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Martin Bureau

Professor of Astrophysics

Research theme

  • Astronomy and astrophysics

Sub department

  • Astrophysics

Research groups

  • Galaxy formation and evolution
  • Hintze Centre for Astrophysical Surveys
martin.bureau@physics.ox.ac.uk
Telephone: 01865 (2)73377
Denys Wilkinson Building, room 701
Home page
ORCID
  • About
  • Publications

The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 259:2 (2022) ARTN 35

Authors:

Abdurro'uf, Katherine Accetta, Conny Aerts, Victor Silva Aguirre, Romina Ahumada, Nikhil Ajgaonkar, N Filiz Ak, Shadab Alam, Carlos Allende Prieto, Andres Almeida, Friedrich Anders, Scott F Anderson, Brett H Andrews, Borja Anguiano, Erik Aquino-Ortiz, Alfonso Aragon-Salamanca, Maria Argudo-Fernandez, Metin Ata, Marie Aubert, Vladimir Avila-Reese, Carles Badenes, Rodolfo H Barba, Kat Barger, Jorge K Barrera-Ballesteros, Rachael L Beaton, Timothy C Beers, Francesco Belfiore, Chad F Bender, Mariangela Bernardi, Matthew A Bershady, Florian Beutler, Christian Moni Bidin, Jonathan C Bird, Dmitry Bizyaev, Guillermo A Blanc, Michael R Blanton, Nicholas Fraser Boardman, Adam S Bolton, Mederic Boquien, Jura Borissova, Jo Bovy, WN Brandt, Jordan Brown, Joel R Brownstein, Marcella Brusa, Johannes Buchner, Kevin Bundy, Joseph N Burchett, Martin Bureau, Adam Burgasser, Tuesday K Cabang, Stephanie Campbell, Michele Cappellari, Joleen K Carlberg, Fabio Carneiro Wanderley, Ricardo Carrera, Jennifer Cash, Yan-Ping Chen, Wei-Huai Chen, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S Drew Chojnowski, Haeun Chung, Nicolas Clerc, Roger E Cohen, Julia M Comerford, Johan Comparat, Luiz da Costa, Kevin Covey, Jeffrey D Crane, Irene Cruz-Gonzalez, Connor Culhane, Katia Cunha, Y Sophia Dai, Guillermo Damke, Jeremy Darling, Davidson James W Jr, Roger Davies, Kyle Dawson, Nathan De Lee, Aleksandar M Diamond-Stanic, Mariana Cano-Diaz, Helena Dominguez Sanchez, John Donor, Chris Duckworth, Tom Dwelly, Daniel J Eisenstein, Yvonne P Elsworth, Eric Emsellem, Mike Eracleous, Stephanie Escoffier, Xiaohui Fan, Emily Farr, Shuai Feng, Jose G Fernandez-Trincado, Diane Feuillet, Andreas Filipp, Sean P Fillingham, Peter M Frinchaboy, Sebastien Fromenteau, Lluis Galbany, Rafael A Garcia, DA Garcia-Hernandez, Junqiang Ge, Doug Geisler, Joseph Gelfand, Tobias Geron, Benjamin J Gibson, Julian Goddy, Diego Godoy-Rivera, Kathleen Grabowski, Paul J Green, Michael Greener, Catherine J Grier, Emily Griffith, Hong Guo, Julien Guy, Massinissa Hadjara, Paul Harding, Sten Hasselquist, Christian R Hayes, Fred Hearty, Lewis Hill, David W Hogg, Jon A Holtzman, Danny Horta, Bau-Ching Hsieh, Chin-Hao Hsu, Yun-Hsin Hsu, Daniel Huber, Marc Huertas-Company, Brian Hutchinson, Ho Seong Hwang, Hector J Ibarra-Medel, Jacob Ider Chitham, Gabriele S Ilha, Julie Imig, Will Jaekle, Tharindu Jayasinghe, Xihan Ji, Jennifer A Johnson, Amy Jones, Henrik Jonsson, Ivan Katkov, Arman Khalatyan, Karen Kinemuchi, Shobhit Kisku, Johan H Knapen, Jean-Paul Kneib, Juna A Kollmeier, Miranda Kong, Marina Kounkel, Kathryn Kreckel, Dhanesh Krishnarao, Ivan Lacerna, Richard R Lane, Rachel Langgin, Ramon Lavender, David R Law, Daniel Lazarz, Henry W Leung, Ho-Hin Leung, Hannah M Lewis, Cheng Li, Ran Li, Jianhui Lian, Fu-Heng Liang, Lihwai Lin, Yen-Ting Lin, Sicheng Lin, Chris Lintott, Dan Long, Penelope Longa-Pena, Carlos Lopez-Coba, Shengdong Lu, Britt F Lundgren, Yuanze Luo, J Ted Mackereth, Axel de la Macorra, Suvrath Mahadevan, Steven R Majewski, Arturo Manchado, Travis Mandeville, Claudia Maraston, Berta Margalef-Bentabol, Thomas Masseron, Karen L Masters, Savita Mathur, Richard M McDermid, Myles Mckay, Andrea Merloni, Michael Merrifield, Szabolcs Meszaros, Andrea Miglio, Francesco Di Mille, Dante Minniti, Rebecca Minsley, Antonela Monachesi, Jeongin Moon, Benoit Mosser, John Mulchaey, Demitri Muna, Ricardo R Munoz, Adam D Myers, Natalie Myers, Seshadri Nadathur, Preethi Nair, Kirpal Nandra, Justus Neumann, Jeffrey A Newman, David L Nidever, Farnik Nikakhtar, Christian Nitschelm, Julia E O'Connell, Luis Garma-Oehmichen, Gabriel Luan Souza de Oliveira, Richard Olney, Daniel Oravetz, Mario Ortigoza-Urdaneta, Yeisson Osorio, Justin Otter, Zachary J Pace, Nelson Padilla, Kaike Pan, Hsi-An Pan, Taniya Parikh, James Parker, Sebastien Peirani, Karla Pena Ramirez, Samantha Penny, Will J Percival, Ismael Perez-Fournon, Marc Pinsonneault, Frederick Poidevin, Vijith Jacob Poovelil, Adrian M Price-Whelan, Anna Barbara de Andrade Queiroz, M Jordan Raddick, Amy Ray, Sandro Barboza Rembold, Nicole Riddle, Rogemar A Riffel, Rogerio Riffel, Hans-Walter Rix, Annie C Robin, Aldo Rodriguez-Puebla, Alexandre Roman-Lopes, Carlos Roman-Zuniga, Benjamin Rose, Ashley J Ross, Graziano Rossi, Kate HR Rubin, Mara Salvato, Sebastian F Sanchez, Jose R Sanchez-Gallego, Robyn Sanderson, Felipe Antonio Santana Rojas, Edgar Sarceno, Regina Sarmiento, Conor Sayres, Elizaveta Sazonova, Adam L Schaefer, Ricardo Schiavon, David J Schlegel, Donald P Schneider, Mathias Schultheis, Axel Schwope, Aldo Serenelli, Javier Serna, Zhengyi Shao, Griffin Shapiro, Anubhav Sharma, Yue Shen, Matthew Shetrone, Yiping Shu, Joshua D Simon, MF Skrutskie, Rebecca Smethurst, Verne Smith, Jennifer Sobeck, Taylor Spoo, Dani Sprague, David V Stark, Keivan G Stassun, Matthias Steinmetz, Dennis Stello, Alexander Stone-Martinez, Thaisa Storchi-Bergmann, Guy S Stringfellow, Amelia Stutz, Yung-Chau Su, Manuchehr Taghizadeh-Popp, Michael S Talbot, Jamie Tayar, Eduardo Telles, Johanna Teske, Ani Thakar, Christopher Theissen, Andrew Tkachenko, Daniel Thomas, Rita Tojeiro, Hector Hernandez Toledo, Nicholas W Troup, Jonathan R Trump, James Trussler, Jacqueline Turner, Sarah Tuttle, Eduardo Unda-Sanzana, Jose Antonio Vazquez-Mata, Marica Valentini, Octavio Valenzuela, Jaime Vargas-Gonzalez, Mariana Vargas-Magana, Pablo Vera Alfaro, Sandro Villanova, Fiorenzo Vincenzo, David Wake, Jack T Warfield, Jessica Diane Washington, Benjamin Alan Weaver, Anne-Marie Weijmans, David H Weinberg, Achim Weiss, Kyle B Westfall, Vivienne Wild, Matthew C Wilde, John C Wilson, Robert F Wilson, Mikayla Wilson, Julien Wolf, WM Wood-Vasey, Renbin Yan, Olga Zamora, Gail Zasowski, Kai Zhang, Cheng Zhao, Zheng Zheng, Zheng Zheng, Kai Zhu
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WISDOM Project - X. The morphology of the molecular ISM in galaxy centres and its dependence on galaxy structure

Monthly Notices of the Royal Astronomical Society Oxford University Press (2022)

Authors:

Timothy A Davis, Jindra Gensior, Martin Bureau, Michele Cappellari, Woorak Choi, Jacob S Elford, JM Diederik Kruijssen, Federico Lelli, Fu-Heng Liang, Lijie Liu, Ilaria Ruffa, Toshiki Saito, Marc Sarzi, Andreas Schruba, Thomas G Williams

Abstract:

We use high-resolution maps of the molecular interstellar medium (ISM) in the centres of eighty-six nearby galaxies from the millimetre-Wave Interferometric Survey of Dark Object Masses (WISDOM) and Physics at High Angular Resolution in Nearby GalaxieS (PHANGS) surveys to investigate the physical mechanisms setting the morphology of the ISM at molecular cloud scales. We show that early-type galaxies tend to have smooth, regular molecular gas morphologies, while the ISM in spiral galaxy bulges is much more asymmetric and clumpy when observed at the same spatial scales. We quantify these differences using non-parametric morphology measures (Asymmetry, Smoothness and Gini), and compare these measurements with those extracted from idealised galaxy simulations. We show that the morphology of the molecular ISM changes systematically as a function of various large scale galaxy parameters, including galaxy morphological type, stellar mass, stellar velocity dispersion, effective stellar mass surface density, molecular gas surface density, star formation efficiency and the presence of a bar. We perform a statistical analysis to determine which of these correlated parameters best predicts the morphology of the ISM. We find the effective stellar mass surface (or volume) density to be the strongest predictor of the morphology of the molecular gas, while star formation and bars maybe be important secondary drivers. We find that gas self-gravity is not the dominant process shaping the morphology of the molecular gas in galaxy centres. Instead effects caused by the depth of the potential well such as shear, suppression of stellar spiral density waves and/or inflow affect the ability of the gas to fragment.
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The AGN fuelling/feedback cycle in nearby radio galaxies – IV. Molecular gas conditions and jet–ISM interaction in NGC 3100

Monthly Notices of the Royal Astronomical Society Oxford University Press 510:3 (2021) 4485-4503

Authors:

Ilaria Ruffa, Isabella Prandoni, Timothy A Davis, Robert A Laing, Rosita Paladino, Viviana Casasola, Paola Parma, Martin Bureau

Abstract:

This is the fourth paper of a series investigating the AGN fuelling/feedback processes in a sample of 11 nearby low-excitation radio galaxies (LERGs). In this paper, we present follow-up Atacama Large Millimeter/submillimeter Array (ALMA) observations of one source, NGC 3100, targeting the 12CO(1-0), 12CO(3-2), HCO+(4-3), SiO(3-2), and HNCO(6-5) molecular transitions. 12CO(1-0) and 12CO(3-2) lines are nicely detected and complement our previous 12CO(2-1) data. By comparing the relative strength of these three CO transitions, we find extreme gas excitation conditions (i.e. Tex ≳ 50 K) in regions that are spatially correlated with the radio lobes, supporting the case for a jet–ISM interaction. An accurate study of the CO kinematics demonstrates that although the bulk of the gas is regularly rotating, two distinct non-rotational kinematic components can be identified in the inner gas regions: one can be associated to inflow/outflow streaming motions induced by a two-armed spiral perturbation; the second one is consistent with a jet-induced outflow with vmax ≈ 200 km s−1 and $\dot{M}\lesssim 0.12$ M⊙ yr−1. These values indicate that the jet-CO coupling ongoing in NGC 3100 is only mildly affecting the gas kinematics, as opposed to what expected from existing simulations and other observational studies of (sub-)kpc scale jet–cold gas interactions. HCO+(4-3) emission is tentatively detected in a small area adjacent to the base of the northern radio lobe, possibly tracing a region of jet-induced gas compression. The SiO(3-2) and HNCO(6-5) shock tracers are undetected: this – along with the tentative HCO+(4-3) detection – may be consistent with a deficiency of very dense (i.e. ncrit > 106 cm−3) cold gas in the central regions of NGC 3100.
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The HASHTAG Project: the first submillimeter images of the Andromeda galaxy from the ground

Astrophysical Journal Supplement IOP Science 257 (2021) 52

Authors:

Martin Bureau, Dimitra Rigopoulou

Abstract:

Observing nearby galaxies with submillimeter telescopes on the ground has two major challenges. First, the brightness is significantly reduced at long submillimeter wavelengths compared to the brightness at the peak of the dust emission. Second, it is necessary to use a high-pass spatial filter to remove atmospheric noise on large angular scales, which has the unwelcome by-product of also removing the galaxy’s large-scale structure. We have developed a technique for producing high-resolution submillimeter images of galaxies of large angular size by using the telescope on the ground to determine the small-scale structure (the large Fourier components) and a space telescope (Herschel or Planck) to determine the large-scale structure (the small Fourier components). Using this technique, we are carrying out the HARP and SCUBA-2 High Resolution Terahertz Andromeda Galaxy Survey (HASHTAG), an international Large Program on the James Clerk Maxwell Telescope, with one aim being to produce the first high-fidelity high-resolution submillimeter images of Andromeda. In this paper, we describe the survey, the method we have developed for combining the space-based and ground-based data, and present the first HASHTAG images of Andromeda at 450 and 850 µm. We also have created a method to predict the CO(J=3–2) line flux across M 31, which contaminates the 850 µm band. We find that while normally the contamination is below our sensitivity limit, the contamination can be significant (up to 28%) in a few of the brightest regions of the 10 kpc ring. We therefore also provide images with the predicted line emission removed.
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Cross-checking SMBH mass estimates in NGC 6958 – I. Stellar dynamics from adaptive optics-assisted MUSE observations

Monthly Notices of the Royal Astronomical Society Oxford University Press 509:4 (2021) 5416-5436

Authors:

Sabine Thater, Davor Krajnović, Peter M Weilbacher, Dieu D Nguyen, Martin Bureau, Michele Cappellari, Timothy A Davis, Satoru Iguchi, Richard McDermid, Kyoko Onishi, Marc Sarzi, Glenn van de Ven

Abstract:

Supermassive black hole masses (MBH) can dynamically be estimated with various methods and using different kinematic tracers. Different methods have only been cross-checked for a small number of galaxies and often show discrepancies. To understand these discrepancies, detailed cross-comparisons of additional galaxies are needed. We present the first part of our cross-comparison between stellar- and gas-based MBH estimates in the nearby fast-rotating early-type galaxy NGC 6958. The measurements presented here are based on ground-layer adaptive optics-assisted Multi-Unit Spectroscopic Explorer (MUSE) science verification data at around 0′′.6 spatial resolution. The spatial resolution is a key ingredient for the measurement and we provide a Gaussian parametrisation of the adaptive optics-assisted point spread function (PSF) for various wavelengths. From the MUSE data, we extracted the stellar kinematics and constructed dynamical models. Using an axisymmetric Schwarzschild technique, we measured an MBH of (3.6+2.7−2.4)×108M⊙ at 3σ significance taking kinematical and dynamical systematics (e.g. radially-varying mass-to-light ratio) into account. We also added a dark halo, but our data does not allow to constrain the dark matter fraction. Adding dark matter with an abundance matching prior results in a 25 per cent more massive black hole. Jeans anisotropic models return MBH of (4.6+2.5−2.7)×108M⊙ and (8.6+0.8−0.8)×108M⊙ at 3σ confidence for spherical and cylindrical alignment of the velocity ellipsoid, respectively. In a follow-up study, we will compare the stellar-based MBH with those from cold and warm gas tracers, which will provide additional constraints for the MBH for NGC 6958, and insights into assumptions that lead to potential systematic uncertainty.
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