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Structure and Kinematics of the Peculiar Galaxy NGC A&A manuscript no. (will be inserted by hand later) ASTRONOMY Your thesaurus codes are: AND 04 (11.09.1 NGC 128; 11.05.1; 11.11.1; 11.16.1; 11.19.6; 11.07.1) ASTROPHYSICS Structure and kinematics of the peculiar galaxy NGC 128. ⋆ M. D'Onofrio1, M. Capaccioli2,3, P. Merluzzi2, S. Zaggia2, and J. Boulesteix4 1 Dipartimento di Astronomia, Universit`adi Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 2 Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131 Napoli, Italy 3 Dipartimento di Scienze Fisiche, Universit`adi Napoli, Mostra d’Oltremare, Padiglione 19, I-80125, Napoli, Italy 4 Observatoire de Marseille, 2 Place Le Verrier, F-13248 Marseille Cedex 04, France Received ; accepted Abstract. This is a multiband photometric and spectroscopic vationally. The main difficulty comes from the fact that the pe- study of the peculiar S0 galaxy NGC 128. We present results culiar morphologycan be seen only in almost edge-on systems. from broad (B and R) and narrow (Hα) band optical CCD pho- Photometric evidences of a bar in boxy/peanut galaxies tometry, near (NIR) and far (FIR) infrared observations, long have been found only in a few cases, e.g. the barred galaxy slit spectroscopy, and Fabry-Perot interferometry (CIGALE). NGC 4442 at intermediate inclination (Bettoni & Galletta The peculiar peanut shape morphology of the galaxy is 1994), the edge-on S0 galaxy NGC 1381 (de Carvalho & observed both at optical and near-infrared wavelengths. The da Costa 1987), NGC 5170 (Dettmar & Barteldrees 1988), stellar disk is thick and distorted (arc-bended), with a color NGC 2654, and NGC 4469 (Jarvis 1986). asymmetry along the major axis due to the presence of a The kinematic observations offer further evidences of this large amount of dust, estimated through NIR and FIR data of connection. Kuijken & Merrifield (1995) obtained a character- 6 ∼ 6 × 10 M⊙, in the region of interaction with the companion istic “figure-of-eight” rotation curve, which is likely the strong galaxy NGC 127. signature for the presence of a bar, for two peanut shape ob- The color maps are nearly uniform over the whole galaxy, jects: NGC 5746 and NGC 5965. Other known cases of galax- but for the major axis asymmetry, and a small gradient toward ies with these peculiar rotation curves are IC 5096 (Bureau the center indicating the presence of a redder disk-like com- & Freeman 1997), NGC 2683 (Merrifield 1996), NGC 5907 ponent. The Hα image indeed reveals the existence of a tilted (Miller & Rubin 1995, and UGC 10205 (Vega et al. 1997). gaseous “disk” around the center, oriented with the major axis Of course, given the small number of cases, new accurate toward the companion galaxy NGC 127. photometric and spectroscopic observations are necessary for Long slit and CIGALE data confirm the presence of gas in solving the peanut/bar connection. a disk-like component counter-rotating and inclined approxi- Here we present a large data-set for the most representa- ◦ mately of 50 to the line of sight. The mass of the gas disk in tive object of this class: NGC 128, the standard peanut-shaped 4 arXiv:astro-ph/9809213v1 16 Sep 1998 the inner region is ∼ 2.7 × 10 M⊙. galaxy (Sandage 1961). The stellar velocity field is cylindrical up to the last mea- In the following sections we describe the peculiar morphol- sured points of the derived rotation curves, while the velocity ogy of NGC 128 and its group, present a 2D approximated dispersion profiles are typical for an S0 galaxy, but for an ex- model of the surface brightness of the galaxy (Sec. 2), give the tended constant behaviour along the minor axis. results of long slit and CIGALE data (Sec. 3), show the surface brightness and color profiles of the galaxy at optical and near Key words: Galaxies: individual: NGC 128 – Galaxies: ellipti- infrared wavelengths (Sec. 4), present the results of Hα and cal and lenticular, cD – Galaxies: photometry – Galaxies: kine- NIR observations (Sec. 5 and Sec. 6), analyze the far infrared matics and dynamics – Galaxies: structure – Galaxies: general IRAS data (Sec. 7), and briefly summarize the whole datasets (Sec. 8). The technical solutions adopted for the data reduction are given in the Appendix. 1. Introduction The connection between the boxy/peanutmorphologyof galac- 2. Morphology tic bulges and the presence of a bar is difficult to prove obser- The peculiar edge-on S0 galaxy NGC 128 is the domi- Send offprint requests to: M. D’Onofrio nant member of a group which includes NGC 126 (E/SB0), ⋆ Based on observations taken at ESO La Silla and at the Special NGC 127 (Sa), NGC 130 (E5), a faint anonymous Sa galaxy Astrophysical Observatory (SAO) of the Russian Academy of Sci- 5.′6 North and 9.′5 preceding NGC 128, and possibly NGC 125 ences (RAS). (S0 pec) (Zwicky et al. 1965). The membership of NGC 125 is 2 D’Onofrio et al.: The peculiar galaxy NGC 128 controversial since its recession velocity is higher than average by ∼ 1000 km s−1. Burbidge & Burbidge (1959), Hodge & Merchant (1966), and Bertola & Capaccioli (1977, BC77) provided the first data for NGC 128 and its group. The galaxies of this group are late Ellipticals and early Spirals, and the recession velocities are in the range 4200–4600 km s−1. NGC 128 is connected by a bridge to NGC 127, and according to BC77 a set of filaments protrudes southwards to NGC 126. The galaxy NGC 125 is surrounded by a large ring (BC77 estimated a diameter of ∼ 70 kpc) which is asymmetrically placed with respect to the center of the galaxy. NGC 128 is classified as BS-I in the list of de Souza & dos Anjos (1987). The peculiar peanut shape of the bulge is clearly visible even in the innermost isophotes: the bulge appears squared by four symmetric bumps, forming an X-structure with arms at ∼ 45◦ from the major axis of the galaxy and extended, in projection, for ∼ 20′′ (5.4 kpc)1. The peculiar morphology is not due to extinction effects (see next sections). As suggested by Pfenniger & Friedli (1991) the X-structure is likely an optical illusion. We clearly see this effect in the Fig. 1. B-band maps of the O-C residuals for NGC 128: Up- original frame by changing the cuts: a thin disk and a small, per panel: the result of the unsharp masking technique; Middle and approximately round, bulge are seen in the center at the panel: the X-structure and the disk of NGC 128 after the sub- higher counts, while an increase of the thickness of the disk traction of a model of the bulge component, obtained by fitting is apparent at lower counts. Such “flaring” seems to originate the inner isophotes with ellipses; Bottom panel: the result of the X-structure. The impression one has is that of looking to a the subtraction of a model of the bulge and disk component ′′ “papillon”. The stars seem pulled out of the disk, the maximum (see text). North is on the left, West is up. The image is ∼ 100 effect taking place at ∼ 11 arcsec, corresponding to ∼ 3 kpc. in the N-S direction. The galaxy is seen approximately edge-on. We derived a log(a25/b25) ratio of 0.76, a value which is in relative good ness of the disk in the outer region is possibly the result of the agreement with that found by Guthrie (1992) in his sample of bulge subtraction (we verified this fact by simulating an edge- edge-on galaxies for the S0 class. The observed major axis di- on S0 galaxy and subtracting the bulge component). Using the −2 ameter is ∼ 50 kpc (at µB = 26.0 mag arcsec ), and the thick- unsharp masking technique (Fig. 1, upper panel) we were able ness along the minor axis ∼ 21 kpc. to confirm the bending of the disk on both sides, but not the The disk appears bended toward West on both sides, either flaring of the outer disk. The X-structure is obviously not visi- in the visual and in the NIR images, in particular toward the ble in such image. South-West direction, where the bending starts at r = 37′′ (10 Notice that in Fig. 1 (middle and lower panels) the disk is kpc) from the center. The peaks of the light distribution along fainter along the North direction. Here there is a strong absorp- cuts perpendicularto the disk major axis have a maximum shift tion in correspondenceof the encounterof the disk of NGC 128 of 7′′ (1.9 kpc). with the arm of NGC 127. We tempted to highlight the peculiar morphology of Since the X-structure is the result of the subtraction of a NGC 128 in different ways using the images with the best see- model built with elliptical isophotes on a galaxy with a pro- ing and higher S/N ratio (the B-band frames). First we sub- nounced boxy shape, we realized a new 2D model of the galaxy tracted a model of the bulge component of the galaxy (Fig. 1, taking into account the boxiness of the bulge. The 2D surface middle panel) obtained by fitting with ellipses the inner isopho- brightness distribution of the entire galaxy (within µB < 25 tal contours of the galaxy. In the residual map we identify the mag arcsec−2, masking the center, the region of the disk af- X-structure (in white color) and the disk component, which ap- fected by the interaction with NGC 127, and the distorted outer pears thicker in the outer region.
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