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Photometric Study of Polar-Ring Galaxies. III. Forming Rings

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Photometric Study of Polar-Ring Galaxies. III. Forming Rings A&A manuscript no. (will be inserted by hand later) ASTRONOMY AND Your thesaurus codes are: ASTROPHYSICS 03 (11.09.1 NGC 3808B; 11.09.1 NGC 6286; 11.09.2; 11.16.1) 30.9.2018 Photometric study of polar-ring galaxies. III. Forming rings V.P. Reshetnikov1, V.A. Hagen-Thorn2, V.A. Yakovleva2 1 Astronomical Institute of St.Petersburg State University, 198904 St.Petersburg, Russia 2 St.Petersburg State University, 198904 St.Petersburg, Russia Received 16 January 1996; accepted 29 March 1996 Abstract. We present the results of detailed surface pho- Whitmore et al. 1990 (PRC)) are symmetric objects in tometry of NGC 3808B and NGC 6286 - two spiral which the remnants of interacting galaxies are not mixed galaxies with possibly forming ring-like structures rotat- but stay in a quasi-stationary state for a long time, may ing around major axes of the galaxies. The formation of be comparable with Hubble time. Detailed investigation rings in NGC 3808B and NGC 6286 being accompanied of PRGs supply the new approaches to the study of such by accretion of matter on galactic disk results in some important problems as the shape of galactic potential, the interesting gasdynamical and stellardynamical effects in frequency of interactions and mergings, influence of inter- these galaxies. One can note, for instance, peculiar rota- actions on global structure of galaxies, on their nuclear tion curve of NGC 3808B gaseous disk; strong infrared and activity etc. Hα emission from the galaxies; bending and flaring stellar Probably the most important problem concerning disks in both galaxies. Our observations clearly illustrate PRGs is their origin. It is usually contended that the col- the possibility that polar-ring galaxies may be formed as lapse of single protogalactic cloud cannot create the object a result of matter accretion from one galaxy to another. with two nearly orthogonal large-scale kinematic systems and therefore in the history of such objects some second Key words: galaxies: interactions; photometry; NGC event (for instance, interaction or merging) has occured 3808B; NGC 6286 (Schweizer et al. 1983, Whitmore et al. 1987). From the other side, recent simulations by Curir & Diaferio (1994) seem to indicate that a single dissipationless collapse of rotating triaxial system can produce misaligned spins. Here we give the results of new observations of two can- 1. Introduction didates to PRGs from the PRC which obviously demon- The general picture of the observed part of the Universe strate the possibility of polar-ring galaxy formation as a has been in a marked degree due to the gravitational in- result of interaction between galaxies. arXiv:astro-ph/9608100v1 15 Aug 1996 teractions and mergings between galaxies. Observations Throught this paper the value H0 =75 km/s/Mpc is and model calculations show that mutual interactions and adopted. accretion may change such fundamental galaxy character- istics as mass and luminosity distributions, morphological 2. Observations and reductions type, the rate of star formation, etc. Galaxies with polar rings (PRGs) keep aloof among The photometric observations of galaxies were carried the objects which traditionally are considered as a result out in 1992 and 1994 in the prime focus of the 6-m of interaction between galaxies. Indeed, close encounters telescope of the Special Astrophysical Observatory of are the reason of disturbance of the galaxy form and ap- Russian Academy of Sciences. The photon collector was × × pearance of asymmetric structures such as bridges, tails virtual phase CCD of 520 580 pixels, each 18 24 µm × ′′ and so on, while the merging between the galaxies is con- (0.15 0.2 ) (Borisenko et al.1991). Reimaged optics, that × ′ sidered to result in the origin of smoothed elliptical-like realized a field of view 4.5 6.9 with angular resolution × objects where the remnants of merged objects are well 0.53 0.71”, was used during our observations of NGC mixed. To the contrary, ”classic” PRGs (category A in 6286. Observations of NGC 3808 were obtained without reimaged optics − with a field of view 1.3 × 2.0′ and reso- Send offprint requests to: V.P. Reshetnikov lution 0.15 × 0.2”. The data were acquired with standard 2 V.P. Reshetnikov, V.A. Hagen-Thorn, V.A. Yakovleva: Photometric study of polar-ring galaxies. Johnson B, V and Cousins R filters for NGC 6286, and in the case of NGC 3808B we observe the formation of with Johnson V and Cousins R, I filters for NGC 3808. polar ring as a result of mass transfer from the nearby Photometric calibration was accomplished using repeated galaxy. This suggestion is confirmed by spectral observa- observations of the BV RI standard stars from Landolt tions which have shown that the main body of the galaxy (1983) and Smith et al. (1991). The seeing during our ob- rotates around minor axis whereas the matter of twined servations was about 2′′. A log of observations is given arm moves around the major axis of the galaxy as in clas- in Table 1 (extinction corrected sky brightnesses in each sic PRGs (Reshetnikov & Yakovleva 1990). frame in magarcsec−2 are presented in the last column of the table). Reduction of the raw CCD data was made in standard manner (for details see Paper I - Reshetnikov et al. 1994). The ESO-MIDAS package (MIDAS User Guide 1994) was used. Fig. 1. Reproduction of NGC3808 from the Atlas of Peculiar Table 1. Observations Galaxies by Arp (1966). North is at the top, east to the left Object Data Band- Exp. Air- Sky pass (sec) mass mag. 3.1.1. Photometric characteristics Global photometric parameters of NGC 3808B are sum- NGC 3808 10/11.03.94 V 600 1.075 21.14 marized in Table 2 (the value of Bt in the table was derived R 300 1.079 20.66 from our Vt magnitude and colour index from Gavazzi et I 600 1.075 19.24 al. (1991): B − V = +0.65). There are some published results of photometric ob- NGC 6286 6/7.05.92 B 1000 1.049 21.94 servations of NGC 3808B. Tomov (1978) has found V = V 600 1.043 21.19 14.27 for the 54” aperture which covers almost whole R 300 1.040 20.58 galaxy. This value is more bright than that found by us (Vt =14.39) probably because of getting in the aperture the star, located to SW from the galaxy. Spectral observations of the galaxies were obtained Gavazzi et al. (1991) give the results of photoelectric earlier at the 1.93-m telescope of the Observatoire de observations of NGC 3808B with three various apertures. Haute-Provence, using the spectrograph CARELEC and The mean difference between these values and our mea- − ± the CCD TK512. For details of observations and reduc- surements for the same apertures is 0.05 0.02 (σ). In tions see Reshetnikov & Combes (1994) (RC). the work of Gavazzi & Randone (1994) the apparent mag- nitude in the V band within the elliptical isophote of 25 −2 mag arcsec is given: V25 = 14.61. Taking in mind the 3. Results and discussion mean difference between their V25 and total magnitudes 3.1. NGC 3808B (PRC D-19) in RC3 (+0.3 ± 0.2) we make the conclusion about good agreement between our Vt value and the data of Gavazzi NGC 3808 (Arp 87, VV 300) is M 51-type interacting dou- & Randone (1994). ble system, which consists of Sc spiral with Bt = 14.1±0.3 The isophotes of NGC 3808B in the V band are given (de Vaucouleurs et al. 1991, RC3) seen nearly face-on and in Fig.2. The main body of the galaxy is viewed practically a companion located at the end of spiral arm of the main edge-on. The twined arm become apparent as ”swelling” galaxy and seen edge-on. In what follows we shall refer of isophotes to NW and SE from the main body. Outside to the main galaxy as NGC 3808A and the companion as the main body the arm does not end but goes to NW NGC 3808B. The distance to the system is D =93 Mpc from its edge as far as ≈40” (18 kpc). In Fig.2 one can see (RC) and the angular separation between companions is faint (V =18.7) galaxy projected on the NE edge of NGC about 1.1’ (30 kpc). Our unpublished observations with 6- 3808B. We think this galaxy is background one seen here m telescope show that a radial velocity difference between by chance. However, it may be gravitationally bound with two galaxies is only 33 km/s. NGC 3808A,B but because of its non-distorted structure As one can see in Fig.1 where a contrast copy from it is located sufficiently far from the pair and does not the ”Atlas of Peculiar Galaxies” (Arp 1966) is given, the participate in strong gravitational interaction between A spiral arm of the main galaxy is not only drawn out to and B galaxies. the companion but twines it forming an unrolled spi- ral. For this reason Schweizer (1986) has supposed that V.P. Reshetnikov, V.A. Hagen-Thorn, V.A. Yakovleva: Photometric study of polar-ring galaxies. 3 Table 2. General characteristics NGC 3808B NGC 6286 D (Mpc) [RC] 93.0 76.5 Ag(B) [RC3] 0.00 0.02 Bt (± 0.10) 15.04 14.2 [1] (B − V )t +0.65 +0.75 ± 0.05 (V − R)t +0.48 ± 0.03 +0.50 ± 0.03 (R − I)t +0.46 ± 0.03 a (µB = 26) 0.77’ (20.7 kpc) 1.68’ (37.5 kpc) b/a (µB = 26) 0.36: 0.36: [2] µ0 18.5(V ) 20.4 (B) h 3.9” (1.8 kpc) 6.6” (2.5 kpc)[2] [3] [3] z0 2.2” (1.0 kpc) 3.8” (1.4 kpc) Vmax (km/s) 120±10 P ossible forming ring : M -18(V ) -18.4(B) B − V +0.5: V − R +0.4: +0.3: R − I +0.4: Vmax(km/s) 120 100: Ring-to-central galaxy ratio 0.1(V ) 0.2(B) (1) Gavazzi et al.
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