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Self-consistent bulge/disk/halo galaxy dynamical modeling using integral field kinematics

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Taranu_2017_ApJ_850_70.pdf (9.402Mb)
Date
20/11/2017
Author
Taranu, D. S.
Obreschkow, D.
Dubinski, J. J.
Fogarty, L. M. R.
Sande, J. van de
Catinella, B.
Cortese, L.
Moffett, A.
Robotham, A. S. G.
Allen, J. T.
Bland-Hawthorn, J.
Bryant, J. J.
Colless, M.
Croom, S. M.
D'Eugenio, F.
Davies, R. L.
Drinkwater, M. J.
Driver, S. P.
Goodwin, M.
Konstantopoulos, I. S.
Lawrence, J. S.
López-Sánchez, Á. R.
Lorente, N. P. F.
Medling, A. M.
Mould, J. R.
Owers, M. S.
Power, C.
Richards, S. N.
Tonini, C.
Keywords
Galaxies: fundamental parameters
Galaxies: spiral
Galaxies: structure
Methods: data analysis
QB Astronomy
QC Physics
3rd-NDAS
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Abstract
We introduce a method for modeling disk galaxies designed to take full advantage of data from integral field spectroscopy (IFS). The method fits equilibrium models to simultaneously reproduce the surface brightness, rotation, and velocity dispersion profiles of a galaxy. The models are fully self-consistent 6D distribution functions for a galaxy with a Sérsic profile stellar bulge, exponential disk, and parametric dark-matter halo, generated by an updated version of GalactICS. By creating realistic flux-weighted maps of the kinematic moments (flux, mean velocity, and dispersion), we simultaneously fit photometric and spectroscopic data using both maximum-likelihood and Bayesian (MCMC) techniques. We apply the method to a GAMA spiral galaxy (G79635) with kinematics from the SAMI Galaxy Survey and deep g- and r-band photometry from the VST-KiDS survey, comparing parameter constraints with those from traditional 2D bulge–disk decomposition. Our method returns broadly consistent results for shared parameters while constraining the mass-to-light ratios of stellar components and reproducing the H i-inferred circular velocity well beyond the limits of the SAMI data. Although the method is tailored for fitting integral field kinematic data, it can use other dynamical constraints like central fiber dispersions and H i circular velocities, and is well-suited for modeling galaxies with a combination of deep imaging and H i and/or optical spectra (resolved or otherwise). Our implementation (MagRite) is computationally efficient and can generate well-resolved models and kinematic maps in under a minute on modern processors.
Citation
Taranu , D S , Obreschkow , D , Dubinski , J J , Fogarty , L M R , Sande , J V D , Catinella , B , Cortese , L , Moffett , A , Robotham , A S G , Allen , J T , Bland-Hawthorn , J , Bryant , J J , Colless , M , Croom , S M , D'Eugenio , F , Davies , R L , Drinkwater , M J , Driver , S P , Goodwin , M , Konstantopoulos , I S , Lawrence , J S , López-Sánchez , Á R , Lorente , N P F , Medling , A M , Mould , J R , Owers , M S , Power , C , Richards , S N & Tonini , C 2017 , ' Self-consistent bulge/disk/halo galaxy dynamical modeling using integral field kinematics ' , Astrophysical Journal , vol. 850 , no. 1 , 70 . https://doi.org/10.3847/1538-4357/aa9221
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/aa9221
ISSN
0004-637X
Type
Journal article
Rights
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-4357/aa9221
Collections
  • University of St Andrews Research
URL
http://arxiv.org/abs/1710.03241v1
URI
http://hdl.handle.net/10023/12536

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