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The second generation VLT instrument MUSE: Science drivers and instrument design

P SOC PHOTO-OPT INS 5492 (2004) 1145-1149

Authors:

R Bacon, S Bauer, R Bower, S Cabrit, M Cappellari, M Carollo, FO Combes, R Davies, B Delabre, H Dekker, J Devriendt, S Djidel, M Duchateau, JP Dubois, E Emsellem, P Ferruit, M Franx, G Gilmore, B Guiderdoni, F Henault, N Hubin, B Jungwiert, A Kelz, M Le Louarn, I Lewis, JL Lizon, R Mc Dermid, S Morris, U Laux, O Le Fevre, B Lantz, S Lilly, J Lynn, L Pasquin, A Pecontal, PPD Popovic, A Quirrenbach, R Reiss, M Roth, M Steinmetz, R Stuik, L Wisotzki, T de Zeeuw

Abstract:

The Multi Unit Spectroscopic Explorer (MUSE) is a second generation VLT panoramic integral-field spectrograph operating in the visible wavelength range. MUSE has a field of 1x1 arcmin(2) sampled at 0.20.2 arcsec(2) and is assisted by a ground layer adaptive optics system using four laser guide stars. The simultaneous spectral range is 0.465-0.93 mum, at a resolution of Rsimilar to3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. MUSE has also a high spatial resolution mode with 7.5x7.5 arcsec(2) field of view sampled at 25 milli-arcsec. In this mode MUSE should be able to get diffraction limited data-cube in the 0.6-1 mum wavelength range. Although MUSE design has been optimized for the study of galaxy formation and evolution, it has a wide range of possible applications; e.g. monitoring of outer planets atmosphere, young stellar objects environment, supermassive black holes and active nuclei in nearby galaxies or massive spectroscopic survey of stellar fields.

Towards a Unified Description of the Jet-Accretion Coupling in Stellar and Super Massive Black Holes

Progress of Theoretical and Experimental Physics Oxford University Press (OUP) 155 (2004) 83-86

Authors:

Elena Gallo, Rob Fender, Tom Maccarone, Peter Jonker

Short-Term Radio-X-ray Correlations of Cygnus X-1

(2003)

Authors:

T Gleissner, J Wilms, GG Pooley, MA Nowak, K Pottschmidt, S Markoff, M Klein-Wolt, RP Fender, R Staubert

The K-band Hubble diagram of submillimetre galaxies and hyperluminous galaxies

Monthly Notices of the Royal Astronomical Society 346:4 (2003) L51-L56

Authors:

S Serjeant, D Farrah, J Geach, T Takagi, A Verma, A Kaviani, M Fox

Abstract:

We present the K-baad Hubble diagrams (K-z relations) of submillimetre-selected galaxies and hyperluminous galaxies (HLIRGs). We report the discovery of a remarkably tight K-z relation of HLIRGs, indistinguishable from that of the most luminous radio galaxies. Like radio galaxies, the HLIRG K-z relation at z ∼ 3 is consistent with a passively evolving ∼3L* instantaneous starburst starting from a redshift of z ∼ 10. In contrast, many submillimetre-selected galaxies are ≳2 mag fainter, and the population has a much larger dispersion. We argue that dust obscuration and/or a larger mass range may be responsible for this scatter. The galaxies so far proved to be hyperluminous may have been biased towards higher AGN bolometric contributions than submillimetre-selected galaxies due to the 60-μm selection of some, so the location on the K-z relation may be related to the presence of the most massive active galactic nucleus. Alternatively, a particular host galaxy mass range may be responsible for both extreme star formation and the most massive active nuclei.

Measurement of prompt charm meson production cross sections in p p̄ collisions at √s = 1.96 TeV

Physical Review Letters 91:24 (2003) 241804/7

Authors:

D Acosta, T Affolder, MH Ahn, T Akimoto, MG Albrow, D Ambrose, D Amidei, A Anastassov, K Anikeev, A Annovi, J Antos, M Aoki, G Apollinari, JF Arguin, T Arisawa, A Artikov, T Asakawa, W Ashmanskas, A Attal, F Azfar, P Azzi-Bacchetta, N Bacchetta, H Bachacou, W Badgett, S Bailey, A Barbaro-Galtieri, G Barker, VE Barnes, BA Barnett, S Baroiant, M Barone, G Bauer, F Bedeschi, S Behari, S Belforte, WH Bell, G Bellettini, J Bellinger, D Benjamin, A Beretvas, A Bhatti, M Binkley, D Bisello, M Bishai, RE Blair, C Blocker, K Bloom, B Blumenfeld, A Bocci, A Bodek, G Bolla, A Bolshov, PSL Booth, D Bortoletto, J Boudreau, S Bourov, C Bromberg, M Brozovic, E Brubaker, J Budagov, HS Budd, K Burkett, G Busetto, P Bussey, KL Byrum, S Cabrera, P Calafiura, M Campanelli, M Campbell, A Canepa, D Carlsmith, S Carron, R Carosi, M Casarsa, W Caskey, A Castro, P Catastini, D Cauz, A Cerri, C Cerri, L Cerrito, J Chapman, C Chen, YC Chen, M Chertok, G Chiarelli, G Chlachidze, F Chlebana, K Cho, D Chokheli, ML Chu, JY Chung, WH Chung, YS Chung, CI Ciobanu, MA Ciocci, AG Clark, MN Coca, A Connolly, ME Convery

Abstract:

Differential cross sections dσ/dPT for prompt charm meson production in pp̄ collisions at √s=1.96 TeV were measured. The measured differential cross sections are higher than the theoretical predictions by about 100% at low pT and 50% at high pT. However, they are compatible within uncertainties. The models also underestimate Β meson productions at √s=1.8 TeV by similar factors [2,4,5].