Identifying the progenitors of present-day early-type galaxies in observational surveys: correcting 'progenitor bias' using the Horizon-AGN simulation


G Martin, S Kaviraj, JEG Devriendt, Y Dubois, C Pichon, C Laigle

A Compact Quad-Ridge Orthogonal Mode Transducer with Wide Operational Bandwidth

IEEE Antennas and Wireless Propagation Letters (2018)

AW Pollak, ME Jones

IEEE We present the design and the measured performance of a compact quad-ridge orthomode transducer (OMT) operating in C-band with more than 100% fractional bandwidth. The OMT comprises two sets of identical orthogonal ridges mounted in a circular waveguide. The profile of these ridges was optimised to reduce significantly the transition length, while retaining the wide operational bandwidth of the quad-ridge OMT. In this letter, we show that the optimised compact OMT has better than -15dB return loss with the cross-polarisation well below -40dB in the designated 4.0-8.5GHz band.

Models of gravitational lens candidates from Space Warps CFHTLS


R Kung, P Saha, I Ferreras, E Baeten, J Coles, C Cornen, C Macmillan, P Marshall, A More, L Oswald, A Verma, JK Wilcox

The new galaxy evolution paradigm revealed by the Herschel surveys


S Eales, D Smith, N Bourne, J Loveday, K Rowlands, P van der Werf, S Driver, L Dunne, S Dye, C Furlanetto, RJ Ivison, S Maddox, A Robotham, MWL Smith, EN Taylor, E Valiante, A Wright, P Cigan, G De Zotti, MJ Jarvis, L Marchetti, MJ Michalowski, S Phillipps, S Viaene, C Vlahakis

Gas flows in the circumgalactic medium around simulated high-redshift galaxies


PD Mitchell, J Blaizot, J Devriendt, T Kimm, L Michel-Dansac, J Rosdahl, A Slyz

Electron acceleration by wave turbulence in a magnetized plasma

Nature Physics (2018) 1-5

A Rigby, F Cruz, B Albertazzi, R Bamford, AR Bell, JE Cross, F Fraschetti, P Graham, Y Hara, PM Kozlowski, Y Kuramitsu, DQ Lamb, S Lebedev, JR Marques, F Miniati, T Morita, M Oliver, B Reville, Y Sakawa, S Sarkar, C Spindloe, R Trines, P Tzeferacos, LO Silva, R Bingham, M Koenig, G Gregori

© 2018 The Author(s) Astrophysical shocks are commonly revealed by the non-thermal emission of energetic electrons accelerated in situ 1–3 . Strong shocks are expected to accelerate particles to very high energies 4–6 ; however, they require a source of particles with velocities fast enough to permit multiple shock crossings. While the resulting diffusive shock acceleration 4 process can account for observations, the kinetic physics regulating the continuous injection of non-thermal particles is not well understood. Indeed, this injection problem is particularly acute for electrons, which rely on high-frequency plasma fluctuations to raise them above the thermal pool 7,8 . Here we show, using laboratory laser-produced shock experiments, that, in the presence of a strong magnetic field, significant electron pre-heating is achieved. We demonstrate that the key mechanism in producing these energetic electrons is through the generation of lower-hybrid turbulence via shock-reflected ions. Our experimental results are analogous to many astrophysical systems, including the interaction of a comet with the solar wind 9 , a setting where electron acceleration via lower-hybrid waves is possible.

On the far-infrared metallicity diagnostics: applications to high-redshift galaxies


D Rigopoulou, M Pereira-Santaella, GE Magdis, A Cooray, D Farrah, R Marques-Chaves, I Perez-Fournon, D Riechers

X-ray metrology of an array of active edge pixel sensors for use at synchrotron light sources


R Plackett, K Arndt, D Bortoletto, I Horswell, G Lockwood, I Shipsey, N Tartoni, S Williams

Impact of relativistic effects on cosmological parameter estimation

PHYSICAL REVIEW D 97 (2018) ARTN 023537

CS Lorenz, D Alonso, PG Ferreira

Measurement of Atmospheric Neutrino Oscillations at 6-56 GeV with IceCube DeepCore.

Physical review letters 120 (2018) 071801-

MG Aartsen, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, I Al Samarai, D Altmann, K Andeen, T Anderson, I Ansseau, G Anton, C Argüelles, J Auffenberg, S Axani, H Bagherpour, X Bai, JP Barron, SW Barwick, V Baum, R Bay, JJ Beatty, J Becker Tjus, K-H Becker, S BenZvi, D Berley, E Bernardini, DZ Besson, G Binder, D Bindig, E Blaufuss, S Blot, C Bohm, M Börner, F Bos, D Bose, S Böser, O Botner, J Bourbeau, F Bradascio, J Braun, L Brayeur, M Brenzke, H-P Bretz, S Bron, J Brostean-Kaiser, A Burgman, T Carver, J Casey, M Casier, E Cheung, D Chirkin, A Christov, K Clark, L Classen, S Coenders, GH Collin, JM Conrad, DF Cowen, R Cross, M Day, JPAM de André, C De Clercq, JJ DeLaunay, H Dembinski, S De Ridder, P Desiati, KD de Vries, G de Wasseige, M de With, T DeYoung, JC Díaz-Vélez, V di Lorenzo, H Dujmovic, JP Dumm, M Dunkman, B Eberhardt, T Ehrhardt, B Eichmann, P Eller, PA Evenson, S Fahey, AR Fazely, J Felde, K Filimonov, C Finley, S Flis, A Franckowiak, E Friedman, T Fuchs, TK Gaisser, J Gallagher, L Gerhardt, K Ghorbani, W Giang, T Glauch, T Glüsenkamp, A Goldschmidt, JG Gonzalez, D Grant, Z Griffith, C Haack, A Hallgren, F Halzen, K Hanson, D Hebecker, D Heereman, K Helbing, R Hellauer, S Hickford, J Hignight, GC Hill, KD Hoffman, R Hoffmann, B Hokanson-Fasig, K Hoshina, F Huang, M Huber, K Hultqvist, M Hünnefeld, S In, A Ishihara, E Jacobi, GS Japaridze, M Jeong, K Jero, BJP Jones, P Kalaczynski, W Kang, A Kappes, T Karg, A Karle, U Katz, M Kauer, A Keivani, JL Kelley, A Kheirandish, J Kim, M Kim, T Kintscher, J Kiryluk, T Kittler, SR Klein, G Kohnen, R Koirala, H Kolanoski, L Köpke, C Kopper, S Kopper, JP Koschinsky, DJ Koskinen, M Kowalski, K Krings, M Kroll, G Krückl, J Kunnen, S Kunwar, N Kurahashi, T Kuwabara, A Kyriacou, M Labare, JL Lanfranchi, MJ Larson, F Lauber, D Lennarz, M Lesiak-Bzdak, M Leuermann, QR Liu, L Lu, J Lünemann, W Luszczak, J Madsen, G Maggi, KBM Mahn, S Mancina, R Maruyama, K Mase, R Maunu, F McNally, K Meagher, M Medici, M Meier, T Menne, G Merino, T Meures, S Miarecki, J Micallef, G Momenté, T Montaruli, RW Moore, M Moulai, R Nahnhauer, P Nakarmi, U Naumann, G Neer, H Niederhausen, SC Nowicki, DR Nygren, A Obertacke Pollmann, A Olivas, A O'Murchadha, T Palczewski, H Pandya, DV Pankova, P Peiffer, JA Pepper, C Pérez de Los Heros, D Pieloth, E Pinat, M Plum, PB Price, GT Przybylski, C Raab, L Rädel, M Rameez, K Rawlins, IC Rea, R Reimann, B Relethford, M Relich, E Resconi, W Rhode, M Richman, S Robertson, M Rongen, C Rott, T Ruhe, D Ryckbosch, D Rysewyk, T Sälzer, SE Sanchez Herrera, A Sandrock, J Sandroos, S Sarkar, S Sarkar, K Satalecka, P Schlunder, T Schmidt, A Schneider, S Schoenen, S Schöneberg, L Schumacher, D Seckel, S Seunarine, J Soedingrekso, D Soldin, M Song, GM Spiczak, C Spiering, J Stachurska, M Stamatikos, T Stanev, A Stasik, J Stettner, A Steuer, T Stezelberger, RG Stokstad, A Stößl, NL Strotjohann, GW Sullivan, M Sutherland, I Taboada, J Tatar, F Tenholt, S Ter-Antonyan, A Terliuk, G Tešić, S Tilav, PA Toale, MN Tobin, S Toscano, D Tosi, M Tselengidou, CF Tung, A Turcati, CF Turley, B Ty, E Unger, M Usner, J Vandenbroucke, W Van Driessche, N van Eijndhoven, S Vanheule, J van Santen, M Vehring, E Vogel, M Vraeghe, C Walck, A Wallace, M Wallraff, FD Wandler, N Wandkowsky, A Waza, C Weaver, MJ Weiss, C Wendt, J Werthebach, S Westerhoff, BJ Whelan, K Wiebe, CH Wiebusch, L Wille, DR Williams, L Wills, M Wolf, J Wood, TR Wood, E Woolsey, K Woschnagg, DL Xu, XW Xu, Y Xu, JP Yanez, G Yodh, S Yoshida, T Yuan, M Zoll

We present a measurement of the atmospheric neutrino oscillation parameters using three years of data from the IceCube Neutrino Observatory. The DeepCore infill array in the center of IceCube enables the detection and reconstruction of neutrinos produced by the interaction of cosmic rays in Earth's atmosphere at energies as low as ∼5  GeV. That energy threshold permits measurements of muon neutrino disappearance, over a range of baselines up to the diameter of the Earth, probing the same range of L/E_{ν} as long-baseline experiments but with substantially higher-energy neutrinos. This analysis uses neutrinos from the full sky with reconstructed energies from 5.6 to 56 GeV. We measure Δm_{32}^{2}=2.31_{-0.13}^{+0.11}×10^{-3}  eV^{2} and sin^{2}θ_{23}=0.51_{-0.09}^{+0.07}, assuming normal neutrino mass ordering. These results are consistent with, and of similar precision to, those from accelerator- and reactor-based experiments.

Photometric redshifts for the next generation of deep radio continuum surveys - I. Template fitting


KJ Duncan, MJI Brown, WL Williams, PN Best, V Buat, D Burgarella, MJ Jarvis, K Malek, SJ Oliver, HJA Rottgering, DJB Smith

Galaxy evolution in the metric of the cosmic web


K Kraljic, S Arnouts, C Pichon, C Laigle, S de la Torre, D Vibert, C Cadiou, Y Dubois, M Treyer, C Schimd, S Codis, V de Lapparent, J Devriendt, HS Hwang, D Le Borgne, N Malavasi, B Milliard, M Musso, D Pogosyan, M Alpaslan, J Bland-Hawthorn, AH Wright

The State-of-Play of Anomalous Microwave Emission (AME) research

New Astronomy Reviews 80 (2018) 1-28

C Dickinson, Y Ali-Haïmoud, A Barr, ES Battistelli, A Bell, L Bernstein, S Casassus, K Cleary, BT Draine, R Génova-Santos, SE Harper, B Hensley, J Hill-Valler, T Hoang, FP Israel, L Jew, A Lazarian, JP Leahy, J Leech, CH López-Caraballo, I McDonald, EJ Murphy, T Onaka, R Paladini, MW Peel, Y Perrott, F Poidevin, ACS Readhead, JA Rubiño-Martín, AC Taylor, CT Tibbs, M Todorović, M Vidal

© 2018 Elsevier B.V. Anomalous Microwave Emission (AME) is a component of diffuse Galactic radiation observed at frequencies in the range ≈ 10–60 GHz. AME was first detected in 1996 and recognised as an additional component of emission in 1997. Since then, AME has been observed by a range of experiments and in a variety of environments. AME is spatially correlated with far-IR thermal dust emission but cannot be explained by synchrotron or free–free emission mechanisms, and is far in excess of the emission contributed by thermal dust emission with the power-law opacity consistent with the observed emission at sub-mm wavelengths. Polarization observations have shown that AME is very weakly polarized (≲ 1 %). The most natural explanation for AME is rotational emission from ultra-small dust grains (“spinning dust”), first postulated in 1957. Magnetic dipole radiation from thermal fluctuations in the magnetization of magnetic grain materials may also be contributing to the AME, particularly at higher frequencies (≳ 50 GHz). AME is also an important foreground for Cosmic Microwave Background analyses. This paper presents a review and the current state-of-play in AME research, which was discussed in an AME workshop held at ESTEC, The Netherlands, June 2016.

The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field


CL Hale, MJ Jarvis, I Delvecchio, PW Hatfield, M Novak, V Smolcic, G Zamorani

Improving photometric redshift estimation using GPZ: Size information, post processing, and improved photometry

Monthly Notices of the Royal Astronomical Society 475 (2018) 331-342

Z Gomes, MJ Jarvis, IA Almosallam, SJ Roberts

© 2017 The Author(s). The next generation of large-scale imaging surveys (such as those conducted with the Large Synoptic Survey Telescope and Euclid) will require accurate photometric redshifts in order to optimally extract cosmological information. Gaussian Process for photometric redshift estimation (GPZ) is a promising new method that has been proven to provide efficient, accurate photometric redshift estimations with reliable variance predictions. In this paper,we investigate a number of methods for improving the photometric redshift estimations obtained using GPZ (but which are also applicable to others). We use spectroscopy from the Galaxy and Mass Assembly Data Release 2 with a limiting magnitude of r < 19.4 along with corresponding Sloan Digital Sky Survey visible (ugriz) photometry and the UKIRT Infrared Deep Sky Survey Large Area Survey near-IR (YJHK) photometry. We evaluate the effects of adding near-IR magnitudes and angular size as features for the training, validation, and testing of GPZ and find that these improve the accuracy of the results by ~15-20 per cent. In addition, we explore a post-processing method of shifting the probability distributions of the estimated redshifts based on their Quantile-Quantile plots and find that it improves the bias by ~40 per cent. Finally, we investigate the effects of using more precise photometry obtained from the Hyper Suprime-Cam Subaru Strategic Program Data Release 1 and find that it produces significant improvements in accuracy, similar to the effect of including additional features.

Comparison of Einstein-Boltzmann solvers for testing general relativity

PHYSICAL REVIEW D 97 (2018) ARTN 023520

E Bellini, A Barreira, N Frusciante, B Hu, S Peirone, M Raveri, M Zumalacarregui, A Avilez-Lopez, M Ballardini, RA Battye, B Bolliet, E Calabrese, Y Dirian, PG Ferreira, F Finelli, Z Huang, MM Ivanov, J Lesgourgues, B Li, NA Lima, F Pace, D Paoletti, I Sawicki, A Silvestri, C Skordis, C Umilta, F Vernizzi

General theories of linear gravitational perturbations to a Schwarzschild black hole

PHYSICAL REVIEW D 97 (2018) ARTN 044021

OJ Tattersall, PG Ferreira, M Lagos

Shape of LOSVDs in Barred Disks: Implications for Future IFU Surveys


Z-Y Li, J Shen, M Bureau, Y Zhou, M Du, VP Debattista

Reconstruction of a direction-dependent primordial power spectrum from Planck CMB data


A Durakovic, P Hunt, S Mukherjee, S Sarkar, T Souradeep

Reconstructing the gravitational field of the local Universe


H Desmond, PG Ferreira, G Lavaux, J Jasche