Structure and dynamics of giant low surface brightness galaxies

F. Lelli; F. Fraternali; R. Sancisi

doi:10.1051/0004-6361/200913808

Free Access

Issue		A&A Volume 516, June-July 2010


Article Number		A11
Number of page(s)		11
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/200913808
Published online		16 June 2010

A&A 516, A11 (2010)

Structure and dynamics of giant low surface brightness galaxies

F. Lelli^1,3 - F. Fraternali¹ - R. Sancisi^2,3

1 - Department of Astronomy, University of Bologna, via Ranzani 1, 40127 Bologna, Italy
2 - INAF - Astronomical Observatory of Bologna, via Ranzani 1, 40127 Bologna, Italy
3 - Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, The Netherlands

Received 4 December 2009 / Accepted 25 February 2010

Abstract
Giant low surface brightness (GLSB) galaxies are commonly thought to be massive, dark matter dominated systems. However, this conclusion is based on highly uncertain rotation curves. We present here a new study of two prototypical GLSB galaxies: Malin 1 and NGC 7589. We re-analysed existing H I observations and derived new rotation curves, which were used to investigate the distributions of luminous and dark matter in these galaxies.

In contrast to previous findings, the rotation curves of both galaxies show a steep rise in the central parts, typical of high surface brightness (HSB) systems. Mass decompositions with a dark matter halo show that baryons may dominate the dynamics of the inner regions. Indeed, a ``maximum disk'' fit gives stellar mass-to-light ratios in the range of values typically found for HSB galaxies.

These results, together with other recent studies, suggest that GLSB galaxies are systems with a double structure: an inner HSB early-type spiral galaxy and an outer extended LSB disk.

We also tested the predictions of MOND: the rotation curve of NGC 7589 is reproduced well, whereas Malin 1 represents a challenging test for the theory.

Key words: dark matter - galaxies: structure - galaxies: kinematics and dynamics - galaxies: individual: Malin 1 - galaxies: individual: NGC 7589 - methods: data analysis

1 Introduction

Low surface brightness (LSB) galaxies span a wide range of galaxy sizes, masses and morphologies, from dwarf spheroidals and dwarf irregulars to medium-size late-type disks (Sc-Sd) and to bulge-dominated early-type spirals (Sa-Sb). According to Beijersbergen et al. (1999), LSB spirals form a LSB Hubble sequence, parallel to the classical HSB one.

Giant low surface brightness (GLSB) galaxies are usually considered as extreme cases of early-type LSB spirals (Beijersbergen et al. 1999). They have exceedingly extended LSB disks, with scale lengths ranging from $\sim$ 10 to $\sim$ 50 kpc, and central luminous components resembling the bulges of HSB spirals (e.g. Bothun et al. 1987; Sprayberry et al. 1995). They are massive systems, with $L \sim L_{*}$ . Like the ordinary LSB spirals, GLSB galaxies have low H I surface densities (Pickering et al. 1997), but they are among the most gas rich galaxies known, with $M_{\rm {{\rm H}~{\small\rm I}~}}\approx 10^{10} ~M_{\odot}$ (Matthews et al. 2001).

Few dynamical studies exist on GLSB galaxies. Pickering et al. (1997) studied four GLSB galaxies and found slowly rising rotation curves, similar to those of late-type LSB disks (e.g. Kuzio de Naray et al. 2006; de Blok & McGaugh 1997). They concluded that GLSB galaxies are ``the first examples of galaxies that are both massive and dark matter dominated''. However, they warned that their rotation curves are highly uncertain, due to the low signal-to-noise ratio and the low spatial resolution of the observations.

A slowly rising rotation curve in the presence of an inner concentration of light, as seen in those galaxies (see top panels of Fig. 7), is in marked contrast with the rule that there is a close correlation between the concentration of light and the shape of the rotation curve (Sancisi 2004 and references therein). For this reason, Sancisi & Fraternali (2007) started a re-analysis of the 21-cm data from Pickering et al. (1997). This paper concludes that preliminary work with the study of the structure and dynamics of two GLSB galaxies: Malin 1 and NGC 7589.

2 H I data analysis

We re-analysed the H I datacubes of Malin 1 and NGC 7589, obtained with the VLA by Pickering et al. (1997). The angular resolutions are low: $20\hbox{$.\!\!^{\prime\prime}$ }9 \times 20\hbox{$.\!\!^{\prime\prime}$ }8$ for Malin 1 (corresponding to $\sim$ 32 kpc for an angular-diameter distance $D_{\rm {A}} = 322$ Mpc) and $21\hbox{$.\!\!^{\prime\prime}$ }4 \times 17\hbox{$.\!\!^{\prime\prime}$ }3$ for NGC 7589 ( $\sim$ $12 \times 10$ kpc for $D_{\rm {A}}= 123$ Mpc). We used the Groningen imaging processing system (GIPSY) (van der Hulst et al. 1992). The main physical properties of both galaxies are listed in Table 1.

Total H I maps were obtained by adding the channel maps with line emission (from 24581 km s^-1 to 24 955 km s^-1 for Malin 1 and from 8566 km s^-1 to 9157 km s^-1 for NGC 7589). In order to define the areas of emission in each channel map, we used masks, which were obtained by smoothing the original datacubes to lower spatial resolutions. We inspected by eye each channel map overlaying different masks. We obtained the best results by smoothing to 40'' and 50'' and clipping at 2 $\sigma_{\rm {s}}$ and 3 $\sigma_{\rm {s}}$ for Malin 1 and NGC 7589 respectively ( $\sigma_{\rm {s}}$ is the rms noise in the smoothed cube). The resulting total H I maps are shown in Fig. 1.

Table 1: Physical properties of Malin 1 and NGC 7589.

From the masked data, we calculated the H I fluxes (correcting for primary beam attenuation). For Malin 1, we obtained $S_{\rm tot} = 2.0 \pm 0.2$ Jy km s^-1, consistent within the errors with the value derived by Pickering et al. (1997) ( $S_{\rm tot} = 2.5 \pm 0.2$ Jy km s^-1) and the single-dish measurement by Matthews et al. (2001) ( $S_{\rm {tot}}=1.80 \pm 0.50$ Jy km s^-1). For NGC 7589, we obtained $S_{\rm {tot}} = 3.8 \pm 0.3$ Jy km s^-1, whereas Pickering et al. (1997) derived $S_{\rm {tot}}=2.7 \pm 0.3$ Jy km s^-1. The differences are probably due to the different masks used; the values are consistent within 2 $\sigma$ . Single-dish observations gave intermediate values, consistent with our value within about $1\sigma$ : $S_{\rm {tot}}=2.96 \pm 0.51$ Jy km s^-1 (Matthews et al. 2001) and $S_{\rm {tot}}=3.07 \pm 0.36$ Jy km s^-1 (Springob et al. 2005) (this latter value is without the correction for H I self absorption). H I masses were estimated using the luminosity distance $D_{\rm {L}}$ , given by:

$\begin{displaymath}D_{\rm {L}} = \frac{c}{H_{0}} ~ [z + 0.5 \times (1 - q_{0}) ~ z^{2}]\cdot \end{displaymath}$

(1)

We assumed H₀=70 km s^-1 Mpc^-1, $\Omega_{\rm {m}}=0.27$ and $\Omega_{\rm {\Lambda}}=0.73 ~$ ( q₀=-0.59). Since we are dealing with low redshift galaxies, the exact value of q₀ affects our results only slightly. The redshift was calculated as $z = V_{\rm {sys}}/c$ , where $V_{\rm {sys}}$ is the galaxy systemic velocity derived from the tilted ring analysis (see Sect. 2.2). Our results are listed in Table 1.

2.1 H I velocity fields

The derivation of the velocity fields is not straightforward because of beam-smearing effects, which are particularly severe here because of the low spatial resolution. Indeed, especially in the inner regions, the 21-cm line profiles are unusually broad and asymmetric. A Gaussian fit or an intensity-weighted mean (IWM), as used by Pickering et al. (1997), give velocities far from the profile peaks and biased towards the systemic velocity. This leads to velocity fields with systematically underestimated inner velocity gradients and consequently to slowly rising rotation curves. This is illustrated by Fig. 7 of Pickering et al. (1997), which shows the rotation curves of Malin 1 and of NGC 7589 overlaid on slices of the datacubes along the major axes of the galaxies. Clearly, the inner points of the rotation curves are at lower velocities than the emission peaks, suggesting that they are underestimated. The importance of beam-smearing effects is demonstrated by the galaxy models presented in Sect. 2.4.

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{13808fg1.eps} \end{figure}$

Figure 1:

Left panels: Malin 1. Top: R-band image (Moore & Parker 2006). Middle: total H I map. Contours range from $0.9 \times 10^{20}$ to $5.4 \times 10^{20}$ atoms cm^-2 with steps of $0.45 \times 10^{20}$ atoms cm^-2. Bottom: H I velocity field. The receding side is in dark-grey. Contours range from 24 623 km s^-1 to 24 887 km s^-1 with steps of 24 km s^-1 (2 times the channel spacing). Right panels: NGC 7589. Top: R-band image (Galaz et al. 2006). Middle: total H I map. Contours range from $1.1 \times 10^{20}$ to $9.9 \times 10^{20}$ atoms cm^-2 with steps of $1.1 \times 10^{20}$ atoms cm^-2. Bottom: H I velocity field. The receding side is in dark-grey. Contours range from 8772 km s^-1 to 9080 km s^-1 with steps of 22 km s^-1 (the channel spacing).

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We have derived new velocity fields with a different technique to minimize beam-smearing effects. We selected velocities near the peaks of the emission, estimating an IWM velocity from the upper part of the line profile (above $\sim$ $75\%$ of the peak intensity) and neglecting the broad wings. This is like taking the profile peak velocities, but with the advantage of less noise in the resulting velocity field. In the outer regions of the galaxies, where the line profiles are more regular and symmetric, we used a Gaussian fit. The resulting velocity fields are shown in Fig. 1.

The left panels of Fig. 1 show the R-band image of Malin 1 from Moore & Parker (2006) (top), the total H I map (middle) and the H I velocity field (bottom). The H I distribution is approximately as extended as the optical LSB disk. The outer H I radius measures $\sim$ 64'', which corresponds to $\sim$ 100 kpc. On the southern side, a spiral arm is visible. It extends for more than 80 kpc and apparently it is the gaseous counterpart of the spiral arm detected by Moore & Parker (2006). The velocity field shows a strong variation of the position angle of the major axis with radius, both in the approaching and in the receding sides of the galaxy. Such behaviour is usually attributed to the presence of a warp. Overall, the velocity field is regular and symmetric.

Table 2: Kinematical parameters of Malin 1 and NGC 7589.

The right panels of Fig. 1 show the R-band image of NGC 7589 from Galaz et al. (2006) (top), the total H I map (middle) and the H I velocity field (bottom). The H I distribution is as extended as the optical LSB disk. The outer H I radius measures $\sim$ 80'', which corresponds to $\sim$ 48 kpc. The H I distribution follows that of the light, with two main concentrations (North-East and South-West) and two faint outer spiral arms. The velocity field is regular and symmetric.

2.2 Rotation curves

$\begin{figure} \mbox{\parbox{10cm}{\includegraphics[width=10cm,clip]{13808fg3.ep... ....5mm}\includegraphics[width=6.5cm]{13808fg5.eps}\hspace*{2.5mm}} }\end{figure}$

Figure 2:

Left panel: Position-Velocity diagram for Malin 1 along the line of nodes (LON). The white squares show the projected rotation curve. Full lines show iso-emission contours from 1 $\sigma$ to 8 $\sigma$ with steps of 1 $\sigma$ , where 1 $\sigma = 0.24$ mJy/beam. Dashed lines show contours at $-1\sigma$ and $-2\sigma$ . Top-right panel: Position angle of the major axis for Malin 1 as a function of radius. The dotted and dash-dotted lines show the fits to the tilted-ring results. Bottom-right panel: Malin 1 velocity field. Iso-velocity contours range from 24647 km s^-1 to 24887 km s^-1 with steps of 24 km s^-1 (2 times the channel spacing). The black line shows the LON.

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Kinematical parameters and rotation curves were derived by fitting a tilted-ring model to the observed velocity fields (Begeman 1987). We assumed purely circular motions and described the galaxy by a set of concentric rings. We used all the points of the velocity fields to maximize the statistics of the least-square fit. The points were weighted by $\cos^{2}(\theta)$ , where $\theta$ is the azimuthal angle in the plane of the galaxy.

As a first step, we determined the kinematical centre $(\alpha_{\rm {kin}}, \delta_{\rm {kin}})$ and the mean systemic velocity $V_{\rm {sys}}$ . Then, we kept $(\alpha_{\rm {kin}}, \delta_{\rm {kin}})$ and $V_{\rm {sys}}$ fixed and determined the position angle PA as a function of radius. Subsequently, we tried to determine the inclination angle i. Unfortunately, because of the low spatial resolutions, inclination angles and rotational velocities are strongly correlated and no independent determination of i was possible. Therefore, we kept the inclination angles constant, adopting values derived from optical observations. We used $i = 38^\circ$ for Malin 1 (Moore & Parker 2006) and $i = 58^{\circ}$ for NGC 7589 (Pickering et al. 1997). Inclinations derived from the total H I maps are consistent with those values. Finally, we determined the circular velocity $V_{\rm {c}}$ in each ring, keeping all the other parameters fixed. Our results are listed in Tables 2 and 3.

In the tilted-ring analysis of NGC 7589, we used a ring width of $20'' \sim 1$ beam. For the kinematical centre, we obtained values which are consistent within the errors with the optical ones. The values obtained for $V_{\rm {sys}}$ and PA approximately agree with those of Pickering et al. (1997).

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{13808fg2.eps} \end{figure}$	Figure 3: H I rotation curves for Malin 1 (top) and NGC 7589 (bottom), derived separately for the receding (up-triangles) and approaching (down-triangles) halves.
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For Malin 1, we used a ring width of $10'' \sim 1/2$ beam. To determine the kinematical centre, we used the points inside $40'' \sim 62$ kpc. The derived values agree within the errors with the optical ones. The value of $V_{\rm {sys}}$ agrees within the errors with that derived by Pickering et al. (1997). The PA for Malin 1 is not constant. For the inner $15'' \sim 24$ kpc we found $-1\hbox{$.\!\!^\circ$ }0 \pm 1\hbox{$.\!\!^\circ$ }6$ and for the outer radii a linear increase up to $65\hbox{$.\!\!^\circ$ }1 \pm 4\hbox{$.\!\!^\circ$ }9$ at R = 65'' (see the right panels of Fig. 2). For comparison, Pickering et al. (1997) let the PA vary from $0^{\circ} \pm 10^{\circ}$ to $34^{\circ} \pm 3^{\circ}$ . To derive the rotation curve of Malin 1, we used a ring width of $16'' \sim 2/3$ beam. In this way, the points of the rotation curve are almost independent.

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{13808fg6.eps} \end{figure}$	Figure 4: H I rotation curves for Malin 1 (left) and NGC 7589 (right). Diamonds show the rotation curves derived by Pickering et al. (1997), filled circles show our new rotation curves. The rotation curve of Malin 1 from Pickering et al. (1997) has been rescaled to $i = 38^\circ$ , adopted in our analysis. The open circle was derived only from the approaching half of Malin 1.
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Table 3: Rotation curves for Malin 1 and NGC 7589.

The errors $\sigma_{V_{\rm {c}}}$ on the circular velocities have been estimated as $\sigma_{V_{\rm {c}}}^{2} = \sigma_{\rm {fit}}^{2} + \sigma_{\rm {asym}}^{2}$ , where $\sigma_{\rm {fit}}$ is the formal error given by the fit and $\sigma_{\rm {asym}}$ is an additional uncertainty due to asymmetries between approaching and receding halves. Following Swaters (1999), we define $\sigma_{\rm {asym}} = (V_{\rm {c, app}} - V_{\rm {c, rec}})/4$ , where $V_{\rm {c, app}}$ and $V_{\rm {c, rec}}$ are respectively the approaching and receding rotation curves. Thus, we are assuming that the differences between the rotation curve from the entire velocity field and those from the approaching or receding side correspond to a deviation of $2 \sigma_{\rm {asym}}$ . Other uncertainties come from possible variations of the inclination angle. For example, for a change of i equal to 3 $^{\circ}$ , the rotation curve varies by about 14 km s^-1 for Malin 1 and 5 km s^-1 for NGC 7589.

Figure 3 compares the rotation curves derived separately for the approaching and receding sides. For NGC 7589, there is a high degree of symmetry between the two halves. For Malin 1, the symmetry is good out to $R \leq 48'' \sim 75$ kpc. At $R = 56'' \sim 87$ kpc there is a difference of $\sim$ 45 km s^-1 between the two halves, whereas the last point at $R = 72'' \sim 112$ kpc has been derived only for the approaching half. It has a large uncertainty and will be neglected.

Figure 2 shows the line of nodes of Malin 1 overlaid onto the velocity field (bottom right panel) and the corresponding position-velocity diagram extracted from the datacube (left panel). The position-velocity diagram is not completely symmetric: the approaching side is more extended than the receding one (see also Fig. 3). The projected rotation curve (white squares) closely follows the gas distribution. In particular, in contrast with Fig. 7 of Pickering et al. (1997), our first point of the rotation curve corresponds to the peak of the emission.

2.3 Comparison between the new and the old rotation curves

Figure 4 compares our new rotation curves with those derived by Pickering et al. (1997). The main difference is that our rotation curves rise more steeply and remain approximately flat out to the last measured points. As pointed out in Sect. 2.1, the slow rises of the old rotation curves are due to the strong beam smearing effects in the inner regions. In the next section, we construct 3-dimensional galaxy models based on the rotation curves from Pickering et al. (1997) and those derived here and demonstrate that the latter are the correct ones.

In the rotation curve of NGC 7589, our last two points lie below those of Pickering et al. (1997). The kinematical models described in Sect. 2.4 show that Pickering et al. (1997) over-estimated the rotation curve at large radii, but the reason is not clear.

2.4 Kinematical models

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg7.eps} \end{figure}$

Figure 5:

Position-Velocity diagrams extracted from the observations and the model datacubes. From left to right: observations; model using the steeply rising rotation curve and the other parameters derived in this work; model using the slowly rising rotation curve and the parameters derived by Pickering et al. (1997). For Malin 1 (top) we took a slice along ${\rm PA} = 35^{\circ }$ , for NGC 7589 (bottom) along ${\rm PA} = 305^{\circ }$ . Full lines show iso-emission contours from 2 $\sigma$ to 9 $\sigma$ with steps of 1 $\sigma$ . Dashed lines show contours at $-2\sigma$ . For Malin 1 (top) $\sigma = 0.24$ mJy/beam, for NGC 7589 (bottom) $\sigma = 0.35$ mJy/beam.

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In order to verify the correctness of the new rotation curves, 3-dimensional galaxy models were built. We used the GIPSY task GALMOD, that creates model datacubes by describing a galaxy disk with a set of rings. Each ring is characterized by: the kinematical parameters ( x₀, y₀), $V_{\rm {sys}}$ , PA and i, the rotation velocity $V_{\rm {c}}$ , the gas velocity dispersion $\sigma_{\rm {{\rm H}~{\small\rm I}~}}$ , the face-on gas column density $\Sigma_{\rm {{\rm H}~{\small\rm I}~}}$ and the scale-height h_z.

We created two different sets of models. The first set was built out of our new kinematical parameters and rotation curves. These are the ``steeply rising curve'' models. The second set was built out of the kinematical parameters and rotation curves derived by Pickering et al. (1997). These are the ``slowly rising curve'' models. The H I surface density profiles were derived from the total H I maps, azimuthally averaging over a set of ellipses, determined by the assumed kinematical parameters. For the H I vertical distribution, we assumed an exponential profile $\exp(-z/h_{z})$ , with h_z = 200 pc. For the gas velocity dispersion, we used $\sigma_{\rm {{\rm H}~{\small\rm I}~}} = 8$ km s^-1 over the entire disk. The models are almost indistinguishable for differences in $\sigma_{\rm {{\rm H}~{\small\rm I}~}}$ of $\pm$ 4 km s^-1. All the models were smoothed to the spatial resolution of the observations, thus they also reproduce beam-smearing effects.

In Fig. 5, we compare position-velocity diagrams from the models and the data. For NGC 7589, we took a slice through the datacubes along a position angle of $305^{\circ}$ . This is a mean value between our result of $307\hbox{$.\!\!^\circ$ }7$ and that of $302^{\circ}$ by Pickering et al. (1997). For Malin 1, we took a slice along a position angle of $35^{\circ}$ . This is a mean value for the major axis.

For both galaxies, the observed datacubes (left panels of Fig. 5) show the presence of H I emission at high rotational velocities near the galaxy centre ( $R \la 20''$ ). The ``slowly rising curve'' models (right panels) do not reproduce such emission, as the H I is spread from low rotational velocities near the centre to high rotational velocities at large radii. On the contrary, in the ``steeply rising curve'' models (middle panels) the H I emission is concentrated at high rotational velocities, as seen in the data. Both models show tails of emission toward the systemic velocity due to beam-smearing effects. Overall, the observed data are reproduced better by the ``steeply rising curve'' models based on our new results than by the ``slowly rising curve'' models based on those by Pickering et al. (1997).

We also note that the ``slowly rising curve'' model of NGC 7589 at large radii ( $R \ga 50''$ ) exhibits H I emission at rotational velocities higher than those observed. This demonstrates that the rotation curve by Pickering et al. (1997) is over-estimated in the outer regions.

3 Mass models

The steeply rising rotation curves found for Malin 1 and NGC 7589 suggest that GLSB galaxies have a dynamical behaviour more similar to a HSB than to a LSB galaxy. To determine the relative contributions of luminous (gas and stars) and dark matter to the gravitational potential, we built mass models following Begeman (1987).

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg8.eps} \end{figure}$	Figure 6: HI surface density profile for Malin 1 (left) and NGC 7589 (right), corrected for inclination and cosmological dimming.
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3.1 Gas and stars

The contribution of the gaseous disk was computed using the surface density profiles derived from the total H I maps (Fig. 6). These were multiplied by a factor (1+z)⁴ to correct for cosmological dimming and by a factor 1.4 to take into account the presence of Helium. Molecular and ionized gas were not explicitly considered in the mass model. However, since they are usually distributed as the stellar component, their contribution is reflected in a small increase of M_*/L. Consistently with the models built in Sect. 2.4, we assumed an exponential vertical distribution with a scale height of 200 pc.

To compute the contribution of the stellar component, we used surface brightness profiles from the literature. For the vertical distribution of the stellar disk, we assumed $Z(z) = {\rm sech}^{2}(z/z_{0})/z_{0}$ (van der Kruit & Searle 1981b,a), with z₀ = 300 pc.

For Malin 1, we used the I-band profile from Barth (2007) for $R \la 10$ kpc and the R-band profile from Moore & Parker (2006) for $R \ga 10$ kpc. We estimated the R - I colour of the inner galaxy regions using the SDSS data and the relations from Fukugita et al. (1996). We found r' - i' = 0.46, which corresponds to R - I = 0.70. Using this colour, the match between the two profiles is very good (see the upper-left panel of Fig. 7). As noted by Barth (2007), Malin 1 is a ``normal'' SB0/a galaxy, embedded in an extended LSB disk. This double structure is clearly shown by our combined luminosity profile. The HSB disk extends out to about 20 kpc, where a photometrically distinct LSB disk appears.

For NGC 7589, we used the R-band profile by Galaz et al. (2006) for $R \la 25$ kpc and the R-band profile by Pickering et al. (1997) for $R \ga 25$ kpc. In the inner regions, where both profiles are available, there is a systematic difference, maybe due to the different calibration of the observations. Therefore, we applied a correction of 0.2 mag to the points given by Pickering et al. (1997), by requiring that the two profiles match in the inner regions. This correction is within the 1 $\sigma$ uncertainties in the photometric measurements. The result is shown in the upper-right panel of Fig. 7. Inside $\sim$ 20 kpc, the luminosity profile is typical of a HSB galaxy with a bulge ( $R \la 5$ kpc), a lens component ( $R \sim 5$ -13 kpc) and a HSB exponential disk ( $R \sim 13{-}20$ kpc). In the outer regions, a photometrically distinct LSB disk extends out to $\sim$ 50 kpc.

3.2 Dark matter

For the dark matter distribution, we assumed pseudo-isothermal haloes described by equation:

$\begin{displaymath} \rho_{\rm {ISO}}(r) = \frac{\rho_{\rm {0}}}{1 + (r/r_{\rm {C}})^{2}}, \end{displaymath}$

(2)

where $\rho_{\rm {0}}$ is the central density and $r_{\rm {C}}$ is the core radius. $\rho_{\rm {0}}$ and $r_{\rm {C}}$ are free parameters of the mass models.

We also tried rotation curve decompositions with NFW dark matter haloes (Navarro et al. 1995) but found that the results are not significantly different.

3.3 Rotation curve decompositions

The H I rotation curves have much lower spatial resolution than the surface brightness profiles (and their resulting dynamical contributions). Thus, a least-square fit done only on the observed points of the rotation curves would neglect some features present in the luminosity profiles. To avoid this problem, we have linearly interpolated the rotation curves and performed a fit with steps of 1''. Errors on the rotation curves were used as weights in the fit.

Figure 7 shows the ``maximum disk'' decompositions of the rotation curves. The resulting mass-to-light ratios are M_*/L_R = 3.4 for Malin 1 and M_*/L_R = 2.5 for NGC 7589 (Table 4). These values are somewhat uncertain due to the lack of resolution in the central regions. However, we estimate that the mass-to-light ratio cannot be higher than 5 for Malin 1 and 3 for NGC 7589. Thus, they surely are in the range of values typically found for HSB early-type spirals (Noordermeer 2005). Under the maximum disk hypothesis, the baryons dominate the galaxy dynamics out to a radius of $R\sim 20$ kpc for Malin 1 and $R\sim 30$ kpc for NGC 7589. In contrast with the results of Pickering et al. (1997), dark matter does not necessarily dominate everywhere.

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg9.eps} \end{figure}$	Figure 7: Upper panels: R-band surface brightness profiles for Malin 1 (left) and NGC 7589 (right). See text for details. Lower panels: rotation curve decompositions for Malin 1 (left) and NGC 7589 (right). Dots show the observed rotation curves. The curves show the contributions due to gas, stars and dark matter and the resulting total rotation curve.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{13808fg10.eps} \end{figure}$

Figure 8:

Upper panels: R-band surface brightness profiles for Malin 1 (left) and NGC 7589 (right). The curves show the HSB-LSB decompositions. See text for details. Lower panels: rotation curve decompositions for Malin 1 (left) and NGC 7589 (right). Dots show the observed rotation curves. The curves show the contributions from the HSB and the LSB stellar disks, the gaseous disk, the dark matter halo and the resulting total rotation curve.

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Both Malin 1 and NGC 7589 show colour gradients, which may indicate different stellar populations. Bothun et al. (1987) studied the luminous ``blobs'' in the outer disk of Malin 1 (see Fig. 1) and found a mean B - V colour of 0.37, whereas in the inner parts ( $R \la 20''$ ) the mean B - V colour is 0.90 (Impey & Bothun 1989). Galaz et al. (2006) traced the B-R colour profile of NGC 7589 out to $R\sim 20$ kpc and found complex trends, but in general the galaxy tends to become bluer at large radii. It makes sense, therefore, to decompose the luminosity profiles and use two different M_*/L_R for the inner and the outer regions.

We separated the LSB disk by fitting an exponential profile to the points beyond $R \ga 20$ kpc. The resulting disk parameters are: $\mu_{R}(0) = 24.7$ mag arcsec^-2, h = 51.7 kpc for Malin 1 and $\mu_{R}(0) = 23.3$ mag arcsec^-2, h = 14 kpc for NGC 7589. The HSB component was isolated by subtracting the LSB disk from the total photometric profile (see top panels of Fig. 8). We maximized the contribution of the HSB component and found $M_{\rm {HSB}}/L_{R} = 3.3$ for Malin 1 and $M_{\rm {HSB}}/L_{R} = 2.6$ for NGC 7589, very similar to the previous values. Maximizing also the contribution of the LSB disk, the outer parts of the rotation curve can be reproduced without the need for a dark matter halo. However, the resulting $M_{\rm {LSB}}/L_{R}$ ratios would be unrealistically high ( $\sim$ 25 for Malin 1 and $\sim$ 15 for NGC 7589), as it is usually found by maximizing the disks of ``ordinary'' LSB galaxies (e.g. de Blok et al. 2001). Therefore, we estimated $M_{\rm {LSB}}/L_{R} = 0.9$ using the relations of Bell et al. (2003) and assuming B - V = 0.44. The latter value is the mean colour found by McGaugh & Bothun (1994) for a sample of bulgeless LSB disks. The results of the fits are listed in Table 4 and shown in the bottom panels of Fig. 8.

We also performed a standard bulge-disk decomposition for the inner HSB part and found a degeneracy of the mass-to-light ratios of bulge and disk. Different combinations of $M_{\rm {bulge}}/L_{R}$ and $M_{\rm {disk}}/L_{R}$ provide comparable fits, as the rotation curves are not resolved in the inner regions. By maximizing both bulge and disk we found that their contributions to the first point of the rotation curve are approximately equal. Therefore, in this ``maximum light'' hypothesis, the inner steep rise is not explained only with the bulge, but also the disk is dynamically important. This further suggests that Malin 1 and NGC 7589 have an inner ``normal'' HSB disk (see also Barth 2007).

Following McGaugh (2005), we used the derived values of M_*/L_R and $M_{\rm {{\rm H}~{\small\rm I}}}$ to check the position of Malin 1 and NGC 7589 on the baryonic Tully-Fisher relation. We found that both galaxies follow the relation within the observed scatter.

Table 4: Mass models for Malin 1 and NGC 7589.

3.4 MOND

The modified Newtonian dynamics (MOND) was proposed by Milgrom (1983) as an alternative to dark matter. This theory modifies the force law at accelerations a lower than a critical value a₀ and naturally explains the flatness of rotation curves (see the review by Sanders & McGaugh 2002).

GLSB galaxies are ideal systems to test MOND. Firstly, they are very diffuse and extended, thus the test is possible down to very low values of $a/a_{\rm {0}}$ (deep MONDian regime). Secondly, they have massive gaseous disks. In the MONDian framework, this gives an important contribution to the galaxy dynamics, which is not subject to uncertainties as that of stars (i.e. the value of M_*/L). For the MOND fit to the rotation curves, we followed Begeman et al. (1991) and assumed a₀ = 3000 km² s^-2 kpc^-1 (Bottema et al. 2002). Two different M/L ratios for the inner and outer regions of the galaxies have been used as free parameters in the fit.

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{13808fg11.eps}\vspace{-4mm} \end{figure}$	Figure 9: MOND applied to Malin 1 using two different M_*/L_R for the inner HSB region ( $M_{\rm {HSB}}/L_{R} = 3.7$ ) and the outer LSB disk ( $M_{\rm {LSB}}/L_{R} = 0.5$ ). Dots show the observed rotation curve. Lines show the Newtonian contributions due to the gaseous, the HSB and the LSB disk and the result of the MOND fit. See text for details.
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For NGC 7589, we obtained a good fit by using a bulge-disk decomposition. The stellar mass-to-light ratios predicted by MOND are acceptable: $M_{\rm {bulge}}/L_{R} = 4.7$ and $M_{\rm {disk}}/L_{R} = 1.3$ . For Malin 1, it is preferable to use the HSB-LSB decomposition shown in Fig. 8, but it is not possible to leave both $M_{\rm {HSB}}/L_{R}$ and $M_{\rm {LSB}}/L_{R}$ free. Indeed, the fit would require a negative value for $M_{\rm {LSB}}/L_{R}$ . This suggests that the presence of the extended LSB disk, combined with the large amount of gas, creates problems for MOND. We fixed $M_{\rm {LSB}}/L_{R}$ and used only $M_{\rm {HSB}}/L_{R}$ as a free parameter. Figure 9 shows the result for $M_{\rm {LSB}}/L_{R} = 0.5$ . Using the relations by Bell et al. (2003), this corresponds to an extremely blue colour for the outer disk, i.e. B-V = 0.2. Higher values of $M_{\rm {LSB}}/L_{R}$ worsen the fit, whereas lower values only slightly improve it, as the gas becomes dominating in the outer regions. A bulge-disk decomposition, as that used for NGC 7589, does not improve the fit. Higher values of the critical acceleration, as a₀ = 3700 km² s^-2 kpc^-1 (Begeman et al. 1991) or a₀ = 4000 km² s^-2 kpc^-1 (McGaugh 2004), worsen the fit. Interpolation functions different from the standard one, as those proposed by Famaey & Binney (2005) or Milgrom & Sanders (2008), give slightly worse fits.

Although the rotation curve of Malin 1 is not of high quality, the discrepancies between the observed velocities and the MOND prediction are significant as they are equal to $\sim$ 25 km s^-1, i.e. $\sim$ $12{-}13 \%$ . However, the warp in the outer disk of Malin 1 may greatly affect these results. The rotation curve used here was derived by varying the PA with radius (see Fig. 2) but assuming a constant inclination angle of $38^{\circ}$ . It was not possible to obtain a better determination of i from the velocity field. A change of the inclination angle in the outer parts of only $6^{\circ}$ from $i = 38^\circ$ to $i=32^{\circ}$ , which cannot be ruled out, would result in a rotation curve in total agreement with the MOND prediction. Note that here we have used the simplest formulation of MOND (Milgrom 1983), that may not strictly apply to warped non-axisymmetric disks.

4 Discussion

4.1 GLSB galaxies and their double HSB-LSB nature

It is known that there is a dichotomy between HSB and LSB systems (e.g. Verheijen & Tully 1999). HSB galaxies usually have steeply rising rotation curves and can be described by a maximum disk, whereas LSB galaxies have slowly rising rotation curves and are thought to be dominated by dark-matter everywhere. The dynamics of Malin 1 and NGC 7589 is typical of HSB systems. The concentration of mass, indicated by the steeply rising rotation curve, follows the inner concentration of light. For both galaxies, maximum-disk solutions have been found with reasonable values of M_*/L_R. Thus, we conclude that in the inner regions either baryons are dominating or, in case dark matter dominates, it must follow the distribution of light. This may be in line with some recent numerical simulations (Tissera et al. 2010), which suggest a gravitational effect of baryons on shaping the distribution of dark matter.

Both surface photometry and gas dynamics indicate that Malin 1 and NGC 7589 have a double structure: an inner ``normal'' spiral galaxy (with a bulge and an HSB disk) and an outer extended LSB disk. Is such a double structure present in the other GLSB galaxies as well? The other two GLSB galaxies studied by Pickering et al. (1997) are F568-6 (Malin 2) and UGC 6614. F568-6 is kinematically lopsided and difficult to interpret. UGC 6614 was observed in H $\alpha$ by McGaugh et al. (2001) who found a steeply rising rotation curve (see their Fig. 5) and thus a dynamical behaviour similar to that of a HSB system (see also de Blok et al. 2001). Walsh et al. (1997) studied the GLSB galaxy NGC 289 using optical and radio observations. They found an inner HSB disk and a steeply rising rotation curve that can be fitted by a maximum disk with M_*/L_I = 2.3. They drew conclusions very similar to ours. Another example is NGC 5383. This barred spiral galaxy fits in the GLSB class. It has a LSB disk with $h \sim 9.7$ kpc and a G-band absolute magnitude of M_G = -20.6 (van der Kruit & Bosma 1978). Its surface brightness profile is very similar to that of NGC 7589 and extends out to $\sim$ 54 kpc (see Barton & Thompson 1997). The HI mass is $M_{{\rm H}~{\small\rm I}} = 5.9 \times 10^{9}$ $M_{\odot}$ and the gas dynamics is typical of a HSB system (Sancisi et al. 1979).

Sprayberry et al. (1995) catalogued another 13 objects as GLSB galaxies. As argued by Barth (2007), their inner HSB disk could have been missed due to the low spatial resolution of the optical observations. However, for some of them, H I rotation curves were derived. These galaxies are NGC 5533 (Noordermeer et al. 2007), NGC 5905 (van Moorsel 1982), NGC 4017 (van Moorsel 1983), NGC 2770 (García-Ruiz et al. 2002), UGC 2936 (Pickering et al. 1999) and PGC 45080 (Das et al. 2007). All of them show a dynamical behaviour typical of HSB systems, with the possible exception of PGC 45080 that is kinematically lopsided (see Fig. 11 of Das et al. 2007). Therefore, it seems unlikely that GLSB galaxies constitute a sub-class of the bulge-dominated LSB galaxies (e.g. Beijersbergen et al. 1999, Galaz et al. 2006). It is likely, instead, that they are ``normal'' HSB galaxies which possess an outer extended LSB disk.

GLSB galaxies do show some physical properties closer to HSB than to LSB systems. Usually, LSB galaxies are quite amorphous and rarely host an AGN (Bothun et al. 1997; Impey & Bothun 1997). In contrast, GLSB galaxies can have a well-defined spiral pattern (Beijersbergen et al. 1999) and show nuclear activity with the same probability as HSB spirals (Schombert 1998). Moreover, LSB galaxies are deficient in molecular gas (e.g. O'Neil et al. 2003; Matthews et al. 2005), whereas CO emission has been detected in some GLSB galaxies (e.g. Das et al. 2006; O'Neil & Schinnerer 2004).

At this point it is natural to ask how common it is for HSB galaxies to have diffuse outer LSB stellar disks. This question has been addressed in the past (see e.g. Bosma & Freeman 1993 and references therein) and examples were found such as NGC 3642 (Verdes-Montenegro et al. 2002). More recently, Erwin et al. (2008) studied a sample of 66 S0-Sb galaxies and found that $\sim$ $24 \%$ of them show ``anti-truncated'' disks, i.e. the surface brightness profile of the disk can be described by two exponentials, the outer one with larger scalelength than the inner one. Such ``up-bending'' luminosity profiles have also been observed in late-type spiral galaxies (Pohlen & Trujillo 2006; Hunter & Elmegreen 2006). GLSB galaxies may be extreme examples of anti-truncated early-type HSB spirals. Moreover, GALEX observations have recently revealed extended XUV-disks around HSB spirals (Thilker et al. 2007). Also some GLSB galaxies have been observed with GALEX (Boissier et al. 2008) and, at such wavelengths, they resemble the XUV-disk galaxies of Thilker et al. (2007) (see in particular Malin 1, Malin 2 and NGC 7589).

Regarding gaseous disks, it is known that a large number of spiral galaxies, perhaps the majority, have H I disks extending far beyond the bright optical ones (e.g. Sancisi et al. 2008). The outlying H I has typical surface densities of 1-2 $M_{\odot}$ pc^-2, close to the values measured in GLSB galaxies. Similar results have been found also for early-type galaxies in the field. Oosterloo et al. (2007) have observed at 21-cm a sample of 30 gas rich E/S0 galaxies and discovered that about 2/3 are embedded in rotating H I disks with masses, densities and sizes comparable to the gaseous disk of Malin 1. Deep optical observations would be useful to verify whether such spirals and ellipticals have extended LSB stellar disks associated with the gaseous ones. If this is the case, these objects could be considered to be in the same class of GLSB galaxies.

4.2 The formation of GLSB galaxies

GLSB galaxies are a challenge for theories of galaxy formation. The main properties to be explained are: i) the double HSB-LSB nature; ii) the large extent of the outer LSB disks and iii) the regular and symmetric large-scale kinematics of the latter, as observed in both Malin 1 and NGC 7589 (see Fig. 3). Given the very large orbital periods at the outermost radii (e.g. $t_{\rm {dyn}} \sim 2.8$ Gyr for Malin 1 and $t_{\rm dyn} \sim 1.4$ Gyr for NGC 7589) it is clear that these outer disks must have been in place and undisturbed for several Gyrs.

CDM cosmological simulations of galaxy formation tend to produce dense and compact disks, as much angular momentum is lost during the hierarchical assemblage (see Kaufmann et al. 2007 and references therein). Hoffman et al. (1992) showed that rare density peaks ( $\sim$ 3 $\sigma$ ) in underdense environments (voids) may lead to the formation of a GLSB galaxy. However, GLSB galaxies show the same clustering properties of HSB spirals and are not necessarily associated with voids (Sprayberry et al. 1995).

Mapelli et al. (2008) simulated the evolution of a collisional ring galaxy. The propagation of the ring leads to the formation of a large and diffuse system, with structural properties similar to those of GLSB galaxies. However, these simulations predict slowly rising rotation curves and therefore a different dynamics from that of GLSB galaxies.

Noguchi (2001) proposed a secular-evolution scenario, starting from a massive barred HSB galaxy. The bar-instability can redistribute the matter and the angular momentum in the disk, but the scale length h cannot increase by more than a factor of 2-2.5 (see also Debattista et al. 2006). Therefore, this mechanism cannot explain the formation of an extended LSB disk as that of Malin 1 (with $h \sim 50$ kpc). Moreover, it should explain why the majority of barred early-type spirals do not have an outer LSB disk (Erwin et al. 2008).

Simulations by Penarrubia et al. (2006) investigated the formation of LSB disks around HSB galaxies by interactions with dwarf companions. They found that the dwarf galaxies are disrupted by tidal forces and the debris settle on an extended disk with a nearly exponential profile. Interestingly, the scale length of the resulting disk depends on the compactness of the original stellar distribution in the dwarfs and, in extreme cases, it can be as large as $\sim$ 50 kpc. Thus, it would be possible to explain a wide range of disk structural parameters as those observed in GLSB galaxies. However, such simulations predict a decrease in the rotation velocity of the outer stellar disk of about 30-50 km s^-1 with respect to the inner one. Such a decrease is not observed in the H I rotation curves of GLSB galaxies.

5 Conclusions

We studied the structural and dynamical properties of two giant low surface brightness galaxies: Malin 1 and NGC 7589. For both galaxies, we re-analysed existing 21-cm line observations, obtained with the VLA by Pickering et al. (1997), and derived new rotation curves. The quality of these curves was tested by building model datacubes. Finally, we decomposed the rotation curves using available optical surface brightness profiles and assuming pseudo-isothermal dark matter haloes. We also studied the predictions of MOND. Our main results can be summarized as follows:

1.: In contrast with the previous results by Pickering et al. (1997), both Malin 1 and NGC 7589 have steeply rising rotation curves. From a dynamical point of view, these GLSB galaxies are more similar to early-type HSB than to late-type LSB disks. This agrees with the result of the optical study by Barth (2007) that described Malin 1 as a normal SB0/a galaxy surrounded by a huge LSB disk. Both surface photometry and gas dynamics indicate that also NGC 7589 has such a double HSB-LSB structure.
2.: In these two GLSB galaxies, the concentration of mass indicated by the steeply rising rotation curve corresponds to the inner concentration of light. The rotation curves of both galaxies can be fitted by a maximum disk with $M_{*}/L_{R} \sim 3$ . Contrary to the case of the less massive LSB disks where dark matter is believed to dominate everywhere, in the inner regions of GLSB galaxies either the baryons dominate or the dark matter follows the distribution of light.
3.: Malin 1 provides a severe test for MOND because of its extraordinary size and high H I mass. The rotation curve derived here differs significantly from the one predicted by MOND. However, the discrepancies would disappear if the outer disk of Malin 1 were warped and turned to more face-on. Unfortunately, the present observations are not adequate to determine the trend of the inclination angle.

Acknowledgements

We thank Tim Pickering and his co-authors for kindly making their HI datacubes available to us. We also thank Gaspar Galaz and his co-authors for the photometric data of NGC 7589 and Lesa Moore for the optical image of Malin 1. We are grateful to Carlo Nipoti and Bob Sanders for stimulating discussions about MOND and to the referee Albert Bosma for helpful comments and suggestions.

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Footnotes

...(van der Kruit & Bosma 1978): The original values have been rescaled to a distance of 33.7 Mpc, as we assume H₀ = 70 km s^-1 Mpc^-1.

All Tables

Table 1: Physical properties of Malin 1 and NGC 7589.

Table 2: Kinematical parameters of Malin 1 and NGC 7589.

Table 3: Rotation curves for Malin 1 and NGC 7589.

Table 4: Mass models for Malin 1 and NGC 7589.

All Figures

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{13808fg1.eps} \end{figure}$	Figure 1: Left panels: Malin 1. Top: R-band image (Moore & Parker 2006). Middle: total H I map. Contours range from $0.9 \times 10^{20}$ to $5.4 \times 10^{20}$ atoms cm^-2 with steps of $0.45 \times 10^{20}$ atoms cm^-2. Bottom: H I velocity field. The receding side is in dark-grey. Contours range from 24 623 km s^-1 to 24 887 km s^-1 with steps of 24 km s^-1 (2 times the channel spacing). Right panels: NGC 7589. Top: R-band image (Galaz et al. 2006). Middle: total H I map. Contours range from $1.1 \times 10^{20}$ to $9.9 \times 10^{20}$ atoms cm^-2 with steps of $1.1 \times 10^{20}$ atoms cm^-2. Bottom: H I velocity field. The receding side is in dark-grey. Contours range from 8772 km s^-1 to 9080 km s^-1 with steps of 22 km s^-1 (the channel spacing).
Open with DEXTER
In the text

$\begin{figure} \mbox{\parbox{10cm}{\includegraphics[width=10cm,clip]{13808fg3.ep... ....5mm}\includegraphics[width=6.5cm]{13808fg5.eps}\hspace*{2.5mm}} }\end{figure}$	Figure 2: Left panel: Position-Velocity diagram for Malin 1 along the line of nodes (LON). The white squares show the projected rotation curve. Full lines show iso-emission contours from 1 $\sigma$ to 8 $\sigma$ with steps of 1 $\sigma$ , where 1 $\sigma = 0.24$ mJy/beam. Dashed lines show contours at $-1\sigma$ and $-2\sigma$ . Top-right panel: Position angle of the major axis for Malin 1 as a function of radius. The dotted and dash-dotted lines show the fits to the tilted-ring results. Bottom-right panel: Malin 1 velocity field. Iso-velocity contours range from 24647 km s^-1 to 24887 km s^-1 with steps of 24 km s^-1 (2 times the channel spacing). The black line shows the LON.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{13808fg2.eps} \end{figure}$	Figure 3: H I rotation curves for Malin 1 (top) and NGC 7589 (bottom), derived separately for the receding (up-triangles) and approaching (down-triangles) halves.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{13808fg6.eps} \end{figure}$	Figure 4: H I rotation curves for Malin 1 (left) and NGC 7589 (right). Diamonds show the rotation curves derived by Pickering et al. (1997), filled circles show our new rotation curves. The rotation curve of Malin 1 from Pickering et al. (1997) has been rescaled to $i = 38^\circ$ , adopted in our analysis. The open circle was derived only from the approaching half of Malin 1.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg7.eps} \end{figure}$	Figure 5: Position-Velocity diagrams extracted from the observations and the model datacubes. From left to right: observations; model using the steeply rising rotation curve and the other parameters derived in this work; model using the slowly rising rotation curve and the parameters derived by Pickering et al. (1997). For Malin 1 (top) we took a slice along ${\rm PA} = 35^{\circ }$ , for NGC 7589 (bottom) along ${\rm PA} = 305^{\circ }$ . Full lines show iso-emission contours from 2 $\sigma$ to 9 $\sigma$ with steps of 1 $\sigma$ . Dashed lines show contours at $-2\sigma$ . For Malin 1 (top) $\sigma = 0.24$ mJy/beam, for NGC 7589 (bottom) $\sigma = 0.35$ mJy/beam.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg8.eps} \end{figure}$	Figure 6: HI surface density profile for Malin 1 (left) and NGC 7589 (right), corrected for inclination and cosmological dimming.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{13808fg9.eps} \end{figure}$	Figure 7: Upper panels: R-band surface brightness profiles for Malin 1 (left) and NGC 7589 (right). See text for details. Lower panels: rotation curve decompositions for Malin 1 (left) and NGC 7589 (right). Dots show the observed rotation curves. The curves show the contributions due to gas, stars and dark matter and the resulting total rotation curve.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{13808fg10.eps} \end{figure}$	Figure 8: Upper panels: R-band surface brightness profiles for Malin 1 (left) and NGC 7589 (right). The curves show the HSB-LSB decompositions. See text for details. Lower panels: rotation curve decompositions for Malin 1 (left) and NGC 7589 (right). Dots show the observed rotation curves. The curves show the contributions from the HSB and the LSB stellar disks, the gaseous disk, the dark matter halo and the resulting total rotation curve.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{13808fg11.eps}\vspace{-4mm} \end{figure}$	Figure 9: MOND applied to Malin 1 using two different M_*/L_R for the inner HSB region ( $M_{\rm {HSB}}/L_{R} = 3.7$ ) and the outer LSB disk ( $M_{\rm {LSB}}/L_{R} = 0.5$ ). Dots show the observed rotation curve. Lines show the Newtonian contributions due to the gaseous, the HSB and the LSB disk and the result of the MOND fit. See text for details.
Open with DEXTER
In the text

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