# The study of two barred galaxies with curious kinematical features

A. Saburova, I. Katkov, A. Khoperskov, A. Zasov, I. Uklein

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A. Saburova, I. Katkov, A. Khoperskov, A. Zasov, I. Uklein. The study of two barred galaxies with curious kinematical features. Monthly Notices of the Royal Astronomical Society, 2017, 470 (1), pp.20-33. 10.1093/mnras/stx1200. hal-02161874

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# The study of two barred galaxies with curious kinematical features

A. S. Saburova,<fnref n="1" />* I. Y. Katkov,<fnref n="1" /> S. A. Khoperskov,<fnref n="2" />,<fnref n="3" /> A. V. Zasov<fnref n="1" />,<fnref n="4" /> and R. I. Uklein<fnref n="5" />

Accepted 2017 May 12. Received 2017 May 11; in original form 2017 February 5

## ABSTRACT

We performed long-slit spectral observations of two SB-type galaxies: NGC 5347 and UGC 1344. They were previously suspected as the galaxies with unusually low mass-to-light ratios (on the ground of mass estimates from the H₁ linewidths), which are in conflict with their observed colours. The observations were conducted at the Russian 6-m telescope. The aim of this study was to clarify the kinematics and structure, as well as the properties of stellar populations of the galaxies. The results of observations disproved the peculiarly low mass-to-light ratios of both galaxies. The most probable reasons of underestimation of their masses are discussed. We tried to reproduce the main observed features of kinematical profiles of the galaxies in the N-body simulations of barred galaxies. We found that both galaxies possess central components of different structures. Indeed, the age and velocity dispersion of stellar population in NGC 5347 are low in its innermost part in comparison to that of the bulge or a bar, which agrees with the presence of nuclear kinematically decoupled disc. It probably was formed due to the bar that supplied the inner region with gas. The kinematical profiles of the second galaxy UGC 1344 give evidence in favour of the central peanut-shaped bulge. In spite of the different luminosities of the two galaxies, they possess nearly equal (close to solar) central stellar abundance and the flattening of the stellar metallicity gradient in the bar regions. However, in the less luminous NGC 5347, the mean stellar age is younger than that in UGC 1344.

**Key words:** galaxies: evolution – galaxies: individual: UGC 1344, NGC 5347 – galaxies: kinematics and dynamics.

## 1 INTRODUCTION

Stellar initial mass function (IMF) has a fundamental meaning to understand the evolution of galaxies and star formation. However, the question of its universality still remains a matter of hot discussion. There is evidence either in its favour or against it (see e.g. Kroupa 2002; Gilmore 2001; Bastian, Covey & Meyer 2010; Davis & McDermid 2016). In Saburova, Shaldenkova & Zasov (2009), we tried to find the candidates of discy galaxies where one can suspect a significant difference of stellar IMF from the ‘standard’ Salpeter IMF (Salpeter 1955) or Kroupa (Kroupa 2001) one. We were looking for such galaxies among the objects with peculiarly low or high dynamical mass-to-light ratios $M/L_B = v^2 r_{25}/(GL_B)$, which conflict with observed colour indices, where v is the velocity of rotation, $r_{25}$ is the optical radius and $L_B$ is the B-band total luminosity. We studied in details several galaxies suspected for unusual M/L of their stellar

populations in subsequent papers: Saburova et al. (2013, 2015), and Saburova, Bizyaev & Zasov (2011). For the candidates we considered in these papers, the new photometric and kinematic data have not confirmed the expected peculiarity, giving evidence in favour of the universality of the IMF in discy galaxies. However, we continue our study of the galaxies suspected with peculiar M/L.

The aim of this paper is the study of two galaxies from our list of galaxies with presumably unusually low $M/L_B$ ratio on the basis of Hyperleda<fnref n="1" /> catalogue data (Makarov et al. 2014): NGC 5347 and UGC 1344. Their main properties are presented in Table 1. Both are early-type disc galaxies, possessing similar red colours of stellar population, a ring and a prominent bar. The luminosity of UGC 1344 is significantly higher than that of NGC 5347. The inner ring of NGC 5347 is distinguished by its far-ultraviolet (FUV) continuum and is conspicuous in the continuum-subtracted $H\alpha$ images, which indicates the active star formation there (Comerón 2013). The ring

<footnote n="1">¹Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Universitetskij pr., 13, Moscow 119991, Russia</footnote>

<footnote n="2">²GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen, F-92190 Meudon, France</footnote>

<footnote n="3">³Institute of Astronomy, Russian Academy of Sciences, 48 Pyatnitskaya st., 119017 Moscow, Russia</footnote>

<footnote n="4">⁴Faculty of Physics, Moscow M.V. Lomonosov State University, Leninskie gory 1, Moscow 119991, Russia</footnote>

<footnote n="5">⁵Special Astrophysical Observatory, Russian Academy of Sciences, Nizhniy Arkhyz, Karachai-Cherkessian Republic 357147, Russia</footnote>

<footnote>* E-mail: saburovaann@gmail.com</footnote>

<footnote n="1">¹ http://leda.univ-lyon1.fr/</footnote>
<table><caption>**Table 1.** Main properties of the observed galaxies: name; adopted distance; morphological type; apparent B-band stellar magnitude corrected for the extinction; inclination angle; and B-V colour index corrected for the extinction.</caption><thead><tr><th>Galaxy</th><th><i>D</i><br>(Mpc)</th><th>Type</th><th><i>m</i><sub>B</sub><br>(mag)</th><th><i>i</i><br>(°)</th><th>(<i>B</i> − <i>V</i>)<sub>0</sub><br>(mag)</th></tr></thead><tbody><tr><td>NGC 5347</td><td>32</td><td>SBab</td><td>13.16</td><td>45</td><td>0.7</td></tr><tr><td>UGC 1344</td><td>58</td><td>SBa</td><td>12.98</td><td>61</td><td>0.74</td></tr></tbody></table>

<table><caption>**Table 2.** Log of observations.</caption><thead><tr><th>Galaxy</th><th>Slit PA<br>(°)</th><th>Date</th><th>Exposure time<br>(s)</th><th>Seeing<br>(arcsec)</th></tr></thead><tbody><tr><td>NGC 5347</td><td>103</td><td>11.05.2016</td><td>3600</td><td>3</td></tr><tr><td>NGC 5347</td><td>120</td><td>11.05.2016</td><td>3600</td><td>2.9</td></tr><tr><td>NGC 5347</td><td>30</td><td>11.05.2016</td><td>1866</td><td>3</td></tr><tr><td>UGC 1344</td><td>45</td><td>17.09.2015</td><td>13 200</td><td>1.7</td></tr><tr><td>UGC 1344</td><td>82</td><td>19.09.2015</td><td>18 000</td><td>2</td></tr></tbody></table>

of UGC 1344 is not perceptible in FUV; hence, it should be also passive in $H\alpha$ (Comerón 2013), being a fossil ring not hosting star formation. NGC 5347 is a Seyfert 2 galaxy with the mass of central black hole of $\log(M_{bh}/M_{\odot}) = 8.73$ (Izumi, Kawakatu & Kohno 2016). The $H\alpha$ observations of NGC 5347 demonstrate that it has a peculiar morphology: The gaseous disc position angle is almost perpendicular to that of the optical disc. There is a hint that the $H\alpha$ is elongated along the major axis of the optical disc in the inner part of the galaxy: In this case, the galaxy may have a strong warp; however, new $H\alpha$ observations with better resolution are needed to confirm or disprove it (Noordermeer et al. 2005). Another interesting detail considering this galaxy is that according to *Hubble Space Telescope (HST)* observations, it possesses a very well-defined nuclear dust spiral structure (Martini et al. 2003). This finding is in good agreement with the kinematical properties obtained in this paper (see below). It seems unlikely that the formation of NGC 5347 was

affected by recent interaction. According to García-Barreto, Carrillo & Vera-Villamizar (2003), NGC 5347 does not have companions within the distance of its 10–20 diameters; however, it belongs to Canes Venatici Camelopardalis cloud (Tully 1987). UGC 1344 belongs to a group (Garcia 1993) and, as we will show below, has a small companion 2MASX J01522797+3629533 at the distance of roughly 24 kpc.

As it will be demonstrated in this paper, the peculiarity of the *M/L* of the considered galaxies did not find a confirmation by the new kinematical data. Nevertheless, these systems represent the interesting cases due to the curious inner kinematical features and deserve the detailed study we have performed.

This paper is organized as follows: Section 2 is devoted to the details of data reduction and the results of observations; the discussion including the comparison with our *N*-body simulations is given in Section 3; and the main results are summarized in Section 4.

## 2 OBSERVATIONS

### 2.1 Reduction of spectral observations

We carried out the long-slit spectral observations of NGC 5347 and UGC 1344 with the SCORPIO focal reducer (see Afanasiev & Moiseev 2005) at the Russian 6-m BTA telescope in 2015 and 2016. In Table 2, we give the position angles of the slit, the exposure times, the dates of observations and seeing. We used VPHG2300G grism with the spectral range of 4800–5570 Å and reciprocal dispersion of 0.38 Å pixel$^{-1}$. This corresponds to spectral resolution $R \approx 2200$. The scale along the slit is 0.36 arcsec pixel$^{-1}$. Fig. 1 demonstrates the slit positions for the galaxies.

The data were processed as it was described in Saburova et al. (2015). The data reduction included the following steps: bias subtraction and truncation of overscan regions; division by normalized flat-field frames; the wavelength calibration using the spectrum of He–Ne–Ar calibration lamp; linearization and summation; the night sky subtraction; and the flux calibration using the spectra of the standard spectrophotometric stars HZ2 and Feige 56. We also took into account the variation of instrumental profile of the

<figure><img src="image_3.png" /><figcaption>**Figure 1.** Images of the galaxies with the overplotted positions of the slits. Left-hand panel: composite SDSS gri-image of NGC 5347, right-hand panel: R-band image of UGC 1344 taken with BTA.</figcaption></figure>
spectrograph by analysing the twilight sky spectrum observed in the same observational run (for more details, see e.g. Saburova et al. 2015).

After the primary reduction, we fitted the spectra with high-resolution PEGASE.HR (Le Borgne et al. 2004) simple stellar population (SSP) models convolved with the instrumental profile. For this purpose, we used the *NBURSTS* full spectral-fitting technique (Chilingarian et al. 2007a,b). The advantage of this technique is that it allows us to fit the spectrum in a pixel space. In this method, the parameters of the stellar populations are derived by the non-linear minimization of the quadratic difference chi-square between the observed and model spectra. The parameters of SSP that we utilized are the age *T* (Gyr) and metallicity [*Z*/*H*] (dex) of stellar population. The line-of-sight velocity distribution (LOSVD) of stars was parametrized by the Gauss-Hermite series (see van der Marel & Franx 1993). From the modelling, we determined the luminosity-weighted stellar age and metallicity, LOS velocity, velocity dispersion and Gauss-Hermite moments *h*<sub>3</sub> and *h*<sub>4</sub> that characterize the deviation of LOSVD from the Gaussian profile.

We estimated the parameter uncertainties of our stellar population model by means of Monte Carlo simulations for a hundred realizations of synthetic spectra for each spatial bin, which were created by adding a random noise corresponding to the signal-to-noise ratio (S/N) in the bin to the best-fitting model.

We also analysed the emission spectra that we obtained by subtraction of model stellar spectra from the observed ones. To derive the velocity and velocity dispersion of ionized gas, we fitted the emission lines by Gaussian profiles. To increase the S/N of the spectra, the adaptive binning was used in the fitting. We specified S/N = 15 for all slices besides that with PA = 30° of NGC 5347 for which we adopted S/N = 10.

## 2.2 The non-parametric LOSVD reconstruction

Parallel with the parametric LOSVD reconstruction described in the previous section, we also applied to UGC 1344 – the galaxy with the highest S/N of the spectra – a non-parametric recovery technique based on the full spectral fitting. The technique is described in details in Katkov, Sil'chenko & Afanasiev (2013) and Katkov et al. (2016).

The main idea of the method is that observed galaxy spectrum logarithmically rebinned in the wavelength domain can be represented by the convolution of LOSVD and a typical stellar (template) spectrum. The reconstruction technique does not require any a priori knowledge about the LOSVD shape and searches for the solution of the convolution problem as a linear inverse ill-conditioned problem by using a smoothing regularization. We used the SSP model from the *NBURSTS* fitting, pre-convolved with the line spread function output, as a template spectrum. In the case of contribution to the integrated spectrum of very different stellar populations, the technique should be applied with caution. Since the method fits observed spectrum by only one given template, the mismatch template problem can lead to a biased LOSVD recovery. For UGC 1344, we show below that stellar population parameters of two components are similar; hence, the non-parametric LOSVD recovery is not affected by the mismatch template problem.

The stellar position–velocity diagram for UGC 1344 obtained by this technique for PA = 45° (left-hand panel) and 82° (right-hand panel) is presented in Fig. 2. This method allowed us to reveal the asymmetry of stellar LOSVD of UGC 1344 for spectral slice PA = 45° at $r \approx \pm 5$ arcsec. We demonstrate two-component velocity distribution at these radii in Fig. 3 for two bins at the right- and left-hand sides from the centre of the galaxy. The narrow range of the radii for the two bins corresponds to the transitional region between the slower component dominating in all central area and the faster rotating component. Green (light-grey in printed version) lines denote the dominating component with slower rotation and blue (dark-grey in printed version) lines mark another faster rotating component. The resulting model is demonstrated by the dashed line and the observed LOSVD is shown by the black histogram. The corresponding decomposition of the spectra in the right- and left-hand bins is demonstrated in Fig. 4. Red (grey in printed version) and black lines show the model and the observed spectra, respectively; the two components are denoted by blue (dark-grey in printed version) and green (light-grey in printed version) similarly to the previous figure. The properties of stellar population of these components are given in Table 3. From Table 3, one can see that the dominating component has slower rotation and higher velocity dispersion. Its age and metallicity are close to that of the second component. Thus, we can propose that the slow decoupled

<figure><img src="image_4.png" /><figcaption>**Figure 2.** The stellar position–velocity diagrams of UGC 1344 obtained by non-parametric LOSVD reconstruction method for PA = 45° (left-hand panel) and 82° (right-hand panel). Dash-dotted lines show the transitional region where kinematically decoupled component is clearly seen. These regions were used for the non-parametric analysis as well as for the spectral decomposition. The LOSVD is normalized for a given radial position.</figcaption></figure>
<figure><img src="image_5.png" /><figcaption>**Figure 3.** Decomposition of stellar LOSVD of UGC 1344 in ±5 arcsec from the nucleus where slow component is detected. Recovered stellar LOSVDs are shown by black stepped lines. Green (light-grey in printed version) and blue (dark grey in printed version) lines demonstrate LOSVD decomposition into two Gaussian components (main component and kinematically decoupled one). Pink dashed line marks the resulting model.</figcaption></figure>

<figure><img src="image_6.png" /><figcaption>**Figure 4.** Spectral decomposition in two bins at ±5.5 arcsec from the nucleus of UGC 1344 where kinematically decoupled component is detected. The red line corresponds to the best-fitting model overplotted on top of the observed spectrum (black line). Green (light-grey in printed version) and blue (dark-grey in printed version) lines show the different components. Residuals are shown on the bottom of each panel. Magenta line presents noise level of observed spectra.</figcaption></figure>

component has the internal origin and most probably was formed by dynamical evolution of the bar and could be the x-shaped bulge (for more details, see Discussion). The fast-rotating component apparently represents the main disc of the galaxy.

Note that the slowly rotating component is clearly seen only in the cut running along the major axis. For the cut along the bar at PA = 82°, it shows itself very marginally. It may be explained

by the lower LOS component of rotational velocity of the bar, which makes it difficult to note the spectral input of slowly rotating second component parallel with the fact that the slow component can have lower surface brightness in comparison to the bar. When the slit is oriented along the bar, the latter dominates the dynamics in this region, making it difficult to reveal the faint detail of velocity distribution.
<table><caption>**Table 3.** Results of spectral decomposition for two positions from the left- and right-hand sides from the centre of UGC 1344: the light fraction of the component, the LOS stellar velocity, the stellar velocity dispersion, SSP-age and SSP-metallicity of stars. Component weights are the same for both bins; hence, only one column is shown in the table.</caption><thead><tr><th rowspan="2"></th><th rowspan="2">w<sub>1,2</sub></th><th rowspan="2">v<sub>1</sub> (km s<sup>-1</sup>)</th><th colspan="3">R = -5.5 ± 1 arcsec</th><th colspan="3">R = 5.5 ± 1 arcsec</th></tr><tr><th>σ<sub>1</sub> (km s<sup>-1</sup>)</th><th>T<sub>SSP,1</sub> (Gyr)</th><th>Z<sub>SSP,1</sub> (dex)</th><th>σ<sub>2</sub> (km s<sup>-1</sup>)</th><th>T<sub>SSP,2</sub> (Gyr)</th><th>Z<sub>SSP,2</sub> (dex)</th></tr></thead><tbody><tr><td>Cmp.1</td><td>0.75 ± 0.02</td><td>4454.1 ± 16.5</td><td>114.2 ± 11.6</td><td>7.63 ± 0.32</td><td>-0.17 ± 0.02</td><td>4340.7 ± 15.3</td><td>111.2 ± 8.4</td><td>8.21 ± 0.57</td><td>-0.18 ± 0.02</td></tr><tr><td>Cmp.2</td><td>0.25 ± 0.02</td><td>4609.5 ± 48.9</td><td>91.0 ± 20.7</td><td>6.98 ± 0.65</td><td>-0.13 ± 0.02</td><td>4166.4 ± 45.5</td><td>80.4 ± 29.2</td><td>9.18 ± 0.83</td><td>-0.25 ± 0.04</td></tr></tbody></table>

## 2.3 Kinematical profiles

In Figs 5 and 6 (the third and fourth panels from the top), we show the radial profiles of LOS velocity and velocity dispersion of stars and ionized gas for different spectral slices of NGC 5347 and UGC 1344, respectively, obtained by parametric LOSVD reconstruction. In these figures, we also give the reference images from SDSS and SCOPRIO (top panels) and the radial profiles of fluxes of continuum and emission lines (second panels from the top).

The unusual behaviour of the emission gas velocities in the central regions of the galaxies is worth noting. In both galaxies, the gas possesses high velocity dispersion here, which is equal or exceeds the stellar one. In NGC 5347, the LOS gas velocities are shifted at 40–80 km s⁻¹ towards the observer with respect to the stellar ones along the slits PA = 120° and 103°, which is natural to connect with the active galactic nucleus (AGN) activity in this galaxy. The ionized gas velocity profile of UGC 1344 is asymmetric and rises much steeper than that of stars in the left half of the galaxy, which is evident from both spectral slices. Moreover, the deviation of the ionized gas velocity profile is more prominent for [O III] line than for H β, especially for the slice with PA = 45°. The flux ratio [O III] versus H β lines is quite high, it roughly equals to 5 in the centre, increasing to the left part of the galaxy and decreasing to the opposite side (see Fig. 6, second panel from the top). The high flux ratio together with high velocity dispersion of ionized gas is a clear indication of AGN in the galaxy, which also could be one of the causes of the asymmetry of velocity distribution noted above. Another probable cause of the asymmetry is the gas interaction with the contrasting bar in the presence of dust absorption, which is usually observed along the bar in SB-galaxies.

As one can see from the figures, the radial profiles of stellar LOS velocity of both galaxies are not smooth for the position angles close to the major axis. There are regions where the velocity gradient changes its sign. We mark by dotted vertical lines the areas where the steep velocity profile becomes shallower or even begins to decrease. This behaviour is typical for barred galaxies. The velocity turnover was already observed in 1980s by Peterson & Huntley (1980) in the barred galaxy NGC1300. It was also found in edge-on systems with boxy or peanut-shaped bulges by Chung & Bureau (2004) and predicted by simulations of Bureau & Athanassoula (2005). The double hump in the velocity profile was found in 60 per cent of barred galaxies in Seidel et al. (2015) and was considered as a hint towards the existence of inner discs or rings in barred galaxies.

The stellar velocity dispersion profiles demonstrate a different behaviour for NGC 5347 and UGC 1344. For NGC 5347, they show central minima for all spectral slices. Similar minima were found previously for many barred galaxies (see e.g. Bettoni & Galletta 1997). The presence of the minimum of the stellar velocity dispersion can give evidence in favour of the inner disc. At the same time, for UGC 1344, we observe a peak of the velocity dispersion and the flattening of the decrease for both sides from the centre. Evidently, this galaxy possesses more concentrated and massive stellar bulge.

We did not find any significant changes of the velocity and velocity dispersion in the regions of the ends of the bars.

In fifth and sixth panels from the top of Figs 5 and 6, we show the radial profiles of Gauss-Hermite moments $h_3$ and $h_4$ of stars for NGC 5347 and UGC 1344. These parameters characterize the deviation of LOSVD from the Gaussian profile. The value of $h_3$ is related to the skewness of the LOSVD, while $h_4$ is a measure of the kurtosis. As one can see from the profiles, both $h_3$ and $h_4$ moments differ from 0 in the central parts of the galaxies. The values of $h_3$ and $h_4$ are lower for NGC 5347 than that in UGC 1344. It could be because the stellar velocity dispersion of NGC 5347 is also significantly lower than that in UGC 1344 and is compatible with the resolution. The important diagnostic feature is that $h_3$ anticorrelates with the LOS velocity for both galaxies in the centre. It could also provide evidence in favour of inner discs or rings (see e.g. Seidel et al. 2015).

## 2.4 The properties of stellar population

Two bottom panels of Figs 5 and 6 demonstrate the radial profiles of luminosity-weighted age and metallicity of stellar population for NGC 5347 and UGC 1344, correspondingly. The age profile in NGC 5347 reveals a depression of stellar age in the centre, presenting at all spectral slices. The age of the nuclear component of NGC 5347 is close to that of the main disc, while the bar is relatively old. This finding is in good agreement with the conclusion made for several barred galaxies by Seidel et al. (2016), evidencing the low or absent star formations in bars of early-type discy galaxies and more extended star formation history in the very inner region. In contrast, UGC 1344 does not demonstrate the central decrease of age, instead, it has a flat inner part: Stellar population is old there all over the central region.

In both cases, the ages of stellar population in bars are relatively old, i.e. 5–10 Gyr, confirming that a bar is long-lived structure in good agreement with the previous studies (see e.g. Shen & Sellwood 2004; Gadotti & de Souza 2006; Pérez, Sánchez-Blázquez & Zurita 2007). We also observe the flattening of the stellar metallicity gradient in the regions of bars where the velocity gradient changes – the effect possibly caused by the stellar radial migration. Seidel et al. (2016) also found the metallicity flattening, however, only for bar major axis.

Interestingly, while the metallicity profiles of UGC 1344 and NGC 5347 show similar nearly solar metallicities in the centres, the situation is different at the outskirts of galaxies: The stellar metallicity profiles of NGC 5347 demonstrate a decrease in the outer radii especially for PA = 103° not presented in UGC 1344. Note that the B-V and V-R azimuthally averaged radial profiles do not show a sharp decrease in the outer region of NGC 5347 (see Saburova et al. 2011). It could indicate that the colour indices reflect a current rate of star formation, not the stellar underabundance.
<figure><img src="image_7.png" /><figcaption>**Figure 5.** From the left- to right-hand side: the radial profiles of the properties of stars and ionized gas of NGC 5347 obtained for PA = 103°, 120° and 30°. The top panels show the reference composite *g*,*r*,*i* images from SDSS. Next panels correspond to the radial profiles of the total flux (black line) and flux in H β [green (light-grey in printed version) dots] and [O iii] [blue (dark-grey in printed version) dots] lines. Two panels below demonstrate the profiles of the LOS velocities and velocity dispersions. Black and coloured symbols correspond to stars and ionized gas, respectively. Zero-point for the velocity is 2410 km s⁻¹. Vertical dotted lines mark the positions of the centre of the galaxy and radial distances of the noticeable fractures of profiles of LOS velocity. Next two panels give the radial profiles of Gauss–Hermite moments *h*₃ and *h*₄ of stars. The bottom two panels correspond to the radial distributions of age and metallicity of stars.</figcaption></figure>
<figure><img src="image_8.png" /><figcaption>**Figure 6.** From the left- to right-hand side: the radial profiles of properties of stars and ionized gas of UGC 1344 obtained for PA = 45° and 82°. The top panel shows the reference images from SCORPIO. Next panels correspond to the radial profiles of the total flux (black line) and flux in H β [green (light-grey in printed version) dots] and [O III] [blue (dark-grey in printed version) dots] lines. Two panels below demonstrate the profiles of the LOS velocities and velocity dispersions. Black and coloured symbols correspond to stars and ionized gas, respectively. Zero-point for the velocity is 4390 km s⁻¹. Vertical dotted lines mark the positions of the centre of the galaxy and radial distances of the noticeable fractures of profiles of LOS velocity. The insertion in the velocity profile for PA=82° shows the zoomed-in velocity profile for the companion 2MASX J01522797+3629533. Next two panels give the radial profiles of Gauss-Hermite moments *h*₃ and *h*₄ of stars. The bottom two panels correspond to the radial distributions of age and metallicity of stars.</figcaption></figure>
# 3 DISCUSSION

## 3.1 On the M/L

As we noted in Section 1, the considered galaxies were chosen as the candidates of systems with low M/L of stellar population. The new kinematic data allowed us to verify this peculiarity.

### 3.1.1 UGC 1344

For UGC 1344, all previously available estimates of the rotation velocity were based on the measurements of the H I linewidth. Different sources give the following values corrected for the same inclination taken from the Hyperleda data base (see Table 1): $v = 40$ km s$^{-1}$ (Hyperleda); $v = 56$ km s$^{-1}$ (RC3; de Vaucouleurs et al. 1991); $v = 59$ km s$^{-1}$ (Wilkerson 1980). All these estimates correspond to low dynamical M/L within the optical radius: $M/L_B < 0.34$, which is more than six times lower than expected from the observed red colour ($B-V)_0$ and stellar model relations for a scaled Salpeter IMF (Bell & de Jong 2001). From the radial profiles of velocity obtained in this article for UGC 1344 (see Fig. 6), it follows that the rotational velocity amplitude corrected for inclination is at least three times higher than that determined from H I linewidth: $v = 196$ km s$^{-1}$. It corresponds to the dynamical $M/L_B = 3.75$, which is quite normal for spiral galaxies containing a comparable fraction of light and dark matter within the optical borders.

One of the possible explanations of the differences in the rotation velocity estimates could be a confusion of UGC 1344 with the small companion seen at the distance of about 1.4 arcmin from UGC 1344 with the systemic velocity of 4490 km s$^{-1}$ (the full width at half-maximum of the beam is ~3.2 arcmin in Wilkerson 1980). This companion was crossed by the slit with PA = 82°. In Fig. 6, we also demonstrate its radial profiles of LOS stellar velocity and velocity dispersion. From this figure, one can see that the slit is not oriented along the major axis of the companion. From the image of this galaxy, it follows that the angle between the slit and major axis is $\phi \approx 45^\circ$ and inclination of the companion is $i \approx 70^\circ$. Assuming these values, one can calculate roughly the rotational velocity amplitude of this galaxy

$$v(R) = \frac{v_r(R)\sqrt{(\sec^2(i) - \tan^2(i)\cos^2(\phi))}}{\sin(i)\cos(\phi)}, \quad (1)$$

where $v_r \approx 10$ km s$^{-1}$ is the total range of LOS velocity of this galaxy corrected for the systemic velocity and divided by 2. Then, the rough estimate of the rotation velocity of the companion is $v \approx 44$ km s$^{-1}$,<fnref n="2" /> which is close to that found from H I linewidth. However, this explanation looks not too realistic since the companion does not seem to be a gas-rich galaxy (we do not see bright emission lines in its spectrum).

Another possible explanation of the difference between the obtained velocity of UGC 1344 and that based on H I linewidth is the concentration of the neutral hydrogen in the inner part of the galaxy where the rotational amplitude is low, so the gas traces only the central part of the rotational curve. However, H I data with good resolution and sensitivity are needed to verify this hypothesis.

### 3.1.2 NGC 5347

For NGC 5347, the situation is different. This galaxy is more studied in comparison to UGC 1344. The rotational amplitudes were available both from long-slit optical observations (Márquez et al. 2004): $v/\sin(i) = 56$ km s$^{-1}$, H I observations (Noordermeer et al. 2005): $v/\sin(i) \approx 77$ km s$^{-1}$ (though with low resolution) and H I linewidth measurements: $v/\sin(i) = 61$ km s$^{-1}$ (RC3; de Vaucouleurs et al. 1991). Here, we used the inclination taken from Hyperleda, which is close to the value found in Saburova et al. (2011) for $R = 20$ arcsec. The ionized gas rotational amplitude measurements of Márquez et al. (2004) are in satisfactorily agreement with this paper, although we failed to detect counter rotation of ionized gas found in central 5 arcsec by Márquez et al. (2004) for PA = 40° and 130°. However, our ionized gas data are uncertain in the inner part of the velocity profile due to the presence of AGNs that we did not take into account in the analysis. By the same reason, we give preferences to stellar velocities. However, as far as the rotational amplitude is rather low, the asymmetric drift correction may be very critical for this system. We calculated a rough correction of stellar rotation velocity for asymmetric drift in the epicyclic approximation for an exponential stellar disc using the following equation based on Binney & Tremaine (2008):

$$v_c^2 = v_r^2 + \sigma_r^2 \left( 0.5 \frac{d \ln(v_r)}{d \ln(R)} - 0.5 + \frac{R}{r_d} - \frac{d \ln(\sigma_r^2)}{d \ln(R)} \right), \quad (2)$$

where $v_c$ is the circular velocity, $v_r$ is the observed rotation velocity of stars, $\sigma_r$ is radial velocity dispersion of stars and $r_d$ is the exponential scale-length of disc taken from Saburova et al. (2011). We estimated radial velocity dispersion from the observed LOS stellar velocity dispersion $\sigma_{obs}$ at PA = 103°, taking into account the expected links between the dispersion along the radial, azimuthal and vertical directions:

$$\sigma_{\text{obs}}^2(R) = \sigma_z^2 \cos^2(i) + \sigma_\phi^2 \sin^2(i) \cos^2(\alpha) + \sigma_r \sin^2(i) \sin^2(\alpha), \quad (3)$$

where $\alpha$ is the angle between the slit and the major axis and $\sigma_z$, $\sigma_\phi$ and $\sigma_r$ are the dispersions along the vertical, azimuthal and radial directions, projected upon the plane of the galaxy, respectively.

To solve equation (3), we used two additional conditions: $\sigma_r = 2\Omega\sigma_\phi/\kappa$ (Lindblad formula for the epicyclic approximation), where $\kappa$ is the epicyclic frequency: $\kappa(R) = \frac{2v(R)}{R} \sqrt{\frac{1}{2} + \frac{R}{2v(R)} \frac{\partial v(R)}{\partial R}}$ and $\sigma_r = k\sigma_\phi$. The coefficient $k$ was taken to be 0.6 in accordance with direct measurements of other galaxies, which show that it could lie in the range 0.5–0.8 (see e.g. Shapiro, Gerssen & van der Marel 2003).

The asymmetric drift correction may increase the velocity by roughly a factor of 2. The corrected value of the maximal velocity is $v_c \approx 100$ km s$^{-1}$, which is higher than the rotational amplitude related to the disc (Saburova et al. 2011) and corresponds to a quite normal dynamical $M/L_R = 2.3$, which is higher than that expected from the observed colour index for a scaled Salpeter IMF for the disc: $(M/L_R)_d = 1.3$ and for the galaxy as a whole: $(M/L_R)_{tot} = 1.79$ evidently due to the presence of dark halo. Thus, our new kinematical data do not confirm the unusually low M/L and hence the peculiar stellar IMF of this galaxy.

Of course, for both galaxies, the dynamical mass estimates depend on the adopted inclination angle. However, both galaxies have moderate inclinations (they are not seen close to face-on), and the expected uncertainties of the inclination are significantly lower than

<footnote n="2">² The asymmetric drift correction will increase this value, but much less than by three times.</footnote>
the difference between the new and old measurements of the circular velocity.

## 3.2 On the central components: a comparison with the N-body models

Despite the fact that we did not confirm the peculiarity of stellar population in the considered galaxies, they are certainly worth studying. These galaxies possess some remarkable features in both kinematical profiles and the profiles of the properties of stellar population. For both galaxies, we obtained the so-called double-humped rotation curves – the rise of the velocity is followed by the local decrease or flat spot after which the increase continues. The profiles of $h_3$ moment related to the skewness of the LOSVD are not equal to zero and anticorrelate with the LOS velocity in the central part for both galaxies. These two factors can be regarded as indication of the presence of an inner disc or ring (Seidel et al. 2015). For NGC 5347, the additional confirmation of the presence of central component could come from the prominent double-armed nuclear spiral structure found by Martini et al. (2003) based on the HST H- and V-band images. However, this structure could also be related to the motions of gas due to the bar.

In order to figure out what kind of structural details could be responsible for the observed features on the kinematical profiles, we compared the results of N-body simulations of barred galaxies to our galaxies. Numerous and significant efforts were previously done in this field (see e.g. Combes & Sanders 1981; Debbastita & Sellwood 2000; Athanassoula 2003; Wozniak et al. 2003; Bureau & Athanassoula 2005; Minchev & Famaey 2010).

Our simulations were performed with a Tree N-body code (Khoperskov et al. 2014). We set up a disc galaxy that consists of a live dark matter halo, stellar bulge and pure stellar disc. The model disc has an exponential surface density profile with total mass $3.8 \times 10^{10} M_{\odot}$ and scale-length $r_d = 2.5$ kpc. The vertical profile is Gaussian with a scaleheight $z_d = 0.3$ kpc. The dark matter halo density profile follows that of pseudo-isothermal sphere with mass $8.6 \times 10^{10} M_{\odot}$ and scale-length 2 kpc. Initially, the halo is non-rotating. We adopted bulge as a Plummer sphere with mass $6 \times 10^9 M_{\odot}$ and size of 1 kpc. For the experiment described below, we generate a model containing $10^6$ disc particles, $10^6$ halo particles and $2 \times 10^4$ particles for the stellar bulge. The initial rotation curve and contributions of separate components together with the equilibrium radial velocity dispersion of stellar disc $\sigma_r$ are shown

in Fig. 7 (left-hand panel). The opening angle of TreeCode is taken to be 0.5 and softening radius is 50 pc.

The simulated galaxy evolved for 5 Gyr. We describe the bar strength as $m = 2$ Fourier moment $A_2$. Fig. 7 (right-hand panel) shows that the bar strength grows since the beginning of simulation and reaches a saturation level at about 2 Gyr. Time-dependent evolution of face-on stellar density is given in Fig. 8. Eventually, the disc develops a strong bar with the size $\approx 5-7$ kpc. We address our analysis of the LOSVD to the time $T = 2$ Gyr.

We compared the model profiles of velocity, velocity dispersion, $h_3$ and $h_4$ moments with the observed ones. For this purpose, we created two different types of models: In the first one, a bar is oriented along the major kinematical axis; and in the second one, it is inclined at the angle of 40° to the major axis (in the plain of a galaxy). In Figs 9 and 10, we show the maps of the surface density, stellar velocity, velocity dispersion and $h_3, h_4$ moments for the models with bar inclined to the major axis and aligned with it, respectively. The linear and velocity resolutions of the models are 500 pc and 20 km s⁻¹.

For the convenience of comparison with the observed data, we performed slices of model maps of velocity, velocity dispersion and $h_3, h_4$ along the major (dashed lines) and minor axes (solid lines) (see the right-hand columns of Figs 9 and 10 for two types of bar orientation).

### 3.2.1 UGC 1344

As one can see from Fig. 9, the slices for the model with the bar inclined to the major axis show excellent agreement with that obtained for UGC 1344. The LOS velocity profile shows similar changes of gradient. The model $h_3$ radial profile anticorrelates with that of the velocity in the centre as the observed one. It is worth noting, however, that the observed behaviour of $h_3$ profile is more complex in the innermost region than in the model. It could be due to the absence of massive boxy bulge in our model (see the face-on and edge-on view of the density contours of the model at 2 Gyr in the top and bottom panels of Fig. 11, respectively). The stellar velocity dispersion profile shows the flattening at large radial distance that resembles the observed one, being, however, more prominent. It is worth noting that the double-humped rotation curve and a shoulder in the velocity dispersion profile were also reproduced in previous papers on N-body simulations of barred galaxies (see e.g. Bureau & Athanassoula 2005).

<figure><img src="image_9.png" /><figcaption>**Figure 7.** Left-hand panel: rotation curve decomposition of simulated galaxy as well as the radial velocity dispersion of the stellar disc $\sigma_r$ at the beginning of simulation. Right-hand panel: strength of the bar in terms of $A_2$ as a function of time.</figcaption></figure>
<figure><img src="image_10.png" /><figcaption>Figure 8. Formation and evolution of bar in the simulated galaxy.</figcaption></figure>

Our model $h_4$ map looks not very similar to observations (see Figs 9j and 6) – the observed profile does not possess such a remarkable central minimum as it is seen in the model. However, the overall model behaviour resembles that of UGC 1344, where the major kinematical axis is inclined with respect to the bar, as it is apparent from the kinematical profiles. We conclude that the observed kinematical features of UGC 1344, including the anticorrelation of $h_3$ and the velocity in the central region, can be explained by the presence of the bar inclined with respect to the major axis without introducing additional nuclear ring or disc, which is in a good agreement with the conclusions done in Section 2.2. We suspect that the inner structure represents the peanut-shaped bulge, which is a result of the vertical buckling instability of the bar during the secular evolution phase that has been suggested by a number of N-body simulations (Combes et al. 1990; Raha et al. 1991; Martinez-Valpuesta, Shlosman & Heller 2006). This conclusion follows from the stellar properties of the inner structure not differing from the surrounding bar, its relatively high velocity dispersion and from the fact that kinematical features of UGC 1344 are in good agreement with that obtained for boxy or peanut-shaped bulges by Chung & Bureau (2004), concerning the shape of the velocity profile and the inner anticorrelation of $h_3$ and the LOS velocity.

### 3.2.2 NGC 5347

The situation with NGC 5347 is quite different. One should note that even though the two considered galaxies have many common features (similar kinematical behaviour, the presence of a bar and a ring, the red colour of stellar population, etc.), there are some differences that could indicate the dissimilarity of formation history of these systems. First, NGC 5347, unlike UGC 1344, demonstrates the central minimum of the stellar velocity dispersion. Secondly, the age of the central component of NGC 5347 is significantly younger than that of the bar and bulge, while for UGC 1344, the central part consists of old stars. The activity of star formation throughout the entire discs of two galaxies is also different. Based on FUV images

from the GALEX All-Sky Imaging Survey, we found out that UGC 1344 is bright in FUV only in the central region with a radius of ~5 arcsec, while the disc and the ring are almost invisible in FUV. At the same time, NGC 5347 has an FUV-bright ring, indicating active star formation in the disc.

As one can see from the kinematical profiles of NGC 5347, the bar is most likely oriented along the major axis, in contrast to UGC 1344. A comparison with the model with the same bar orientation (see Fig. 10) does not show a good concordance. The model velocity profile demonstrates the change of the gradient in agreement with observations, although it is not so sharp as observed. The $h_3$ profile for the model does not demonstrate the anticorrelation with the velocity in the central part, instead, the model $h_3$ profile shows a slight positive trend with LOS velocity, although the values of $h_3$ are close to zero. The difference in the behaviour of model $h_3$ horizontal cuts for the bar aligned along the major axis of the disc and inclined to it can be explained as follows. The horizontal cut for the model with the bar inclined to the major axis crosses the bar region in central ±2 kpc, where one can see the dramatic change of $h_3$, which anticorrelates with LOS velocity, since the bar rotates slower than the part of stars of the disc with circular orbits. The contribution of the bar to the surface brightness is very high in this region, so this detail is very prominent on the profile. For the model with the bar elongated along the major axis of the disc, the cut is oriented along the bar, so the stars belonging to the bar make the major contribution to the luminosity and thus to the line profiles. Some fraction of stars does not belong to the bar and thus rotate faster, which seeks to provide a positive trend of $h_3$ with the LOS velocity along the cut. However, this component is faint in comparison to the bar, which results in much less dramatic changes in the $h_3$ profile. The model velocity dispersion profile also does not have such prominent central minimum as we found for NGC 5347. Thus, our simple barred model cannot reproduce the kinematical features of NGC 5347. We compared our profiles for this galaxy with the results of high-resolution simulation of a galaxy forming out of gas that cools and settles into a disc, considered by Cole et al.
<figure><img src="image_11.png" /><figcaption>**Figure 9.** Left-hand column, from the top to bottom, represents two-dimensional maps of the stellar density, LOS velocity, LOS velocity dispersion, $h_3$ and $h_4$ of model barred galaxy, respectively. The white dashed and solid lines correspond to the slit positions used to extract one-dimensional data. Bar is inclined relative to the major axis on angle 40°. Maps have been created for 500 pc spatial resolution and 20 km s⁻¹ resolution for the LOS velocity distribution in each spatial pixel. We adopted 30° inclination for the simulated galaxy. In the left-hand column, we show one-dimensional data along the slits shown in the right-hand side. Dashed line profiles correspond to the horizontal slit (also dashed in the left-hand side). Profiles along the vertical slit are shown by solid lines.</figcaption></figure>
<figure><img src="image_12.png" /><figcaption>**Figure 10.** Same as in Fig. 9, but for the bar orientated along the major axis.</figcaption></figure>

(2014). They studied a model galaxy with a nuclear disc formed by gas that was driven by bar to the centre. According to their model maps, there is a minimum of the stellar age and velocity dispersion in the centre and a slight peak of $h_4$ that postulates the

presence of a kinematically cold stellar population. Similar drop of the stellar velocity dispersion was also reproduced in Wozniak et al. (2003), where the young population dominates the observed LOS kinematics of the circumnuclear regions. A number of numerical
<figure><img src="image_13.png" /><figcaption>**Figure 11.** The face-on (top panel) and edge-on (bottom panel) view of the density contour map of the simulated barred galaxy at 2 Gyr.</figcaption></figure>

simulations suggest that bars induce torques that force the gas to shock, subsequently losing angular momentum and funnelling to the centre (Athanassoula 1992; Regan & Teuben 2004; Kim, Seo & Kim 2012). Such gas inflow is stabilized by inner Lindblad resonance creating a star-forming nuclear disc (Sheth et al. 2005; Ellison et al. 2011). There is also observational evidence that the presence of bar and bar-driven inflow leads to rejuvenation of stellar population in the nuclear region (Moorthy & Holtzman 2006; Coelho & Gadotti 2011; Pérez & Sánchez-Blázquez 2011; Sil’Chenko & Chilingarian 2011; Lin et al. 2017). This picture agrees with our findings for NGC 5347 and indicates the presence of a kinematically cold nuclear disc formed through the bar-driven inflow and the following star formation.

## 4 CONCLUSIONS

The first result of this work is the disproof of the previously suspected peculiarly low stellar *M/L* of NGC 5347 and UGC 1344, adding evidence in favour of the universality of the IMF in discy galaxies. In both galaxies, the rotational velocities obtained from the linewidth of H I and presented in Hyperleda appear to be strongly underestimated. We found the following new estimates of *M/L* within the optical radii: for UGC 1344, *M/L*<sub>B</sub> = 3.75 (*M/L*<sub>B</sub> < 0.34 according to H I linewidth measurements); for NGC 5347, *M/L*<sub>R</sub> = 2.3 (*M/L*<sub>R</sub> = 0.65 according to previous velocity measurements). However, our long-slit spectral observations reveal some curious features in their kinematical profiles that we tried to reproduce in our *N*-body simulations of barred galaxies. Both galaxies have double-humped rotation curves within several kpc from the centres and the central components, probably connected with the presence of a bar.

These two galaxies look quite similar at the first sight: Both are early-type discy galaxies possessing a bar and inner ring. However, NGC 5347 has a younger stellar population and lower luminosity in comparison to UGC 1344. FUV images reveal that star formation is active throughout the disc of NGC 5347 while UGC 1344 is noticeable in FUV only in the central region. The presence of bars evidently has played a significant role in the evolutions of central parts of both galaxies, but in a different way. In UGC 1344, the bar led to the formation of inner component with high velocity dispersion and low rotation velocity but with the age and metallicity close to that of the bar. This central component most probably is a peanut-shaped bulge. In NGC 5347, the bar induced the formation of the other type of structure – a kinematically cold nuclear disc. Its presence is evident from the central minima on the stellar velocity dispersion and the stellar age profiles and the anti-correlation between *h*<sub>3</sub> moment and velocity that are not reproduced by our *N*-body model with similar orientation of the bar, but agrees with the simulation of a galaxy with nuclear disc of Cole et al. (2014).

We found that stellar abundances in the central parts of the galaxies have similar nearly solar values in spite of their different luminosities. Both galaxies demonstrate the flattening of the stellar metallicity gradient in the bar regions, although their radial profiles of abundance and mean stellar age are very different, evidencing a different history of star formation in these barred galaxies.

## ACKNOWLEDGEMENTS

This paper is based on observations obtained with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS). We thank the anonymous referee for helpful comments. Authors thank Daniela Bettoni for useful discussion and comments. The Russian Science Foundation (RSCF) grant No. 14-22-00041 supported the study of stellar and ionized gas kinematics. Authors are also grateful to the Russian foundation for basic research grants 15-52-15050, 16-02-00649 and 16-32-60043 for support. The project used computational resources at the Research Computing Center funded by the M.V. Lomonosov Moscow State University Programme of Development. The Russian 6-m telescope is exploited under the financial support by the Russian Federation Ministry of Education and Science (agreement No. 14.619.21.0004, project ID RFMEFI61914X0004). This work has been supported by the ANR (Agence Na- tionale de la Recherche) through the MOD4Gaia project (ANR-15-CE31-0007, P.I.: P. Di Matteo). This research has made use of the Lyon Extragalactic Database (LEDA, http://leda.univ-lyon1.fr). In this study, we used the SDSS DR13 data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/.

## REFERENCES

* Afanasiev V. L., Moiseev A. V., 2005, Astron. Lett., 31, 194

* Athanassoula E., 1992, MNRAS, 259, 345

* Athanassoula E., 2003, MNRAS, 341, 1179

* Bastian N., Covey K. R., Meyer M. R., 2010, ARA&A, 48, 339

* Bell E. F., de Jong R. S., 2001, ApJ, 550, 212

* Bettoni D., Galletta G., 1997, A&AS, 124
Binney J., Tremaine S., 2008, Galactic Dynamics, 2nd edn. Princeton Univ. Press, Princeton, NJ

Bureau M., Athanassoula E., 2005, ApJ, 626, 159

Chilingarian I., Prugniel P., Sil'Chenko O., Koleva M., 2007a, in Vazdekis A., Peletier R., eds, Proc. IAU Symp. 241, Stellar Populations as Building Blocks of Galaxies. Kluwer, Dordrecht, p. 175

Chilingarian I. V., Prugniel P., Sil'Chenko O. K., Afanasiev V. L., 2007b, MNRAS, 376, 1033

Chung A., Bureau M., 2004, AJ, 127, 3192

Coelho P., Gadotti D. A., 2011, ApJ, 743, L13

Cole D. R., Debattista V. P., Erwin P., Earp S. W. F., Roškar R., 2014, MNRAS, 445, 3352

Combes F., Sanders R. H., 1981, A&A, 96, 164

Combes F., Debbasch F., Friedli D., Pfenniger D., 1990, A&A, 233, 82

Comerón S., 2013, A&A, 555, L4

Davis T. A., McDermid R. M., 2016, MNRAS,

de Vaucouleurs G., de Vaucouleurs A., Corwin H. G. Jr, Buta R. J., Paturel G., Fouqué P., 1991, Third Reference Catalogue of Bright Galaxies. Volume I: Explanations and References. Volume II: Data for Galaxies between 0$^h$ and 12$^h$. Volume III: Data for Galaxies between 12$^h$ and 24$^h$.

Debattista V. P., Sellwood J. A., 2000, ApJ, 543, 704

Ellison S. L., Nair P., Patton D. R., Scudder J. M., Mendel J. T., Simard L., 2011, MNRAS, 416, 2182

Gadotti D. A., de Souza R. E., 2006, ApJS, 163, 270

Garcia A. M., 1993, A&AS, 100, 47

García-Barreto J. A., Carrillo R., Vera-Villamizar N., 2003, AJ, 126, 1707

Gilmore G., 2001, in Tacconi L., Lutz D., eds, Starburst Galaxies: Near and Far. Springer-Verlag, Berlin, p. 34

Izumi T., Kawakatu N., Kohno K., 2016, ApJ, 827, 81

Katkov I. Y., Sil'chenko O. K., Afanasiev V. L., 2013, ApJ, 769, 105

Katkov I. Y., Sil'chenko O. K., Chilingarian I. V., Uklein R. I., Egorov O. V., 2016, MNRAS, 461, 2068

Khoperskov S. A., Vasiliev E. O., Khoperskov A. V., Lubimov V. N., 2014, J. Phys. Conf. Ser., 510, 012011

Kim W.-T., Seo W.-Y., Kim Y., 2012, ApJ, 758, 14

Kroupa P., 2001, MNRAS, 322, 231

Kroupa P., 2002, Science, 295, 82

Le Borgne D., Rocca-Volmerange B., Prugniel P., Lançon A., Fioc M., Soubiran C., 2004, A&A, 425, 881

Lin L., Li C., He Y., Xiao T., Wang E., 2017, ApJ, 838, 105

Makarov D., Prugniel P., Terekhova N., Courtois H., Vauglin I., 2014, A&A, 570, A13

Márquez I. et al., 2004, A&A, 416, 475

Martinez-Valpuesta I., Shlosman I., Heller C., 2006, ApJ, 637, 214

Martini P., Regan M. W., Mulchaey J. S., Pogge R. W., 2003, ApJS, 146, 353

Minchev I., Famaey B., 2010, ApJ, 722, 112

Moorthy B. K., Holtzman J. A., 2006, MNRAS, 371, 583

Noordermeer E., van der Hulst J. M., Sancisi R., Swaters R. A., van Albada T. S., 2005, A&A, 442, 137

Pérez I., Sánchez-Blázquez P., 2011, A&A, 529, A64

Pérez I., Sánchez-Blázquez P., Zurita A., 2007, A&A, 465, L9

Peterson C. J., Huntley J. M., 1980, ApJ, 242, 913

Raha N., Sellwood J. A., James R. A., Kahn F. D., 1991, Nature, 352, 411

Regan M. W., Teuben P. J., 2004, ApJ, 600, 595

Saburova A. S., Shaldenkova E. S., Zasov A. V., 2009, Astron. Rep., 53, 801

Saburova A. S., Bizyaev D. V., Zasov A. V., 2011, Astron. Lett., 37, 751

Saburova A. S., Józsa G. I. G., Zasov A. V., Bizyaev D. V., 2013, A&A, 554, A128

Saburova A., Zasov A., Uklein R., Katkov I., 2015, MNRAS, 453, 1344

Salpeter E. E., 1955, ApJ, 121, 161

Seidel M. K., Falcón-Barroso J., Martínez-Valpuesta I., Díaz-García S., Laurikainen E., Salo H., Knapen J. H., 2015, MNRAS, 451, 936

Seidel M. K., Falcón-Barroso J., Martínez-Valpuesta I., Sánchez-Blázquez P., Pérez I., Peletier R., Vazdekis A., 2016, MNRAS, 460, 3784

Shapiro K. L., Gerssen J., van der Marel R. P., 2003, AJ, 126, 2707

Shen J., Sellwood J. A., 2004, ApJ, 604, 614

Sheth K., Vogel S. N., Regan M. W., Thornley M. D., Teuben P. J., 2005, ApJ, 632, 217

Sil'Chenko O. K., Chilingarian I. V., 2011, Astron. Lett., 37, 1

Tully R. B., 1987, ApJ, 321, 280

van der Marel R. P., Franx M., 1993, ApJ, 407, 525

Wilkerson M. S., 1980, ApJ, 240, L115

Wozniak H., Combes F., Emsellem E., Friedli D., 2003, A&A, 409, 469

This paper has been typeset from a *TEX/LATEX* file prepared by the author.