Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations

By M. Cappellari, Y. Copin. 2003

904 citations recorded by the source corpus.

We present new techniques to perform adaptive spatial binning of integral-field spectroscopic (IFS) data to reach a chosen constant signal-to-noise ratio per bin. These methods are required for the proper analysis of IFS observations, but can also be used for standard photometric imagery or any other two-dimensional data. Various schemes are tested and compared by binning and extracting the stellar kinematics of the Sa galaxy NGC 2273 from spectra obtained with the panoramic IFS SAURON.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6992516843c531045f5a7604671ad466b4c0be0f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. M. Cappellari
2. P. Hopkins
3. L. Hernquist
4. C. Conroy
5. R. Somerville
6. R. Dav'e
7. T. Naab
8. P. V. van Dokkum

In Ecology

1. M. Blanton
2. F. V. D. Bosch
3. H. Mo
4. Xiaohu Yang
5. J. Brinkmann
6. G. Kauffmann
7. M. Cappellari
8. H. Böhringer

In Instrumentation

1. M. Cappellari
2. P. Hopkins
3. C. Conroy
4. L. Hernquist
5. P. V. van Dokkum
6. T. Naab
7. A. Dekel
8. R. Somerville

Citations in the corpus

• The Milky Way stellar halo out to 40 kpc: squashed, broken but smooth (2011, methodology): “To circumvent this problem, we usethe Voronoi binning method of Cappellari & Copin (2003) to partition the data in pixels on the sky.”
• Triaxial orbit based galaxy models with an application to the (apparent) decoupled core galaxy NGC 4365 (2007, methodology): “To increase the signal-to-noise ratio (S/N) to sufficient levels for accurate determination of the kinematics, the data cube was spatially binned into 964 non-overlapping bins using the two-dimensional Voronoi binning of Cappellari & Copin (2003).”
• Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, methodology): “We spatially bin by means of the centroidal Voronoi tessellation algorithm of Cappellari & Copin (2003) to ensure a minimum S/N of 40 (per Å) at 5800 Å, necessary for a reliable determination of the stellar population properties1.”
• The SAURON project - IV. The mass-to-light ratio, the virial mass estimator and the Fundamental Plane of elliptical and lenticular galaxies (2005, methodology): “They where spatially binned to a minimum signal-to-noise ratioS/N ≈ 60 using the Voronoi twodimensional (2D) binning algorithm by Cappellari & Copin (2003) and the stellar kinematics were subsequently extracted with the penalized pixel-fitting (pPXF) method of Cappellari & Emsellem (2004).”
• Parametric Recovery of Line‐of‐Sight Velocity Distributions from Absorption‐Line Spectra of Galaxies via Penalized Likelihood (2003, methodology): “The data cube was spatially binned to a minimum using the Voronoi two-dimensional (2D) binningS/N p 60 method of Cappellari & Copin (2003).”
• SDSS IV MaNGA – spatially resolved diagnostic diagrams: a proof that many galaxies are LIERs (2016, methodology): “The effect of noise covariance between spaxels is taken into account by modifying the original Voronoi binning procedure of Cappellari & Copin (2003) and scaling the binned noise vector according to an analytical prescription similar to the one adopted by the CALIFA survey (Garcia-Benito et al.…”
• The SAURON project – XII. Kinematic substructures in early-type galaxies: evidence for discs in fast rotators (2008, methodology): “All maps used in this work are Voronoi binned (Cappellari & Copin 2003) to the same signal-to-noise ratio.”
• BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “Next, a Voronoi-binning scheme from Cappellari & Copin (2003) is applied in order to ensure a minimum S/N level of 10 for each bin in the corresponding H-band image.”
• The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres (2006, methodology): “This was achieved using the binning method developed by Cappellari & Copin (2003), in which spectra are coadded starting from the highestS/N lenslet, and accreting additional lenslets closest to the current bin centroid.”
• Kinemetry of SINS High-Redshift Star-Forming Galaxies: Distinguishing Rotating Disks from Major Mergers (2008, methodology): “The data analysis is described in Förster Schreiber et al. (2006); here we add the additional step of spatially binning the data cube to a minimum amplitude-to-noise ratio of 5 with the Voronoi binning technique of Cappellari & Copin (2003).”
• The Star-forming Torus and Stellar Dynamical Black Hole Mass in the Seyfert 1 Nucleus of NGC 3227 (2006, methodology): “Smoothing All the images presented in this paper have been smoothed using optimal Voronoi tessellations, as described and implemented by Cappellari & Copin (2003).”
• The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “…JAM models (A), Vk and σ k are the stellar velocity and dispersion, extracted via PPXF adopting a Gaussian LOSVD, and Fk is the flux contained within that bin, for the P Voronoi bins (Cappellari & Copin 2003) falling within the ‘effective’ ellipse of major axis Rmaje and ellipticity εe (Table 1).”
• Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, neutral): “The Voronoi binned (Cappellari & Copin 2003) kinematics were taken from Emsellem et al. (2004).”
• The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic axes of early-type galaxies (2011, background): “Maps are Voronoi binned (Cappellari & Copin 2003).”
• GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, methodology): “Then we performthe fit of spatially binned spectra based on signal-to-noise ratio (S/N= 10for most galaxies), as described in Cappellari & Copin (2003), with the weighted Voronoi tessellation modification proposed by Diehl & Statler (2006).”
• Simulations of binary galaxy mergers and the link with fast rotators, slow rotators, and kinematically distinct cores (2011, methodology): “The maps have been Voronoi binned (Cappellari & Copin 2003) to have a minimum number of 400 particles per bin.”
• Bursty stellar populations and obscured active galactic nuclei in galaxy bulges (2007, methodology): “In the following subsections, 2D histograms weighted by physical properties were created using an adapted version of the adaptive mesh algorithm of Cappellari & Copin (2003), in order to avoid bins containing a small number of objects biasing our perception of overall trends.”
• IMPROVED AND QUALITY-ASSESSED EMISSION AND ABSORPTION LINE MEASUREMENTS IN SLOAN DIGITAL SKY SURVEY GALAXIES (2011, methodology): “2), which we determined using the Voronoi binning scheme(Cappellari & Copin 2003), and fitted the resulting median and sigma values (red crosses) with a polynomial function (orange lines).”
• The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library (2018, methodology): “In the first mode (VOR10-GAU-MILESHC), the spaxels are binned using the Voronoi-binning scheme from Cappellari & Copin (2003) to a minimum g-band S/N of 10 per spectral pixel.”
• Contour binning: a new technique for spatially-resolved X-ray spectroscopy applied to Cassiopeia A (2006, methodology): “We also show a binned image using a signal-to-noise ratio of 100using the bin-accretion algorithm of Cappellari & Copin (2003), and simple adaptive binning (Sanders & Fabian 2002) for comparison.”