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

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

Construction progress of WEAVE: The next generation wide-field spectroscopy facility for the William Herschel Telescope

Proceedings of SPIE - The International Society for Optical Engineering 10702 (2018)

G Dalton, S Trager, DC Abrams, P Bonifacio, JAL Aguerri, A Vallenari, K Middleton, C Benn, K Dee, F Sayède, I Lewis, J Pragt, S Picó, N Walton, J Rey, C Allende, É Lhomé, D Terrett, M Brock, J Gilbert, A Ridings, M Verheijen, I Tosh, I Steele, R Stuik, G Kroes, N Tromp, J Kragt, D Lesman, C Mottram, S Bates, F Gribbin, JA Burgal, JM Herreros, JM Delgado, C Martin, D Cano, R Navarro, M Irwin, J Lewis, E Gonzales Solares, N O'Mahony, A Bianco, C Zurita, R Ter Horst, E Molinari, M Lodi, J Guerra, A Baruffolo, E Carrasco, S Farkas, E Schallig, V Hill, D Smith, J Drew, B Poggianti, M Pieri, S Jin, L Dominquez Palmero, C Fariña, A Martin, C Worley, D Murphy, A Hidalgo, S Mignot, G Bishop, S Guest, E Elswijk, M De Haan, H Hanenburg, B Salasnich, D Mayya, R Izazaga-Pérez

© 2018 SPIE. We present an update on the overall construction progress of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), now that all the major fabrication contracts are in place. We also present a summary of the current planning behind the 5-year initial phase of survey operations, and some detailed end-to-end science simulations that have been effected to evaluate the final on-sky performance after data processing. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R∼5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R∼20000. The project has experienced some delays in procurement and now has first light expected for the middle of 2019.

MOSAIC: The ELT multi-object spectrograph

Proceedings of SPIE - The International Society for Optical Engineering 10702 (2018)

P Jagourel, E Fitzsimons, F Hammer, F De Frondat, M Puech, CJ Evans, R Sanchez, I Guinouard, F Chemla, M Frotin, Y Yang, P Parr-Burman, T Morris, M Dubbeldam, M Close, K Middleton, G Rousset, Gendron, A Kelz, A Janssen, J Pragt, R Navarro, M Larrieu, K El Hadi, K Dohlen, G Dalton, I Lewis, M Rodrigues, S Morris, L Kaper, B Barbuy, JG Cuby, O Le Fèvre

© 2018 SPIE. Following a successful Phase A study, we introduce the delivered conceptual design of the MOSAIC1 multi-object spectrograph for the ESO Extremely Large Telescope (ELT). MOSAIC will provide R∼5000 spectroscopy over the full 460-1800 nm range, with three additional high-resolution bands (R∼15000) targeting features of particular interest. MOSAIC will combine three operational modes, enabling integrated-light observations of up to 200 sources on the sky (high-multiplex mode) or spectroscopy of 10 spatially-extended fields via deployable integral-field units: MOAO6 assisted high-definition (HDM) and Visible IFUs (VIFU). We will summarise key features of the sub-systems of the design, e.g. the smart tiled focal-plane for target selection and the multi-object adaptive optics used to correct for atmospheric turbulence, and present the next steps toward the construction phase.

Testing process for the WEAVE prime focus corrector lenses for the William Herschel Telescope

Proceedings of SPIE - The International Society for Optical Engineering 10700 (2018)

D Bogunovic, G Jonas, D Cochrane, A Rakich, P Connor, A Romeril, J Romeril, L Gers, E Howick, C Young, T Reed, I Tosh, É Lhomé, KM Dee, G Dalton, S Trager, JAL Aguerri, P Bonifacio, A Vallenari, E Carrasco, DC Abrams, K Middleton

© 2018 SPIE. A new prime focus corrector for the WEAVE project for the William Herschel Telescope is being produced. The corrector consists of six lens elements, the largest being 1.1 m in diameter. It also incorporates an Atmospheric Dispersion Corrector. Testing procedures for the WEAVE prime focus corrector lens elements are described here. Critical issues encountered in practice, including the influence of the lens size, wedge and weight on the testing procedure are discussed. Due to large lens dimensions, a dedicated test tower and lens support system has been developed to measure the optical surface form errors of the concave surfaces and the transmitted wavefront of each lens. For some of the lens elements, sub-aperture measurements have been performed using an off-axis Hindle sphere and the resultant OPD maps have been stitched together. The challenge of testing a wedged lens with a combination of a long radius convex surface and a short radius concave surface has been resolved by using another lens from the system as an auxiliary lens. The practice of testing convex surfaces via internal reflection/transmission through the lens element has been avoided entirely in this case and some discussion justifying the choices of metrology approach taken is given. The fabrication and acceptance testing of the lens elements has been completed within the expected time and budget, and all elements have been shown to meet requirements.

VIRUS: status and performance of the massively-replicated fiber integral field spectrograph for the upgraded Hobby-Eberly Telescope

Proceedings of SPIE - The International Society for Optical Engineering Society of Photo-optical Instrumentation Engineers (2018)

G Hill, G Dalton

The WEAVE prime focus corrector: From design to integration

Proceedings of SPIE - The International Society for Optical Engineering 10706 (2018)

A Tomas, M Canchado, JM Casalta, F Dalmases, O Maroto, C Martin-Nuno, A Romero, JAL Aguerri, JM Herreros, JM Delgado, JA Burgal, DC Abrams, K Dee, E Lhome, G Dalton, K Middleton, P Bonifacio, SC Trager, A Vallenari, E Carrasco

©2018 SPIE. WEAVE is a new wide-field multi-object spectroscopy (MOS) facility proposed for the prime focus of the 4.2m William Herschel Telescope (WHT), situated on the island of La Palma, Canary Islands, Spain. To allow for the compensation of the effects of temperature-induced and gravity-induced image degradation, the WEAVE prime focus assembly will be translated along the telescope optical axis. The assembly comprises the prime focus corrector (PFC), a central mount for the corrector known as FTS[1], an instrument rotator and a twin-focal-plane fibre positioner. SENER, that manufactured and delivered the FTS, is also responsible for the final design, manufacturing, integration, alignment and testing of the PFC and its ancillary equipment. This manuscript describes the final design of the PFC along with the analyses and simulations performed and presents the procedures for the integration and alignment of the lenses in the corrector.

A Search for Neutrino Emission from Fast Radio Bursts with Six Years of IceCube Data

Astrophysical Journal University of Chicago Press 857 (2018) ARTN 117

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 Arguelles, J Auffenberg, S Axani, H Bagherpour, X Bai, JP Barron, SW Barwick, V Baum, R Bay, JJ Beatty, JB Tjus, K-H Becker, S BenZvi, D Berley, E Bernardini, DZ Besson, G Binder, D Bindig, E Blaufuss, S Blot, C Bohm, M Boerner, F Bos, S Boeser, O Botner, E Bourbeau, J Bourbeau, F Bradascio, J Braun, M Brenzke, H-P Bretz, S Bron, J Brostean-Kaiser, A Burgman, RS Busse, T Carver, E Cheung, D Chirkin, A Christov, K Clark, L Classen, GH Collins, JM Conrad, P Coppin, P Correa, DF Cowen, R Cross, P Dave, M Day, JPAM de Andre, C De Clercq, JJ DeLaunay, H Dembinski, S De Ridder, P Desiati, KD de Vries, G de Wasseige, M de With, T DeYoung, JC Diaz-Velez, V di Lorenzo, H Dujmovic, JP Dumm, M Dunkman, E Dvorak, 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, A Fritz, TK Gaisser, J Gallagher, L Gerhardt, K Ghorbani, W Giang, T Glauch, T Gluesenkamp, 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, T Hoinka, B Hokanson-Fasig, K Hoshina, F Huang, M Huber, K Hultqvist, M Huennefele, R Hussain, S In, N Iovine, A Ishihara, E Jacobi, GS Japaridze, M Jeong, K Jero, BJP Jones, P Kalaczynski, W Kang, A Kappes, D Kappesser, 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, R Koirala, H Kolanoski, L Koepke, C Kopper, S Kopper, JP Koschinsky, DJ Koskinen, M Kowalski, K Krings, M Kroll, G Krueckl, S Kunwar, N Kurahashi, T Kuwabara, A Kyriacou, M Labare, JL Lanfranchi, MJ Larson, F Lauber, K Leonard, M Lesiak-Bzdak, M Leuermann, QR Liu, CJL Mariscal, L Lu, J Luenemann, W Luszczak, J Madsen, G Maggi, KBM Mahn, S Mancina, R Maruyama, K Mase, R Maunu, K Meagher, M Medici, M Meier, T Menne, G Merino, T Meures, S Miarecki, J Micallef, G Momente, T Montaruli, RW Moore, M Moulai, R Nahnhauer, P Nakarmi, U Naumann, G Neer, H Niederhausen, SC Nowicki, DR Nygren, AO Pollmann, A Olivas, A O'Murchadha, E O'Sullivan, T Palczewski, H Pandya, DV Pankova, P Peiffer, JA Pepper, CP de los Heros, D Pieloth, E Pinat, M Plum, PB Price, GT Przybylski, C Raab, L Raedel, M Rameez, L Rauch, 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, I Safa, T Saelzer, SES Herrera, A Sandrock, J Sandroos, M Santander, S Sarkar, K Satalecka, P Schlunder, T Schmidt, A Schneider, S Schoenen, S Schoenberg, L Schumacher, S Sclafani, D Seckel, S Seunarine, J Soedingrekso, D Soldin, M Song, GM Spiczak, C Spiering, J Stachurska, M Stamatikos, T Stanev, A Stasik, R Stein, J Stettner, A Steuer, T Stezelberger, RG Stokstad, A Stossl, NL Strotjohann, T Stuttard, GW Sullivan, M Sutherland, I Taboada, J Tatar, F Tenholt, S Ter-Antonyan, A Terliuk, S Tilav, PA Toale, MN Tobin, C Toennis, S Toscano, D Tosi, M Tselengidou, CF Tung, A Turcati, CF Turley, B Ty, E Unger, M Usner, J Vandenbroucke, W Van Driessche, D van Eijk, N van Eijndhoven, S Vanheule, J van Santen, 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, I Collaboration

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

CO Tully-Fisher relation of star-forming galaxies at z = 0.05 – 0.3

Monthly Notices of the Royal Astronomical Society (2018)

S Topal, M Bureau, AL Tiley, TA Davis, K Torii

Electron acceleration by wave turbulence in a magnetized plasma

Nature Physics 14 (2018) 475-479

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 situ1-3. Strong shocks are expected to accelerate particles to very high energies4-6; however, they require a source of particles with velocities fast enough to permit multiple shock crossings. While the resulting diffusive shock acceleration4process 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 pool7,8. 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 wind9, a setting where electron acceleration via lower-hybrid waves is possible.

SPLASH-SXDF Multi-wavelength Photometric Catalog


V Mehta, C Scarlata, P Capak, I Davidzon, A Faisst, BC Hsieh, O Ilbert, M Jarvis, C Laigle, J Phillips, J Silverman, MA Strauss, M Tanaka, R Bowler, J Coupon, S Foucaud, S Hemmati, D Masters, HJ McCracken, B Mobasher, M Ouchi, T Shibuya, W-H Wang

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


(2018) ARTN 030001

M Tanabashi, PD Grp, K Hagiwara, K Hikasa, K Nakamura, Y Sumino, F Takahashi, J Tanaka, K Agashe, G Aielli, C Amsler, M Antonelli, DM Asner, H Baer, S Banerjee, RM Barnett, T Basaglia, CW Bauer, JJ Beatty, VI Belousov, J Beringer, S Bethke, A Bettini, H Bichsel, O Biebel, KM Black, E Blucher, O Buchmuller, V Burkert, MA Bychkov, RN Cahn, M Carena, A Ceccucci, A Cerri, D Chakraborty, M-C Chen, RS Chivukula, 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 D'Onofrio, M Doser, M Drees, HK Dreiner, DA Dwyer, P Eerola, S Eidelman, J Ellis, J Erler, VV Ezhela, W Fetscher, BD Fields, R Firestone, B Foster, A Freitas, H Gallagher, L Garren, H-J Gerber, G Gerbier, T Gershon, Y Gershtein, T Gherghetta, AA Godizov, M Goodman, C Grab, AV Gritsan, C Grojean, DE Groom, M Grunewald, A Gurtu, T Gutsche, HE Haber, C Hanhart, S Hashimoto, Y Hayato, KG Hayes, A Hebecker, S Heinemeyer, B Heltsley, JJ Hernandez-Rey, J Hisano, A Hocker, J Holder, A Holtkamp, T Hyodo, KD Irwin, KF Johnson, M Kado, M Karliner, UF Katz, SR Klein, E Klempt, RV Kowalewski, F Krauss, M Kreps, B Krusche, YV Kuyanov, Y Kwon, O Lahav, J Laiho, J Lesgourgues, A Liddle, Z Ligeti, C-J Lin, C Lippmann, TM Liss, L Littenberg, KS Lugovsky, SB Lugovsky, A Lusiani, Y Makida, F Maltoni, T Mannel, AV Manohar, WJ Marciano, AD Martin, A Masoni, J Matthews, U-G Meissner, D Milstead, RE Mitche, K Moenig, P Molaro, F Moortgat, M Moskovic, H Murayama, M Narain, P Nason, S Navas, M Neubert, P Nevski, Y Nir, KA Olive, SP Griso, J Parsons, C Patrignani, JA Peacock, M Pennington, ST Petcov, VA Petrov, E Pianori, A Piepke, A Pomarol, A Quadt, J Rademacker, G Raffelt, BN Ratcliff, P Richardson, A Ringwald, S Roesler, S Rolli, A Romaniouk, LJ Rosenberg, JL Rosner, G Rybka, RA Ryutin, CT Sachrajda, Y Sakai, GP Salam, S Sarkar, F Sauli, O Schneider, K Scholberg, AJ Schwartz, D Scott, V Sharma, SR Sharpe, T Shutt, M Silari, T Sjostrand, P Skands, T Skwarnicki, JG Smith, GF Smoot, S Spanier, H Spieler, C Spiering, A Stah, SL Stone, T Sumiyoshi, MJ Syphers, K Terashi, J Terning, U Thoma, RS Thorne, L Tiator, M Titov, NP Tkachenko, NA Tornqvist, DR Tovey, G Valencia, R Van de Water, N Varelas, G Venanzoni, L Verde, MG Vincter, P Voge, A Vogt, SP Wakely, W Walkowiak, CW Walter, D Wands, DR Ward, MO Wascko, G Weiglein, DH Weinberg, EJ Weinberg, M White, LR Wiencke, S Willocq, CC Woh, J Womersley, CL Woody, RL Workman, W-M Yao, GP Zeller, OV Zenin, R-Y Zhu, S-L Zhu, F Zimmermann, PA Zyla, J Anderson, L Fuller, VS Lugovsky, P Schaffner

The XMM-SERVS survey: new XMM-Newton point-source catalogue for the XMM-LSS field


C-TJ Chen, WN Brandt, B Luo, P Ranalli, G Yang, DM Alexander, FE Bauer, DD Kelson, M Lacy, K Nyland, P Tozzi, F Vito, M Cirasuolo, R Gilli, MJ Jarvis, BD Lehmer, M Paolillo, DP Schneider, O Shemmer, I Smail, M Sun, M Tanaka, M Vaccari, C Vignali, YQ Xue, M Banerji, KE Chow, B Haussler, RP Norris, JD Silverman, JR Trump

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

Long-term radio and X-ray evolution of the tidal disruption event ASASSN-14li


JS Bright, RP Fender, SE Motta, K Mooley, YC Perrott, S van Velzen, S Carey, J Hickish, N Razavi-Ghods, D Titterington, P Scott, K Grainge, A Scaife, T Cantwell, C Rumsey

A Subarcsecond Near-infrared View of Massive Galaxies at z > 1 with Gemini Multi-conjugate Adaptive Optics


M Lacy, K Nyland, M Mao, P Jagannathan, J Pforr, SE Ridgway, J Afonso, D Farrah, P Guarnieri, E Gonzales-Solares, MJ Jarvis, C Maraston, DM Nielsen, AO Petric, A Sajina, JA Surace, M Vaccari

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

Journal of Cosmology and Astroparticle Physics 2018 (2018)

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

© 2018 IOP Publishing Ltd and Sissa Medialab. We consider the possibility that the primordial curvature perturbation is direction-dependent. To first order this is parameterised by a quadrupolar modulation of the power spectrum and results in statistical anisotropy of the CMB, which can be quantified using 'bipolar spherical harmonics'. We compute these for the Planck DR2-2015 SMICA map and estimate the noise covariance from Planck Full Focal Plane 9 simulations. A constant quadrupolar modulation is detected with 2.2 σ significance, dropping to 2σ when the primordial power is assumed to scale with wave number k as a power law. Going beyond previous work we now allow the spectrum to have arbitrary scale-dependence. Our non-parametric reconstruction then suggests several spectral features, the most prominent at k ∼ 0.006 Mpc-1. When a constant quadrupolar modulation is fitted to data in the range 0.005 ≤ k/Mpc-1≤ 0.008, its preferred directions are found to be related to the cosmic hemispherical asymmetry and the CMB dipole. To determine the significance we apply two test statistics to our reconstructions of the quadrupolar modulation from data, against reconstructions of realisations of noise only. With a test statistic sensitive only to the amplitude of the modulation, the reconstructions from the multipole range 30 ≤ ℓ ≤ 1200 are unusual with 2.1σ significance. With the second test statistic, sensitive also to the direction, the significance rises to 6.9σ. Our approach is easily generalised to include other data sets such as polarisation, large-scale structure and forthcoming 21-cm line observations which will enable these anomalies to be investigated further.

HST Grism Confirmation of 16 Structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey


G Noirot, D Stern, S Mei, D Wylezalek, EA Cooke, C De Breuck, A Galametz, NA Hatch, J Vernet, M Brodwin, P Eisenhardt, AH Gonzalez, M Jarvis, A Rettura, N Seymour, SA Stanford