Institution
European Southern Observatory
Facility•Garching bei München, Germany•
About: European Southern Observatory is a facility organization based out in Garching bei München, Germany. It is known for research contribution in the topics: Galaxy & Stars. The organization has 3594 authors who have published 16157 publications receiving 823095 citations. The organization is also known as: The European Southern Observatory,ESO & ESO.
Topics: Galaxy, Stars, Star formation, Redshift, Population
Papers published on a yearly basis
Papers
More filters
••
European Southern Observatory1, Liverpool John Moores University2, University of Western Australia3, University of St Andrews4, Max Planck Society5, Ames Research Center6, Australian Astronomical Observatory7, University of the Western Cape8, Durham University9, University of Sussex10, University of Melbourne11, University of Nottingham12, University of Sydney13, Monash University, Clayton campus14, University of Queensland15, University of Edinburgh16, University of Central Lancashire17, Australian National University18, University of Turku19, University of Canterbury20, University of Hertfordshire21, University of Oxford22, Leiden University23, Institute of Cosmology and Gravitation, University of Portsmouth24, National Institute of Astrophysics, Optics and Electronics25, Macquarie University26, National Autonomous University of Mexico27, Carnegie Institution for Science28, University of Bristol29, University of Hull30, Romanian Academy31, Queen Mary University of London32, University of Innsbruck33
TL;DR: The Galaxy And Mass Assembly (GAMA) survey as mentioned in this paper is one of the largest contemporary spectroscopic surveys of low redshift galaxies, covering an area of ∼286 deg2 (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, and collecting spectra and reliable redshifts for 238'000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope.
Abstract: The Galaxy And Mass Assembly (GAMA) survey is one of the largest contemporary spectroscopic surveys of low redshift galaxies. Covering an area of ∼286 deg2 (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, we have collected spectra and reliable redshifts for 238 000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope. In addition, we have assembled imaging data from a number of independent surveys in order to generate photometry spanning the wavelength range 1 nm–1 m. Here, we report on the recently completed spectroscopic survey and present a series of diagnostics to assess its final state and the quality of the redshift data. We also describe a number of survey aspects and procedures, or updates thereof, including changes to the input catalogue, redshifting and re-redshifting, and the derivation of ultraviolet, optical and near-infrared photometry. Finally, we present the second public release of GAMA data. In this release, we provide input catalogue and targeting information, spectra, redshifts, ultraviolet, optical and near-infrared photometry, single-component Sersic fits, stellar masses, Hα-derived star formation rates, environment information, and group properties for all galaxies with r < 19.0 mag in two of our survey regions, and for all galaxies with r < 19.4 mag in a third region (72 225 objects in total). The data base serving these data is available at http://www.gama-survey.org/.
494 citations
••
TL;DR: Sensitive near-infrared measurements of the light from background stars as it is absorbed and scattered by trace amounts of dust are used to probe the internal structure of the dark cloud Barnard 68 with unprecedented detail and find the cloud's density structure to be very well described by the equations for a pressure-confined, self-gravitating isothermal sphere that is critically stable according to the Bonnor–Ebert criteria.
Abstract: Stars and planets form within dark molecular clouds, but little is understood about the internal structure of these clouds, and consequently about the initial conditions that give rise to star and planet formation. The clouds are primarily composed of molecular hydrogen, which is virtually inaccessible to direct observation. But the clouds also contain dust, which is well mixed with the gas and which has well understood effects on the transmission of light. Here we use sensitive near-infrared measurements of the light from background stars as it is absorbed and scattered by trace amounts of dust to probe the internal structure of the dark cloud Barnard 68 with unprecedented detail. We find the cloud's density structure to be very well described by the equations for a pressure-confined, self-gravitating isothermal sphere that is critically stable according to the Bonnor-Ebert criteria. As a result we can precisely specify the physical conditions inside a dark cloud on the verge of collapse to form a star.
492 citations
••
TL;DR: In this article, the smallest intrinsic dispersions of σ ≤ 1% in θ LD are obtained for the surface brightness relations of these stars using exclusively direct angular diameter measurements.
Abstract: The availability of a number of new interferometric measurements of Main Sequence and subgiant stars makes it possible to calibrate the surface brightness relations of these stars using exclusively direct angular diameter measurements. These empirical laws make it possible to predict the limb darkened angular diameters θ LD of dwarfs and subgiants using their dereddened Johnson magnitudes, or their effective temperature. The smallest intrinsic dispersions of σ ≤ 1% in θ LD are obtained for the relations based on the K and L magnitudes, for instance log θ LD = 0.0502 (B - L) + 0.5133 - 0.2 L or log θ LD = 0.0755 (V - K) + 0.5170 - 0.2 K. Our calibrations are valid between the spectral types A0 and M2 for dwarf stars (with a possible extension to later types when using the effective temperature), and between A0 and K0 for subgiants. Such relations are particularly useful for estimating the angular sizes of calibrators for long-baseline interferometry from readily available broadband photometry.
488 citations
••
TL;DR: In this paper, it was shown that the transient optical source associated with the gamma-ray burst brightened to about 60 times the expected flux, based upon an extrapolation of the initial light curve.
Abstract: Cosmic γ-ray bursts have now been firmly established as one of the most powerful phenomena in the Universe, releasing almost the rest-mass energy of a neutron star within the space of a few seconds (ref. 1). The two most popular models to explain γ-ray bursts are the coalescence of two compact objects such as neutron stars or black holes, or the catastrophic collapse of a massive star in a very energetic supernova-like explosion. Here we show that, about three weeks after the gamma-ray burst of 26 March 1998, the transient optical source associated with the burst brightened to about 60 times the expected flux, based upon an extrapolation of the initial light curve. Moreover, the spectrum changed dramatically, with the colour becoming extremely red. We argue that the new source is an underlying supernova. If our hypothesis is true then this provides evidence linking cosmologically located γ-ray bursts with deaths of massive stars.
485 citations
••
Liverpool John Moores University1, University of St Andrews2, University of Western Australia3, University of Sussex4, University of Sydney5, University of Melbourne6, European Southern Observatory7, Durham University8, Australian Astronomical Observatory9, University of Nottingham10, University of Edinburgh11, Monash University, Clayton campus12, University of Central Lancashire13, Australian National University14, Max Planck Society15
TL;DR: In this paper, the low-redshift field galaxy stellar mass function (GSMF) was determined from a sample of 5210 galaxies using a density-corrected maximum volume method.
Abstract: We determine the low-redshift field galaxy stellar mass function (GSMF) using an area of 143 deg 2 from the first three years of the Galaxy And Mass Assembly (GAMA) survey. The magnitude limits of this redshift survey are r < 19.4 mag over two-thirds and 19.8 mag over one-third of the area. The GSMF is determined from a sample of 5210 galaxies using a densitycorrected maximum volume method. This efficiently overcomes the issue of fluctuations in the number density versus redshift. With H0 = 70 km s −1 Mpc −1 , the GSMF is well described
485 citations
Authors
Showing all 3617 results
Name | H-index | Papers | Citations |
---|---|---|---|
Robert C. Nichol | 187 | 851 | 162994 |
Richard S. Ellis | 169 | 882 | 136011 |
Rob Ivison | 166 | 1161 | 102314 |
Alvio Renzini | 162 | 908 | 95452 |
Timothy C. Beers | 156 | 934 | 102581 |
Krzysztof M. Gorski | 132 | 380 | 105912 |
Emanuele Daddi | 129 | 581 | 63187 |
P. R. Christensen | 127 | 313 | 88445 |
Mark Dickinson | 124 | 389 | 66770 |
Christopher W. Stubbs | 122 | 622 | 109429 |
Eva K. Grebel | 118 | 863 | 83915 |
Martin Asplund | 118 | 612 | 52527 |
Jesper Sollerman | 118 | 726 | 53436 |
E. F. van Dishoeck | 115 | 742 | 49190 |
Jørgen Christensen-Dalsgaard | 114 | 585 | 48272 |