Publications


No surviving non-compact stellar companion to Cassiopeia A

ASTRONOMY & ASTROPHYSICS 623 (2019) ARTN A34

WE Kerzendorf, T Do, SE de Mink, Y Gotberg, D Milisavljevic, E Zapartas, M Renzo, S Justham, P Podsiadlowski, RA Fesen


Ultrahigh energy cosmic rays from shocks in the lobes of powerful radio galaxies

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 482 (2019) 4303-4321

JH Matthews, AR Bell, KM Blundell, AT Araudo


Search for non-relativistic magnetic monopoles with IceCube: IceCube Collaboration (vol 74, 2938, 2014)

EUROPEAN PHYSICAL JOURNAL C 79 (2019) ARTN 124

MG Aartsen, R Abbasi, M Ackermann, J Adams, JA Aguilar, M Ahlers, D Altmann, C Arguelles, TC Arlen, J Auffenberg, X Bai, M Baker, SW Barwick, V Baum, R Bay, JJ Beatty, JB Tjus, K-H Becker, ML Benabderrahmane, S BenZvi, P Berghaus, D Berley, E Bernardini, A Bernhard, DZ Besson, G Binder, D Bindig, M Bissok, E Blaufuss, J Blumenthal, DJ Boersma, C Bohm, D Bose, S Boeser, O Botner, L Brayeur, H-P Bretz, AM Brown, R Bruijn, J Casey, M Casier, D Chirkin, A Christov, B Christy, K Clark, L Classen, F Clevermann, S Coenders, S Cohen, DF Cowen, AHC Silva, M Danninger, J Daughhetee, JC Davis, M Day, JPAM de Andre, C De Clercq, S De Ridder, P Desiati, KD de Vries, M de With, T DeYoung, JC Diaz-Velez, M Dunkman, R Eagan, B Eberhardt, B Eichmann, J Eisch, S Euler, PA Evenson, O Fadiran, AR Fazely, A Fedynitch, J Feintzeig, T Feusels, K Filimonov, C Finley, T Fischer-Wasels, S Flis, A Franckowiak, K Frantzen, T Fuchs, TK Gaisser, J Gallagher, L Gerhardt, L Gladstone, T Gluesenkamp, A Goldschmidt, G Golup, JG Gonzalez, JA Goodman, D Gora, DT Grandmont, D Grant, P Gretskov, JC Groh, A Gross, C Ha, C Haack, AH Ismail, P Hallen, A Hallgren, F Halzen, K Hanson, D Hebecker, D Heereman, D Heinen, K Helbing, R Hellauer, S Hickford, GC Hill, KD Hoffman, R Hoffmann, A Homeier, K Hoshina, F Huang, W Huelsnitz, PO Hulth, K Hultqvist, S Hussain, A Ishihara, E Jacobi, J Jacobsen, K Jagielski, GS Japaridze, K Jero, O Jlelati, B Kaminsky, A Kappes, T Karg, A Karle, M Kauer, JL Kelley, J Kiryluk, J Klaes, SR Klein, J-H Koehne, G Kohnen, H Kolanoski, L Kopke, C Kopper, S Kopper, DJ Koskinen, M Kowalski, M Krasberg, A Kriesten, K Krings, G Kroll, J Kunnen, N Kurahashi, T Kuwabara, M Labare, H Landsman, MJ Larson, M Lesiak-Bzdak, M Leuermann, J Leute, J Luenemann, O Macias, J Madsen, G Maggi, R Maruyama, K Mase, HS Matis, F McNally, K Meagher, A Meli, M Merck, T Meures, S Miarecki, E Middell, N Milke, J Miller, L Mohrmann, T Montaruli, R Morse, R Nahnhauer, U Naumann, H Niederhausen, SC Nowicki, DR Nygren, A Obertacke, S Odrowski, A Olivas, A Omairat, A O'Murchadha, T Palczewski, L Paul, JA Pepper, CP de los Heros, C Pfendner, D Pieloth, E Pinat, J Posselt, PB Price, GT Przybylski, M Quinnan, L Raedel, M Rameez, K Rawlins, P Redl, R Reimann, E Resconi, W Rhode, M Ribordy, M Richman, B Riedel, S Robertson, JP Rodrigues, C Rott, T Ruhe, B Ruzybayev, D Ryckbosch, SM Saba, H-G Sander, M Santander, S Sarkar, K Schatto, F Scheriau, T Schmidt, M Schmitz, S Schoenen, S Schoeneberg, A Schoenwald, A Schukraft, L Schulte, O Schulz, D Seckel, Y Sestayo, S Seunarine, R Shanidze, C Sheremata, MWE Smith, D Soldin, GM Spiczak, C Spiering, M Stamatikos, T Stanev, NA Stanisha, A Stasik, T Stezelberger, RG Stokstad, A Stoessl, EA Strahler, R Stroem, NL Strotjohann, GW Sullivan, H Taavola, I Taboada, A Tamburro, A Tepe, S Ter-Antonyan, G Tesic, S Tilav, PA Toale, MN Tobin, S Toscano, M Tselengidou, E Unger, M Usner, S Vallecorsa, N van Eijndhoven, J van Santen, M Vehring, M Voge, M Vraeghe, C Walck, M Wallraff, C Weaver, M Wellons, C Wendt, S Westerhoff, BJ Whelan, N Whitehorn, K Wiebe, CH Wiebusch, DR Williams, H Wissing, M Wolf, TR Wood, K Woschnagg, DL Xu, XW Xu, JP Yanez, G Yodh, S Yoshida, P Zarzhitsky, J Ziemann, S Zierke, M Zoll, I Collaboration


Zooming in on supermassive black holes: how resolving their gas cloud host renders their accretion episodic

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2018)

RS Beckmann, J Devriendt, A Slyz

Born in rapidly evolving mini-halos during the first billion years of the Universe, super- massive black holes (SMBH) feed from gas flows spanning many orders of magnitude, from the cosmic web in which they are embedded to their event horizon. As such, accretion onto SMBHs constitutes a formidable challenge to tackle numerically, and currently requires the use of sub-grid models to handle the flow on small, unresolved scales. In this paper, we study the impact of resolution on the accretion pattern of SMBHs initially inserted at the heart of dense galactic gas clouds, using a custom super-Lagrangian refinement scheme to resolve the black hole (BH) gravitational zone of influence. We find that once the self-gravitating gas cloud host is sufficiently well re- solved, accretion onto the BH is driven by the cloud internal structure, independently of the BH seed mass, provided dynamical friction is present during the early stages of cloud collapse. For a pristine gas mix of hydrogen and helium, a slim disc develops around the BH on sub-parsec scales, turning the otherwise chaotic BH accretion duty cycle into an episodic one, with potentially important consequences for BH feedback. In the presence of such a nuclear disc, BH mass growth predominantly occurs when infalling dense clumps trigger disc instabilities, fuelling intense albeit short-lived gas accretion episodes.


Suppressed effective viscosity in the bulk intergalactic plasma

Nature Astronomy (2019)

I Zhuravleva, E Churazov, AA Schekochihin, SW Allen, A Vikhlinin, N Werner

© 2019, The Author(s), under exclusive licence to Springer Nature Limited. Transport properties, such as viscosity and thermal conduction, of the hot intergalactic plasma in clusters of galaxies are largely unknown. Whereas for laboratory plasmas these characteristics are derived from the gas density and temperature1, such recipes can be fundamentally different for the intergalactic plasma2 owing to a low rate of particle collisions and a weak magnetic field3. In numerical simulations, these unknowns can often be avoided by modelling these plasmas as hydrodynamic fluids4–6, even though local, non-hydrodynamic features observed in clusters contradict this assumption7–9. Using deep Chandra observations of the Coma Cluster10,11, we probe gas fluctuations in intergalactic medium down to spatial scales where the transport processes should prominently manifest themselves—provided that hydrodynamic models12 with pure Coulomb collision rates are indeed adequate. We do not find evidence of such transport processes, implying that the effective isotropic viscosity is orders of magnitude smaller than naively expected. This indicates either an enhanced collision rate in the plasma due to particle scattering off microfluctuations caused by plasma instabilities2,13,14 or that the transport processes are anisotropic with respect to the local magnetic field15. This also means that numerical models with high Reynolds number appear more consistent with observations. Our results demonstrate that observations of turbulence in clusters16,17 are giving rise to a branch of astrophysics that can sharpen theoretical views on galactic plasmas.


Search for transient optical counterparts to high-energy IceCube neutrinos with Pan-STARRS1

ASTRONOMY & ASTROPHYSICS 626 (2019) ARTN A117

E Kankare, M Huber, SJ Smartt, K Chambers, KW Smith, O McBrien, T-W Chen, H Flewelling, T Lowe, E Magnier, A Schultz, C Waters, RJ Wainscoat, M Willman, D Wright, D Young, MG Aartsen, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, C Alispach, D Altmann, K Andeen, T Anderson, I Ansseau, G Anton, C Arguelles, J Auffenberg, S Axani, P Backes, H Bagherpour, X Bai, A Barbano, SW Barwick, V Baum, R Bay, JJ Beatty, K-H Becker, JB Tjus, S BenZvi, D Berley, E Bernardini, DZ Besson, G Binder, D Bindig, E Blaufuss, S Blot, C Bohm, M Boerner, S Boeser, O Botner, E Bourbeau, J Bourbeau, F Bradascio, J Braun, H-P Bretz, S Bron, J Brostean-Kaiser, A Burgman, RS Busse, T Carver, C Chen, E Cheung, D Chirkin, K Clark, L Classen, GH Collin, JM Conrad, P Coppin, P Correa, DF Cowen, R Cross, P Dave, JPAM de Andre, C De Clercq, JJ DeLaunay, H Dembinski, K Deoskar, S De Ridder, P Desiati, KD de Vries, G de Wasseige, M de With, T DeYoung, JC Diaz-Velez, H Dujmovic, M Dunkman, E Dvorak, B Eberhardt, T Ehrhardt, P Eller, PA Evenson, S Fahey, AR Fazely, J Felde, K Filimonov, C Finley, A Franckowiak, E Friedman, A Fritz, TK Gaisser, J Gallagher, E Ganster, S Garrappa, L Gerhardt, K Ghorbani, T Glauch, T Glsenkamp, A Goldschmidt, JG Gonzalez, D Grant, Z Griffith, M Guenduez, C Haack, A Hallgren, L Halve, F Halzen, K Hanson, D Hebecker, D Heereman, K Helbing, R Hellauer, F Henningsen, S Hickford, J Hignight, GC Hill, KD Hoffman, R Hoffmann, T Hoinka, B Hokanson-Fasig, K Hoshina, F Huang, K Hultqvist, M Huennefeld, 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, M Karl, A Karle, U Katz, M Kauer, A Keivani, JL Kelley, A Kheirandish, J Kim, T Kintscher, J Kiryluk, T Kittler, SR Klein, R Koirala, H Kolanoski, L Koepke, C Kopper, S Kopper, DJ Koskinen, M Kowalski, K Krings, G Krueckl, N Kulacz, S Kunwar, N Kurahashi, A Kyriacou, M Labare, JL Lanfranchi, MJ Larson, F Lauber, JP Lazar, K Leonard, M Leuermann, QR Liu, E Lohfink, CJL Mariscal, L Lu, F Lucarelli, J Lunemann, W Luszczak, J Madsen, G Maggi, KBM Mahn, Y Makino, K Mallot, S Mancina, IC Mari, R Maruyama, K Mase, R Maunu, K Meagher, M Medici, A Medina, M Meier, S Meighen-Berger, T Menne, G Merino, T Meures, S Miarecki, J Micallef, G Momente, T Montaruli, RW Moore, M Moulai, R Nagai, 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, N Park, P Peiffer, CP de los Heros, D Pieloth, E Pinat, A Pizzuto, M Plum, PB Price, GT Przybylski, C Raab, A Raissi, M Rameez, L Rauch, K Rawlins, IC Rea, R Reimann, B Relethford, G Renzi, E Resconi, W Rhode, M Richman, S Robertson, M Rongen, C Rott, T Ruhe, D Ryckbosch, D Rysewyk, I Safa, SES Herrera, A Sandrock, J Sandroos, M Santander, S Sarkar, K Satalecka, M Schaufel, P Schlunder, T Schmidt, A Schneider, J Schneider, L Schumacher, S Sclafani, D Seckel, S Seunarine, M Silva, R Snihur, 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, F Tenholt, S Ter-Antonyan, A Terliuk, S Tilav, L Tomankova, C Tonnis, S Toscano, D Tosi, M Tselengidou, CF Tung, A Turcati, R Turcotte, CF Turley, B Ty, E Unger, MAU Elorrieta, M Usner, J Vandenbroucke, W Van Driessche, D van Eijk, N van Eijndhoven, S Vanheule, J van Santen, M Vraeghe, C Walck, A Wallace, M Wallraff, N Wandkowsky, TB Watson, C Weaver, MJ Weiss, J Weldert, C Wendt, J Werthebach, S Westerhoff, BJ Whelan, N Whitehorn, K Wiebe, CH Wiebusch, L Wille, DR Williams, L Wills, M Wolf, J Wood, TR Wood, K Woschnagg, G Wrede, DL Xu, XW Xu, Y Xu, JP Yanez, G Yodh, S Yoshida, T Yuan, J Nordin, Pan-STARRS, I Collaboration


Investigation of Two Fermi-LAT Gamma-Ray Blazars Coincident with High-energy Neutrinos Detected by IceCube

ASTROPHYSICAL JOURNAL 880 (2019) ARTN 103

S Garrappa, S Buson, A Franckowiak, BJ Shappee, JF Beacom, S Dong, TW-S Holoien, CS Kochanek, JL Prieto, KZ Stanek, TA Thompson, MG Aartsen, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, C Alispach, K Andeen, T Anderson, I Ansseau, G Anton, C Arguelles, J Auffenberg, S Axani, P Backes, H Bagherpour, X Bai, A Barbano, SW Barwick, V Baum, R Bay, JJ Beatty, K-H Becker, JB Tjus, S BenZvi, D Berley, E Bernardini, DZ Besson, G Binder, D Bindig, E Blaufuss, S Blot, C Bohm, M Boerner, S Boeser, O Botner, E Bourbeau, J Bourbeau, F Bradascio, J Braun, H-P Bretz, S Bron, J Brostean-Kaiser, A Burgman, RS Busse, T Carver, C Chen, E Cheung, D Chirkin, K Clark, L Classen, GH Collin, JM Conrad, P Coppin, P Correa, DF Cowen, R Cross, P Dave, JPAM de Andre, C De Clercq, JJ DeLaunay, H Dembinski, K Deoskar, S De Ridder, P Desiati, KD de Vries, G de Wasseige, M de With, T DeYoung, A Diaz, JC Diaz-Velez, H Dujmovic, M Dunkman, E Dvorak, B Eberhardt, T Ehrhardt, P Eller, PA Evenson, S Fahey, AR Fazely, J Felde, K Filimonov, C Finley, E Friedman, A Fritz, TK Gaisser, J Gallagher, E Ganster, L Gerhardt, K Ghorbani, T Glauch, T Gluesenkamp, A Goldschmidt, JG Gonzalez, D Grant, Z Griffith, M Guender, M Guenduez, C Haack, A Hallgren, L Halve, F Halzen, K Hanson, D Hebecker, D Heereman, K Helbing, R Hellauer, F Henningsen, S Hickford, J Hignight, GC Hill, KD Hoffman, R Hoffmann, T Hoinka, B Hokanson-Fasig, K Hoshina, F Huang, M Huber, K Hultqvist, M Huennefeld, R Hussain, S In, N Iovine, A Ishihara, E Jacobi, GS Japaridze, M Jeong, K Jero, BJP Jones, W Kang, A Kappes, D Kappesser, T Karg, M Karl, A Karle, U Katz, M Kauer, A Keivani, JL Kelley, A Kheirandish, J Kim, T Kintscher, J Kiryluk, T Kittler, SR Klein, R Koirala, H Kolanoski, L Koepke, C Kopper, S Kopper, DJ Koskinen, M Kowalski, K Krings, G Krueckl, N Kulacz, S Kunwar, N Kurahashi, A Kyriacou, M Labare, JL Lanfranchi, MJ Larson, F Lauber, JP Lazar, K Leonard, M Leuermann, QR Liu, E Lohfink, CJL Mariscal, L Lu, F Lucarelli, J Lunemann, W Luszczak, J Madsen, G Maggi, KBM Mahn, Y Makino, K Mallot, S Mancina, IC Maris, R Maruyama, K Mase, R Maunu, K Meagher, M Medici, A Medina, M Meier, S Meighen-Berger, T Menne, G Merino, T Meures, S Miarecki, J Micallef, G Momente, T Montaruli, RW Moore, M Moulai, R Nagai, 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, N Park, P Peiffer, CP de los Heros, D Pieloth, E Pinat, A Pizzuto, M Plum, PB Price, GT Przybylski, C Raab, A Raissi, M Rameez, L Rauch, K Rawlins, IC Rea, R Reimann, B Relethford, G Renzi, E Resconi, W Rhode, M Richman, S Robertson, M Rongen, C Rott, T Ruhe, D Ryckbosch, D Rysewyk, I Safa, SES Herrera, A Sandrock, J Sandroos, M Santander, S Sarkar, K Satalecka, M Schaufel, P Schlunder, T Schmidt, A Schneider, J Schneider, L Schumacher, S Sclafani, D Seckel, S Seunarine, M Silva, R Snihur, 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, F Tenholt, S Ter-Antonyan, A Terliuk, S Tilav, L Tomankova, C Tonnis, S Toscano, D Tosi, M Tselengidou, CF Tung, A Turcati, R Turcotte, CF Turley, B Ty, E Unger, MAU Elorrieta, M Usner, J Vandenbroucke, W Van Driessche, D van Eijk, N van Eijndhoven, S Vanheule, J van Santen, M Vraeghe, C Walck, A Wallace, M Wallraff, N Wandkowsky, TB Watson, C Weaver, MJ Weiss, J Weldert, C Wendt, J Werthebach, S Westerhoff, BJ Whelan, N Whitehorn, K Wiebe, CH Wiebusch, L Wille, DR Williams, L Wills, M Wolf, J Wood, TR Wood, K Woschnagg, G Wrede, DL Xu, XW Xu, Y Xu, JP Yanez, G Yodh, S Yoshida, T Yuan, F-L Collaboration, ASAS-SN Collaboration, I Collaboration


Intrinsic rotation driven by turbulent acceleration

PLASMA PHYSICS AND CONTROLLED FUSION 61 (2019) ARTN 025003

M Barnes, FI Parra


Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 487 (2019) 5902-5921

H Katz, TP Galligan, T Kimm, J Rosdahl, MG Haehnelt, J Blaizot, J Devriendt, A Slyz, N Laporte, R Ellis


On the observed diversity of star formation efficiencies in Giant Molecular Clouds

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 486 (2019) 5482-5491

K Grisdale, O Agertz, F Renaud, AB Romeo, J Devriendt, A Slyz


$\texttt{stella}$: a mixed implicit-explicit, delta-f gyrokinetic code for general magnetic field configurations

Journal of Computational Physics Elsevier (2019)

M Barnes, F Parra-Diaz, M Landreman

Here we present details of a mixed implicit-explicit numerical scheme for the solution of the gyrokinetic-Poisson system of equations in the local limit. This scheme has been implemented in a new code called $\texttt{stella}$, which is capable of evolving electrostatic fluctuations with full kinetic electron effects and an arbitrary number of ion species in general magnetic geometry. We demonstrate the advantages of this mixed approach over a fully explicit treatment and provide linear and nonlinear benchmark comparisons for both axisymmetric and non-axisymmetric magnetic equilibria.


Thomson scattering cross section in a magnetized, high-density plasma.

Physical review. E 99 (2019) 063204-

AFA Bott, G Gregori

We calculate the Thomson scattering cross section in a nonrelativistic, magnetized, high-density plasma-in a regime where collective excitations can be described by magnetohydrodynamics. We show that, in addition to cyclotron resonances and an elastic peak, the cross section exhibits two pairs of peaks associated with slow and fast magnetosonic waves; by contrast, the cross section arising in pure hydrodynamics possesses just a single pair of Brillouin peaks. Both the position and the width of these magnetosonic-wave peaks depend on the ambient magnetic field and temperature, as well as transport and thermodynamic coefficients, and so can therefore serve as a diagnostic tool for plasma properties that are otherwise challenging to measure.


Galaxies flowing in the oriented saddle frame of the cosmic web

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 483 (2019) 3227-3254

K Kraljic, C Pichon, Y Dubois, S Codis, C Cadiou, J Devriendt, M Musso, C Welker, S Arnouts, HS Hwang, C Laigle, S Peirani, A Slyz, M Treyer, D Vibert


Laboratory study of stationary accretion shock relevant to astrophysical systems.

Scientific reports 9 (2019) 8157-

P Mabey, B Albertazzi, E Falize, T Michel, G Rigon, L Van Box Som, A Pelka, F-E Brack, F Kroll, E Filippov, G Gregori, Y Kuramitsu, DQ Lamb, C Li, N Ozaki, S Pikuz, Y Sakawa, P Tzeferacos, M Koenig

Accretion processes play a crucial role in a wide variety of astrophysical systems. Of particular interest are magnetic cataclysmic variables, where, plasma flow is directed along the star's magnetic field lines onto its poles. A stationary shock is formed, several hundred kilometres above the stellar surface; a distance far too small to be resolved with today's telescopes. Here, we report the results of an analogous laboratory experiment which recreates this astrophysical system. The dynamics of the laboratory system are strongly influenced by the interplay of material, thermal, magnetic and radiative effects, allowing a steady shock to form at a constant distance from a stationary obstacle. Our results demonstrate that a significant amount of plasma is ejected in the lateral direction; a phenomenon that is under-estimated in typical magnetohydrodynamic simulations and often neglected in astrophysical models. This changes the properties of the post-shock region considerably and has important implications for many astrophysical studies.


The formation and evolution of low-surface-brightness galaxies

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 485 (2019) 796-818

G Martin, S Kaviraj, C Laigle, JEG Devriendt, RA Jackson, S Peirani, Y Dubois, C Pichon, A Slyz


Overview of new MAST physics in anticipation of first results from MAST Upgrade

NUCLEAR FUSION 59 (2019) ARTN 112011

JR Harrison, RJ Akers, SY Allan, JS Allcock, JO Allen, L Appel, M Barnes, N Ben Ayedl, W Boeglin, C Bowman, J Bradley, P Browning, P Bryant, M Carr, M Cecconello, CD Challis, S Chapman, IT Chapman, GJ Colyer, S Conroy, NJ Conway, M Cox, G Cunningham, RO Dendy, W Dorland, BD Dudson, L Easy, SD Elmore, T Farley, X Feng, AR Field, A Fil, GM Fishpool, M Fitzgerald, K Flesch, MFJ Fox, H Frerichs, S Gadgil, D Gahle, L Garzotti, Y-C Ghim, S Gibson, KJ Gibson, S Hall, C Ham, N Heiberg, SS Henderson, E Highcock, B Hnat, J Howard, J Huang, SWA Irvine, AS Jacobsen, O Jones, I Katramados, D Keeling, A Kirk, I Klimek, L Kogan, J Leland, B Lipschultz, B Lloyd, J Lovell, B Madsen, O Marshall, R Martin, G McArdle, K McClements, B McMillan, A Meakins, HF Meyer, F Militello, J Milnes, S Mordijck, AW Morris, D Moulton, D Muir, K Mukhi, S Murphy-Sugrue, O Myatra, G Naylor, P Naylor, SL Newton, T O'Gorman, J Omotani, MG O'Mullane, S Orchard, SJP Pamela, L Pangione, F Parra, RV Perez, L Piron, M Price, ML Reinke, F Riva, CM Roach, D Robb, D Ryan, S Saarelma, M Salewski, S Scannell, AA Schekochihin, O Schmitz, S Sharapov, R Sharples, SA Silburn, SF Smith, A Sperduti, R Stephen, NT Thomas-Davies, AJ Thornton, M Turnyanskiy, M Valovic, F Van Wyk, RGL Vann, NR Walkden, I Waters, HR Wilson, MAST-U Team, EM Team


Magnetogenesis at Cosmic Dawn: Tracing the Origins of Cosmic Magnetic Fields

MNRAS (0)

H Katz, S Martin-Alvarez, J Devriendt, A Slyz, T Kimm

Despite their ubiquity, the origin of cosmic magnetic fields remains unknown. Various mechanisms have been proposed for their existence including primordial fields generated by inflation, or amplification and injection by compact astrophysical objects. Separating the potential impact of each magnetogenesis scenario on the magnitude and orientation of the magnetic field and their impact on gas dynamics may give insight into the physics that magnetised our Universe. In this work, we demonstrate that because the induction equation and solenoidal constraint are linear with $B$, the contribution from different sources of magnetic field can be separated in cosmological magnetohydrodynamics simulations and their evolution and influence on the gas dynamics can be tracked. Exploiting this property, we develop a magnetic field tracer algorithm for cosmological simulations that can track the origin and evolution of different components of the magnetic field. We present a suite of cosmological magnetohydrodynamical RAMSES simulations that employ this algorithm where the primordial field strength is varied to determine the contributions of the primordial and supernovae-injected magnetic fields to the total magnetic energy as a function of time and spatial location. We find that, for our specific model, the supernova-injected fields rarely penetrate far from haloes, despite often dominating the total magnetic energy in the simulations. The magnetic energy density from the supernova-injected field scales with density with a power-law slope steeper than 4/3 and often dominates the total magnetic energy inside of haloes. However, the star formation rates in our simulations are not affected by the presence of magnetic fields, for the ranges of primordial field strengths examined. These simulations represent a first demonstration of the magnetic field tracer algorithm (abridged).


Massive Stellar Mergers as Precursors of Hydrogen-rich Pulsational Pair Instability Supernovae

ASTROPHYSICAL JOURNAL LETTERS 876 (2019) ARTN L29

A Vigna-Gomez, S Justham, I Mandel, SE de Mink, P Podsiadlowski


Horizon-AGN virtual observatory-1. SED-fitting performance and forecasts for future imaging surveys

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 486 (2019) 5104-5123

C Laigle, I Davidzon, O Ilbert, J Devriendt, D Kashino, C Pichon, P Capak, S Arnouts, S de la Torre, Y Dubois, G Gozaliasl, D Le Borgne, S Lilly, HJ McCracken, M Salvato, A Slyz


Probing Cosmic Dawn: Modelling the Assembly History, SEDs, and Dust Content of Selected $z\sim9$ Galaxies

MNRAS (0)

H Katz, N Laporte, RS Ellis, J Devriendt, A Slyz

The presence of spectroscopically confirmed Balmer breaks in galaxy spectral energy distributions (SEDs) at $z>9$ provides one of the best probes of the assembly history of the first generations of stars in our Universe. Recent observations of the gravitationally lensed source, MACS 1149_JD1 (JD1), indicate that significant amounts of star formation likely occurred at redshifts as high as $z\simeq15$. The inferred stellar mass, dust mass, and assembly history of JD1, or any other galaxy at these redshifts that exhibits a strong Balmer break, can provide a strong test of our best theoretical models from high-resolution cosmological simulations. In this work, we present the results from a cosmological radiation-hydrodynamics simulation of the region surrounding a massive Lyman-break galaxy. For two of our most massive systems, we show that dust preferentially resides in the vicinity of the young stars thereby increasing the strength of the measured Balmer break such that the simulated SEDs are consistent with the photometry of JD1 and two other $z>9$ systems (GN-z10-3 and GN-z9-1) that have proposed Balmer breaks at high redshift. We find strong variations in the shape and luminosity of the SEDs of galaxies with nearly identical stellar and halo masses, indicating the importance of morphology, assembly history, and dust distribution in making inferences on the properties of individual galaxies at high redshifts. Our results stress the importance that dust may play in modulating the observable properties of galaxies, even at the extreme redshifts of $z>9$.

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