J/ApJS/280/55 MaNGA DynPop. VII. Circular velocity curves (Zhu+, 2025)
MaNGA DynPop.
VII. A unified bulge-disk-halo model for explaining diversity in circular
velocity curves of 6000 spiral and early-type galaxies.
Zhu K., Cappellari M., Mao S., Lu S., Li R., Shi Y., Simon D.A., Fu Y.,
Wang X.
<Astrophys. J. Suppl. Ser., 280, 55 (2025)>
=2025ApJS..280...55Z 2025ApJS..280...55Z
ADC_Keywords: Galaxies, radius; Spectra, optical; Space velocities
Keywords: Galaxy dynamics ; Galaxy formation ; Galaxy evolution ;
Galaxy structure ; Galaxy mass distribution
Abstract:
We derive circular velocity curves (CVCs) from stellar dynamical
models for ∼6000 nearby galaxies in the final data release of the
Sloan Digital Sky Survey-IV MaNGA survey with integral-field
spectroscopy, exploring connections between the inner gravitational
potential (traced by CVC amplitude/shape) and galaxy properties. The
maximum circular velocity (Vcircmax) and circular velocity at the
half-light radius (Vcirc(Remaj)) both scale linearly with the
stellar second velocity moment σe2=<V2+σ2> within
the half-light isophote, following Vcircmax∼1.72σe
(7% error) and Vcirc(Remaj)∼1.62σe (7% error). CVC shapes
(rising, flat, declining) correlate strongly with structural and
stellar population properties: declining curves dominate in massive,
early-type, bulge-dominated galaxies with old, metal-rich stars and
early quenching, while rising CVCs prevail in disk-dominated systems
with younger stellar populations and ongoing star formation. Using a
unified bulge-disk-halo model, we predict CVC shapes with minimal
bias, identifying three governing parameters: bulge-to-total mass
ratio (B/T), dark matter fraction within Re, and bulge Sersic index.
The distribution of CVC shapes across the mass-size plane reflects
evolutionary pathways driven by (i) in situ star formation (spurring
bulge growth) and (ii) dry mergers. This establishes CVC morphology as
a diagnostic for galaxy evolution, linking dynamical signatures to
structural and stellar population histories.
Description:
We performed the Jeans anisotropic modeling (JAM;
Cappellari 2008MNRAS.390...71C 2008MNRAS.390...71C & 2020MNRAS.494.4819C 2020MNRAS.494.4819C) to construct
dynamical models for the whole MaNGA sample in Zhu+ (2023MNRAS.522.6326Z 2023MNRAS.522.6326Z).
Throughout this paper, we use the circular velocity in the equatorial
plane (z=0), which means r=(R2+z2)0.5=R.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 109 10296 Parameters of circular velocity curves for
6000 nearby galaxies
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See also:
J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/469/2539 : New classification of CALIFA galaxies (Kalinova+, 2017)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
J/MNRAS/477/4711 : Stellar angular momentum for MaNGA galaxies (Graham+, 2018)
J/MNRAS/483/2057 : SDSS-IV MaNGA Morphological Catalogues (Fischer+, 2019)
J/MNRAS/527/7438 : MaNGA kinematic catalogue (Ristea+, 2024)
http://manga-dynpop.github.io/ : MaNGA DynPop project
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PlateIFU Plate ID + IFU design ID
13- 21 A9 --- MaNGAId Unique MaNGA identifier
23- 29 F7.3 Mpc DA [16.3/556]? Angular diameter distance (1)
31- 36 F6.3 arcsec Re [0.6/30]? Effective radius
38- 43 F6.3 arcsec amaj [0.79/31.5]? Major axis of SDSS r-band
elliptical half-light isophote from MGE
fitting
45- 49 F5.3 arcsec FWHM [2/3.2]? r-band PSF FWHM value of IFU
observation
51- 56 F6.3 arcsec R(Vcmax) [2.16/27.43]? Galactocentric radius at
maximum circular velocity
58- 63 F6.3 arcsec rmax [2.66/27.43]? Largest radius of the Voronoi
bins
65- 72 F8.3 km/s Vc(Re) [22/2636.2]? Circular velocity at half-light
radius in equatorial plane
74- 81 F8.3 km/s Vc(amaj) [22.1/2637.1]? Circular velocity at major
axis of half-light ellipse in equatorial
plane
83- 90 F8.3 km/s Vcmax [18.98/3697]? Maximum circular velocity
within kinematic data range
92- 99 F8.3 km/s Vc(rmax) [18.98/3697]? Circular velocity at rmax
101- 106 F6.3 [Msun] logMBH [0.25/11.87]? Log central super massive
black hole mass (2)
108- 109 I2 --- Qual [-1/3] JAM model quality (-1 to 3 from worst
to best) (3)
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Note (1): Which assumes a flat Universe with Ωm=0.307 and h=0.677
(Planck Coll. 2016A&A...594A..13P 2016A&A...594A..13P).
Note (2): Adopted in our dynamical models, which is derived from scaling
relation (see Section 2.2).
Note (3): Only galaxies with Qual≥1 have reliable CVC measurements.
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History:
From electronic version of the journal
License: CC-BY-4.0
References:
Zhu et al. Paper I. 2023MNRAS.522.6326Z 2023MNRAS.522.6326Z
Lu et al. Paper II. 2023MNRAS.526.1022L 2023MNRAS.526.1022L
Zhu et al. Paper III. 2024MNRAS.527..706Z 2024MNRAS.527..706Z
Wang et al. Paper IV. 2024MNRAS.527.1580W 2024MNRAS.527.1580W
Lu et al. Paper V. 2024MNRAS.530.4474L 2024MNRAS.530.4474L
Li et al. Paper VI. 2024MNRAS.529.4633L 2024MNRAS.529.4633L
Zhu et al. Paper VII. 2025ApJS..280...55Z 2025ApJS..280...55Z This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Jun-2026