J/A+A/709/A120 z∼1 star-forming galaxies Tully-Fisher relation (Jeanneau+, 2026)
MUSE-DARK. II. 3D morpho-kinematic modelling of strongly lensed galaxies:
I. Tully-Fisher relation of z ∼ 1 star-forming galaxies.
Jeanneau A., Richard J., Bouche N.F., Krajnovic D., Ciocan B.-I.,
Freundlich J., Epinat B., Contini T.
<Astron. Astrophys. 709, A120 (2026)>
=2026A&A...709A.120J 2026A&A...709A.120J (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, rotation ; Models ;
Gravitational lensing
Keywords: gravitational lensing: strong - methods: data analysis -
galaxies: evolution - galaxies: formation - galaxies: high-redshift -
galaxies: kinematics and dynamics
Abstract:
Extending local kinematic studies to earlier cosmic times is valuable
to understand how galaxies evolve in relation to their dark matter
haloes.
In a series of papers on lensed kinematics, we seek to combine the
sensitivity of 3D forward modelling to low signal-to-noise ratio
outskirts with the enhanced spatial resolution provided by cluster
lensing.
In this first paper, we (i) present and validate our methodology,
which directly constrains the source parameters by incorporating
lensing deflections into the GalPaK3D forward-modelling algorithm, and
(ii) investigate the evolution of the stellar-mass and baryonic-mass
Tully-Fisher relations (sTFR and bTFR) since z∼1 as a demonstration.
We define a robust sample of strongly lensed star-forming galaxies
(SFGs) from the MUSE Lensing Cluster survey, spanning magnifications
mu=1.4-12.4 and stellar masses M*=108.1-1010.3M☉_. Using a
series of mock galaxies representative of our sample, we find that our
method is significantly more reliable at recovering morpho-kinematic
properties than approaches that ignore differential magnification,
even for relatively modest magnifications (mu<6). Restricting the
analysis to 95 rotationally supported SFGs with well-constrained
velocities, we find a significant evolution of the sTFR zero-point
(ΔbsTFR=-0.42+0.05-0.05dex in stellar mass) but no
detectable evolution of the bTFR zero-point
(ΔbbTFR=0.00+0.06-0.06dex in baryonic mass) relative to
z∼0. Our results are consistent with a mild evolution of the
stellar-to-halo mass ratio and support the view that the sTFR has
evolved only weakly over the past ∼8Gyr, aside from shifts driven by
the redshift dependence of halo-defining quantities such as the
critical density and overdensity. The absence of detectable evolution
in the bTFR zero-point suggests that the increasing contribution of
cold gas mass at higher redshift fully compensates the evolution
observed in the stellar component alone.
Description:
Catalog used in the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 308 95 Catalog (table E1)
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See also:
J/ApJS/235/14 : HFF-DeepSpace photometric cat. of 12 HFF fields
(Shipley+, 2018)
J/A+A/646/A83 : 12 massive lensing clusters MUSE observations (Richard+, 2021)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Cluster Name of the lensing cluster (CLUSTER) (1)
12- 16 I5 --- IdR21 Source ID from the MUSE Atlas of Lensing
Clusters (Richard et al.,
2021A&A...646A..83R 2021A&A...646A..83R, Cat. J/A+A/646/A83)
(ID_R21)
18- 72 A55 --- IdHFFDS Source ID from the HFF-DeepSpace catalogue
(Shipley et al., 2018ApJS..235...14S 2018ApJS..235...14S,
Cat. J/ApJS/235/14) (ID_HFFDS)
74- 83 F10.6 deg RAdeg Right ascension (J2000) of the
morphological centre (RA)
85- 94 F10.6 deg DEdeg Declination (J2000) of the
morphological centre (DEC)
96-103 F8.6 --- zR21 Systemic redshift from the MUSE Atlas of
Lensing Clusters (Z_R21)
105-113 F9.6 --- muR21 Lensing magnification from the MUSE Atlas
of Lensing Clusters (MU_R21)
115-123 F9.6 --- S/NMax S/N of the brightest [OII] spaxel
(S/N_MAX)
125-132 F8.6 arcsec RPSF MUSE PSF radius (R_PSF)
134-141 F8.6 arcsec Reff Effective radius from a single-Sersic fit
to the F160W flux (EFF_RADIUS)
143-151 F9.6 deg Incl Inclination from a single-Sersic fit
to the F160W flux (INCLINATION)
153-162 E10.5 --- FB/T Bulge-to-total flux ratio in the
F160W band (B/T_FLUX)
164-172 F9.6 [Msun] b_logM* 16th percentile of the log10 stellar mass
posterior (LOGMSTAR16)
174-182 F9.6 [Msun] logM* Median of the log10 stellar mass posterior
(LOGMSTARMED) (2)
184-192 F9.6 [Msun] B_logM* 84th percentile of the log10 stellar mass
posterior (LOGMSTAR84)
194-203 E10.5 [Msun/yr] b_logSFR 16th percentile of the log10 star
formation rate posterior (LOGSFR16)
205-213 F9.6 [Msun/yr] logSFR Median of the log10 star formation rate
posterior (LOGSFRMED) (2)
215-223 F9.6 [Msun/yr] B_logSFR 84th percentile of the log10 star
formation rate posterior (LOGSFR84)
225-233 F9.6 [Msun] logMHI log10 atomic gas mass (including Helium)
inferred from scaling relations (LOG_MHI)
235-243 F9.6 [Msun] logMMol log10 molecular gas mass inferred from
scaling relations (LOG_MMOL)
245-253 F9.6 [Msun] logMBar log10 total baryonic mass (LOG_MBAR)
255-262 F8.6 [km/s] logV1.8 Median of the log10 circular velocity
posterior at 1.8 Re (GalPaK3D + Lensing)
(LOGV1.8MED)
264-271 F8.6 [km/s] s_logV1.8 Standard deviation of the log10 circular
velocity posterior at 1.8 Re
(GalPaK3D + Lensing) (LOGV1.8STD)
273-280 F8.6 [km/s] logV2.0 Median of the log10 circular velocity
posterior at 2.0 Re (GalPaK3D + Lensing)
(LOGV2.0MED)
282-289 F8.6 [km/s] s_logV2.0 Standard deviation of the log10 circular
velocity posterior at 2.0 Re
(GalPaK3D + Lensing) (LOGV2.0STD)
291-299 F9.6 km/s sigma0 Median of the log10 velocity dispersion
posterior (GalPaK3D + Lensing) (SIG0_MED)
301-308 F8.6 km/s s_sigma0 Standard deviation of the log10 velocity
dispersion posterior (GalPaK3D + Lensing)
(SIG0_STD)
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Note (1): The MACS0416 North (N) and South (S) pointings have been analysed
separately.
Note (2): Stellar masses and star formation rates have been converted to the
Chabrier (2003PASP..115..763C 2003PASP..115..763C) initial mass function.
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Acknowledgements:
From Alexandre Jeanneau, alexandre.jeanneau(at)univ-lyon1.fr
This work utilises gravitational lensing models produced by PIs
Natarajan & Kneib (CATS), Sharon, Keeton, Diego, and the GLAFIC group.
This lens modeling was partially funded by the HST Frontier Fields
program conducted by STScI. STScI is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NAS
5-26555. The lens models were obtained from the Mikulski Archive for
Space Telescopes (MAST). Beyond those already cited, this work makes
use of the following open-source Python libraries: Astropy, NumPy,
matplotlib, MPDAF, SciPy, and corner. NB and BC acknowledge support
from the ANR DARK grant (ANR-22-CE31-0006).
References:
Ciocan et al. Paper I 2026A&A...708A.112C 2026A&A...708A.112C
License: CC-BY-4.0
(End) Patricia Vannier [CDS] 30-Mar-2026