> pi* transition in CO2 and CO. Evidence for temporal variability of the X-ray flux was found at the 2.6 sigma level, with fluctuations by factors of a few times indicated on time scales of minutes. All these findings are fully consistent with fluorescent scattering of solar X-rays. No other source of X-ray emission was detected, in particular none from charge exchange interactions between highly charged heavy solar wind ions and atmospheric neutrals, the dominant process for the X-ray emission of comets. This is in agreement with the sensitivity of the observation., Comment: additional information to A&A 386, 319-330, 2002 (astro-ph/0204237); to appear in Proc. Symp. `New Visions of the X-ray Universe in the XMM-Newton and Chandra Era', 26-30 November 2001, ESTEC, The Netherlands

Published
2002

6. Discovery of X-rays from Venus with Chandra

Author

Dennerl, K., Burwitz, V., Englhauser, J., Lisse, C., and Wolk, S.

Subjects
Astrophysics
Abstract

On January 10 and 13, 2001, Venus was observed for the first time with an X-ray astronomy satellite. The observation, performed with the ACIS-I and LETG/ACIS-S instruments on Chandra, yielded data of high spatial, spectral, and temporal resolution. Venus is clearly detected as a half-lit crescent, with considerable brightening on the sunward limb. The morphology agrees well with that expected from fluorescent scattering of solar X-rays in the planetary atmosphere. The radiation is observed at discrete energies, mainly at the O-K_alpha energy of 0.53 keV. Fluorescent radiation is also detected from C-K_alpha at 0.28 keV and, marginally, from N-K_alpha at 0.40 keV. An additional emission line is indicated at 0.29 keV, which might be the signature of the C 1s --> pi* transition in CO_2 and CO. Evidence for temporal variability of the X-ray flux was found at the 2.6 sigma level, with fluctuations by factors of a few times indicated on time scales of minutes. All these findings are fully consistent with fluorescent scattering of solar X-rays. No other source of X-ray emission was detected, in particular none from charge exchange interactions between highly charged heavy solar wind ions and atmospheric neutrals, the dominant process for the X-ray emission of comets. This is in agreement with the sensitivity of the observation., Comment: 12 pages, 9 figures

Published
2002
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7. A bright X-ray transient towards NGC 5128 (Centaurus A)

Author

Steinle, H., Dennerl, K., and Englhauser, J.

Subjects
Astrophysics
Abstract

During five ROSAT HRI observations in July 1995, a bright X-ray source (designated 1RXH J132519.8-430312) was detected 2.5' south-west of the nucleus of NGC 5128 (Centaurus A) at the outer regions of the elliptical galaxy. At that time it was the brightest point source in the ROSAT HRI field-of-view. All other ROSAT observations made before and after these observations show no trace of the source suggesting that this is a highly variable object. Chandra observations of Cen A made in September 1999 show a source at the ROSAT position which may be the quiescent counterpart of the transient. It is very probable that the transient is located in NGC 5128. Given the existence of a transient source that close to the direction of NGC 5128, all observations (at least in soft X-rays) of Cen A, with instruments of low spatial resolution, must take the presence and variability of this object into account., Comment: accepted for Astron. Astrophys. Lett. in April 2000; more info at http://www.mpe.mpg.de/Cen-A/

Published
2000

8. Properties of the X-ray pulsar GX 301-2 in hard X-rays

Author

Borkus, V., Kaniovsky, A., Sunyaev, R., Efremov, V., Kretschmar, P., Staubert, R., Englhauser, J., and Pietsch, W.

Subjects
Astrophysics
Abstract

In 1993-1994 a series of observations of the X-ray pulsar GX 301-2 by HEXE onboard Mir-Kvant was made. A period of pulsations was measured (it varied between 675 and 678 s) and pulse profiles in different energy bands were produced. The measured luminosity in the 20-100 keV energy range changed substantially between 8x10^34 and 7x10^35 d^2 erg/s (d is the distance to the source in kpc). The obtained spectrum is quite satisfactory described by the canonical model for X-ray pulsars with gamma=1.3, E_c~23 keV, E_f~9 keV. It changed weakly between the observations, but was softest at brightness maximum. Significant variations of the spectral hardness over the pulse phase were detected, but the accumulated data are insufficient to quantify variations in spectral parameters. No significant traces of cyclotron lines were found. An interpretation of the pulse profiles as superposition of emissions from two flat polar caps (with inclusion of gravitational lensing) leads to an estimate of the angle between the magnetic axis and axis of rotation of 40-70 deg and an angle between the direction to the observer and the rotation axis of 75-85 deg., Comment: 12 pages, 7 figures

Published
1997

10. ROSAT’s All-Sky X-Ray View

Author

Voges, W., Boller, Th, Englhauser, J., Freyberg, M. J., Supper, R., Banday, Anthony J., editor, Zaroubi, Saleem, editor, and Bartelmann, Matthias, editor

Published
2001
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14. X-Ray and Extreme Ultraviolet Emission from Comet P/Encke 1997

Author

Lisse, C.M., Christian, D., Dennerl, K., Englhauser, J., Trumper, Desch, M., Marshall, F.E., Petre, R., and Snowden, S.

Subjects
Comets -- Spectra, Solar wind -- Analysis, X-ray astronomy -- Research, Ultraviolet astronomy -- Analysis, Astronomy, Earth sciences
Abstract

In an effort to understand the newly discovered phenomenon of cometary X-ray emission, we have obtained observations of the short period (3.3 years), well-studied comet 2P/Encke (Encke) during its July 1997 close approach to Earth. Extended, variable emission on the sunward side of the nucleus was found in the Rontgen X-ray satellite High Resolution Imager (HRI) at 0.090-0.75 keV and in the Extreme Ultraviolet Explorer (EUVE) scanner telescopes' Lexan B 0.090- to 0.28-keV and Al/Ti/C 0.050- to 0.16-keV bandpasses; useful upper limits were found in the Ti/Sb/Al 0.020- to 0.040-eV bandpass. Similar to our results for C/Hyakutake, the emission morphology was roughly symmetric with respect to a vector from the comet's nucleus toward the Sun, with a light curve consisting of a slowly varying baseline emission and a large impulsive event on 7 July 1997 with a time scale of approximately 3 h and an amplitude of approximately 3 times the baseline. A count rate of approximately 0.17 counts s(super -1) in the HRI was measured for the slowly varying emission, corresponding to a total luminosity L(sub x) of 4 x 10(super 14) erg s(super -1). Unlike Hyakutake, however, the bulk of the emission clearly originates outside the comet's bow-shock, arguing against the magnetic reconnection and plasma dust emission models. The comet's lightcurve does not correlate with the solar X-ray lightcurve, ruling out scattering of solar X-rays as the emission mechanism. The multiwavelength HRI/EUVE photometry is inconsistent with the Haberli et al. (1997, Science 276, 939-942) charge transfer, plasma dust, and attogram dust models of cometary X-ray emission and is consistent with the Wegmann et al. (1988, Planet. Space Sci. 46, 603-612) charge exchange, 0.15- to 0.45-keV thermal bremsstrahlung, and photon index 1.6-2.0 power law models. While the impulsive event correlates very well with the passage of a solar magnetic field boundary at the Earth and an increase in the solar wind particle flux, it is not coincident, according to current models of the solar wind magnetic current sheet, with the passage of the sector boundary by the comet, suggesting that new models of the current sheet are necessary. Key Words: comets; atmospheres; coma; solar wind; spectrometry, X-rays.

Published
1999

16. The Rosat All-Sky Survey Bright Source Catalog

Author

Voges, W., Aschenbach, B., Boller, Th., Bräuninger, H., Briel, U., Burkert, W., Dennerl, K., Englhauser, J., Gruber, R., Haberl, F., Hartner, G., Hasinger, G., Kürster, M., Pfeffermann, E., Pietsch, W., Predehl, P., Rosso, C., Schmitt, J. H. M. M., Trümper, J., Zimmermann, U., McLean, Brian J., editor, Golombek, Daniel A., editor, Hayes, Jeffrey J. E., editor, and Payne, Harry E., editor

Published
1998
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18. The Rosat All-Sky Survey Bright Source Catalog

Author

Voges, W., primary, Aschenbach, B., additional, Boller, Th., additional, Bräuninger, H., additional, Briel, U., additional, Burkert, W., additional, Dennerl, K., additional, Englhauser, J., additional, Gruber, R., additional, Haberl, F., additional, Hartner, G., additional, Hasinger, G., additional, Kürster, M., additional, Pfeffermann, E., additional, Pietsch, W., additional, Predehl, P., additional, Rosso, C., additional, Schmitt, J. H. M. M., additional, Trümper, J., additional, and Zimmermann, U., additional

Published
1997
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19. Spectral and temporal properties of the X-ray pulsar SMC X-1 at hard X-rays

Author

Kunz, M, Gruber, D. E, Kendziorra, E, Kretschmar, P, Maisack, M, Mony, B, Staubert, R, Doebereiner, S, Englhauser, J, and Pietsch, W

Subjects
Astrophysics
Abstract

The binary X-ray pulsar SMC X- 1 has been observed at hard X-rays with the High Energy X-Ray Experiment (HEXE) on nine occasions between Nov. 1987 and March 1989. A thin thermal bremsstrahlung fit to the phase averaged spectrum yields a plasma temperature (14.4 +/- 1.3) keV and a luminosity above (1.1 +/- 0.1) x 10 exp 38 erg/s in the 20-80 keV band. Pulse period values have been established for three observations, confirming the remarkably stable spin-up trend of SMC X-1. In one of the three observations the pulse profile was seen to deviate from a dominant double pulsation, while at the same time the pulsed fraction was unusually large. For one observation we determined for the first time the pulsed fraction in narrow energy bands. It increases with photon energy from about 20 percent up to over 60 percent in the energy range from 20 to 80 keV.

Published
1993

20. Hard x ray observations of Vela X-1 and A0535+26 with HEXE: Discovery of cyclotron lines

Author

Kendziorra, E, Mony, B, Kretschmar, P, Maisack, M, Staubert, R, Doebereiner, S, Englhauser, J, Pietsch, W, Reppin, C, and Truemper, J

Subjects
Space Radiation
Abstract

The X ray pulsars Vela X-1 (4U 0900-40) and A0535+26) were observed with the High Energy X ray Experiment (HEXE) onboard the Mir space station at energies above 20 keV. The pulse profiles of Vela X-1 (P = 283.22 s for JD 244 7486) and A0535+26 (P = 103.27 s for JD 244 7626) were measured up to at least 100 keV. The time averaged pulse profiles of the two sources both show a clear double peak structure with an asymmetric main pulse and a more symmetric secondary pulse. The spectrum of the main pulse is significantly harder than that of the secondary. Pulse phase resolved spectra show absorption features at 54 keV and possibly 27 keV for Vela X-1 and around 100 keV for A0535+26. If these features are interpreted as second and first harmonic (fundamental) cyclotron absorption lines, lower limits are derived of 2.6 x 10(exp 12) and 4.3 x 10(exp 12) Gauss for the magnetic fields of the neutron stars in Vela X-1 and A0535+26, respectively.

Published
1992

21. X ray radiation from Supernova 1987A. The results of the Kvant module in 1987-1989

Author

Sunyaev, Rashid A, Kaniovsky, A. S, Efremov, V. V, Grebenev, S. A, Kuznetsov, A. V, Churasov, E, Gilfanov, M, Yamburenko, N, Englhauser, J, and Doebereiner, S

Subjects
Astrophysics
Abstract

The results of two years of SN1987A hard X-ray observations by the HEXE instrument aboard the Kvant module are summarized. By May to June 1989, the hard x-ray flux had declined more than 8.5 times in comparison with the maximum of the x-ray light curve. The upper limit of the ratio of Co-57/Co-56 abundances at the level of ratio of Fe-57/Fe-56 abundances at the Earth is a factor of 1.5.

Published
1991

22. Search for Solar Axions: CAST

Author

Lakić, Biljana, Andriamonje, S., Aune, S., Autiero, D., Avignone, F., Barth, K., Belov, A., Beltrán, B., Bräuninger, H., Carmona, J.M., Cebrián, S., Chesi, E., Collar, J.I., Creswick, R., Dafni, T., Davenport, M., Di Lella, L., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Farach, H., Ferrer, E., Fischer, H., Franz, J., Friedrich, P., Geralis, T., Giomataris, I., Gninenko, S., Goloubev, N., Hartmann, R., Hasinoff, M.D., Heinsius, F.H., Hoffmann, D.H.H., Irastorza, I.G., Jacoby, J., Kang, D., Königsmann, K., Kotthaus, R., Krčmar, Milica, Kousouris, K., Kuster, M., Lasseur, C., Liolios, A., Ljubičić, Ante, Lutz, G., Luzón, G., Miller, D.W, Morales, A., Morales, J., Ortiz, A., Papaevangelou, T., Placci, A., Raffelt, G., Ruz, J., Riege, H., Sarsa, M.L., Savvidis, I., Serpico, P., Semertzidis, Y., Stewart, L., Vieira, J.D., Villar, J., Walckiers, L., Zachariadou, K., and Zioutas, K.

Subjects
Physics::Instrumentation and Detectors, Physics, High Energy Physics::Phenomenology, solar axions, axion-photon coupling
Abstract

The CERN Axion Solar Telescope (CAST) is searching for axions produced in the Sun´s core by the Primakoff process. CAST is using a decommissioned Large Hadron Collider (LHC) test magnet where axions could be converted back into X-rays with energies up to 10 keV. Analysis of the 2003 data showed no signal above background implying an upper limit for the axion-photon coupling constant g_(a gamma) < 1.16 × 10^(-10) GeV^(-1) at 95% C.L. for m_a < = 0.02 eV [1]. The higher quality 2004 data is presently under analysis. CAST Phase II is scheduled to start in late 2005. This will be the first step in extending CAST´s sensitivity to axion rest masses up to 1 eV.

Published
2007

23. Results on axion physics from the CAST Experiment at CERN

Author

Eleftheriadis, Christos, Andriamonje, Samuel A, Aune, S, Barth, K, Belov, A, Beltran, B, Bräuninger, H, Carmona, J, Cebrián, S, Collar, J I, Dafni, T, Davenport, M, Di Lella, L, Englhauser, J, Fanourakis, G K, Ferrer-Ribas, E, Fischer, H, Franz, J, Friedrich, P, Geralis, T, Giomataris, Ioanis, Gninenko, S, Gomez, H, Hasinoff, M, Heinsius, F H, Hoffmann, D H H, Irastorza, I G, Jacoby, J, Jakovcic, K, Kang, D, Königsmann, K C, Kotthaus, R, Krcmar, M, Kousouris, K, Kuster, M, Laki, B, Lasseur, C, Liolios, A, Ljubicic, cA, Lutz, G, Luzón, G, Miller, D, Morales, A, Morales, J, Nordt, A, Ortiz, A, Papaevangelou, T, Placci, A, Raffelt, G, Riege1, H, Rodríguez, A, Ruz, J, Savvidis, I, Semertzidis, Y K, Serpico, Pasquale Dario, Stewart, L, Villar, J, Vogel, J, Walckiers, L, and Zioutas, K

Subjects
High Energy Physics::Theory, High Energy Physics - Experiment (hep-ex), Physics::Instrumentation and Detectors, High Energy Physics::Phenomenology, FOS: Physical sciences, Particle Physics - Experiment, High Energy Physics - Experiment
Abstract

Axions are expected to be produced in the sun via the Primakoff process. They may be detected through the inverse process in the laboratory, under the influence of a strong magnetic field, giving rise to X-rays of energies in the range of a few keV. Such an Axion detector is the CERN Axion Solar Telescope (CAST), collecting data since 2003. Results have been published, pushing the axion-photon coupling g$_{a\gamma}$ below the 10$^{-10}$ GeV$^{-1}$ limit at 95% CL, for axion masses less than 0.02 eV. This limit is nearly an order of magnitude lower than previous experimental limits and surpassed for the first time limits set from astrophysical arguments based on the energy-loss concept. The experiment is currently exploring axion masses in the range of 0.02 eV $< m_a, Comment: 13 pages, 5 figures, presented in the conference "Les Rencontres de Physique de la Vallee d'Aoste, La Thuile, 4 - 10 March 2007, Italy"

Published
2007
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24. First results from the CAST experiment

Author

Dafni, T., Andriamonje, S., Aune, S., Autiero, D., Avignone, F., Barth, K., Belov, A., Beltrán, B., Bräuninger, H., Carmona, J.M., Cebrián, S., Chesi, E., Collar, J., Davenport, M., Di Lella, L., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Farach, H., Ferrer, E., Fischer, H., Franz, J., Friedrich, P., Geralis, T., Giomataris, I., Gninenko, S., Goloubev, N., Hasinoff, M., Heinsius, F.H., Hoffmann, D.H.H., Irastorza, I.G., Jacoby, J., Kang, D., Königsmann, K., Kotthaus, R., Krčmar, Milica, Kousouris, K., Kuster, M., Lakić, Biljana, Lasseur, C., Liolios, A., Ljubičić, Ante, Lutz, G., Luzón, G., Miller, D., Morales, A., Morales, J., Ortiz, A., Papaevangelou, T., Placci, A., Raffelt, G., Ruz, J., Riege, H., Sarsa, M.L., Savvidis, I., Semertzidis, Y., Serber, W., Serpico, P., Stewart, L., Vieira, J., Villar, J., Walckiers, L., and Zioutas, K.

Subjects
Physics::Instrumentation and Detectors, High Energy Physics::Phenomenology, axions, axion-photon coupling
Abstract

The CAST Experiment commenced its first phase of solar axion-searching in 2003, and ran successfully for two years. In the transverse field of a decommissioned Large Hadron Collider (LHC) test magnet (9.26m, 9T), the CERN Axion Solar Telescope intends to transform axions -that would be produced in the sun- into X-rays with energies of a few keV. The first results from the analysis of the data taken in 2003 show no signature of axions, implying an upper limit to the axion-photon coupling g(a gamma) < 1.16 × 10-10 GeV-1 at 95% C.L. for ma < 0.02 eV, already a factor 100 better than previous searches. In Phase I the twin bores of the magnet were kept in vacuum. In Phase II (due to start in November 2005) the bores of the magnet will be filled with a buffer gas, which will allow CAST to explore the region of higher axion masses.

Published
2006

25. Search for solar axions: the CAST experiment at CERN

Author

Beltran, Berta, Andriamonje, S., Arsov, V., Aune, S., Autiero, D., Avignone, F., Barth, K., Belov, A., Brauninger, H., Carmona, J. M., Cebrian, S., Chesi, E., Collar, J. I., Creswick, R., Dafni, T., Davenport, M., Di Lella, L., Eleftheriadis, C., Englhauser, J., Fanourakis, G., Farach, H., Ferrer, E., Fischer, H., Franz, J., Friedrich, P., Geralis, T., Giomataris, I., Gninenko, S., Goloubev, N., Hartmann, R., Hasinoff, M. D., Fritz-Herbert Heinsius, Hoffmann, D. H. H., Irastorza, I. G., Jacoby, J., Kang, D., Konigsmann, Kay, Kotthaus, R., Krcmar, M., Kousouris, K., Kuster, M., Lakic, B., Lasseur, C., Liolios, A., Ljubicic, A., Lutz, G., Luzon, G., Miller, David Wilkins, Morales, A., Morales, J., Mutterer, M., Nikolaidis, A., Ortiz, A., Papaevangelou, T., Placci, A., Raffelt, G., Ruz, J., Riege, H., Sarsa, M. L., Savvidis, I., Serber, W., Serpico, P., Semertzidis, Y., Stewart, L., Vieira, J. D., Villar, J., Walckiers, L., Zachariadou, K., Zioutas, K., Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Girod, Dominique

Subjects
[PHYS.ASTR.SR] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Physics::Instrumentation and Detectors, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics::Phenomenology, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], solar axions, dark matter, low background, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Particle Physics - Experiment, ComputingMilieux_MISCELLANEOUS
Abstract

Hypothetical axion-like particles with a two-photon interaction would be produced in the sun by the Primakoff process. In a laboratory magnetic field they would be transformed into X-rays with energies of a few keV. The CAST experiment at CERN is using a decommissioned LHC magnet as an axion helioscope in order to search for these axion-like particles. The analysis of the 2003 data has shown no signal above the background, thus implying an upper limit to the axion-photon coupling < 1.16*10^{-10} GeV^{-1} at 95% CL for m_{a}

Published
2005

27. CAST constraints on the axion-electron coupling

Author

Barth, K, primary, Belov, A, additional, Beltran, B, additional, Bräuninger, H, additional, Carmona, J.M, additional, Collar, J.I, additional, Dafni, T, additional, Davenport, M, additional, Lella, L. Di, additional, Eleftheriadis, C, additional, Englhauser, J, additional, Fanourakis, G, additional, Ferrer-Ribas, E, additional, Fischer, H, additional, Franz, J, additional, Friedrich, P, additional, Galán, J, additional, García, J.A, additional, Geralis, T, additional, Giomataris, I, additional, Gninenko, S, additional, Gómez, H, additional, Hasinoff, M.D, additional, Heinsius, F.H, additional, Hoffmann, D.H.H, additional, Irastorza, I.G, additional, Jacoby, J, additional, Jakovčić, K, additional, Kang, D, additional, Königsmann, K, additional, Kotthaus, R, additional, Kousouris, K, additional, Krčmar, M, additional, Kuster, M, additional, Lakić, B, additional, Liolios, A, additional, Ljubičić, A, additional, Lutz, G, additional, Luzón, G, additional, Miller, D.W, additional, Papaevangelou, T, additional, Pivovaroff, M.J, additional, Raffelt, G, additional, Redondo, J, additional, Riege, H, additional, Rodríguez, A, additional, Ruz, J, additional, Savvidis, I, additional, Semertzidis, Y, additional, Stewart, L, additional, Bibber, K. Van, additional, Vieira, J.D, additional, Villar, J.A, additional, Vogel, J.K, additional, Walckiers, L, additional, and Zioutas, K, additional

Published
2013
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28. Discovery of x-ray and extreme ultraviolet emission from comet C/Hyakutake 1996 B2

Author

Lisse, Cm M., Dennerl, K., Marshall, Fe E., Englhauser, J., Mumma, Mj J., Harden, M., Petre, R., Schmitt, J., Pye, Jp P., Ricketts, Mj J., Trümper, J., and West, Rg G.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

During its close approach to Earth, comet C/Hyakutake 1996 B2 was observed at extreme ultraviolet and x-ray wavelengths with the Rœntgen X-ray Satellite and Rossi X-ray Timing Explorer. The emission morphology was symmetric with respect to a vector from the comet's nucleus toward the sun, but not symmetric around the direction of motion of the comet with respect to interplanetary dust. A slowly varying emission and a large impulsive event that varied on time scales of 1 to 2 hours were observed. An interaction between the comet and the solar wind/solar magnetic field seems to be the most likely mechanism for the observed emission.

Published
1996

29. Search for solar axion emission from7Li and D(p, γ)3He nuclear decays with the CAST γ-ray calorimeter

Author

collaboration, CAST, primary, Andriamonje, S, additional, Aune, S, additional, Autiero, D, additional, Barth, K, additional, Belov, A, additional, Beltrán, B, additional, Bräuninger, H, additional, Carmona, J.M, additional, Cebrián, S, additional, Collar, J.I, additional, Dafni, T, additional, Davenport, M, additional, Lella, L. Di, additional, Eleftheriadis, C, additional, Englhauser, J, additional, Fanourakis, G, additional, Ferrer-Ribas, E, additional, Fischer, H, additional, Franz, J, additional, Friedrich, P, additional, Geralis, T, additional, Giomataris, I, additional, Gninenko, S, additional, Gómez, H, additional, Hasinoff, M, additional, Heinsius, F.H, additional, Hoffmann, D.H.H, additional, Irastorza, I.G, additional, Jacoby, J, additional, Jakovcić, K, additional, Kang, D, additional, Königsmann, K, additional, Kotthaus, R, additional, Krcmar, M, additional, Kousouris, K, additional, Kuster, M, additional, Lakić, B, additional, Lasseur, C, additional, Liolios, A, additional, Ljubicić, A, additional, Lutz, G, additional, Luzón, G, additional, Miller, D.W, additional, Morales, J, additional, Ortiz, A, additional, Papaevangelou, T, additional, Placci, A, additional, Raffelt, G, additional, Riege, H, additional, Rodríguez, A, additional, Ruz, J, additional, Savvidis, I, additional, Semertzidis, Y, additional, Serpico, P, additional, Stewart, L, additional, Vieira, J. D, additional, Villar, J, additional, Vogel, J, additional, Walckiers, L, additional, and Zioutas, K, additional

Published
2010
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30. Search for 14.4 keV solar axions emitted in the M1-transition of57Fe nuclei with CAST

Author

collaboration, CAST, primary, Andriamonje, S, additional, Aune, S, additional, Autiero, D, additional, Barth, K, additional, Belov, A, additional, Beltrán, B, additional, Bräuninger, H, additional, Carmona, J.M, additional, Cebrián, S, additional, Collar, J.I, additional, Dafni, T, additional, Davenport, M, additional, Lella, L. Di, additional, Eleftheriadis, C, additional, Englhauser, J, additional, Fanourakis, G, additional, Ferrer-Ribas, E, additional, Fischer, H, additional, Franz, J, additional, Friedrich, P, additional, Geralis, T, additional, Giomataris, I, additional, Gninenko, S, additional, Gómez, H, additional, Hasinoff, M, additional, Heinsius, F.H, additional, Hoffmann, D.H. H, additional, Irastorza, I.G, additional, Jacoby, J, additional, Jakovčić, K, additional, Kang, D, additional, Königsmann, K, additional, Kotthaus, R, additional, Krcmar, M, additional, Kousouris, K, additional, Kuster, M, additional, Lakić, B, additional, Lasseur, C, additional, Liolios, A, additional, Ljubičić, A, additional, Lutz, G, additional, Luzón, G, additional, Miller, D, additional, Morales, J, additional, Ortiz, A, additional, Papaevangelou, T, additional, Placci, A, additional, Raffelt, G, additional, Riege, H, additional, Rodríguez, A, additional, Ruz, J, additional, Savvidis, I, additional, Semertzidis, Y, additional, Serpico, P, additional, Stewart, L, additional, Vieira, J, additional, Villar, J, additional, Vogel, J, additional, Walckiers, L, additional, and Zioutas, K, additional

Published
2009
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31. Search for Solar Axions: CAST

Author

Lakic, Biljana, primary, Andriamonje, S., additional, Arsov, V., additional, Aune, S., additional, Autiero, D., additional, Avignone, F., additional, Barth, K., additional, Belov, A., additional, Beltran, B., additional, Brauninger, H., additional, Carmona, J. M., additional, Cebrian, S., additional, Chesi, E., additional, Collar, J. I., additional, Creswick, R., additional, Dafni, T., additional, Davenport, M., additional, Di Lella, L., additional, Eleftheriadis, C., additional, Englhauser, J., additional, Fanourakis, G., additional, Farach, H. A., additional, Ferrer, Efrain J., additional, Fischer, H., additional, Franz, J., additional, Friedrich, P., additional, Geralis, T., additional, Giomataris, I., additional, Gninenko, S., additional, Goloubev, N., additional, Hartmann, R., additional, Hasinoff, M. D., additional, Heinsius, F. H., additional, Hoffmann, D. H.H., additional, Irastorza, I. G., additional, Jacoby, J., additional, Kang, D., additional, Konigsmann, K., additional, Kotthaus, R., additional, Krcmar, M., additional, Kousouris, K., additional, Kuster, M., additional, Lasseur, C., additional, Liolios, A., additional, Ljubicic, A., additional, Lutz, G., additional, Luzon, G., additional, Miller, D. W., additional, Morales, A., additional, Morales, J., additional, Ortiz, A., additional, Papaevangelou, T., additional, Placci, A., additional, Raffelt, G., additional, Ruz, J., additional, Riege, H., additional, Sarsa, M. L., additional, Savvidis, I., additional, Serpico, P., additional, Semertzidis, Yannis, additional, Stewart, L., additional, Vieira, J. D., additional, Villar, J., additional, Walckiers, L., additional, Zachariadou, K., additional, and Zioutas, K., additional

Published
2007
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32. An improved limit on the axion–photon coupling from the CAST experiment

Author

Andriamonje, S, primary, Aune, S, additional, Autiero, D, additional, Barth, K, additional, Belov, A, additional, Beltrán, B, additional, Bräuninger, H, additional, Carmona, J M, additional, Cebrián, S, additional, Collar, J I, additional, Dafni, T, additional, Davenport, M, additional, Lella, L Di, additional, Eleftheriadis, C, additional, Englhauser, J, additional, Fanourakis, G, additional, Ribas, E Ferrer, additional, Fischer, H, additional, Franz, J, additional, Friedrich, P, additional, Geralis, T, additional, Giomataris, I, additional, Gninenko, S, additional, Gómez, H, additional, Hasinoff, M, additional, Heinsius, F H, additional, Hoffmann, D H H, additional, Irastorza, I G, additional, Jacoby, J, additional, Jakovčić, K, additional, Kang, D, additional, Königsmann, K, additional, Kotthaus, R, additional, Krčmar, M, additional, Kousouris, K, additional, Kuster, M, additional, Lakić, B, additional, Lasseur, C, additional, Liolios, A, additional, Ljubičić, A, additional, Lutz, G, additional, Luzón, G, additional, Miller, D, additional, Morales, A, additional, Morales, J, additional, Ortiz, A, additional, Papaevangelou, T, additional, Placci, A, additional, Raffelt, G, additional, Riege, H, additional, Rodríguez, A, additional, Ruz, J, additional, Savvidis, I, additional, Semertzidis, Y, additional, Serpico, P, additional, Stewart, L, additional, Vieira, J, additional, Villar, J, additional, Vogel, J, additional, Walckiers, L, additional, Zioutas, K, additional, and Collaboration, CAST, additional

Published
2007
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33. First observation of Mars with XMM-Newton

Author

Dennerl, K., primary, Lisse, C. M., additional, Bhardwaj, A., additional, Burwitz, V., additional, Englhauser, J., additional, Gunell, H., additional, Holmström, M., additional, Jansen, F., additional, Kharchenko, V., additional, and Rodríguez-Pascual, P. M., additional

Published
2006
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34. Search for solar axions: the CAST experiment

Author

Andriamonje, S., primary, Aune, S., additional, Barth, K., additional, Belov, A., additional, Beltrán, B., additional, Bräuninger, H., additional, Carmona, J. M., additional, Cebrián, S., additional, Collar, J. I., additional, Dafni, T., additional, Davenport, M., additional, Di Lella, L., additional, Eleftheriadis, C., additional, Englhauser, J., additional, Fanourakis, G., additional, Ferrer-Ribas, E., additional, Fischer, H., additional, Franz, J., additional, Friedrich, P., additional, Geralis, T., additional, Giomataris, I., additional, Gninenko, S., additional, Hasinoff, M. D., additional, Heinsius, F. H., additional, Hoffmann, D. H. H., additional, Irastorza, I. G., additional, Jacoby, J., additional, Jakovčić, K., additional, Kang, D., additional, Königsmann, K., additional, Kotthaus, R., additional, Krčmar, M., additional, Kousouris, K., additional, Kuster, M., additional, Lakić, B., additional, Lasseur, C., additional, Liolios, A., additional, Ljubičić, A., additional, Lutz, G., additional, Luzón, G., additional, Miller, D. W., additional, Morales, A., additional, Morales, J., additional, Ortiz, A., additional, Papaevangelou, T., additional, Placci, A., additional, Raffelt, G., additional, Ruz, J., additional, Riege, H., additional, Serpico, P., additional, Stewart, L., additional, Vieira, J. D., additional, Villar, J., additional, Vogel, J., additional, Walckiers, L., additional, and Zioutas, K., additional

Published
2006
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35. First Results from the CERN Axion Solar Telescope

Author

Zioutas, K., primary, Andriamonje, S., additional, Arsov, V., additional, Aune, S., additional, Autiero, D., additional, Avignone, F. T., additional, Barth, K., additional, Belov, A., additional, Beltrán, B., additional, Bräuninger, H., additional, Carmona, J. M., additional, Cebrián, S., additional, Chesi, E., additional, Collar, J. I., additional, Creswick, R., additional, Dafni, T., additional, Davenport, M., additional, Di Lella, L., additional, Eleftheriadis, C., additional, Englhauser, J., additional, Fanourakis, G., additional, Farach, H., additional, Ferrer, E., additional, Fischer, H., additional, Franz, J., additional, Friedrich, P., additional, Geralis, T., additional, Giomataris, I., additional, Gninenko, S., additional, Goloubev, N., additional, Hasinoff, M. D., additional, Heinsius, F. H., additional, Hoffmann, D. H. H., additional, Irastorza, I. G., additional, Jacoby, J., additional, Kang, D., additional, Königsmann, K., additional, Kotthaus, R., additional, Krčmar, M., additional, Kousouris, K., additional, Kuster, M., additional, Lakić, B., additional, Lasseur, C., additional, Liolios, A., additional, Ljubičić, A., additional, Lutz, G., additional, Luzón, G., additional, Miller, D. W., additional, Morales, A., additional, Morales, J., additional, Mutterer, M., additional, Nikolaidis, A., additional, Ortiz, A., additional, Papaevangelou, T., additional, Placci, A., additional, Raffelt, G., additional, Ruz, J., additional, Riege, H., additional, Sarsa, M. L., additional, Savvidis, I., additional, Serber, W., additional, Serpico, P., additional, Semertzidis, Y., additional, Stewart, L., additional, Vieira, J. D., additional, Villar, J., additional, Walckiers, L., additional, and Zachariadou, K., additional

Published
2005
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37. FIRST RESULTS FROM THE CERN AXION SOLAR TELESCOPE (CAST).

Author

ANDRIAMONJE, S., ARSO, V., AUNE, S., AUTIERO, D., AVIGNONE, F., BART, K., BELOV, A., BELTRÁN, B., BRÄUNINGER, H., CARMON, J. M., CEBRIAN, S., CHESI, E., COLLAR, J. I ., CRESWICK, R., DAFNI, T., DAVENPORT, M., DI LELLA, L., ELEFTHERIADIS, C., ENGLHAUSER, J., and FANOURAKIS, G.

Subjects
AXIONS, SOLAR telescopes, MAGNETIC fields, LARGE Hadron Collider
Published
2005

39. ROSAT's All-Sky X-Ray View.

Author

Banday, Anthony J., Zaroubi, Saleem, Bartelmann, Matthias, Voges, W., Boller, Th, Englhauser, J., Freyberg, M. J., and Supper, R.

Abstract

This paper deals with the various data products ROSAT has produced during its 8.5 years lifetime. We present the catalogues of sources detected in the ROSAT All-Sky Survey and in the pointed observations and show some highlights of the ROSAT mission and what one can do with respect to mining the sky. [ABSTRACT FROM AUTHOR]

Published
2001
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40. Discovery of X–rays from Venuswith Chandra

Author

Dennerl, K., Burwitz, V., Englhauser, J., Lisse, C., Wolk, S., Dennerl, K., Burwitz, V., Englhauser, J., Lisse, C., and Wolk, S.

Abstract

On January 10 and 13, 2001, Venuswas observed for the first time with an X–ray astronomy satellite. The observation, performed with the ACIS–I and LETG/ACIS–S instruments on Chandra, yielded data of high spatial, spectral, and temporal resolution. Venusis clearly detected as a half–lit crescent, with considerable brightening on the sunward limb. The morphology agrees well with that expected from fluorescent scattering of solar in the planetary atmosphere. The radiation is observed at discrete energies, mainly at the energy of 0.53 keV. Fluorescent radiation is also detected from C–Kαat 0.28 keV and, marginally, from N–Kαat 0.40 keV. An additional emission line is indicated at 0.29 keV, which might be the signature of the C $1{\rm s}\to\pi^{\star}$transition in CO2and CO. Evidence for temporal variability of the X–ray flux was found at the $2.6\,\sigma$level, with fluctuations by factors of a few times indicated on time scales of minutes. All these findings are fully consistent with fluorescent scattering of solar X–rays. No other source of X–ray emission was detected, in particular none from charge exchange interactions between highly charged heavy solar wind ions and atmospheric neutrals, the dominant process for the X–ray emission of comets. This is in agreement with the sensitivity of the observation.

Published
2002
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42. The Hamburg/RASS Catalogue of optical identifications

Author

Bade, N., primary, Engels, D., additional, Voges, W., additional, Beckmann, V., additional, Boller, Th., additional, Cordis, L., additional, Dahlem, M., additional, Englhauser, J., additional, Molthagen, K., additional, Nass, P., additional, Studt, J., additional, and Reimers, D., additional

Published
1998
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43. The Rosat All-Sky Survey Bright Source Catalog

Author

Voges, W., primary, Aschenbach, B., additional, Boller, Th., additional, Bräuninger, H., additional, Briel, U., additional, Burkert, W., additional, Dennerl, K., additional, Englhauser, J., additional, Gruber, R., additional, Haberl, F., additional, Hartner, G., additional, Hasinger, G., additional, Kürster, M., additional, Pfeffermann, E., additional, Pietsch, W., additional, Predehl, P., additional, Rosso, C., additional, Schmitt, J.H.M.M., additional, Trümper, J., additional, and Zimmermann, U., additional

Published
1998
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44. Three hard X-ray transients: GRO J0422+32, GRS 1716-24, GRS 1009-45. Broad band observations by roentgen-MIR-KVANT observatory

Author

Kaniovsky, A.S, primary, Arefiev, V.A, additional, Aleksandrovich, N.L, additional, Borkous, V.V, additional, Borozdin, K.N, additional, Efremov, V.V, additional, Sunyaev, R.A, additional, Kendziorra, E, additional, Kretschmar, P, additional, Kunz, M, additional, Maisack, M, additional, Staubert, R, additional, Doebereiner, S, additional, Englhauser, J, additional, Pietsch, W, additional, Reppin, C, additional, Truemper, J, additional, Skinner, G.K, additional, Willmore, A.P, additional, Brinkman, A.C, additional, Heise, J, additional, and Jager, R, additional

Published
1997
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45. Broad-band X-ray observations of Cir X-1

Author

Maisack, M., primary, Staubert, R., additional, Balucinska-Church, M., additional, Skinner, G., additional, Döbereiner, S., additional, Englhauser, J., additional, Arefev, V.A., additional, Efremov, V.V., additional, and Sunyaev, R.A., additional

Published
1995
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49. The results of the MIR-KVANT in 1987–1989

Author

Sunyaev, R.A., primary, Aref'ev, V., additional, Borozdin, K., additional, Churazov, E.M., additional, Efremov, V., additional, Gilfanov, M.R., additional, Grebenev, S., additional, Kaniovsky, A., additional, Kuznetsov, A.V., additional, Lapshov, I., additional, Yamburenko, N.S., additional, Englhauser, J., additional, Doebereiner, S., additional, Pietsch, W., additional, Reppin, C., additional, Truemper, J., additional, Boer, M., additional, Kendziorra, E., additional, Maisack, M., additional, Mony, B., additional, Staubert, R., additional, Skinner, G.K., additional, Patterson, T.G., additional, Willmore, A.P., additional, Eman, O., additional, Pan, H., additional, Nottingham, M.R., additional, Brinkman, A.C., additional, Heise, J., additional, in't Zand, J.J.M., additional, and Jager, R., additional

Published
1991
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50. Highlights from the KVANT mission

Author

Sunyaev, R.A., primary, Churazov, E., additional, Efremov, V., additional, Gilfanov, M., additional, Grebenev, S., additional, Kaniovsky, A., additional, Stepanov, D., additional, Yunin, S., additional, Kuznetsov, A., additional, Melioransky, A., additional, Yamburenko, N., additional, Kiselev, S., additional, Lapshov, I., additional, Pappe, N., additional, Boyarsky, M., additional, Loznikov, V., additional, Prudkoglyad, A., additional, Terekhov, O., additional, Reppin, C., additional, Pietsch, W., additional, Englhauser, J., additional, Trümper, J., additional, Voges, W., additional, Kendziorra, E., additional, Bezler, M., additional, Staubert, R., additional, Brinkman, A.C., additional, Heise, J., additional, in 't Zand, J.J.M., additional, Jager, R., additional, Skinner, G.K., additional, Al-Emam, O., additional, Patterson, T.G., additional, Willmore, A.P., additional, Smith, A., additional, and Parmar, A., additional

Published
1990
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