Search

Your search keyword '"Massey A"' showing total 320 results
Start Over Author "Massey A" Journal monthly notices of the royal astronomical society
320 results on '"Massey A"'

2. Strong gravitational lensing’s ‘external shear’ is not shear

Author

Etherington, Amy, primary, Nightingale, James W, additional, Massey, Richard, additional, Tam, Sut-Ieng, additional, Cao, XiaoYue, additional, Niemiec, Anna, additional, He, Qiuhan, additional, Robertson, Andrew, additional, Li, Ran, additional, Amvrosiadis, Aristeidis, additional, Cole, Shaun, additional, Diego, Jose M, additional, Frenk, Carlos S, additional, Frye, Brenda L, additional, Harvey, David, additional, Jauzac, Mathilde, additional, Koekemoer, Anton M, additional, Lagattuta, David J, additional, Lange, Samuel, additional, Limousin, Marceau, additional, Mahler, Guillaume, additional, Sirks, Ellen, additional, and Steinhardt, Charles L, additional

Published
2024
Full Text
View/download PDF

4. A complex node of the cosmic web associated with the massive galaxy cluster MACS J0600.1-2008.

Author

Furtak, Lukas J, Zitrin, Adi, Richard, Johan, Eckert, Dominique, Sayers, Jack, Ebeling, Harald, Fujimoto, Seiji, Laporte, Nicolas, Lagattuta, David, Limousin, Marceau, Mahler, Guillaume, Meena, Ashish K, Andrade-Santos, Felipe, Frye, Brenda L, Jauzac, Mathilde, Koekemoer, Anton M, Kohno, Kotaro, Espada, Daniel, Lu, Harry, and Massey, Richard

Subjects
LARGE scale structure (Astronomy), GRAVITATIONAL lenses, DARK matter, GALAXIES, X-rays, GALAXY clusters
Abstract

MACS J0600.1-2008 (MACS0600) is an X-ray-luminous, massive galaxy cluster at |$z_{\mathrm{d}}=0.43$|⁠ , studied previously by the REionization LensIng Cluster Survey and ALMA Lensing Cluster Survey projects which revealed a complex, bimodal mass distribution and an intriguing high-redshift object behind it. Here, we report on the results of a combined analysis of the extended strong lensing (SL), X-ray, Sunyaev–Zeldovich (SZ), and galaxy luminosity-density properties of this system. Using new JWST and ground-based Gemini-N and Keck data, we obtain 13 new spectroscopic redshifts of multiply-imaged galaxies and identify 12 new photometric multiple-image systems and candidates, including two multiply-imaged |$z\sim 7$| objects. Taking advantage of the larger areal coverage, our analysis reveals an additional bimodal, massive SL structure which we measure spectroscopically to lie adjacent to the cluster and whose existence was implied by previous SL-modelling analyses. While based in part on photometric systems identified in ground-based imaging requiring further verification, our extended SL model suggests that the cluster may have the second-largest critical area and effective Einstein radius observed to date, |$A_{\mathrm{crit}}\simeq 2.16\, \mathrm{arcmin}^2$| and |$\theta _{\mathrm{E}}=49.7^{\prime \prime }\pm 5.0^{\prime \prime }$| for a source at |$z_{\mathrm{s}}=2$|⁠ , enclosing a total mass of |$M(\lt \theta _{\mathrm{E}})=(4.7\pm 0.7)\times 10^{14}\, \mathrm{M}_{\odot }$|⁠. These results are also supported by the galaxy luminosity distribution, and the SZ and X-ray data. Yet another, probably related massive cluster structure, discovered in X-rays 5 arcmin (1.7 Mpc) further north, suggests that MACS0600 is part of an even larger filamentary structure. This discovery adds to several recent detections of massive structures around SL galaxy clusters and establishes MACS0600 as a prime target for future high-redshift surveys with JWST. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

5. Unveiling lens light complexity with a novel multi-Gaussian expansion approach for strong gravitational lensing.

Author

He, Qiuhan, Nightingale, James W, Amvrosiadis, Aris, Robertson, Andrew, Cole, Shaun, Frenk, Carlos S, Massey, Richard, Li, Ran, Cao, Xiaoyue, Lange, Samuel C, and França, João Paulo C

Subjects
GRAVITATIONAL lenses, GALACTIC magnitudes, IMAGE processing
Abstract

In a strong gravitational lensing system, the distorted light from a source is analysed to infer the properties of the lens. However, light emitted by the lens itself can contaminate the image of the source, introducing systematic errors in the analysis. We present a simple and efficient lens light model based on the well-tested multi-Gaussian expansion (MGE) method for representing galaxy surface brightness profiles, which we combine with a semi-linear inversion scheme for pixelized source modelling. Testing it against realistic mock lensing images, we show that our scheme can fit the lensed images to the noise level, with relative differences between the true input and best-fitting lens light model remaining below 5 per cent. We apply the MGE lens light model to 38 lenses from the HST SLACS sample. We find that the new scheme provides a good fit for the majority of the sample with only 3 exceptions – these show clear asymmetric residuals in the lens light. We examine the radial dependence of the ellipticity and position angles and confirm that it is common for a typical lens galaxy to exhibit twisting non-elliptical isophotes and boxy / disky isophotes. Our MGE lens light model will be a valuable tool for understanding the hidden complexity of the lens mass distribution. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

9. The dark matter haloes of moderate luminosity X-ray AGN as determined from weak gravitational lensing and host stellar masses

Author

Leauthaud, Alexie, J. Benson, Andrew, Civano, Francesca, L. Coil, Alison, Bundy, Kevin, Massey, Richard, Schramm, Malte, Schulze, Andreas, Capak, Peter, Elvis, Martin, Kulier, Andrea, and Rhodes, Jason

Subjects
galaxies: abundances, galaxies: active, galaxies: haloes, galaxies: Seyfert, galaxies: stellar content, Astronomical and Space Sciences, Astronomy & Astrophysics
Published
2015

10. Euclid: the selection of quiescent and star-forming galaxies using observed colours

Author

L Bisigello, U Kuchner, C J Conselice, S Andreon, M Bolzonella, P-A Duc, B Garilli, A Humphrey, C Maraston, M Moresco, L Pozzetti, C Tortora, G Zamorani, N Auricchio, J Brinchmann, V Capobianco, J Carretero, F J Castander, M Castellano, S Cavuoti, A Cimatti, R Cledassou, G Congedo, L Conversi, L Corcione, M S Cropper, S Dusini, M Frailis, E Franceschi, P Franzetti, M Fumana, F Hormuth, H Israel, K Jahnke, S Kermiche, T Kitching, R Kohley, B Kubik, M Kunz, O Le Fèvre, S Ligori, P B Lilje, I Lloro, E Maiorano, O Marggraf, R Massey, D C Masters, S Mei, Y Mellier, G Meylan, C Padilla, S Paltani, F Pasian, V Pettorino, S Pires, G Polenta, M Poncet, F Raison, J Rhodes, M Roncarelli, E Rossetti, R Saglia, M Sauvage, P Schneider, A Secroun, S Serrano, F Sureau, A N Taylor, I Tereno, R Toledo-Moreo, L Valenziano, Y Wang, M Wetzstein, and J Zoubian

Published
2020
Full Text
View/download PDF

11. Hydrodynamical simulations of merging galaxy clusters: giant dark matter particle colliders, powered by gravity.

Author

Sirks, Ellen L, Harvey, David, Massey, Richard, Oman, Kyle A, Robertson, Andrew, Frenk, Carlos, Everett, Spencer, Gill, Ajay S, Lagattuta, David, and McCleary, Jacqueline

Subjects
GALAXY clusters, DARK matter, CHARGED particle accelerators, DARK energy, GALAXY mergers, GRAVITY
Abstract

Terrestrial particle accelerators collide charged particles, then watch the trajectory of outgoing debris – but they cannot manipulate dark matter. Fortunately, dark matter is the main component of galaxy clusters, which are continuously pulled together by gravity. We show that galaxy cluster mergers can be exploited as enormous, natural dark matter colliders. We analyse hydrodynamical simulations of a universe containing self-interacting dark matter (SIDM) in which all particles interact via gravity, and dark matter particles can also scatter off each other via a massive mediator. During cluster collisions, SIDM spreads out and lags behind cluster member galaxies. Individual systems can have quirky dynamics that makes them difficult to interpret. Statistically, however, we find that the mean or median of dark matter's spatial offset in many collisions can be robustly modelled, and is independent of our viewing angle and halo mass even in collisions between unequal-mass systems. If the SIDM cross-section were σ/ m  = 0.1 cm2 g−1 = 0.18 barn GeV−1, the 'bulleticity' lag would be ∼5 per cent that of gas due to ram pressure, and could be detected at 95 per cent confidence level in weak lensing observations of ∼100 well-chosen clusters. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

13. Beyond the bulge–halo conspiracy? Density profiles of early-type galaxies from extended-source strong lensing

Author

Amy Etherington, James W Nightingale, Richard Massey, Andrew Robertson, XiaoYue Cao, Aristeidis Amvrosiadis, Shaun Cole, Carlos S Frenk, Qiuhan He, David J Lagattuta, Samuel Lange, and Ran Li

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Observations suggest that the dark matter and stars in early-type galaxies `conspire' to produce a surprisingly simple distribution of total mass, $\rho(r)\propto\rho^{-\gamma}$, with $\gamma\approx2$. We measure the distribution of mass in 48 early-type galaxies that gravitationally lens a resolved background source. By fitting the source light in every pixel of images from the Hubble Space Telescope, we find a mean $\langle\gamma\rangle=2.075_{-0.024}^{+0.023}$ with intrinsic scatter between galaxies of $\sigma_\gamma=0.172^{+0.022}_{-0.032}$ for the overall sample. This is consistent with, and has similar precision to traditional techniques that employ spectroscopic observations to supplement lensing with mass estimates from stellar dynamics. Comparing measurements of $\gamma$ for individual lenses using both techniques, we find a statistically insignificant correlation of $-0.150^{+0.223}_{-0.217}$ between the two, indicating a lack of statistical power or deviations from a power-law density in certain lenses. At fixed surface mass density, we measure a redshift dependence, $\partial\langle\gamma\rangle/\partial z=0.345^{+0.322}_{-0.296}$, that is consistent with traditional techniques for the same sample of SLACS and GALLERY lenses. Interestingly, the consistency breaks down when we measure the dependence of $\gamma$ on the surface mass density of a lens galaxy. We argue that this is tentative evidence for an inflection point in the total-mass density profile at a few times the galaxy effective radius -- breaking the conspiracy., Comment: 14 pages, 11 figures, 5 tables, submitted to MNRAS

Published
2023
Full Text
View/download PDF

14. Another shipment of six short-period giant planets from TESS

Author

Joseph E Rodriguez, Samuel N Quinn, Andrew Vanderburg, George Zhou, Jason D Eastman, Erica Thygesen, Bryson Cale, David R Ciardi, Phillip A Reed, Ryan J Oelkers, Karen A Collins, Allyson Bieryla, David W Latham, Erica J Gonzales, B Scott Gaudi, Coel Hellier, Matías I Jones, Rafael Brahm, Kirill Sokolovsky, Jack Schulte, Gregor Srdoc, John Kielkopf, Ferran Grau Horta, Bob Massey, Phil Evans, Denise C Stephens, Kim K McLeod, Nikita Chazov, Vadim Krushinsky, Mourad Ghachoui, Boris S Safonov, Cayla M Dedrick, Dennis Conti, Didier Laloum, Steven Giacalone, Carl Ziegler, Pere Guerra Serra, Ramon Naves Nogues, Felipe Murgas, Edward J Michaels, George R Ricker, Roland K Vanderspek, Sara Seager, Joshua N Winn, Jon M Jenkins, Brett Addison, Owen Alfaro, D R Anderson, Elias Aydi, Thomas G Beatty, Timothy R Bedding, Alexander A Belinski, Zouhair Benkhaldoun, Perry Berlind, Cullen H Blake, Michael J Bowen, Brendan P Bowler, Andrew W Boyle, Dalton Branson, César Briceño, Michael L Calkins, Emma Campbell, Jessie L Christiansen, Laura Chomiuk, Kevin I Collins, Matthew A Cornachione, Ahmed Daassou, Courtney D Dressing, Gilbert A Esquerdo, Dax L Feliz, William Fong, Akihiko Fukui, Tianjun Gan, Holden Gill, Maria V Goliguzova, Jarrod Hansen, Thomas Henning, Eric G Hintz, Melissa J Hobson, Jonathan Horner, Chelsea X Huang, David J James, Jacob S Jensen, Samson A Johnson, Andrés Jordán, Stephen R Kane, Khalid Barkaoui, Myung-Jin Kim, Kingsley Kim, Rudolf B Kuhn, Nicholas Law, Pablo Lewin, Hui-Gen Liu, Michael B Lund, Andrew W Mann, Nate McCrady, Matthew W Mengel, Jessica Mink, Lauren G Murphy, Norio Narita, Patrick Newman, Jack Okumura, Hugh P Osborn, Martin Paegert, Enric Palle, Joshua Pepper, Peter Plavchan, Alexander A Popov, Markus Rabus, Jessica Ranshaw, Jennifer A Rodriguez, Dong-Goo Roh, Michael A Reefe, Arjun B Savel, Richard P Schwarz, Avi Shporer, Robert J Siverd, David H Sliski, Keivan G Stassun, Daniel J Stevens, Abderahmane Soubkiou, Eric B Ting, C G Tinney, Noah Vowell, Payton Walton, R G West, Maurice L Wilson, Robert A Wittenmyer, Justin M Wittrock, Shania Wolf, Jason T Wright, Hui Zhang, and Evan Zobel

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery and characterization of six short-period, transiting giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS) -- TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), & TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9, Comment: 20 Pages, 6 Figures, 8 Tables, Accepted by MNRAS

Published
2023
Full Text
View/download PDF

17. Scanning for dark matter subhaloes in Hubble Space Telescope imaging of 54 strong lenses.

Author

Nightingale, James W, He, Qiuhan, Cao, Xiaoyue, Amvrosiadis, Aristeidis, Etherington, Amy, Frenk, Carlos S, Hayes, Richard G, Robertson, Andrew, Cole, Shaun, Lange, Samuel, Li, Ran, and Massey, Richard

Subjects
SPACE telescopes, DARK matter, GRAVITATIONAL lenses, DEGREES of freedom, GALAXIES
Abstract

The cold dark matter (DM) model predicts that every galaxy contains thousands of DM subhaloes; almost all other DM models include a physical process that smooths away the subhaloes. The subhaloes are invisible, but could be detected via strong gravitational lensing, if they lie on the line of sight to a multiply imaged background source, and perturb its apparent shape. We present a predominantly automated strong lens analysis framework, and scan for DM subhaloes in Hubble Space Telescope imaging of 54 strong lenses. We identify five DM subhalo candidates, including two especially compelling candidates (one previously known in SLACS0946 + 1006) where a subhalo is favoured after all of our tests for systematics. We find that the detectability of subhaloes depends upon the assumed parametric form for the lens galaxy's mass distribution, especially its degree of azimuthal freedom. Using separate components for DM and stellar mass reveals two DM subhalo candidates and removes four false positives compared to the single power-law mass model that is common in the literature. We identify 45 lenses without substructures, the number of which is key to statistical tests able to rule out models of, for example, warm or self-interacting DM. Our full analysis results are available at https://github.com/Jammy2211/autolens_subhalo. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

19. TESS spots a mini-neptune interior to a hot saturn in the TOI-2000 system

Author

Sha, Lizhou, primary, Vanderburg, Andrew M, additional, Huang, Chelsea X, additional, Armstrong, David J, additional, Brahm, Rafael, additional, Giacalone, Steven, additional, Wood, Mackenna L, additional, Collins, Karen A, additional, Nielsen, Louise D, additional, Hobson, Melissa J, additional, Ziegler, Carl, additional, Howell, Steve B, additional, Torres-Miranda, Pascal, additional, Mann, Andrew W, additional, Zhou, George, additional, Delgado-Mena, Elisa, additional, Rojas, Felipe I, additional, Abe, Lyu, additional, Trifonov, Trifon, additional, Adibekyan, Vardan, additional, Sousa, Sérgio G, additional, Fajardo-Acosta, Sergio B, additional, Guillot, Tristan, additional, Howard, Saburo, additional, Littlefield, Colin, additional, Hawthorn, Faith, additional, Schmider, François-Xavier, additional, Eberhardt, Jan, additional, Tan, Thiam-Guan, additional, Osborn, Ares, additional, Schwarz, Richard P, additional, Strøm, Paul, additional, Jordán, Andrés, additional, Wang, Gavin, additional, Henning, Thomas, additional, Massey, Bob, additional, Law, Nicholas, additional, Stockdale, Chris, additional, Furlan, Elise, additional, Srdoc, Gregor, additional, Wheatley, Peter J, additional, Barrado Navascués, David, additional, Lissauer, Jack J, additional, Stassun, Keivan G, additional, Ricker, George R, additional, Vanderspek, Roland K, additional, Latham, David W, additional, Winn, Joshua N, additional, Seager, Sara, additional, Jenkins, Jon M, additional, Barclay, Thomas, additional, Bouma, Luke G, additional, Christiansen, Jessie L, additional, Guerrero, Natalia, additional, and Rose, Mark E, additional

Published
2023
Full Text
View/download PDF

20. Abell 1201: detection of an ultramassive black hole in a strong gravitational lens

Author

Nightingale, J W, primary, Smith, Russell J, additional, He, Qiuhan, additional, O’Riordan, Conor M, additional, Kegerreis, Jacob A, additional, Amvrosiadis, Aristeidis, additional, Edge, Alastair C, additional, Etherington, Amy, additional, Hayes, Richard G, additional, Kelly, Ash, additional, Lucey, John R, additional, and Massey, Richard J, additional

Published
2023
Full Text
View/download PDF

22. Beyond the bulge–halo conspiracy? Density profiles of early-type galaxies from extended-source strong lensing

Author

Etherington, Amy, primary, Nightingale, James W, additional, Massey, Richard, additional, Robertson, Andrew, additional, Cao, XiaoYue, additional, Amvrosiadis, Aristeidis, additional, Cole, Shaun, additional, Frenk, Carlos S, additional, He, Qiuhan, additional, Lagattuta, David J, additional, Lange, Samuel, additional, and Li, Ran, additional

Published
2023
Full Text
View/download PDF

24. Another shipment of six short-period giant planets from TESS

Author

Rodriguez, Joseph E, primary, Quinn, Samuel N, additional, Vanderburg, Andrew, additional, Zhou, George, additional, Eastman, Jason D, additional, Thygesen, Erica, additional, Cale, Bryson, additional, Ciardi, David R, additional, Reed, Phillip A, additional, Oelkers, Ryan J, additional, Collins, Karen A, additional, Bieryla, Allyson, additional, Latham, David W, additional, Gonzales, Erica J, additional, Scott Gaudi, B, additional, Hellier, Coel, additional, Jones, Matías I, additional, Brahm, Rafael, additional, Sokolovsky, Kirill, additional, Schulte, Jack, additional, Srdoc, Gregor, additional, Kielkopf, John, additional, Grau Horta, Ferran, additional, Massey, Bob, additional, Evans, Phil, additional, Stephens, Denise C, additional, McLeod, Kim K, additional, Chazov, Nikita, additional, Krushinsky, Vadim, additional, Ghachoui, Mourad, additional, Safonov, Boris S, additional, Dedrick, Cayla M, additional, Conti, Dennis, additional, Laloum, Didier, additional, Giacalone, Steven, additional, Ziegler, Carl, additional, Guerra Serra, Pere, additional, Naves Nogues, Ramon, additional, Murgas, Felipe, additional, Michaels, Edward J, additional, Ricker, George R, additional, Vanderspek, Roland K, additional, Seager, Sara, additional, Winn, Joshua N, additional, Jenkins, Jon M, additional, Addison, Brett, additional, Alfaro, Owen, additional, Anderson, D R, additional, Aydi, Elias, additional, Beatty, Thomas G, additional, Bedding, Timothy R, additional, Belinski, Alexander A, additional, Benkhaldoun, Zouhair, additional, Berlind, Perry, additional, Blake, Cullen H, additional, Bowen, Michael J, additional, Bowler, Brendan P, additional, Boyle, Andrew W, additional, Branson, Dalton, additional, Briceño, César, additional, Calkins, Michael L, additional, Campbell, Emma, additional, Christiansen, Jessie L, additional, Chomiuk, Laura, additional, Collins, Kevin I, additional, Cornachione, Matthew A, additional, Daassou, Ahmed, additional, Dressing, Courtney D, additional, Esquerdo, Gilbert A, additional, Feliz, Dax L, additional, Fong, William, additional, Fukui, Akihiko, additional, Gan, Tianjun, additional, Gill, Holden, additional, Goliguzova, Maria V, additional, Hansen, Jarrod, additional, Henning, Thomas, additional, Hintz, Eric G, additional, Hobson, Melissa J, additional, Horner, Jonathan, additional, Huang, Chelsea X, additional, James, David J, additional, Jensen, Jacob S, additional, Johnson, Samson A, additional, Jordán, Andrés, additional, Kane, Stephen R, additional, Barkaoui, Khalid, additional, Kim, Myung-Jin, additional, Kim, Kingsley, additional, Kuhn, Rudolf B, additional, Law, Nicholas, additional, Lewin, Pablo, additional, Liu, Hui-Gen, additional, Lund, Michael B, additional, Mann, Andrew W, additional, McCrady, Nate, additional, Mengel, Matthew W, additional, Mink, Jessica, additional, Murphy, Lauren G, additional, Narita, Norio, additional, Newman, Patrick, additional, Okumura, Jack, additional, Osborn, Hugh P, additional, Paegert, Martin, additional, Palle, Enric, additional, Pepper, Joshua, additional, Plavchan, Peter, additional, Popov, Alexander A, additional, Rabus, Markus, additional, Ranshaw, Jessica, additional, Rodriguez, Jennifer A, additional, Roh, Dong-Goo, additional, Reefe, Michael A, additional, Savel, Arjun B, additional, Schwarz, Richard P, additional, Shporer, Avi, additional, Siverd, Robert J, additional, Sliski, David H, additional, Stassun, Keivan G, additional, Stevens, Daniel J, additional, Soubkiou, Abderahmane, additional, Ting, Eric B, additional, Tinney, C G, additional, Vowell, Noah, additional, Walton, Payton, additional, West, R G, additional, Wilson, Maurice L, additional, Wittenmyer, Robert A, additional, Wittrock, Justin M, additional, Wolf, Shania, additional, Wright, Jason T, additional, Zhang, Hui, additional, and Zobel, Evan, additional

Published
2023
Full Text
View/download PDF

25. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

Author

Hawthorn, Faith, primary, Bayliss, Daniel, additional, Wilson, Thomas G, additional, Bonfanti, Andrea, additional, Adibekyan, Vardan, additional, Alibert, Yann, additional, Sousa, Sérgio G, additional, Collins, Karen A, additional, Bryant, Edward M, additional, Osborn, Ares, additional, Armstrong, David J, additional, Abe, Lyu, additional, Acton, Jack S, additional, Addison, Brett C, additional, Agabi, Karim, additional, Alonso, Roi, additional, Alves, Douglas R, additional, Anglada-Escudé, Guillem, additional, Bárczy, Tamas, additional, Barclay, Thomas, additional, Barrado, David, additional, Barros, Susana C C, additional, Baumjohann, Wolfgang, additional, Bendjoya, Philippe, additional, Benz, Willy, additional, Bieryla, Allyson, additional, Bonfils, Xavier, additional, Bouchy, François, additional, Brandeker, Alexis, additional, Broeg, Christopher, additional, Brown, David J A, additional, Burleigh, Matthew R, additional, Buttu, Marco, additional, Cabrera, Juan, additional, Caldwell, Douglas A, additional, Casewell, Sarah L, additional, Charbonneau, David, additional, Charnoz, Sébastian, additional, Cloutier, Ryan, additional, Cameron, Andrew Collier, additional, Collins, Kevin I, additional, Conti, Dennis M, additional, Crouzet, Nicolas, additional, Czismadia, Szilárd, additional, Davies, Melvyn B, additional, Deleuil, Magali, additional, Delgado-Mena, Elisa, additional, Delrez, Laetitia, additional, Demangeon, Olivier D S, additional, Demory, Brice-Olivier, additional, Dransfield, Georgina, additional, Dumusque, Xavier, additional, Egger, Jo Ann, additional, Ehrenreich, David, additional, Eigmüller, Philipp, additional, Erickson, Anders, additional, Essack, Zahra, additional, Fortier, Andrea, additional, Fossati, Luca, additional, Fridlund, Malcolm, additional, Günther, Maximilian N, additional, Güdel, Manuel, additional, Gandolfi, Davide, additional, Gillard, Harvey, additional, Gillon, Michaël, additional, Gnilka, Crystal, additional, Goad, Michael R, additional, Goeke, Robert F, additional, Guillot, Tristan, additional, Hadjigeorghiou, Andreas, additional, Hellier, Coel, additional, Henderson, Beth A, additional, Heng, Kevin, additional, Hooton, Matthew J, additional, Horne, Keith, additional, Howell, Steve B, additional, Hoyer, Sergio, additional, Irwin, Jonathan M, additional, Jenkins, James S, additional, Jenkins, Jon M, additional, Jensen, Eric L N, additional, Kane, Stephen R, additional, Kendall, Alicia, additional, Kielkopf, John F, additional, Kiss, Laszlo L, additional, Lacedelli, Gaia, additional, Laskar, Jacques, additional, Latham, David W, additional, Etangs, Alain Lecavalier des, additional, Leleu, Adrien, additional, Lendl, Monika, additional, Lillo-Box, Jorge, additional, Lovis, Christophe, additional, Mékarnia, Djamel, additional, Massey, Bob, additional, Masters, Tamzin, additional, Maxted, Pierre F L, additional, Nascimbeni, Valerio, additional, Nielsen, Louise D, additional, O’Brien, Sean M, additional, Olofsson, Göran, additional, Osborn, Hugh P, additional, Pagano, Isabella, additional, Pallé, Enric, additional, Persson, Carina M, additional, Piotto, Giampaolo, additional, Plavchan, Peter, additional, Pollacco, Don, additional, Queloz, Didier, additional, Ragazzoni, Roberto, additional, Rauer, Heike, additional, Ribas, Ignasi, additional, Ricker, George, additional, Ségransan, Damien, additional, Salmon, Sébastien, additional, Santerne, Alexandre, additional, Santos, Nuno C, additional, Scandariato, Gaetano, additional, Schmider, François-Xavier, additional, Schwarz, Richard P, additional, Seager, Sara, additional, Shporer, Avi, additional, Simon, Attila E, additional, Smith, Alexis M S, additional, Srdoc, Gregor, additional, Steller, Manfred, additional, Suarez, Olga, additional, Szabó, Gyula M, additional, Teske, Johanna, additional, Thomas, Nicolas, additional, Tilbrook, Rosanna H, additional, Triaud, Amaury H M J, additional, Udry, Stéphane, additional, Van Grootel, Valérie, additional, Walton, Nicholas, additional, Wang, Sharon X, additional, Wheatley, Peter J, additional, Winn, Joshua N, additional, Wittenmyer, Robert A, additional, and Zhang, Hui, additional

Published
2023
Full Text
View/download PDF

28. Dealing with density discontinuities in planetary SPH simulations

Author

Josh Borrow, Thomas Sandnes, Luis Teodoro, Sergio Ruiz-Bonilla, Vincent Eke, Jacob Kegerreis, and Richard Massey

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Computational Physics (physics.comp-ph), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics - Computational Physics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Density discontinuities cannot be precisely modelled in standard formulations of smoothed particles hydrodynamics (SPH) because the density field is defined smoothly as a kernel-weighted sum of neighbouring particle masses. This is a problem when performing simulations of giant impacts between proto-planets, for example, because planets typically do have density discontinuities both at their surfaces and at any internal boundaries between different materials. The inappropriate densities in these regions create artificial forces that effectively suppress mixing between particles of different material and, as a consequence, this problem introduces a key unknown systematic error into studies that rely on SPH simulations. In this work we present a novel, computationally cheap method that deals simultaneously with both of these types of density discontinuity in SPH simulations. We perform standard hydrodynamical tests and several example giant impact simulations, and compare the results with standard SPH. In a simulated Moon-forming impact using $10^7$ particles, the improved treatment at boundaries affects at least 30% of the particles at some point during the simulation., 9 pages, 8 figures. Submitted to MNRAS

Published
2022
Full Text
View/download PDF

29. Weak gravitational lensing shear measurement with FPFS: analytical mitigation of noise bias and selection bias

Author

Xiangchong Li, Yin Li, and Richard Massey

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dedicated 'Stage IV' observatories will soon observe the entire extragalactic sky, to measure the 'cosmic shear' distortion of galaxy shapes by weak gravitational lensing. To measure the apparent shapes of those galaxies, we present an improved version of the Fourier Power Function Shapelets (FPFS) shear measurement method. This now includes analytic corrections for sources of bias that plague all shape measurement algorithms: including noise bias (due to noise in nonlinear combinations of observable quantities) and selection bias (due to sheared galaxies being more or less likely to be detected). Crucially, these analytic solutions do not rely on calibration from external image simulations. For isolated galaxies, the small residual $\sim$$10^{-3}$ multiplicative bias and $\lesssim$$10^{-4}$ additive bias now meet science requirements for Stage IV experiments. FPFS also works accurately for faint galaxies and robustly against stellar contamination. Future work will focus on deblending overlapping galaxies. The code used for this paper can process $>$$1000$ galaxy images per CPU second and is available from https://github.com/mr-superonion/FPFS., 12 pages, 8 figures, 3 tables; MNRAS (in press)

Published
2022
Full Text
View/download PDF

30. Discovering gravitationally lensed gravitational waves: predicted rates, candidate selection, and localization with the Vera Rubin Observatory

Author

Graham P Smith, Andrew Robertson, Guillaume Mahler, Matt Nicholl, Dan Ryczanowski, Matteo Bianconi, Keren Sharon, Richard Massey, Johan Richard, Mathilde Jauzac, HEP, INSPIRE, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
neutron star: binary, catastrophe theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), mass: gap, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, localization, dark matter: halo, gravitation: lens, black hole, general relativity, structure, detector: optical, Astrophysics::Galaxy Astrophysics, halo: mass, High Energy Astrophysical Phenomena (astro-ph.HE), gravitational radiation, Astronomy and Astrophysics, moment, observatory, Space and Planetary Science, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Secure confirmation that a gravitational wave (GW) has been gravitationally lensed would bring together these two pillars of General Relativity for the first time. This breakthrough is challenging for many reasons, including: GW sky localization uncertainties dwarf the angular scale of gravitational lensing, the mass and structure of gravitational lenses is diverse, the mass function of stellar remnant compact objects is not yet well constrained, and GW detectors do not operate continuously. We introduce a new approach that is agnostic to the mass and structure of the lenses, compare the efficiency of different methods for lensed GW discovery, and explore detection of lensed kilonova counterparts as a direct method for localising candidates. Our main conclusions are: (1) lensed neutron star mergers (NS-NS) are magnified into the "mass gap" between NS and black holes, therefore selecting candidates from public GW alerts with high mass gap probability is efficient, (2) the rate of detectable lensed NS-NS will approach one per year in the mid-2020s, (3) the arrival time difference between lensed NS-NS images is $1\,\rm sec\lesssim\Delta t\lesssim1\,year$, and thus well-matched to the operations of GW detectors and optical telescopes, (4) lensed kilonova counterparts are faint at peak (e.g.\ $r_{\rm AB}\simeq24-26$ in the mid-2020s), fade quickly ($d, Comment: Accepted by MNRAS. 20 pages, 10 figures

Published
2023
Full Text
View/download PDF

31. Fundamental parameters of the massive eclipsing binary HM1 8

Author

Rodolfo H. Barbá, Philip Massey, Roberto Claudio Gamen, Omar Gustavo Benvenuto, G. Ferrero, Nidia Morrell, C. Rodriguez, and José Ignacio Arias

Subjects
Physics, Orbital elements, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, Light curve, Spectral line, Orbital inclination, Stars, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Spectroscopy, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present a comprehensive study of the massive binary system HM1~8, based on multi-epoch high resolution spectroscopy, $V$-band photometry and archival X-ray data. Spectra from the OWN Survey, a high resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5~IV(f) and O9.7~V, respectively. From a radial-velocity (RV) study we derived a set of orbital parameters for the system. We found an eccentric orbit ($e=0.14 \pm 0.01$) with a period of $P = 5.87820 \pm 0.00008$~days. Through the simultaneous analysis of the RVs and the $V$-band light curve we derived an orbital inclination of $70.0^{\circ} \pm 2.0$ and stellar masses of $M_a=33.6^{+1.4}_{-1.2}~\text{M}_{\sun}$ for the primary, and $M_b=17.7^{+0.5}_{-0.7}~\text{M}_{\sun}$ for the secondary. The components show projected rotational velocities $v_1\sin{i}=105 \pm 14~\text{km~s}^{-1}$ and $v_2\sin{i}=82 \pm 15~\text{km~s}^{-1}$, respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region, therefore the X-ray emission is attributed to stellar winds., Comment: 15 pages, 15 figures, to be published in MNRAS

Published
2021
Full Text
View/download PDF

32. Euclid: the selection of quiescent and star-forming galaxies using observed colours

Author

F. J. Castander, Rafael Toledo-Moreo, L. Bisigello, Marc Sauvage, M. Poncet, Ulrike Kuchner, H. Israel, R. Cledassou, S. Kermiche, Crescenzo Tortora, F. Sureau, Sebastiano Ligori, R. Kohley, Sandrine Pires, Jarle Brinchmann, Mauro Roncarelli, Michele Moresco, G. Zamorani, Andy Taylor, G. Meylan, Andrea Cimatti, Natalia Auricchio, J. Carretero, B. Kubik, M. Wetzstein, Lucia Pozzetti, Thomas D. Kitching, Felix Hormuth, Stefano Andreon, E. Franceschi, Claudia Maraston, M. Bolzonella, Roberto P. Saglia, Martin Kunz, Simona Mei, D. Masters, M. Frailis, Andrew Humphrey, Leonardo Corcione, A. Secroun, Mark Cropper, Ismael Tereno, G. Polenta, V. Capobianco, Jason Rhodes, L. Valenziano, Ivan Lloro, S. Serrano, Peter Schneider, Elisabetta Maiorano, L. Conversi, Fabio Pasian, Ole Marggraf, G. Congedo, P. B. Lilje, S. Dusini, S. Paltani, Y. Mellier, Valeria Pettorino, P. Franzetti, C. J. Conselice, F. Raison, B. Garilli, Yu Wang, Marco Castellano, M. Fumana, O. Le Fevre, Richard Massey, Knud Jahnke, Pierre-Alain Duc, Stefano Cavuoti, Emanuel Rossetti, C. Padilla, Julien Zoubian, Zoubian, J, Wetzstein, M, Wang, Y, Valenziano, L, Toledo-Moreo, R, Tereno, I, Taylor, A N, Sureau, F, Serrano, S, Secroun, A, Schneider, P, Sauvage, M, Saglia, R, Rossetti, E, Roncarelli, M, Rhodes, J, Raison, F, Poncet, M, Polenta, G, Pires, S, Pettorino, V, Pasian, F, Paltani, S, Padilla, C, Meylan, G, Mellier, Y, Mei, S, Masters, D C, Massey, R, Marggraf, O, Maiorano, E, Lloro, I, Lilje, P B, Ligori, S, Le Fèvre, O, Kunz, M, Kubik, B, Kohley, R, Kitching, T, Kermiche, S, Jahnke, K, Israel, H, Hormuth, F, Fumana, M, Franzetti, P, Franceschi, E, Frailis, M, Dusini, S, Cropper, M S, Corcione, L, Conversi, L, Congedo, G, Cledassou, R, Cimatti, A, Cavuoti, S, Castellano, M, Castander, F J, Carretero, J, Capobianco, V, Brinchmann, J, Auricchio, N, Zamorani, G, Tortora, C, Pozzetti, L, Moresco, M, Maraston, C, Humphrey, A, Garilli, B, Duc, P-A, Bolzonella, M, Andreon, S, Conselice, C J, Kuchner, U, Bisigello, L, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
photometric redshifts, challenge lightcone simulation, Sample (material), FOS: Physical sciences, Astrophysics, Star (graph theory), 01 natural sciences, law.invention, Telescope, environmental dependence, law, 0103 physical sciences, Galaxy formation and evolution, formation rates, luminosity function, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, legacy survey, evolution survey cosmos, Astrophysics - Astrophysics of Galaxies, galaxies: general, red sequence, Galaxy, Redshift, galaxies: photometry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), magnitude distribution, stellar mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution
Abstract

The Euclid mission will observe well over a billion galaxies out to $z\sim6$ and beyond. This will offer an unrivalled opportunity to investigate several key questions for understanding galaxy formation and evolution. The first step for many of these studies will be the selection of a sample of quiescent and star-forming galaxies, as is often done in the literature by using well known colour techniques such as the `UVJ' diagram. However, given the limited number of filters available for the Euclid telescope, the recovery of such rest-frame colours will be challenging. We therefore investigate the use of observed Euclid colours, on their own and together with ground-based u-band observations, for selecting quiescent and star-forming galaxies. The most efficient colour combination, among the ones tested in this work, consists of the (u-VIS) and (VIS-J) colours. We find that this combination allows users to select a sample of quiescent galaxies complete to above $\sim70\%$ and with less than 15$\%$ contamination at redshifts in the range $0.7565\%$ completeness level and contamination below 20$\%$ at $1, Comment: 19 pages, 15 figures, 5 tables, accepted for publication in MNRAS

Published
2020
Full Text
View/download PDF

33. Assessing the sources of reionization: a spectroscopic case study of a 30× lensed galaxy at z ∼ 5 with Lyα, C <scp>iv</scp>, Mg <scp>ii</scp>, and [Ne <scp>iii</scp>]

Author

Mark Swinbank, Nicolas Laporte, Mirko Curti, Johan Richard, Richard Massey, Roberto Maiolino, Renske Smit, Joris Witstok, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Active galactic nucleus, Metallicity, first stars, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, dark ages, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, Redshift, Gravitational lens, [SDU]Sciences of the Universe [physics], Space and Planetary Science, reionization, methods: observational, Equivalent width, techniques: spectroscopic
Abstract

We present a detailed spectroscopic analysis of a galaxy at z ≃ 4.88 that is, by chance, magnified ∼30× by gravitational lensing. Only three sources at z ≳ 5 are known with such high magnification. This particular source has been shown to exhibit widespread, high equivalent width ${{\rm C\, \small {IV}}}\ \lambda 1549\, \mathring{\rm A}$ emission, implying it is a unique example of a metal-poor galaxy with a hard radiation field, likely representing the galaxy population responsible for cosmic reionization. Using ultraviolet (UV) nebular line ratio diagnostics, Very Large Telescope (VLT)/X-shooter observations rule out strong active galactic nuclei (AGN) activity, indicating a stellar origin of the hard radiation field instead. We present a new detection of ${[{\rm Ne\, \small {III}}]}\ \lambda 3870\, \mathring{\rm A}$ and use the [${\rm Ne\, \small {III}}$]/[${\rm O\, \small {II}}$] line ratio to constrain the ionization parameter and gas-phase metallicity. Closely related to the commonly used [${\rm O\, \small {III}}$]/[${\rm O\, \small {II}}$] ratio, our [${\rm Ne\, \small {III}}$]/[${\rm O\, \small {II}}$] measurement shows this source is similar to local ‘Green Pea’ galaxies and Lyman-continuum leakers. It furthermore suggests this galaxy is more metal poor than expected from the fundamental metallicity relation, possibly as a consequence of excess gas accretion diluting the metallicity. Finally, we present the highest redshift detection of ${{\rm Mg\, \small {II}}}\ \lambda 2796\, \mathring{\rm A}$, observed at high equivalent width in emission, in contrast to more evolved systems predominantly exhibiting ${\rm Mg\, \small {II}}$ absorption. Strong ${\rm Mg\, \small {II}}$ emission has been observed in most z ∼ 0 Lyman-continuum leakers known and has recently been proposed as an indirect tracer of escaping ionizing radiation. In conclusion, this strongly lensed galaxy, observed just $300\, \mathrm{Myr}$ after reionization ends, enables testing of observational diagnostics proposed to constrain the physical properties of distant galaxies in the James Webb Space Telescope (JWST)/Extremely Large Telescope (ELT) era.

Published
2021
Full Text
View/download PDF

34. Testing strong lensing subhalo detection with a cosmological simulation

Author

He, Qiuhan, primary, Nightingale, James, additional, Robertson, Andrew, additional, Amvrosiadis, Aristeidis, additional, Cole, Shaun, additional, Frenk, Carlos S, additional, Massey, Richard, additional, Li, Ran, additional, Amorisco, Nicola C, additional, Metcalf, R Benton, additional, Cao, Xiaoyue, additional, and Etherington, Amy, additional

Published
2022
Full Text
View/download PDF

35. Automated galaxy–galaxy strong lens modelling: No lens left behind

Author

Etherington, Amy, primary, Nightingale, James W, additional, Massey, Richard, additional, Cao, XiaoYue, additional, Robertson, Andrew, additional, Amorisco, Nicola C, additional, Amvrosiadis, Aristeidis, additional, Cole, Shaun, additional, Frenk, Carlos S, additional, He, Qiuhan, additional, Li, Ran, additional, and Tam, Sut-Ieng, additional

Published
2022
Full Text
View/download PDF

36. Pilot-WINGS: An extended MUSE view of the structure of Abell 370

Author

Lagattuta, David J, primary, Richard, Johan, additional, Bauer, Franz Erik, additional, Cerny, Catherine, additional, Claeyssens, Adélaïde, additional, Guaita, Lucia, additional, Jauzac, Mathilde, additional, Jeanneau, Alexandre, additional, Koekemoer, Anton M, additional, Mahler, Guillaume, additional, Prieto Lyon, Gonzalo, additional, Acebron, Ana, additional, Meneghetti, Massimo, additional, Niemiec, Anna, additional, Zitrin, Adi, additional, Bianconi, Matteo, additional, Connor, Thomas, additional, Cen, Renyue, additional, Edge, Alastair, additional, Faisst, Andreas L, additional, Limousin, Marceau, additional, Massey, Richard, additional, Sereno, Mauro, additional, Sharon, Keren, additional, and Weaver, John R, additional

Published
2022
Full Text
View/download PDF

37. What does strong gravitational lensing? The mass and redshift distribution of high-magnification lenses

Author

Dan Ryczanowski, Graham P. Smith, Matteo Bianconi, Vincent R. Eke, Richard Massey, Mathilde Jauzac, and Andrew Robertson

Subjects
Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, Population, Strong gravitational lensing, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, law.invention, Lens (optics), Gravitational lens, 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, Halo, 010306 general physics, education, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Many distant objects can only be detected, or become more scientifically valuable, if they have been highly magnified by strong gravitational lensing. We use EAGLE and BAHAMAS, two recent cosmological hydrodynamical simulations, to predict the probability distribution for both the lens mass and lens redshift when point sources are highly magnified by gravitational lensing. For sources at a redshift of two, we find the distribution of lens redshifts to be broad, peaking at z=0.6. The contribution of different lens masses is also fairly broad, with most high-magnification lensing due to lenses with halo masses between 10^12 and 10^14 solar masses. Lower mass haloes are inefficient lenses, while more massive haloes are rare. We find that a simple model in which all haloes have singular isothermal sphere density profiles can approximately reproduce the simulation predictions, although such a model over-predicts the importance of haloes with mass, 15 pages, 5 figures, updated to match MNRAS version

Published
2020
Full Text
View/download PDF

38. On building a cluster watchlist for identifying strongly lensed supernovae, gravitational waves and kilonovae

Author

Dan Ryczanowski, Graham P. Smith, Matteo Bianconi, Andrew Robertson, Mathilde Jauzac, and Richard Massey

Subjects
Physics, 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Lower limit, Galaxy, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Magnitude (astronomy), Dark energy, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Motivated by discovering strongly-lensed supernovae, gravitational waves, and kilonovae in the 2020s, we investigate whether to build a watch-list of clusters based on observed cluster properties (i.e. lens-plane selection) or on the detectability of strongly-lensed background galaxies (i.e. source-plane selection). First, we estimate the fraction of high-redshift transient progenitors that reside in galaxies that are themselves too faint to be detected as being strongly-lensed. We find $\sim15-50$ per cent of transient progenitors reside in $z = 1-2$ galaxies too faint to be detected in surveys that reach ${\rm AB}\simeq23$, such as the Dark Energy Survey. This falls to $\ls10$ per cent at depths that will be probed by early data releases of LSST (${\rm AB}\simeq25$). Second, we estimate a conservative lower limit on the fraction of strong lensing clusters that will be missed by magnitude limited searches for multiply-imaged galaxies and giant arcs due to the faintness of such images. We find that DES-like surveys will miss $\sim75$ per cent of $10^{15}$M$_\odot$ strong lensing clusters, rising to $\sim100$ per cent of $10^{14}$M$_\odot$ clusters. Deeper surveys, such as LSST, will miss $\sim40$ per cent at $10^{15}$M$_\odot$, and $\sim95$ per cent at $10^{14}$M$_\odot$. Our results motivate building a cluster watch-list for strongly-lensed transients that includes those found by lens-plane selection., Comment: 7 pages, 2 figures. MNRAS, accepted

Published
2020
Full Text
View/download PDF

39. The effects of self-interacting dark matter on the stripping of galaxies that fall into clusters

Author

Ellen L Sirks, Kyle A Oman, Andrew Robertson, Richard Massey, and Carlos Frenk

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use the Cluster-EAGLE (c-eagle) hydrodynamical simulations to investigate the effects of self-interacting dark matter (SIDM) on galaxies as they fall into clusters. We find that SIDM galaxies follow similar orbits to their cold dark matter (CDM) counterparts, but end up with ∼25 per cent less mass by the present day. One in three SIDM galaxies is entirely disrupted, compared to one in five CDM galaxies. However, the excess stripping will be harder to observe than suggested by previous DM-only simulations because the most stripped galaxies form cores and also lose stars: The most discriminating objects become unobservable. The best test will be to measure the stellar-to-halo mass relation (SHMR) for galaxies with stellar mass $10^{10}\!-\!10^{11}\, \mathrm{M}_{\odot }$. This is 8 times higher in a cluster than in the field for a CDM universe, but 13 times higher for an SIDM universe. Given intrinsic scatter in the SHMR, these models could be distinguished with noise-free galaxy–galaxy strong lensing of ∼32 cluster galaxies.

Published
2022
Full Text
View/download PDF

45. Testing strong lensing subhalo detection with a cosmological simulation.

Author

He, Qiuhan, Nightingale, James, Robertson, Andrew, Amvrosiadis, Aristeidis, Cole, Shaun, Frenk, Carlos S, Massey, Richard, Li, Ran, Amorisco, Nicola C, Metcalf, R Benton, Cao, Xiaoyue, and Etherington, Amy

Subjects
GRAVITATIONAL lenses, HYPERGEOMETRIC series, DARK matter, GAUSSIAN distribution, GALACTIC halos, GALAXIES, GALAXY clusters
Abstract

Strong gravitational lensing offers a compelling test of the cold dark matter paradigm, as it allows for subhaloes with masses of ∼109 M⊙ and below to be detected. We test commonly used techniques for detecting subhaloes superposed in images of strongly lensed galaxies. For the lens we take a simulated galaxy in a ∼1013 M⊙ halo grown in a high-resolution cosmological hydrodynamical simulation, which we view from two different directions. Though the resolution is high, we note the simulated galaxy still has an artificial core which adds additional complexity to the baryon dominated region. To remove particle noise, we represent the projected galaxy mass distribution by a series of Gaussian profiles which precisely capture the features of the projected galaxy. We first model the lens mass as a (broken) power-law density profile and then search for small haloes. Of the two projections, one has a regular elliptical shape, while the other has distinct deviations from an elliptical shape. For the former, the broken power-law model gives no false positives and correctly recovers the mass of the superposed small halo; however, for the latter we find false positives and the inferred halo mass is overestimated by ∼4–5 times. We then use a more complex model in which the lens mass is decomposed into stellar and dark matter components. In this case, we show that we can capture the simulated galaxy's complex projected structures and correctly infer the input small halo. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

48. Planetary giant impacts: convergence of high-resolution simulations using efficient spherical initial conditions and swift

Author

Vincent R. Eke, Pedro Gonnet, Matthieu Schaller, Richard Massey, J. A. Kegerreis, D. G. Korycansky, and L. F. A. Teodoro

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Particle number, Uranus, FOS: Physical sciences, Astronomy and Astrophysics, Escape velocity, Computational Physics (physics.comp-ph), 01 natural sciences, Spherical shell, Computational physics, Smoothed-particle hydrodynamics, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Roche limit, Particle, Astrophysics::Earth and Planetary Astrophysics, Physics - Computational Physics, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

We perform simulations of giant impacts onto the young Uranus using smoothed particle hydrodynamics (SPH) with over 100 million particles. This 100--1000$\times$ improvement in particle number reveals that simulations with below 10^7 particles fail to converge on even bulk properties like the post-impact rotation period, or on the detailed erosion of the atmosphere. Higher resolutions appear to determine these large-scale results reliably, but even 10^8 particles may not be sufficient to study the detailed composition of the debris -- finding that almost an order of magnitude more rock is ejected beyond the Roche radius than with 10^5 particles. We present two software developments that enable this increase in the feasible number of particles. First, we present an algorithm to place any number of particles in a spherical shell such that they all have an SPH density within 1% of the desired value. Particles in model planets built from these nested shells have a root-mean-squared velocity below 1% of the escape speed, which avoids the need for long precursor simulations to produce relaxed initial conditions. Second, we develop the hydrodynamics code SWIFT for planetary simulations. SWIFT uses task-based parallelism and other modern algorithmic approaches to take full advantage of contemporary supercomputer architectures. Both the particle placement code and SWIFT are publicly released., Fixed typo in Appx B equation and updated urls

Published
2019
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results