Bayes versus the virial theorem: inferring the potential of a galaxy from a kinematical snapshot

Monthly Notices of the Royal Astronomical Society 437 (2014) 2230-2248

SJ Magorrian

I present a new framework for estimating a galaxy's gravitational potential, Phi, from its stellar kinematics. It adopts a fully non-parametric model for the galaxy's unknown phase-space distribution function, f, that takes full advantage of Jeans' theorem. Given an expression for the joint likelihood of Phi and f, the likelihood of Phi is calculated by using a Dirichlet process mixture to represent the prior on f and marginalising. I demonstrate that modelling machinery constructed using this framework is successful at recovering the potentials of some simple systems given perfect kinematical data, a situation handled effortlessly by traditional moment-based methods, such as the virial theorem, but in which the more modern extended-Schwarzschild method fails. Unlike moment-based methods, however, the models constructed using this framework can easily be generalised to take account of realistic observational errors and selection functions.

Exploring Mbar shock conditions and isochorically heated aluminum at the Matter in Extreme Conditions end station of the Linac Coherent Light Source (invited).

The Review of scientific instruments 85 (2014) 11E702-

LB Fletcher, HJ Lee, B Barbrel, M Gauthier, E Galtier, B Nagler, T Döppner, S LePape, T Ma, A Pak, D Turnbull, T White, G Gregori, M Wei, RW Falcone, P Heimann, U Zastrau, JB Hastings, SH Glenzer

Recent experiments performed at the Matter in Extreme Conditions end station of the Linac Coherent Light Source (LCLS) have demonstrated the first spectrally resolved measurements of plasmons from isochorically heated aluminum. The experiments have been performed using a seeded 8-keV x-ray laser beam as a pump and probe to both volumetrically heat and scatter x-rays from aluminum. Collective x-ray Thomson scattering spectra show a well-resolved plasmon feature that is down-shifted in energy by 19 eV. In addition, Mbar shock pressures from laser-compressed aluminum foils using velocity interferometer system for any reflector have been measured. The combination of experiments fully demonstrates the possibility to perform warm dense matter studies at the LCLS with unprecedented accuracy and precision.

Performance of the K-band multi-object spectrograph (KMOS) on the ESO VLT


R Sharples, R Bender, AA Berbel, R Bennett, N Bezawada, R Castillo, M Cirasuolo, P Clark, G Davidson, R Davies, R Davies, M Dubbeldam, A Fairley, G Finger, NF Schreiber, R Genzel, R Haefner, A Hess, I Jung, I Lewis, D Montgomery, J Murray, B Muschielok, J Pirard, S Ramsey, P Rees, J Richter, D Robertson, I Robson, S Rolt, R Saglia, I Saviane, J Schlichter, L Schmidtobreik, A Segovia, A Smette, M Tecza, S Todd, M Wegner, E Wiezorrek

The diverse formation histories of simulated disc galaxies

Monthly Notices of the Royal Astronomical Society 441 (2014) 3679-3695

M Aumer, SDM White, T Naab

We analyse the formation histories of 19 galaxies from cosmological smoothed particle hydrodynamics zoom-in resimulations. We construct mock three-colour images and show that the models reproduce observed trends in the evolution of galaxy colours and morphologies. However, only a small fraction of galaxies contains bars. Many galaxies go through phases of central mass growth by in situ star formation driven by gas-rich mergers or misaligned gas infall. These events lead to accretion of low angular momentum gas to the centres and leave imprints on the distributions of z = 0 stellar circularities, radii and metallicities as functions of age. Observations of the evolution of structural properties of samples of disc galaxies at z = 2.5-0.0 infer continuous mass assembly at all radii. Our simulations can only explain this if there is a significant contribution from mergers or misaligned infall, as expected in a Λ cold dark matter universe. Quiescent merger histories lead to high kinematic disc fractions and inside-out growth, but show little central growth after the last 'destructive' merger at z > 1.5. For sufficiently strong feedback, as assumed in our models, a moderate amount of merging does not seem to be a problem for the z = 0 disc galaxy population, but may rather be a requirement. The average profiles of simulated disc galaxies agree with observations at z≥1.5. At z≤1, there is too much growth in size and too little growth in centralmass, possibly due to the underabundance of bars. The discrepancies may partly be caused by differences between the star formation histories of the simulations and those assumed for observations. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

An observational and theoretical view of the radial distribution of HI gas in galaxies

Monthly Notices of the Royal Astronomical Society 441 (2014) 2159-2172

J Wang, J Fu, M Aumer, G Kauffmann, GIG Józsa, P Serra, ML Huang, J Brinchmann, T Van Der Hulst, F Bigiel

We analyse the radial distribution of HI gas for 23 disc galaxies with unusually high HI content from the Bluedisk sample, along with a similar-sized sample of 'normal' galaxies. We propose an empirical model to fit the radial profile of the HI surface density, an exponential function with a depression near the centre. The radial HI surface density profiles are very homogeneous in the outer regions of the galaxy; the exponentially declining part of the profile has a scalelength of ~0.18 R1, where R1 is the radius where the column density of the HI is 1 M⊙ pc-2. This holds for all galaxies, independent of their stellar or HI mass. The homogenous outer profiles, combined with the limited range in HI surface density in the nonexponential inner disc, results in the well-known tight relation between HI size and HI mass. By comparing the radial profiles of the HI-rich galaxies with those of the control systems, we deduce that in about half the galaxies, most of the excess gas lies outside the stellar disc, in the exponentially declining outer regions of the HI disc. In the other half, the excess is more centrally peaked. We compare our results with existing smoothed particle hydrodynamical simulations and semi-analytic models of disc galaxy formation in a Λ cold dark matter universe. Both the hydro simulations and the semi-analytic models reproduce the HI surface density profiles and the HI size-mass relation without further tuning of the simulation and model inputs. In the semi-analytic models, the universal shape of the outer HI radial profiles is a consequence of the assumption that infalling gas is always distributed exponentially. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

The ATLAS(3D) project - XXIV. The intrinsic shape distribution of early-type galaxies


A-M Weijmans, PT de Zeeuw, E Emsellem, D Krajnovic, P-Y Lablanche, K Alatalo, L Blitz, M Bois, F Bournaud, M Bureau, M Cappellari, AF Crocker, RL Davies, TA Davis, P-A Duc, S Khochfar, H Kuntschner, RM McDermid, R Morganti, T Naab, T Oosterloo, M Sarzi, N Scott, P Serra, GV Kleijn, LM Young

Focus on high energy density physics

New Journal of Physics 16 (2014)

R Paul Drake, P Norreys

High-energy-density physics concerns the behavior of systems at high pressure, often involving the interplay of plasma, relativistic, quantum mechanical and electromagnetic effects. The field is growing rapidly in its scope of activity thanks to advances in experimental, laser and computational technologies. This 'focus on' collection presents papers discussing forefront research that spans the field, providing a sense of its breadth and of the interlinking of its parts. © 2014 IOP Publishing Ltd and Deutsche Physikalische Gesellschaft.

Do high-redshift quasars have powerful jets?


AC Fabian, SA Walker, A Celotti, G Ghisellini, P Mocz, KM Blundell, RG McMahon

The ATLAS(3D) project - XXV. Two-dimensional kinematic analysis of simulated galaxies and the cosmological origin of fast and slow rotators


T Naab, L Oser, E Emsellem, M Cappellari, D Krajnovic, RM McDermid, K Alatalo, E Bayet, L Blitz, M Bois, F Bournaud, M Bureau, A Crocker, RL Davies, TA Davis, PT de Zeeuw, P-A Duc, M Hirschmann, PH Johansson, S Khochfar, H Kuntschner, R Morganti, T Oosterloo, M Sarzi, N Scott, P Serra, G van de Ven, A Weijmans, LM Young

Non-thermal enhancement of electron–positron pair creation in burning thermonuclear laboratory plasmas

High Energy Density Physics 13 (2014) C

EG Hill, SJ Rose

Optimizing stellarators for large flows


I Calvo, FI Parra, J Arturo Alonso, J Luis Velasco


CHINESE PHYSICS C 38 (2014) ARTN 090001

KA Olive, K Agashe, C Amsler, M Antonelli, J-F Arguin, DM Asner, H Baer, HR Band, RM Barnett, T Basaglia, CW Bauer, JJ Beatty, VI Belousov, J Beringer, G Bernardi, S Bethke, H Bichsel, O Biebel, E Blucher, S Blusk, G Brooijmans, O Buchmueller, V Burkert, MA Bychkov, RN Cahn, M Carena, A Ceccucci, A Cerri, D Chakraborty, M-C Chen, RS Chivukula, K Copic, G Cowan, O Dahl, G D'Ambrosio, T Damour, D de Florian, A de Gouvea, T DeGrand, P de Jong, G Dissertori, BA Dobrescu, M Doser, M Drees, HK Dreiner, DA Edwards, S Eidelman, J Erler, VV Ezhela, W Fetscher, BD Fields, B Foster, A Freitas, TK Gaisser, H Gallagher, L Garren, H-J Gerber, G Gerbier, T Gershon, T Gherghetta, S Golwala, M Goodman, C Grab, AV Gritsan, C Grojean, DE Groom, M Grunewald, A Gurtu, T Gutsche, HE Haber, K Hagiwara, C Hanhart, S Hashimoto, Y Hayato, KG Hayes, M Heffner, B Heltsley, JJ Hernandez-Rey, K Hikasa, A Hoecker, J Holder, A Holtkamp, J Huston, JD Jackson, KF Johnson, T Junk, M Kado, D Karlen, UF Katz, SR Klein, E Klempt, RV Kowalewski, F Krauss, M Kreps, B Krusche, YV Kuyanov, Y Kwon, O Lahav, J Laiho, P Langacker, A Liddle, Z Ligeti, C-J Lin, TM Liss, L Littenberg, KS Lugovsky, SB Lugovsky, F Maltoni, T Mannel, AV Manohar, WJ Marciano, AD Martin, A Masoni, J Matthews, D Milstead, P Molaro, K Moenig, F Moortgat, MJ Mortonson, H Murayama, K Nakamura, M Narain, P Nason, S Navas, M Neubert, P Nevski, Y Nir, L Pape, J Parsons, C Patrignani, JA Peacock, M Pennington, ST Petcov, A Piepke, A Pomarol, A Quadt, S Raby, J Rademacker, G Raffelt, BN Ratcliff, P Richardson, A Ringwald, S Roesler, S Rolli, A Romaniouk, LJ Rosenberg, JL Rosner, G Rybka, CT Achrajda, Y Sakai, GP Salam, S Sarkar, F Sauli, O Schneider, K Scholberg, D Scott, V Sharma, SR Sharpe, M Silari, T Sjostrand, P Skands, JG Smith, GF Smoot, S Spanier, H Spieler, C Spiering, A Stah, T Stanev, SL Stone, T Sumiyoshi, MJ Sphers, F Takahashi, M Tanabashi, J Terning, L Tiator, M Titov, NP Tkachenko, NA Tornqvist, D Tovey, G Valencia, G Venanzoni, MG Vincter, P Vogel, A Vogt, SP Wakely, W Walkowiak, CW Walter, DR Ward, G Weiglein, DH Weinberg, EJ Weinberg, M White, LR Wiencke, CC Woh, L Wofenstein, J Womersley, CL Woody, RL Workman, A Yamamoto, W-M Yao, GP Zeller, OV Zenin, J Zhang, R-Y Zhu, F Zimmermann, PA Zyla, G Harper, VS Lugovsky, P Schaffner, PD Grp



JE Cross, B Reville, G Gregori

The ATLAS(3D) project - XXVII. Cold gas and the colours and ages of early-type galaxies


LM Young, N Scott, P Serra, K Alatalo, E Bayet, L Blitz, M Bois, F Bournaud, M Bureau, AF Crocker, M Cappellari, RL Davies, TA Davis, PT de Zeeuw, P-A Duc, E Emsellem, S Khochfar, D Krajnovic, H Kuntschner, RM McDermid, R Morganti, T Naab, T Oosterloo, M Sarzi, A-M Weijmans

Compact laser accelerators for X-ray phase-contrast imaging

Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372 (2014)

Z Najmudin, S Kneip, MS Bloom, SPD Mangles, O Chekhlov, AE Dangor, A Dopp, K Ertel, SJ Hawkes, J Holloway, CJ Hooker, J Jiang, NC Lopes, H Nakamura, PA Norreys, PP Rajeev, C Russo, MJV Streeter, DR Symes, M Wing

Advances in X-ray imaging techniques have been driven by advances in novel X-ray sources. The latest fourth-generation X-ray sources can boast large photon fluxes at unprecedented brightness. However, the large size of these facilities means that these sources are not available for everyday applications. With advances in laser plasma acceleration, electron beams can now be generated at energies comparable to those used in light sources, but in university-sized laboratories. By making use of the strong transverse focusing of plasma accelerators, bright sources of betatron radiation have been produced. Here, we demonstrate phase-contrast imaging of a biological sample for the first time by radiation generated by GeV electron beams produced by a laser accelerator. The work was performed using a greater than 300TW laser, which allowed the energy of the synchrotron source to be extended to the 10100 keV range. © 2014 The Author(s) Published by the Royal Society. All rights reserved.

Proton-driven plasma wakefield acceleration: a path to the future of high-energy particle physics


R Assmann, R Bingham, T Bohl, C Bracco, B Buttenschoen, A Butterworth, A Caldwell, S Chattopadhyay, S Cipiccia, E Feldbaumer, RA Fonseca, B Goddard, M Gross, O Grulke, E Gschwendtner, J Holloway, C Huang, D Jaroszynski, S Jolly, P Kempkes, N Lopes, K Lotov, J Machacek, SR Mandry, JW McKenzie, M Meddahi, BL Militsyn, N Moschuering, P Muggli, Z Najmudin, TCQ Noakes, PA Norreys, E Oez, A Pardons, A Petrenko, A Pukhov, K Rieger, O Reimann, H Ruhl, E Shaposhnikova, LO Silva, A Sosedkin, R Tarkeshian, RMGN Trines, T Tueckmantel, J Vieira, H Vincke, M Wing, G Xia

Nanosecond Imaging of Shock- and Jet-Like Features


ER Tubman, R Crowston, R Alraddadi, HW Doyle, J Meinecke, JE Cross, R Bolis, D Lamb, P Tzeferacos, D Doria, B Reville, H Ahmed, M Borghesi, G Gregori, NC Woolsey

From cosmic ray source to the galactic pool

Monthly Notices of the Royal Astronomical Society 437 (2014) 2802-2805

KM Schure, AR Bell

The Galactic cosmic ray spectrum is a remarkably straight power law. Our current understanding is that the dominant sources that accelerate cosmic rays up to the knee (3 × 1015 eV) or perhaps even the ankle (3 × 1018 eV), are young Galactic supernova remnants. In theory, however, there are various reasons why the spectrum may be different for different sources, and may not even be a power law if non-linear shock acceleration applies during the most efficient stages of acceleration.We show how the spectrum at the accelerator translates to the spectrum that makes up the escaping cosmic rays that replenish the Galactic pool of cosmic rays. We assume that cosmic ray confinement, and thus escape, is linked to the level of magnetic field amplification, and that the magnetic field is amplified by streaming cosmic rays according to the non-resonant hybrid or resonant instability. When a fixed fraction of the energy is transferred to cosmic rays, it turns out that a source spectrum that is flatter than E-2 will result in an E-2 escape spectrum, whereas a steeper source spectrum will result in an escape spectrum with equal steepening. This alleviates some of the concern that may arise from expected flat or concave cosmic ray spectra associated with non-linear shock modification. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

In-depth Plasma-Wave Heating of Dense Plasma Irradiated by Short Laser Pulses

Physical Review Letters 113 (2014)

M Sherlock, EG Hill, RG Evans, SJ Rose, W Rozmus

HARMONI: the first light integral field spectrograph for the E-ELT


NA Thatte, F Clarke, I Bryson, H Schnetler, M Tecza, RM Bacon, A Remillieux, E Mediavilla, JM Herreros Linares, S Arribas, CJ Evans, DW Lunney, T Fusco, K O'Brien, IA Tosh, DJ Ives, G Finger, R Houghton, RL Davies, JD Lynn, JR Allen, SD Zieleniewski, S Kendrew, V Ferraro-Wood, A Pecontal-Rousset, J Kosmalski, J Richard, A Jarno, AM Gallie, DM Montgomery, D Henry, G Zins, D Freeman, B Garcia-Lorenzo, L Fernando Rodriguez-Ramos, J Sanchez-Capuchino Revuelta, E Hernandez-Suarez, A Bueno-Bueno, JV Gigante-Ripoll, A Garcia, K Dohlen, B Neichel