Galaxy Zoo: 3D -- Crowd-sourced Bar, Spiral and Foreground Star Masks for MaNGA Target Galaxies
Karen L. Masters, Coleman Krawczyk, Shoaib Shamsi, Alexander Todd, Daniel Finnegan, Matthew Bershady, Kevin Bundy, Brian Cherinka, Amelia Fraser-McKelvie, Dhane… 展开作者
Karen L. Masters, Coleman Krawczyk, Shoaib Shamsi, Alexander Todd, Daniel Finnegan, Matthew Bershady, Kevin Bundy, Brian Cherinka, Amelia Fraser-McKelvie, Dhanesh Krishnarao, Sandor Kruk, Richard R. Lane, David Law, Chris Lintott, Michael Merrifield, Brooke Simmons, Anne-Marie Weijmans, Renbin Yan
The challenge of consistent identification of internal structure in galaxies - in particular disc galaxy components like spiral arms, bars, and bulges - has hindered our ability to study the physical impact of such structure across large samples. In this paper we present Galaxy Zoo: 3D (GZ: 3D) a crowdsourcing project built on the Zooniverse platform which we used to create spatial pixel (spaxel) maps that identify galaxy centres, foreground stars, galactic bars and spiral arms for 29831 galaxies which were potential targets of the MaNGA survey (Mapping Nearby Galaxies at Apache Point Observatory, part of the fourth phase of the Sloan Digital Sky Surveys or SDSS-IV), including nearly all of the 10,010 galaxies ultimately observed. Our crowd-sourced visual identification of asymmetric, internal structures provides valuable insight on the evolutionary role of non-axisymmetric processes that is otherwise lost when MaNGA data cubes are azimuthally averaged. We present the publicly available GZ:3D catalog alongside validation tests and example use cases. These data may in the future provide a useful training set for automated identification of spiral arm features. As an illustration, we use the spiral masks in a sample of 825 galaxies to measure the enhancement of star formation spatially linked to spiral arms, which we measure to be a factor of three over the background disc, and how this enhancement increases with radius.
Ionised gas outflows driven by active galactic nuclei (AGN) are ubiquitous in high luminosity AGN with outflow speeds apparently correlated with the total bolometric luminosity of the AGN. This empirical relation and theoretical work suggest that in the range L_bol ~ 10^43-45 erg/s there must exist a threshold luminosity above which the AGN becomes powerful enough to launch winds that will be able to escape the galaxy potential. In this paper, we present pilot observations of two AGN in this transitional range that were taken with the Gemini North Multi-Object Spectrograph Integral Field Unit …
Multi-component modelling of galaxies is a valuable tool in the effort to quantitatively understand galaxy evolution, yet the use of the technique is plagued by issues of convergence, model selection and parameter degeneracies. These issues limit its application over large samples to the simplest models, with complex models being applied only to very small samples. We attempt to resolve this dilemma of "quantity or quality" by developing a novel framework, built inside the Zooniverse citizen science platform, to enable the crowdsourcing of model creation for Sloan Digitial Sky Survey galaxies.…
The Impact of Bars, Spirals and Bulge-Size on Gas-Phase Metallicity Gradients in MaNGA Galaxies
University of California（加州大学）；Bryn Mawr College（布林茅尔学院）；Haverford College（哈弗福德学院）；University of Arizona（亚利桑那大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Istituto Nazionale di Astrofisica–Arcetri（意大利国家天体物理研究所-阿切特里）
The knowledge commons research framework is applied to a case of commons governance grounded in research in modern astronomy. The case, Galaxy Zoo, is a leading example of at least three different contemporary phenomena. In the first place Galaxy Zoo is a global citizen science project, in which volunteer non-scientists have been recruited to participate in large-scale data analysis via the Internet. In the second place Galaxy Zoo is a highly successful example of peer production, sometimes known colloquially as crowdsourcing, by which data are gathered, supplied, and/or analyzed by very large…
We study the bar pattern speeds and corotation radii of 225 barred galaxies, using IFU data from MaNGA and the Tremaine-Weinberg method. Our sample, which is divided between strongly and weakly barred galaxies identified via Galaxy Zoo, is the largest that this method has been applied to. We find lower pattern speeds for strongly barred galaxies than for weakly barred galaxies. As simulations show that the pattern speed decreases as the bar exchanges angular momentum with its host, these results suggest that strong bars are more evolved than weak bars. Interestingly, the corotation radius is n…
Galaxy Zoo: Cosmic Dawn -- morphological classifications for over 41,000 galaxies in the Euclid Deep Field North from the Hawaii Two-0 Cosmic Dawn survey
The Open University（开放大学）；University of Toronto（多伦多大学）；University of Minnesota（明尼苏达大学）；European Space Agency (ESA)（欧洲航天局）；Haverford College（哈弗福德学院）；Lancaster University（兰卡斯特大学）；University of Oxford（牛津大学）
We present the data release paper for the Galaxy Zoo: Hubble (GZH) project. This is the third phase in a large effort to measure reliable, detailed morphologies of galaxies by using crowdsourced visual classifications of colour composite images. Images in GZH were selected from various publicly-released Hubble Space Telescope Legacy programs conducted with the Advanced Camera for Surveys, with filters that probe the rest-frame optical emission from galaxies out to $z \sim 1$. The bulk of the sample is selected to have $m_{I814W} < 23.5$,but goes as faint as $m_{I814W} < 26.8$ for deep images c…
Deep Learning Segmentation of Spiral Arms and Bars for 600,000 Galaxies in DESI
University of Hertfordshire（赫特福德大学）；Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学邓普天体物理研究所）；Jodrell Bank Centre for Astrophysics, Department of Physics & Astronomy, University of Manchester（曼彻斯特大学物理与天文系乔德雷克天体物理学中心）；Department of Physics and Astronomy, Haverford College（哈弗福德学院物理与天文系）；Masaryk University（马萨里克大学）；Lancaster University（兰卡斯特大学）；The Open University（开放大学）
Galaxy spins can be predicted from the initial conditions in the early Universe through the tidal tensor twist. In simulations, their directions are well preserved through cosmic time, consistent with expectations of angular momentum conservation. We report a $\sim 3 σ$ detection of correlation between observed oriented directions of galaxy angular momenta and their predictions based on the initial density field reconstructed from the positions of SDSS galaxies. The detection is driven by a group of spiral galaxies classified by the Galaxy Zoo as (anti-)clockwise, with a modest improvement fro…
Fishing for Jellyfish Galaxies: Exploring ram-pressure stripping with crowd science
INAF- Osservatorio astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；University of Nottingham（诺丁汉大学）；Universidad Técnica Federico Santa María（费德里科·圣玛丽亚技术大学）；Millennium Nucleus for Galaxies (MINGAL)（银河系千年核）；University of Birmingham（伯明翰大学）
Deep learning from the crowd Fundamentals of morphological galaxy classification
Instituto Nacional de Astrofísica, Óptica y Electrónica（国家天体物理、光学与电子学研究所）；Universidad de la Laguna（拉古纳大学）；Universidad Autónoma de Tlaxcala（特拉斯卡拉自治大学）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）
Ghent University（根特大学）；University of Minnesota（明尼苏达大学）
Measuring the morphological parameters of galaxies is a key requirement for studying their formation and evolution. Surveys such as the Sloan Digital Sky Survey (SDSS) have resulted in the availability of very large collections of images, which have permitted population-wide analyses of galaxy morphology. Morphological analysis has traditionally been carried out mostly via visual inspection by trained experts, which is time-consuming and does not scale to large ($\gtrsim10^4$) numbers of images. Although attempts have been made to build automated classification systems, these have not been abl…
Statistics of the projected angles between the black-hole spin and the host-galaxy rotation axes from NewHorizon
ILANCE, CNRS – University of Tokyo International Research Laboratory（ILANCE，CNRS-东京大学国际研究实验室）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（卡弗里宇宙物理学与国际前沿研究中心（WPI），UTIAS，东京大学）；Department of Physics, School of Science, The University of Tokyo（东京大学理学部物理系）；Research Institute, Kochi University of Technology（高知工科大学研究所）；Co-creation Organization of Regional Innovation, Kochi University of Technology（高知工科大学区域创新共创组织）；Institut d’Astrophysique de Paris, CNRS and Sorbonne Université（巴黎天体物理研究所，CNRS和索邦大学）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Department of Astronomy and Yonsei University Observatory, Yonsei University（延世大学天文系及延世大学天文台）
The effects of bar strength and kinematics on galaxy evolution II: The global and local impacts of slow-strong bars
Haverford College（哈弗福德学院）；University of California Santa Cruz（加州大学圣克鲁兹分校）；University of Oxford（牛津大学）；University of Toronto（多伦多大学）；Lancaster University（兰开斯特大学）
The discrepancy between the mass of galaxies and their rotational velocity is one of the most puzzling scientific phenomena. Despite over a century of research, this phenomenon is not fully understood. Common explanations include dark matter and MOND, among other theories. Here we report on another observation that shows tension between the physics of galaxy rotation and its rotational velocity. We compare the brightness of galaxies, and find that galaxies that spin in the same direction as the Milky Way have different brightness than galaxies that spin in the opposite direction. While such di…
