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An H$\alpha$ kinematic survey of the $Herschel$ Reference Survey -- I. Fabry-Perot observations with the 1.93m telescope at OHP

T0 review · 2 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read This paper builds a homogeneous Hα kinematic sample of 152 nearby star-forming galaxies and uses it to tie baryonic mass to dynamical mass and to define the first dynamical main sequence.

desk verdict The HRS kinematic dataset is the real deliverable; the derived scaling relations need a robustness pass on the α coefficient before their slopes are quoted. read the letter →

arxiv 1908.10295 v1 pith:C4OMNU2W submitted 2019-08-27 astro-ph.GA

Jesús A. Gómez-López , P. Amram , B. Epinat , A. Boselli , M. Rosado , M. Marcelin , S. Boissier , J.-L. Gach
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M. Sánchez-Cruces M. Sardaneta
This is my paper · ORCID
classification astro-ph.GA
keywords galaxykinematicsrotationcurvesTully-Fisherrelationdynamicalmassbaryonicstar-forminggalaxiesFabry-PerotspectroscopyHerschelReferenceSurvey
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Using Fabry-Perot Hα observations of 152 star-forming galaxies from the Herschel Reference Survey, the paper constructs a homogeneous set of 2D velocity fields and rotation curves; combined with 40 galaxies from the literature, this covers 73.6% of the HRS star-forming sample. The paper argues these data are accurate enough that maximum velocities from Hα and H I agree, and that the sample reproduces the i-band, near-infrared, stellar, and baryonic Tully-Fisher relations found from much larger heterogeneous samples. From the same data it derives a baryonic-to-dynamical mass relation with slope 1.11 ± 0.12 and, for the first time, baryonic and dynamical mass main sequences for a representative local sample. A reader should care because this turns the HRS into a local reference anchor for scaling relations connecting gas, stars, and dark matter on a statistical basis.

What carries the argument

The load-bearing machinery is the combination of Voronoi-tessellation adaptive binning that preserves spatial resolution in bright H II regions while recovering faint diffuse emission; a tilted-ring kinematical model in which the observed velocity is $V_{\mathrm{obs}}(r) = V_{\mathrm{sys}} + V_{\mathrm{rot}}(r)\cos\theta\,\sin i$ with $V_{\mathrm{rot}}(r)$ given by a modified Zhao function, fitted by Levenberg-Marquardt $\chi^2$ minimization; a modified Courteau profile $v(r) = v_c (1 + r_t/r)^\beta (1 + (r_t/r)^\gamma)^{1/\gamma}$ with $\beta=0$ to define $V_{\mathrm{max}}$ from the rotation curve; Monte-Carlo uncertainty estimates from the power spectrum of residual velocity fields; and the dynamical-mass estimator $M_{\mathrm{dyn}} = \alpha\, r_{\mathrm{opt}} V_{\mathrm{max}}^2 / G$ with $\alpha = 1.0$ for all galaxies, the $0.6 \le \alpha \le 1.0$ range being shown as a shaded band. The machinery converts several thousand independent velocity measurements per galaxy into one robust $V_{\mathrm{max}}$ and one $M_{\mathrm{dyn}}$ per galaxy.

What would settle it

Take a subset of roughly twenty HRS galaxies with resolved H I rotation curves extending beyond the optical radius, fit disk-plus-bulge-plus-dark-halo mass models, and recover Mdyn independently of the α prescription; if the implied α is systematically below 1 or varies with mass, the reported Mbar-Mdyn slope and the dynamical main sequence will not reproduce.

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Extended reading notes

Core claim

On the paper's own terms, the discovery is that a complete, K-band-selected local sample can yield homogeneous Hα kinematics with quality sufficient to measure global scaling relations: the maximum rotation velocity Vmax derived from a Courteau-profile fit to the Hα rotation curve is statistically indistinguishable from Vmax measured from H I line widths for unperturbed galaxies, and the resulting i-band and 3.6 µm Tully-Fisher relations match literature templates once luminosity distributions are matched. Combining these kinematics with directly measured baryonic components (stars, atomic and molecular gas, helium, metals, dust), the paper finds Mbar ∝ $Mdyn^{1}$.11±0.12 with roughly 0.12 dex scatter and a baryon fraction that rises with dynamical mass; it then introduces the baryonic and dynamical main sequences, where star formation rate scales with baryonic and dynamical mass with nearly the same slope and scatter as the stellar main sequence. The intended significance is that galaxy evolution can be phrased in dynamical rather than stellar mass terms on a statistically representative local sample.

Load-bearing premise

Dynamical masses are computed with a single spherical-mass coefficient α = 1.0 for every galaxy; if galaxies instead behave like flattened discs (α ≈ 0.6), every dynamical mass shrinks by 40% and the quoted scaling relations shift.

Editorial extensions

If this is right

  • The remaining 26.4% of the HRS without Fabry-Perot data can be added to statistical studies using H I line widths, since Vmax,Hα matches Vmax,HI for unperturbed objects.
  • The HRS can serve as a local reference for Tully-Fisher calibrations, giving i-band and 3.6 µm slopes consistent with larger samples once luminosity selection is matched.
  • Baryonic masses assembled from direct measurements of stars, atomic and molecular gas, helium, metals, and dust make baryon fractions an observable function of dynamical mass rather than an assumed input.
  • The main sequence of star formation can be expressed in terms of dynamical mass, extending the classic SFR-stellar-mass relation to a mass tracer closer to the total halo scale.
  • The roughly unit slope of the baryonic-to-dynamical mass relation and its small scatter give local constraints for models of galaxy formation that predict how baryons are distributed within dark-matter halos.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • I infer that if a disc-like correction (α ≈ 0.6) applies, the zero point of the baryonic-to-dynamical mass relation shifts by about 0.22 dex and the reported baryon fractions roughly double; the qualitative trend that low-mass systems are more gas-dominated would likely survive, but the absolute baryon fractions should not be read as model-independent.
  • I infer that a mass-dependent α would change the slope of the dynamical main sequence, so fitting resolved mass models (disk plus bulge plus dark halo) on a subsample is a direct test the paper leaves open.
  • I infer that the homogeneous Vmax catalog is a natural local anchor for high-redshift kinematic surveys, provided they adopt the same Vmax definition, namely a Courteau-profile fit within the optical radius.
  • I infer that because the sample is K-band-selected and volume-limited, the baryonic and dynamical main sequences could separate mass-driven from environment-driven quenching by comparing Virgo and field galaxies at fixed Mdyn.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. Gómez-López et al. present Fabry-Perot Hα datacubes, velocity fields, and rotation curves for 152 HRS star-forming galaxies observed at OHP, and combine these with 40 literature galaxies to reach 192/261 (73.6%) of the HRS late-type sample. The data reduction includes Voronoi adaptive binning, sky-line subtraction, FSR corrections, and a Monte-Carlo residual-field method for parameter uncertainties. Kinematic parameters are derived from a modified Zhao model, and Vmax from a modified Courteau profile. The internal validation is thorough: Vmax,Hα versus Vmax,HI has slope 0.9975±0.01 for Flag A objects, and the i-band, 3.6 μm, stellar, and baryonic Tully-Fisher relations agree with literature samples (Masters et al. 2006, Sorce et al. 2014, McGaugh et al. 2000, Bell & de Jong 2001) and with EAGLE predictions. The paper then uses Mdyn = α ropt Vmax^2/G, fixing α = 1.0 (with 0.6 ≤ α ≤ 1.0 shown as a shaded band), to derive the Mbar-Mdyn relation (slope 1.11±0.12), baryon-fraction trends, and the baryonic and dynamical main sequences (SFR-Mdyn slope 0.87±0.19).

Significance. The survey products are a valuable community resource, and the kinematic pipeline is careful: parameters carry Monte-Carlo uncertainties, quality flags are assigned by an automatic procedure, and the external HI and Tully-Fisher cross-checks are convincing. Public availability through HeDAM and the Fabry-Perot database further strengthens the contribution. If the α systematic is properly propagated, the Mbar-Mdyn relation and the first dynamical main sequence on a representative local sample would be useful constraints for galaxy formation models and simulations. The key validations are against independent external data and published calibrations, so I do not see a circularity problem. The main weakness is that the dynamical-mass-based relations depend on a single fixed α with no propagated systematic error.

major comments (2)
  1. [Section 5.4, Eq. (9), Tables 6-7, Figs. 12-14] The dynamical masses used in the Mbar-Mdyn relation and in the Mdyn main sequence are computed with Mdyn = α ropt Vmax^2/G adopting α = 1.0 for every galaxy, with the 0.6 ≤ α ≤ 1.0 range shown only as a shaded band. This is load-bearing: α is meant to interpolate between disk-like (α ≈ 0.6) and spherical (α ≈ 1.0) mass distributions, and the low-mass, gas-rich galaxies at the low-Mdyn end are exactly the systems expected to be disk-dominated, whereas massive bulge-dominated galaxies should be closer to spherical. If α therefore increases with Mdyn, the slope 1.11±0.12 of the Mbar-Mdyn relation and the slope 0.87±0.19 of the SFR-Mdyn main sequence are biased, and the reported rising baryon fraction with Mdyn in Fig. 13 could be weakened or erased because low-mass galaxies with α ≈ 0.6 would have true baryon fractions roughly 1.7 times larger. I request a quantitative treatment: either propagate a per-galaxy α prior (for example based on morphology or bulge-to-total light ratio), or at minimum quote all fit parameters for both α = 0.6 and α = 1.0 and add a systematic error term to the headline slopes and baryon fractions.
  2. [Section 5.1 and Tables 6-7] After defining the quality flags, the analysis deliberately excludes Flag B and HI-deficient (HI-Def > 0.4) galaxies. These objects are preferentially cluster members with truncated gas discs, so the resulting 123-object sample is not the full HRS and may be biased at the low-mass, high-environment end. Since the abstract and conclusions claim representative local-universe relations, the paper should either qualify the claims as applying to unperturbed systems or show that re-including these galaxies (with appropriate weights or as a robustness test) does not change the fitted slopes and zero points. At minimum, the paper should quantify what fraction of the HRS star-forming population is excluded and discuss the possible selection effect on the reported slopes.
minor comments (4)
  1. [Throughout] There are several typographical errors, including “constitue,” “avalibale,” “gouverned,” and “OSL” where “OLS” is intended; a careful proofreading pass is needed.
  2. [Section 5.5] The sentence “the SFR is studied considering the mean value derived using the three tracers Mdyn, Mbar and Mstar” should read “the three mass estimators,” since SFR is a single physical quantity and the three quantities are galaxy mass tracers.
  3. [Table 5 note] The baryonic mass definition in the Table 5 note, Mbar = Mstar + 1.4(MHI + MH2) + Mz + Mdust, appears inconsistent with Eqs. (6)-(7), where the factor 1/(1-Y-Z) already accounts for both helium and metals; please clarify whether Mz is double-counted.
  4. [Section 5.1, Fig. 7] The text reports an “intrinsic scatter” of 0.82 for the full sample and 0.11 for Flag A galaxies; the units and definition of this scatter should be stated explicitly, since it does not have the usual dex units of a log-log relation.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: scaling relations are independently benchmarked; the fixed Mdyn shape parameter is an acknowledged assumption, not a recycled input.

full rationale

The claimed derivation chain is self-contained with respect to its results. Rotation curves and Vmax are measured from new Fabry-Perot datacubes, not fitted to any of the paper's scaling-relation outputs; the HI comparison (Fig. 7, slope 0.9975 for Flag A) is an external consistency check, not a fitted calibration. The i-band, NIR, stellar, and baryonic Tully-Fisher relations are compared with independent samples (Masters et al. 2006, Sorce et al. 2014, McGaugh et al. 2000, Bell & de Jong 2001, Torres-Flores et al. 2011, EAGLE simulations) using matched luminosity distributions and identical OLS bisector methods, so the agreement is meaningful rather than forced. Dynamical masses are computed from Eq. (9) with a fixed spherical assumption alpha=1.0; the paper explicitly acknowledges this and shows the 0.6<=alpha<=1.0 interval as a shaded band rather than hiding it. That is an unpropagated systematic assumption and a correctness risk, but it is not circular: no fitted parameter is renamed as a prediction, and no target result is used to define its own input. Self-citations to Epinat et al. (2008a,b), Daigle et al. (2006b), and Boselli et al. (2015) concern data-reduction, flux-calibration, and multifrequency reference data that are published independently of this paper's scaling-relation claims; they are not uniqueness theorems or ansatz-carrying citations that force the central results. The paper's own benchmarks are external, and no step reduces equation to equation by construction.

Assumptions & free parameters 5 free parameters · 8 assumptions · 0 invented entities

The kinematic survey itself introduces no new physical entities. The scientific output depends on standard galaxy-model assumptions plus the fitted per-galaxy rotation-curve parameters. The most consequential choice is the uniform α=1.0 in the dynamical mass estimator: it is not fitted to data, but it is chosen by hand and the quoted relations do not include its 0.6-1.0 range. All other inputs are prior published calibrations.

free parameters (5)
  • Virial-shape coefficient α in Mdyn = α ropt Vmax^2 / G = 1.0 (range 0.6-1.0 admitted)
    Set by hand to the spherical model for all galaxies (Section 5.4). Adopting α=0.6 would lower every dynamical mass by 40% and shift the Mbar-Mdyn relation and main sequence zero points; a mass-dependent α would change slopes.
  • Per-galaxy Courteau profile parameters (vc, rt, γ) = varies per galaxy (β fixed to 0)
    Vmax is defined as the maximum of the fitted Courteau profile between r=0 and r_RC (Section 4.1.6). These fits are standard measurement parameters but Vmax, the key dynamical variable, is their output.
  • Per-galaxy kinematic model parameters (PA, i, Vsys, vt, rt, g, a) = varies per galaxy; PA or i fixed to morphological values for 42 and 78 galaxies, respectively
    Used to build the rotation curves (Section 4.1.1). Inclination directly scales Vmax; galaxies with i≥70° or i≤30° are fixed to morphological values because of degeneracies.
  • r24/r25 conversion factor = 0.920 ± 0.01
    Bisector regression on the HRS sample, used to define ropt for the 5 galaxies lacking r24 (Section 4.1.7). Minor but fitted.
  • Fabry-Perot flux calibration coefficient = 1 ph/s = 0.50 ± 0.05 ×10^-13 erg s^-1 cm^-2
    OLS bisector fit forced through the origin against Boselli et al. (2015) Hα fluxes (Section 3.4). Used for Hα maps and SFR-related products, not for the kinematic relations.
assumptions (8)
  • domain assumption Thin rotating disk: Vobs = Vsys + Vrot(r) cosθ sin i, with negligible radial and vertical motions (Eq. 1)
    Standard assumption for late-type galaxy kinematics, invoked in Section 4.1.1 before the Zhao model is fitted.
  • domain assumption Position angle and inclination are constant within the optical radius
    Adopted after Epinat et al. (2008b); justified by small variations inside ropt (Section 4.1.1).
  • domain assumption Modified Zhao and Courteau analytic functions adequately represent the rotation curves and allow Vmax extrapolation
    Four-parameter (then three-parameter) fits used for all galaxies (Eqs. 2 and 3); the choice of Courteau over Zhao changes Vmax, as the authors discuss.
  • domain assumption Lequeux (1983) dynamical mass estimator Mdyn = α ropt Vmax^2/G with uniform α=1.0
    Spherical-model choice in Section 5.4; the paper shows the 0.6≤α≤1.0 interval but does not propagate it.
  • domain assumption HI line width converts as WHI = 2 Vmax,HI sin(i)
    Used in Section 5.1 to derive Vmax,HI from homogenized HI widths of Boselli et al. (2014a).
  • domain assumption Helium mass fraction Y=0.28 and solar metal fraction Z_sun=1.34e-2, 12+log(O/H)_sun=8.69
    From Pagel (2009) and Asplund et al. (2009), used in Eq. 7 to convert hydrogen mass to total gas mass.
  • domain assumption Luminosity-dependent XCO conversion factor (Boselli et al. 2002) for MH2
    Adopted in Eq. 6 for molecular gas mass; prior calibration from the same group.
  • domain assumption Stellar masses, SFRs and metallicities from prior HRS catalogs (Zibetti et al. 2009; Boselli et al. 2013, 2015; Hughes et al. 2013)
    These external data products are inputs to the stellar/baryonic TF and main-sequence fits; the paper does not re-derive them.

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Pith. "Pith review of An H$\alpha$ kinematic survey of the $Herschel$ Reference Survey -- I. Fabry-Perot observations with the 1.93m telescope at OHP." pith.science (2026). https://pith.science/paper/C4OMNU2W

@misc{pith2026190810295,
  author       = {Pith},
  title        = {Pith review of: An H$\alpha$ kinematic survey of the $Herschel$ Reference Survey -- I. Fabry-Perot observations with the 1.93m telescope at OHP},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/C4OMNU2W}},
  note         = {Machine review of arXiv:1908.10295}
}
abstract

We present new 2D high resolution Fabry-Perot spectroscopic observations of 152 star-forming galaxies which are part of the $Herschel$ Reference Survey (HRS), a complete $K$-band selected, volume-limited sample of nearby galaxies, spanning a wide range in stellar mass and morphological type. Using improved data reduction techniques that provide adaptive binning based on Voronoi tessellation, using large field-of-view observations, we derive high spectral resolution (R$>$10,000) H$\alpha$ datacubes from which we compute H$\alpha$ maps and radial 2D velocity fields that are based on several thousand independent measurements. A robust method based on such fields allows us to accurately compute rotation curves and kinematical parameters, for which uncertainties are calculated using a method based on the power spectrum of the residual velocity fields. We check the consistency of the rotation curves by comparing our maximum rotational velocities to those derived from HI data, and computing the $i$-band, NIR, stellar and baryonic Tully-Fisher relations. We use this set of kinematical data combined to those available at other frequencies to study for the first time the relation between the dynamical and the total baryonic mass (stars, atomic and molecular gas, metals and dust), and derive the baryonic and dynamical main sequence on a representative sample of the local universe.

Figures

Figures reproduced from arXiv: 1908.10295 by the authors.

Figure 1
Figure 1. Top panel: Histogram of the stellar mass distribution of the HRS star-forming sample. Bottom panel: Histogram of the galaxy type distribution. Out of the 261 galaxies (white histograms), 152 have been observed at the OHP and are presented in this work (red), while 40 observations are available in the literature (green). galaxies from the following references: GHASP (Garrido et al. 2005; Epinat et al. 2008b), SINGS (… view at source ↗
Figure 2
Figure 2. Top panel (and top-left insert): Hα integrated fluxes measured by GHASP compared with Hα integrated fluxes from Boselli et al. (2015); the solid red line represents the OLS bisector linear regression on the data from which results our calibration; the insert at the top-left shows the same calibration plot but using a linear scale. Bottom panel: normalised residual values, where fNB are fluxes from Boselli et al. (20… view at source ↗
Figure 3
Figure 3. Standard deviation of each residual velocity field as a function of the mean amplitude of the velocity field. The colors correspond to the different quality Flags: red dots are galaxies with Flag “1", yellow triangles are galaxies with Flag “2", green “x" symbols are galaxies with Flag “3" and blue “+" symbols are galaxies with Flag “4". The size of the symbols corresponds to the complementary Flag“A" (big symbols) … view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: Example of the products derived from Fabry-Perot observations. Top left: XDSS R-band image. Top right: Hα velocity field. Middle left: Hα monochromatic image. Middle right: Hα velocity dispersion field. Bottom left: rotation curve. Bottom right: residual velocity field…
Figure 5
Figure 5. Figure 5: Top panel: Histogram of the the difference between the kinematical and morphological PA, where the red part of the histogram represent galaxies for which the kinematical PA has been fixed to the morphological one. The X-axis in the last three panels represents the diff…
Figure 6
Figure 6. Figure 6: Histogram of the difference between the kinematical and morphological inclination; the red part of the histogram represents the galaxies for which the kinematical inclination was fixed to the morphological one. and possibly shift Vmax at a different radius (i.e. galaxy…
Figure 8
Figure 8. Figure 8: Top panel: i-band Tully-Fisher relation. Red and blue dots indicate HRS galaxies with Hα and Hi kinematical data. The solid red line indicates the OLS bisector regression to the HRS data. The dotted blue line represents the template I-band TF relation for the nearby ga…
Figure 9
Figure 9. Figure 9: NIR S4G-3.6µm band Tully-Fisher relation. The dashed blue line represents the Tully-Fisher relation determined by Sorce et al. (2014) for nearby galaxies, while the solid red line the OLS bisector regression to our data. Colors and symbols as in [PITH_FULL_IMAGE:figur…
Figure 10
Figure 10. Figure 10: Stellar Tully-Fisher relation. The dashed green line represents the relation determined by Bell & de Jong (2001), the dashed blue line that of McGaugh et al. (2000), the solid red line the OLS bisector regression to our sample. Colors and symbols are as [PITH_FULL_IM…
Figure 11
Figure 11. Figure 11: Baryonic Tully-Fisher relation. The dashed green line represents the relation determined by McGaugh et al. (2000), the dotted blue line that of Bell & de Jong (2001), the solid red line the OLS bisector regression to our sample. Colors and symbols are as [PITH_FULL_I…
Figure 12
Figure 12. Figure 12: Baryonic versus dynamical mass. Colors and symbols are as in [PITH_FULL_IMAGE:figures/full_fig_p015_12.png]
Figure 14
Figure 14. Figure 14: Relationship between the SFR and Mstar (top panel), Mbar (middle panel), and Mdyn (bottom panel). The OLS bisector regressions are represented with the solid red lines. The colors represent the i−band magnitudes in logarithmic scale. interesting to derive the main seq…
Figure 13
Figure 13. Figure 13: Variation of the different baryonic components to the total baryonic mass of the total dynamical mass, from top to bottom: stellar (first panel), Hi (second panel), H2 (third panel), metal elements (fourth panel), and dust (fifth panel). The black dashed line shows th…

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Works this paper leans on

58 extracted references · 58 canonical work pages

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    Aquino-Ortíz, E., Valenzuela, O., Sánchez, S. F., et al. 2018, MNRAS, 479, 2133 Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481 Bacon, R., Conseil, S., Mary, D., et al. 2017, A&A, 608, A1 Barnes, E. I. & Sellwood, J. A. 2003, AJ, 125, 1164 Bauer, A. E., Drory, N., Hill, G. J., & Feulner, G. 2005, ApJ, 621, L89 Bell, E. F. & de J...

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    A" and Flag “B

    Poor estimation of the rotation curve and Vmax probably not reached. In addition to these 4 flags, we defined a supplementary quality classification flags called Flag “A" and Flag “B". The Flag “B" corresponds to those peculiar cases leading to a non-realistic kinematical fitting: a) Galaxies for which i≥ 70◦, since the absorption e ffects due to high inclinati...

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    Otherwise the agreement between the kinematical and morphological PA of the major axis is perfect

    Because this galaxy is almost edge-on, the kinematical inclination was di fficult to determine and we adopted the morphological value when computing our Hα rotation curve. Otherwise the agreement between the kinematical and morphological PA of the major axis is perfect. The rotation of the redshifted side appears more chaotic because of some faint Hα emissi...

    work page 2015

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    The rotation of the blueshifted side is more chaotic and the outermost part was not taken into account when tracing the rotation curve

    For this edge-on galaxy we adopted the morphological values for the inclination, as well as for the PA of the major axis, when computing our H α rotation curve. The rotation of the blueshifted side is more chaotic and the outermost part was not taken into account when tracing the rotation curve. Indeed, the residual velocity field shows exceedingly large v...

    work page 2015

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    (2015) also shows bright spots

    The H α emission is mainly seen on the southern and western part of the galaxy, where the H α + [NII] image from Boselli et al. (2015) also shows bright spots. The velocity field is dominated by an almost constant value around 1410 km s−1 which could be due to a contamination of the observed velocities by an OH night-sky line (Osterbrock et al. (1996)). As...

    work page 2015

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    The velocity field is regular, except for some high velocity points on the eastern edge of the disc (probably spurious since the H α + [NII] image from Boselli et al

    There is an excellent agreement between the kinematical and morphological inclination (2 ◦ difference) as well as for the PA of the major axis (1◦ difference). The velocity field is regular, except for some high velocity points on the eastern edge of the disc (probably spurious since the H α + [NII] image from Boselli et al. (2015) shows no significant emissi...

    work page 2015

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    (2015) (showing an abrupt fall of emission on the edge of the inner disc)

    The Hα emission is limited to the inner disc of this galaxy and the outer parts of our velocity field are clearly not significant as suggested by the H α + [NII] image from Boselli et al. (2015) (showing an abrupt fall of emission on the edge of the inner disc). This is confirmed by the residual velocity field where extreme values are seen all around the disc...

    work page 2015

  8. [13]

    The Hα + [NII] image from Boselli et al. (2015) suggests that the southwestern extension of the disc, near the strong spiral arm, is spurious (which is confirmed by the extreme values of the residual velocity field) but the easternmost points, on the major axis, seem real. There is a fairly good agreement between the kinematical and morphological inclinatio...

    work page 2015

Show all 58 references
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    Our continuum image is contaminated by many ghost images of field stars as well as by a ghost image of the galaxy itself (about 20 arcsec below the true image of HRS023) caused by a reflection of light between the Fabry-Perot interferometer and the interference filter. The extens...

    2015

  2. [32]

    This face-on galaxy, although it is of Sb type, has almost none Hα emission, as confirmed by the Hα + [NII] image from Boselli et al. (2015). Our Hα image and velocity field are mainly noise and we could not draw any H α rotation curve for this galaxy. HRS

    2015

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    (2015) shows many small HII regions dispersed in the disc that we miss here

    The Hα + [NII] image of this galaxy from Boselli et al. (2015) shows many small HII regions dispersed in the disc that we miss here. Indeed our H α map and velocity field only show the central part of the galaxy and none of these small regions. We find a fairly good agreement be...

    2015

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    We adopted the morphological values for the inclination as well as for the PA of the major axis, when computing our Hα rotation curve

    This galaxy is almost edge-on and the blueshifted side (west) on our H α map seems brighter and more extended than the redshifted side (east), maybe because of dust absorption. We adopted the morphological values for the inclination as well as for the PA of the major axis, whe...

    2015

  5. [61]

    The outermost extension to the north of our Hα map and velocity field is doubtful (there is no hint of any counterpart there on the Hα + [NII] image from Boselli et al

    This galaxy is almost edge-on and the agreement between kinematical and morphological inclination is not very good (9◦ difference) but it is perfect for the PA of the major axis. The outermost extension to the north of our Hα map and velocity field is doubtful (there is no hint ...

    2015

  6. [67]

    The faint extension of our H α map and velocity field, on the southern side of the galaxy, seems spurious (no counterpart can be seen on the H α + [NII] image from Boselli et al. 2015). We adopted the morphological value of the inclination for computing our H α rotation curve a...

    2015

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    This galaxy is almost face-on and the Hα emission is concentrated in the center of the disc, as confirmed by the Hα + [NII] image from Boselli et al. (2015). As a result, the dispersion is very high in the outer parts of the velocity field, as can be seen also on the residual ve...

    2015

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    The lack of H α emission on the northern side (redshifted) of this galaxy is confirmed by the Hα + [NII] image from Boselli et al. (2015). The high inclination of the disc led us to adopt the morphological values for the inclination and for the PA of the major axis when computi...

    2015

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    The Hα emission is brighter on the northern side (blueshifted) of this galaxy, as can be seen also on the Hα + [NII] image from Boselli et al

    The agreement between morphological and kinematical values is rather good for the inclination as well as for the PA of the major axis. The Hα emission is brighter on the northern side (blueshifted) of this galaxy, as can be seen also on the Hα + [NII] image from Boselli et al....

    2015

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    The Hα emission is much brighter on the southern part of the disc of this galaxy, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). As a result, our Hα rotation curve is mainly traced by the blueshifted side (south). Also, there is some lack of emission i...

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    (2015), led to think that its disc is more inclined than suggested by the morphological value (56 ◦)

    The very thin stripe of Hα emission of this galaxy, as can be seen also on the Hα + [NII] image from Boselli et al. (2015), led to think that its disc is more inclined than suggested by the morphological value (56 ◦). Anyway, we adopted that value when tracing our H α rotation...

    2015

  12. [104]

    This Sb type galaxy has no significant Hα emission, as confirmed by the Hα + [NII] image from Boselli et al. (2015). No H α velocity field nor rotation curve could be extracted from our data. Note also that the isolated spot at about 30 arcsec north from the nucleus is probably b...

    2015

  13. [112]

    There is some di ffuse Hα emission in the disc of this galaxy but its surface brightness is very faint, as can be seen also on the H α + [NII] image from Boselli et al. (2015). As a result, the signal to noise ratio of our H α map is also very faint and, despite the relatively ...

    2015

  14. [117]

    This galaxy is almost edge-on and we adopted the morphological values for the inclination and for the PA of the major axis when computing our H α rotation curve. The Hα emission is limited to a few spots in the central part of the disc of this galaxy, mainly on the southwester...

    2015

  15. [118]

    Apart a few bright spots in the center, the Hα emission of this galaxy is rather faint in this galaxy, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). Nevertheless it covers fairly well the optical disc of the galaxy. We adopted the morphological value ...

    2015

  16. [133]

    (2015) show that we miss the outermost emission regions on the western side (redshifted) of the disc

    The comparison of our H α map with the H α + [NII] image from Boselli et al. (2015) show that we miss the outermost emission regions on the western side (redshifted) of the disc. This galaxy is almost edge-on and we adopted the morphological values for the inclination as well ...

    2015

  17. [134]

    Although this edge-on galaxy is classified as Sc type, its Hα emission is limited to two bright spots on each side of the nucleus, as confirmed by the H α + [NII] image from Boselli et al. (2015). We adopted the morphological values for the inclination as well as for the PA of t...

    2015

  18. [136]

    This Sa type galaxy has no significant Hα emission, as confirmed by the Hα + [NII] image from Boselli et al. (2015). The spots on our maps are probably more noise than signal and no H α rotation curve can be obtained for this galaxy. HRS

    2015

  19. [142]

    There is a strong H α emission in the inner disc of this Sa type galaxy but it is very faint beyond the e ffective radius, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). Despite the relatively high inclination of the disc, the gradient of the H α veloci...

    2015

  20. [148]

    2015), maybe because of dust absorption

    The disc of this almost edge-on galaxy appears more extended on the southeastern side (redshifted), both on continuum images and Hα images (also on the Hα + [NII] image from Boselli et al. 2015), maybe because of dust absorption. We adopted the morphological values for the inc...

    2015

  21. [157]

    The Hα emission is rich and perfectly covers the whole optical disc of this Sbc type galaxy. We find a perfect agreement between the morphological and kinematical values of the inclination and a rather good agreement between the morphological and kinematical values of the PA of...

    2015

  22. [164]

    No significant Hα emission can be detected in this Sa type galaxy, as confirmed by the H α + [NII] image from Boselli et al. (2015). We could not draw any velocity field nor rotation curve. HRS

    2015

  23. [171]

    The extension that can be seen on the northern side of the galaxy on our maps seems doubtful when comparing with the Hα + [NII] image from Boselli et al

    The Hα emission of this Sbc galaxy is very bright but limited to the inner disc. The extension that can be seen on the northern side of the galaxy on our maps seems doubtful when comparing with the Hα + [NII] image from Boselli et al. (2015) and we did not take it into account...

    2015

  24. [184]

    There is but a small patch of H α emission in the center of this Sa type galaxy, as confirmed by the H α + [NII] image from Boselli et al. (2015). The other small spots on our maps are but noise or ghost image. We could not draw any realistic velocity field nor rotation curve. HRS

    2015

  25. [185]

    The H α emission of this Sa galaxy has a faint surface brightness and is mainly located in a central ring of about 10 arcsec radius, as can be seen also on the H α + [NII] image from Boselli et al. (2015). Its disc is almost face-on and we adopted the morphological value for t...

    2015

  26. [189]

    The H α emission of this galaxy is asymmetric, with a very bright patch north of the nucleus, otherwise it is distributed rather uniformly in the central disc, as can be seen also on the H α + [NII] image from Boselli et al. (2015). We find a rather good agreement between the m...

    2015

  27. [192]

    The Hα emission of this Sa type galaxy is limited to a few spots in the very center, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). We nevertheless tried to draw the Hα rotation curve, using the morphological values of the inclination and PA of the maj...

    2015

  28. [195]

    No significant Hα emission can be seen in this Sab galaxy, as confirmed by the Hα + [NII] image from Boselli et al. (2015). The few spots seen on our maps are probably but noise. We could not draw any realistic velocity field nor rotation curve. HRS

    2015

  29. [199]

    The Hα emission of this Sb galaxy is very bright but limited to the inner disc as can be seen also on the H α + [NII] image from Boselli et al. (2015). We find an acceptable agreement between the morphological and kinematical values of the inclination (16 ◦ difference) but a qui...

    2015

  30. [225]

    The Hα emission of this Sb type galaxy is limited to a fuzzy patch on the southeastern side of the nucleus, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). The faint northern spot seen on our H α map is probably but noise. We nevertheless tried to draw ...

    2015

  31. [238]

    The large extension bordering the whole northeastern side of the disc has a very faint surface brightness and seems doubtful (N.B

    The H α emission of this Sm galaxy is rather faint and patchy. The large extension bordering the whole northeastern side of the disc has a very faint surface brightness and seems doubtful (N.B. It was not imaged by Boselli et al. 2015). The fact that all this area appears with...

    2015

  32. [252]

    The disc of this Sd galaxy is peppered with many bright HII regions covering almost completely the southern part of its optical disc, but less numerous on the northern side (redshifted) as can be seen also on the H α + [NII] image from Boselli et al. (2015). We find an excellen...

    2015

  33. [255]

    The spiral pattern of this Scd galaxy is underlined by many HII regions, as can be seen on the H α + [NII] image from Boselli et al. (2015). This galaxy is not far from face-on, we adopted the morphological value for the inclination of its disc and find a large di fference betwe...

    2015

  34. [256]

    The Hα emission is bright but limited to the inner disc of this Sa type galaxy, as can be seen also on the H α + [NII] image from Boselli et al. (2015). Despite the relatively high inclination of the disc, the velocity gradient of the H α velocity field of this galaxy is rather...

    2015

  35. [276]

    The Hα emission of this Sbc type galaxy covers fairly well the northeastern side of the optical disc but is patchy for the southwestern side (redshifted) as can be seen also on the H α + [NII] image from Boselli et al. (2015). We adopted the morphological value for the inclina...

    2015

  36. [278]

    The Hα emission of this edge-on Sb type galaxy has a faint surface brightness and is limited to the inner disc as can be seen also on the H α + [NII] image from Boselli et al. (2015). We adopted the morphological values for the inclination and for the PA of the major axis when...

    2015

  37. [280]

    The Hα emission of this Sb type galaxy shows a bright inner disc, with an extension of faint surface brightness on the western extremity of the disc (blueshifted side) as can be seen also on the H α + [NII] image from Boselli et al. (2015). The inclination of the disc is rathe...

    2015

  38. [291]

    We cannot check if they are real or mere noise since it was not imaged by Boselli et al

    The Hα emission of this Sab type galaxy is limited to a few faint spots around the nucleus. We cannot check if they are real or mere noise since it was not imaged by Boselli et al. (2015). We could not draw any reliable H α velocity field nor rotation curve. HRS

    2015

  39. [292]

    The H α emission of this Sb type galaxy is very bright but limited to the inner disc, as can be seen also on the H α + [NII] image from Boselli et al. (2015). We find an acceptable agreement between the morphological and kinematical values of the PA of the major axis (14◦ differ...

    2015

  40. [294]

    Apart from a few bright spots, the Hα emission of this edge-on Sb type galaxy has a rather faint surface brightness, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). We adopted the morphological values for the inclination and for the PA of the major axis...

    2015

  41. [297]

    It is strongly inclined and we adopted the morphological values for the inclination as well as for the PA of the major axis when computing our rotation curve

    The whole optical disc of this Sbc type galaxy is peppered with bright HII regions. It is strongly inclined and we adopted the morphological values for the inclination as well as for the PA of the major axis when computing our rotation curve. Despite some waves on both sides, ...

    2015

  42. [300]

    (2015) that shows only a very faint fuzzy spot in the center

    There is no significant H α emission in this Sab type galaxy, as confirmed by the Hα + [NII] image from Boselli et al. (2015) that shows only a very faint fuzzy spot in the center. The spots on our maps are probably more noise than signal and we could not draw any reliable H α v...

    2015

  43. [301]

    The whole optical disc of this Sc type galaxy is peppered with numerous HII regions as can be seen also on the Hα + [NII] image from Boselli et al. (2015). We find a good agreement between the morphological and kinematical values of the inclination (8◦ difference) as well as bet...

    2015

  44. [305]

    The Hα emission of this peculiar galaxy is limited to two relatively bright spots on each side of the nucleus, as can be seen also on the Hα + [NII] image from Boselli et al. (2015). Some velocity gradient can be seen anyway on our velocity field and we adopted the morphologica...

    2015

  45. [308]

    The H α emission of this Sb type galaxy is limited to a faint fuzzy central patch as can be seen also on the Hα + [NII] image from Boselli et al. (2015). Anyway, our velocity field shows some gradient and we tried to draw the rotation curve. The disc is strongly inclined and we...

    2015

  46. [314]

    The H α emission of this Sd type galaxy is asymmetric, with brighter HII regions on the northern side (blueshifted) as can be also on the H α + [NII] image from Boselli et al. (2015). The whole optical disc is nevertheless well covered on both sides by ionized gas. We find a go...

    2015

  47. [317]

    We then find an excellent agreement between the morphological and kinematical values of the PA of the major axis (less than 1◦ difference) when computing our Hα rotation curve

    This galaxy is almost edge-on and we adopted the morphological value for the inclination. We then find an excellent agreement between the morphological and kinematical values of the PA of the major axis (less than 1◦ difference) when computing our Hα rotation curve. Despite the ...

    2015

  48. [321]

    The Hα emission of this Sb type galaxy is very bright but limited to the inner disc as can be seen also on the Hα + [NII] image from Boselli et al. (2015). We adopted the morphological value for the inclination and find a good agreement between the morphological and kinematical...

    2015

  49. [323]

    The Hα emission of this almost edge-on Sb galaxy is asymmetric, much brighter on the northern side (blueshifted), as can be seen also on the Hα + [NII] image from Boselli et al. (2015). We adopted the morphological values for the inclination as well as for the PA of the major ...

    2015

  50. [2012]

    2014a); the solid black curve is the best fit Courteau function to the rotation curve

    and the green horizontal line the HI Vmax (if available in Boselli et al. 2014a); the solid black curve is the best fit Courteau function to the rotation curve. Article number, page 37 of 43 A&A proofs: manuscript no. ms Appendix E: Tables Article number, page 38 of 43 Gómez-Ló...

    2000

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Reviewed August 14, 2026 · model on record in the stance chip above.