11institutetext: Departamento de Física Teórica, Universidad Autónoma de
Madrid, 28049 Madrid, Spain 22institutetext: CIAFF, Universidad Autónoma de
Madrid, 28049 Madrid, Spain 33institutetext: Instituto de Astrofísica, Óptica
y Electrónica, 72840 Puebla, México 44institutetext: Institute of Astronomy,
University of Cambridge, Madingley Road, Cambridge, UK 55institutetext:
Facultad de Astronomia y Geofisica, Universidad de La Plata, La Plata,
Argentina 66institutetext: Instituto de Investigación Multidisciplinar en
Ciencia y Tecnología, Universidad de La Serena, La Serena, Chile.
77institutetext: Departamento de Astronomía, Universidad de La Serena, La
Serena, Chile.

# Physical properties of circumnuclear ionising clusters. III. Kinematics of
gas and stars in NGC 7742

S. Zamora , PhD fellow of Ministerio de Educación y Ciencia, Spain,
BES-2017-080509, CEAL-AL/2017-021122 A. I. Díaz 1122 Roberto Terlevich 334455
Elena Terlevich 3355 R. Amorín 6677

(Received XXX; accepted YYY)

###### Abstract

Aims.  In this third paper of a series, we study the kinematics of the ionised
gas and stars, calculating the dynamical masses of the circumnuclear star-
forming regions in the ring of of the face-on spiral NGC 7742.

Methods.  We have used high spectral resolution data from the MEGARA
instrument attached to the Gran Telescopio Canarias (GTC) to measure the
kinematical components of the nebular emission lines of selected HII regions
and the stellar velocity dispersions from the CaT absorption lines that allow
the derivation of the associated cluster virialized masses.

Results.  The emission line profiles show two different kinematical
components: a narrow one with velocity dispersion $\sim$ 10 km/s and a broad
one with velocity dispersion similar to those found for the stellar absorption
lines. The derived star cluster dynamical masses range from 2.5 $\times$ 106
to 10.0 $\times$ 107 M⊙.

Conclusions.  The comparison of gas and stellar velocity dispersions suggests
a scenario where the clusters have formed simultaneously in a first star
formation episode with a fraction of the stellar evolution feedback remaining
trapped in the cluster, subject to the same gravitational potential as the
cluster stars. Between 0.15 and 7.07 % of the total dynamical mass of the
cluster would have cooled down and formed a new, younger, population of stars,
responsible for the ionisation of the gas currently observed.

###### Key Words.:

ISM: abundances – ISM: H II regions – galaxies: ISM – galaxies: starburst –
galaxies: star clusters – galaxies: star formation

##  1 Introduction

Circumnuclear Star Forming Regions (CNSFR), also referred to as “hotspots”,
are similar to luminous and large disk HII regions, but look more compact and
show higher peak surface brightness (Kennicutt et al., 1989). In early type
spirals they are expected to be of higher metallicity as it corresponds to
their position near the galactic bulge (Díaz et al., 2007). In many cases,
CNSFR contribute substantially to the emission of the entire nuclear region
seen in the presence of an active nucleus. In fact, their large H$\alpha$
luminosities, typically higher than 1039 erg s-1, overlap with those of HII
galaxies pointing to relatively massive star clusters as their ionization
source. Hence, these regions constitute excellent places to study how star
formation proceeds in circumnuclear environments.

In previous works Hägele et al. (2007, 2009, 2010) analysed long slit high
spectral resolution data of CNSFR in three nearby galaxies, NGC 3351, NGC 2903
and NGC 3310. They used the 4.2-m William Herschel Telescope (WHT) and the
ISIS spectrograph in the blue and red configurations which provides a
comparable velocity resolution of about 13 km/s in both spectral ranges. The
H$\beta$ and [OIII]$\lambda$5007 Å emission lines and the CaII triplet lines
(CaT) were present in the spectra thus allowing the measurement of the gas and
star velocity dispersions which, together with their sizes measured on
WPC2-HST camera and assuming virialization, made possible the derivation of
the dynamical masses of the young clusters in the regions. These masses, found
to be between 4.9 $\times$ 106 and 1.9 $\times$ 108 M⊙, seem to be rather high
pointing to star-forming complexes rather than individual clusters. However,
the masses of the corresponding ionizing clusters, as derived from H$\alpha$
luminosities under the assumption of no photon escape, only accounts for
between 1 % and 10 % of the derived dynamical mass which raises the question
of the possible presence of more than one stellar population in these massive
circumnuclear star clusters.

On the other hand, one of the main results of these works shows that for the
three observed galaxies, the gas velocity dispersions as measured from
hydrogen recombination lines (H$\beta$ and Paschen emission lines) are found
to be considerably smaller (by about 25 km/s) than those measured from the
stellar CaT lines. In turn, the velocity dispersion obtained from the
[OIII]$\lambda$5007 Å line is very close to the measured stellar one. This
result suggests the possible existence of two kinematically distinct
components in the gas in all regions, although not all of them being
associated with the ionising clusters (see Hägele et al., 2013).

The best possibility to resolve this question is to gather observations with
both high spatial and spectral resolution simultaneously. At present, the
ideal instrument to do this is MEGARA, a high-resolution integral field
spectrograph (IFS) installed on the 10.4-m GTC telescope, covering a field of
view (FoV) of 12.5 × 11.3 arcsec2 with a spatial resolution of 0.62 arcsec and
a spectral range from 3650 to 9700 Å at three different resolutions, R $\sim$
6000, 12000, and 20000. The MEGARA spatial and spectral resolution
characteristics ensure the proper identification and resolution of the
ionising clusters present in CNSFR so that the derived masses obtained can be
meaningful and reliable.

In the first paper of this series, we have analysed CNSFRs in the galaxy NGC
7742 using IFS data obtained with the MUSE spectrograph which provides
spectral resolutions between R $\sim$ 1770 - 3590 at 4800 and 9300 Å
respectively. This galaxy is classified as an SA(r)b galaxy and its morphology
is dominated by a circumnuclear ring located at around 1 kpc from the galaxy
centre. The galaxy harbours a mildly active nucleus whose spectrum is
dominated by emission lines characteristic of both LINER and HII regions. In
total, 88 ring HII regions with H$\alpha$ fluxes larger than 10-18erg/s/cm2
were selected and characterised using their nebular spectra with the help of
photoionization and stellar population synthesis models (Cloudy and PopStar,
respectively). These regions seem to be ionised by young clusters with mean
ages of about 5 Ma. The chemical composition of the ionised gas was calculated
using sulphur as tracer and were found to be between 0.25 and 2.4 times the
solar value, with most regions showing values slightly below solar. This
result is consistent with the effective temperature of the cluster stars,
between 35000 K and 40000 K as estimated from the ratio of HeI to H ionising
photons. The high spatial resolution offered by MUSE allowed the measurement
of the CNSFR sizes on H$\alpha$ flux maps, all of them being spatially
resolved. These measured sizes are fully consistent with those predicted by
photoionisation models, thus leaving little room for photon escape and
justifying the assumption of the regions being radiation bounded. The young
ionising star clusters powering this radiation have masses around 3.5 $\times$
104 M⊙, comparable to the mass of ionised gas and about 19 % of the corrected
photometric cluster mass that includes a young non ionising stellar population
whose estimated age is around 300 Ma. A minor merger scenario is proposed for
the formation of these clusters due to the counter rotating nature of the ring
(Pizzella et al., 2004; de Zeeuw et al., 2002) and the homogeneity of
abundances and continuum colours.

The present work is focused on three principal objectives. First, testing the
capabilities of the new MEGARA instrument for the study of resolved
kinematical components in the ionised gas of HII regions; second, determining
the kinematic origin of such components if present, for which observing both
recombination lines (H$\alpha$) and collisionally excited lines ([NII] and
[SIII] is needed; and third, measuring the stellar velocity dispersion along
the line of sight from the CaT lines in order to derive cluster dynamical
masses. Accomplishing these objectives will ensure the cluster origin of the
CaT lines and the reliability of this derivation. It should be said that a
proper comparison between ionising and dynamical masses for ionising young
star clusters has not yet been done and is much needed.

In Section 2, we describe the observations and the reduction of the data,
focusing on the new MEGARA observations. Section 3 is devoted to the
presentation of our results. The discussion of cluster sizes and dynamical
masses and the comparison between gas and star kinematical components is
presented in Section 4. Finally, Section 5 summarizes this work and our
conclusions.

##  2 Observations and data reduction

In this work, we have used data for the ring HII regions of NGC 7742 (J2000,
RA=356.065542 deg, DEC=10.767083 deg, Skrutskie et al., 2006) obtained with
the high resolution integral field spectrograph MEGARA (Multi-Espectrógrafo en
GTC de Alta Resolución para Astronomía, Carrasco et al., 2018) attached to the
GTC 10.4 m telescope at La Palma Observatory. We have used MEGARA in the
integral-field Unit (IFU) mode working in the visible wavelength range from
3655 to 9700 Å and providing a high spectral (up to RFWHM =
$\lambda/\Delta\lambda$ $\sim$ 20000) and spatial resolution (0.62 arcsec
spaxel size) simultaneously in a moderate size field of view (FoV) (12.5
$\times$ 11.3 arcsec2). It has a total of 623 hexagonal fibers distributed in
567 science-fibers and 56 sky-fibers located at the edges of the FoV at
distances from 1.7 arcmin to 2.5 arcmin from the centre of the fiber bundle.

Figure 1: WPC2-HST image in the F336W filter showing the circumnuclear region
of NGC7742 and the MEGARA fields of view. North is at the top and east is to
the left.

The observations were acquired during 3 nights on 2021 August 28th, 31th and
September 14th111Proposal GTC28-21A: A high spatial and spectral resolution
study of circumnuclear star-forming regions
PI: Ángeles I. Díaz. Semester 2021-A. under spectroscopic conditions. The
seeing during the observations ranged between approximately 0.7 and 0.9 arcsec
and the airmass of the science images was always less than 1.25. Four
pointings were needed to cover the whole circumnuclear ring extension of NGC
7742 (approximately the central 24x24 arcsec2, see Fig. 1).

Table 1: Target observations.

Target |  | RA
---
(hh:mm:ss.ss)
| DEC
---
(dd:mm:ss.ss)
| Field of View
---
Position Anglea
(degrees)
| Exp. Timeb (s)
---
VPH863_HR
| Exp. Timeb (s)
---
VPH890_LR
| Exp. Timeb (s)
---
VPH665_HR
NGC7742_P1 | 23:44:16.02 | 10:46:05.80 | 0 | 1050 | 450 | 684
NGC7742_P2 | 23:44:15.28 | 10:46:06.40 | 0 | 1050 | - | 684
NGC7742_P2 | 23:44:15.28 | 10:46:06.40 | 90 | 1050 | 450 | 342
NGC7742_P3 | 23:44:16.02 | 10:45:55.60 | 0 | 1050 | 450 | 684
NGC7742_P4 | 23:44:15.28 | 10:45:55.00 | 90 | 1050 | 450 | 342

  * •

a From North toward East. The orientation of 0 deg implies that the North is
aligned with the short side and the East-West axis with the long side of the
detector.

  * •

b Total target observed time without overheads.

Three dispersion elements (VPHs) were used: VPH863_HR (HR-I, RFWHM $\sim$
20500), including the calcium triplet stellar lines (CaT) at high spectral
resolution; VPH890_LR (LR-Z, RFWHM $\sim$ 5800) including the
[SIII]$\lambda\lambda$9069,9532 Å emission lines and the CaT lines at low
resolution; and VPH665_HR (HR-R, RFWHM $\sim$ 20050) including the
[NII]$\lambda\lambda$6548,84 Å, H$\alpha$, and [SII]$\lambda\lambda$6717,32 Å
emission lines at high resolution. A relation of the total integration times
and their splitting in different exposures for each of the used setups is
given in Tab. 1. Using these configurations, velocity dispersions around 6.4
km/s and 22.5 km/s in FWHM were expected at high and low spectral resolutions
respectively.

Calibration images were acquired on the observing nights and on the preceding
and following ones. They consisted of: bias frames to create a CCD spatial
response function; flat field frames necessary to locate each fiber spectrum
on the CCD and to perform a spatial instrumental response function; arc
calibration exposures needed for wavelength calibration; and 3
spectrophotometric standard star exposures needed for performing a spectral
instrumental response function. The standard procedures of: bias subtraction;
tracing and extraction of each fiber spectra; flat field correction; and
wavelength calibration were followed applying some required modifications to
the standard MEGARA pipeline. (Pascual et al., 2018) 222see
https://github.com/guaix-ucm/megaradrp/ using calibration files present in
Cardiel & Pascual (2018). Flux calibration was not needed for our work and we
decided not to do it in order not to introduce additional errors in our
subsequent analysis. After the reduction procedure, a data cube per pointing
was produced (i. e. 8, 5, and 4 cubes for the HR-R, HR-I and LR-Z setups
respectively) with a spatial binning of 0.2 arcsec/pix.

Table 2: Extraction parameters for emission line and continuum maps.

MEGARA
---
Line |  $\lambda_{c}$ (Å) |  $\Delta\lambda$ (Å) |  $\Delta\lambda_{left}$ (Å) |  $\Delta\lambda_{right}$ (Å)
H$\alpha$ | 6563 | 5 | 6596 - 6606 | 6530 - 6540
$[SIII]$ | 9532 | 10 | 9472 - 9492 | 9545 - 9565
Continuum | 8810 | 5 | - | -
MUSE
Line |  $\lambda_{c}$ (Å) |  $\Delta\lambda$ (Å) |  $\Delta\lambda_{left}$ (Å) |  $\Delta\lambda_{right}$ (Å)
H$\alpha$ | 6563 | 8 | 6531.5 - 6539.5 | 6597 - 6605
$[SIII]$ | 9069 | 15 | 9010 - 9040 | 9115 - 9145
Continuum | 8810 | 5 | - | -

  * •

All wavelengths are in the rest frame.

Astrometric aligning was achieved by comparing our MEGARA data with those
extracted from the publicly available observations of NGC 7742 obtained by the
IFS MUSE (Science Verification run on 2014 June 22, ESO Programme
60.A-9301(A), M. Sarzi) and already analysed in Zamora & Díaz (2023b). The 2D
cross correlation technique proposed by Tonry & Davis (1979) was used to find
the spatial shift between MEGARA and MUSE data. We have constructed H$\alpha$
and [SIII]$\lambda$9532 Å emission line maps for the HR-R and LR-Z setups
respectively, and a continuum map near the CaT absorption lines for the HR-I
setup. For the emission line maps, a linear behavior of the continuum emission
in the region of interest was assumed choosing appropriate side-bands of a
given width for each line. Table 2 lists in columns 1 to 5: (1) the
identification of each line; (2) its central wavelength; (3) its width; and
(4,5) the limits of the two continuum side-bands. The upper and lower table
panels show these parameters for MEGARA and MUSE data respectively. The
followed procedure ensures that our pointings are correctly aligned.

Figure 2: Example of HR-R final data cube compressed in the spectral
direction. Superimposed are the contours of MUSE data (same range of
wavelengths). The colour scale is linear. North is up and East to the left.

Finally, we have combined the overlapping individual cubes in a single one
using the average of the data available in each pixel with no spatial
smoothing applied. Figure 2 shows the resulting cube for HR-R setup as an
example. It is compressed in the spectral direction and superimposed are
contours of data obtained with MUSE showing the consistency with those
obtained from MEGARA.

##  3 Results

###  3.1 HII region selection

The HII region selection has been accomplished as described in the first paper
of this series (see Zamora & Díaz, 2023b) consisting in the application of an
iterative procedure for the detection of high intensity clumps on an H$\alpha$
emission line map. This method requires as input the maximum and minimum
extent of regions (500 pc and the point spread function of observations
respectively) and the relative flux intensity in each of the regions with
respect to the emission of its centre (10%). Then, the program tried different
values for the absolute flux intensity background of the complete map adopting
the one that minimizes the dispersion of the spatial residuals in the map.

We consider that this HII region segmentation is appropriate for our MEGARA
study since the astrometry correction has been made with respect to MUSE data.
Also, since the selected pixel scale for the cube construction is the same as
the MUSE one (0.2 arcsec/pix) we can assure that all the ring HII regions are
spatially resolved. Additionally, the measured angular radii of the regions
calculated using this method were found to be compatible with radiation
bounded ionised nebulae (see Zamora & Díaz, 2023b). Regions R2, R13, R24, R39,
R40, R46, R49, R68, and R82 fall outside the area covered by the FoV of
MEGARA, and therefore are not included in the present study. In the end, we
have selected a total of 79 HII regions in the ring.

###  3.2 Nebular emission line measurements

We have extracted each region spectrum by integrating the flux inside its
corresponding aperture and we have used the code LiMe (LIne MEasuring library
Fernández et al., 2022) to separate the different kinematical components
present in each emission line. This program uses a defined window for each
line and two additional ones to calculate the continuum below. After the
fitting, we have taken into account only those components that meet the
requirement: $A_{g}>3\sigma_{l}$, with $A_{g}$ being the Gaussian amplitude
and $\sigma_{l}$ the local standard deviation of the continuum bands selected
for each fit. Next, we have measured the radial velocity, $v$, and the
velocity dispersion, $\sigma$, of each component in the following emission
lines: H$\alpha$, [NII]$\lambda\lambda$6548,84 Å and
[SII]$\lambda\lambda$6716,31 Å from the HR-R setup, and
[SIII]$\lambda\lambda$9069,9532 Å from the LR-Z ones. We have performed an
individual fitting for each emission line and adopted a kinematical bond
between the components of lines of the same element: [NII]$\lambda$6548 Å with
[NII]$\lambda$6584 Å; [SII]$\lambda$6716 Å with [SII]$\lambda$6731 Å; and
[SIII]$\lambda$9069 Å with [SIII]$\lambda$9532 Å.

Figure 3: Spectra of regions R1 and R9 (upper and bottom panels respectively)
showing the kinematical components fitted. From left to right: H$\alpha$ and
[NII]$\lambda\lambda$ 6548,6584 Å; [SII]$\lambda\lambda$ 6717,6731 Å;
[SIII]$\lambda$ 9069 Å; and [SIII]$\lambda$ 9532 Å emission lines.

Fig. 3 shows two examples of the procedure for regions R1 and R9, showing in
different panels from left to right the emission lines: H$\alpha$ and
[NII]$\lambda\lambda$6548,84 Å; [SII]$\lambda\lambda$6716,31 Å; and
[SIII]$\lambda$9069 Å and [SIII]$\lambda$9532 Å. Eight regions out of 79
($\sim$ 10%), labeled R6, R48, R78, R79, R81, R84, R85, and R88, have been
found to have one only component; the rest of them show at least two in the
H$\alpha$ emission line; and only one region, R1, shows two components in the
[SIII] lines. In fact, in this region, which is shown in the upper panel of
the figure, three components are clearly identified in the H$\alpha$ and [NII]
lines, and also a third can be appreciable in the[SIII]$\lambda$9532 Å
emission line. The region is located near a supernova event: SN 1993R.

Table 3: Emission line radial velocities in km/s. The complete table is available online and in Apendix A; here only a part is shown as an example. Region ID | Component |  | v(H$\alpha$)
---
(km/s)
| v([NII]$\lambda$6584 Å)
---
(km/s)
| v([SII]$\lambda$6717 Å)
---
(km/s)
| v([SIII]$\lambda$9532 Å)
---
(km/s)
R1 | Narrow | 8.45 $\pm$ 0.41 | 8.36 $\pm$ 8.52 | 6.80 $\pm$ 0.65 | 6.71 $\pm$ 1.71
| Broad | 5.48 $\pm$ 0.85 | 5.76 $\pm$ 12.02 | 7.00 $\pm$ 5.35 | 12.20 $\pm$ 9.46
| Aditional | 15.4 $\pm$ 1.2 | 12.86 $\pm$ 37.74 | - | -
R3 | Narrow | 16.76 $\pm$ 0.09 | 16.57 $\pm$ 2.90 | 16.23 $\pm$ 0.58 | 15.42 $\pm$ 0.93
| Broad | 20.70 $\pm$ 0.95 | 18.72 $\pm$ 25.72 | 31.55 $\pm$ 9.52 | -
R4 | Narrow | 31.52 $\pm$ 0.20 | 32.54 $\pm$ 2.70 | 30.17 $\pm$ 1.12 | 30.07 $\pm$ 1.29
| Broad | 36.34 $\pm$ 0.78 | 36.35 $\pm$ 19.61 | 44.89 $\pm$ 5.20 | -
| Aditional | 18.2 $\pm$ 6.8 | - | - | -

Measured velocities have been corrected to rest frame using the redshift
derived value of v = 1652.364 km/s (z = 0.00553). Errors in the velocity of
each component are given by the LiMe code using a Monte-Carlo procedure and
the noise calculated in the continuum bands. Table 3 shows the velocity
results listing in columns 1 to 6: (1) the region ID; (2) the line component;
and (3-6) the velocity of the H$\alpha$, [NII], [SII], and [SIII] emission
lines respectively. The corresponding errors in the velocity dispersions have
been calculated as the difference between the FWHM of the largest and smallest
fitted Gaussian function taking into account the noise of the fitted spectrum.
Using the amplitude of the Gaussian fitted, $A_{g}$, and the noise calculated
in the residuals of the fit, $\sigma_{f}$, the error can be calculated as:

$\Delta[\sigma]=\frac{\sigma}{2\sqrt{ln(2)}}\cdot
ln\left(\frac{1+\sigma_{f}/A_{g}}{1-\sigma_{f}/A_{g}}\right)$ (1)

The measured velocity dispersions of the gas needs to be corrected for
instrumental dispersion, $\sigma_{inst}$ and thermal broadening,
$\sigma_{th}$, hence the corrected value for the gas velocity dispersion will
be:

$\sigma_{gas}=\sqrt{\sigma^{2}_{measured}-\sigma^{2}_{inst}-\sigma^{2}_{th}}$
(2)

The instrumental dispersion values are 6.4 km/s and 22.5 km/s for the MEGARA
high and low resolution configurations respectively (see Sec. 2). The thermal
broadening can be calculated assuming a Maxwellian velocity distribution of
the ions using the following equation:

$\sigma_{th}=\sqrt{\frac{k\cdot t_{e}}{m}}$ (3)

where k is Boltzmann’ constant (k=1.380649 $\times$ 10-23 J/K), te is the
electron temperature in degrees Kelvin and m is the mass of the ion involed
(m${}_{H^{+}}$ = 1.6726 $\times$ 10-27 kg; m${}_{N^{+}}$ = 2.3257 $\times$
10-26 kg; m${}_{S^{+}}$ = 5.3244 $\times$ 10-26 kg; m${}_{S^{++}}$ = 5.3243
$\times$ 10-26 kg). We have assumed the electron temperature of [SIII]
(te[SIII]) calculated in Zamora & Díaz (2023b) for each CNSFR, and its average
value is 7967 K, hence the mean thermal corrections are 8.11 km/s for H+; 2.17
km/s for N+; and 1.44 km/s for S+ and S++.

Table 4: Emission line velocity dispersions in km/s. The complete table is available online and in Apendix A; here only a part is shown as an example. Region ID | Component |  |  $\sigma$(H$\alpha$)
---
(km/s)
|  $\sigma$([NII]$\lambda$6584 Å)
---
(km/s)
|  $\sigma$([SII]$\lambda$6717 Å)
---
(km/s)
|  $\sigma$([SIII]$\lambda$9532 Å)
---
(km/s)
R1 | Narrow | 10.29 $\pm$ 0.09 | 7.88 $\pm$ 0.15 | 12.41 $\pm$ 0.80 | 18.98 $\pm$ 0.53
| Broad | 19.60 $\pm$ 0.20 | 18.30 $\pm$ 0.28 | 40.22 $\pm$ 4.14 | 62.64 $\pm$ 6.50
| Aditional | 47.7 $\pm$ 1.1 | 48.30 $\pm$ 2.34 | - | -
R3 | Narrow | 14.46 $\pm$ 0.08 | 12.67 $\pm$ 0.13 | 13.82 $\pm$ 0.65 | 13.68 $\pm$ 0.44
| Broad | 43.68 $\pm$ 1.66 | 34.51 $\pm$ 2.02 | 53.56 $\pm$ 8.84 | -
R4 | Narrow | 10.53 $\pm$ 0.12 | 12.44 $\pm$ 0.21 | 12.00 $\pm$ 1.34 | 14.06 $\pm$ 0.58
| Broad | 27.88 $\pm$ 0.59 | 45.04 $\pm$ 3.09 | 33.12 $\pm$ 3.54 | -
| Aditional | 69.2 $\pm$ 10.3 | - | - | -

Tables 3 and 4 show the velocity and velocity dispersions results listing in
columns 1 to 6: (1) the region ID; (2) the line component; (3-6) the velocity
or velocity dispersion of the H$\alpha$, [NII], [SII], and [SIII] emission
lines respectively.

###  3.3 Stellar absorption lines

The main objective of our work is to estimate the properties of the stellar
population of the clusters associated to the observed CNSFR. In order to do
that we have used two sets of absorption lines: the MgIb triplet at 5167-5183
detected in the MUSE data (unresolved) and the CaII triplet (CaT) at
$\lambda\lambda$ 8498, 8542, 8662 Å (CaT) resolved with MEGARA.

We have measured the equivalent widths (EW) of these stellar absorption lines
by integrating the line fluxes and taking as continuum values the linear
interpolation between the mean integrated fluxes in 30 Å continuum bands at
both sides of the line. The details of the measuring procedure can be seen in
Tab. 8 of Zamora & Díaz (2023a). The EW errors have been calculated using the
standard deviation in the two continuum bands and propagating them in
quadrature. In principle, absorption line EW measurements in objects with
different velocity dispersions should be for the broadening of the spectral
lines; this effect decreases the continuum level providing lower EW values.
However, this correction for MUSE data was found to be negligible (¡ 1 Å for
velocity dispersions of around 170 km/s for MUSE spectral resolution), then no
correction has been applied. Table 5 lists in columns 1 to 3: (1) the region
ID; (2) the CaT EW in Å; and (3) the MgIb EW also in Å .

Table 5: Equivalent widths of stellar absorption lines of the observed CNSFRs.
The complete table is available online and in Apendix A; here only a part is
shown as an example.

Region ID |  | EW(CaII)a
---
(Å)
| EW(MgI)
---
(Å)
R1 | 7.307 $\pm$ 0.264 | 1.686 $\pm$ 0.035
R3 | 7.301 $\pm$ 0.278 | 2.329 $\pm$ 0.063
R4 | 7.558 $\pm$ 0.303 | 1.868 $\pm$ 0.044
R5 | 7.418 $\pm$ 0.338 | 2.147 $\pm$ 0.048
R6 | 7.118 $\pm$ 0.318 | 2.141 $\pm$ 0.073
R7 | 6.732 $\pm$ 0.339 | 1.972 $\pm$ 0.056
R8 | 7.350 $\pm$ 0.299 | 2.156 $\pm$ 0.060
R9 | 7.571 $\pm$ 0.346 | 2.013 $\pm$ 0.054
R10 | 7.008 $\pm$ 0.297 | 1.987 $\pm$ 0.048
R11 | 7.281 $\pm$ 0.211 | 2.840 $\pm$ 0.092

  * •

a ($\lambda$8542Å + $\lambda$8662Å+ $\lambda$8498Å).

The presence of a non negligible contribution by the nebular continuum can
dilute the starlight weakening and distorting the absorption features. This
component is usually not taken into account, but it provides information about
the origin of the features measured. Thus, we have calculated a dilution
factor, D, for each set of lines with respect to a reference average value
measured in the spectra of normal spiral galaxy nuclei which corresponds to
old, metal rich stellar populations (EWref(CaII) = 7.7 $\pm$ 0.5 Å, EWref(MgI)
= 5.18 $\pm$ 0.71 Å; Terlevich et al., 1990; Keel, 1983). We have calculated
this dilution factor as the ratio between the measured EWs and the adopted
reference values: D = EWobs / EWref and compared it to that dilution produced
by the nebular continuum associated with a nebula ionised by a young star
cluster synthesised using the PopStar code (Mollá et al., 2009) with
Salpeter’s IMF (mlow = 0.85 M⊙, mup = 120 M⊙ Salpeter, 1955) and an age of 5.5
Ma.

Figure 4:  Comparison between the dilution factors calculated for the MgIb and
CaT stellar absorption features for the observed CNSFRs. The red lines
represent the dilution produced by the nebular continuum in the optical and
near IR.

Figure 4 shows the comparison between the dilution factors, D, calculated for
the MgIb and CaT stellar absorption features for the studied CNSFRs. The red
lines represent the dilution produced by the nebular continuum in the optical
and near IR. We can see that the mean value of the MgIb dilution is about 50%,
consistent with the contribution by a nebular continuum. However, the CaT
lines are shown almost undiluted. This result can be explained by the presence
of red supergiant stars whose CaT features are stronger than those in normal
early spiral galaxies while the reference value probably consists of a stellar
population dominated by red giants. This points to the occurrence of a
relatively recent star formation episode. The same behaviour has already been
found for circumnuclear star clusters in both rings of NGC 7469 (see Zamora &
Díaz, 2023a) and in earlier work (Terlevich et al., 1990; Garcia Vargas et
al., 1993; Oliva et al., 1995).

###  3.4 Stellar velocity dispersions

Stellar velocity dispersions can be obtained from the stellar absorption
lines. In the second paper of this series (see Zamora & Díaz, 2023a) we used
the CaT lines detected in MUSE data for this calculation. However, the
spectral resolution reached in MUSE data was insufficient to resolve the CaT
lines in the case of the HII ring regions in NGC 7742 and therefore we
acquired higher resolution data using MEGARA which provides about 14 km/s of
spectral resolution (see Sec. 2). As in the case of NGC 7469, the clusters
studied in this work have red supergiant stars dominating the near IR range of
the spectrum and the CaT $\lambda\lambda$ 8498, 8542, 8662 Å lines (see Sec.
3.3) are easily detected. The use of the near IR spectra provides two
principal advantages for this study: the contamination by TiO bands and
nebular lines is small and the velocity resolution at longer wavelengths is
higher than in the blue part of the spectrum for the same spectral dispersion.
Additionally, using the cross correlation technique, stellar weak lines
present in this part of the spectra also contribute to the goodness of the
results.

We have used the cross-correlation technique proposed by Tonry & Davis (1979).
In this traditional method, a comparison between a stellar template with the
observed stellar population spectrum is done. The assumption made assumes that
a galaxy spectrum can be represented by the sum of different stellar spectra
with different velocity offsets convolved with a broadening function:
$g\sim\alpha[t(n)\ast b(\lambda-\delta)]$, where b is the broadening function,
g and t are the cluster and the stellar template spectra respectively, and
$\delta$ is the velocity shift between stars. The width of this broadening
function is calculated using two correlations: the cluster spectrum with the
stellar template (g $\otimes$ t) and the stellar template with itself (t
$\otimes$ t). The convolution products are applied assuming a periodic
spectrum with discrete Fourier transforms and the broadening function is
assumed to be Gaussian. However, this last assumption is not correct for the
(t $\otimes$ t) correlation at spectral resolutions as high as the one
provided by MEGARA and this technique needs to be modified. We have used the
adapted methods proposed in Zamora & Díaz (2023c) of the (g $\otimes$ g)
correlation which is broader than the other two ones and whose Gaussian
behavior can be ensured. In order to test these two additional methods and the
traditional ones with our data, we have selected a region with high S/N (R52,
located in the pointing with the higher exposure time in the HR-I setup). For
the stellar template, we have used late-type red giants and supergiants
obtained from the MEGARA stellar library (García-Vargas et al., 2020) aligning
all available stellar spectra in velocity and calculating the average between
them, verifying that no apparent broadening is introduced in the procedure.
The use of only two stellar types of stars for the correlation analysis could
introduce errors in our velocity dispersion measures. However, the use of CaT
lines minimises the mismatch between the stellar template and the cluster
spectrum since they are very strong in most stars of moderate to high
metallicity.

Figure 5: Upper panel: R52 absorption spectrum from MEGARA/HR-I and LR-Z
configurations, red and purple lines respectively. Absorption stellar lines
and emmision lines present in this wavelength range are indicated. The stellar
template is also shown with a blue line. Bottom panel: Sky template (see
text).

The upper panel of Figure 5 shows the stellar spectrum of the selected cluster
R52 at high and low MEGARA spectral resolutions, with red and purple lines
respectively. The stellar template is also shown with a blue line and the
nebular lines present in this spectral range are marked. We can see that the
S/N of these spectra is low, even in this region which was observed with twice
the average exposure time. This could be due to the noise component or to
errors associated with the subtraction of the sky background which is very
prominent in the near IR. Thus, we have calculated a mean spectrum of the sky,
using the MEGARA fibers earmarked for this purpose. The lower panel of the
figure shows this spectrum that shares some features with the cluster one.

We have used the modified version of Tonry & Davis’ method described above for
the application of the cross-correlation technique to the data obtained from
the MEGARA in the HR-I configuration in the spectral range 8450 Åto 8850 Å.
Prior to this, we have binned the spectrum into 4069 logarithmic wavelength
bins corresponding to a velocity resolution of $\sim$ 3.4 km/s. Then, we have
estimated the continuum by fitting a second order polynomial after masking the
features present in the spectrum. The masks have been built assuming a width
of 3 Å and 10 Å at each side of the central wavelength of the nebular and
stellar lines involved respectively. This continuum has subsequently been
subtracted.

Figure 6: Absorption line spectrum of R52 from the MEGARA/HR-I configuration,
in logarithmic wavelength. The light and dark red lines show the spectrum
before and after applying the pass-band filter for higher frequencies. The
stellar template is also shown with a blue line.

Next, the high and low frequency variations have been filtered using a band-
pass filter in the Fourier spectrum transform. The minimum and maximum wave
numbers are kmin = 3 and kmax = 350 which correspond to wavelength values
lower than 10 Å and to the nominal MEGARA/HR-I spectral resolution. The low
frequency variations are associated with continuum subtracted errors and the
high ones with the noise component. Figure 6 shows, in a small range of
wavelengths, in light red the original spectrum and in dark red the spectrum
after the band-pass filter. The stellar template is also shown in blue for
comparison. We can see that this filter removes part of the noise, recovering
some stellar features. However, the S/N continues to be low and we can see
residuals for example in the central part of the strongest line. Thus, the
noise present in our spectrum probably comes from the errors associated with
the pipeline sky subtraction. Therefore, we have decided to use the data
without the sky subtraction to be able to quantify this additional component
in the cross correlation technique and obtain a more reliable result in the
stellar dispersion determination.

An important step in the cross correlation procedure is the subtraction of the
non-stellar component of the spectra, which can introduce errors in the
velocity dispersions of up to 5 km/s (see Zamora & Díaz, 2023c). In order to
remove correctly the nebular component of the spectrum, we have first removed
the proper motion of the cluster by shifting the spectrum to the rest frame
position. For this step, we have used the position of the (g $\otimes$ t)
cross correlation. Then, we have masked the nebular lines shown in Fig. 5
assuming a width of 0.4 Å at each side of their central wavelength.

Figure 7: Upper left panel: auto-cross correlation function of the sky
template. Upper right: auto-cross correlation of the spectrum of region R52.
Bottom panel: cross correlation between the cluster spectrum and the stellar
template. The lower panel of each plot shows the residuals of the fitting.

Finally, we have calculated four cross correlation functions for this HII
region: (t $\otimes$ t), (g $\otimes$ t), (g $\otimes$ g) and (s $\otimes$ s),
with t being the stellar template, g the cluster spectrum and s the mean sky
spectrum of our observations. The upper left panel of Figure 7 shows the (s
$\otimes$ s) correlation. Two components can be seen, one associated with the
sky lines and another associated with the detector response. They have been
fitted with two Gaussian functions and their widths are $\mu_{ss1}$ = 0.2098 Å
and $\mu_{ss2}$ = 12.1445 Å respectively. The width of the first component
corresponds to a value $\Delta\lambda$ = 0.15 Å in $\sigma$-units, which is
slightly lower than the MEGARA resolution for this setup, $\Delta\lambda$ =
0.18.

The upper right panel of Figure 7 shows, as an example, the (g $\otimes$ g)
correlation for the R52 cluster. In this figure we can identify the component
associated with the sky lines and the component associated with the stars of
the cluster. According to this, we have fitted simultaneously two Gaussian
functions, one of them using the $\mu_{ss1}$ value calculated for the (s
$\otimes$ s) correlation. The width of the cluster component is $\mu_{gg}$ =
2.2680 Å. The correlation (g $\otimes$ t) is shown in the lower panel of the
same figure. In this case the sky emission affects only the cluster spectrum
and hence the sky component does not show up. The cluster component is
$\mu_{gt}$ = 2.1147 Å.

We have combined these results, together with the width of the (t $\otimes$ t)
correlation function ($\mu_{tt}$ = 1.241 Å) and we have applied the three
methods studied in Zamora & Díaz (2023c):

$(i)\quad\sigma=\sqrt{\frac{\mu_{gg}^{2}-\mu_{tt}^{2}}{2}}$
$(ii)\quad\sigma=\sqrt{\mu_{gg}^{2}-\mu_{gt}^{2}}$
$(iii)\quad\sigma=\sqrt{\mu_{gt}^{2}-\mu_{tt}^{2}}$

the last equation being the one proposed by Tonry & Davis (1979). We have
performed theses calculations for R52 correcting methods (i) and (ii) for the
non-Gaussian behaviour of the (t $\otimes$ t) correlation. The final results
are (i) $\sigma$ = 27.87 km/s; (ii) $\sigma$ = 28.42 km/s; and (iii) $\sigma$
= 28.44 km/s. We can see that the three methods show very similar results,
thus we can conclude that the reduction and treatment of these high resolution
data and the application of the cross-correlation method is correct.

Table 6: Stellar cluster velocity dispersions in units of km/s. Region ID |  |  $\sigma_{*}$(CaT)
---
(km/s)
R1 | 22.61 $\pm$ 6.65
R3 | 31.43 $\pm$ 4.68
R5 | 77.08 $\pm$ 1.37
R7 | 20.19 $\pm$ 4.39
R8 | 37.75 $\pm$ 19.32
R14 | 19.34 $\pm$ 5.87
R15 | 27.88 $\pm$ 6.61
R16 | 50.82 $\pm$ 3.95
R22 | 37.10 $\pm$ 9.98
R23 | 38.75 $\pm$ 8.66
R26 | 19.26 $\pm$ 6.86
R31 | 45.87 $\pm$ 9.38
R33 | 47.73 $\pm$ 5.41
R36 | 72.04 $\pm$ 0.49
R41 | 50.82 $\pm$ 4.95
R45 | 56.26 $\pm$ 14.67
R47 | 38.95 $\pm$ 13.01
R50 | 44.64 $\pm$ 4.94
R51 | 36.78 $\pm$ 6.83
R52 | 28.40 $\pm$ 9.85
R53 | 50.53 $\pm$ 1.13
R55 | 44.67 $\pm$ 7.63
R57 | 14.46 $\pm$ 4.49
R60 | 33.36 $\pm$ 7.53
R63 | 32.93 $\pm$ 7.31
R69 | 14.25 $\pm$ 6.79
R72 | 26.40 $\pm$ 4.24
R74 | 23.56 $\pm$ 5.80
R75 | 43.76 $\pm$ 6.35
R88 | 20.65 $\pm$ 3.52

Therefore, for the rest of CNSFRs, we have decided to apply method (iii) in
order not to use the (g $\otimes$ g) correlation due to the sky subtraction
problems. The velocity dispersion errors have been calculated as the semi-
difference between the largest and smallest Gaussian width that can be fitted
considering the asymmetries in the correlation peak as suggested in Zamora &
Díaz (2023c), although it could lead to the error being somewhat
overestimated. Applying the described methodology, we have obtained reliable
CaT velocity dispersion values for 30 of the selected CNSFR regions. They are
shown in Table 6 and they take values from 14.3 to 77.1 km/s.

##  4 Discussion

###  4.1 Cluster sizes

Figure 8: Results of the stellar cluster radius measurement procedure for
regions R1 and R52, upper and lower panels respectively (see text for
details). The angular scale is in the panels corner.

We have calculated the effective radii of the star clusters from the Hubble
Space Telescope (HST) continuum image. These data were acquired on 2009
November 5 with the Wide Field and Planetary Camera 2 (WFPC2) and the F555W
continuum filter where stellar clusters are easily identified. These data are
a part of proposal 6276 (IP: J. Westphal) organised in 3 exposures of 480 s.
The data have been downloaded from the Hubble Legacy Archive and reduced by
the Space Telescope Science Institute (STScI) using available calibration
files taken for this observation and keeping in mind different dithering
positions.

The effective radii of the star clusters have been calculated using the
following procedure. First, we have estimated the region background by fitting
a three-order polynomial. After subtracting it, we fitted the surface
brightness of each knot present in the observed clusters assuming a two-
dimensional Gaussian profile. Fig. 8 shows two examples of the described
procedure as applied to regions R1, and R52. The left panels of the figure
show the F555W WFPC2-HST image for each selected region and the right panels
show the same image after background subtraction. Selected clusters are shown
by blue circles. The radius of each knot has been taken as 1/2$\cdot$ FWHM.
There are three regions, R72, R75, and R88, where no knot is readily
appreciable in the continuum at 5550 Å thus, we have not calculated their
sizes.

As opposed to other CNSFRs from the literature, this galaxy does not seem to
have large star-forming complexes and $\sim$ 60 % of the CNSFRs (16 out of 27)
seem to host single clusters and $\sim$ 27 % (7 out of 27) are composed by
two. Three regions show three different knots, and one shows four. We can
compare these values with the results obtained for NGC 7469 (see Zamora &
Díaz, 2023a) which shows two regions with 20 and 19 knots respectively and
only 15 % of the regions (4 of 27) seem to have only one star cluster. These
later results, are similar to those found for the regions analysed in NGC 2903
showing more than 20 knots (Hägele et al., 2009), NGC 3310 hosting two great
complexes with 28 and 30 clusters each (Hägele et al., 2010) and NGC 3351 with
a large region showing 17 distinct knots (Hägele et al., 2007). In the case of
NGC 7469 one can imagine this effect to be due to the galaxy being further
away since in this case we may be selecting larger star-forming complexes due
to lack of spatial resolution; however, the distances to the other three
galaxies mentioned are of the same order as the one studied here. In
particular, NGC 3310 at a similar distance to NGC 7742 seems to have only one
region hosting an individual knot. It is probable that the difference between
the CNSFR is related to their different formation processes which in the
latter case seem to be due to gas accretion after a minor merger event.

Figure 9: Histograms of the distributions of the radius of each knot in the
CNSFRs of NGC 7742 as compared to those of data from the literature.

The effective radii of the studied single knots range between 8.5 and 60.5 pc,
with a mean value of 12.6 pc. Figure 9 shows the distribution of the radius of
each knot for the CNSFRs in this work and those found in the literature used
for comparison (Hägele et al., 2009, 2007, 2010). The range of radius found
for NGC 7469 is wider than in the other galaxies and the same is true for the
mean radii for the inner and outer ring regions. On the other hand, NGC 3351,
NGC 2903, and NGC 3310 have smaller knots than NGC 7742.

###  4.2 Dynamical masses

We have calculated the dynamical masses for each observed cluster from its
measured CaT velocity dispersion and size assuming a virialised system and
using the expression given by (Ho & Filippenko, 1996a, b):

$M^{dyn}=3\cdot\sigma^{2}\cdot\frac{R}{G}$ (4)

where $\sigma$ is the one-dimensional velocity dispersion of the system, R is
its radius and G is the gravitational constant.

Figure 10: Distributions of the dynamical masses of each knot for the CNSFRs.
The upper panel shows the results in this work and the outer and inner ring
regions of NGC 7469. The bottom panel shows data from the literature (Hägele
et al., 2010, 2007, 2009, labeled (H+07), (H+09), and (H+10) respectively).

This calculation assumes that the clusters (i), have spherical symmetry; (ii),
are gravitationally bound; and (iii), have an isotropic velocity distribution.
Most of the clusters show only one knot at thus the calculated masses under
this assumption seem to be appropriate. However a small number are clearly
multiple, in this case the total mass of the cluster was estimated by adding
the masses of its individual knots inferred using the velocity dispersion of
the entire region a procedure that most likely result on an overestimate.

Figure 10 shows the distribution of the cluster dynamical masses for NGC 7742
compared with those of the inner and outer rings of NGC 7469. We can see that
NGC 7742 knots show lower masses which is to be expected from their smaller
sizes. However, they tend to be more massive than CNSFRs from the literature
(Hägele et al., 2010, 2007, 2009, NGC 3351, NGC 2903, and NGC 3310).

Table 7: Stellar cluster masses and sizes for observed CNSFRs. | Region
---
ID
Nknots |  | R${}^{*}_{mean}$
---
(pc/knot)
| Mdyn
---
(M⊙)
| Mion/Mdyn
---
(per cent)
R1 | 1 | 13.9 | (6.2 $\pm$ 3.6) $\times$ 106 | 2.57
R3 | 2 | 15.0 | (25.9 $\pm$ 2.7) $\times$ 106 | 1.47
R5 | 1 | 16.3 | (84.6 $\pm$ 3.0) $\times$ 106 | 0.15
R7 | 1 | 9.9 | (3.5 $\pm$ 1.5) $\times$ 106 | 6.61
R8 | 1 | 20.1 | (2.5 $\pm$ 2.6) $\times$ 107 | 1.32
R14 | 2 | 12.8 | (8.3 $\pm$ 2.0) $\times$ 106 | 2.20
R15 | 1 | 12.1 | (8.2 $\pm$ 3.9) $\times$ 106 | 1.45
R16 | 1 | 10.1 | (22.8 $\pm$ 3.6) $\times$ 106 | 2.26
R22 | 1 | 10.1 | (12.2 $\pm$ 6.5) $\times$ 106 | 2.24
R23 | 2 | 14.6 | (38.3 $\pm$ 8.6) $\times$ 106 | 0.73
R26 | 2 | 14.6 | (9.5 $\pm$ 2.3) $\times$ 106 | 3.00
R31 | 4 | 10.1 | (74.4 $\pm$ 7.6) $\times$ 106 | 0.40
R33 | 1 | 15.2 | (30.2 $\pm$ 6.8) $\times$ 106 | 0.77
R36 | 1 | 10.6 | (481.8 $\pm$ 6.6) $\times$ 105 | 0.77
R41 | 3 | 14.8 | (100.4 $\pm$ 6.7) $\times$ 106 | 0.59
R45 | 2 | 18.1 | (10.0 $\pm$ 2.3) $\times$ 107 | 0.19
R47 | 2 | 12.2 | (3.2 $\pm$ 1.1) $\times$ 107 | 0.55
R50 | 1 | 10.1 | (17.6 $\pm$ 3.9) $\times$ 106 | 1.21
R51 | 1 | 71.3 | (8.4 $\pm$ 3.1) $\times$ 107 | 0.39
R52 | 3 | 14.9 | (31.4 $\pm$ 4.9) $\times$ 106 | 1.46
R53 | 1 | 10.1 | (22.6 $\pm$ 1.0) $\times$ 106 | 0.58
R55 | 3 | 14.1 | (73.4 $\pm$ 6.7) $\times$ 106 | 0.13
R57 | 2 | 14.7 | (5.4 $\pm$ 1.1) $\times$ 106 | 7.07
R60 | 1 | 13.1 | (12.7 $\pm$ 5.8) $\times$ 106 | 0.90
R63 | 1 | 10.1 | (9.6 $\pm$ 4.3) $\times$ 106 | 1.33
R69 | 1 | 14.4 | (2.5 $\pm$ 2.4) $\times$ 106 | 4.16
R74 | 1 | 19.2 | (9.3 $\pm$ 4.6) $\times$ 106 | 1.14

Table 7 lists for each region in columns 1 to 5: (1) the region ID; (2) the
number of stellar knots present in the region, (3) the mean radius in pc, (4)
the dynamical mass in M⊙ and (5) the ratio of ionising to dynamical mass. To
calculate this ratio, we have used the ionising masses calculated in the first
paper of the series from the number of hydrogen ionising photons,
Q(H$\alpha$), and the equivalent width of the H$\beta$ emission line to take
into account the cluster evolution. We used a Salpeter IMF
$\phi(m)=m^{-\alpha}$, with $\alpha=2.35$, $m_{low}(M_{\odot})$ = 0.85 and
$m_{up}(M_{\odot})$ = 120 that seems the most suitable for the age of our
regions.

Figure 11: Histograms of the distribution of dynamical masses for the CNSFRs
in this work, the outer and inner ring regions of NGC 7469, and data from the
literature as labeled (Hägele et al., 2010, 2007, 2009, (H+07), (H+09), and
(H+10) respectively).

Figure 11 shows the distribution of the calculated dynamical masses for each
CNSFR. The dynamical masses of inner and outer ring regions of NGC 7469,
calculated in the second paper of this series are also shown. Additionally, we
show the masses of CNSFRs reported in the literature for NGC 3351, NGC 2903,
and NGC 3310, which have been calculated with the same method described in
this work (Hägele et al., 2010, 2007, 2009). The dynamical masses of NGC 7742
clusters range from 2.5 $\times$ 106 to 1.0 $\times$ 108 M⊙, values similar to
those found in the rest of the galaxies shown but lower than those obtained
for the two rings of NGC 7469.

The ratio of ionising to dynamical masses has values ranging from 0.15 to 7.07
% implying a contribution by recent star formation for the ring regions larger
than found in other galaxies. For comparison, this percentage ranges from 0.02
to 0.91 % for the CNSFRs in the outer ring of NGC 7469 whose distance to the
galactic nucleus is similar to that of the NGC 7742 ring to its nucleus.

###  4.3 Kinematics of stars and ionised gas

Figure 12: Velocity of different components of H$\alpha$ measured in each
region. The narrow component velocity is shown against the broad and
additional ones, in left and right panels respectively. All velocities are
shown in km/s.

In Section 3.2 we have derived the radial velocities and velocity dispersions
of the ionised gas in the apertures of the selected HII regions. Our results
suggest the existence of at least two kinematically distinct H$\alpha$
components that can be identified in the spectra of CNSFR with high S/N. We
have compared their radial velocities in order to find out which of them are
associated with the ionising clusters.

The left panel of Figure 12 shows the comparison of the velocities of the
H$\alpha$ broad and narrow components with the 1 to 1 line represented by a
dashed grey line. We can see that both radial velocities coincide within the
errors. Only two regions seem to fall off the 1 to 1 line: R62, and R65. An
additional component of the H$\alpha$ emission line has been identified in 7
of the regions and a comparison of their velocities and those of the narrow
component is shown in the right panel of the same figure. Only three of these
additional components, in regions R1, R7, and R67, seem to be associated with
the ionising clusters, hence they can be attributed to local effects inside
the regions. In the other four cases that component may have an external
origin.

Figure 13: Comparison of the radial velocity of the different measured
components of the [NII], [SII], and [SIII] lines in each region (top to bottom
panels) with those of the narrow and broad H$\alpha$ components (left to right
panels). All velocities are shown in km/s.

The left panels of Figure 13 show the gas velocity of the narrow component of
forbidden emission lines as a function of the corresponding H$\alpha$ one.
Results for the [NII]$\lambda$6584 Å, [SII]$\lambda$6731 Å, and
[SIII]$\lambda$9532 Å emission lines are shown from top to bottom. All regions
follow the 1 to 1 relation within the errors, hence assuring that the selected
kinematical components are associated to the observed HII regions. Only in the
case of the [SIII] emission line a few regions seem to deviate from the
identity relation; these regions show large observational errors related to
low S/N spectra. The right panels of the figure show the same relations but
for the broad line component of both forbidden and H$\alpha$ lines. All [NII]
broad components follow the 1 to 1 relation, their association with the
observed HII regions is guaranteed; for the [SII] lines, only in three of the
regions the presence of a broad component is consistent with the S/N ratio,
and only one region shows a broad component in the [SIII] emission lines; this
region, R1, displays a complex kinematics with three different width velocity
components, clearly identified in the H$\alpha$ and
[NII]$\lambda\lambda$6548,84 Å lines, that seem to be associated with the HII
region (see Figure 3).

Figure 14: Relation between the velocity dispersion of stars (CaT) and ionised
gas (H$\alpha$, [NII]$\lambda$ 6584 Å, [SII]$\lambda$ 6731 Å, and
[SIII]$\lambda$ 9532 Å emission lines) for the selected CNSFRs. The red
horizontal solid line represents the average velocity dispersion of the gas
narrow component; dashed red lines correspond to the $\pm$ 1 $\sigma$ value.

Figure 14 shows the comparison between the derived velocity dispersion for
stars and gas in the selected CNSFRs. Gas narrow and broad components are
represented by blue dots and green triangles respectively while regions
showing a single component are represented by purple squares. The dashed grey
line shows the 1 to 1 relation. The upper left panel of this figure shows the
results for the H$\alpha$ emission line. We can see that the narrow components
have velocity dispersions lower than the stellar ones and in a narrow range
with a mean value of $\overline{\sigma}_{H\alpha}$ = 9.26 km/s, shown by a red
solid line with dotted red lines representing the standard deviation of the
distribution. Regions which have only one component show a similar behaviour.
On the other hand, the broad components lie slightly above the 1 to 1 relation
in regions with low star velocity dispersions. This behaviour seems to be lost
for higher values of $\sigma_{CaT}$. The upper right panel of the figure shows
the results for [NII] having the same behaviour as the H$\alpha$ line. In this
case, the mean velocity dispersion of the narrow component is
$\overline{\sigma}_{[NII]}$ = 11.2 km/s and the standard deviation is slightly
larger. For the broad component the same trend seen for the H$\alpha$ line is
easily recognizable. The only component identified in the [SII] lines, shows
the same velocity dispersion associated to the gas narrow component, showing a
mean value of $\overline{\sigma}_{[SII]}$ = 15.8 km/s (see the lower right
panel of the figure) while for the [SIII] lines velocity dispersions show a
more complex behaviour as shown in the lower right panel of the figure; the
single component present shows a wider velocity dispersion distribution,
although mostly below the 1 to 1 line. The only region with a broad component
in [SIII] is R1 appearing in the upper left corner of the diagram, with a gas
velocity dispersion of 65 km/s (this region is close to supernova SN 1993R).

Similar results to those presented above have also been found in other
extragalactic HII region studies in the literature. For example in Firpo et
al. (2010), where some giant HII regions in the NGC 7479 spiral galaxy were
analysed using echelle spectroscopy data with a similar spectral resolution to
that of MEGARA. In this work, region III is reported to show a broad Gaussian
component in the H$\alpha$ and [NII] emission lines with a velocity dispersion
in the range between 37.8 km/s and 51.2 km/s while the narrow one is around 10
km/s and no broad component was found in the [OIII] profile whose velocity
profile can be fitted with a Gaussian with a value of $\sigma$ around 20 km/s.
Also, CNSFRs of different galaxies studied in Hägele et al. (2009, 2010) show
broad components in the emission lines at the same radial velocity as the
narrow ones within the errors; the authors identified the narrow and broad
components with ionised gas supported by rotation and dynamical pressure
respectively. Interestingly, the CNSFR rings in both galaxies are thought to
have been produced in a minor merger event.

A diversity of line broadening mechanisms have been proposed to explain the
line profiles of HII regions. Winds associated with WR stars or young main
sequence O stars (i. e. Diaz et al., 1987; Terlevich et al., 1996) could
produce them. However, the expected broadening due to WR winds would, in
general, be larger than observed in our clusters since these stars can have
winds of thousands of km/s. On the other hand, we have estimated the number of
O stars that may be present in the CNSFRs of this study. For that, we have
used the Salpeter (1955, mlow = 0.85M⊙, mup = 120 M⊙) IMF and models from
(Smith et al., 2002, Z⊙, log(g) = 4, R∗ = 7.1 - 10.6 R⊙) deriving the
following equation:

$N_{O}=6.437\cdot 10^{-5}M_{cluster}$ (5)

where Mcluster is expressed in solar masses. For the clusters with derived
dynamical mass this number is between 1 and 38, with a mean value of $\sim$ 10
stars. However, normal O stars have winds with velocities $\sim$ 103 km/s,
depending on the density of the environment. Thus, they would also provide a
broadening larger than observed. In conclusion, we rule out stellar winds as
the main broadening mechanism in our CNSFRs.

A second alternative could be related to the interaction of the hot phase of
the ISM with cooler gas knots forming a turbulent mixing layer with velocities
of about 100 to 400 km/s (Westmoquette et al., 2007b, a); Champagne flows
arising from the photo-erosion of denser clumps of gas also would produce
velocities larger than observed although they can contribute to the turbulence
of the ISM (Tenorio-Tagle et al., 1985).

Other possible explanation proposed in the literature is the turbulence of the
interstellar gas. In 1994, Chu & Kennicutt (1994) studied the 30 Doradus giant
HII region, in the Large Magellanic Cloud. The outer regions of the nebula
have a smooth turbulent velocity field with velocities of 13 to 17 km/s and,
at the central regions, the velocity is dominated by multiple expanding
structures from 8.5 to 85 km/s (in units of $\sigma$). They corroborated that
the integration of all these structures produced a simple broad Gaussian
profile with faint extended wings. Additionally, several fast expanding shells
were found with velocities from $\sim$ 40 to 130 km/s. (Medina Tanco et al.,
1997) studied the giant HII region NGC 604, in M33 finding structure in the
velocity field projected along the line of sight that could be attributed to
turbulence and suggesting that this turbulence could be powered by recent star
formation processes. According to this, the broad component of velocity
dispersions found in our particular case look similar to those produced by
interstellar gas turbulence.

However, the works just mentioned above lack the information related to the
comparison between gas and stars velocity dispersions and this fact provides
additional important information: the stars and the gas associated to the
broad component of the emission lines showing similar values of velocity
dispersion, sharing a common kinematics, can be explained if they respond to
the same gravitational potential of the cluster. From the results obtained in
the first paper of this series, we concluded that ring clusters are composed
by a young non-ionising intermediate age population about 300 Ma old, plus an
ionising population of 4.7 Ma in a 4:1 ratio. In this scenario, the ring
clusters would have formed almost simultaneously in a first star formation
episode. The stars in such a population would return part of their gas to the
interstellar medium during their evolution. A fraction of this gas could
escape from the cluster, while some of it would be unable to do so thus
remaining trapped in the cluster (Silich & Tenorio-Tagle, 2018). This gas
would feel the same gravitational potential as the cluster stars, consistent
with our results. A fraction of the gas that cooled down would form a new
stellar population, which would be responsible for the ionising photons. In
this scenario, the narrow gas component would be associated with the HII
region ionisation shell. According to the results presented here (see Sec.
4.2, this young ionising stellar population accounts for between 0.15 and 7.07
% of the total dynamical mass of the cluster.

##  5 Conclusions

In this third paper of a series, we analyse the kinematics of gas and stars in
the circumnuclear ring of NGC 7742 estimating the dynamical masses of their
CNSFRs from high spectral resolution data.

We have extracted spectra for each region using the apertures selected from
H$\alpha$ images.

The analysis of the emission line profiles, show the presence of two different
kinematical components with the same radial velocity. These two different
components have been found in the H$\alpha$ emission line in $\sim$ 90 % of
the analysed regions with most of them showing the same component also in the
[NII] emission lines. The narrow component has an almost constant value
between 10 km/s and 15 km/s while the broad component velocities are between
20 and 45 km/s.

In spite of the contribution to the nebular continuum, the CaT lines are seen
almost undiluted pointing to the stellar population being dominated by red
giant or supergiant stars.

The sizes of the star clusters have been measured from a F555W WFPC2-HST
image. About $\sim$ 60 % show a single star forming knot with the rest of them
showing between 2 and 4 knots each. Cluster velocity dispersions have been
derived from the CaT absorption lines using a modified version of Tonry &
Davis’ cross-correlation technique. These velocities together with the
measured sizes have been used to calculate the cluster dynamical masses under
the assumption that the clusters are virialised. The masses have been found to
be between 2.5 $\times$ 106 and 1.0 $\times$ 108 M⊙, values similar to those
found in the literature for circumnuclear clusters.

Finally, a comparison of the gas and star velocity dispersion, seldom found in
the literature, has been made revealing a complex internal structure of the
gas. A scenario has been put forward suggesting that the circumnuclear ring
clusters would have formed simultaneously in a first star formation episode
whose high mass stars would have returned part of their gas to the
interstellar medium during their evolution. A fraction of this initial ejecta
remains trapped in the gravitational potential of the cluster. A fraction of
the gas trapped would cooled down and form the young stellar population
responsible for the ionisation of the gas currently observed. This young
stellar population accounts for between 0.15 and 7.07 % of the total dynamical
mass of the cluster.

###### Acknowledgements.

This research has made use of the services of the ESO Science Archive Facility
and NASA’s Astrophysics Data System Abstract Service. It is based on
observations collected at the European Organisation for Astronomical Research
in the Southern Hemisphere under ESO programme 60.A-9301(A) and data products
created thereof. Also we have used observations obtained with the NASA/ESA HST
and also from the Hubble Legacy Archive, which is a collaboration between the
Space Telescope Science Institute (STScI/NASA), the Space Telescope European
Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre
(CADC/NRC/CSA). This work has been supported by Spanish grants from the former
Ministry of Economy, Industry and Competitiveness through the MINECO-FEDER
research grant AYA2016-79724-C4-1-P, and the present Ministry of Science and
Innovation through the research grant PID2019-107408GB-C42. S.Z. acknowledges
the support from contract: BES-2017-080509 associated to the first of these
grants. This work is based on observations made with the Gran Telescopio
Canarias (GTC), installed at the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofísica de Canarias, on the island of La
Palma. The data was obtained with the instrument MEGARA funded by European
Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER
2014–2020.

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##  Appendix A Tables

Table 8: Emission line radial velocities in km/s. Region ID | Component |  | v(H$\alpha$)
---
(km/s)
| v([NII]$\lambda$6584 Å)
---
(km/s)
| v([SII]$\lambda$6717 Å)
---
(km/s)
| v([SIII]$\lambda$9532 Å)
---
(km/s)
R1 | Narrow | 8.45 $\pm$ 0.41 | 8.36 $\pm$ 8.52 | 6.80 $\pm$ 0.65 | 6.71 $\pm$ 1.71
| Broad | 5.48 $\pm$ 0.85 | 5.76 $\pm$ 12.02 | 7.00 $\pm$ 5.35 | 12.20 $\pm$ 9.46
| Aditional | 15.4 $\pm$ 1.2 | 12.86 $\pm$ 37.74 | - | -
R3 | Narrow | 16.76 $\pm$ 0.09 | 16.57 $\pm$ 2.90 | 16.23 $\pm$ 0.58 | 15.42 $\pm$ 0.93
| Broad | 20.70 $\pm$ 0.95 | 18.72 $\pm$ 25.72 | 31.55 $\pm$ 9.52 | -
R4 | Narrow | 31.52 $\pm$ 0.20 | 32.54 $\pm$ 2.70 | 30.17 $\pm$ 1.12 | 30.07 $\pm$ 1.29
| Broad | 36.34 $\pm$ 0.78 | 36.35 $\pm$ 19.61 | 44.89 $\pm$ 5.20 | -
| Aditional | 18.2 $\pm$ 6.8 | - | - | -
R5 | Narrow | 26.16 $\pm$ 0.14 | 26.08 $\pm$ 2.50 | 24.49 $\pm$ 1.03 | 20.76 $\pm$ 0.71
| Broad | 8.65 $\pm$ 2.35 | 14.25 $\pm$ 2.81 | - | -
R6 | Narrow | 29.24 $\pm$ 0.12 | 29.47 $\pm$ 1.50 | 30.00 $\pm$ 1.20 | 25.99 $\pm$ 0.73
R7 | Narrow | -1.17 $\pm$ 0.18 | -1.76 $\pm$ 2.25 | -5.16 $\pm$ 1.16 | -8.95 $\pm$ 1.11
| Broad | -11.31 $\pm$ 2.00 | -12.18 $\pm$ 34.27 | - | -
R8 | Narrow | -12.66 $\pm$ 0.14 | -12.87 $\pm$ 2.25 | -15.13 $\pm$ 1.69 | -17.56 $\pm$ 1.10
| Broad | -20.15 $\pm$ 1.89 | -10.34 $\pm$ 1.99 | - | -
R9 | Narrow | 20.77 $\pm$ 0.14 | 20.17 $\pm$ 1.74 | 16.97 $\pm$ 0.92 | 15.72 $\pm$ 0.86
| Broad | 17.62 $\pm$ 1.73 | 12.72 $\pm$ 4.85 | - | -
R10 | Narrow | 13.33 $\pm$ 0.18 | 14.05 $\pm$ 2.75 | 10.04 $\pm$ 1.06 | 7.21 $\pm$ 1.32
| Broad | 12.28 $\pm$ 0.82 | 4.99 $\pm$ 2.79 | - | -
| Aditional | 22.0 $\pm$ 3.7 | - | - | -
R11 | Narrow | -34.76 $\pm$ 0.13 | -35.52 $\pm$ 2.35 | -34.80 $\pm$ 1.11 | -28.15 $\pm$ 1.98
| Broad | -32.66 $\pm$ 0.67 | -32.13 $\pm$ 12.97 | - | -
R12 | Narrow | 7.43 $\pm$ 0.20 | 7.75 $\pm$ 1.97 | 7.47 $\pm$ 1.11 | 0.42 $\pm$ 1.09
| Broad | 9.76 $\pm$ 1.08 | 13.28 $\pm$ 4.84 | - | -
R14 | Narrow | 33.16 $\pm$ 0.57 | 33.19 $\pm$ 1.87 | 32.44 $\pm$ 1.08 | 29.22 $\pm$ 1.52
| Broad | 32.80 $\pm$ 0.83 | 27.62 $\pm$ 2.30 | - | -
R15 | Narrow | 21.59 $\pm$ 0.20 | 21.20 $\pm$ 2.13 | 23.34 $\pm$ 1.25 | 19.14 $\pm$ 1.88
| Broad | 28.75 $\pm$ 2.27 | 29.54 $\pm$ 13.00 | - | -
R16 | Narrow | 29.96 $\pm$ 0.11 | 29.77 $\pm$ 2.06 | 30.20 $\pm$ 0.71 | 34.24 $\pm$ 1.26
| Broad | 33.72 $\pm$ 0.96 | 33.29 $\pm$ 2.21 | - | -
R17 | Narrow | 19.51 $\pm$ 0.48 | 19.75 $\pm$ 1.74 | 17.85 $\pm$ 1.08 | 18.66 $\pm$ 1.08
| Broad | 22.23 $\pm$ 2.07 | -2.46 $\pm$ 8.15 | - | -
| Aditional | -5.6 $\pm$ 3.7 | - | - | -
R18 | Narrow | -32.03 $\pm$ 0.23 | -32.19 $\pm$ 2.36 | -33.38 $\pm$ 0.78 | -28.76 $\pm$ 1.11
| Broad | -32.32 $\pm$ 0.77 | -31.15 $\pm$ 13.14 | - | -
R19 | Narrow | 24.30 $\pm$ 0.35 | 24.18 $\pm$ 2.95 | 24.44 $\pm$ 1.85 | 18.76 $\pm$ 1.95
| Broad | 27.52 $\pm$ 1.21 | 27.58 $\pm$ 18.10 | - | -
R20 | Narrow | 22.41 $\pm$ 0.21 | 21.58 $\pm$ 1.66 | 18.83 $\pm$ 1.63 | 15.92 $\pm$ 1.32
| Broad | 20.35 $\pm$ 1.82 | 35.15 $\pm$ 4.77 | - | -
R21 | Narrow | -22.03 $\pm$ 0.18 | -22.28 $\pm$ 1.93 | -22.68 $\pm$ 1.23 | -18.00 $\pm$ 2.02
| Broad | -21.05 $\pm$ 1.17 | -21.67 $\pm$ 18.40 | - | -
R22 | Narrow | 5.10 $\pm$ 0.18 | 5.02 $\pm$ 2.09 | 8.86 $\pm$ 1.40 | 9.60 $\pm$ 1.40
| Broad | 10.42 $\pm$ 1.14 | 12.67 $\pm$ 21.81 | - | -
R23 | Narrow | -32.87 $\pm$ 0.14 | -32.53 $\pm$ 2.16 | -32.46 $\pm$ 1.05 | -31.03 $\pm$ 2.33
| Broad | -28.32 $\pm$ 0.74 | -26.28 $\pm$ 21.73 | - | -
R25 | Narrow | -6.54 $\pm$ 0.29 | -7.28 $\pm$ 2.03 | -8.44 $\pm$ 1.64 | -12.23 $\pm$ 1.95
| Broad | -8.81 $\pm$ 1.48 | -1.92 $\pm$ 36.18 | - | -
R26 | Narrow | 2.20 $\pm$ 0.11 | 1.94 $\pm$ 2.83 | 2.88 $\pm$ 0.72 | 3.06 $\pm$ 1.21
| Broad | 2.15 $\pm$ 0.71 | 4.05 $\pm$ 14.49 | - | -
R27 | Narrow | 36.94 $\pm$ 0.17 | 36.00 $\pm$ 1.65 | 40.85 $\pm$ 1.65 | 33.51 $\pm$ 1.38
| Broad | 34.07 $\pm$ 2.48 | 37.55 $\pm$ 3.81 | - | -
R28 | Narrow | 11.51 $\pm$ 0.28 | 11.17 $\pm$ 2.75 | 9.57 $\pm$ 1.71 | 4.82 $\pm$ 2.29
| Broad | 7.78 $\pm$ 1.81 | 9.02 $\pm$ 3.04 | - | -
R29 | Narrow | -14.42 $\pm$ 0.17 | -14.11 $\pm$ 1.97 | -11.46 $\pm$ 2.50 | -18.38 $\pm$ 1.61
| Broad | -11.40 $\pm$ 2.70 | -8.94 $\pm$ 3.24 | - | -
R30 | Narrow | 18.25 $\pm$ 0.26 | 18.33 $\pm$ 1.90 | 18.33 $\pm$ 1.62 | 8.58 $\pm$ 1.60
| Broad | 18.49 $\pm$ 1.31 | 15.02 $\pm$ 12.76 | - | -
R31 | Narrow | 36.84 $\pm$ 0.20 | 37.15 $\pm$ 1.84 | 37.46 $\pm$ 1.26 | 35.65 $\pm$ 3.19
| Broad | 40.23 $\pm$ 1.20 | 38.44 $\pm$ 18.80 | - | -
R32 | Narrow | 22.39 $\pm$ 0.38 | 21.35 $\pm$ 1.92 | 20.17 $\pm$ 3.26 | 18.47 $\pm$ 3.59
| Broad | 13.25 $\pm$ 5.38 | 15.06 $\pm$ 23.31 | - | -
R33 | Narrow | 36.32 $\pm$ 0.19 | 35.78 $\pm$ 1.82 | 34.69 $\pm$ 1.09 | 34.17 $\pm$ 1.60
| Broad | 34.71 $\pm$ 0.98 | 35.38 $\pm$ 13.34 | - | -
R34 | Narrow | 3.65 $\pm$ 0.51 | 5.38 $\pm$ 4.40 | 4.42 $\pm$ 2.49 | 0.82 $\pm$ 1.80
| Broad | 8.36 $\pm$ 1.31 | - | - | -
R35 | Narrow | 2.89 $\pm$ 0.21 | 2.33 $\pm$ 1.86 | 2.10 $\pm$ 1.31 | 2.94 $\pm$ 1.64
| Broad | -0.14 $\pm$ 2.01 | -2.11 $\pm$ 19.32 | - | -
R36 | Narrow | -25.79 $\pm$ 0.19 | -26.63 $\pm$ 2.51 | -24.12 $\pm$ 1.11 | -25.83 $\pm$ 2.17
| Broad | -23.90 $\pm$ 0.77 | -19.77 $\pm$ 16.98 | - | -
R37 | Narrow | 24.90 $\pm$ 0.35 | 23.52 $\pm$ 2.03 | 14.58 $\pm$ 2.32 | 22.89 $\pm$ 2.69
| Broad | 13.91 $\pm$ 2.94 | 12.83 $\pm$ 19.68 | - | -
R38 | Narrow | 36.11 $\pm$ 0.21 | 35.79 $\pm$ 3.00 | 34.75 $\pm$ 1.30 | 28.96 $\pm$ 1.73
| Broad | 36.86 $\pm$ 1.35 | 36.11 $\pm$ 4.37 | - | -
R41 | Narrow | 34.67 $\pm$ 0.15 | 34.64 $\pm$ 1.92 | 35.04 $\pm$ 1.32 | 27.98 $\pm$ 2.33
| Broad | 33.56 $\pm$ 1.89 | 39.69 $\pm$ 32.18 | - | -
R42 | Narrow | -32.40 $\pm$ 0.13 | -31.92 $\pm$ 2.04 | -32.07 $\pm$ 1.17 | -31.60 $\pm$ 1.69
| Broad | -31.31 $\pm$ 1.71 | -42.44 $\pm$ 4.57 | - | -
R43 | Narrow | -8.73 $\pm$ 0.25 | -9.00 $\pm$ 1.87 | -10.08 $\pm$ 1.08 | -13.03 $\pm$ 2.53
| Broad | -3.94 $\pm$ 2.88 | -0.58 $\pm$ 31.93 | - | -
R44 | Narrow | 35.03 $\pm$ 0.28 | 35.21 $\pm$ 2.17 | 35.13 $\pm$ 1.44 | 33.02 $\pm$ 4.99
| Broad | 30.09 $\pm$ 2.93 | 28.49 $\pm$ 12.51 | - | -
R45 | Narrow | 24.60 $\pm$ 0.23 | 25.20 $\pm$ 2.35 | 27.57 $\pm$ 2.00 | 20.57 $\pm$ 6.19
| Broad | 23.16 $\pm$ 1.40 | 21.84 $\pm$ 18.15 | - | -
R48 | Narrow | 39.32 $\pm$ 0.31 | 38.96 $\pm$ 2.31 | 40.78 $\pm$ 1.64 | 30.08 $\pm$ 4.62
R50 | Narrow | 15.98 $\pm$ 0.19 | 15.83 $\pm$ 2.77 | 16.41 $\pm$ 1.20 | 15.44 $\pm$ 1.51
| Broad | 15.36 $\pm$ 1.45 | 14.01 $\pm$ 17.63 | - | -
R51 | Narrow | 2.94 $\pm$ 0.47 | 2.88 $\pm$ 2.97 | -0.77 $\pm$ 1.90 | -1.27 $\pm$ 2.43
| Broad | 3.98 $\pm$ 1.64 | 1.92 $\pm$ 8.11 | - | -
| Aditional | 70.0 $\pm$ 5.1 | - | - | -
R52 | Narrow | -38.04 $\pm$ 0.23 | -37.78 $\pm$ 2.06 | -37.94 $\pm$ 1.26 | -
| Broad | -38.93 $\pm$ 0.94 | -30.11 $\pm$ 28.29 | - | -
R53 | Narrow | 35.75 $\pm$ 0.31 | 34.68 $\pm$ 1.50 | 35.72 $\pm$ 1.28 | 32.18 $\pm$ 2.17
| Broad | 36.98 $\pm$ 1.76 | 43.82 $\pm$ 3.42 | - | -
R54 | Narrow | 25.28 $\pm$ 0.52 | 24.02 $\pm$ 2.51 | 17.09 $\pm$ 1.89 | 17.19 $\pm$ 14.77
| Broad | 23.41 $\pm$ 1.46 | 25.02 $\pm$ 9.82 | - | -
R55 | Narrow | 25.21 $\pm$ 0.34 | 25.25 $\pm$ 2.84 | 28.07 $\pm$ 1.47 | 28.46 $\pm$ 4.25
| Broad | 24.85 $\pm$ 1.70 | - | - | -
R56 | Narrow | -35.97 $\pm$ 0.25 | -36.12 $\pm$ 2.09 | -34.34 $\pm$ 1.73 | -36.20 $\pm$ 3.34
| Broad | -37.27 $\pm$ 1.38 | -39.26 $\pm$ 3.71 | - | -
R57 | Narrow | -14.13 $\pm$ 0.33 | -13.65 $\pm$ 0.44 | -11.87 $\pm$ 1.73 | -8.81 $\pm$ 3.74
| Broad | -11.79 $\pm$ 1.38 | - | - | -
R58 | Narrow | -10.75 $\pm$ 0.46 | -11.11 $\pm$ 2.99 | -8.87 $\pm$ 1.48 | -11.74 $\pm$ 2.75
| Broad | -5.86 $\pm$ 1.47 | -8.30 $\pm$ 7.53 | - | -
R59 | Narrow | 8.48 $\pm$ 0.80 | 6.90 $\pm$ 3.24 | 12.30 $\pm$ 1.46 | 13.59 $\pm$ 3.33
| Broad | 12.47 $\pm$ 1.39 | 16.39 $\pm$ 9.83 | - | -
R60 | Narrow | -27.44 $\pm$ 1.13 | -29.83 $\pm$ 1.78 | -24.40 $\pm$ 2.44 | -
| Broad | -29.94 $\pm$ 1.72 | -25.08 $\pm$ 19.39 | - | -
| Aditional | -23.1 $\pm$ 8.3 | - | - | -
R61 | Narrow | -18.37 $\pm$ 0.43 | -17.74 $\pm$ 1.89 | -25.36 $\pm$ 2.13 | -
| Broad | -23.49 $\pm$ 2.30 | -53.79 $\pm$ 8.01 | - | -
R62 | Narrow | 9.08 $\pm$ 0.24 | 9.47 $\pm$ 1.85 | 5.95 $\pm$ 1.29 | -0.53 $\pm$ 2.26
| Broad | -21.94 $\pm$ 1.30 | -8.71 $\pm$ 4.24 | - | -
R63 | Narrow | -23.16 $\pm$ 0.43 | -23.09 $\pm$ 0.02 | -23.19 $\pm$ 1.63 | -5.17 $\pm$ 8.10
| Broad | -27.74 $\pm$ 4.19 | - | - | -
R64 | Narrow | -28.54 $\pm$ 0.31 | -28.33 $\pm$ 2.00 | -30.42 $\pm$ 0.43 | -
| Broad | -29.32 $\pm$ 0.96 | -27.62 $\pm$ 18.21 | - | -
R65 | Narrow | 22.12 $\pm$ 1.90 | 19.99 $\pm$ 3.36 | 15.27 $\pm$ 2.99 | 21.07 $\pm$ 6.32
| Broad | -11.48 $\pm$ 17.52 | 3.89 $\pm$ 20.36 | - | -
R66 | Narrow | 2.72 $\pm$ 0.72 | -0.11 $\pm$ 3.34 | 2.49 $\pm$ 4.77 | -
| Broad | -3.87 $\pm$ 9.61 | - | - | -
R67 | Narrow | -30.25 $\pm$ 0.57 | -31.57 $\pm$ 0.44 | -30.12 $\pm$ 2.88 | -35.77 $\pm$ 3.54
| Broad | -37.18 $\pm$ 2.95 | - | - | -
| Aditional | -30.3 $\pm$ 41.2 | - | - | -
R69 | Narrow | -37.75 $\pm$ 0.45 | -37.11 $\pm$ 0.44 | -36.20 $\pm$ 1.66 | -30.85 $\pm$ 4.43
| Broad | -37.30 $\pm$ 0.80 | - | - | -
R70 | Narrow | -27.76 $\pm$ 0.41 | -27.34 $\pm$ 0.44 | -19.86 $\pm$ 2.79 | -27.51 $\pm$ 4.44
| Broad | -25.25 $\pm$ 1.40 | -19.36 $\pm$ 0.44 | - | -
R71 | Narrow | -23.83 $\pm$ 0.81 | -23.05 $\pm$ 2.16 | -25.74 $\pm$ 4.82 | 11.83 $\pm$ 8.24
| Broad | -12.49 $\pm$ 3.11 | -15.99 $\pm$ 5.19 | - | -
R72 | Narrow | -9.06 $\pm$ 0.76 | -6.67 $\pm$ 2.36 | -3.37 $\pm$ 1.66 | 3.74 $\pm$ 9.92
| Broad | -13.21 $\pm$ 14.51 | - | - | -
R73 | Narrow | -4.25 $\pm$ 0.49 | -4.58 $\pm$ 1.71 | -0.47 $\pm$ 3.67 | 4.78 $\pm$ 5.77
| Broad | 3.05 $\pm$ 3.26 | - | - | -
R74 | Narrow | -26.39 $\pm$ 0.83 | -25.15 $\pm$ 4.40 | -20.34 $\pm$ 2.70 | -
| Broad | -23.90 $\pm$ 1.09 | - | - | -
R75 | Narrow | -36.09 $\pm$ 0.52 | -36.79 $\pm$ 2.43 | -37.62 $\pm$ 2.41 | -3.99 $\pm$ 10.24
| Broad | -39.62 $\pm$ 1.17 | -36.99 $\pm$ 9.10 | - | -
R76 | Narrow | -36.02 $\pm$ 1.02 | -36.29 $\pm$ 0.44 | - | -
| Broad | -36.20 $\pm$ 2.76 | - | - | -
R77 | Narrow | 32.96 $\pm$ 0.88 | 34.81 $\pm$ 2.80 | 32.86 $\pm$ 2.89 | 42.18 $\pm$ 6.19
| Broad | 45.81 $\pm$ 12.91 | 28.09 $\pm$ 17.70 | - | -
R78 | Narrow | -34.01 $\pm$ 0.36 | -36.51 $\pm$ 2.98 | -30.98 $\pm$ 2.36 | -19.15 $\pm$ 5.50
R79 | Narrow | -38.11 $\pm$ 0.44 | -36.15 $\pm$ 2.73 | -42.11 $\pm$ 2.27 | -
R80 | Narrow | 36.02 $\pm$ 1.06 | 35.75 $\pm$ 3.72 | 34.29 $\pm$ 4.18 | 44.44 $\pm$ 11.54
| Broad | 23.15 $\pm$ 5.84 | - | - | -
R81 | Narrow | -33.21 $\pm$ 4.42 | -34.57 $\pm$ 1.97 | -32.45 $\pm$ 4.78 | -2.29 $\pm$ 9.84
R83 | Narrow | -31.66 $\pm$ 0.70 | -28.97 $\pm$ 2.22 | -30.74 $\pm$ 2.78 | -12.99 $\pm$ 12.92
| Broad | -28.34 $\pm$ 1.62 | - | - | -
R84 | Narrow | -24.83 $\pm$ 0.48 | -24.72 $\pm$ 2.17 | -19.45 $\pm$ 3.54 | -23.27 $\pm$ 6.79
R85 | Narrow | 40.32 $\pm$ 0.42 | 41.97 $\pm$ 2.35 | 44.65 $\pm$ 3.02 | 43.90 $\pm$ 4.47
R86 | Narrow | 38.53 $\pm$ 0.82 | 36.80 $\pm$ 2.58 | 33.48 $\pm$ 7.05 | 12.24 $\pm$ 9.29
| Broad | 42.41 $\pm$ 4.32 | 33.96 $\pm$ 9.17 | - | -
R87 | Narrow | 32.97 $\pm$ 1.57 | 33.07 $\pm$ 2.41 | - | -
| Broad | 37.86 $\pm$ 4.69 | 36.43 $\pm$ 8.65 | - | -
R88 | Narrow | -14.69 $\pm$ 0.59 | -14.98 $\pm$ 2.47 | -4.36 $\pm$ 2.96 | 4.40 $\pm$ 6.90
Table 8: continued.

Table 9: Emmision line velocity dispersions in km/s. Region ID | Component |  |  $\sigma$(H$\alpha$)
---
(km/s)
|  $\sigma$([NII]$\lambda$6584 Å)
---
(km/s)
|  $\sigma$([SII]$\lambda$6717 Å)
---
(km/s)
|  $\sigma$([SIII]$\lambda$9532 Å)
---
(km/s)
R1 | Narrow | 10.29 $\pm$ 0.09 | 7.88 $\pm$ 0.15 | 12.41 $\pm$ 0.80 | 18.98 $\pm$ 0.53
| Broad | 19.60 $\pm$ 0.20 | 18.30 $\pm$ 0.28 | 40.22 $\pm$ 4.14 | 62.64 $\pm$ 6.50
| Aditional | 47.7 $\pm$ 1.1 | 48.30 $\pm$ 2.34 | - | -
R3 | Narrow | 14.46 $\pm$ 0.08 | 12.67 $\pm$ 0.13 | 13.82 $\pm$ 0.65 | 13.68 $\pm$ 0.44
| Broad | 43.68 $\pm$ 1.66 | 34.51 $\pm$ 2.02 | 53.56 $\pm$ 8.84 | -
R4 | Narrow | 10.53 $\pm$ 0.12 | 12.44 $\pm$ 0.21 | 12.00 $\pm$ 1.34 | 14.06 $\pm$ 0.58
| Broad | 27.88 $\pm$ 0.59 | 45.04 $\pm$ 3.09 | 33.12 $\pm$ 3.54 | -
| Aditional | 69.2 $\pm$ 10.3 | - | - | -
R5 | Narrow | 11.95 $\pm$ 0.09 | 10.36 $\pm$ 0.14 | 15.29 $\pm$ 1.02 | 5.87 $\pm$ 0.12
| Broad | 30.27 $\pm$ 1.40 | 28.68 $\pm$ 1.95 | - | -
R6 | Narrow | 11.75 $\pm$ 0.11 | 11.09 $\pm$ 0.19 | 12.89 $\pm$ 0.97 | 5.34 $\pm$ 0.17
R7 | Narrow | 10.35 $\pm$ 0.12 | 10.66 $\pm$ 0.24 | 17.71 $\pm$ 0.96 | 12.19 $\pm$ 0.59
| Broad | 34.20 $\pm$ 2.12 | 44.95 $\pm$ 7.76 | - | -
R8 | Narrow | 11.07 $\pm$ 0.12 | 10.65 $\pm$ 0.24 | 20.54 $\pm$ 1.44 | 5.47 $\pm$ 0.19
| Broad | 40.85 $\pm$ 3.06 | 37.46 $\pm$ 4.33 | - | -
R9 | Narrow | 11.41 $\pm$ 0.11 | 10.77 $\pm$ 0.18 | 13.59 $\pm$ 0.77 | 10.10 $\pm$ 0.25
| Broad | 34.60 $\pm$ 2.60 | 55.29 $\pm$ 13.54 | - | -
R10 | Narrow | 9.37 $\pm$ 0.09 | 10.25 $\pm$ 0.19 | 14.87 $\pm$ 0.88 | 13.97 $\pm$ 0.59
| Broad | 25.02 $\pm$ 0.73 | 31.00 $\pm$ 2.90 | - | -
| Aditional | 91.4 $\pm$ 47.2 | - | - | -
R11 | Narrow | 9.54 $\pm$ 0.08 | 8.20 $\pm$ 0.14 | 15.92 $\pm$ 0.94 | 10.16 $\pm$ 0.61
| Broad | 25.85 $\pm$ 0.68 | 27.36 $\pm$ 1.51 | - | -
R12 | Narrow | 10.09 $\pm$ 0.14 | 12.29 $\pm$ 0.29 | 14.00 $\pm$ 0.90 | 10.74 $\pm$ 0.65
| Broad | 32.02 $\pm$ 1.49 | 63.10 $\pm$ 19.95 | - | -
R14 | Narrow | 7.83 $\pm$ 0.07 | 8.97 $\pm$ 0.15 | 16.32 $\pm$ 0.88 | 20.11 $\pm$ 1.13
| Broad | 25.41 $\pm$ 0.79 | 41.01 $\pm$ 4.28 | - | -
R15 | Narrow | 8.76 $\pm$ 0.10 | 7.97 $\pm$ 0.19 | 13.37 $\pm$ 0.99 | 18.32 $\pm$ 1.40
| Broad | 27.77 $\pm$ 1.86 | 24.11 $\pm$ 1.70 | - | -
R16 | Narrow | 10.18 $\pm$ 0.07 | 10.38 $\pm$ 0.14 | 17.69 $\pm$ 0.58 | 12.26 $\pm$ 0.57
| Broad | 32.21 $\pm$ 1.18 | 38.31 $\pm$ 3.09 | - | -
R17 | Narrow | 10.12 $\pm$ 0.13 | 11.85 $\pm$ 0.23 | 14.46 $\pm$ 0.87 | 10.94 $\pm$ 0.40
| Broad | 20.61 $\pm$ 0.66 | 67.10 $\pm$ 38.19 | - | -
| Aditional | 56.2 $\pm$ 19.7 | - | - | -
R18 | Narrow | 9.77 $\pm$ 0.10 | 9.00 $\pm$ 0.16 | 12.35 $\pm$ 0.61 | 8.77 $\pm$ 0.44
| Broad | 21.93 $\pm$ 0.57 | 27.39 $\pm$ 1.72 | - | -
R19 | Narrow | 10.56 $\pm$ 0.21 | 11.27 $\pm$ 0.40 | 20.29 $\pm$ 1.60 | 11.04 $\pm$ 0.80
| Broad | 28.58 $\pm$ 1.22 | 31.66 $\pm$ 4.27 | - | -
R20 | Narrow | 9.46 $\pm$ 0.13 | 10.50 $\pm$ 0.26 | 15.92 $\pm$ 1.32 | 9.73 $\pm$ 0.49
| Broad | 28.46 $\pm$ 2.30 | 52.29 $\pm$ 21.03 | - | -
R21 | Narrow | 10.71 $\pm$ 0.13 | 10.49 $\pm$ 0.22 | 18.39 $\pm$ 1.01 | 14.14 $\pm$ 1.27
| Broad | 32.84 $\pm$ 1.67 | 39.08 $\pm$ 4.47 | - | -
R22 | Narrow | 10.31 $\pm$ 0.10 | 11.17 $\pm$ 0.21 | 20.41 $\pm$ 1.16 | 8.64 $\pm$ 0.51
| Broad | 26.64 $\pm$ 0.93 | 36.56 $\pm$ 3.88 | - | -
R23 | Narrow | 9.31 $\pm$ 0.08 | 10.07 $\pm$ 0.17 | 15.81 $\pm$ 0.85 | -
| Broad | 26.19 $\pm$ 0.69 | 35.65 $\pm$ 3.30 | - | -
R25 | Narrow | 6.98 $\pm$ 0.15 | 9.97 $\pm$ 0.36 | 9.66 $\pm$ 1.26 | 9.46 $\pm$ 0.68
| Broad | 29.94 $\pm$ 2.00 | 47.27 $\pm$ 20.12 | - | -
R26 | Narrow | 10.41 $\pm$ 0.08 | 10.13 $\pm$ 0.16 | 14.80 $\pm$ 0.59 | 10.40 $\pm$ 0.42
| Broad | 30.04 $\pm$ 0.97 | 25.22 $\pm$ 1.37 | - | -
R27 | Narrow | 9.94 $\pm$ 0.11 | 9.47 $\pm$ 0.19 | 14.73 $\pm$ 1.32 | 6.12 $\pm$ 0.33
| Broad | 31.70 $\pm$ 3.32 | 47.44 $\pm$ 12.08 | - | -
R28 | Narrow | 8.99 $\pm$ 0.18 | 11.94 $\pm$ 0.50 | 7.64 $\pm$ 1.18 | 16.24 $\pm$ 1.24
| Broad | 31.40 $\pm$ 2.45 | 38.83 $\pm$ 12.25 | - | -
R29 | Narrow | 9.72 $\pm$ 0.13 | 10.03 $\pm$ 0.32 | 23.05 $\pm$ 2.16 | -
| Broad | 46.27 $\pm$ 5.53 | 50.99 $\pm$ 14.53 | - | -
R30 | Narrow | 6.12 $\pm$ 0.10 | 6.80 $\pm$ 0.20 | 12.79 $\pm$ 1.29 | 11.74 $\pm$ 0.95
| Broad | 22.06 $\pm$ 1.27 | 23.59 $\pm$ 2.72 | - | -
R31 | Narrow | 10.36 $\pm$ 0.14 | 10.80 $\pm$ 0.24 | 18.52 $\pm$ 1.04 | 17.96 $\pm$ 2.12
| Broad | 30.33 $\pm$ 1.45 | 46.99 $\pm$ 5.77 | - | -
R32 | Narrow | 8.48 $\pm$ 0.21 | 6.86 $\pm$ 0.33 | 15.81 $\pm$ 2.74 | 3.67 $\pm$ 0.44
| Broad | 35.29 $\pm$ 6.62 | 27.44 $\pm$ 10.01 | - | -
R33 | Narrow | 7.66 $\pm$ 0.09 | 8.41 $\pm$ 0.18 | 13.81 $\pm$ 0.79 | -
| Broad | 24.64 $\pm$ 1.01 | 29.96 $\pm$ 2.83 | - | -
R34 | Narrow | 4.95 $\pm$ 0.15 | 13.44 $\pm$ 0.52 | 17.72 $\pm$ 2.15 | 4.98 $\pm$ 0.44
| Broad | 20.81 $\pm$ 0.90 | - | - | -
R35 | Narrow | 9.20 $\pm$ 0.14 | 9.53 $\pm$ 0.28 | 12.83 $\pm$ 1.01 | 16.65 $\pm$ 1.03
| Broad | 34.45 $\pm$ 2.97 | 37.56 $\pm$ 6.46 | - | -
R36 | Narrow | 7.68 $\pm$ 0.10 | 8.41 $\pm$ 0.21 | 14.11 $\pm$ 0.87 | 13.05 $\pm$ 0.98
| Broad | 25.87 $\pm$ 0.87 | 31.60 $\pm$ 2.78 | - | -
R37 | Narrow | 10.09 $\pm$ 0.21 | 10.35 $\pm$ 0.42 | 11.40 $\pm$ 1.66 | -
| Broad | 31.68 $\pm$ 2.72 | 40.25 $\pm$ 8.20 | - | -
R38 | Narrow | 6.97 $\pm$ 0.10 | 4.21 $\pm$ 0.19 | 12.62 $\pm$ 1.00 | -
| Broad | 23.90 $\pm$ 1.51 | 16.62 $\pm$ 0.74 | - | -
R41 | Narrow | 11.91 $\pm$ 0.12 | 12.55 $\pm$ 0.25 | 18.88 $\pm$ 1.07 | 18.31 $\pm$ 1.41
| Broad | 41.70 $\pm$ 3.34 | 60.96 $\pm$ 10.48 | - | -
R42 | Narrow | 11.13 $\pm$ 0.10 | 10.37 $\pm$ 0.18 | 14.25 $\pm$ 0.90 | -
| Broad | 30.96 $\pm$ 2.51 | 42.24 $\pm$ 8.52 | - | -
R43 | Narrow | 11.55 $\pm$ 0.16 | 10.64 $\pm$ 0.30 | 12.69 $\pm$ 0.85 | 14.99 $\pm$ 1.45
| Broad | 29.91 $\pm$ 2.93 | 46.25 $\pm$ 12.56 | - | -
R44 | Narrow | 10.43 $\pm$ 0.21 | 9.06 $\pm$ 0.35 | 15.51 $\pm$ 1.14 | 27.95 $\pm$ 3.84
| Broad | 36.42 $\pm$ 4.41 | 26.70 $\pm$ 3.23 | - | -
R45 | Narrow | 9.50 $\pm$ 0.14 | 10.45 $\pm$ 0.38 | 17.98 $\pm$ 1.47 | 21.76 $\pm$ 5.07
| Broad | 28.71 $\pm$ 1.82 | 43.38 $\pm$ 6.65 | - | -
R48 | Narrow | 8.18 $\pm$ 0.19 | 13.34 $\pm$ 0.54 | 16.93 $\pm$ 1.30 | 17.43 $\pm$ 4.00
R50 | Narrow | 12.32 $\pm$ 0.14 | 11.97 $\pm$ 0.28 | 18.73 $\pm$ 1.03 | -
| Broad | 33.93 $\pm$ 1.99 | 30.08 $\pm$ 2.95 | - | -
R51 | Narrow | 7.05 $\pm$ 0.19 | 6.25 $\pm$ 0.41 | 16.80 $\pm$ 1.57 | -
| Broad | 20.33 $\pm$ 1.34 | 26.24 $\pm$ 2.72 | - | -
| Aditional | 139.6 $\pm$ 76.2 | - | - | -
R52 | Narrow | 8.57 $\pm$ 0.11 | 11.37 $\pm$ 0.29 | 17.03 $\pm$ 1.06 | -
| Broad | 25.61 $\pm$ 0.94 | 56.11 $\pm$ 9.65 | - | -
R53 | Narrow | 10.07 $\pm$ 0.19 | 10.89 $\pm$ 0.32 | 13.81 $\pm$ 1.01 | 15.46 $\pm$ 1.20
| Broad | 26.34 $\pm$ 1.96 | 65.51 $\pm$ 23.35 | - | -
R54 | Narrow | 7.88 $\pm$ 0.25 | 9.99 $\pm$ 0.63 | 16.48 $\pm$ 1.59 | 48.95 $\pm$ 21.75
| Broad | 25.72 $\pm$ 1.54 | 39.64 $\pm$ 5.50 | - | -
R55 | Narrow | 10.27 $\pm$ 0.20 | 15.42 $\pm$ 0.56 | 14.52 $\pm$ 1.18 | 22.84 $\pm$ 3.33
| Broad | 25.14 $\pm$ 1.85 | - | - | -
R56 | Narrow | 8.12 $\pm$ 0.15 | 10.99 $\pm$ 0.39 | 15.00 $\pm$ 1.43 | -
| Broad | 29.55 $\pm$ 1.89 | 61.53 $\pm$ 21.19 | - | -
R57 | Narrow | 10.86 $\pm$ 0.22 | 15.50 $\pm$ 0.47 | 20.19 $\pm$ 1.41 | 21.58 $\pm$ 2.17
| Broad | 27.27 $\pm$ 1.48 | - | - | -
R58 | Narrow | 7.78 $\pm$ 0.17 | 7.73 $\pm$ 0.34 | 12.98 $\pm$ 1.13 | 1.96 $\pm$ 0.17
| Broad | 20.68 $\pm$ 0.78 | 19.72 $\pm$ 1.37 | - | -
R59 | Narrow | 7.75 $\pm$ 0.22 | 7.53 $\pm$ 0.36 | 14.92 $\pm$ 1.13 | 20.25 $\pm$ 2.36
| Broad | 19.60 $\pm$ 0.56 | 21.82 $\pm$ 1.41 | - | -
R60 | Narrow | 7.11 $\pm$ 0.25 | 9.97 $\pm$ 0.38 | 19.17 $\pm$ 2.03 | -
| Broad | 16.61 $\pm$ 0.56 | 46.88 $\pm$ 10.37 | - | -
| Aditional | 53.9 $\pm$ 16.5 | - | - | -
R61 | Narrow | 9.62 $\pm$ 0.24 | 11.16 $\pm$ 0.45 | 11.74 $\pm$ 1.50 | -
| Broad | 27.83 $\pm$ 2.18 | 73.67 $\pm$ 27.62 | - | -
R62 | Narrow | 9.01 $\pm$ 0.19 | 8.64 $\pm$ 0.37 | 6.62 $\pm$ 0.85 | 6.74 $\pm$ 0.57
| Broad | 73.66 $\pm$ 21.55 | 50.73 $\pm$ 14.11 | - | -
R63 | Narrow | 9.47 $\pm$ 0.21 | 12.55 $\pm$ 0.53 | 15.19 $\pm$ 1.37 | 31.98 $\pm$ 6.23
| Broad | 25.75 $\pm$ 3.31 | - | - | -
R64 | Narrow | 3.11 $\pm$ 0.07 | 9.11 $\pm$ 0.35 | 16.11 $\pm$ 4.13 | -
| Broad | 21.80 $\pm$ 1.04 | 36.57 $\pm$ 7.47 | - | -
R65 | Narrow | 10.79 $\pm$ 0.30 | 13.66 $\pm$ 1.03 | 20.31 $\pm$ 2.44 | -
| Broad | 16.04 $\pm$ 2.95 | 43.69 $\pm$ 10.07 | - | -
R66 | Narrow | 12.53 $\pm$ 0.71 | 20.60 $\pm$ 2.26 | 25.61 $\pm$ 4.07 | -
| Broad | 62.39 $\pm$ 16.46 | - | - | -
R67 | Narrow | 8.64 $\pm$ 0.25 | 13.89 $\pm$ 0.61 | 20.49 $\pm$ 2.21 | -
| Broad | 24.97 $\pm$ 1.97 | - | - | -
| Aditional | 107.1 $\pm$ 60.4 | - | - | -
R69 | Narrow | 2.36 $\pm$ 0.09 | 15.15 $\pm$ 0.82 | 8.55 $\pm$ 1.11 | -
| Broad | 18.65 $\pm$ 0.86 | - | - | -
R70 | Narrow | 6.80 $\pm$ 0.20 | 9.11 $\pm$ 0.49 | 21.58 $\pm$ 2.33 | 14.70 $\pm$ 2.17
| Broad | 27.54 $\pm$ 1.71 | 39.91 $\pm$ 5.20 | - | -
R71 | Narrow | 6.30 $\pm$ 0.31 | - | 26.32 $\pm$ 3.93 | 30.00 $\pm$ 8.37
| Broad | 27.08 $\pm$ 2.36 | 27.03 $\pm$ 3.31 | - | -
R72 | Narrow | 8.42 $\pm$ 0.46 | 7.45 $\pm$ 0.75 | 5.52 $\pm$ 1.11 | 28.71 $\pm$ 8.92
| Broad | 37.55 $\pm$ 13.56 | - | - | -
R73 | Narrow | 7.44 $\pm$ 0.22 | 11.12 $\pm$ 0.50 | 18.87 $\pm$ 3.13 | -
| Broad | 23.58 $\pm$ 2.39 | - | - | -
R74 | Narrow | 3.88 $\pm$ 0.19 | 12.69 $\pm$ 0.55 | 20.64 $\pm$ 2.43 | -
| Broad | 18.01 $\pm$ 0.72 | - | - | -
R75 | Narrow | 6.27 $\pm$ 0.23 | 8.96 $\pm$ 0.56 | 16.42 $\pm$ 1.94 | 30.85 $\pm$ 16.07
| Broad | 24.80 $\pm$ 1.23 | 33.70 $\pm$ 4.61 | - | -
R76 | Narrow | 1.38 $\pm$ 0.11 | 11.82 $\pm$ 1.16 | - | -
| Broad | 23.41 $\pm$ 3.21 | - | - | -
R77 | Narrow | 12.34 $\pm$ 0.64 | 11.89 $\pm$ 1.32 | 17.13 $\pm$ 2.58 | 14.31 $\pm$ 4.20
| Broad | 14.85 $\pm$ 3.35 | 41.70 $\pm$ 10.83 | - | -
R78 | Narrow | 14.61 $\pm$ 0.42 | 14.73 $\pm$ 1.01 | 19.33 $\pm$ 2.00 | -
R79 | Narrow | 14.24 $\pm$ 0.43 | 14.83 $\pm$ 1.09 | 12.96 $\pm$ 1.79 | -
R80 | Narrow | 8.31 $\pm$ 0.56 | 20.28 $\pm$ 3.05 | 13.39 $\pm$ 2.68 | 25.07 $\pm$ 8.35
| Broad | 29.48 $\pm$ 5.07 | - | - | -
R81 | Narrow | 10.49 $\pm$ 0.38 | 13.53 $\pm$ 1.07 | 12.32 $\pm$ 3.04 | 15.98 $\pm$ 5.06
R83 | Narrow | 2.67 $\pm$ 0.14 | 15.04 $\pm$ 1.03 | 11.39 $\pm$ 2.37 | 16.80 $\pm$ 4.93
| Broad | 21.92 $\pm$ 1.62 | - | - | -
R84 | Narrow | 13.88 $\pm$ 0.53 | 15.14 $\pm$ 1.13 | 12.03 $\pm$ 3.18 | -
R85 | Narrow | 10.46 $\pm$ 0.39 | 18.51 $\pm$ 1.42 | 16.01 $\pm$ 2.57 | -
R86 | Narrow | 6.13 $\pm$ 0.43 | 6.36 $\pm$ 0.99 | 34.38 $\pm$ 5.99 | 34.37 $\pm$ 8.38
| Broad | 31.72 $\pm$ 7.24 | 35.05 $\pm$ 11.08 | - | -
| Broad | 20.82 $\pm$ 4.51 | 9.20 $\pm$ 3.17 | - | -
R88 | Narrow | 17.89 $\pm$ 0.87 | 17.76 $\pm$ 1.67 | 14.69 $\pm$ 2.73 | -
Table 9: continued.

Table 10: Equivalent widths of stellar absorption lines and velocity dispersions of the observed CNSFRs. Region ID |  | EW(CaII)a
---
(Å)
| EW(MgI)
---
(Å)
R1 | 7.307 $\pm$ 0.264 | 1.686 $\pm$ 0.035
R3 | 7.301 $\pm$ 0.278 | 2.329 $\pm$ 0.063
R4 | 7.558 $\pm$ 0.303 | 1.868 $\pm$ 0.044
R5 | 7.418 $\pm$ 0.338 | 2.147 $\pm$ 0.048
R6 | 7.118 $\pm$ 0.318 | 2.141 $\pm$ 0.073
R7 | 6.732 $\pm$ 0.339 | 1.972 $\pm$ 0.056
R8 | 7.350 $\pm$ 0.299 | 2.156 $\pm$ 0.060
R9 | 7.571 $\pm$ 0.346 | 2.013 $\pm$ 0.054
R10 | 7.008 $\pm$ 0.297 | 1.987 $\pm$ 0.048
R11 | 7.281 $\pm$ 0.211 | 2.840 $\pm$ 0.092
R12 | 7.279 $\pm$ 0.304 | 2.377 $\pm$ 0.062
R14 | 7.150 $\pm$ 0.288 | 2.474 $\pm$ 0.065
R15 | 7.033 $\pm$ 0.384 | 2.308 $\pm$ 0.066
R16 | 8.796 $\pm$ 0.328 | 2.230 $\pm$ 0.063
R17 | 8.094 $\pm$ 0.283 | 1.911 $\pm$ 0.054
R18 | 7.138 $\pm$ 0.351 | 2.322 $\pm$ 0.076
R19 | 6.682 $\pm$ 0.279 | 2.105 $\pm$ 0.064
R20 | 8.003 $\pm$ 0.363 | 2.292 $\pm$ 0.067
R21 | 7.592 $\pm$ 0.343 | 2.677 $\pm$ 0.082
R22 | 7.549 $\pm$ 0.224 | 2.905 $\pm$ 0.109
R23 | 6.828 $\pm$ 0.257 | 2.773 $\pm$ 0.093
R25 | 7.429 $\pm$ 0.298 | 2.619 $\pm$ 0.078
R26 | 7.350 $\pm$ 0.219 | 2.306 $\pm$ 0.063
R27 | 8.381 $\pm$ 0.381 | 2.025 $\pm$ 0.064
R28 | 7.490 $\pm$ 0.340 | 2.429 $\pm$ 0.083
R29 | 7.267 $\pm$ 0.268 | 2.741 $\pm$ 0.082
R30 | 7.277 $\pm$ 0.283 | 2.733 $\pm$ 0.088
R31 | 6.737 $\pm$ 0.297 | 2.336 $\pm$ 0.083
R32 | 7.288 $\pm$ 0.282 | 2.784 $\pm$ 0.100
R33 | 7.050 $\pm$ 0.255 | 2.496 $\pm$ 0.079
R34 | 7.029 $\pm$ 0.338 | 2.119 $\pm$ 0.087
R35 | 6.148 $\pm$ 0.342 | 2.338 $\pm$ 0.079
R36 | 7.320 $\pm$ 0.257 | 2.913 $\pm$ 0.099
R37 | 8.513 $\pm$ 0.348 | 2.273 $\pm$ 0.077
R38 | 6.462 $\pm$ 0.286 | 2.263 $\pm$ 0.078
R41 | 7.412 $\pm$ 0.295 | 2.799 $\pm$ 0.089
R42 | 6.753 $\pm$ 0.332 | 2.411 $\pm$ 0.070
R43 | 7.127 $\pm$ 0.268 | 2.800 $\pm$ 0.089
R44 | 7.775 $\pm$ 0.390 | 2.620 $\pm$ 0.079
R45 | 7.637 $\pm$ 0.233 | 2.928 $\pm$ 0.101
R47 | 6.918 $\pm$ 0.297 | 2.580 $\pm$ 0.084
R48 | 6.770 $\pm$ 0.296 | 2.583 $\pm$ 0.096
R50 | 7.659 $\pm$ 0.252 | 2.587 $\pm$ 0.082
R51 | 7.489 $\pm$ 0.238 | 3.024 $\pm$ 0.118
R52 | 6.840 $\pm$ 0.283 | 2.486 $\pm$ 0.081
R53 | 7.125 $\pm$ 0.298 | 2.128 $\pm$ 0.075
R54 | 6.640 $\pm$ 0.241 | 2.416 $\pm$ 0.080
R55 | 7.522 $\pm$ 0.310 | 2.708 $\pm$ 0.100
R56 | 6.720 $\pm$ 0.268 | 2.682 $\pm$ 0.082
R57 | 6.945 $\pm$ 0.258 | 3.077 $\pm$ 0.120
R58 | 7.636 $\pm$ 0.296 | 2.936 $\pm$ 0.104
R59 | 8.311 $\pm$ 0.296 | 2.896 $\pm$ 0.112
R60 | 6.606 $\pm$ 0.362 | 2.272 $\pm$ 0.068
R61 | 8.889 $\pm$ 0.723 | 2.482 $\pm$ 0.080
R62 | 7.057 $\pm$ 0.377 | 2.564 $\pm$ 0.092
R63 | 8.640 $\pm$ 0.489 | 2.321 $\pm$ 0.077
R64 | 6.857 $\pm$ 0.299 | 2.387 $\pm$ 0.068
R65 | 7.876 $\pm$ 0.254 | 2.609 $\pm$ 0.080
R66 | 7.559 $\pm$ 0.224 | 2.485 $\pm$ 0.084
R67 | 9.055 $\pm$ 0.422 | 2.408 $\pm$ 0.076
R69 | 6.696 $\pm$ 0.229 | 2.881 $\pm$ 0.108
R70 | 7.076 $\pm$ 0.278 | 2.845 $\pm$ 0.111
R71 | 6.958 $\pm$ 0.236 | 3.010 $\pm$ 0.106
R72 | 7.296 $\pm$ 0.242 | 3.173 $\pm$ 0.131
R73 | 6.577 $\pm$ 0.209 | 3.506 $\pm$ 0.166
R74 | 6.576 $\pm$ 0.323 | 2.888 $\pm$ 0.114
R75 | 6.743 $\pm$ 0.241 | 3.244 $\pm$ 0.125
R76 | 6.631 $\pm$ 0.251 | 3.348 $\pm$ 0.167
R77 | 8.194 $\pm$ 0.343 | 2.700 $\pm$ 0.131
R78 | 7.981 $\pm$ 0.419 | 2.773 $\pm$ 0.094
R79 | 6.794 $\pm$ 0.301 | 2.623 $\pm$ 0.082
R80 | 7.454 $\pm$ 0.330 | 2.621 $\pm$ 0.093
R81 | 7.236 $\pm$ 0.288 | 2.300 $\pm$ 0.109
R83 | 7.441 $\pm$ 0.310 | 3.077 $\pm$ 0.109
R84 | 7.582 $\pm$ 0.350 | 3.898 $\pm$ 0.371
R85 | 7.359 $\pm$ 0.261 | 2.937 $\pm$ 0.110
R86 | 7.711 $\pm$ 0.244 | 3.111 $\pm$ 0.109
R87 | 7.025 $\pm$ 0.473 | 2.943 $\pm$ 0.105
R88 | 8.033 $\pm$ 0.345 | 3.605 $\pm$ 0.184
Table 10: continued.

  * •

a ($\lambda$8542Å + $\lambda$8662Å+ $\lambda$8498Å).