Parametric Recovery of Line‐of‐Sight Velocity Distributions from Absorption‐Line Spectra of Galaxies via Penalized Likelihood

By M. Cappellari, Eric Emsellem. 2003

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We investigate the accuracy of the parametric recovery of the line‐of‐sight velocity distribution (LOSVD) of the stars in a galaxy while working in pixel space. Problems appear when the data have a low signal‐to‐noise ratio or the observed LOSVD is not well sampled by the data. We propose a simple solution based on maximum penalized likelihood, and we apply it to the common situation in which the LOSVD is described by a Gauss‐Hermite series. We compare different techniques by extracting the stellar kinematics from observations of the barred lenticular galaxy NGC 3384 obtained with the SAURON integral‐field spectrograph.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Plant Science

View Paper: https://www.semanticscholar.org/paper/f1e3ff9e96e9fc6a12ade5ae8895ccf08a949602

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Citations in the corpus

An updated MILES stellar library and stellar population models (2011, methodology): “We measured the broadening of the different datasets using the penalized pixel-fitting (pPXF) method of Cappellari & Emsellem (2004), with the data and templates described above.”
Observational evidence for AGN feedback in early-type galaxies (2007, methodology): “We measure the kinematics of the stars and the emission-linefluxes of our galaxies from their SDSS spectra following the methods of Cappellari & Emsellem (2004) and Sarzi et al. (2006), respectively1.”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, methodology): “…a σ larger than the LIS resolution an additive correction was made using the kinematic templates (the combination of SSP-models that better reproduced the galaxy spectra obtained in the measurement of σ using ppxf (Cappellari & Emsellem 2004)), following the prescriptions in Kelson et al. (2006).”
The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, methodology): “The kinematics of all galaxies in the ATLAS3D sample was homogeneously extracted as described in Paper I, using the penalized pixel-fitting (PPXF) software1 (Cappellari & Emsellem 2004) and the full MILES stellar library (SánchezBlázquez et al. 2006; Falcón-Barroso et al. 2011) as templates.”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, background): “In practice, most codes designed to fit galaxy spectra (e.g. PPXF, Cappellari & Emsellem 2004; STARLIGHT, Cid Fernandes et al. 2005; STECKMAP, Ocvirk et al. 2006; ULYSS, Koleva et al. 2009) suffer from intrinsic limitations.”
Supermassive Black Holes in Active Galactic Nuclei. II. Calibration of the Black Hole Mass-Velocity Dispersion Relationship for Active Galactic Nuclei (2004, background): “3See Cappellari & Emsellem (2004), and http://www.strw.leidenuniv.nl/∼mcappell/idl/ for details.”
The SAURON project - VI. Line strength maps of 48 elliptical and lenticular galaxies (2006, positive): “Journal compilation C© 2006 RAS, MNRAS 369, 497–528 Downloaded from https://academic.oup.com/mnras/article-abstract/369/2/497/3101467 by guest on 28 July 2018 Cappellari & Emsellem 2004) and then determine the line strength as presented in Section 4.”
The ATLAS3D project - X. On the origin of the molecular and ionized gas in early-type galaxies (2011, methodology): “The SAURON stellar kinematics were derived using a penalized pixel fitting routine (Cappellari & Emsellem 2004), providing parametric estimates of the line-of-sight velocity distribution for each spaxel.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, methodology): “…2011; Conroy & van Dokkum 2012a), the studies of the stellar population from integralfield data has moved to the full-spectrum fitting approach (using fitting codes like ppxf Cappellari & Emsellem 2004; starlight Cid Fernandes et al. 2005; steckmap Ocvirk et al. 2006; vespa Tojeiro et al. 2007).”
Stellar Population Inference with Prospector (2020, methodology): “…diagrams (e.g., Dolphin 1997; Harris & Zaritsky 2001; Weisz et al. 2011; Cook et al. 2019) and have been used in maximum-likelihood “inversion” codes for unresolved spectra (e.g., Cappellari & Emsellem 2004; Cid Fernandes et al. 2005; Ocvirk et al. 2006; Tojeiro et al. 2007; Koleva et al. 2009).”
The SAURON project – X. The orbital anisotropy of elliptical and lenticular galaxies: revisiting the (V/σ, ɛ) diagram with integral‐field stellar kinematics (2007, methodology): “…& Franx 1993; Gerhard 1993) of the line-of-sight stellar velocity distribution (LOSVD) up toh3–h6, using the penalised pixel-fitting method (pPXF, Cappellari & Emsellem 2004); (ii) To measure the meanvelocity V and the velocity dispersionσ to be used in the(V/σ, ε) diagram we did not fit the…”
SUPERDENSE MASSIVE GALAXIES IN THE NEARBY UNIVERSE (2009, methodology): “We have also checked these values using the Penalized Pixel-Fitting method developed by Cappellari & Emsellem (2004) and we find an excellent agreement with the SDSS measurements ∆σ/σ=0.00±0.07.”
The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early-and late-type galaxies (2014, methodology): “The spectroscopic classifications, especially the AGN-classifications, derive from analysis with the Gas AND Absorption Line Fitting (GANDALF) code (Cappellari & Emsellem 2004; Sarzi et al. 2006).”
The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library (2018, methodology): “The stellar velocity dispersion and ionized-gas velocity dispersions are provided as measured from the core pPXF software (Cappellari & Emsellem 2004; Cappellari 2017) used by the DAP.”
Triaxial orbit based galaxy models with an application to the (apparent) decoupled core galaxy NGC 4365 (2007, methodology): “The stellar kinematics where extracted using the penalized pixel-fitting method (pPXF) of Cappellari & Emsellem (2004).”
The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “We use the publicly available3 penalized pixel fitting code (PPXF; Cappellari & Emsellem 2004) to fit a linear combination of SSP model spectra from the MIUSCAT model library (Vazdekis et al. 2012), spanning a regular grid of log (age) (0.1–14 Gyr) and metallicity ([Z/H] = −1.71 to 0.22, equivalent…”
STELLAR KINEMATICS OF z ∼ 2 GALAXIES AND THE INSIDE-OUT GROWTH OF QUIESCENT GALAXIES, (2012, methodology): “We use the unbinned spectra in combination with the Penalized PixelFitting (pPXF) method by Cappellari & Emsellem (2004) and our best-fitting BC03 models as templates.”
The ATLAS3D project - XIV. The extent and kinematics of the molecular gas in early-type galaxies (2012, methodology): “The SAURON stellar kinematics were derived using a penalized pixel fitting routine (Cappellari & Emsellem 2004), providing parametric estimates of the line-of-sight velocity distribution for each bin.”