S. Lumsden - Leeds

S. Lumsden
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S. Lumsden
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Leeds
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Astrophysics of Galaxies (26)
 
Solar and Stellar Astrophysics (14)
 
Astrophysics (8)
 
Physics - Instrumentation and Detectors (6)
 
Nuclear Experiment (4)
 
High Energy Physics - Experiment (4)
 
Instrumentation and Methods for Astrophysics (1)
 
Cosmology and Nongalactic Astrophysics (1)

Publications Authored By S. Lumsden

Until recently, there have been few studies of the protostellar evolution of intermediate-mass (IM) stars, which may bridge the low- and high-mass regimes. This paper aims to investigate whether the properties of an IM protostar within the IRAS 05373+2349 embedded cluster are similar to that of low- and/or high-mass protostars. We carried out Very Large Array as well as Combined Array for Research in Millimeter Astronomy continuum and 12CO(J=1-0) observations, which uncover seven radio continuum sources (VLA 1-7). Read More

We present the results of the application of locally linear embedding (LLE) to reduce the dimensionality of dereddened and continuum subtracted near-infrared spectra using a combination of models and real spectra of massive protostars selected from the Red MSX Source survey database. A brief comparison is also made with two other dimension reduction techniques; Principal Component Analysis (PCA) and Isomap using the same set of spectra as well as a more advanced form of LLE, Hessian locally linear embedding. We find that whilst LLE certainly has its limitations, it significantly outperforms both PCA and Isomap in classification of spectra based on the presence/absence of emission lines and provides a valuable tool for classification and analysis of large spectral data sets. Read More

We present 1.3mm Submillimeter Array (SMA) observations at $\sim$3$^{\prime\prime}$ resolution towards the brightest section of the intermediate/massive star forming cluster NGC 2264-C. The millimetre continuum emission reveals ten 1. Read More

We analyse C$^{18}$O ($J=3-$2) data from a sample of 99 infrared-bright massive young stellar objects (MYSOs) and compact HII regions that were identified as potential molecular-outflow sources in the Red MSX source (RMS) survey. We extract a distance limited (D $<$ 6 kpc) sample shown to be representative of star formation covering the transition between the source types. At the spatial resolution probed, Larson-like relationships are found for these cores, though the alternative explanation, that Larson's relations arise where surface-density-limited samples are considered, is also consistent with our data. Read More

We have observed 99 mid-infrared-bright, massive young stellar objects and compact HII regions drawn from the Red MSX source (RMS) survey in the J=3$-$2 transition of $^{12}$CO and $^{13}$CO, using the James Clerk Maxwell Telescope. 89 targets are within 6 kpc of the Sun, covering a representative range of luminosities and core masses. These constitute a relatively unbiased sample of bipolar molecular outflows associated with massive star formation. Read More

We present early results from the JCMT Plane Survey (JPS), which has surveyed the northern inner Galactic plane between longitudes l=7 and l=63 degrees in the 850-{\mu}m continuum with SCUBA-2, as part of the James Clerk Maxwell Telescope Legacy Survey programme. Data from the l=30 degree survey region, which contains the massive star-forming regions W43 and G29.96, are analysed after approximately 40% of the observations had been completed. Read More

Correlations between the accretion luminosity and emission line luminosities (L_acc and L_line) of pre-main sequence (PMS) stars have been published for many different spectral lines, which are used to estimate accretion rates. Despite the origin of those correlations is unknown, this could be attributed to direct or indirect physical relations between the emission line formation and the accretion mechanism. This work shows that all (near-UV/optical/near-IR) L_acc-L_line correlations are the result of the fact that the accretion luminosity and the stellar luminosity (L_star) are correlated, and are not necessarily related with the physical origin of the line. Read More

2015Jul
Affiliations: 1MPIfR, 2Wartburg College, 3LJMU, 4MPIfR, 5Leeds, 6MPIfR, 7Herts, 8Universite de Strasbourg, 9LJMU

We present the results of ammonia observations towards 66 massive star forming regions identified by the Red MSX source survey. We have used the Green Bank Telescope and the K-band focal plane array to map the ammonia NH3 (1,1) and (2,2) inversion emission at a resolution of 30 arcsec in 8 arcmin regions towards the positions of embedded massive star formation. We have identified a total of 115 distinct clumps, approximately two-thirds of which are associated with an embedded massive young stellar object or compact HII region, while the others are classified as quiescent. Read More

Tomographic imaging techniques using the Coulomb scattering of cosmic-ray muons have been shown previously to successfully identify and characterise low- and high-Z materials within an air matrix using a prototype scintillating-fibre tracker system. Those studies were performed as the first in a series to assess the feasibility of this technology and image reconstruction techniques in characterising the potential high-Z contents of legacy nuclear waste containers for the UK Nuclear Industry. The present work continues the feasibility study and presents the first images reconstructed from experimental data collected using this small-scale prototype system of low- and high-Z materials encapsulated within a concrete-filled stainless-steel container. Read More

2014Jun
Affiliations: 1MPIfR, 2LJMU, 3MPIfR, 4MPIfR, 5ESO, 6Leeds, 7Leeds, 8Leiden, 9Hertfordshire, 10MPIfR, 11Arcetri, 12Universidad de Chile, 13MPIfR, 14MPIfR, 15MPIfR

By matching infrared-selected, massive young stellar objects (MYSOs) and compact HII regions in the RMS survey to massive clumps found in the submillimetre ATLASGAL survey, we have identified ~1000 embedded young massive stars between 280\degr < $\ell$ < 350\degr and 10degr < $\ell$ < 60\degr with |b|<1.5degr. Combined with an existing sample of radio-selected methanol masers and compact HII regions, the result is a catalogue of ~1700 massive stars embedded within ~1300 clumps located across the inner Galaxy, containing three observationally distinct subsamples, methanol-maser, MYSO and HII-region associations, covering the most important tracers of massive star formation, thought to represent key stages of evolution. Read More

The OLYMPUS experiment was designed to measure the ratio between the positron-proton and electron-proton elastic scattering cross sections, with the goal of determining the contribution of two-photon exchange to the elastic cross section. Two-photon exchange might resolve the discrepancy between measurements of the proton form factor ratio, $\mu_p G^p_E/G^p_M$, made using polarization techniques and those made in unpolarized experiments. OLYMPUS operated on the DORIS storage ring at DESY, alternating between 2. Read More

2013Oct
Affiliations: 1MPIfR, 2Wartburg College, 3Liverpool John Moores University, 4Liverpool John Moores University, 5University of Leeds, 6University of Leeds, 7Leiden Observatory, 8University of Hertfordshire, 9University of Leeds

Abridged: We have used the well-selected sample of ~1750 embedded, young, massive stars identified by the RMS survey to investigate the Galactic distribution of recent massive star formation. We describe the various methods used to assign distances extracted from the literature, and solve the distance ambiguities towards ~200 sources located within the Solar circle using archival HI data. These distances are used to calculate bolometric luminosities and estimate the survey completeness (~2x10^4 lsun). Read More

Tomographic imaging techniques using the Coulomb scattering of cosmic-ray muons are increasingly being exploited for the non-destructive assay of shielded containers in a wide range of applications. One such application is the characterisation of legacy nuclear waste materials stored within industrial containers. The design, assembly and performance of a prototype muon tomography system developed for this purpose are detailed in this work. Read More

We present medium resolution ($R\approx5300$) $K$-band integral field spectroscopy of six MYSOs. The targets are selected from the RMS survey, and we used the NIFS on the Gemini North telescope. The data show various spectral line features including Br$\gamma$, CO, H$_2$, and \mbox{He\,{\sc i}}. Read More

Cosmic-ray muons are highly penetrative charged particles that are observed at sea level with a flux of approximately one per square centimetre per minute. They interact with matter primarily through Coulomb scattering, which is exploited in the field of muon tomography to image shielded objects in a wide range of applications. In this paper, simulation studies are presented that assess the feasibility of a scintillating-fibre tracker system for use in the identification and characterisation of nuclear materials stored within industrial legacy waste containers. Read More

2013Aug
Affiliations: 1University of Leeds, Leeds, UK, 2University of Leeds, Leeds, UK, 3Max-Planck-Institut fur Radioastronomie, Bonn, Germany, 4University of Leeds, Leeds, UK, 5Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK, 6Leiden Observatory, Leiden University, Leiden, The Netherlands, 7University of Leeds, Leeds, UK, 8Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK

We present the Red MSX Source (RMS) Survey, the largest statistically selected catalog of young massive protostars and HII regions to date. We outline the construction of the catalog using mid and near infrared color selection, as well as the detailed follow up work at other wavelengths, and at higher spatial resolution in the infrared. We show that within the adopted selection bounds we are more than 90% complete for the massive protostellar population, with a positional accuracy of the exciting source of better than 2 arcseconds. Read More

2013Jul
Affiliations: 1MPIfR, 2Hertfordshire, 3LJMU, 4Leeds, 5Leeds, 6ESO, 7MPIfR, 8MPIfR, 9MPIfR, 10Leeds, 11Universidad Nacional Autonoma de Mexico, 12Arcetri, 13Universidad de Chile, 14LJMU, 15LJMU, 16Marseille

We present a complete sample of molecular clumps containing compact and ultra-compact (UC) HII regions between \ell=10\degr and 60\degr\ and $|b|<1\degr, identified by combining the the ATLASGAL submm and CORNISH radio continuum surveys with visual examination of archival infrared data. Our sample is complete to optically thin, compact and UCHII regions driven by a zero age main sequence star of spectral type B0 or earlier embedded within a 1,000 Msun clump. In total we identify 213 compact and UCHII regions, associated with 170 clumps. Read More

For the final running period of HERA, a recoil detector was installed at the HERMES experiment to improve measurements of hard exclusive processes in charged-lepton nucleon scattering. Here, deeply virtual Compton scattering is of particular interest as this process provides constraints on generalised parton distributions that give access to the total angular momenta of quarks within the nucleon. The HERMES recoil detector was designed to improve the selection of exclusive events by a direct measurement of the four-momentum of the recoiling particle. Read More

2013Jan
Affiliations: 1University of Leeds, 2University of Leeds, 3University of Leeds, 4University of Leeds, 5University of Leeds, 6Max Planck Institute for Radioastronomy, 7Leiden Observatory, 8Liverpool John Moores University, 9Liverpool John Moores University

Near-infrared H- and K-band spectra are presented for 247 objects, selected from the Red MSX Source (RMS) survey as potential young stellar objects (YSOs). 195 (~80%) of the targets are YSOs, of which 131 are massive YSOs (L_BOL > 5x10^3 L_solar), M > 8M_solar. This is the largest spectroscopic study of massive YSOs to date, providing a valuable resource for the study of massive star formation. Read More

Massive stars play an important role in many areas of astrophysics, but numerous details regarding their formation remain unclear. In this paper we present and analyse high resolution (R ~ 30,000) near-infrared 2.3 micron spectra of 20 massive young stellar objects from the RMS database, in the largest such study of CO first overtone bandhead emission to date. Read More

The CORNISH project is the highest resolution radio continuum survey of the Galactic plane to date. It is the 5 GHz radio continuum part of a series of multi-wavelength surveys that focus on the northern GLIMPSE region (10 deg < l < 65 deg), observed by the Spitzer satellite in the mid-infrared. Observations with the Very Large Array in B and BnA configurations have yielded a 1. Read More

We describe the motivation, design and implementation of the CORNISH survey, an arcsecond resolution radio continuum survey of the inner Galactic plane at 5 GHz using the Karl G. Jansky Very Large Array (VLA). It is a blind survey co-ordinated with the northern Spitzer GLIMPSE I region covering 10 deg < l < 65 deg and |b| < 1 deg at similar resolution. Read More

We present a study of the kinematical properties of a small sample of nearby near-infrared bright massive and intermediate mass young stellar objects using emission lines sensitive to discs and winds. We show for the first time that the broad ($\sim500$kms$^{-1}$) symmetric line wings on the HI Brackett series lines are due to Stark broadening or electron scattering, rather than pure Doppler broadening due to high speed motion. The results are consistent with the presence of a very dense circumstellar environment. Read More

Massive stars form whilst they are still embedded in dense envelopes. As a result, the roles of rotation, mass loss and accretion in massive star formation are not well understood. This study evaluates the source of the Q-band, lambda=19. Read More

We present high-resolution HI data obtained using the Australia Telescope Compact Array to resolve the near/far distance ambiguities towards a sample of compact HII regions from the Red MSX Source (RMS) survey. The high resolution data are complemented with lower resolution archival HI data extracted from the Southern and VLA Galactic Plane surveys. We resolve the distance ambiguity for nearly all of the 105 sources where the continuum was strong enough to allow analysis of the HI absorption line structure. Read More

2011Jul
Affiliations: 1CASS, 2Liverpool John Moores, 3Wartburg College, 4Liverpool John Moores, 5Leeds, 6Leeds, 7Leeds, 8Exeter, 9Cambridge, 10Yale

The Red MSX Source (RMS) survey has identified a sample of ~1200 massive young stellar objects (MYSOs), compact and ultra compact HII regions from a sample of ~2000 MSX and 2MASS colour selected sources. We have used the 100 m Green Bank telescope to search for 22-24 GHz water maser and ammonia (1,1), (2,2) and (3,3) emission towards ~600 RMS sources located within the northern Galactic plane. We have identified 308 H2O masers which corresponds to an overall detection rate of ~50%. Read More

There is currently no accepted theoretical framework for the formation of the most massive stars, and the manner in which protostars continue to accrete and grow in mass beyond \sim10Msun is still a controversial topic. In this study we use several prescriptions of stellar accretion and a description of the Galactic gas distribution to simulate the luminosities and spatial distribution of massive protostellar population of the Galaxy. We then compare the observables of each simulation to the results of the Red MSX Source (RMS) survey, a recently compiled database of massive young stellar objects. Read More

We present a determination of the luminosity functions of massive young stellar objects (MYSOs) and compact (C)HII regions within the Milky Way Galaxy using the large, well-selected sample of these sources identified by the Red MSX Source (RMS) survey. The MYSO luminosity function decreases monotonically such that there are few with $L\gtrsim 10^{5}$Lsol, whilst the CHII regions are detected up to ~10$^{6}Lsol. The lifetimes of these phases are also calculated as a function of luminosity by comparison with the luminosity function for local main-sequence OB stars. Read More

We apply mid-infrared spectro-interferometry to the massive young stellar object CRL2136. The observations were performed with the Very Large Telescope Interferometer and the MIDI instrument at a 42m baseline probing angular scales of 50 milli-arcseconds. We model the observed visibilities in parallel with diffraction-limited images at both 24. Read More

Context: The Red MSX Source (RMS) survey is returning a large sample of massive young stellar objects (MYSOs) and ultra-compact (UC) \HII{} regions using follow-up observations of colour-selected candidates from the MSX point source catalogue. Aims: To obtain the bolometric fluxes and, using kinematic distance information, the luminosities for young RMS sources with far-infrared fluxes. Methods: We use a model spectral energy distribution (SED) fitter to obtain the bolometric flux for our sources, given flux data from our work and the literature. Read More

2010Aug
Affiliations: 1CSIRO Astronomy and Space Science, 2Liverpool John Moores University, 3University of Leeds, 4University of Leeds, 5University of Leeds, 6CSIRO Astronomy and Space Science, 7University of Exeter, 8University of Leeds, 9University of Leeds

The Red MSX Source (RMS) survey has identified a large sample of massive young stellar objects (MYSOs) and ultra compact (UC) HII regions from a sample of ~2000 MSX and 2MASS colour selected sources. Using a recent catalogue of molecular clouds derived from the Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey (GRS), and by applying a Galactic scaleheight cut off of 120 pc, we solve the distance ambiguity for RMS sources located within 18\degr < |l| > 54\degr. These two steps yield kinematic distances to 291 sources out of a possible 326 located within the GRS longitude range. Read More

We present high resolution (R~50,000) spectroastrometry over the CO 1st overtone bandhead of a sample of seven intermediate/massive young stellar objects. These are primarily drawn from the red MSX source (RMS) survey, a systematic search for young massive stars which has returned a large, well selected sample of such objects. The mean luminosity of the sample is approximately 5 times 10^4 L_\odot, indicating the objects typically have a mass of ~15 solar masses. Read More

2009Dec
Affiliations: 1University of Leeds, 2University of Leeds, 3University of Leeds, 4University of Leeds

The circumstellar structure on 100 AU scales of the massive young stellar object W33A is probed using the VLTI and the MIDI instrument. N-band visibilities on 4 baselines are presented which are inconsistent with a spherically symmetric geometry. The visibility spectra and SED are simultaneously compared to 2D axi-symmetric dust radiative transfer models with a geometry including a rotationally flattened envelope and outflow cavities. Read More

Context: The Red MSX Source (RMS) survey is a multi-wavelength campaign of follow-up observations of a colour-selected sample of candidate massive young stellar objects (MYSOs) in the galactic plane. This survey is returning the largest well-selected sample of MYSOs to date, while identifying other dust contaminant sources with similar mid-infrared colours including a large number of new ultra-compact (UC)HII regions. Aims:To measure the far-infrared (IR) flux, which lies near the peak of the spectral energy distribution (SED) of MYSOs and UCHII regions, so that, together with distance information, the luminosity of these sources can be obtained. Read More

The Young Stellar Object (YSO) W33A is one of the best known examples of a massive star still in the process of forming. Here we present Gemini North ALTAIR/NIFS laser-guide star adaptive-optics assisted K-band integral-field spectroscopy of W33A and its inner reflection nebula. In our data we make the first detections of a rotationally-flattened outer envelope and fast bi-polar jet of a massive YSO at near-infrared wavelengths. Read More

Context: The Red MSX Source (RMS) survey has identified a large sample of candidate massive young stellar objects (MYSOs) and ultra compact (UC) HII regions from a sample of ~2000 MSX and 2MASS colour selected sources. Aims: To search for H2O masers towards a large sample of young high mass stars and to investigate the statistical correlation of H2O masers with the earliest stages of massive star formation. Methods: We have used the Mopra Radio telescope to make position-switched observations towards ~500 UCHII regions and MYSOs candidates identified from the RMS survey and located between 190\degr < l < 30\degr. Read More

2009Jul
Authors: The PANDA Collaboration, W. Erni1, I. Keshelashvili2, B. Krusche3, M. Steinacher4, Y. Heng5, Z. Liu6, H. Liu7, X. Shen8, O. Wang9, H. Xu10, J. Becker11, F. Feldbauer12, F. -H. Heinsius13, T. Held14, H. Koch15, B. Kopf16, M. Pelizaeus17, T. Schroeder18, M. Steinke19, U. Wiedner20, J. Zhong21, A. Bianconi22, M. Bragadireanu23, D. Pantea24, A. Tudorache25, V. Tudorache26, M. De Napoli27, F. Giacoppo28, G. Raciti29, E. Rapisarda30, C. Sfienti31, E. Bialkowski32, A. Budzanowski33, B. Czech34, M. Kistryn35, S. Kliczewski36, A. Kozela37, P. Kulessa38, K. Pysz39, W. Schaefer40, R. Siudak41, A. Szczurek42, W. Czy. zycki43, M. Domagala44, M. Hawryluk45, E. Lisowski46, F. Lisowski47, L. Wojnar48, D. Gil49, P. Hawranek50, B. Kamys51, St. Kistryn52, K. Korcyl53, W. Krzemien54, A. Magiera55, P. Moskal56, Z. Rudy57, P. Salabura58, J. Smyrski59, A. Wronska60, M. Al-Turany61, I. Augustin62, H. Deppe63, H. Flemming64, J. Gerl65, K. Goetzen66, R. Hohler67, D. Lehmann68, B. Lewandowski69, J. Luehning70, F. Maas71, D. Mishra72, H. Orth73, K. Peters74, T. Saito75, G. Schepers76, C. J. Schmidt77, L. Schmitt78, C. Schwarz79, B. Voss80, P. Wieczorek81, A. Wilms82, K. -T. Brinkmann83, H. Freiesleben84, R. Jaekel85, R. Kliemt86, T. Wuerschig87, H. -G. Zaunick88, V. M. Abazov89, G. Alexeev90, A. Arefiev91, V. I. Astakhov92, M. Yu. Barabanov93, B. V. Batyunya94, Yu. I. Davydov95, V. Kh. Dodokhov96, A. A. Efremov97, A. G. Fedunov98, A. A. Feshchenko99, A. S. Galoyan100, S. Grigoryan101, A. Karmokov102, E. K. Koshurnikov103, V. Ch. Kudaev104, V. I. Lobanov105, Yu. Yu. Lobanov106, A. F. Makarov107, L. V. Malinina108, V. L. Malyshev109, G. A. Mustafaev110, A. Olshevski111, M. A. . Pasyuk112, E. A. Perevalova113, A. A. Piskun114, T. A. Pocheptsov115, G. Pontecorvo116, V. K. Rodionov117, Yu. N. Rogov118, R. A. Salmin119, A. G. Samartsev120, M. G. Sapozhnikov121, A. Shabratova122, G. S. Shabratova123, A. N. Skachkova124, N. B. Skachkov125, E. A. Strokovsky126, M. K. Suleimanov127, R. Sh. Teshev128, V. V. Tokmenin129, V. V. Uzhinsky130, A. S. Vodopianov131, S. A. Zaporozhets132, N. I. Zhuravlev133, A. G. Zorin134, D. Branford135, K. Foehl136, D. Glazier137, D. Watts138, P. Woods139, W. Eyrich140, A. Lehmann141, A. Teufel142, S. Dobbs143, Z. Metreveli144, K. Seth145, B. Tann146, A. Tomaradze147, D. Bettoni148, V. Carassiti149, A. Cecchi150, P. Dalpiaz151, E. Fioravanti152, I. Garzia153, M. Negrini154, M. Savri`e155, G. Stancari156, B. Dulach157, P. Gianotti158, C. Guaraldo159, V. Lucherini160, E. Pace161, A. Bersani162, M. Macri163, M. Marinelli164, R. F. Parodi165, I. Brodski166, W. Doering167, P. Drexler168, M. Dueren169, Z. Gagyi-Palffy170, A. Hayrapetyan171, M. Kotulla172, W. Kuehn173, S. Lange174, M. Liu175, V. Metag176, M. Nanova177, R. Novotny178, C. Salz179, J. Schneider180, P. Schoenmeier181, R. Schubert182, S. Spataro183, H. Stenzel184, C. Strackbein185, M. Thiel186, U. Thoering187, S. Yang188, T. Clarkson189, E. Cowie190, E. Downie191, G. Hill192, M. Hoek193, D. Ireland194, R. Kaiser195, T. Keri196, I. Lehmann197, K. Livingston198, S. Lumsden199, D. MacGregor200, B. McKinnon201, M. Murray202, D. Protopopescu203, G. Rosner204, B. Seitz205, G. Yang206, M. Babai207, A. K. Biegun208, A. Bubak209, E. Guliyev210, V. S. Jothi211, M. Kavatsyuk212, H. Loehner213, J. Messchendorp214, H. Smit215, J. C. van der Weele216, F. Garcia217, D. -O. Riska218, M. Buescher219, R. Dosdall220, R. Dzhygadlo221, A. Gillitzer222, D. Grunwald223, V. Jha224, G. Kemmerling225, H. Kleines226, A. Lehrach227, R. Maier228, M. Mertens229, H. Ohm230, D. Prasuhn231, T. Randriamalala232, J. Ritman233, M. Roeder234, T. Stockmanns235, P. Wintz236, P. Wuestner237, J. Kisiel238, S. Li239, Z. Li240, Z. Sun241, H. Xu242, S. Fissum243, K. Hansen244, L. Isaksson245, M. Lundin246, B. Schroeder247, P. Achenbach248, M. C. Mora Espi249, J. Pochodzalla250, S. Sanchez251, A. Sanchez-Lorente252, V. I. Dormenev253, A. A. Fedorov254, M. V. Korzhik255, O. V. Missevitch256, V. Balanutsa257, V. Chernetsky258, A. Demekhin259, A. Dolgolenko260, P. Fedorets261, A. Gerasimov262, V. Goryachev263, A. Boukharov264, O. Malyshev265, I. Marishev266, A. Semenov267, C. Hoeppner268, B. Ketzer269, I. Konorov270, A. Mann271, S. Neubert272, S. Paul273, Q. Weitzel274, A. Khoukaz275, T. Rausmann276, A. Taeschner277, J. Wessels278, R. Varma279, E. Baldin280, K. Kotov281, S. Peleganchuk282, Yu. Tikhonov283, J. Boucher284, T. Hennino285, R. Kunne286, S. Ong287, J. Pouthas288, B. Ramstein289, P. Rosier290, M. Sudol291, J. Van de Wiele292, T. Zerguerras293, K. Dmowski294, R. Korzeniewski295, D. Przemyslaw296, B. Slowinski297, G. Boca298, A. Braghieri299, S. Costanza300, A. Fontana301, P. Genova302, L. Lavezzi303, P. Montagna304, A. Rotondi305, N. I. Belikov306, A. M. Davidenko307, A. A. Derevschikov308, Y. M. Goncharenko309, V. N. Grishin310, V. A. Kachanov311, D. A. Konstantinov312, V. A. Kormilitsin313, V. I. Kravtsov314, Y. A. Matulenko315, Y. M. Melnik316, A. P. Meschanin317, N. G. Minaev318, V. V. Mochalov319, D. A. Morozov320, L. V. Nogach321, S. B. Nurushev322, A. V. Ryazantsev323, P. A. Semenov324, L. F. Soloviev325, A. V. Uzunian326, A. N. Vasiliev327, A. E. Yakutin328, T. Baeck329, B. Cederwall330, C. Bargholtz331, L. Geren332, P. E. Tegner333, S. Belostotski334, G. Gavrilov335, A. Itzotov336, A. Kisselev337, P. Kravchenko338, S. Manaenkov339, O. Miklukho340, Y. Naryshkin341, D. Veretennikov342, V. Vikhrov343, A. Zhadanov344, L. Fava345, D. Panzieri346, D. Alberto347, A. Amoroso348, E. Botta349, T. Bressani350, S. Bufalino351, M. P. Bussa352, L. Busso353, F. De Mori354, M. Destefanis355, L. Ferrero356, A. Grasso357, M. Greco358, T. Kugathasan359, M. Maggiora360, S. Marcello361, G. Serbanut362, S. Sosio363, R. Bertini364, D. Calvo365, S. Coli366, P. De Remigis367, A. Feliciello368, A. Filippi369, G. Giraudo370, G. Mazza371, A. Rivetti372, K. Szymanska373, F. Tosello374, R. Wheadon375, O. Morra376, M. Agnello377, F. Iazzi378, K. Szymanska379, R. Birsa380, F. Bradamante381, A. Bressan382, A. Martin383, H. Clement384, C. Ekstroem385, H. Calen386, S. Grape387, B. Hoeistad388, T. Johansson389, A. Kupsc390, P. Marciniewski391, E. Thome392, J. Zlomanczuk393, J. Diaz394, A. Ortiz395, S. Borsuk396, A. Chlopik397, Z. Guzik398, J. Kopec399, T. Kozlowski400, D. Melnychuk401, M. Plominski402, J. Szewinski403, K. Traczyk404, B. Zwieglinski405, P. Buehler406, A. Gruber407, P. Kienle408, J. Marton409, E. Widmann410, J. Zmeskal411
Affiliations: 1Basel U, 2Basel U, 3Basel U, 4Basel U, 5Beijing, Inst. High Energy Phys, 6Beijing, Inst. High Energy Phys, 7Beijing, Inst. High Energy Phys, 8Beijing, Inst. High Energy Phys, 9Beijing, Inst. High Energy Phys, 10Beijing, Inst. High Energy Phys, 11Ruhr U., Bochum, 12Ruhr U., Bochum, 13Ruhr U., Bochum, 14Ruhr U., Bochum, 15Ruhr U., Bochum, 16Ruhr U., Bochum, 17Ruhr U., Bochum, 18Ruhr U., Bochum, 19Ruhr U., Bochum, 20Ruhr U., Bochum, 21Ruhr U., Bochum, 22Brescia U, 23Bukarest-Magurele U, 24Bukarest-Magurele U, 25Bukarest-Magurele U, 26Bukarest-Magurele U, 27Catania U. & INFN, Catania, 28Catania U. & INFN, Catania, 29Catania U. & INFN, Catania, 30Catania U. & INFN, Catania, 31Catania U. & INFN, Catania, 32Cracow, INP, 33Cracow, INP, 34Cracow, INP, 35Cracow, INP, 36Cracow, INP, 37Cracow, INP, 38Cracow, INP, 39Cracow, INP, 40Cracow, INP, 41Cracow, INP, 42Cracow, INP, 43Cracow Tech. U, 44Cracow Tech. U, 45Cracow Tech. U, 46Cracow Tech. U, 47Cracow Tech. U, 48Cracow Tech. U, 49Jagiellonian U, 50Jagiellonian U, 51Jagiellonian U, 52Jagiellonian U, 53Jagiellonian U, 54Jagiellonian U, 55Jagiellonian U, 56Jagiellonian U, 57Jagiellonian U, 58Jagiellonian U, 59Jagiellonian U, 60Jagiellonian U, 61Darmstadt, GSI, 62Darmstadt, GSI, 63Darmstadt, GSI, 64Darmstadt, GSI, 65Darmstadt, GSI, 66Darmstadt, GSI, 67Darmstadt, GSI, 68Darmstadt, GSI, 69Darmstadt, GSI, 70Darmstadt, GSI, 71Darmstadt, GSI, 72Darmstadt, GSI, 73Darmstadt, GSI, 74Darmstadt, GSI, 75Darmstadt, GSI, 76Darmstadt, GSI, 77Darmstadt, GSI, 78Darmstadt, GSI, 79Darmstadt, GSI, 80Darmstadt, GSI, 81Darmstadt, GSI, 82Darmstadt, GSI, 83Dresden, Tech. U, 84Dresden, Tech. U, 85Dresden, Tech. U, 86Dresden, Tech. U, 87Dresden, Tech. U, 88Dresden, Tech. U, 89Dubna, JINR, 90Dubna, JINR, 91Dubna, JINR, 92Dubna, JINR, 93Dubna, JINR, 94Dubna, JINR, 95Dubna, JINR, 96Dubna, JINR, 97Dubna, JINR, 98Dubna, JINR, 99Dubna, JINR, 100Dubna, JINR, 101Dubna, JINR, 102Dubna, JINR, 103Dubna, JINR, 104Dubna, JINR, 105Dubna, JINR, 106Dubna, JINR, 107Dubna, JINR, 108Dubna, JINR, 109Dubna, JINR, 110Dubna, JINR, 111Dubna, JINR, 112Dubna, JINR, 113Dubna, JINR, 114Dubna, JINR, 115Dubna, JINR, 116Dubna, JINR, 117Dubna, JINR, 118Dubna, JINR, 119Dubna, JINR, 120Dubna, JINR, 121Dubna, JINR, 122Dubna, JINR, 123Dubna, JINR, 124Dubna, JINR, 125Dubna, JINR, 126Dubna, JINR, 127Dubna, JINR, 128Dubna, JINR, 129Dubna, JINR, 130Dubna, JINR, 131Dubna, JINR, 132Dubna, JINR, 133Dubna, JINR, 134Dubna, JINR, 135Edinburgh U, 136Edinburgh U, 137Edinburgh U, 138Edinburgh U, 139Edinburgh U, 140Erlangen - Nuremberg U, 141Erlangen - Nuremberg U, 142Erlangen - Nuremberg U, 143Northwestern U, 144Northwestern U, 145Northwestern U, 146Northwestern U, 147Northwestern U, 148Ferrara U. & INFN, Ferrara, 149Ferrara U. & INFN, Ferrara, 150Ferrara U. & INFN, Ferrara, 151Ferrara U. & INFN, Ferrara, 152Ferrara U. & INFN, Ferrara, 153Ferrara U. & INFN, Ferrara, 154Ferrara U. & INFN, Ferrara, 155Ferrara U. & INFN, Ferrara, 156Ferrara U. & INFN, Ferrara, 157Frascati, 158Frascati, 159Frascati, 160Frascati, 161Frascati, 162INFN, Genoa, 163INFN, Genoa, 164INFN, Genoa, 165INFN, Genoa, 166Giessen U, 167Giessen U, 168Giessen U, 169Giessen U, 170Giessen U, 171Giessen U, 172Giessen U, 173Giessen U, 174Giessen U, 175Giessen U, 176Giessen U, 177Giessen U, 178Giessen U, 179Giessen U, 180Giessen U, 181Giessen U, 182Giessen U, 183Giessen U, 184Giessen U, 185Giessen U, 186Giessen U, 187Giessen U, 188Giessen U, 189Glasgow U, 190Glasgow U, 191Glasgow U, 192Glasgow U, 193Glasgow U, 194Glasgow U, 195Glasgow U, 196Glasgow U, 197Glasgow U, 198Glasgow U, 199Glasgow U, 200Glasgow U, 201Glasgow U, 202Glasgow U, 203Glasgow U, 204Glasgow U, 205Glasgow U, 206Glasgow U, 207Groningen, KVI, 208Groningen, KVI, 209Groningen, KVI, 210Groningen, KVI, 211Groningen, KVI, 212Groningen, KVI, 213Groningen, KVI, 214Groningen, KVI, 215Groningen, KVI, 216Groningen, KVI, 217Helsinki U, 218Helsinki U, 219Julich, Forschungszentrum, 220Julich, Forschungszentrum, 221Julich, Forschungszentrum, 222Julich, Forschungszentrum, 223Julich, Forschungszentrum, 224Julich, Forschungszentrum, 225Julich, Forschungszentrum, 226Julich, Forschungszentrum, 227Julich, Forschungszentrum, 228Julich, Forschungszentrum, 229Julich, Forschungszentrum, 230Julich, Forschungszentrum, 231Julich, Forschungszentrum, 232Julich, Forschungszentrum, 233Julich, Forschungszentrum, 234Julich, Forschungszentrum, 235Julich, Forschungszentrum, 236Julich, Forschungszentrum, 237Julich, Forschungszentrum, 238Silesia U, 239Lanzhou, Inst. Modern Phys, 240Lanzhou, Inst. Modern Phys, 241Lanzhou, Inst. Modern Phys, 242Beijing, Inst. High Energy Phys, 243Lund U, 244Lund U, 245Lund U, 246Lund U, 247Lund U, 248Mainz U., Inst. Phys, 249Mainz U., Inst. Phys, 250Mainz U., Inst. Phys, 251Mainz U., Inst. Phys, 252Mainz U., Inst. Phys, 253Belarus State U, 254Belarus State U, 255Belarus State U, 256Belarus State U, 257Moscow, ITEP, 258Moscow, ITEP, 259Moscow, ITEP, 260Moscow, ITEP, 261Moscow, ITEP, 262Moscow, ITEP, 263Moscow, ITEP, 264Moscow Power Engineering Institute, 265Moscow Power Engineering Institute, 266Moscow Power Engineering Institute, 267Moscow Power Engineering Institute, 268Munich, Tech. U, 269Munich, Tech. U, 270Munich, Tech. U, 271Munich, Tech. U, 272Munich, Tech. U, 273Munich, Tech. U, 274Munich, Tech. U, 275Munster U., ITP, 276Munster U., ITP, 277Munster U., ITP, 278Munster U., ITP, 279Indian Inst. Tech., Mumbai, 280Novosibirsk, IYF, 281Novosibirsk, IYF, 282Novosibirsk, IYF, 283Novosibirsk, IYF, 284Orsay, IPN, 285Orsay, IPN, 286Orsay, IPN, 287Orsay, IPN, 288Orsay, IPN, 289Orsay, IPN, 290Orsay, IPN, 291Orsay, IPN, 292Orsay, IPN, 293Orsay, IPN, 294Otwock-Swierk, Inst. Atomic Energy, 295Otwock-Swierk, Inst. Atomic Energy, 296Otwock-Swierk, Inst. Atomic Energy, 297Otwock-Swierk, Inst. Atomic Energy, 298Pavia U. & INFN, Pavia, 299Pavia U. & INFN, Pavia, 300Pavia U. & INFN, Pavia, 301Pavia U. & INFN, Pavia, 302Pavia U. & INFN, Pavia, 303Pavia U. & INFN, Pavia, 304Pavia U. & INFN, Pavia, 305Pavia U. & INFN, Pavia, 306Serpukhov, IHEP, 307Serpukhov, IHEP, 308Serpukhov, IHEP, 309Serpukhov, IHEP, 310Serpukhov, IHEP, 311Serpukhov, IHEP, 312Serpukhov, IHEP, 313Serpukhov, IHEP, 314Serpukhov, IHEP, 315Serpukhov, IHEP, 316Serpukhov, IHEP, 317Serpukhov, IHEP, 318Serpukhov, IHEP, 319Serpukhov, IHEP, 320Serpukhov, IHEP, 321Serpukhov, IHEP, 322Serpukhov, IHEP, 323Serpukhov, IHEP, 324Serpukhov, IHEP, 325Serpukhov, IHEP, 326Serpukhov, IHEP, 327Serpukhov, IHEP, 328Serpukhov, IHEP, 329Royal Inst. Tech., Stockholm, 330Royal Inst. Tech., Stockholm, 331Stockholm U, 332Stockholm U, 333Stockholm U, 334St. Petersburg, INP, 335St. Petersburg, INP, 336St. Petersburg, INP, 337St. Petersburg, INP, 338St. Petersburg, INP, 339St. Petersburg, INP, 340St. Petersburg, INP, 341St. Petersburg, INP, 342St. Petersburg, INP, 343St. Petersburg, INP, 344St. Petersburg, INP, 345Piemonte Orientale U., Alessandria, 346Piemonte Orientale U., Alessandria, 347Turin U, 348Turin U, 349Turin U, 350Turin U, 351Turin U, 352Turin U, 353Turin U, 354Turin U, 355Turin U, 356Turin U, 357Turin U, 358Turin U, 359Turin U, 360Turin U, 361Turin U, 362Turin U, 363Turin U, 364INFN, Turin, 365INFN, Turin, 366INFN, Turin, 367INFN, Turin, 368INFN, Turin, 369INFN, Turin, 370INFN, Turin, 371INFN, Turin, 372INFN, Turin, 373INFN, Turin, 374INFN, Turin, 375INFN, Turin, 376INAF-IFSI Turin, 377Turin Polytechnic, 378Turin Polytechnic, 379INFN, Turin, 380Trieste U. & INFN, Trieste, 381Trieste U. & INFN, Trieste, 382Trieste U. & INFN, Trieste, 383Trieste U. & INFN, Trieste, 384Tubingen U, 385TSL Uppsala, 386Uppsala U, 387Uppsala U, 388Uppsala U, 389Uppsala U, 390Uppsala U, 391Uppsala U, 392Uppsala U, 393Uppsala U, 394Valencia U, 395Valencia U, 396Warsaw, Inst. Nucl. Studies, 397Warsaw, Inst. Nucl. Studies, 398Warsaw, Inst. Nucl. Studies, 399Warsaw, Inst. Nucl. Studies, 400Warsaw, Inst. Nucl. Studies, 401Warsaw, Inst. Nucl. Studies, 402Warsaw, Inst. Nucl. Studies, 403Warsaw, Inst. Nucl. Studies, 404Warsaw, Inst. Nucl. Studies, 405Warsaw, Inst. Nucl. Studies, 406Vienna, OAW, 407Vienna, OAW, 408Vienna, OAW, 409Vienna, OAW, 410Vienna, OAW, 411Vienna, OAW

This document is the Technical Design Report covering the two large spectrometer magnets of the PANDA detector set-up. It shows the conceptual design of the magnets and their anticipated performance. It precedes the tender and procurement of the magnets and, hence, is subject to possible modifications arising during this process. Read More

2009May
Affiliations: 1Leeds, ATNF, 2Leeds, 3Jodrell Bank, 4Leeds, 5Leeds, 6Liverpool John Moores, 7Leeds, 8Leeds, Exeter, 9Leeds

(Abridged) Context: The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, well-selected sample of massive young stellar objects (MYSOs). We have identified $\sim$2000 MYSO candidates located throughout the Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. Aims: To identify the populations of UCHII regions and PNe within the sample and examine their Galactic distribution. Read More

2009Mar
Authors: PANDA Collaboration, W. Erni1, I. Keshelashvili2, B. Krusche3, M. Steinacher4, Y. Heng5, Z. Liu6, H. Liu7, X. Shen8, O. Wang9, H. Xu10, J. Becker11, F. Feldbauer12, F. -H. Heinsius13, T. Held14, H. Koch15, B. Kopf16, M. Pelizaeus17, T. Schroeder18, M. Steinke19, U. Wiedner20, J. Zhong21, A. Bianconi22, M. Bragadireanu23, D. Pantea24, A. Tudorache25, V. Tudorache26, M. De Napoli27, F. Giacoppo28, G. Raciti29, E. Rapisarda30, C. Sfienti31, E. Bialkowski32, A. Budzanowski33, B. Czech34, M. Kistryn35, S. Kliczewski36, A. Kozela37, P. Kulessa38, K. Pysz39, W. Schaefer40, R. Siudak41, A. Szczurek42, W. Czy. zycki43, M. Domagala44, M. Hawryluk45, E. Lisowski46, F. Lisowski47, L. Wojnar48, D. Gil49, P. Hawranek50, B. Kamys51, St. Kistryn52, K. Korcyl53, W. Krzemien54, A. Magiera55, P. Moskal56, Z. Rudy57, P. Salabura58, J. Smyrski59, A. Wronska60, M. Al-Turany61, I. Augustin62, H. Deppe63, H. Flemming64, J. Gerl65, K. Goetzen66, R. Hohler67, D. Lehmann68, B. Lewandowski69, J. Luehning70, F. Maas71, D. Mishra72, H. Orth73, K. Peters74, T. Saito75, G. Schepers76, C. J. Schmidt77, L. Schmitt78, C. Schwarz79, B. Voss80, P. Wieczorek81, A. Wilms82, K. -T. Brinkmann83, H. Freiesleben84, R. Jaekel85, R. Kliemt86, T. Wuerschig87, H. -G. Zaunick88, V. M. Abazov89, G. Alexeev90, A. Arefiev91, V. I. Astakhov92, M. Yu. Barabanov93, B. V. Batyunya94, Yu. I. Davydov95, V. Kh. Dodokhov96, A. A. Efremov97, A. G. Fedunov98, A. A. Feshchenko99, A. S. Galoyan100, S. Grigoryan101, A. Karmokov102, E. K. Koshurnikov103, V. Ch. Kudaev104, V. I. Lobanov105, Yu. Yu. Lobanov106, A. F. Makarov107, L. V. Malinina108, V. L. Malyshev109, G. A. Mustafaev110, A. Olshevski111, M. A. . Pasyuk112, E. A. Perevalova113, A. A. Piskun114, T. A. Pocheptsov115, G. Pontecorvo116, V. K. Rodionov117, Yu. N. Rogov118, R. A. Salmin119, A. G. Samartsev120, M. G. Sapozhnikov121, A. Shabratova122, G. S. Shabratova123, A. N. Skachkova124, N. B. Skachkov125, E. A. Strokovsky126, M. K. Suleimanov127, R. Sh. Teshev128, V. V. Tokmenin129, V. V. Uzhinsky130, A. S. Vodopianov131, S. A. Zaporozhets132, N. I. Zhuravlev133, A. G. Zorin134, D. Branford135, K. Foehl136, D. Glazier137, D. Watts138, P. Woods139, W. Eyrich140, A. Lehmann141, A. Teufel142, S. Dobbs143, Z. Metreveli144, K. Seth145, B. Tann146, A. Tomaradze147, D. Bettoni148, V. Carassiti149, A. Cecchi150, P. Dalpiaz151, E. Fioravanti152, I. Garzia153, M. Negrini154, M. Savri`e155, G. Stancari156, B. Dulach157, P. Gianotti158, C. Guaraldo159, V. Lucherini160, E. Pace161, A. Bersani162, M. Macri163, M. Marinelli164, R. F. Parodi165, I. Brodski166, W. Doering167, P. Drexler168, M. Dueren169, Z. Gagyi-Palffy170, A. Hayrapetyan171, M. Kotulla172, W. Kuehn173, S. Lange174, M. Liu175, V. Metag176, M. Nanova177, R. Novotny178, C. Salz179, J. Schneider180, P. Schoenmeier181, R. Schubert182, S. Spataro183, H. Stenzel184, C. Strackbein185, M. Thiel186, U. Thoering187, S. Yang188, T. Clarkson189, E. Cowie190, E. Downie191, G. Hill192, M. Hoek193, D. Ireland194, R. Kaiser195, T. Keri196, I. Lehmann197, K. Livingston198, S. Lumsden199, D. MacGregor200, B. McKinnon201, M. Murray202, D. Protopopescu203, G. Rosner204, B. Seitz205, G. Yang206, M. Babai207, A. K. Biegun208, A. Bubak209, E. Guliyev210, V. S. Jothi211, M. Kavatsyuk212, H. Loehner213, J. Messchendorp214, H. Smit215, J. C. van der Weele216, F. Garcia217, D. -O. Riska218, M. Buescher219, R. Dosdall220, R. Dzhygadlo221, A. Gillitzer222, D. Grunwald223, V. Jha224, G. Kemmerling225, H. Kleines226, A. Lehrach227, R. Maier228, M. Mertens229, H. Ohm230, D. Prasuhn231, T. Randriamalala232, J. Ritman233, M. Roeder234, T. Stockmanns235, P. Wintz236, P. Wuestner237, J. Kisiel238, S. Li239, Z. Li240, Z. Sun241, H. Xu242, S. Fissum243, K. Hansen244, L. Isaksson245, M. Lundin246, B. Schroeder247, P. Achenbach248, M. C. Mora Espi249, J. Pochodzalla250, S. Sanchez251, A. Sanchez-Lorente252, V. I. Dormenev253, A. A. Fedorov254, M. V. Korzhik255, O. V. Missevitch256, V. Balanutsa257, V. Chernetsky258, A. Demekhin259, A. Dolgolenko260, P. Fedorets261, A. Gerasimov262, V. Goryachev263, A. Boukharov264, O. Malyshev265, I. Marishev266, A. Semenov267, C. Hoeppner268, B. Ketzer269, I. Konorov270, A. Mann271, S. Neubert272, S. Paul273, Q. Weitzel274, A. Khoukaz275, T. Rausmann276, A. Taeschner277, J. Wessels278, R. Varma279, E. Baldin280, K. Kotov281, S. Peleganchuk282, Yu. Tikhonov283, J. Boucher284, T. Hennino285, R. Kunne286, S. Ong287, J. Pouthas288, B. Ramstein289, P. Rosier290, M. Sudol291, J. Van de Wiele292, T. Zerguerras293, K. Dmowski294, R. Korzeniewski295, D. Przemyslaw296, B. Slowinski297, G. Boca298, A. Braghieri299, S. Costanza300, A. Fontana301, P. Genova302, L. Lavezzi303, P. Montagna304, A. Rotondi305, N. I. Belikov306, A. M. Davidenko307, A. A. Derevschikov308, Y. M. Goncharenko309, V. N. Grishin310, V. A. Kachanov311, D. A. Konstantinov312, V. A. Kormilitsin313, V. I. Kravtsov314, Y. A. Matulenko315, Y. M. Melnik316, A. P. Meschanin317, N. G. Minaev318, V. V. Mochalov319, D. A. Morozov320, L. V. Nogach321, S. B. Nurushev322, A. V. Ryazantsev323, P. A. Semenov324, L. F. Soloviev325, A. V. Uzunian326, A. N. Vasiliev327, A. E. Yakutin328, T. Baeck329, B. Cederwall330, C. Bargholtz331, L. Geren332, P. E. Tegner333, S. Belostotski334, G. Gavrilov335, A. Itzotov336, A. Kisselev337, P. Kravchenko338, S. Manaenkov339, O. Miklukho340, Y. Naryshkin341, D. Veretennikov342, V. Vikhrov343, A. Zhadanov344, L. Fava345, D. Panzieri346, D. Alberto347, A. Amoroso348, E. Botta349, T. Bressani350, S. Bufalino351, M. P. Bussa352, L. Busso353, F. De Mori354, M. Destefanis355, L. Ferrero356, A. Grasso357, M. Greco358, T. Kugathasan359, M. Maggiora360, S. Marcello361, G. Serbanut362, S. Sosio363, R. Bertini364, D. Calvo365, S. Coli366, P. De Remigis367, A. Feliciello368, A. Filippi369, G. Giraudo370, G. Mazza371, A. Rivetti372, K. Szymanska373, F. Tosello374, R. Wheadon375, O. Morra376, M. Agnello377, F. Iazzi378, K. Szymanska379, R. Birsa380, F. Bradamante381, A. Bressan382, A. Martin383, H. Clement384, C. Ekstroem385, H. Calen386, S. Grape387, B. Hoeistad388, T. Johansson389, A. Kupsc390, P. Marciniewski391, E. Thome392, J. Zlomanczuk393, J. Diaz394, A. Ortiz395, S. Borsuk396, A. Chlopik397, Z. Guzik398, J. Kopec399, T. Kozlowski400, D. Melnychuk401, M. Plominski402, J. Szewinski403, K. Traczyk404, B. Zwieglinski405, P. Buehler406, A. Gruber407, P. Kienle408, J. Marton409, E. Widmann410, J. Zmeskal411, M. F. M. Lutz, B. Pire, O. Scholten, R. Timmermans
Affiliations: 1Basel U, 2Basel U, 3Basel U, 4Basel U, 5Beijing, Inst. High Energy Phys, 6Beijing, Inst. High Energy Phys, 7Beijing, Inst. High Energy Phys, 8Beijing, Inst. High Energy Phys, 9Beijing, Inst. High Energy Phys, 10Beijing, Inst. High Energy Phys, 11Ruhr U., Bochum, 12Ruhr U., Bochum, 13Ruhr U., Bochum, 14Ruhr U., Bochum, 15Ruhr U., Bochum, 16Ruhr U., Bochum, 17Ruhr U., Bochum, 18Ruhr U., Bochum, 19Ruhr U., Bochum, 20Ruhr U., Bochum, 21Ruhr U., Bochum, 22Brescia U, 23Bukarest-Magurele U, 24Bukarest-Magurele U, 25Bukarest-Magurele U, 26Bukarest-Magurele U, 27Catania U. & INFN, Catania, 28Catania U. & INFN, Catania, 29Catania U. & INFN, Catania, 30Catania U. & INFN, Catania, 31Catania U. & INFN, Catania, 32Cracow, INP, 33Cracow, INP, 34Cracow, INP, 35Cracow, INP, 36Cracow, INP, 37Cracow, INP, 38Cracow, INP, 39Cracow, INP, 40Cracow, INP, 41Cracow, INP, 42Cracow, INP, 43Cracow Tech. U, 44Cracow Tech. U, 45Cracow Tech. U, 46Cracow Tech. U, 47Cracow Tech. U, 48Cracow Tech. U, 49Jagiellonian U, 50Jagiellonian U, 51Jagiellonian U, 52Jagiellonian U, 53Jagiellonian U, 54Jagiellonian U, 55Jagiellonian U, 56Jagiellonian U, 57Jagiellonian U, 58Jagiellonian U, 59Jagiellonian U, 60Jagiellonian U, 61Darmstadt, GSI, 62Darmstadt, GSI, 63Darmstadt, GSI, 64Darmstadt, GSI, 65Darmstadt, GSI, 66Darmstadt, GSI, 67Darmstadt, GSI, 68Darmstadt, GSI, 69Darmstadt, GSI, 70Darmstadt, GSI, 71Darmstadt, GSI, 72Darmstadt, GSI, 73Darmstadt, GSI, 74Darmstadt, GSI, 75Darmstadt, GSI, 76Darmstadt, GSI, 77Darmstadt, GSI, 78Darmstadt, GSI, 79Darmstadt, GSI, 80Darmstadt, GSI, 81Darmstadt, GSI, 82Darmstadt, GSI, 83Dresden, Tech. U, 84Dresden, Tech. U, 85Dresden, Tech. U, 86Dresden, Tech. U, 87Dresden, Tech. U, 88Dresden, Tech. U, 89Dubna, JINR, 90Dubna, JINR, 91Dubna, JINR, 92Dubna, JINR, 93Dubna, JINR, 94Dubna, JINR, 95Dubna, JINR, 96Dubna, JINR, 97Dubna, JINR, 98Dubna, JINR, 99Dubna, JINR, 100Dubna, JINR, 101Dubna, JINR, 102Dubna, JINR, 103Dubna, JINR, 104Dubna, JINR, 105Dubna, JINR, 106Dubna, JINR, 107Dubna, JINR, 108Dubna, JINR, 109Dubna, JINR, 110Dubna, JINR, 111Dubna, JINR, 112Dubna, JINR, 113Dubna, JINR, 114Dubna, JINR, 115Dubna, JINR, 116Dubna, JINR, 117Dubna, JINR, 118Dubna, JINR, 119Dubna, JINR, 120Dubna, JINR, 121Dubna, JINR, 122Dubna, JINR, 123Dubna, JINR, 124Dubna, JINR, 125Dubna, JINR, 126Dubna, JINR, 127Dubna, JINR, 128Dubna, JINR, 129Dubna, JINR, 130Dubna, JINR, 131Dubna, JINR, 132Dubna, JINR, 133Dubna, JINR, 134Dubna, JINR, 135Edinburgh U, 136Edinburgh U, 137Edinburgh U, 138Edinburgh U, 139Edinburgh U, 140Erlangen - Nuremberg U, 141Erlangen - Nuremberg U, 142Erlangen - Nuremberg U, 143Northwestern U, 144Northwestern U, 145Northwestern U, 146Northwestern U, 147Northwestern U, 148Ferrara U. & INFN, Ferrara, 149Ferrara U. & INFN, Ferrara, 150Ferrara U. & INFN, Ferrara, 151Ferrara U. & INFN, Ferrara, 152Ferrara U. & INFN, Ferrara, 153Ferrara U. & INFN, Ferrara, 154Ferrara U. & INFN, Ferrara, 155Ferrara U. & INFN, Ferrara, 156Ferrara U. & INFN, Ferrara, 157Frascati, 158Frascati, 159Frascati, 160Frascati, 161Frascati, 162INFN, Genoa, 163INFN, Genoa, 164INFN, Genoa, 165INFN, Genoa, 166Giessen U, 167Giessen U, 168Giessen U, 169Giessen U, 170Giessen U, 171Giessen U, 172Giessen U, 173Giessen U, 174Giessen U, 175Giessen U, 176Giessen U, 177Giessen U, 178Giessen U, 179Giessen U, 180Giessen U, 181Giessen U, 182Giessen U, 183Giessen U, 184Giessen U, 185Giessen U, 186Giessen U, 187Giessen U, 188Giessen U, 189Glasgow U, 190Glasgow U, 191Glasgow U, 192Glasgow U, 193Glasgow U, 194Glasgow U, 195Glasgow U, 196Glasgow U, 197Glasgow U, 198Glasgow U, 199Glasgow U, 200Glasgow U, 201Glasgow U, 202Glasgow U, 203Glasgow U, 204Glasgow U, 205Glasgow U, 206Glasgow U, 207Groningen, KVI, 208Groningen, KVI, 209Groningen, KVI, 210Groningen, KVI, 211Groningen, KVI, 212Groningen, KVI, 213Groningen, KVI, 214Groningen, KVI, 215Groningen, KVI, 216Groningen, KVI, 217Helsinki U, 218Helsinki U, 219Julich, Forschungszentrum, 220Julich, Forschungszentrum, 221Julich, Forschungszentrum, 222Julich, Forschungszentrum, 223Julich, Forschungszentrum, 224Julich, Forschungszentrum, 225Julich, Forschungszentrum, 226Julich, Forschungszentrum, 227Julich, Forschungszentrum, 228Julich, Forschungszentrum, 229Julich, Forschungszentrum, 230Julich, Forschungszentrum, 231Julich, Forschungszentrum, 232Julich, Forschungszentrum, 233Julich, Forschungszentrum, 234Julich, Forschungszentrum, 235Julich, Forschungszentrum, 236Julich, Forschungszentrum, 237Julich, Forschungszentrum, 238Silesia U, 239Lanzhou, Inst. Modern Phys, 240Lanzhou, Inst. Modern Phys, 241Lanzhou, Inst. Modern Phys, 242Beijing, Inst. High Energy Phys, 243Lund U, 244Lund U, 245Lund U, 246Lund U, 247Lund U, 248Mainz U., Inst. Phys, 249Mainz U., Inst. Phys, 250Mainz U., Inst. Phys, 251Mainz U., Inst. Phys, 252Mainz U., Inst. Phys, 253Belarus State U, 254Belarus State U, 255Belarus State U, 256Belarus State U, 257Moscow, ITEP, 258Moscow, ITEP, 259Moscow, ITEP, 260Moscow, ITEP, 261Moscow, ITEP, 262Moscow, ITEP, 263Moscow, ITEP, 264Moscow Power Engineering Institute, 265Moscow Power Engineering Institute, 266Moscow Power Engineering Institute, 267Moscow Power Engineering Institute, 268Munich, Tech. U, 269Munich, Tech. U, 270Munich, Tech. U, 271Munich, Tech. U, 272Munich, Tech. U, 273Munich, Tech. U, 274Munich, Tech. U, 275Munster U., ITP, 276Munster U., ITP, 277Munster U., ITP, 278Munster U., ITP, 279Indian Inst. Tech., Mumbai, 280Novosibirsk, IYF, 281Novosibirsk, IYF, 282Novosibirsk, IYF, 283Novosibirsk, IYF, 284Orsay, IPN, 285Orsay, IPN, 286Orsay, IPN, 287Orsay, IPN, 288Orsay, IPN, 289Orsay, IPN, 290Orsay, IPN, 291Orsay, IPN, 292Orsay, IPN, 293Orsay, IPN, 294Otwock-Swierk, Inst. Atomic Energy, 295Otwock-Swierk, Inst. Atomic Energy, 296Otwock-Swierk, Inst. Atomic Energy, 297Otwock-Swierk, Inst. Atomic Energy, 298Pavia U. & INFN, Pavia, 299Pavia U. & INFN, Pavia, 300Pavia U. & INFN, Pavia, 301Pavia U. & INFN, Pavia, 302Pavia U. & INFN, Pavia, 303Pavia U. & INFN, Pavia, 304Pavia U. & INFN, Pavia, 305Pavia U. & INFN, Pavia, 306Serpukhov, IHEP, 307Serpukhov, IHEP, 308Serpukhov, IHEP, 309Serpukhov, IHEP, 310Serpukhov, IHEP, 311Serpukhov, IHEP, 312Serpukhov, IHEP, 313Serpukhov, IHEP, 314Serpukhov, IHEP, 315Serpukhov, IHEP, 316Serpukhov, IHEP, 317Serpukhov, IHEP, 318Serpukhov, IHEP, 319Serpukhov, IHEP, 320Serpukhov, IHEP, 321Serpukhov, IHEP, 322Serpukhov, IHEP, 323Serpukhov, IHEP, 324Serpukhov, IHEP, 325Serpukhov, IHEP, 326Serpukhov, IHEP, 327Serpukhov, IHEP, 328Serpukhov, IHEP, 329Royal Inst. Tech., Stockholm, 330Royal Inst. Tech., Stockholm, 331Stockholm U, 332Stockholm U, 333Stockholm U, 334St. Petersburg, INP, 335St. Petersburg, INP, 336St. Petersburg, INP, 337St. Petersburg, INP, 338St. Petersburg, INP, 339St. Petersburg, INP, 340St. Petersburg, INP, 341St. Petersburg, INP, 342St. Petersburg, INP, 343St. Petersburg, INP, 344St. Petersburg, INP, 345Piemonte Orientale U., Alessandria, 346Piemonte Orientale U., Alessandria, 347Turin U, 348Turin U, 349Turin U, 350Turin U, 351Turin U, 352Turin U, 353Turin U, 354Turin U, 355Turin U, 356Turin U, 357Turin U, 358Turin U, 359Turin U, 360Turin U, 361Turin U, 362Turin U, 363Turin U, 364INFN, Turin, 365INFN, Turin, 366INFN, Turin, 367INFN, Turin, 368INFN, Turin, 369INFN, Turin, 370INFN, Turin, 371INFN, Turin, 372INFN, Turin, 373INFN, Turin, 374INFN, Turin, 375INFN, Turin, 376INAF-IFSI Turin, 377Turin Polytechnic, 378Turin Polytechnic, 379INFN, Turin, 380Trieste U. & INFN, Trieste, 381Trieste U. & INFN, Trieste, 382Trieste U. & INFN, Trieste, 383Trieste U. & INFN, Trieste, 384Tubingen U, 385TSL Uppsala, 386Uppsala U, 387Uppsala U, 388Uppsala U, 389Uppsala U, 390Uppsala U, 391Uppsala U, 392Uppsala U, 393Uppsala U, 394Valencia U, 395Valencia U, 396Warsaw, Inst. Nucl. Studies, 397Warsaw, Inst. Nucl. Studies, 398Warsaw, Inst. Nucl. Studies, 399Warsaw, Inst. Nucl. Studies, 400Warsaw, Inst. Nucl. Studies, 401Warsaw, Inst. Nucl. Studies, 402Warsaw, Inst. Nucl. Studies, 403Warsaw, Inst. Nucl. Studies, 404Warsaw, Inst. Nucl. Studies, 405Warsaw, Inst. Nucl. Studies, 406Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans, 407Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans, 408Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans, 409Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans, 410Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans, 411Vienna, OAW) , M.F.M. Lutz, B. Pire, O. Scholten, R. Timmermans

To study fundamental questions of hadron and nuclear physics in interactions of antiprotons with nucleons and nuclei, the universal PANDA detector will be built. Gluonic excitations, the physics of strange and charm quarks and nucleon structure studies will be performed with unprecedented accuracy thereby allowing high-precision tests of the strong interaction. The proposed PANDA detector is a state-of-the art internal target detector at the HESR at FAIR allowing the detection and identification of neutral and charged particles generated within the relevant angular and energy range. Read More

2008Oct
Authors: PANDA Collaboration, W. Erni1, I. Keshelashvili2, B. Krusche3, M. Steinacher4, Y. Heng5, Z. Liu6, H. Liu7, X. Shen8, O. Wang9, H. Xu10, J. Becker11, F. Feldbauer12, F. -H. Heinsius13, T. Held14, H. Koch15, B. Kopf16, M. Pelizaeus17, T. Schroeder18, M. Steinke19, U. Wiedner20, J. Zhong21, A. Bianconi22, M. Bragadireanu23, D. Pantea24, A. Tudorache25, V. Tudorache26, M. De Napoli27, F. Giacoppo28, G. Raciti29, E. Rapisarda30, C. Sfienti31, E. Bialkowski32, A. Budzanowski33, B. Czech34, M. Kistryn35, S. Kliczewski36, A. Kozela37, P. Kulessa38, K. Pysz39, W. Schaefer40, R. Siudak41, A. Szczurek42, W. Czy. zycki43, M. Domagala44, M. Hawryluk45, E. Lisowski46, F. Lisowski47, L. Wojnar48, D. Gil49, P. Hawranek50, B. Kamys51, St. Kistryn52, K. Korcyl53, W. Krzemien54, A. Magiera55, P. Moskal56, Z. Rudy57, P. Salabura58, J. Smyrski59, A. Wronska60, M. Al-Turany61, I. Augustin62, H. Deppe63, H. Flemming64, J. Gerl65, K. Goetzen66, R. Hohler67, D. Lehmann68, B. Lewandowski69, J. Luehning70, F. Maas71, D. Mishra72, H. Orth73, K. Peters74, T. Saito75, G. Schepers76, C. J. Schmidt77, L. Schmitt78, C. Schwarz79, B. Voss80, P. Wieczorek81, A. Wilms82, K. -T. Brinkmann83, H. Freiesleben84, R. Jaekel85, R. Kliemt86, T. Wuerschig87, H. -G. Zaunick88, V. M. Abazov89, G. Alexeev90, A. Arefiev91, V. I. Astakhov92, M. Yu. Barabanov93, B. V. Batyunya94, Yu. I. Davydov95, V. Kh. Dodokhov96, A. A. Efremov97, A. G. Fedunov98, A. A. Feshchenko99, A. S. Galoyan100, S. Grigoryan101, A. Karmokov102, E. K. Koshurnikov103, V. Ch. Kudaev104, V. I. Lobanov105, Yu. Yu. Lobanov106, A. F. Makarov107, L. V. Malinina108, V. L. Malyshev109, G. A. Mustafaev110, A. Olshevski111, M. A. . Pasyuk112, E. A. Perevalova113, A. A. Piskun114, T. A. Pocheptsov115, G. Pontecorvo116, V. K. Rodionov117, Yu. N. Rogov118, R. A. Salmin119, A. G. Samartsev120, M. G. Sapozhnikov121, A. Shabratova122, G. S. Shabratova123, A. N. Skachkova124, N. B. Skachkov125, E. A. Strokovsky126, M. K. Suleimanov127, R. Sh. Teshev128, V. V. Tokmenin129, V. V. Uzhinsky130, A. S. Vodopianov131, S. A. Zaporozhets132, N. I. Zhuravlev133, A. G. Zorin134, D. Branford135, K. Foehl136, D. Glazier137, D. Watts138, P. Woods139, W. Eyrich140, A. Lehmann141, A. Teufel142, S. Dobbs143, Z. Metreveli144, K. Seth145, B. Tann146, A. Tomaradze147, D. Bettoni148, V. Carassiti149, A. Cecchi150, P. Dalpiaz151, E. Fioravanti152, I. Garzia153, M. Negrini154, M. Savri`e155, G. Stancari156, B. Dulach157, P. Gianotti158, C. Guaraldo159, V. Lucherini160, E. Pace161, A. Bersani162, M. Macri163, M. Marinelli164, R. F. Parodi165, I. Brodski166, W. Doering167, P. Drexler168, M. Dueren169, Z. Gagyi-Palffy170, A. Hayrapetyan171, M. Kotulla172, W. Kuehn173, S. Lange174, M. Liu175, V. Metag176, M. Nanova177, R. Novotny178, C. Salz179, J. Schneider180, P. Schoenmeier181, R. Schubert182, S. Spataro183, H. Stenzel184, C. Strackbein185, M. Thiel186, U. Thoering187, S. Yang188, T. Clarkson189, E. Cowie190, E. Downie191, G. Hill192, M. Hoek193, D. Ireland194, R. Kaiser195, T. Keri196, I. Lehmann197, K. Livingston198, S. Lumsden199, D. MacGregor200, B. McKinnon201, M. Murray202, D. Protopopescu203, G. Rosner204, B. Seitz205, G. Yang206, M. Babai207, A. K. Biegun208, A. Bubak209, E. Guliyev210, V. S. Jothi211, M. Kavatsyuk212, H. Loehner213, J. Messchendorp214, H. Smit215, J. C. van der Weele216, F. Garcia217, D. -O. Riska218, M. Buescher219, R. Dosdall220, R. Dzhygadlo221, A. Gillitzer222, D. Grunwald223, V. Jha224, G. Kemmerling225, H. Kleines226, A. Lehrach227, R. Maier228, M. Mertens229, H. Ohm230, D. Prasuhn231, T. Randriamalala232, J. Ritman233, M. Roeder234, T. Stockmanns235, P. Wintz236, P. Wuestner237, J. Kisiel238, S. Li239, Z. Li240, Z. Sun241, H. Xu242, S. Fissum243, K. Hansen244, L. Isaksson245, M. Lundin246, B. Schroeder247, P. Achenbach248, M. C. Mora Espi249, J. Pochodzalla250, S. Sanchez251, A. Sanchez-Lorente252, V. I. Dormenev253, A. A. Fedorov254, M. V. Korzhik255, O. V. Missevitch256, V. Balanutsa257, V. Chernetsky258, A. Demekhin259, A. Dolgolenko260, P. Fedorets261, A. Gerasimov262, V. Goryachev263, A. Boukharov264, O. Malyshev265, I. Marishev266, A. Semenov267, C. Hoeppner268, B. Ketzer269, I. Konorov270, A. Mann271, S. Neubert272, S. Paul273, Q. Weitzel274, A. Khoukaz275, T. Rausmann276, A. Taeschner277, J. Wessels278, R. Varma279, E. Baldin280, K. Kotov281, S. Peleganchuk282, Yu. Tikhonov283, J. Boucher284, T. Hennino285, R. Kunne286, S. Ong287, J. Pouthas288, B. Ramstein289, P. Rosier290, M. Sudol291, J. Van de Wiele292, T. Zerguerras293, K. Dmowski294, R. Korzeniewski295, D. Przemyslaw296, B. Slowinski297, G. Boca298, A. Braghieri299, S. Costanza300, A. Fontana301, P. Genova302, L. Lavezzi303, P. Montagna304, A. Rotondi305, N. I. Belikov306, A. M. Davidenko307, A. A. Derevschikov308, Y. M. Goncharenko309, V. N. Grishin310, V. A. Kachanov311, D. A. Konstantinov312, V. A. Kormilitsin313, V. I. Kravtsov314, Y. A. Matulenko315, Y. M. Melnik316, A. P. Meschanin317, N. G. Minaev318, V. V. Mochalov319, D. A. Morozov320, L. V. Nogach321, S. B. Nurushev322, A. V. Ryazantsev323, P. A. Semenov324, L. F. Soloviev325, A. V. Uzunian326, A. N. Vasiliev327, A. E. Yakutin328, T. Baeck329, B. Cederwall330, C. Bargholtz331, L. Geren332, P. E. Tegner333, S. Belostotski334, G. Gavrilov335, A. Itzotov336, A. Kisselev337, P. Kravchenko338, S. Manaenkov339, O. Miklukho340, Y. Naryshkin341, D. Veretennikov342, V. Vikhrov343, A. Zhadanov344, L. Fava345, D. Panzieri346, D. Alberto347, A. Amoroso348, E. Botta349, T. Bressani350, S. Bufalino351, M. P. Bussa352, L. Busso353, F. De Mori354, M. Destefanis355, L. Ferrero356, A. Grasso357, M. Greco358, T. Kugathasan359, M. Maggiora360, S. Marcello361, G. Serbanut362, S. Sosio363, R. Bertini364, D. Calvo365, S. Coli366, P. De Remigis367, A. Feliciello368, A. Filippi369, G. Giraudo370, G. Mazza371, A. Rivetti372, K. Szymanska373, F. Tosello374, R. Wheadon375, O. Morra376, M. Agnello377, F. Iazzi378, K. Szymanska379, R. Birsa380, F. Bradamante381, A. Bressan382, A. Martin383, H. Clement384, C. Ekstroem385, H. Calen386, S. Grape387, B. Hoeistad388, T. Johansson389, A. Kupsc390, P. Marciniewski391, E. Thome392, J. Zlomanczuk393, J. Diaz394, A. Ortiz395, S. Borsuk396, A. Chlopik397, Z. Guzik398, J. Kopec399, T. Kozlowski400, D. Melnychuk401, M. Plominski402, J. Szewinski403, K. Traczyk404, B. Zwieglinski405, P. Buehler406, A. Gruber407, P. Kienle408, J. Marton409, E. Widmann410, J. Zmeskal411
Affiliations: 1Basel U, 2Basel U, 3Basel U, 4Basel U, 5Beijing, Inst. High Energy Phys, 6Beijing, Inst. High Energy Phys, 7Beijing, Inst. High Energy Phys, 8Beijing, Inst. High Energy Phys, 9Beijing, Inst. High Energy Phys, 10Beijing, Inst. High Energy Phys, 11Ruhr U., Bochum, 12Ruhr U., Bochum, 13Ruhr U., Bochum, 14Ruhr U., Bochum, 15Ruhr U., Bochum, 16Ruhr U., Bochum, 17Ruhr U., Bochum, 18Ruhr U., Bochum, 19Ruhr U., Bochum, 20Ruhr U., Bochum, 21Ruhr U., Bochum, 22Brescia U, 23Bukarest-Magurele U, 24Bukarest-Magurele U, 25Bukarest-Magurele U, 26Bukarest-Magurele U, 27Catania U. & INFN, Catania, 28Catania U. & INFN, Catania, 29Catania U. & INFN, Catania, 30Catania U. & INFN, Catania, 31Catania U. & INFN, Catania, 32Cracow, INP, 33Cracow, INP, 34Cracow, INP, 35Cracow, INP, 36Cracow, INP, 37Cracow, INP, 38Cracow, INP, 39Cracow, INP, 40Cracow, INP, 41Cracow, INP, 42Cracow, INP, 43Cracow Tech. U, 44Cracow Tech. U, 45Cracow Tech. U, 46Cracow Tech. U, 47Cracow Tech. U, 48Cracow Tech. U, 49Jagiellonian U, 50Jagiellonian U, 51Jagiellonian U, 52Jagiellonian U, 53Jagiellonian U, 54Jagiellonian U, 55Jagiellonian U, 56Jagiellonian U, 57Jagiellonian U, 58Jagiellonian U, 59Jagiellonian U, 60Jagiellonian U, 61Darmstadt, GSI, 62Darmstadt, GSI, 63Darmstadt, GSI, 64Darmstadt, GSI, 65Darmstadt, GSI, 66Darmstadt, GSI, 67Darmstadt, GSI, 68Darmstadt, GSI, 69Darmstadt, GSI, 70Darmstadt, GSI, 71Darmstadt, GSI, 72Darmstadt, GSI, 73Darmstadt, GSI, 74Darmstadt, GSI, 75Darmstadt, GSI, 76Darmstadt, GSI, 77Darmstadt, GSI, 78Darmstadt, GSI, 79Darmstadt, GSI, 80Darmstadt, GSI, 81Darmstadt, GSI, 82Darmstadt, GSI, 83Dresden, Tech. U, 84Dresden, Tech. U, 85Dresden, Tech. U, 86Dresden, Tech. U, 87Dresden, Tech. U, 88Dresden, Tech. U, 89Dubna, JINR, 90Dubna, JINR, 91Dubna, JINR, 92Dubna, JINR, 93Dubna, JINR, 94Dubna, JINR, 95Dubna, JINR, 96Dubna, JINR, 97Dubna, JINR, 98Dubna, JINR, 99Dubna, JINR, 100Dubna, JINR, 101Dubna, JINR, 102Dubna, JINR, 103Dubna, JINR, 104Dubna, JINR, 105Dubna, JINR, 106Dubna, JINR, 107Dubna, JINR, 108Dubna, JINR, 109Dubna, JINR, 110Dubna, JINR, 111Dubna, JINR, 112Dubna, JINR, 113Dubna, JINR, 114Dubna, JINR, 115Dubna, JINR, 116Dubna, JINR, 117Dubna, JINR, 118Dubna, JINR, 119Dubna, JINR, 120Dubna, JINR, 121Dubna, JINR, 122Dubna, JINR, 123Dubna, JINR, 124Dubna, JINR, 125Dubna, JINR, 126Dubna, JINR, 127Dubna, JINR, 128Dubna, JINR, 129Dubna, JINR, 130Dubna, JINR, 131Dubna, JINR, 132Dubna, JINR, 133Dubna, JINR, 134Dubna, JINR, 135Edinburgh U, 136Edinburgh U, 137Edinburgh U, 138Edinburgh U, 139Edinburgh U, 140Erlangen - Nuremberg U, 141Erlangen - Nuremberg U, 142Erlangen - Nuremberg U, 143Northwestern U, 144Northwestern U, 145Northwestern U, 146Northwestern U, 147Northwestern U, 148Ferrara U. & INFN, Ferrara, 149Ferrara U. & INFN, Ferrara, 150Ferrara U. & INFN, Ferrara, 151Ferrara U. & INFN, Ferrara, 152Ferrara U. & INFN, Ferrara, 153Ferrara U. & INFN, Ferrara, 154Ferrara U. & INFN, Ferrara, 155Ferrara U. & INFN, Ferrara, 156Ferrara U. & INFN, Ferrara, 157Frascati, 158Frascati, 159Frascati, 160Frascati, 161Frascati, 162INFN, Genoa, 163INFN, Genoa, 164INFN, Genoa, 165INFN, Genoa, 166Giessen U, 167Giessen U, 168Giessen U, 169Giessen U, 170Giessen U, 171Giessen U, 172Giessen U, 173Giessen U, 174Giessen U, 175Giessen U, 176Giessen U, 177Giessen U, 178Giessen U, 179Giessen U, 180Giessen U, 181Giessen U, 182Giessen U, 183Giessen U, 184Giessen U, 185Giessen U, 186Giessen U, 187Giessen U, 188Giessen U, 189Glasgow U, 190Glasgow U, 191Glasgow U, 192Glasgow U, 193Glasgow U, 194Glasgow U, 195Glasgow U, 196Glasgow U, 197Glasgow U, 198Glasgow U, 199Glasgow U, 200Glasgow U, 201Glasgow U, 202Glasgow U, 203Glasgow U, 204Glasgow U, 205Glasgow U, 206Glasgow U, 207Groningen, KVI, 208Groningen, KVI, 209Groningen, KVI, 210Groningen, KVI, 211Groningen, KVI, 212Groningen, KVI, 213Groningen, KVI, 214Groningen, KVI, 215Groningen, KVI, 216Groningen, KVI, 217Helsinki U, 218Helsinki U, 219Julich, Forschungszentrum, 220Julich, Forschungszentrum, 221Julich, Forschungszentrum, 222Julich, Forschungszentrum, 223Julich, Forschungszentrum, 224Julich, Forschungszentrum, 225Julich, Forschungszentrum, 226Julich, Forschungszentrum, 227Julich, Forschungszentrum, 228Julich, Forschungszentrum, 229Julich, Forschungszentrum, 230Julich, Forschungszentrum, 231Julich, Forschungszentrum, 232Julich, Forschungszentrum, 233Julich, Forschungszentrum, 234Julich, Forschungszentrum, 235Julich, Forschungszentrum, 236Julich, Forschungszentrum, 237Julich, Forschungszentrum, 238Silesia U, 239Lanzhou, Inst. Modern Phys, 240Lanzhou, Inst. Modern Phys, 241Lanzhou, Inst. Modern Phys, 242Beijing, Inst. High Energy Phys, 243Lund U, 244Lund U, 245Lund U, 246Lund U, 247Lund U, 248Mainz U., Inst. Phys, 249Mainz U., Inst. Phys, 250Mainz U., Inst. Phys, 251Mainz U., Inst. Phys, 252Mainz U., Inst. Phys, 253Belarus State U, 254Belarus State U, 255Belarus State U, 256Belarus State U, 257Moscow, ITEP, 258Moscow, ITEP, 259Moscow, ITEP, 260Moscow, ITEP, 261Moscow, ITEP, 262Moscow, ITEP, 263Moscow, ITEP, 264Moscow Power Engineering Institute, 265Moscow Power Engineering Institute, 266Moscow Power Engineering Institute, 267Moscow Power Engineering Institute, 268Munich, Tech. U, 269Munich, Tech. U, 270Munich, Tech. U, 271Munich, Tech. U, 272Munich, Tech. U, 273Munich, Tech. U, 274Munich, Tech. U, 275Munster U., ITP, 276Munster U., ITP, 277Munster U., ITP, 278Munster U., ITP, 279Indian Inst. 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This document presents the technical layout and the envisaged performance of the Electromagnetic Calorimeter (EMC) for the PANDA target spectrometer. The EMC has been designed to meet the physics goals of the PANDA experiment, which is being developed for the Facility for Antiproton and Ion Research (FAIR) at Darmstadt, Germany. The performance figures are based on extensive prototype tests and radiation hardness studies. Read More

2008Jun
Affiliations: 1University of Leeds, 2University of Leeds, 3University of Leeds, 4University of Leeds, 5University of Leeds, 6, Liverpool John Moores University, 7University of British Columbia, 8University of New South Wales, 9University of New South Wales, 10École Normale Supérieure, 11Purple Mountain Observatory, 12Purple Mountain Observatory
Category: Astrophysics

Context: The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects. Aims: A critical part of our follow-up programme is to conduct 13CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will allow us to identify and remove nearby low-mass YSOs and help in identifying evolved stars which are weak CO emitters. Read More

2007Nov
Affiliations: 1University of Leeds), 2University of Leeds), 3University of Leeds), 4University of Leeds), 5Liverpool John Moores University
Category: Astrophysics

Here we describe the Red MSX Source (RMS) survey which is the largest, systematic, galaxy-wide search for massive young stellar objects (MYSOs) yet undertaken. Mid-IR bright point sources from the MSX satellite survey have been followed-up with ground-based radio, millimetre, and infrared observations to identify the contaminating sources and characterise the MYSOs and UCHII regions. With the initial classification now complete the distribution of sources in the galaxy will be discussed, as well as some programmes being developed to exploit our sample. Read More

Abridged abstract: The Red MSX Source (RMS) survey is an ongoing effort to return a large, well-selected sample of massive young stellar objects (MYSOs) within our Galaxy. A series of ground-based follow-up observations are being undertaken in order to remove contaminant objects from our list of 2000 candidates, and to begin characterising these MYSOs. As a part of these follow-up observations, high resolution (~1") mid-IR imaging aids the identification of contaminant objects which are resolved (UCHII regions, PN) as opposed to those which are unresolved (YSOs, evolved stars) as well as identifying YSOs near UCHII regions and other multiple sources. Read More

Abridged: The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, well-selected sample of massive young stellar objects (MYSOs). Here we present 13CO observations made towards 854 MYSOs candidates located in the 3rd and 4th quadrants. We detected 13CO emission towards a total of 751 of the 854 RMS sources observed (~88%). Read More

We have surveyed a ~0.9-square-degree area of the W3 giant molecular cloud and star-forming region in the 850-micron continuum, using the SCUBA bolometer array on the James Clerk Maxwell Telescope. A complete sample of 316 dense clumps was detected with a mass range from around 13 to 2500 Msun. Read More

The Red MSX Source (RMS) survey is a multi-wavelength programme of follow-up observations designed to distinguish between genuine massive young stellar objects (MYSOs) and other embedded or dusty objects, such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe), from a sample of ~2000 MYSOs candidates. These were identified by comparing the colours of objects from the MSX and 2MASS point source catalogues to those of known MYSOs, in order to develop colour selection criteria which have been used to produced the RMS sample of MYSOs candidates. Our ultimate aim is to produce a large unbiased sample of MYSOs (~500) with complementary multi-wavelength data with which to study their properties. Read More

As part of the Red MSX Source Survey of Massive Young Stellar Objects (MYSOs) we have conducted multi-wavelength follow up observations of the well-known object V645 Cygni. We present our data on this object, whose near-infrared spectrum is exceptional and place these in context with previous observations. Our observations of V645 Cyg included near/mid infrared imaging observations, 13CO 2-1 line observations and high signal-to-noise velocity resolved near-infrared spectroscopy. Read More

The Red MSX Source (RMS) survey is a multi-wavelength program of follow-up observations designed to distinguish between genuine massive young stellar objects (MYSOs) and other embedded or dusty objects, such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe). We have identified nearly 2000 massive YSOs candidates by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. Unfortunately, there are several other types of embedded or dust enshrouded objects that have similar colours as MYSOs and contaminate our sample. Read More