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N6L0-AISTRALIAN OBSERVATORY

GAS DYNAMICS IN BARRED SPIRALS, II:

NGC 7496 AND 289

V.D. Pence and C.P. BlackMn

AAO PP 194 * Suonitted to: Mon.Not.R.astr.Soc. Distribution date: February, 1984

P.O. BOX 296. EPPING. N.S.W.. 2121 PHONE 868-1666. TELEX ASTRO 26230

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GAS DYNAMICS IN BARRED SPIRALS, II: NGC 7496 AND 289

W.D.Pence. Anglo-Australian Observatory. P.O. Box 296. Epplng. NSW. Australia. C.P.Blactanan. Department of Astronomy. Edinburgh University.

Received t

SUMMAKT - The gas velocity fields in the barred spiral galaxies NGC 7496 and 289 have been measured by means of long-slit spectra obtained with the Anglo-Australian Telescope. Pronounced deviations fro« circular motion of the type predicted by recent theoretical mooels are seen in NGC 74961 the isovelocity contours are distorted into a characteristic S-shaped pattern and there is a large velocity gradient across the bar. The velocity field is virtually identical to that of a previously observed barred spiral, NGC 5383 for which a number of models have been published. The nuclear [OUI] emission lines are very asymmetric with a wing extending to about 1000 km s-1 to the blue of the systemic velocity; this wing is only faintly seen in the Balmer lines. NGC 289 has a much smaller bar *nd consequently the noncircular motions are less pronounced. The most obvious effect is that the Xinematic major and minor axes are not perpendicular which is a signature of oval distortions. Both galaxies have a mass (within the

10 outermost velocity measurement) of 9 x iO M0 and M/Lß » 6. One significant difference between the galaxies is that the neutral hydrogen contributes about 20% of the mass of NGC 289 but only about 2% of the mass of NGC 7496. As a further test of the models of gas streaming in barred spirals we have collected the results from 11 previously studied galaxies and show that the appearance of the velocity field depends on the orientation of the bar to tne line of sight, in good agreement with the model predictions. Page 2

1 Introduction

This paper continues our study of the gas dynamics in barred spiral galaxies in which we have been looking for observational verification of recent theoretical models of the behaviour of gas in response *:o a rotating stellar bar. In the first paper (Blackman and Pence, 1981), based on spectra taken with the SAAO 19m telescope, we found little evidence of noncircular menions greater than 20 - 30 km s-1 in the barred spirals NCC 2525 and 7741. Since higher resolution seemed to be required to detect the streaming motions, we subsequently obtained better quality data on several more barred spirals using the Anglo-Australian 3.9m telescope. In the previous paper (Pence and Blackman, 1984, hereafter referred to as Paper I) we discussed the results on NGC 6221 which showed a discontinuity of about 150 km s-1 in the gas velocity across the dust lanes on the leading edges of the bar, which provided the firct direct observational proof that the dust lanes mark the location of shock fronts in the gas as predicted by the theore. al models. Now in this last paper in the series, we present the results on two more barred spiral galaxies, NGC 7496 and 289, which provide further support for the models.

2 Observations and Reduction Method

The 3.9m Anglo-Australian telescope was used to obtain long-slit spectra during the period* 5-7 August 1981 The observations were made with the RGO spectrograph with 25 cm camera and 1200 V grating (first order) in conjunction with the IPCS detector. Each digitally recorded spectrum consists of 2044 spectral elements, each approximately 0.45A wide, and 80 cross-sections, each separated by 2.3 arcsec on the sky. A slit width of 270M « 1.8 arcsec was used which projects to a spectral resolution of 1.3A. Most spectra were centred on the Ha region, but some spectra near Bfi were also taken to look for any interesting nuclear phenomena. The data reduction procedure was essentially the same as described in Paper I. The basic wavelength calibration of the spectra was performed with the Starlink SPICA software package, then specialized routines were written to find the wavelength of each emission line using a Gaussian profile fitting algorithm. The radial velocity of the gas at each spatial increment along the slit was Page 3

derived from a weighted mean of the red shifts of all the measurable emission lines. The weights were 6 for Ha, 3 for [NII]6583.6A and 1 for the [NII]6548.06A and [SII]6717.0A and 6731.3A lines. Fro« comparison of the independent velocity measurements at the 23 intersection points of the spectra, the mean error of a single observation in NGC 7496 is measured v.o be 5 km s-1. In NGC 289, which has weaker emission, only the Ha and [NII]6583 lines were measured and the mean error of a single velocity measurement is a « 10 km s » derived from the velocities at 16 intersection points.

We have also observed the 21cm HI line profile of these galaxies for comparison with the optical velocity field (Pig. 1). -These were obtained with the Parkes 210* radio telescope in Nov. 1981 in collaboration with M. Phillips (vTPlO) and A. Turtle (Univ. of Sydney).

3 RESULTS: HGC 7496 3.1 GENERAL

NGC 7496 is a SB(s)b barred spiral (de vaucouleurs, de Vaucouleurs and Corwin, 1976, hereafter RC2) with a pronounced bar about 1 arcmin in length which merges into two spiral arms. There are no companion galaxies of comparable size within a 1 degree radius so there is no possibility of tidal interactions confusing the interpretation of the velocity field. A distance of 16 Mpc is adopted

_1 -1 based on H0 * 1O0 km s Mpc which gives an image scale of 78 pc arcsec-1. The analysis of NGC 7496 is based on the 11 spectra listed in Table 1. The mean velocity of the Ho, [Nil] and [Sil] emission lines were measured at 321 positions in the galaxy, covering all the major features, ao shown in Fig. 2 and listed in Appendix A.

3.2 VELOCITY FIELD

The velocities from each spectrum were smoothed by a 3 point running mean in the spatial direction and then combined into a 2D map using the telescope coordinates and the intensity of the continuum emission along the slit to find their relative positions within the galaxy. The heliocentric isovelocity contours were traced by hand and are shown in Fig. 2. There is very little room for subjective bias in Page 4

Where the contours should be drawn because of the good spatial co\erage and accuracy of the velocity measurements. The main feature of interest in the figure is the way the isovelocity contours deviate froa the symmetric "spider" diagram appearance expected for circular rotation. Instead they are skewed to lie nearly parallel to the bar showing that large systemic streaming motions are present. Before discussing these noncircular notions further, we first derive the basic kinematic and orientation parameters.

3.3 BASIC PARAMETERS

The position angle of the line of nodes usually corresponds to the angle of steepest velocity gradient but in NGC 7496 this is not uniquely defined. In the central region the steepest gradient is nearly perpendicular to the bar whose major axis is at pa « 145*; at larger radii away from the perturbing influence of the bar, the maximum velocity gradient is at pa * 5* ± 5* which we assume is the true pa of the line of nodes. This agrees well with the optical major axis at pa « 0° ± 5* as measured from microdensitometer scans of the image on the SERC J sky survey.

The inclination of a barred spiral galaxy is difficult to determine because of the uncertainty in the intrinsic shape of the galaxy. If we follow the usual procedure of assuming <:'iat the outer optical isophotes define a circle in the galaxy plane, then from the axial ratio, b/a * 0.55, we derive an inclination of i - 55". However this implies that the maximum rotational velocity is

vmax - Av/2 »in(i) - 85 km s"1 where Av - 140 km s-1 is the observed range in radial velocity. This

is unrealistically low for an Sb galaxy, which usually has vnax in the range 200 to 250 km s-1 (Rubin et al., 1982), and leads to an improbably low mass for the galaxy. Since NGC 7496 seems typical of Sb galaxies in most other respects (see the comparison with NGC 53S3 in the following section) we shall reverse the usual procedure and assume

1 that vnax = 225 kms"* , which then implies that the inclination must be about 18*. Assuming that the spiral arms are trailing, then the west side of tht galaxy is nearest to us. Page 5

A» an estimate of the systemic velocity, three of our spectra intersect at the nucleus and give a mean velocity of 1657 ± 2 kms-1• Since the nuclear emission often shows a systematic velocity shift relative to the rest of the galaxy (Heckman et al. 1981) we also used the iterative model fitting procedure used previously for NGC 6221 (Paper I), excluding the points within 25" of the nucleus which are most strongly perturbed by the bar, and found a best fitting systemic velocity of V « 1652. These values are in good agreement with the HI 21cm velocities V(HI) • 1657 ± 8 (Pisher and Tully, 1981) and our own

measurement of V(HI) « 1640 ± 5 (Pig. 1). Thus we adopt V8V8 - 1655 ± 5 as the best estimate of the systemic velocity. The two previous optical radial velocity measurements, based on lower quality spectra, of V = 1470 (Shobbrook, 1966) and V «= 1540 (Martin, 1976) do not agree with the more recent results.

Because of the large ncncircular motions apparent in NGC 7496, the concept of a rotation curve (i.e. the rotational velocity vs. radius) is not well defined. Nevertheless, in Pig. 3 we show the rotation curve derived under the assumption that the gas is in circular motion using Vgyg « 1655, i - 18*, and the pa of the line of nodes - 5*. The large error bars at r < 30" show that these assumptions are not very realistic.

The mass of NGC 7496 c> be estimated from the outermost velocity point (V « 225 km s"1, r « 93" « 7.2 kpc) and Kepler's law to be

2 10 M «= rV /G - 8.5 x 10 M0 with the uncertainty in inclination being the main source of error As shown by Lequeux (1983) the actual mass within this radius is probably in the range 0.6 - 1.0 times the Keplerian value, depending on how the mass is distributed. The corrected total magnitude is B°, « 11.25 (RC2) which at a distance of 16 Mpc gives L « 1.2 x 1010 LQ and M/I -

7. From the 21 cm observations (Pig. 1) we derive Kg » 1,7 x 10* M0 (by comparison, Pisher and Tully (1981) derive 1.2 x 109, corrected to the same distance) and Mg/Kp - 0.02. Pag« 6

3.4 NONCÏRCULAR HOTIONS

The streaming notions of the gas in NGC 7496 are obvious in the isovelocity contour map (Pig. 2); along the minor axis for instance, systematic radial motions of 25 kms-1 are present, which When deprojected by the 18* inclination factor, imply streaming motions in the plane of more than 80 Ions-1.

One of the most striking things about the velocity field of NGC 7496 is its similarity to that of NGC 5383 (Peterson et al. 1978) as shown in Fig. 4. The contour maps are virtually identical, except that the range of velocity is greater in NGC 5383 due to the plane being more inclined to the line of bight. It is remarkable that even the S - shaped wiggle near the end of the bar in one of the contours (our V * 1680 and their V « -100) is reproduced in both maps. He would not have attached much significance to this except for the fact that Huberts, Huntley and van Albada (1979) find a similar feature in their models. In addition to the kinematic resemblance between these two galaxies, most of the other basic properties, such as linear diameter, optical luminosity, 21 cm flux, and colour are also very similar as listed in Table 2. NGC 5383 appears to be slightly larger and more massive, but this could simply be due to errors in the assumed distances. The only significant differences are in the orientation parameters: the galactic plane of NGC 7496 is seen »ore face on, and the bar is more side on. Also, the near side of the bar in NGC 7496 is swinging away from us due to the general rotation, whereas it is moving towards us in NGC 5383.

Recently a number of theoretical models have been applied to NGC 5383 (Huntley, 1978; Roberts, Huntley and van Mbada, 1979; Sanders and Tubbs, i960; van Albada and Roberts, 1981) that have very successfully reproduced the observed velocity field. Generally speaking, these models assume that the mass distribution is not axi8ymmetric but has an oval or bar-like distortion. The ga;t responds to this gravitational field by flowing in elongated o'bits ali med with the bar, and if the bar is massive enough, the gas streamlines intersect, forming shock fronts in the gas along the leading edges of the bar. Fig. 5 shows the predicted velocity field of 2 models by Page 7

Roberts et al. (1979) one with just a bar and disk (dashed contours) and one with an additional central spheroidal component (dashed contours). Because NGC 7496 is so similar to NGC 5363 we can expect these same models to fit NGC 7496 with just a change in orientation.

3.5 NUCLEUS OF NGC 7496

The relative strength of the emission lines in the nucleus of NGC 7496 is typical of normal photoionization found in HII regions. The emission line profiles are unusual however in that they show a long tail on the blue aid? which is mach stronger in the forbidden [OUI] lines than in the Balmer, [Nil] or [Sil] lines (Fig. 6). This same line structure is seen in NGC 6221 (see Paper I, fig. 11) and indicates that the blueshifted gas is more highly excited (because of the larger [OUI] to H0 ratio) and hence is closer *-.o the ionizing source in the nucleus. Unlike NGC 6221, however, the peaks of the emission lines in NGC 7496 are not blueshifted relative to the systemic velocity.

4 Resultst HOC 269 4.1 GENERAL

NGC 269 is an SB(rs)bc barred spiral galaxy with a relatively small bar (compared to NGC 7496) surrounded by two sets of spiral arms. The inner, high surface brightness arms extend to a radius of about 95"; the low surface brightness arms can be seen on the SERC sky survey out to r • 270". Vaucouleurs (1979) derived a distance of 22.4 Mpc which gives an image scale of 108 pc arcsec-1. we obtained 11 spectra (Table 1) in a rectangular grid which cover the main features in the bright central region of NGC 289 (Pig. 7). The slit was not long enough to include the faint outer spiral arms, but judging fro« the strength of the emission in the inner spiral &rms, it is unlikely that any emission would have been detected there. The emission in NGC 289 is generally much weaker than in NGC 6221 or 7496, hence only the Ha and [NII]6583A lines were used to map the velocity field. In total the velocity was measured at 327 positions in the galaxy as given in Appendix 8. Page 8

4.2 THE VELOCITY FIELD

The heliocentric velocity field is shown in Pig. 7. The generally smooth "spider" shape of the isovelocity contours shows that the gas is predominantly in circular motion, however the presence of the small wiggles in the contours near the bar and the fact that the kinematic major and minor axes are not perpendicular to one another indicates that noncircular motions are also present. KB before, we first find the best fitting axisymmetric kinematic model before discussing the noncircular motions.

4.3 AXT SYMMETRIC MODEL

U9ing the iterative technique of finding the best parameters for the circular rotation model (Paper X) we find

vsys m I6 »° * 2 km s"1 pa of line of nodes - 126* ±2* inclination - 45° ± 10* centre of rotation coincident with the nucleus. The systemic velocity agrees well with the midpoint of the 21cm

profile, v21 « 1626 ± 2, shown in Fig. 1 and with the nuclear velocity V « 1636 1 30 measured fron the two spectra which intersect there, however it disagrees with previous low precision measurements of V » 1926 (Humason, Mayall and Sandage, 1956; corrected to V« 1811 ± 69 in RC2) and v - 1740 (Martin, 1976). One difficulty with determining the systemic velocity of NGC 289 is that the steep velocity gradient near the nucleus (> 10 km s"1 axcsec-1) makes the central velocity sensitive to the placement of the spectrograph slit.

The kinematic line of nodes agrees well with pa - 130* of the major axis measured by Lauberts (1982) from the image on the ES0(B) survey. Similarly, the kinematically derived inclination is the same as implied by the axial ratio, b/a « 0.72 (RC2), of the outer optical isophotes. Page 9

4.4 ROTATION CURVE AND MASS

Pig. 8 shows that the rotation curve rises Bteeply out to r» 20" «• 7. .2 kpc, which corresponds to the end of the bar, ana then levels off at V - 225 km s-1- There are few data points within the bar region Itself, so the rotation curve there is not well defined. The minimum in the rotation curve at r » 55" corresponds to the transition region between the bright inner and faint outer spiral arms and suggests that the mass is distributed in two distinct components. Using the familiar Keplerian formula, the mass interior to the outer most measurement (V « 182 ±14, r - 108" « 11.7 kpc) is * M - rV2/G - 9.0 x \010 Kg. Of course the total mass may be much greater than this, especially since the faint outer spiral arms can be seen out to at least 2.5 times greater radius.

The corrected total magnitude, BÇ « 11.5, (de Vaucouleurs, 1979)

10 corresponds to a luminosity of 1.8 z 10 L0 which gives M/L * 5. Prom the 21cm profile we derive a mass for the neutral gas of 1.8 x 1010 Kg (compared with Kg • 1.9 x 1010 derived by Fisher and Tully, 1981) and My/Hp - o.2. This is an unusually large neutral gas fraction and is probably related to the presence of the very extended faint spiral arms.

4.5 NONCIRCOLAR MOTIONS

The average RMS residual of the best fitting circular rotation model is only 14.7 km s-1, not much more than our measuring precision of 10 km s"1, which implies that the non-circular motions are not very significant. The reason for this is two fold. First, our spectra provide little information on the velocities in the bar because of its small size and weak emission. Most of the measurements come from the surrounding spiral arms which would not feel much effect from the bar. Secondly, the bar is aligned at pa • 120* ± 5*, nearly parallel to the line of nodes, which is unfavourable for seeing the streaming motions. The model calculations of van Albada and Roberts (1981) show that when the bar is viewed side on the isovelocity contours are very symmetric except for stns-jl effects in the shock fronts on the leading edges of Page 10

the bar which we would not expect to resolve in NGC 2B9. it is only when the bar is at "45" to the line of nodes that the dramatic S - Biiaped distortions in the isovelocity contours are observed, as in NGC 7496 and 5383. While the contours in the bar region of NGC 289 do show some irregularities, the spatial coverage is not complete enough to say whether the effects are in agreement with the models. There is however clear evidence that elliptical streaming motions are present, from the fact that the kinematic major and minor axes are not perpendicular. The kinematic major axis, defined by the line through the midpoint of the V * 1470 and V - 1790 contours, is at PA - 120* while the minor axis, defined by the V - 1630 contour, is at PA « 40*, i.e., a difference of only 80° . This nonalignment is seen in many galaxies and is classified by Bosma (1981) as due to oval distortions in the disk, in this case caused by the bar.

4.6 NUCLEUS

The relative nuclear emission line strengths axe consistent with photoionization as in normal HI1 regions throughout the galaxy. The lines do not show any of the peculiarities seen in NGC 6221 or 7496, however because the emission is 100 times fainter than in NGC 7496 any small line profile asymmetries would be difficult to detect.

5 Discussion

The main purpose of this series of papers has been to find observational verification of the theoretical models of gas streaming in barred spiral galaxies. As with NGC 6221 in Paper I, we tabulate in the appendix our velocity measurements for use in developing more refined models, of the two galaxies discussed here, NGC 7496 has a more dominant bar and the velocity field clearly shows the predicted streaming motions which cause the iBovelocity contours to be distorted into the characteristic S - shape pattern with a large velocity gradient across the bar. One of the most important results is that the similarity to NGC 5383 shows that this is a general phenomenon in barred spiral galaxies and not an isolated peculiarity caused by a tidal encounter or other unique event. This had been a problem in the interpretation of the velocity field of NGC 53*3 which has a close Page 11

companion, however since NGC 7496 is an isolated galaxy this possibility is ruled out.

In NGC 289 the bar is much smaller and morphologically less significant compared to the large spiral arm pattern, hence the noncircular motions are expected to be much smaller than in NGC 7496. Nevertheless, the predicted noncircular motions are still detected, the most prominent effect being the obliqueness of the kinematic major and minor axes. This is typical of the "oval distortion" class of galaxies discussed by Bosma (1981).

The good agreement between the models and the observed velocity fields in NGC 5383, 6221 and 7496 gives some confidence that the models are realistic. An additional test of the models can be made by comparing tie velocity fields in different galaxies inwhich the bar has different orientations to the line of sight. As was shown in fig. 11 of van ALbaca *nd Roberts (1981) the observed radial velocity map should depend significantly on the bar orientation? the proainant S-shaped distortions of the isovelocity contours, as seen in NGC 7496 and 5383, should only be seen when th«? bar is at an angle of about 45* to the line of sight; when the bar is at about 0* (side-on) or 90* (end-on) the isovelocity contour map should be fairly symmetric, except for small scale effects in the dust lanes (shock fronts) which generally require high spatial resolution to detect, as for example in NGC 6221. To test this prediction, we collected from the literature all the barred spirals with well observed velocity fields to see if the s-shaped distortion is apparent. In table 3 the galaxies are grouped according to whether or not the distortion is present, along with the angle between the major axis of the bar and the line of nodes. Even though the position angle of the line of rodes is often very uncertain, the strong correlation is obvious: all the galaxies with the hax inclined at about 45* show the velocity field distortion, and all the other galaxies do not show it, just as predicted by the models. Other variables were examined (e.g. mass, HI content, presence of nearby companions) but none showed any strong correlation with the appearance of the velocity field. This result clearly shows thai not all barred spirals should show obvious noncircular motions, as the effect is strongly dependant on the orientation of the b&r. 7

Page 12

Acknowledgements

We thank PATT for the allocation of telescope tine, the SERC for financial assistance and David Malin for making the photographic reproductions. Page i3 APPENDIX A Velocity measurments for NGC 7496

The final 321 velocity measurements in NGC 7496 are listed below. The X and Y coordinates are in units of seconds of arc relative to the nucleus with the positive X axis aligned at position angle « 299" . The heliocentric velocity is the mean of measurements of tne redshift of at least two emission lines, except thcje indicated by a * in which only the Bar line could be measured.

X Y V X Y V X Y V X Y V 0.0 11.3 1601* 0.0 12.0 1602 0.0 9.7 1592* 0.0 5.2 1613 0.0 2.9 1638 0.0 0.6 1650 0.0 -17 1663 0.0 -4.0 1677 0.0 -8.6 1687* 0.1 -31.5 1706* 0.1 -42.9 1704* 0.2 -45.2 1697* 0.2 -47.5 1696* 0.2 -40.6 1714* 0.2 -52.1 1693* 0.2 -54.4 1703* 0.2 -56.7 1705* -35.1 -21.2 1700* -33.1 -20.0 1684 -31.1 -18.9 1696 -29.2 -17.7 1677 -27.2 -16.5 1674^ -25.3 -15.3 1675 -23.3 -14.1 1670 -19.4 -11.7 1662 -17.4 -10. ö 1678* -15.5 -9.4 1690* -13.5 -8.2 1670 -11.6 -7.0 1690 -9.6 -5.8 1693 -7.6 -4.6 1660 -5.7 -3.4 1661 -3.7 -2.3 1649 -1.8 -1.1 1662 0.2 0.1 1653 2.2 1.3 1637 4.1 2.5 1620 6.1 3.7 1630 8.0 4.9 1635 13.9 8.4 1639« 15.9 9.6 1629* 19.8 12.0 1618 21.7 13.2 1606 23.7 14.4 1615 25.7 15.5 161F 27.6 16.7 1616 29.6 17.9 1615 31.5 19.1 1617 33.5 20.3 1617 35.5 21.5 1620 37.4 22 .7 1615 39.4 23.8 1611 41 .3 25.0 1606 43.3 26.2 1607 45.2 27.4 1606 47.2 28.6 1596 49.2 29.8 1601 51.1 31.0 1598* 66.8 40.5 1590* 68.8 41.6 1589* -75.8 0.0 1684« -73.5 0.0 1674* -71.2 0.0 16rl* -66.6 0.0 1663* -36.9 0.0 1672* -34.6 0.0 1678 -32.3 0.0 1662 -30.0 0.0 1663 -27.7 0.0 1665 -25.4 0.0 1656 -23.1 0.0 1653 -20.8 0.0 1664» -14.0 0.0 1671* -11.7 0.0 1635* -9.4 0.0 1643 -7.1 0.0 1630 -4.B 0.0 1640 -2.5 0.0 1662 -0.2 0.0 1663 2.1 0.0 1658 4.4 0.0 1669 6.6 0.0 1688 8.9 0.0 1693 11.2 CO 1701 13.5 0.0 1652 15.8 0.0 1670* 18.1 0.0 1669 20.4 0.0 1658 22.7 0.0 1648* 25.0 0.0 1655 27.3 0.0 1650 29.5 0.0 1633 31.8 0.0 1660* 34.1 0.0 1645 36.4 0.0 1643 38.7 0.0 1654 41.0 0.0 1657 43.3 0.0 1635* 16.3 -39.1 1692* 17.0 -37.0 1688 17.7 -34.8 1691* 18.4 -32.6 1668* 19.0 -30.4 1674 19.7 -28.2 1680 20.4 -26.0 1678 21.1 -23.8 1671 21.8 -21.6 1663 23.1 -17.3 1667* 27.9 -2.0 1647 28.6 0.2 1646 29.2 2.4 1640 29.9 4.6 1647 30.6 6.8 1630 31.3 9.0 1629 32.0 11.2 1632 32.7 13.3 1623 33.3 15.5 1630 34.0 17.7 1621 34.7 19.9 1624 35.4 22.1 1628 36.1 24.3 1620 36.7 26.5 1618 37.4 28.6 1609 38.1 30.8 1604 38.8 33.0 1604 39.5 35.2 1597 40.1 37.4 1585* 40.8 39.6 1593* 41.5 41.8 1592* 42.9 46.1 1596* 43.5 48.3 1586* 45.6 54.9 1577* 46.3 57.1 1578 47.0 59.3 1582* 49.0 65.8 1569* 51.7 74.6 1586* -26.4 -63.6 1720* -25.7 -61.4 1713* -25.1 -59.3 1733 -24.4 -57.1 1718 -23.7 -54.9 1712 -23.0 -52.7 1708 -22.3 -50.5 1719 -21.6 -49.3 1708 Paae 14

measurments HGC 7496 (Cont. ) X y V X Y V X T V X Y V -21.0 -46.1 1723 -20.3 -43.9 1721* -19.6 -41.8 1708* -18.9 -39.6 1709 -18.2 -37.4 1707 -17.6 -35.2 1708 -16.9 -33.0 1719 -16.2 -30.8 1694» -8.7 -6.8 1671* -8.0 -4.6 1676* -7.3 -2.4 1664* -6.7 -0.2 1624 -6.0 2.0 1627 -5.3 4.2 1622 -4.6 6.3 1619 9.0 50.1 1588» 9.7 52.3 1581* 11.7 58.8 1572* 12.4 61.0 1586* 14.4 67.6 1574* 15.1 69.7 1597» 15.8 71.9 1591 16.5 74.1 1579 17.2 76.3 1592 -48.8 -14.2 1690* -46.6 -13.5 1684* -44.4 -12.9 1696* -42.2 -12.3 1679* -40.0 -11.6 1689 -37.8 -11.0 1689 -35.6 -10.4 1683 -33.4 -9.7 1690 -31.2 -9.1 1684 -29.0 -8.4 1683 -26.8 -7.8 1678* -24.6 -7.2 1673 -22.4 -6.5 1650* -20.2 -5.9 1648 -18.0 -5.2 1643 -15.8 -4.6 1643 -13.6 -4.0 1652 -11.4 -3.3 1647 -9.2 -2-7 1646 -7.0 -2.0 1858 -4.8 -1.4 1653 -2.6 -0.8 1664 -0.4 -O.l 1660 1.8 0.5 1659 4.0 1.1 1657 6.2 1.8 1665 8.4 2.4 1666 10.6 3.1 1669 12.8 3.7 1673* 15.0 4.3 1668 17.2 5.0 1666 19.4 5.6 1658 21.6 6.3 1659 23.7 6.9 1652 25.9 7.5 1653 28.1 8.2 1639 30.3 8.8 1632 32.5 9.5 1631 34.7 lO.l 1638 36.9 lO 7 162« 39.1 11.4 1625 41.3 12.0 1623 43.5 12.7 1625 45.7 13.3 161 J 47.9 13.9 1619 -23.7 -71.9 1740* -23.9 -69.7 1712* -24.1 -67.4 1726* -24.2 --5.1 1721* -24.4 -62.8 1715 -24.6 -60.5 1718 -24.7 -58.2 1719 -24.9 -56.0 1717 -25.1 -53.7 1712 -25.2 -51.4 1715 -25.4 -49.1 1718 -25.6 -46.8 1722 -2F .7 -44.5 1716 -25.9 -42.3 1708 -26.1 -4O.0 1715» -26.2 -37.7 1729* -26.4 -35.4 1692* -26.6 -33.1 1694* -26.7 -30.8 1718 -26.9 -28.5 1704* -27.1 -26.3 1701 -27.2 -24.0 1704 -27.4 -21.7 1700» -2V.6 -19.4 1691* -27.7 -17.1 1673 -27.9 -14.8 1686 -28.1 -12.6 1675 -28.2 -10.3 1671* -28.4 -8.0 1673 -28.6 -5.7. 1630 -28.7 -3.4 1687 -28.9 -1.1 1672 -29.1 1.1 1667 -29.3 3.4 1664 -29.4 5.7 1651 -29.6 8.0 1649 -31.3 30.8 1621* -31.4 33.1 1633 -12.2 -76.3 1711* -11.5 -74.1 1702* -10.8 -72.0 1704* -6.6 -58.9 1724 -5.9 -56.7 1710 -5.2 -54.5 1710 -4.5 -52.3 1707 -3.8 -50.1 1699 -3.1 -48.0 1701 -2.4 -45.8 1701 -1.7 -43.6 1704 -1.0 -41.4 1713* -0.3 -39..? 1705* 6.0 -19.6 1696* 6.7 -17.4 1705* 7.4 -15.3 1689* 8.1 -13.1 1672» 8.8 -10.9 1699* 9.5 -8.7 1715* 10.2 -6.5 1678 10.9 -4.4 1677* 11.6 -2.2 1666 13.0 2.2 1657* 13.7 4.4 1675 14.4 6.5 1660 15.1 8.7 1649 15.8 10.9 1656* 16.5 13.1 1601* 17.2 15.3 1615 17.9 17.4 1607 20.7 26.2 1583* 21.4 28.3 1602* 22.1 30.5 1598 22.8 32.7 1583* 23.5 34.9 1599* 24.2 37.1 1600 24.9 39.2 1597 2b.6 41.4 1599* 26.3 43.6 1601* 27.0 45.8 1574* 27.7 48.0 1592* 28.4 50.1 1561* 29.1 52.3 15B5* 33.3 65.4 1583* 34.0 67.6 1583* 34.7 69.8 1597* •42.0 -14.3 1680* -*0.5 -12.5 1678 -39.1 -10.7 1677» -37.7 -8.9 1677* -36.2 -7.1 1672 -34.8 -S... 1670 -33.4 -3.6 lt>66 -31.9 -1.8 1660 -30.5 0.0 1656 -29.1 1.8 1649 -27.6 3.6 1647 -26.2 5.4 1640* -24.8 7.1 1631 -23.3 8.9 1634 -16.2 17.9 1624» -14.8 19.7 1626* -13.3 21.4 1619* 25.3 69.7 1578 26.8 71.5 1567 28.2 73.3 1577 2J.6 75.1 1573 31.1 76.8 1573 32.5 78.6 1582 33.9 80.4 1588* Page 15

APPENDIX B Velocity neasurnente for NGC 289

The final 327 velocity measurements in NGC 289 are listed below. The X and T coordinates are in units of seconds of arc relative to the nucleus with the positive X axis aligned at position angle - 270* . The heliocentric velocity is the mean of measurements of the redshift of Ha and [NII]6583A, except those indicated by a * in which only the Ha line could be measured.

X y V X T V X Y V X Y V 42.6 0.0 1567* 40.3 0.0 1524* 38.0 0.0 1519* 35.7 0.0 1526* 31.1 0.0 1561* 28.9 0.0 1531* 26.6 0.0 1520 24.3 0.0 1530 22.0 0.0 1515 19.7 0.0 1520 17.4 0.0 1540* 15.1 0.0 1564* 12.3 0.0 1501* 6.0 0.0 1524* 1.4 0.0 1565 -0.9 0.0 1703 -3.2 0.0 1712 -10.1 0.0 1729* -12 .4 0.0 1714 -16.9 0.0 1751 19.2 0.0 1754 -21.5 0.0 1756, -23.8 0.0 1751 -26.1 0.0 1750* 37.6 0.0 1744* -39.8 0.0 1740* 0.0 -38.7 1700* 0.0 -36.4 1693* 0.0 -34.1 1686 0.0 -31.8 1688 0.0 -29.5 1700 0.0 -27.3 1687 0.0 -25.0 1693 0.0 -22.7 1706* 0.0 -20.4 1693 0.0 -18.1 1698* 00 -15.8 1706* 0.0 -13.5 1690* 0.0 -11.2 1688* 0.0 -8.9 1635* 00 -6.6 1629 0.0 -4.4 1616 0.0 -2.1 1620 CO 0.2 1611 0.0 2.5 1600 0.0 9.4 1592* 0.0 11.7 1555* 0.0 14.0 1557 0.0 16.3 1539 0.0 18.5 1537 O.O 20.8 1548 0.0 23.1 15*2 0 0 25.4 1556 0.0 27.7 1553 0.0 30.0 1564 0.0 32.3 1561* 0.0 34.6 1561* 0.0 36.9 1563 0.0 39.2 1560 0.0 41.4 1555 0.0 43.7 1551 0.0 46.0 1557 0.0 50.6 1550 0.0 52.9 1542 0.0 55.2 1538 0.0 57.5 1530 O.O 59.8 1533 0.0 62.1 1548* 0.0 64.3 1563* 22.0 76.7 1517* 22.0 74.4 1549* 22.0 72.1 1542* 22.0 69.8 1506* 22.0 67.6 1500 22.0 65.3 1507 22.0 63.0 1513* 22.0 60.7 1545* 22.0 58.4 1529* 22.0 56.1 1515 22.0 53.8 1503 22.0 51.5 1511 22.0 49.2 1509 22.0 46.9 1499* 22.0 44.7 1515 22.0 42.4 1510 22.0 40.1 1495* 22.0 37.8 1517* 22.0 33.2 1489» 22.0 30.9 1490 22.0 28.6 1495 22.0 26.3 1488 220 24.0 1503* 22.0 21.8 1499* 22.0 19.5 1473* 22.0 17.2 1477 22.0 14.9 1469 22.0 12.6 1470 22.0 10.3 1470 22.0 8.0 1481 22.0 5.7 1492 22.0 3.4 1511 22.0 1.1 1515 22.0 -1.1 1536 22.0 -3.4 1540 22.0 -5.7 1548 21.0 -8.0 1559 22.0 -10.3 1571 22.0 -12.6 1583 22.0 -14.9 1605 22.0 -17.2 1603 22.0 -19.5 1611 22.0 -21.8 1626« 22.0 -24.0 1625* 22.0 -26.3 1612* 22.0 -69.8 1657* 22.0 -72.1 1646* 22.0 -74.4 1665* 22.0 -76.7 1659* 11.0 69.8 1531* 11.0 67.fi 1521* 11.0 65.3 1517 11.0 63.0 1513 11.C 60.7 1508 11.0 58.4 1521 11.0 56.1 1516* 11 0 53.8 1533* 11.0 51.5 1533* 11.0 49.2 1523« 11.0 46.9 1522* li.O 44.7 15J5 11.0 42.4 1521 11.0 40.1 1520 11.0 37.8 1506* 11.0 35.5 1527 11.0 33.2 1517 11.0 30.9 1518 11.0 26.6 1524 11.0 26.3 1505* 11.0 24.0 1493* 11.0 21.8 1523* 11.0 19.5 1482 11.0 17.2 1489 11.0 14.9 I486* 11.0 12.6 1501 J

Page 16

velocity measurements in HGC 289 • - (Cont •) X Y V X Y V X Y V X Y V 11.0 -14.9 1612» 11.0 -17.2 1646 11.0 -19.5 1640» 11.0 -21.8 1629« 11.0 -24.0 1638 11.0 -26.3 1651 11.0 -M. 6 1657 11.0 -30.9 1665* 11.0 -33.2 1673» 11.0 -42.4 1683* 11.0 -46.9 1674« 11.0 -49. i 1673* -12.0 46.9 1594« -12.0 44.7 1581* -12.0 42.4 1590* -12.0 40.1 1583* -12.0 37.8 1604» -12.0 35.5 1606 -12.0 33.2 1609* -12.0 30.n 1611 -12.0 26.6 1616» -12.0 26.3 1611 -12.0 24.0 1608 -12.0 21 8 1615 -12.0 19.5 1626 -12.0 17.2 1611 -12.0 14.9 1616* -12.0 12.6 16*0* -12.0 3.4 1664* -12.0 1.1 1706* -12.0 -3.4 1720* -12.0 -8.0 1738 -12.0 -10.3 1722 -12.0 -12.6 1750 -12.0 -14.9 1767 -12.0 -17.2 1774 -12.0 -19.5 1769 -12.0 -21.8 1743* -12.0 -24.0 1753* -12.0 -26.3 1765« -12.0 -28.6 1752 -12.0 -30.9 1746 -12.0 -33.2 1743 -12.0 -35-5 1741 -12.0 -37.8 1739 -12.0 -40.1 1735 -12.0 -42.4 1733 -12.0 -44.7 1735 -12.0 -46.9 1732 -12.0 -49.2 1735 -12.0 -65.3 1745* -12.0 -67.6 1744* -26.0 13.7 1704 -26.0 9.2 1705 -26.0 6.9 1733 -26.0 4.6 1721 -26.0 2.3 1741 -26.0 0.0 1756 -26.0 -2.3 1758« -26.0 -4.6 1768 -26.0 -6.9 1771 -26.0 -9.2 1778 -26.0 -11.4 1792* -26.0 -13.7 1792 -26.0 -16.0 1788 -26.0 -18.3 1784 -26.0 -20.6 1783 -26.0 -22.9 1765 -26.0 -25.2 1775 -26.0 -27.5 1781 -26.0 -29.8 1779 -26.0 -32.1 1774 -26.0 -34.3 1751» -26.0 -36.6 1771 -26.0 -38.9 1767 -26.0 -41.2 1767 -26.0 -43.5 1753 -26.0 -45.8 1752 -26.0 -48.1 1758 -26.0 -50.4 1753 -26.0 -52.7 1754 -26.0 -66.4 1751* -26.0 -68.7 1749* -26.0 -71.0 1762* 38.9 -10.0 1571» 34.3 -10.0 1564* 32.1 -10.0 1591* 29.8 -10.0 1556* 27.5 -10.0 1556« 25.2 -1O.0 1546* 22.9 -1O.0 1543* 20.6 -10.0 1582 IB. 3 -10.0 1569 16.0 -10.0 1588 13.7 -10.0 1590* 11.4 -10.0 1652* 6.9 -10.0 1640* 4.6 -10.0 1684* 2.3 -1O.0 1685* 0.0 -10.0 1696 -2.3 -10.0 1672» -4.6 -10.0 1705* -6.9 -10.0 1679* -9.2 -10.0 1716 -114 -10.0 1742» -13.7 -10.0 1785* -16.0 -1O.0 1799 -18.3 -10.0 1787 -20.6 -10.0 1786 -22.9 -10.0 1779 -25.2 -1O.0 1766 -38.9 -10.0 1759* -41.2 -10.0 1764» -43.5 -10.0 1762* 41.2 1O.0 1504« 29.8 10.0 1511* 27.5 10.0 1506 25.2 10.0 1494* 22.9 1O.0 1489 20.6 10.0 1485 16.3 10.0 1475 16.0 10.0 1481 13.7 10.0 1490 11.4 10.0 1512* 9.2 10.0 1516* 6.9 10.0 1563* 4.6 1O.0 1569« 2.3 10.0 1570 0.0 10.0 1609 -2.3 10.0 1586* -16.0 1O.0 1692« -18.3 10.0 1697 -20.6 10.0 1698 -22.9 10.0 1708* -34.3 1O.0 1695« -36.6 10.0 1691 -33.9 10.0 1692 -41.2 10.0 1692* 2.3 -33.0 1695 0.0 -33.0 1686 -2.3 -33.0 1695 -4.6 -33.0 1694 -6.9 -33.0 1728 -9.2 -33.0 1735 -11.4 -33.0 1733 -13.7 -33.0 1747 -16.0 -?3.0 1760 -18.3 -33.0 1766 -20.6 -33.0 1778» -25.2 -33.0 1789 -27.5 -33.0 1791 -29.8 -33.0 1779 -87.0 -33.0 1766* -89.3 -33.0 1754* -91.6 -33.0 1752* 36.6 25.0 1489* 34.3 25.0 1487» 32.1 25.0 1459 29.8 25.0 1478 27.5 25.0 1479* 25.2 25.0 1458» 22.9 25.0 1475* 20.6 25.0 1490* 18.3 25.0 I486* 16.0 25.0 1484» 13.7 25.0 1477* 11.4 25.0 1496 9.2 25.0 1516 6.9 25.0 1538» 4.6 25.0 1534 2.3 25.0 1529 0.0 25.0 1538 -2.3 25.0 1549 -4.6 25.0 1579 -6.9 25.0 1567 -9.2 25.0 1598 -11.4 25.0 1606* -13.7 25.0 1595 -16.0 25.0 1606« -22.9 25.0 1643» -25.2 25.0 1648» -27.5 25.0 1631* -29.8 25.0 1652« Page 17

References

Blackman, c. P. £ Pence, W. D.r 1982. Mon. Kot. R. astr. Soc., 198, 517. Boama, A., 1981. Astron. J., 86. 1025. de Vaucouleurs, G., 1979. Astrophys. J., 227, 729. de Vaucouleurs, G., de Vaucouleurs, A. & Corwin, H., 1976. The Second Reference Catalogue of Bright Galaxies, University of Texas Press, Austin (RC2). Planer, J. R. £ Tully, R. B., 1981. Astrophys. J. Suppi., 47, 139. Gottesman, S. T., 1982. Astron. J., 87, 751. Heckman, T. M., Miley, G. K., Breugel,*W. J. M. and Butcher, H. R., 1981. Astrophya. J., 247, 403. Humason, M. L., Kayall, N. D., £ Sandage, A. R., 1956. Astron. J., 61, 97. Huntley, J. M., 1978. Astrophys. J., 225, L101. Lauberts, A., 1982. "ESO üppsula Survey of the ESO(B) Atlas" European Southern Observatory, Munich. Lequeux, J., 1983. Astron. Astrophys. 125, 394. Martin, W. L., 1976. Mon. Hot. R. astr. Soc. 175, 633. Pence, W. £ Blackman, C. P., 1984. Mon. Not. R. astr. Soc., 206, 000 (Paper 1). Peterson, C. J., 1982. Pub. astr. Soc. Pacific, 94, 409. Peterson, C. J. G Huntley, 7. M., I960. Astrophys. J., 242, 913 Peterson, C. J., Rubin, V. C, Ford, W. K. £ Thonnard, N., 1978. Astrophys. J., 219, 31. Roberts, W. Vf., Huntley, J. M. £ van AJLbada, G. D., 1979. Astrophys. J., 233, 67. Rubin, V. C, Ford, W. K., Thonnard, M. £ Burstein, D., 1982. Astrophya. J. 261, 439. Sanders, R. H. £ Tubes, A. D., 1980. Astrophys. J., 235, 803. Schempp, W. V. £ Wolstencroft, R. D., 1979. Photometry, Kinematics, and Dynamics of Galaxies, ed. Evans, D. S., Univ. of Texas, p. 453. Shobbrook, R. R., 1966. Mon. Not. R. astr. Soc, 131, 293. van Albada, G. D. £ Roberts, W. W., 1981. AstrophyB. J., 246, 740. Page 16

Table 1

NGC 7496 Spectra

Date Exp Slit Seeing PA* Position Spectral (sec) (") (") region

1 5 Aug 81 10O0 1.8 3 29 Nucleus Ha 2 ft 20O0 1.8 2 150 Nucleus Ha 3 M 20O0 1.8 2 119 Nucleus Ha 4 M 20O0 1.8 2 192 N arn Ha 5 •t 20OO 1.8 2 192 E of nucleus Ha 6 6 Aug 81 20O0 1.8 29 Nucleus H* 7 m 20OO 1.8 135 Nucleus Ha 8 fi 2000 1.8 213 SE an Ha 9 pt 25O0 1.8 192 W of nucleus Ha 10 7 Aug 81 1200 1.8 170 E of nucleus Ha 11 m 1OO0 1.8 170 Nucleus H*

NGC 289 Spectra

1 5 Aug 81 2000 1.8 2 90 Nucleus Ha 2 m 20O0 1.8 2 0 Nucleus Ha 3 7 Aug 81 1500 1.8 5 0 22" W Ha 4 r» 12O0 1.8 5 0 11" W na 5 » 1200 1.8 5 0 12" E Ha 6 « 1200 1.8 4 0 26" E sa 7 «• 1000 1.8 4 90 10" S Ha 8 f* 1OO0 1.8 4 90 10" N Ha 9 n 1000 1.8 3 90 33" S Ha 10 «I 1O00 1.8 3 90 25" N Ha 11 8 Sept. 82 500 0.7 3 32 Nucleus H* J

Page 19

Table 2 Comparison of galaxy parameters 1/

NGC 7496 NGC 53832 HOC 289

Type1 SB( 8 )b SB( rs )b SB( rs )bc Radial velocity, km/8 1655 2264 1630 corrected velocity, km/s 1628 2365 1612 Distance, Mpc 16 23.6 22.4 Distance modulus 31.02 31.86 31.75 Image scale, 1" « 78 pc 115 pc 109 pc Inclination let 40 45 Max. rotational vel., km/8 225 s 260 250

Diameter1, D25 (• - kpc) 3.47 - 16.2 3.55 » 24.5 3.72 » 24.3 Bar length (" • Jcpc) 70-5. 5 100 - 11.5 40 - 4.4 PA, line of nodes 5° 82° 126* PA, bar 145° 134° 120°

Angle from bar to 1. of nodes 40* 52# 6°

Corrected mag1, BÇ 11.25 11.79 11.5 Absolute mag, M°, -19.77 -20.07 -20.25

Corrected colour1, (B-V)Ç 0.43 0.57 -

Corrected colour1, (U-B)§ -.11 -.02 -

10 Hase, 10 M0, within r - kpc 8.5

10 "HI- ' MO 1.7 2 18 H/L, solar units 7 7 5

1 From RC2.

2 From Peterson et al. (1978) converted to D » 23.6 Mpc. i Page 20

Table 3 Barred spirals with S-shaped isovelocity contours

NGC 0 Reference 1097 45 Schempp £ Wolstencroft, 1979 5383 52 Peter son, Rubin, Ford £ Thonnard, 1978 7496 40 present paper

Barred spirals without S-shaped isovelocity contours

RGC e Reference 289 6 present paper 1300 3 Peterson S Buntley, 1980 2525 13 Blackman £ Pence, 1982 3359 15 Gottesman, 1982 3504 12 Peterson, 1982 4027 84 Pence et al., in preparation 6221 90 Pence £ Blackman, 1984 7741 70 Blackman £ Pence, 1982

0 - Angle between line of nodes and major axis of bar. Page 21

Figure Captions

Pig. 1 - The HI 21cm line profiles of HGC 7496 (a) and HGC 289 (b). Both were observed with the Parkes 210' telescope using a 15 min. integration followed by a 15 min. integration on the adjacent sky to determine the baseline. Pig. 2 ~ The velocity field of HGC 7496 superposed on an I band CCD image taken at the prime focus of the Ju\T. The squares indicate the position of the 321 velocity measurements. The heliocentric isovelocity contours are labeled in km s-1. Pig. 3 - The rotation curve for HOC 7496 derived with the assumption that the gas in in circular rotation. The bars indicate the error of the mean rotational velocity of all the points falling within successive 5" annuli. The large error bars for r < 40" indicate that noncircular motions are present. Pig. 4 - Comparison of the velocity field in HGC 7496 and HGC 5383 (Peterson et al., 1978) showing the remarkable similarity. X larger range of velocities is observed in HGC 5383 because it is more inclined to the line of sight. rig. 5 - The velocity field predicted by two models produced by Roberts et al. (1979) showing close similarity to HGC 5383 and HGC 7496. The solid contours are from a model with a central spheroid whereas the dashed contours are from a model with just a disk and bar. Fig. 6 - The M/3 and [0IIIJ5007A emission line profiles in the nucleus of HGC 7496. TBe blue shifted wing is relatively much stronger in the higher excitation [OUI] line. The error bars at the right indicate the ± la uncertainty in the [OUI] profile at different intensity levels. The errors in the H/? profile are half as large. Pig. 7 - The velocity field of HGC 289 superposed on the image from the ESO(B) sky survey. The small squares indicate the position of the 327 velocity measurements. Hote that the kinematic major and minor axes are not perpendicular indicating the presence of oval streaming. Fig. 8 - The rotation curve for HGC 289. The small error bars show that the assumed circular rotation model produces a good fit, except within 10" of the nucleus. -T . .. 1 —r •• r i 1

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