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The Ursa Major Supercluster of Galaxies: II

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The Ursa Major Supercluster of Galaxies: II Astronomy Letters, Vol. 27, No. 6, 2001, pp. 345–352. Translated from Pis’ma v Astronomicheskiœ Zhurnal, Vol. 27, No. 6, 2001, pp. 403–411. Original Russian Text Copyright © 2001 by Kopylova, Kopylov. The Ursa Major Supercluster of Galaxies: II. The Structure and Peculiar Velocities F. G. Kopylova and A. I. Kopylov* Special Astrophysical Observatory, Russian Academy of Sciences, Nizniœ Arkhyz, Karachaevo-Cherkessia, 357147 Russia Received October 30, 2000 µ Abstract—Kormendy’s relation ( e–logRe) is used to investigate the structure of the compact Ursa Major supercluster of galaxies (11h30m + 55°, cz = 18 000 km s–1); this relation allows the distances of early-type galaxies to be estimated. The relative distances of 13 clusters in the supercluster and their peculiar velocities are determined with a mean statistical accuracy of 6%. In general, the supercluster obeys the Hubble relation between radial veloc- ity and distance. However, there is reason to suggest that the supercluster consists of two subsystems with mean radial velocities of 16 200 and 19 700 km s–1. For a velocity dispersion in the subsystems of ~1100 km s–1, the fact that each of them is gravitationally bound is not ruled out. © 2001 MAIK “Nauka/Interperiodica”. Key words: galaxies, groups and clusters of galaxies INTRODUCTION (E and S0) galaxies, which dominate at the cluster cen- ter, as this method. The distribution of galaxies and clusters of galaxies is revealed by redshift measurements. Its pattern is dis- Using this purely photometric method, we investi- torted by peculiar motions additional to the Hubble gated the structure and peculiar motions in various sys- expansion that arise as space structures grow due to tems of galaxies: in two compact superclusters of gal- gravitation. The most contrasting structures on scales axies and in the system of galaxy clusters surrounding of 30–300 Mpc are superclusters of galaxies. It follows a void (Kopylov and Kopylova 1998). Our sample from galaxy redshift surveys that the sizes of superclus- includes 39 clusters, in which we measured ~440 gal- 16 axies in total. Our study of the compact Corona Borea- ters reach 20–100 Mpc and their masses are ~10 M( –1 –1 lis supercluster (Kopylova and Kopylov 1998) shows (below, we use H0 = 50 km s Mpc and q0 = 0.5). The growth of nonuniformities in the matter distribution at that the nucleus of this system composed of eight rich the linear stage of the development of gravitational Abell clusters is gravitationally bound and is at the instability or at the onset of gravitational collapse in the stage of gravitational collapse. Preliminary estimates of most compact systems can be traced by the distribution peculiar cluster motions around the void revealed a small and motion of clusters in superclusters. outward-directed motion of clusters (Kopylov and Kopy- lova 1998). Here, our goal is to determine the structure The observationally determined peculiar velocities (along the line of sight) of the second compact superclus- of galaxy clusters generally do not exceed 1000 km s–1. ter in the northern sky, Ursa Major (11h30m + 55°, One might expect larger velocities in rare, compact, and cz = 18 000 km s–1). In comparison with our previous rich superclusters of galaxies, which exhibit elongation paper (Kopylov and Kopylova 1996), we made more along the line of sight if their distances are assumed to accurate measurements for a larger number of galaxies be directly proportional to the redshifts of their constit- and added two additional clusters (A1452 and A1507) uent galaxy clusters. The Ursa Major and Corona Bore- located on the periphery of the supercluster. alis superclusters in the northern sky are of greatest interest in this respect (Rood 1992). OBSERVATIONS For the component additional to the Hubble compo- AND PHOTOMETRIC MEASUREMENTS nent (peculiar velocity) to be separated from the directly observed velocity (cz), the positions of clusters Ursa Major is one of the nearest (z . 0.06) compact within the supercluster along the line of sight must be superclusters. Figure 1 shows the cluster positions in determined by a method independent of redshift deter- the sky in equatorial coordinates. As we see from the mination. We used Kormendy’s relation for early-type figure, the supercluster is a compact group of clusters, at least in projection onto the sky. The apparent density contrast of the system, if it is determined with respect to the number of Abell clusters in the surrounding * E-mail address for contacts: [email protected] region of ~200 Mpc in size, is 30. A more detailed 1063-7737/01/2706-0345 $21.00 © 2001 MAIK “Nauka/Interperiodica” 346 KOPYLOVA, KOPYLOV 62° The observational data were reduced with the PC VISTA (Treffers and Richmond 1989) and MIDAS A1507 (Munich Image Data Analysis System) (Grosbol 1989) 60° 18 200 packages. We also used the RING code (Georgiev 1991), which we adapted for surface photometry of gal- axies through circular apertures. The standard image 58° A1436 A1377 Anon4 A1291 processing procedures were applied: median-dark- 19 300 15 200 18 400 15 700 frame subtraction, flat fielding, and subtraction of the δ Anon3 sky background fitted by a second-degree surface. 56° 20 500 Anon1 21 000 Based on multi-aperture photometry, we determined Sh166 the asymptotic total magnitudes of galaxies. The total A1383 A1318 54° 15 400 17 100 Anon2 magnitude was then used to determine the effective 18 100 A1270 21 100 radius re at which the galaxy luminosity decreased by 20 700 µ 52° A1452 half and the effective surface brightness e at this radius 18 900 [see Kopylova and Kopylov (1998) for more details on this technique]. The photometric parameters were cor- 50° rected for seeing by the method described in Saglia 12.5 12.0 11.5 11h.0 et al. (1993). By comparing independent measure- α ments for 15 galaxies that we observed twice, we found µ m Fig. 1. The positions of clusters from the Ursa Major super- the rms measurement errors of e and logre to be 0 . 09 cluster in equatorial coordinates at epoch B1950. Cluster num- and 0.02, respectively. bers and mean radial velocities rounded off to 100 km s–1 are shown. Clusters from the catalog by Abell et al. (1989) are For several large galaxies with extended envelopes, marked by circled crosses; other clusters (Baier 1980; i.e., those of type cD (these include galaxies 61 in Shectman 1985) are marked by circles. Anon1, 157 and 97 in A1377, and 80 and 19 in A1318), we determined the parameters by fitting an r1/4 profile (de Vaucouleurs 1948) to the observed surface bright- description of the clusters in the supercluster and their ness profile. We had to do this, because the extended luminosity function can be found in Kopylov and envelopes of these galaxies were partially outside our Kopylova (2001), where the sample of objects (bright E images. and S0 galaxies in clusters) was drawn by using the B–R Our photometric and spectroscopic measurements color index. We determined the redshifts of galaxies 1 and clusters from the spectra taken in 1991–1993 with are given in Table 1. The table lists the following gal- a 1024-channel photon counter—the scanner (IPSC) axy parameters: Abell cluster numbers; galaxy num- mounted at the Nasmyth-1 focus of the 6-m telescope bers [all numbers correspond to those from Kopylov and Kopylova (2001)]; galaxy equatorial coordinates at on the SP-124 spectrograph (Drabek et al. 1986; epoch B1950; total (asymptotic) Rc magnitudes; helio- Afanas’ev et al. 1986). The observations were carried –1 –1 centric radial velocities, in km s ; effective galaxy out with the B1 grating (600 lines mm ) in the spec- radii, in arcseconds, corrected for seeing; effective sur- tral range 3600 to 5500 Å with a dispersion of face brightnesses (mag arcsec–2) at the effective radius 1.9 Å per channel. The accuracy of measuring radial corrected for seeing; and mean effective surface bright- –1 velocities was 100–200 km s . nesses (mag arcsec–2) within the effective radius cor- We determined the photometric parameters for rected for seeing. In A1377, the radial velocities for the four galaxies marked in Table 1 by an asterisk were 107 galaxies in 13 clusters from direct (Cron–Cousins) R c taken from Humason et al. (1956). In the same cluster, images obtained with the 6-m Special Astrophysical we give the coordinates for two other galaxies, desig- Observatory (SAO) telescope in 1992–1994 and with nated as D45 and D47, from Dressler (1980). They are a 1-m telescope in 1996–1998. The images were located near the region we studied (Kopylov and Kopy- obtained at a mean seeing of 1″. 7 ± 0″. 3 measured as the lova 2001) and were additionally included in the list for FWHM profiles of stars. We used an ISD015A 520 × CCD photometry, because they were classified by 580 CCD array with a pixel size of 18 × 24 µm, which Dressler (1980) as S0 and E, respectively. corresponded to angular sizes of 0″. 28 × 0″. 37 and Data for the two additional clusters, A1452 and 0″. 154 × 0″. 205 on the 1-m and 6-m telescopes, respec- A1507, which we have not studied previously, are pre- tively. The exposure time was 200 and 500 s on the 6- sented in Table 2. It gives the same parameters as those m and 1-m telescopes, respectively. For photometric in Table 1 and the coordinates of galaxies at epoch calibration, standard stars from Landolt (1992) were B1950. The radial velocities for the galaxies in A1452 observed several times during each night.
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