J/MNRAS/522/6326 MaNGA galaxies DynPop I JAM dynamical properties (Zhu+, 2023)
MaNGA DynPop - I Quality-assessed stellar dynamical modelling from
integral-field spectroscopy of 10K nearby galaxies: a catalogue of masses,
mass-to-light ratios, density profiles, and dark matter.
Zhu K., Lu S., Cappellari M., Li R., Mao S., Gao L.
<Mon. Not. R. Astron. Soc. 522, 6326-6353 (2023)>
=2023MNRAS.522.6326Z 2023MNRAS.522.6326Z (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Spectroscopy ; Photometry ; Infrared ;
Optical ; Positional data ; Extinction ; Models ;
Velocity dispersion ; Radial velocities ; Space velocities ;
Galaxies, radius ; Redshifts ; Morphology ; Stars, masses
Keywords: galaxies: evolution - galaxies: formation -
galaxies: kinematics and dynamics - galaxies: structure
Abstract:
This is the first paper in our series on the combined analysis of the
Dynamics and stellar Population (DynPop) for the MaNGA survey in the
final SDSS Data Release 17 (DR17). Here, we present a catalogue of
dynamically determined quantities for over 10000 nearby galaxies
based on integral-field stellar kinematics from the MaNGA survey. The
dynamical properties are extracted using the axisymmetric Jeans
Anisotropic Modelling (JAM) method, which was previously shown to be
the most accurate for this kind of study. We assess systematic
uncertainties using eight dynamical models with different assumptions.
We use two orientations of the velocity ellipsoid: either
cylindrically aligned JAMcyl or spherically aligned JAMsph. We also
make four assumptions for the models' dark versus luminous matter
distributions: (1) mass-follows-light, (2) free NFW dark halo, (3)
cosmologically constrained NFW halo, (4) generalized NFW dark halo,
i.e. with free inner slope. In this catalogue, we provide the
quantities related to the mass distributions (e.g. the density slopes
and enclosed mass within a sphere of a given radius for total mass,
stellar mass, and dark matter mass components). We also provide the
complete models which can be used to compute the full luminous and
mass distribution of each galaxy. Additionally, we visually assess the
qualities of the models to help with model selections. We estimate the
observed scatter in the measured quantities which decreases as
expected with improvements in quality. For the best data quality, we
find a remarkable consistency of measured quantities between different
models, highlighting the robustness of the results.
Description:
With the final data release of the MaNGA project (SDSS DR17;
Abdurro'uf et al. 2022ApJS..259...35A 2022ApJS..259...35A, Cat. III/286), an
unprecedentedly large sample (10K) of nearby galaxies with abundant
information on the kinematics and stellar population properties is
available. In this series of papers, we aim to build a complete
library of dynamical models for these galaxies, including mass
distributions (for both stellar matter and DM), DM fractions, stellar
mass-to-light ratios, inclinations, and velocity asymmetry properties,
using JAM with different assumptions. With these information, we will
also investigate the scaling relations, galaxy mass density slopes, as
well as initial mass functions of the complete MaNGA sample. Compared
to previous studies our sample size will be enlarged by at least a
factor of five and reach 10K galaxies for the first time. The large
sample span a wide range of galactic properties, e.g. stellar mass,
morphology, and central velocity dispersion, making it a statistically
significant sample to explore the correlations in great detail.
In this paper (Paper I), we construct detailed JAM models for these
10000 nearby galaxies and provide their mass distributions of both
stellar and DM components.
The Mapping Nearby Galaxies at Apache Point Observatory is an IFU
survey which aims at obtaining spectral measurements across the face
of ∼10K nearby galaxies. Using the tightly packed arrays of optical
fibres that feed into the BOSS spectrographs on the Sloan 2.5m teles)
at Apache Point Observatory, MaNGA provides the spatially resolved
spectra that cover a radial range out to 1.5 effective radii (Re) for
the Primary + sample (∼2/3 of total sample) and out to 2.5 Re for the
secondary sample (∼1/3 of total sample) at higher redshift. The spaxel
size of MaNGA is 0.5 arcsec and the average g-band point spread
function (PSF) full width at half-maximum (FWHM) throughout the survey
is about 2.54 arcsec. The spectra provided by MaNGA span a wavelength
range of 3600-10300 Å at a spectral resolution of σ = 72 km/s.
Raw observational data are spectrophotometrically calibrated and
processed by the data reduction pipeline DAP to produce 3D data cubes.
DAP allows us to products stellar kinematics, nebular emission-line
properties, and spectral indices of the galaxies from IFU spectra
fitting processes (i.e. see section 2). Used data are presented in
table1.dat.
As fully detailled in section 3, with JAM plus mass profile models and
MGE fitting techniques, we proposed 8 models parametrized with free
parameters and optimization methods. To find the best-fitting
parameters of the JAM models we used a least-squares fitting methods.
Next as presented in section 4, table2-9.dat provide three radius size
parameters, total/components masses and density slopes, velocity
dispersions, space velocities and quality assessments (as modelling
quality and visual quality classification i.e. section 5).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 670 10296 Astrometrics, photometric, physical properties
extracted from SDSS-IV MaNGA nearby galaxies
IFU survey
table2.dat 98 10296 *Dynamical properties as velocities, inclination
angle,M/L, masses and density slopes for
JAMcyl+MFL parametrized model
table3.dat 106 10296 *Dynamical properties as velocities, inclination
angle,M/L, masses and density slopes for
JAMsph+MFL parametrized model
table4.dat 228 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMcyl+NFW parametrized model
table6.dat 228 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMcyl+fixedNFW parametrized model
table8.dat 228 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMcyl+generalizedNFW parametrized model
table5.dat 236 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMsph+NFW parametrized model
table7.dat 236 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMsph+fixedNFW parametrized model
table9.dat 236 10296 *Dynamical properties as velocities, inclination
angle, M/L,masses and density slopes for
JAMsph+generalizedNFW parametrized model
--------------------------------------------------------------------------------
Note on table2.dat: Jeans Anisotropic Modelling JAM with cylindrically aligned
velocity ellipsoid cyl as JAMcyl combined to Mass-follows-light model as MFL
parametrized as described in section 3.3.
Note on table3.dat: Jeans Anisotropic Modelling JAM with spherical aligned
velocity ellipsoid sph as JAMsph combined to Mass-follows-light model as MFL
parametrized as described in section 3.3.
Note on table4.dat: Jeans Anisotropic Modelling JAM with cylindrically aligned
velocity ellipsoid cyl as JAMcyl combined to NFW dark halo model as NFW
parametrized as described in section 3.3.
Note on table6.dat: Jeans Anisotropic Modelling JAM with cylindrically aligned
velocity ellipsoid cyl as JAMcyl combined to the fixed NFW dark halo model
as fixed NFW parametrized as described in section 3.3.
Note on table8.dat: Jeans Anisotropic Modelling JAM with cylindrically aligned
velocity ellipsoid cyl as JAMcyl combined to the generalized NFW dark halo
model as fixed NFW parametrized as described in section 3.3.
Note on table5.dat: Jeans Anisotropic Modelling JAM with spherical aligned
velocity ellipsoid sph as JAMsph combined to NFW dark halo model as NFW
parametrized as described in section 3.3.
Note on table7.dat: Jeans Anisotropic Modelling JAM with spherical aligned
velocity ellipsoid sph as JAMsph combined to the fixed NFW dark halo model
as NFW parametrized as described in section 3.3.
Note on table9.dat: Jeans Anisotropic Modelling JAM with spherical aligned
velocity ellipsoid sph as JAM_sph combinedto the generalized NFW dark halo
model as NFW parametrized as described in section 3.3.
--------------------------------------------------------------------------------
See also:
J/MNRAS/494/5619 : Precise benchmark for cluster scaling relations
(Shetty+, 2020)
J/MNRAS/477/4711 : Stellar angular momentum for MaNGA galaxies (Graham+, 2018)
J/MNRAS/476/1765 : MaNGA E and S galaxies properties (Li+, 2018)
J/MNRAS/451/2723 : Low-redshift clusters in the SAMI Pilot Survey (Scott+,2015)
J/MNRAS/414/888 : ATLAS3D project. III. (Emsellem+, 2011)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006)
J/A+A/564/A125 : AGN Torus model comparison of AGN in the CDFS
(Buchner+, 2014)
J/ApJ/923/11 : Stellar kinematics of LEGA-C galaxies (van Houdt+, 2021)
J/ApJS/262/36 : SDSS-IV MaNGA: pyPipe3D data for 10000 galaxies
(Sanchez+, 2022)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
VII/233 : 2MASS All-Sky Extended Source Catalog (XSC)
(IPAC-UMass, 2003-2006)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Identifier raw number
7- 11 I5 --- Plate The plate ID (e.g. 7443) (plate)
13- 17 I5 --- IFUdsgn The IFU design ID (e.g.12703) (ifudsgn)
19- 29 A11 --- PlateIFU The plate + ifudsgn name
(e.g. 7443-12703) (plateifu)
31- 39 A9 --- MaNGAId Unique MaNGA ID (e.g. 1-114145)
(mangaid)
41- 58 F18.14 deg RAdeg Right ascension of the science object
(J2000) (obj_ra)
60- 76 E17.14 deg DEdeg Declination of the science object
(J2000) (obj_dec)
78- 87 F10.8 mag E(B-V) E(B-V) value from sdss dust routine for
this IFU (ebvgal)
89 I1 --- Target Flag for subsample of MaNGA primary: 0,
secondary: 1,
colour enhanced: 2 (target)
91- 97 F7.3 arcsec Rmax ? The kinematic data range, which is
defined as the largest radius of the
Voronoi bins (DA)
99-119 F21.18 Mpc DA ? Adopted angular-diameter distance,
with flat Universe of Ωm=0.307,
h=0.677 Planck from Collaboration XIII
2016 (rmax_arcsec)
121-139 F19.16 arcsec ReMGE ? Effective radius projected circular
half-light radius from MGE fitting, in
SDSS r band (RearcsecMGE)
141-159 F19.16 arcsec RmajMGE ? Major axis of elliptical half-light
isophote from MGE fitting, in SDSS r
band (RmajarcsecMGE)
161-166 F6.3 [Lsun] log(LtotMGE) ? Total luminosity from MGE fitting, in
SDSS r band, not corrected for the
Galactic and internal dust extinction
(LumtotMGE)
168-173 F6.3 --- LambdaRe ? Specific stellar angular momentum
within elliptical half-light isophote,
beam corrected (Lambda_Re)
175-179 F5.1 km/s SigmaRe ? Effective velocity dispersion within
elliptical half-light isophote
(Sigma_Re)
181-185 F5.3 --- EpsMGE ? Ellipticity of the half-light
isophote from MGE fitting (Eps_MGE)
187-193 F7.3 deg PAph ? The photometric position angle (PA)
measured from MGE fitting, in SDSS
r-band (PA_phot)
195-199 F5.1 deg PAkin ? The kinematic PA measured from MaNGA
velocity field (PA_kin)
201-203 F3.1 --- f_PAkin The flag for kinematic PA 0 for
unreliable, 1 for reliable (PAkinflag)
205-223 A19 --- IAUname The accepted IAU name (nsa_iauname)
225-236 E12.10 --- z Redshift of the galaxy (z)
238-242 I5 --- Field ?=-9999 The SDSS field covering the
target (nsa_field)
244-248 I5 --- Run ?=-9999 The SDSS run covering the
target (nsa_run)
250-254 I5 --- Camcol ?=-9999 The SDSS camcol covering
catalogue position (nsa_camcol)
256-261 A6 --- Version The version of the NSA catalogue used
to select these targets (nsa_version)
263-268 I6 --- NSAID ?=-9999 The NSAID field in the NSA
catalogue v1 (nsa_id)
270-275 I6 --- NSAIDv1b ?=-9999 The NSAID of the target in the
NSA v1b00_v2 catalogue (if applicable)
(nsansaidv1b)
277-290 F14.8 mag Sersic1Mag ?=-9999 Absolute magnitude 1 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag1)
292-305 F14.8 mag Sersic2Mag ?=-9999 Absolute magnitude 2 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag2)
307-319 F13.7 mag Sersic3Mag ?=-9999 Absolute magnitude 3 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag3)
321-333 F13.7 mag Sersic4Mag ?=-9999 Absolute magnitude 4 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag4)
335-346 F12.6 mag Sersic5Mag ?=-9999 Absolute magnitude 5 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag5)
348-360 F13.7 mag Sersic6Mag ?=-9999 Absolute magnitude 6 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag6)
362-374 F13.7 mag Sersic7Mag ?=-9999 Absolute magnitude 7 estimates
for FNugriz from K-corrections
Ωm=0.3, Ωλ=0.7,
h=1, the value is interpreted as M-5log
(h) (nsasersicabsmag7)
376-388 F13.7 mag Elpetro1Mag ?=-9999 As nsasersicabsmag 1 but from
elliptical Petrosian apertures
(nsaelpetroabsmag1)
390-402 F13.7 mag Elpetro2Mag ?=-9999 As nsasersicabsmag 2 but from
elliptical Petrosian apertures
(nsaelpetroabsmag2)
404-416 F13.7 mag Elpetro3Mag ?=-9999 As nsasersicabsmag 3 but from
elliptical Petrosian apertures
(nsaelpetroabsmag3)
418-429 F12.6 mag Elpetro4Mag ?=-9999 As nsasersicabsmag 4 but from
elliptical Petrosian apertures
(nsaelpetroabsmag4)
431-442 F12.6 mag Elpetro5Mag ?=-9999 As nsasersicabsmag 5 but from
elliptical Petrosian apertures
(nsaelpetroabsmag5)
444-455 F12.6 mag Elpetro6Mag ?=-9999 As nsasersicabsmag 6 but from
elliptical Petrosian apertures
(nsaelpetroabsmag6)
457-468 F12.6 mag Elpetro7Mag ?=-9999 As nsasersicabsmag 7 but from
elliptical Petrosian apertures
(nsaelpetroabsmag7)
470-488 F19.16 [Msun] log(Msersic) ? Logarithm of the stellar mass from
K-correction fit for Sersic fluxes in
Msun/h2 unit (nsasersicmass)
490-507 A18 [Msun] log(Melpetro) Stellar mass from K-correction fit for
elliptical Petrosian fluxes in
Msun/h2 unit (nsaelpetromass)
509-522 F14.8 --- b/aSercic ?=-9999 Axial ratio b/a from 2D Sersic
fit in SDSS r band (nsasersicba)
524-537 F14.8 --- NSersic ?=-9999 Sersic index from 2D Sersic fit
in SDSS r band (nsasersicn)
539-552 F14.8 deg PhiSercic ?=-9999 Angle (E of N) of major axis in
2D Sersic fit (r band) (nsasersicphi)
554-568 F15.9 arcsec Rth50Sercic ?=-9999 Sersic 50 per cent light radius
along major axis (r band)
(nsasersicth50)
570-583 E14.10 --- flux1Sersic ?=-9999 2D Sersic fit flux 1 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux1)
585-597 E13.10 --- flux2Sersic ?=-9999 2D Sersic fit flux 2 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux2)
599-612 F14.7 --- flux3Sersic ?=-9999 2D Sersic fit flux 3 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux3)
614-626 F13.7 --- flux4Sersic ?=-9999 2D Sersic fitt flux 4 in
FNugriz GALEX-SDSS photometric systems
in nanomaggies unit (nsasersicflux4)
628-640 F13.7 --- flux5Sersic ?=-9999 2D Sersic fit flux 5 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux5)
642-653 E12.10 --- flux6Sersic ?=-9999 2D Sersic fit flux 6 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux6)
655-665 E11.9 --- flux7Sersic ?=-9999 2D Sersic fit flux 7 in FNugriz
GALEX-SDSS photometric systems in
nanomaggies unit (nsasersicflux7)
667-668 I2 --- Qual Visual quality of JAM models,
classified as -1, 0, 1, 2, 3 from worst
to best (Qual)
670 I1 --- DRP3Qual Data reduction quality marked by DRP
pipeline, 1 for high-quality, 0 for
critical-quality or unusual quality
(drp3qual)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Identifier raw number
7- 12 F6.3 deg i ? Best-fitting inclination angle,
being 90 for edge-on as modelled in
section 3.2 (inc_deg)
14- 18 F5.3 --- Betaz ? Best-fitting radial velocity
anisotropy Βz in cylindrical
coordinates (beta_z)
20- 25 F6.3 [Msun/Lsun] M/L ? Best-fitting dynamical
mass-to-light ratio in
M☉/L☉ units (logMLdyn)
27- 35 F9.3 --- Kappa ? The ratio between modelled and
observed line-of-sight velocity
field (kappa)
37- 42 F6.3 [Msun] log(Mt<Re) ? Enclosed total stellar matter+DM+BH
mass within a sphere of circularized
effective radius Re which satisfying
that the area of half-light ellipse
A=π*Re2 (logMtRe)
44- 52 E9.6 --- Chi2 ? The reduced chi2 of best-fitting
model, values are scaled to account
for effect of standard dev. of chi2
itself and it should be onlyused in
comparison between models (chi2_dof)
54- 72 F19.16 arcsec Rh ? Radius r1/2 of the 3D sphere which
encloses half the total luminosity
of the galaxy (rhalf_arcsec)
74- 79 F6.3 [Msun] log(Mt<Rh) ? Enclosed total stellar matter+DM+BH
mass within a sphere of 3D half-light
radius Rh (logMtrhalf)
81- 85 F5.3 --- GmwtRe ? Mass-weighted total density slope
Γbart within a sphere of
effective radius Re (MWGtRe)
87- 91 F5.3 --- GmwtRh ? Mass-weighted total density slope
Γbart within a sphere of 3D
half-light radius Rh (MWGtrhalf)
93- 98 F6.3 [-] log(GavtRe) ? Average logarithmic total density
slope Γt between 0.1 and 1
effective radius Re (Gt_Re)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Identifier raw number
7- 12 F6.3 deg i ? Best-fitting inclination angle,
being 90 for edge-on as modelled in
section 3.2 (inc_deg)
14- 19 F6.3 --- Betar ? Best-fitting radial velocity
anisotropy Βrin spherical
coordinates (beta_r)
21- 26 F6.3 [Msun/Lsun] M/L ? Best-fitting dynamical
mass-to-light ratio in
M☉/L☉ units (logMLdyn)
28- 42 E15.12 --- Kappa ? The ratio between modelled and
observed line-of-sight velocity
field (kappa)
44- 49 F6.3 [Msun] log(Mt<Re) ? Enclosed total stellar matter+DM+BH
mass within a sphere of circularized
effective radius Re which satisfying
that the area of half-light ellipse
A=π*Re2 (logMtRe)
51- 60 E10.6 --- Chi2 ? The reduced chi2 of best-fitting
model, values are scaled to account
for effect of standard dev. of chi2
itself and it should be only used in
comparison between models (chi2_dof)
62- 80 F19.16 arcsec Rh ? Radius r1/2 of the 3D sphere which
encloses half the total luminosity
of the galaxy (rhalf_arcsec)
82- 87 F6.3 [Msun] log(Mt<Rh) ? Enclosed total stellar matter+DM+BH
mass within a sphere of 3D half-light
radius Rh (logMtrhalf)
89- 93 F5.3 --- GmwtRe ? Mass-weighted total density slope
Γbart within a sphere of
effective radius Re (MWGtRe)
95- 99 F5.3 --- GmwtRh ? Mass-weighted total density slope
Γbart within a sphere of 3D
half-light radius Rh (MWGtrhalf)
101-106 F6.3 [-] log(GavtRe) ? Average logarithmic total density
slope Γt between 0.1 and 1
effective radius Re (Gt_Re)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat table6.dat table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Identifier raw number
7- 12 F6.3 deg i ? Best-fitting inclination angle,
being 90 for edge-on as modelled in
section 3.2 (inc_deg)
14- 18 F5.3 --- Betaz ? Best-fitting radial velocity
anisotropy Βzin cylindrical
coordinates (beta_z)
20- 25 F6.3 [Msun/Lsun] logM/Ls ? Best-fitting stellar mass-to-light
ratio in M☉/L☉ units
(logMLstellar)
27- 48 E22.19 [Msun/kpc3] logrhos ? The characteristic density of NFW
profile (logrhos)
50- 57 F8.3 kpc rs ? The break radius as characteristic
radius of NFW profile (rs)
59- 67 F9.3 --- Kappa ? The ratio between modelled and
observed line-of-sight velocity
field (kappa)
69- 77 F9.3 [Msun] log(Mt<Re) ? Enclosed total stellar
matter+DM+BH mass within a sphere of
circularized effective radius Re
which satisfying that the area of
half-light ellipse A=π*Re2
(logMtRe)
79- 84 F6.3 [Msun] log(Ms<Re) ? Enclosed stellar matter mass
within a sphere of circularized
effective radius Re which satisfying
that the area of half-light ellipse
A=π*Re2 (logMsRe)
86- 91 F6.3 [Msun] log(Md<Re) ? Enclosed DM mass within a sphere
of circularized effective radius Re
which satisfying that the area of
half-light ellipse A=π*Re2
(logMdRe)
93- 98 F6.3 --- fDM<Re ? DM fraction within a sphere of
effective radius which satisfying
that the area of half-light ellipse
A=π*Re2 (fdm_Re)
100-105 F6.3 [Msun/Lsun] logM/Ldyn ? Best-fitting dynamical
mass-to-light ratio in
M☉/L☉ units (logMLdyn)
107-116 E10.7 --- Chi2 ? The reduced chi2 of best-fitting
model, values are scaled to account
for effect of standard dev. of chi2
itself and it should be only used in
comparison between models (chi2_dof)
118-136 E19.13 arcsec Rh ? Radius r1/2 of the 3D sphere which
encloses half the total luminosity
of the galaxy (rhalf_arcsec)
138-156 F19.16 [Msun] log(Mt<Rh) ? Enclosed total stellar
matter+DM+BH mass within a sphere of
3D half-light radius Rh
(logMtrhalf)
158-163 F6.3 [Msun] log(Ms<Rh) ? Enclosed stellar matter mass
within a sphere of 3D half-light
radius Rh (logMsrhalf)
165-170 F6.3 [Msun] log(Md<Rh) ? Enclosed DM mass within a sphere
of 3D half-light radius Rh
(logMdrhalf)
172-177 F6.3 --- GmwtRe ? Mass-weighted total density slope
Γbart within a sphere of
effective radius Re (MWGtRe)
179-183 F5.3 --- GmwsRe ? Mass-weighted stellar density
slope Γbar* within a sphere
of effective radius Re (MWGsRe)
185-189 F5.3 --- GmwdRe ? Mass-weighted DM density slope
ΓbarDM within a sphere of
effective radius Re (MWGsRe)
191-195 F5.3 --- GmwtRh ? Mass-weighted total density slope
Γbart within a sphere of 3D
half-light radius Rh (MWGtrhalf)
197-201 F5.3 --- GmwsRh ? Mass-weighted stellar density
slope Γbar* within a sphere
of 3D half-light radius Rh
(MWGsrhalf)
203-207 F5.3 --- GmwdRh ? Mass-weighted DM density slope
ΓbarDM within a sphere of 3D
half-light radius Rh (MWGdrhalf)
209-214 F6.3 [-] log(GavtRe) ? Average logarithmic total density
slope Γt between 0.1 and 1
effective radius Re (Gt_Re)
216-221 F6.3 [-] log(GavsRe) ? Average logarithmic stellar
density slope Γ* between 0.1
and 1 effective radius Re (Gs_Re)
223-228 F6.3 [-] log(GavdRe) ? Average logarithmic DM density
slope ΓDM between 0.1 and 1
effective radius Re (Gd_Re)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat table7.dat table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Identifier raw number
7- 12 F6.3 deg i ? Best-fitting inclination angle,
being 90 for edge-on as modelled in
section 3.2 (inc_deg)
14- 19 F6.3 --- Betar ? Best-fitting radial velocity
anisotropy Βrin spherical
coordinates (beta_r)
21- 26 F6.3 [Msun/Lsun] logM/Ls ? Best-fitting stellar mass-to-light
ratio in M☉/L☉ units
(logMLstellar)
28- 48 E21.18 [Msun/kpc3] logrhos ? The characteristic density of NFW
profile (logrhos)
50- 57 F8.3 kpc rs ? The break radius as characteristic
radius of NFW profile (rs)
59- 70 F12.3 --- Kappa ? The ratio between modelled and
observed line-of-sight velocity
field (kappa)
72- 86 E15.9 [Msun] log(Mt<Re) ? Enclosed total stellar
matter+DM+BH mass within a sphere of
circularized effective radius Re
which satisfying that the area of
half-light ellipse A=π*Re2
(logMtRe)
88- 93 F6.3 [Msun] log(Ms<Re) ? Enclosed stellar matter mass
within a sphere of circularized
effective radius Re which satisfying
that the area of half-light ellipse
A=π*Re2 (logMsRe)
95-100 F6.3 [Msun] log(Md<Re) ? Enclosed DM mass within a sphere
of circularized effective radius Re
which satisfying that the area of
half-light ellipse A=π*Re2
(logMdRe)
102-107 F6.3 --- fDM<Re ? DM fraction within a sphere of
effective radius which satisfying
that the area of half-light ellipse
A=π*Re2 (fdm_Re)
109-114 F6.3 [Msun/Lsun] logM/Ldyn ? Best-fitting dynamical
mass-to-light ratio in
M☉/L☉ units (logMLdyn)
116-124 E9.6 --- Chi2 ? The reduced chi-square of
best-fitting model, values are
scaled to account for effect of
standard dev. of the Χ2 itself
and it should be only used in
comparison between models (chi2_dof)
126-144 E19.13 arcsec Rh ? Radius r1/2 of the 3D sphere which
encloses half the total luminosity
of the galaxy (rhalf_arcsec)
146-164 F19.16 [Msun] log(Mt<Rh) ? Enclosed total stellar
matter+DM+BH mass within a sphere of
3D half-light radius Rh
(logMtrhalf)
166-171 F6.3 [Msun] log(Ms<Rh) ? Enclosed stellar matter mass
within a sphere of 3D half-light
radius Rh (logMsrhalf)
173-178 F6.3 [Msun] log(Md<Rh) ? Enclosed DM mass within a sphere
of 3D half-light radius Rh
(logMdrhalf)
180-185 F6.3 --- GmwtRe ? Mass-weighted total density slope
Γbart within a sphere of
effective radius Re (MWGtRe)
187-191 F5.3 --- GmwsRe ? Mass-weighted stellar density
slope Γbar* within a sphere
of effective radius Re (MWGsRe)
193-197 F5.3 --- GmwdRe ? Mass-weighted DM density slope
ΓbarDM within a sphere of
effective radius Re (MWGsRe)
199-203 F5.3 --- GmwtRh ? Mass-weighted total density slope
Γbart within a sphere of 3D
half-light radius Rh (MWGtrhalf)
205-209 F5.3 --- GmwsRh ? Mass-weighted stellar density
slope Γbar* within a sphere
of 3D half-light radius Rh
(MWGsrhalf)
211-215 F5.3 --- GmwdRh ? Mass-weighted DM density slope
ΓbarDM within a sphere of 3D
half-light radius Rh (MWGdrhalf)
217-222 F6.3 [-] log(GavtRe) ? Average logarithmic total density
slope Γt between 0.1 and 1
effective radius Re (Gt_Re)
224-229 F6.3 [-] log(GavsRe) ? Average logarithmic stellar
density slope Γ* between 0.1
and 1 effective radius Re (Gs_Re)
231-236 F6.3 [-] log(GavdRe) ? Average logarithmic DM density
slope ΓDM between 0.1 and 1
effective radius Re (Gd_Re)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
License: CC-BY-4.0
References:
Zhu et al., Paper VII 2025ApJS..280...55Z 2025ApJS..280...55Z
Li et al., Paper VI 2024MNRAS.529.4633L 2024MNRAS.529.4633L
Lu et al., Paper V 2024MNRAS.530.4474L 2024MNRAS.530.4474L
Wang et al., Paper IV 2024MNRAS.527.1580W 2024MNRAS.527.1580W
Zhu et al., Paper III 2024MNRAS.527..706Z 2024MNRAS.527..706Z
Lu et al., Paper II 2023MNRAS.526.1022L 2023MNRAS.526.1022L
Zhu et al., Paper I This work
(End) Luc Trabelsi [CDS] 21-Jul-2026