LARGE-SCALE STRUCTURE AND GALAXY MOTIONS IN THE LEO/CANCER CONSTELLATIONS I. D. Karachentsev1, (*) , O. G. Nasonova1 , V. E. Karachentseva2
arXiv:1502.04253v1 [astro-ph.GA] 14 Feb 2015
2 Main
1 Special Astrophysical Observatory of Russian AS, Nizhnij Arkhyz 369167, Russia Astronomical Observatory, National Academy of Sciences of Ukraine, Kiev, 03680 Ukraine
(Received November 14, 2014; Revised December 4, 2014) In the region of the sky limited by the coordinates RA = 7h. 0–12h. 0, Dec = 0◦ ...+20◦ and extending from the Virgo Cluster to the South Pole of the Local Supercluster, we consider the data on the galaxies with radial velocities VLG . 2000 km/s. For 290 among them, we determine individual distances and peculiar velocities. In this region, known as the local velocity anomaly zone, there are 23 groups and 20 pairs of galaxies for which the estimates of virial/orbital masses are obtained. A nearby group around NGC 3379 = Leo I and NGC 3627 as well as the Local Group show the motion from the Local Void in the direction of Leo cloud with a characteristic velocity of about 400 km/s. Another rich group of galaxies around NGC 3607 reveals peculiar velocity of about −420 km/s in the frame of reference related with the cosmic background radiation. A peculiar scattered association of dwarf galaxies Gemini Flock at a distance of 8 Mpc has the radial velocity dispersion of only 20 km/s and the size of approximately 0.7 Mpc. The virial mass estimate for it is 300 times greater than the total stellar mass. The ratio of the sum of virial masses of groups and pairs in the Leo/Can region to the sum of stellar masses of the galaxies contained in them equals 26, which is equivalent to the local average density Ωm (local) = 0.074, which is 3–4 times smaller than the global average density of matter. Keywords: galaxies: kinematics and dynamics—galaxies: distances and redshifts—galaxies: groups
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Introduction
and groups of galaxies, in the “lethargic” zones, where because of some reasons the process of star formation did not get triggered. Such dark elements of the large-scale structure (massive clumps, extended filaments), if they exist indeed, may manifest themselves both by the effects of weak gravitational lensing [9, 10] and by peculiar motions of nearby galaxies [11]. To determine the peculiar (non-Hubble) velocity of the galaxy, Vpec = VLG − H0 D, we have to measure its radial velocity relative to the centroid of the Local Group, VLG , and the distance D, adopting a fixed value of the Hubble parameter H0 . The field of peculiar velocities can be examined in most detail in the closest volumes, where the amount and quality of data on the galaxy distances is much higher than that in the distant volumes of space. In the series of previous studies we have reviewed the data on the velocities and distances of galaxies in three areas located along the equator of the Local Supercluster: the region Coma I [11] with VLG < 3000 km s−1 and coordinates RA = 11h. 5–13h. 0, Dec = +20◦ ...+40◦ , the region of Ursa Major [12] with VLG < 1500 km s−1 and RA = 11h. 0–13h. 0, ◦ ◦ Dec = +40 ...+60 , and the region of the Virgo Southern Extension [13] with VLG < 2000 km s−1
The modern cosmological paradigm assumes that the galaxy formation occurs in the areas of concentration of dark matter, to where the baryonic matter is inflowing and triggering the star formation processes. Within this concept, the apparent distribution of galaxies follows the distribution of dark matter, but with a somewhat smaller degree of contrast (the so-called biasing effect). The analysis of distribution of dark (virial) matter in the most nearby and well-studied part of the Universe with radial velocities of galaxies of VLG < 3500 km s−1 was conducted by Makarov and Karachentsev in [1, 2, 3]. The main and paradoxical result of this research is that the average density of dark matter in the Local Supercluster and its vicinity Ωm (local) = 0.08 ± 0.02 proved to be 3–4 times smaller than the global average density, Ωm (global) = 0.28–0.30 [4, 5]. The indications of low density of dark matter in the Local Universe have been already revealed [6, 7]. A survey of various explanations for the “missing dark matter” paradox can be found in [8]. One of them is a suggestion that a significant part of dark matter is stored in the space between the known clusters (*) Electronic
address:
[email protected]
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Figure 1: The distribution of galaxies of the Local Supercluster in equatorial coordinates. The Leo/Can region and the areas of our previous studies are highlighted in colors. and RA = 12h. 5–13h. 5, Dec = −20◦ –0◦ as well as the Bo¨ otes [14] zone with VLG < 2000 km s−1 and RA = 13h. 0–18h. 0, Dec = −5◦ ...+10◦ , extending perpendicular to the equator of the Local Supercluster. In the three areas considered, the estimates of virial average density of matter were in the range of Ωm (local) = 0.08–0.11, and in the Coma I region the existence of a dark attractor with a mass of about 2 × 1014 M⊙ at a distance of about 15 Mpc was suspected. The distribution of galaxies of the Local Supercluster with radial velocities VLG < 2000 km s−1 is presented in the equatorial coordinates in Fig. 1. The zone of strong extinction in the Milky Way (the Zone of Avoidance) is demonstrated by a patchy gray stripe. The regions we have previously studied—Coma I, Ursa Major, Virgo SE, Bo¨ otes, and the new area of our interest in the constella tions of Leo and Cancer with the coordinates RA = 7h. 0– 12h. 0, Dec = 0◦ ...+20◦ —are marked by dark rectangles.
optical sky survey [15]. About 40% of the Leo/Can region is covered by the ALFALFA sky survey in the 21 cm line conducted at the Arecibo radio telescope [16]. The Leo/Can belt in its entirety lies in the northern region of the H I Parkes All-Sky Survey (HIPASS) carried out at the Parkes radio telescope [17]. The abundance of data on radial velocities of galaxies, their photometry and H I line width made it possible to determine the distances to 600
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Figure 2: The distribution of 1918 Leo/Can objects from HyperLeda by radial velocity in the Local Group rest frame. The true 543 galaxies are shown in dark.
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Figure 3: The distribution of 543 galaxies in the Leo/Can stripe by radial velocity. The 290 objects with measured distances are marked in dark.
Leo/Can region by distance. Thirty-nine galaxies with high-accuracy distance estimates are marked in dark colors.
galaxies by the Tully–Fisher relation [18] and get the local field of peculiar velocities with high density. According to HyperLeda(**) , the region of h h ◦ RA = 7 . 0–12 . 0, Dec = 0 ...+20◦ contains 1918 objects with radial velocities in the Local Group rest frame of VLG < 2000 km s−1 . Their distribution according to the radial velocity is shown in Fig. 2. Most of the objects have near zero velocities, being the stars of our Galaxy. Our analysis of the HyperLeda data has shown that only 543 out of 1918 objects proved to be real galaxies. They are marked in Fig. 2 in dark. The sample of objects with VLG < 2000 km s−1 not only contains the stellar background objects but also a large number of different fragments of galaxies taken for individual objects in the SDSS. A large proportion of our initial list was also composed of the so-called “ghosts,” the dummy H I-ALFALFA survey sources with a low signalto-noise ratio, not identified with galaxies. Note that the NED database (http://ned.ipac.caltech.edu) contains yet more than 1000 fictitious “galaxies” with VLG < 2000 km s−1 in the considered region. All that indicates that the automatic use of the HyperLeda and NED data without their careful visual analysis can lead to serious distortions of the researched field of peculiar velocities of galaxies. Selecting the galaxies in our list, we also checked and updated their different characteristics. The summary of the data we used is shown in Table 1.(***) The columns contain: (1) the name of the galaxy or its number in the
known catalogs; (2) equatorial coordinates for the epoch J 2000.0; (3) radial velocity relative to the centroid of the Local Group with the parameters of the apex, used in NED; (4) the velocity of the galaxy relative to the threedegree CMB radiation with the parameters of the apex from NED; (5) integral apparent magnitude of the galaxy in the B-band according to NED or HyperLeda; in the presence of strong differences in the B values, we have resorted to our own visual apparent magnitude estimates based on the photometry of other galaxies of similar structure; (6) the half-width W50 of the 21 cm line, measured at 50% of the maximum intensity, the main sources of data on it were the ALFALFA [16, 19] and HIPASS [17] H I-surveys with the addition of data from later publications [20]; (7) distance to the galaxy in Mpc; (8) a method, with which the distance was measured: rgb—by the tip of the red giant branch; cep—by Cepheids; SN—by the supernova luminosity; sbf—by the surface brightness fluctuations; mem—by an obvious membership of galaxies in known groups; tf, TF, TFb—by the Tully–Fisher relation between W50 and the luminosity of the galaxy, where the letters tf mark the median distance estimates adopted from NED, the capital letters TF mark our D estimates by the relation from [21]: c MB = −7.27(log W50 − 2.5) − 19.99,
(1)
c where the width W50 is corrected for the inclination of the galaxy to the line of sight; as noted in [22], low luminosity galaxies rich in gas systematically deviate from relation (1) in need of the so-called “baryon correction”; in late-type galaxies (Ir, Im, Sm) with the H I-magnitude of m21 . mB , where m21 = −2.5 log F (H I) + 17.4, and F (H I) is the flux in the 21 cm line in Jy km s−1 , the hy-
(**) http://leda.univ-lyon1.fr (***) The
electronic version of the table is available from the VizieR database: http://cdsarc.u-strasbg.fr/ /viz-bin/qcat?J/other/AstBu/70.1
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drogen mass exceeds the mass of the star, therefore, in cases when m21 < mB , we determined the distances by the relation log D = 0.2(m − M ) − 5, (2)
ulated groups, and the bottom panel presents in a larger scale, the region, occupied by the nearby NGC 3379 and NGC 3627 groups. The radial velocities of galaxies are marked according to the density scale, shown between the panels. The members of the richest groups are connected by lines with the corresponding main galaxy of the group. As one can see, most of the galaxies with radial velocities VLG < 1000 km s−1 are located in the left upper corner of the studied area immediately adjacent to the west border of the Virgo Cluster. Galaxies with the velocities VLG > 1500 km s−1 dominate the right half of the general Leo/Can map. Figure 7 presents the distribution of galaxies in this area by the distance according to the scale located under the top panel. The bottom panel shows the behavior of the running median with the averaging window of 0h. 5. The distribution of galaxies by the distance looks quite spotty. However, in the area adjacent to the Virgo Cluster (RA > 10h. 4), the average distance of galaxies of the Leo/Can stripe approximately corresponds to the distance of the cluster itself of about 17 Mpc. The typical distances of galaxies in the median zone RA = 8h. 3–10h. 3 exceed 25 Mpc, which is probably due to the presence of a chain of distant groups (NGC 2648, NGC 2894, NGC 2962, NGC 3023) crossing this zone diagonally. In the rightmost region of Fig. 7, the number of galaxies with measured distances is not large, but an unusual diffuse structure stands out among them. We called it the Gemini Flock. Seven galaxies it contains are connected in the figure by the common perimeter. The members of this “flock” are dwarf galaxies with active star formation, they all have anomalously low radial velocities of about 180 km s−1 and rgb distances of around 8–9 Mpc. B. Tully [24] was the first to address this system as an association of four dwarfs. Then three more members were attributed to it [25, 26], two of which were recently discovered and studied in the SHIELD survey [26]. As follows from the data of Table 1, about 80% of distance estimates are inferred by the Tully–Fisher method. The accuracy of the method for normal luminosity galaxies is about 0m. 4, or approximately 20%. When applied to dwarf galaxies, the accuracy of the method decreases because of uncertainty of the W50 correction for the inclination of the galaxy and other factors. However, when averaged over many members of one group its average distance can be determined by the TF-method with quite an acceptable accuracy. Distance estimates via the rgb, cep, SN and sbf methods yield the accuracy 2–4 times better than the TF-method, i.e., one measurement made by the “exact” method is statistically equivalent to about 5–15 TF estimates. However, we encountered cases where the distance estimate made by an accurate method significantly differed from the TF-estimates for the other mem-
using the value of m21 instead of mB ; two dozens of such gas-rich galaxies were marked with TFb; (9) the morphological type of galaxies we have determined regardless of the NED and HyperLeda data; (10) the name of the brightest galaxy in the group to which a given galaxy belongs according to [1, 2, 3]. The distribution of 543 galaxies of our sample by the radial velocities VLG is shown in Fig. 3. Galaxies with individual distance estimates are marked in black. The last interval of the histogram VLG = 2000–2100 km s−1 captured several galaxies owing to the differences in the parameters of the apex in NED and HyperLeda. As shown in Fig. 3, the relative number of galaxies in our sample with known distances and peculiar velocities is quite large, but their fraction systematically decreases with increasing radial velocity (distance). Figure 4 shows the distribution of 290 galaxies in the Leo/Can region by the distance estimates. Thirty-nine galaxies are marked in black, the distances to which are measured by the rgb, cep, SN, sbf methods with an error of approximately 5–10%. A sharp peak in the histogram falls on the nearby group members: NGC 3379 = Leo I and NGC 3627 with the distances of about 10–11 Mpc. The predominant contribution to the broader secondary maximum at D = 18–32 Mpc is given by the groups around the NGC 2962, NGC 3166, NGC 3227, NGC 3686, and NGC 3810 galaxies. The map of the distribution of galaxies in the Leo/Can stripe by the morphological types is presented in Fig. 5. The early-type E-S0a galaxies, spiral Sa–Sm galaxy types and late-type Irr, Im, BCD objects are marked by the circles of different density. The low luminosity galaxies with MB > −17m. 0 are illustrated by small circles. According to the well-known general tendency, late-type dwarf systems are distributed more uniformly than the galaxies of normal luminosity. Most of the early-type galaxies are concentrated in groups. However, the isolated E and S0 galaxies are found even among the field galaxies, generally having low luminosity and emission features (UGC 5923, UGC 6233, IC 676, IC 745). The presence in this region of a compact isolated dE-galaxy CGCG 036-042 = PGC 02947 has been the subject of special discussion in [23]. The panorama of the distribution of galaxies in our sample by the equatorial coordinates and radial velocities relative to the centroid of the Local group is shown in Fig. 6. The top panel of the figure represents the entire the studied area, indicating the names of the most pop-
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Figure 7: The distribution of galaxies in the Leo/Can by distance according to the presented scale. The bottom panel shows the behavior of the median distance along the RA with the window of 0h. 5. bers of the same group. For example, the distance to NGC 3626 based on the fluctuations of surface brightness, 20.0 Mpc [27], looks understated compared with the average distance of the other members of the group, 26.3 Mpc. The obvious reason for underestimating the sbf-distance is caused by the presence in this Sa galaxy of dust bands that lead to an overestimation of the measured brightness fluctuations. The other example is the Sc-galaxy NGC 3389, where the distance 32.8 Mpc by SN Ia [28] proved to be 10 Mpc larger than that found by certain other methods. Both these galaxies are prominent by large peculiar velocities that are cancelled out by the use of alternative distance estimates.
density scale, which in the first case covers the range of −2000 km s−1 to +800 km s−1 , and in the second case—of −1400 km s−1 to +1400 km s−1 . The broken lines under the panels Vpec show the variation of the median peculiar velocity along the stripe with a window of 0h. 5. With an average distance of galaxies of around 25 Mpc and distance measurement error by the Tully–Fisher method of about 20%, the expected error in the estimate of peculiar velocity is approximately 360 km s−1 . The observed variations of Vpec are significantly higher than this value. In the system of the Local Group the median peculiar velocity remains negative throughout the RA range from the Virgo Cluster to the region of the Milky Way at high supergalactic latitudes, varying from −300 km s−1 to −700 km s−1 . This fact is known as the local velocity 3 Peculiar motions of galaxies anomaly phenomenon [29], which is explained by the motion of the Local Group to the Virgo Cluster (12h. 5, +12◦) in the Leo/Cancer region at a velocity of approximately 190 km s−1 and the recesThe field of peculiar velocities of galaxies in the sion from the expanding Local Void in the direction of stripe considered at the Hubble parameter of (7h. 0, −3◦ ) at approximately 260 km s−1 [30]. The volume H0 = 72 km s−1 Mpc−1 is shown in Fig. 8. The up- of space and the number of galaxies involved in this motion per half of the figure corresponds to peculiar motions remains rather uncertain. relative to the centroid of the Local Group, the bottom In the frame of reference related to the microwave rahalf—relative to the three-degree microwave radiation. diation, the median peculiar velocity varies symmetrically The marking of peculiar velocities corresponds to the from +200 km s−1 to −200 km s−1 . The positive values of
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Table 2: Characteristics of galaxy groups Group
Nv
hVLG i, km s−1
hV3K i, km s−1
D, Mpc
σv , km s−1
Rh , kpc
log M ∗ , [M⊙ ]
log MH , [M⊙ ]
log MH /M ∗
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NGC 2648 NGC 2775 NGC 2894 NGC 2962 NGC 2967 UGC 5228 NGC 3023 NGC 3020 NGC 3049 UGC 5376 NGC 3166 NGC 3227 NGC 3338 NGC 3379 NGC 3423 NGC 3521 NGC 3596 NGC 3607 NGC 3626 NGC 3627 NGC 3640 NGC 3686 NGC 3810 Mean
8 9 7 10 6 4 5 3 3 4 10 6 7 36 4 3 3 45 5 20 14 10 5 10
1933 1249 1952 1778 1654 1683 1667 1240 1297 1847 1104 1054 1105 702 850 593 1009 928 1387 697 1240 1057 844 1255
2348 1740 2483 2304 2262 2231 2222 1723 1805 2393 1742 1495 1594 1198 1389 1160 1483 1377 1833 1182 1785 1508 1328 1765
36.0 26.9 39.6 31.6 35.8 32.7 28.8 30.2 30.2 45.3 20.5 25.7 20.1 10.8 23.1 10.7 14.0 25.0 25.6 10.8 27.2 21.9 17.7 25.7
55 89 50 53 62 40 21 45 15 66 44 74 50 193 21 37 42 115 86 136 134 91 43 68
128 296 458 161 507 188 35 44 144 253 126 128 112 191 570 132 41 471 187 201 252 175 360 224
11.09 11.37 11.32 10.99 11.03 10.31 10.44 10.24 10.29 10.87 11.36 11.27 10.77 11.53 10.64 11.10 10.13 11.77 11.06 11.47 11.34 10.97 10.67 10.86
11.98 12.99 12.23 11.94 12.75 11.90 11.40 11.53 11.31 12.23 11.97 12.50 11.05 13.10 12.14 12.52 11.43 13.29 12.75 12.96 12.66 12.65 12.12 12.23
0.89 1.62 0.91 0.95 1.72 1.59 0.96 1.29 1.02 1.36 0.61 1.23 0.28 1.57 1.50 1.42 1.30 1.52 1.69 1.49 1.32 1.68 1.45 1.28
2 2 4 6 1 2 3 2 1 1 5 5 3 14 4 2 0 12 4 15 4 5 5 4
32.78 32.15 32.99 32.50 32.77 32.57 32.30 32.40 32.40 33.28 31.56 32.05 31.52 30.18 31.82 30.15 30.73 31.99 32.04 30.09 32.17 31.70 31.24 31.89
0.10 0.10 0.10 0.32 – 0.05 0.17 0.06 – – 0.35 0.27 0.33 0.31 0.25 0.00 – 0.28 0.39 0.38 0.08 0.37 0.23 0.22
Vpec (3K) in the area 10h. 5–12h. 0 are mainly due to two rich nearby groups around NGC 3379 and NGC 3627, which are moving away from us to the Virgo Cluster, revealing a positive velocity component along the line of sight relative to the observer. Note that the Bo¨ otes stripe, which is located on the other side of Virgo and extends up to the Local Void, also clearly demonstrates the effect of galaxy infall onto the Virgo Cluster [14]. According to the analysis made in [30], the pattern of motions in the Leo/Can region roughly looks like an approach of two elements of the local large-scale structure: the Local Volume and the Leo cloud with the mutual velocity of about 500 km s−1 . New mass measurements of radial velocities and distances of galaxies in the Leo/Can confirm the existence of nearby large-scale flows of galaxies with amplitudes that are comparable to the virial velocities in rich clusters.
columns contain the following main characteristics of the groups: (1) the name of the main galaxy; (2) the number of members with measured radial velocities; (3, 4) the average radial velocity of the group (km s−1 ) relative to the centroid of the Local Group and the three-degree blackbody radiation; (5) the distance to the group (Mpc), corresponding to the mean modulus (m − M ) of its members; (6) radial velocity dispersion (km s−1 ); (7) mean harmonic radius of the group (kpc); (8) logarithm of the total stellar mass of the group, estimated from the luminosity of galaxies in K-band assuming M ∗ /LK = 1 × M⊙ /L⊙ ; (9) logarithm of the projection (virial) mass of the group, which characterizes the mass of the group’s halo MH , Mp = (32/πG)(N − 3/2)−1
N X
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i=1
where ∆Vi and Ri are the radial velocity and projection distance of the i-th member of the group relative to the 4 Galaxy systems in the center of the group [31], N is the number of members, and G is the gravitational constant; (10) logarithm of the Leo/Cancer region projection to stellar mass ratio; (11) the number of group The galaxy clustering algorithm used in [1, 2, 3], led to the members with distance estimates; (12, 13) the average disdetection in the studied area of 23 groups of galaxies, most tance modulus and the mean square scatter of moduli. of which have been previously known. Taking into account The last line of the Table contains the mean values of the the new data on the radial velocities and galaxy distances, presented parameters. the list of these groups is shown in Table 2. The Table 8
4.1
NGC 3379 = Leo I and NGC 3627 For example, some groups of galaxies around NGC 2962, NGC 2967, UGC 5228, and NGC 3023 have similar radial groups velocities and distance estimates. All these four groups are also associated with the NGC 2974 group, which is located outside the southern boundary of our area. For obvious reasons, the dynamic analysis of such hierarchical structures is facing difficulties.
Both groups located at a distance of 10.8 Mpc are the closest and richest systems in the Leo/Can region. The recent measurements of distances to the main galaxies in these groups by rgb: 10.7 Mpc and 10.8 Mpc [32] are in a remarkable agreement with the data in Table 2. The general view of both groups is shown in the bottom panel of Fig. 6. The Leo I group contains a significant amount of E, S0, dSph-type galaxies, indicating its advanced evolutionary status. The literature lists several estimates of the Leo I group virial mass: 0.72 × 1013 M⊙ [33], 1.7 × 1013 M⊙ [1] and 1.7 × 1013 M⊙ [34], which are in good agreement with the mass estimate 1.26 × 1013 M⊙ in Table 2. A compact group NGC 3338 with an average radial velocity of VLG = 1105 km s−1 and the distance of 20.1 Mpc is projected at the north-western outskirts of Leo I. An association of members of this more distant group with the Leo I members would bring an asymmetry in the velocity profile of the Leo I group and overestimate the mass of its halo. Another feature of the Leo I group is the presence of a hydrogen ring with the diameter of about 200 kpc at it center [35]. Being projected on dwarf dSph–members of the group, H I-clouds lead to fictitious radial velocities of the dwarfs. The neighboring group NGC 3627 has a slightly lower halo mass and a smaller percentage of the early-type galaxies. A notable feature of this group is a dwarf galaxy of extremely low surface brightness AGC 215414, where more than 95% of baryons are contained not in the stellar component but rather in its gaseous component [36, 37]. The radius of the “zero velocity sphere” for the NGC 3379 and NGC 3627 groups is R0 ≃ 1.8 Mpc, which is higher than the projection distance between the group centers. We can conclude from this that both groups will eventually merge into a single dynamic system.
4.4
Gemini Flock
In the Leo/Can region there are 13 galaxies with radial velocities VLG < 300 km s−1 . In addition to the four members of the Local Group (Leo-T, Segue-1, Leo-I, Leo V) and its two neighboring dwarfs (Sex B, Leo P), the remaining 7 objects with such velocities are concentrated in the small area of the sky that occupies 1/10 of the studied area. The probability of such an event is approximately 10−6 . Taken the nonrandom nature of this configuration, we obtain a very strange, ephemeral system containing dwarf galaxies only. With the mean radial velocity hVLG i = 190 km s−1 the average distance to this group is 8.5 Mpc, hence, it is approaching the Local Group at a peculiar velocity of −423 km s−1 . This “flock” of galaxies in the Gemini constellation has a radial velocity dispersion σv of only about 20 km s−1 and the projection radius of about 5◦ , or 740 kpc. The virial mass of the group of Mvir ∼ 3 × 1011 M⊙ corresponds to these parameters. At the total stellar mass of the group of M ∗ = 0.96 × 109 M⊙ the virial-to-stellar mass ratio reaches Mvir /M ∗ ≃ 300, i.e., the average density of its dark matter is close to Ωm ≃ 1. However, the obtained values should be rather considered as formal, since the crossing time for such a loose system exceeds the age of the Universe by 2.5 times, meaning that the members of the Gemini Flock cannot be linked with each other in a causal way. An exception is a close pair UGC 3974 and KK 65 with the radial velocity difference of 10 km s−1 and the projection distance of the components of 38 kpc. Note that in the transition to the 4.2 NGC 3607 group reference system of the cosmic microwave radiation, the According to Tully [38], this group, along with the radial velocity dispersion of the group members increases NGC 3686 group and other more northern groups, is a up to σ = 55 km s−1 , while the average peculiar velocity v member of a scattered Leo cloud association number 21- drops to V (3K) = −73 km s−1 (i.e., the system is pracpec 1. As we can see from the bottom panel of Fig. 6, there tically at rest with respect to the CMB). is a subgroup of galaxies (NGC 3454/55/57) on the western side of this group, which is probably in the process of 4.5 Pairs of galaxies merging with the main body of the group. By its luminosity and virial mass, the NGC 3607 group is the most From the list of 509 pairs of galaxies in the Local Supersignificant object in the Leo/Can region. cluster [2], 20 pairs are located in the Leo/Can region. Their main characteristics are presented in Table 3, the columns of which contain: (1) the names of the pair com4.3 Other groups ponents; (2, 3) the average radial velocity relative to the What is noteworthy, some groups of galaxies classified centroid of the Local Group and relative to the CMB rain [1] as dynamically isolated are in fact associated with diation; (4) the radial velocity difference; (5) the average each other, forming hierarchical higher-level structures. 9
Table 3: Characteristics of pairs of galaxies ∆V12 , km s−1
D, Mpc
R12 , kpc
log M ∗ , [M⊙ ]
log MH , [M⊙ ]
log MH /M ∗
ND
σ(m − M ), mag
(3) 476
(4) 10
(5) 8.0
(6) 38
(7) 8.63
(8) 9.65
(9) 1.02
(10) 2
(11) 0.01
1860
2216
9
39.2
540
8.92
10.71
1.79
1
–
1954
2307
43
29.8
57
9.57
11.09
1.52
1
–
1832
2283
3
42.0
516
9.05
9.74
0.69
2
0.25
1776
2248
3
27.0
343
10.05
9.56
−0.49
2
0.49
1308
1806
10
25.5
36
8.36
9.63
1.27
2
0.17
1142
1694
86
22.8
42
10.44
11.56
1.12
1
–
1623
2162
31
35.0
129
10.61
11.16
0.55
2
0.23
1599
2151
21
21.2
232
9.75
11.08
1.33
1
–
1918
2360
52
43.0
110
10.46
11.55
1.09
2
0.16
1231
1714
15
31.6
271
10.03
10.86
0.83
2
0.30
1954
2504
6
31.2
350
10.03
10.17
0.14
2
0.28
1000
1547
26
21.3
53
9.79
10.62
0.83
1
–
1588
2158
38
20.8
24
8.78
10.63
1.85
1
–
857
1414
12
18.6
48
8.57
9.91
1.34
1
–
1219
1740
9
24.1
26
9.62
9.40
−0.22
2
0.13
1513
2052
132
21.0
18
10.15
11.58
1.43
1
–
1419
1959
6
19.4
161
9.34
9.84
0.50
–
–
875
1381
18
16.1
255
10.56
10.99
0.43
2
0.28
818
1345
43
11.2
9
8.28
10.28
2.00
–
–
1383
1876
29
25.4
163
9.55
10.50
0.95
1.6
0.23
Name
hVLG i, km s−1
(1) UGC 3974 KK 65 KK 67 KKH 43 IC 2329 P 1590056 P 1331483 A 182493 UGC 04524 NGC 2644 A 193802 SDSS 0944 NGC 3044 PGC 135730 AGC 192959 NGC 3055 LSBCL 1-099 Ark 227 UGC 05401 UGC 05403 UGC 05633 UGC 05646 NGC 3246 VIII Zw 081 UGC 5708 SDSS 10313 MGC 0013223 PGC 032664 PGC 135768 PGC 032687 AGC 213796 PGC 034135 UGC 06306 NGC 3611 PGC 034965 AGC 214317 IC 2828 NGC 3705 PGC 1218832 PGC 1218144 Mean
(2) 165
hV3K i, km s−1
distance of the components; (6) projection separation between the components; (7, 8) the total stellar mass and 2 orbital mass, Morb = (16/πG) ∆V12 R12 ; (9) the orbitalto-stellar mass ratio; (10) the number of components with an individual distance estimate; (11) the difference in distance moduli of the pair components. The last row of the Table contains the mean values of the parameters for the binary systems. As follows from these data, a typical pair of galaxies has the radial-velocity difference of the components of approximately 30 km s−1 , the projection distance between them is approximately 160 kpc and the halo mass (orbital mass) to the stellar mass ratio of about 9. In the case of pairs of galaxies, as in the case of groups, most of the distance estimates were made by the Tully–Fisher method, the error of which is taken as σ(m − M ) ≃ 0m. 4. The mean squared distance moduli difference in the last column of Tables 2 and 3 are 0m. 25 and 0m. 26 respectively. We can conclude therefore that the membership of galaxies in groups and pairs, selected using algorithm [1, 2], is convincingly confirmed by the
subsequent independent estimates of their distances. The catalogs of groups, triplets and pairs of galaxies in the Local Supercluster [1, 2, 3] obviously contain only a small percentage of fictitious members.
5
Hubble diagram in Leo/Can
The relation between the radial velocities and galaxy distances in the considered stripe is shown in Fig. 9. The top panel of the figure corresponds to the velocities in the Local Group rest frame, and the bottom panel depicts the velocities relative to the cosmic microwave radiation. The squares denote the groups of galaxies with the number of individual distance estimates nD ≥ 2, the triangles—pairs with measured distances for both components, small circles depict isolated galaxies with high accuracy distance estimates (rgb, cep, SN, sbf). The straight line on the panels corresponds to the Hubble parameter H0 = 72 km s−1 Mpc−1 . We can make the following conclusions from the presented data.
10
2500
14.5 Groups Pairs Single galaxies
2000
0. 28
14
=
Groups
Ω
N3607
13
1000
lg MH
VLG, km s−1
m
Pairs 13.5
1500
500
N2775
N3379 N3627
12.5
12
0 0
5
10
15
20
25
30
35
40
45
D, Mpc
11.5 2500 Groups Pairs Single galaxies
N3338
11
2000
10.5
V3K, km s−1
1500
10
9
9.5
10
10.5
11
11.5
12
12.5
13
lg M∗
1000
Figure 10: The relationship between the virial/orbital mass of the halo and the total stellar mass for groups and pairs of galaxies. The cross shows the ratio P P MH / M ∗ = 26 for the entire volume of Leo/Can. The solid line corresponds to the global value of MH /M ∗ = 97 at Ωm = 0.28.
500
0 0
5
10
15
20
25
30
35
40
45
D, Mpc
Figure 9: The Hubble diagram for groups and pairs of galaxies in the Leo/Can region with respect to the Local Group system (the top panel) and the CMB (the bottom panel). The average distance errors are shown by the horizontal segments.
rest in the 3K system. This distinguishes it from other nearby groups: NGC 3379, NGC 3627, and NGC 3521, which are located near the Supercluster’s equator. As an additional analysis shows, the volume around the Local Group, which recesses from the Local Void at a high peculiar velocity, has a flattened shape and is limited by the radius of about 10 Mpc.
• Almost all the groups and pairs of galaxies have radial velocities VLG substantially smaller than the ones expected at H0 = 72 km s−1 Mpc−1 . The typical velocity shift with respect to the expected amounts to Local matter density in Leo/Can ∆V ∼ 500 km s−1 . In the 3K system the deviations 6 −1 −1 from the line H0 = 72 km s Mpc are not so great, The distribution of 23 groups of galaxies from Table 2 which indicates the presence in the Local Group of a in the considered stripe based on their virial halo mass large peculiar velocity relative to the CMB. estimates and the total stellar mass is shown in Fig. 10 • Some groups and pairs with well-determined mean dis- in the logarithmic scale. In spite of the MH estimate tances have significant peculiar velocities relative to scatter, primarily caused by the projection factor, there the 3K system. In particular, rich nearby groups is a positive correlation between the mass of the dark NGC 3379 and NGC 3627 as well as a nearby triple and luminous matter in groups. It is expressed by the system NGC 3521 have peculiar velocities of about log MH = 1.15 log M ∗ − 0.30 regression, described in the +410 km s−1 , while the rich group NGC 3607 has figure by the dashed line. The ratio of the sum of orbital Vpec (3K) ≃ −420 km s−1 . Large peculiar velocities of masses of binary galaxies from Table 3 to the sum of their these groups are real, they are not caused by the errors stellar masses, illustrated by the triangle in the bottom left of distances measurements. corner of the figure, also follows the above dependence. • The closest to us diffuse group of dwarf galaxies Gemini Flock at a high supergalactic latitude is almost at 11
The total mass of the halo, contained in the groups and pairs of Leo/Can is 0.91 × 1014 M⊙ , and their total stellar mass is equal to 3.5 × 1012 M⊙ . The ratio of these P P values, MH / M ∗ = 26 is shown in Fig. 10 by a cross. As follows from the data of Table 1, only 51% of galaxies in the investigated area are the members of groups and pairs. However, the field galaxies are predominantly lowluminosity objects. The computation shows that the additional contribution of single galaxies in the total stellar mass is only 13%. They obviously bring some contribution to the total mass of dark matter too, but with little effect P P on the ratio of MH / M ∗ . According to [39], matter in the Local Universe is 4.5 × 108 M⊙ Mpc−3 at H0 = 72 km s−1 Mpc−1 , while the average cosmic density of matter Ωm = 0.28 at H0 = 72 corresponds to the value of 4.5 × 1010 M⊙ Mpc−3 . The ratio of these global values, equal to 97 is shown in Fig. 10 by the solid line. As we can see, all the systems of galaxies in the Leo/Can are located below the line Ωm = 0.28. P P The ratio MH / M ∗ = 26 for them corresponds to the local average density of Ωm (local) = 0.074, which is significantly lower than the global density. This result is in agreement with the estimate of the mean local density of virial masses we made in other parts of the structure of the Local Supercluster [11, 12, 13, 34]. Curiously, the line of regression log MH = ∗ 1.15 log M − 0.30 crosses the line Ωm = 0.28 at the values log(M ∗ /M⊙ ) ≃ 15.3 and log(MH /M⊙ ) ≃ 17.3, which roughly corresponds to the parameters of the “homogeneity cell” with the diameter of 200 Mpc. This fact may have a deeper meaning than a mere coincidence.
7
move towards the Leo cloud with the characteristic velocity of 400–500 km s−1 . Much of this velocity is caused by the motion of the Local flat “pancake” with the diameter of approximately 20 Mpc away from the center of the Local Void and a fall of the “pancake” towards the Virgo Cluster [30]. At a high supergalactic latitude SGB ≃ −50◦ at a distance of D ≃ 8 Mpc, an unusual diffuse group called the Gemini Flock was noted, consisting of seven dwarf galaxies. The characteristic size of the group of 740 kpc and the dispersion of radial velocities of 20 km s−1 lead to an estimate of its virial mass of Mvir ≃ 3 × 1011 M⊙ , which is 300 times larger than the total stellar mass. The total mass of the halo contained in all the groups and pairs of the Leo/Can region is 0.9 × 1014 M⊙ , and the ratio of this mass to the total stellar mass is 26. Such a ratio is much lower than the global value of MH /M ∗ = 97 which stems from the standard cosmological model with the parameter Ωm = 0.28. We conclude from these data that the problem of “missing dark matter” in the Local Universe yet continues to be an unsolved mystery. Acknowledgments This work was supported by the RFBR grant 13-02-90407 and the Foundation for Basic Research of Ukraine, grant No. F53.2/15. O. Nasonova thanks the non-profit Dmitry Zimin’s Dynasty foundation and the Russian Science Foundation (grant 14-12-00965) for the financial support.
References [1] D. I. Makarov and I. D. Karachentsev, Monthly Notices Roy. Astronom. Soc. 412, 2498 (2011).
Final remarks
The region of the sky in the Leo, Cancer and Gemini constellations, extending between the center of the Local Supercluster and its South Pole is known as the “local velocity anomaly.” We have built the map of the distribution of peculiar velocities of galaxies in it, using the distance estimates for 290 galaxies. We calculated more than a half of distance estimates by the Tully–Fisher method based on the data on the H I-line widths for the galaxies detected within the HIPASS and ALFALFA H I surveys. In the stripe sized 75◦ × 20◦ with a median depth of about 25 Mpc, there are 23 groups and 20 pairs of galaxies for which the virial/orbital mass are determined. In the reference frame related to the centroid of the Local Group, the majority of groups and pairs have negative peculiar velocities of about 500 km s−1 . Relative to the system of the cosmic microwave radiation, the velocities of most of the distant groups are small, but the nearby groups NGC 3379 and NGC 3627 along with the Local Group 12
[2] I. D. Karachentsev and D. I. Makarov, Astrophysical Bulletin 63, 299 (2008). [3] D. I. Makarov and I. D. Karachentsev, Astrophysical Bulletin 64, 24 (2009). [4] D. N. Spergel, R. Bean, O. Dor´e, et al., Astrophys. J. Suppl. 170, 377 (2007). [5] D. N. Spergel, R. Flauger, arXiv:1312.3313 (2013).
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[6] J. Vennik, Tartu Astron. Obs. Publ. 73, 1 (1984). [7] R. B. Tully, Astrophys. J. 321, 280 (1987). [8] I. D. Karachentsev, Astrophysical Bulletin 67, 123 (2012). [9] S. Vegetti, L. V. E. Koopmans, A. Bolton, et al., Monthly Notices Roy. Astronom. Soc. 408, 1969 (2010).
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[11] I. D. Karachentsev, O. G. Nasonova, and H. M. Cour- [25] I. D. Karachentsev, A. Dolphin, R. B. Tully, et al., Astronom. J. 131, 1361 (2006). tois, Astrophys. J. 743, 123 (2011). [12] I. D. Karachentsev, O. G. Nasonova, and H. M. Cour- [26] K. B. W. McQuinn, J. M. Cannon, A. E. Dolphin, et al., Astrophys. J. 785, 3 (2014). tois, Monthly Notices Roy. Astronom. Soc. 429, 2264 (2013). [27] J. L. Tonry, A. Dressler, J. P. Blakeslee, et al., Astrophys. J. 546, 681 (2001). [13] I. D. Karachentsev, O. G. Nasonova, and H. M. Courtois, Monthly Notices Roy. Astronom. Soc. 429, 2677 [28] B. R. Parodi, A. Saha, A. Sandage, and G. A. Tam(2013). mann, Astrophys. J. 540, 634 (2000). [14] I. D. Karachentsev, V. E. Karachentseva, and [29] R. B. Tully, E. J. Shaya, and M. J. Pierce, Astrophys. O. G. Nasonova, Astrophysics 57, 457 (2014). J. Suppl. 80, 479 (1992). [15] K. N. Abazajian, J. K. Adelman-McCarthy, [30] R. B. Tully, E. J. Shaya, I. D. Karachentsev, et al., M. A. Ag¨ ueros, et al., Astrophys. J. Suppl. 182, 543 Astrophys. J. 676, 184 (2008). (2009). [31] J. Heisler, S. Tremaine, and J. N. Bahcall, Astrophys. [16] M. P. Haynes, R. Giovanelli, A. M. Martin, et al., J. 298, 8 (1985). Astronom. J. 142, 170 (2011). [32] M. G. Lee and I. S. Jang, Astrophys. J. 773, 13L (2013). [17] O. L. Wong, E. V. Ryan-Weber, D. A. GarciaAppadoo, et al., Monthly Notices Roy. Astronom. [33] I. D. Karachentsev and V. E. Karachentseva, AstronSoc. 371, 1855 (2006). omy Reports 48, 267 (2004). [18] R. B. Tully and R. Fisher, Astronom. and Astrophys. [34] I. D. Karachentsev and Y. N. Kudrya, Astronom. J. 54, 661 (1977). 148, 50 (2014). [19] S. Stierwalt, M. P. Haynes, R. Giovanelli, et al., Astronom. J. 138, 338 (2009).
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[36] I. D. Karachentsev, D. I. Makarov, V. E. Karachentseva, and O. V. Melnik, Astronomy Letters 34, 832 (2008). [37] B. Nikiel-Wroczynski, M. Soida, D. J. Bomans, and M. Urbanik, Astrophys. J. 786, 144 (2014). [38] R. B. Tully, Nearby Galaxy Catalog (Cambridge Univ. Press, Cambridge, 1988).
[23] S. Paudel, T. Lisker, K. S. A. Hansson, and [39] D. H. Jones, B. A. Peterson, M. Colless, and W. SaunA. P. Huxor, Monthly Notices Roy. Astronom. Soc. ders, Monthly Notices Roy. Astronom. Soc. 369, 25 443, 446 (2014). (2006). Translated by A. Zyazeva
13
Table 1: The original observational data for 543 galaxies in the Leo/Can region Name
RA (2000.0) Dec
(1)
(2)
UGC 03630 UGC 03658 PGC 2802325 NGC 2350 UGC 03755 UGC 03775 UGC 03830 PGC 020981 AGC 171494 AGC 171462 UGC 03895 UGC 03912 AGC 174585 UGC 03946 UGC 3974 KK 65 PGC 021644 AGC 174605 AGC 174514 AGC 174616 SDSS J07565 UGC 04115 PGC 1534834 KK 67 KKH 43 AGC 712516 UGC 04254 SDSS J08103 AGC 182466 AGC 188955 IC 2329 SDSS J08224 PGC 1590056 AGC 188957 UGC 04385 AGC 188875 UGC 04444 PGC 1536571 PGC 023907 PGC 1316080 SDSS J08363 PGC 1331483 UGC 04524 AGC 182493 SDSS J08410 NGC 2644 SDSS J08420 SDSS J08422 SDSS J08423 UGC 04540 SDSS J08423
070103.3+015441 070440.0+173457 070538.7+023720 071312.2+121558 071351.7+103116 071552.6+120654 072330.5+023657 072539.0+091059 072753.6+044146 073059.7+075935 073123.4+000312 073412.6+043247 073610.3+095911 073759.6+031858 074155.4+164809 074231.8+163340 074308.8+035659 075021.7+074740 075230.9+114940 075348.8+100851 075651.0+111300 075702.1+142328 080023.9+173127 080324.6+150828 080612.4+153015 080738.8+105850 080924.0+003634 081030.7+183704 081532.7+091358 082137.0+041901 082219.5+192457 082241.4+162851 082246.3+192229 082341.0+035350 082352.0+144508 082630.5+114711 083001.7+171536 083104.5+173543 083121.6+070000 083218.1+071156 083633.4+051041 083735.5+074831 084014.3+053803 084022.0+075324 084105.9+094730 084131.9+045850 084200.0+103053 084226.9+142533 084232.6+141718 084235.0+103505 084235.7+112950
VLG , km s−1 (3)
V3K , km s−1 (4)
Bt , mag (5)
W50 , km s−1 (6)
D, Mpc (7)
Method
Type
Group
(8)
(9)
(10)
1607 1091 1590 1793 186 2019 1232 1064 1928 1737 1276 1063 217 1026 160 170 768 196 1846 1796 1831 215 1948 1864 1855 1640 1610 1383 1746 575 1975 1862 1932 1983 1832 1740 1956 2009 1677 1836 1684 1834 1757 1831 1881 1754 1848 1905 2046 1884 976
1929 1330 1918 2082 486 2314 1595 1394 2288 2084 1666 1435 562 1411 471 484 1159 578 2207 2169 2203 567 2284 2220 2213 2030 2061 1726 2158 1024 2328 2237 2286 2437 2220 2151 2335 2387 2124 2283 2148 2285 2223 2284 2324 2226 2287 2319 2461 2323 1410
13.98 16.8 18.30 13.30 14.10 16.4 14.99 16.29 18.0 17.20 16.17 14.72 17.9 14.29 13.60 15.30 15.87 18.0 19.0 17.0 18.33 15.20 17.5 17.4 19.0 17.61 14.30 18.33 18.7 17.5 15.01 18.48 18.3 18.6 14.51 17.7 14.41 17.9 16.3 18.32 17.59 16.63 15.17 17.5 18.06 13.79 16.86 17.80 18.15 13.8 18.77
342 146
27.1 35.8
tf TFb
345
31.8 7.41
TF rgb
16.7
tf
33.0
TFb
91 24
20.0 7.91 12.7 8.05 8.02 22.8 10.91
TF rgb TF rgb rgb TF rgb
55
18.4
TF
76
7.73
rgb
91 49 24 152
39.2
TFb
24.2
TF
14.5 29.8
TF TF
Sb Sdm Ir S0a Im Sm Scd Ir Sd Sm Sm Sd Ir Sm Sm Ir Ir Ir Ir BCD BCD Im BCD Ir Ir BCD Sdm Im Ir Ir Sdm Im BCD Ir Sm Ir Scd BCD Sm Ir Ir BCD Scd Ir Sm Sdm Ir BCD Im Sdm Ir
14
94 120 84 38 154 21 90 55
80 38 180
148 27 22.4
tf
126 39 61 121 158 94
29.7
TFb
28.5 44.6 33.9 39.4
TF TFb tf TFb
213
21.6
TF
139
UGC 3974 UGC 3974
KK 67 KK 67
IC 2329 IC 2329
PGC 1331483 NGC 2644 PGC 1331483 NGC 2644 NGC 2648 NGC 2648
(1)
(2)
NGC 2648 PGC 024469 UGC 04550 PGC 1218919 SDSS J08452 UGC 04590 PGC 024666 UGC 04599 PGC 1189545 SDSS J08523 SDSS J08524 SDSS J08584 AGC 182489 UGC 04712 NGC 2725 PGC 1373747 UGC 04781 UGC 04797 AGC 192558 KKH 46 LSBC D634-0 PGC 1200328 NGC 2775 PGC 213577 NGC 2777 UGC 04845 SDSS J09124 SDSS J09125 PGC 1599237 SDSS J09145 AGC 198354 AGC 190238 SDSS J09211 AGC 193816 NGC 2882 PGC 1466669 AGC 198454 NGC 2894 SDSS J09294 AGC 192137 IC 0540 KDG 56 PGC 1324298 NGC 2906 AGC 192607 PGC 027228 LEO-T UGC 05107 AGC 198335 AGC 198430 SDSS J09385 AGC 192830 AGC 192937 IC 0549 NGC 2962 AGC 192833
084239.8+141707 084248.2+141555 084315.9+130509 084522.5+021124 084525.4+151946 084640.0+131249 084647.3+134224 084741.7+132509 084818.7+011551 085233.8+135028 085240.9+135157 085843.9+072631 085854.1+053134 085923.6+110806 090103.2+110553 090515.7+100234 090634.4+061813 090810.6+055539 090824.0+065705 090836.5+051729 090853.7+143459 090920.1+013651 091020.1+070217 091028.7+071118 091041.8+071224 091225.8+095720 091246.6+085620 091250.9+062833 091339.0+193708 091457.3+060019 091630.9+091024 092059.6+110333 092115.0+094352 092127.2+072152 092636.1+075715 092755.6+144559 092811.3+073237 092930.2+074304 092946.2+080236 092951.8+115536 093010.3+075409 093012.8+195923 093155.9+073210 093206.2+082630 093222.2+071808 093444.7+062532 093453.5+170304 093507.4+050712 093704.4+095759 093723.5+040555 093857.1+004134 093922.3+045708 094021.1+044406 094043.2+035733 094053.9+050957 094056.3+050241
(3)
(4)
1917 1973 1919 1687 1504 1839 1941 1924 1294 1365 1430 1840 1791 1827 1913 1870 1259 1122 1390 409 189 1110 1169 1342 1307 1947 1127 1285 324 1242 1162 1116 1199 1208 1974 1980 1193 1966 1934 1461 1856 441 2036 1963 1938 366 -97 1806 1347 1820 1885 1703 1788 1125 1775 1679
2332 2388 2343 2178 1915 2266 2365 2351 1794 1794 1859 2317 2279 2282 2370 2337 1751 1617 1880 908 630 1630 1660 1832 1797 2422 1609 1782 732 1743 1645 1591 1683 1707 2473 2435 1696 2469 2435 1937 2358 859 2542 2463 2445 880 346 2328 1841 2349 2433 2229 2316 1657 2301 2205
(5)
(6)
(7)
(8)
(9)
(10)
12.77 15.14 14.74 16.99 18.61 15.00 16.33 14.98 17.20 17.30 19.70 17.57 18.9 15.73 14.37 18.36 15.40 14.58 17.14 17.1 17.5 17.30 11.14 17.0 14.31 15.25 18.3 17.79 17.4 17.55 18.8 15.82 18.01 17.5 13.51 17.64 18.4 13.23 18.59 17.34 14.72 17.0 18.25 13.40 18.4 15.24 16.5 15.53 19.0 18.4 16.8 16.4 18.08 15.17 12.91 17.2
390 244 276
34.3
tf
37.7
tf
Sb Smp Sb Sm Ir S0a BCD S0 Im Im Ir Ir Ir Scd Scd BCD Sd Sm Sdm Ir Ir BCD Sa Im Sm Scd Sm Ir Im dE Ir Sm BCD Ir Sc Im Ir Sa Ir Sm Sab Ir dE Sbc Ir Im Ir Sd Ir Ir Sm BCD BCD Im S0a Ir
NGC 2648 NGC 2648 NGC 2648
15
72 148 76 44 98 149 186 85 146 73 35 27 47
34.0
TF
36.8
TF
28.0
tf
6.7 9.55
TF rgb
409 107 230 79
25.7 41.3
TF tf
8.9
mem
27 142 23 56 284
39.1
TF
23.6 37.9
TF tf
45 395
26.0 42.3
TF tf
120 256 25
39.2 40.4 8.9
TFb TF mem
312 33 89
38.4
tf
13.0 0.42 37.4
tf rgb tf
27.2 37.0
TF TF
30.5 22.7 33.4
TF TF SN
174 53 46 66 167 44 117 414 49
NGC 2648 NGC 2648 NGC 2648
NGC 2775 NGC 2775 NGC 2775
NGC 2775 NGC 2775 NGC 2775 NGC 2775 NGC 2775 NGC 2903 NGC 2775
NGC 2894
NGC 2894 NGC 2894 NGC 2894 NGC 2903 NGC 2894 NGC 2894 NGC 2894 Milky Way NGC 2962 NGC 2962 NGC 2962 NGC 2962 NGC 2962 NGC 2962
(1)
(2)
PGC 1175027 NGC 2967 NGC 2966 SDSS J09421 AGC 193813 AGC 198337 AGC 192835 AGC 193802 SDSS J09443 IC 0559 AGC 191869 SDSS J09450 SDSS J09454 UGC 05224 IC 560 UGC 05228 PGC 1143397 AGC 198456 UGC 05238 UGC 05242 UGC 05249 PGC 1219995 AGC 191803 PGC 1145436 AGC 193921 NGC 3018 NGC 3023 NGC 3020 NGC 3024 SDSS J09503 AGC 192239 UGC 05288 LSBC L1-47 DDO 65 NGC 3041 NGC 3044 PGC 135729 SDSS J09535 PGC 135730 SDSS J09540 AGC 192423 HIPASSJ095 AGC 192959 PGC 1200167 NGC 3049 NGC 3055 UGCA 188 AGC 192960 UGC 05332 UGC 05347 AGC 198437 LSBC L1-099 PGC 1155688 LSBC L1-100 SEX B PGC 1209966
094117.0+004616 094203.3+002011 094211.5+044024 094218.9+044122 094250.9+045324 094251.2+093800 094302.2+050144 094419.9+100331 094437.1+100046 094443.8+093655 094458.9+082212 094503.8+011350 094541.0+013704 094552.1+025839 094553.4-001606 094603.6+014006 094628.6-002603 094642.4+070807 094654.1+003029 094705.5+005752 094745.4+023738 094759.5+021322 094805.9+070744 094842.3-002115 094914.9+154827 094941.4+003715 094952.6+003705 095006.6+124848 095027.4+124556 095031.3+002427 095036.2+124833 095117.0+074942 095138.6+002210 095144.1+012655 095307.1+164040 095340.9+013447 095359.1+020017 095359.4+025209 095404.5+013223 095407.3+092135 095430.5+095212 095427.8+015548 095435.7+042308 095445.0+013634 095449.6+091617 095518.0+041612 095529.6+082327 095537.8+042836 095548.2+162449 095716.5+043136 095724.2+053942 095828.8+014141 095830.2+000243 095846.8+022050 100000.0+051956 100005.8+015440
(3)
(4)
1755 1682 1850 1842 1746 1290 1771 1303 1313 370 1577 1706 1733 1693 1639 1662 1599 1703 1566 1630 1672 1737 352 1684 1307 1652 1668 1284 1259 1694 1178 378 1685 1637 1271 1082 1551 1574 1168 1291 1318 1603 1579 1751 1283 1610 1097 1778 659 1962 1979 1610 1752 1526 110 1679
2304 2234 2379 2371 2274 1790 2299 1801 1811 871 2086 2255 2281 2234 2196 2210 2157 2220 2120 2182 2216 2283 870 2243 1768 2207 2223 1767 1742 2250 1661 894 2242 2189 1727 1634 2101 2120 1721 1799 1822 2154 2117 2303 1791 2149 1611 2316 1119 2500 2511 2164 2314 2076 645 2232
(5) 18.07 12.28 14.11 18.52 17.2 19.0 18.4 18.6 17.1 14.98 16.49 18.62 18.63 15.81 14.01 13.97 16.3 18.9 15.43 16.95 14.55 17.58 16.5 17.4 19.0 13.89 13.51 13.45 14.07 19.86 17.24 14.44 17.40 16.3 12.30 12.47 18.10 17.96 19.0 17.11 17.95 16.5 17.67 17.53 13.67 12.65 15.59 17.17 16.47 15.30 19.0 17.14 17.91 17.90 11.92 17.86
16
(6) 131 243 87 34 95 43 62 67
(7)
(8)
25.8
tf
38.4 22.5
TF TF
27.5 23.6 9.4
TF TF tf
140
31.4
TF
268
31.9
tf
35.8 33.4 27.7
tf TF tf
14.9
tf
57 214 114
55 39 133 215 245
31.5 29.4 31.1
tf tf TF
93 62 94
11.41 26.1 29.3 26.4 22.8
rgb TF TF tf tf
332
40 127 77 203 266 101 61 52 211 72 93 98 37
27.8 38.9
TFb TF
30.2 31.6 25.9 24.1 16.6 39.4
TF tf TF TF TF TF
21.2
TFb
1.36
rgb
(9)
(10)
BCD Sc Sbc dE Ir Ir Sm Ir Ir BCD BCD BCD BCD Sd S0 Scd dEem Ir Sd Sm Sdm BCD Im dEem Ir Scd Sc Scd Sc Ir BCD Sm Ir Ir Sc Scd Ir Ir Ir BCD BCD Sdm Ir Sm Sb Sc Sm Sm Im Scd Ir Sm BCD Sm Ir Ir
NGC 2967 NGC 2967 NGC 2962 NGC 2962 NGC 2962 NGC 2962 SDSS 0944 SDSS 0944
UGC 5228 UGC 5228 NGC 2967 UGC 5228 NGC 2967 NGC 2967 UGC 5228
NGC 2967 NGC 3023 NGC 3023 NGC 3020 NGC 3020 NGC 3023 NGC 3020 NGC 3023 NGC 3023 NGC 3044
NGC 3044 NGC 3049 NGC 3049 NGC 3055 NGC 3049 NGC 3055
Ark 227
(1)
(2)
Ark 227 UGC 05376 UGC 05377 SDSS J10005 AGC 202171 RFGC 1688 PGC 3121233 AGC 204045 PGC 3279243 UGC 05401 UGC 05403 PGC 3279188 Mrk 714 PGC 1230703 PGC 1201224 AGC 202297 AGC 205108 SEGUE 1 AGC 203862 UGC 05453 UGC 05456 SDSS J10072 PGC 1223942 PGC 029471 Leo I FGC 120A SDSS J10102 NGC 3156 UGC 05504 NGC 3165 PGC 3282143 NGC 3166 UGC 05522 NGC 3169 UGC 05539 KKH 60 SDSS J10165 PGC 1256137 PGC 213680 UGC 05551 AGC 208392 PGC 030133 SDSS J10190 NGC 3213 PGC 1178576 LEO-P PGC 1609953 NGC 3226 NGC 3227 UGC 05633 NGC 3239 AGC 203913 UGC 05646 IC 610 NGC 3246 AGC 208295
100010.4+020922 100027.1+032228 100031.6+031219 100059.1+032752 100109.5+084656 100110.3+005432 100153.8+022450 100200.0+044728 100227.1+021001 100231.3+190159 100235.5+191037 100315.4+020543 100408.7+063038 100425.1+023331 100517.6+013828 100603.8+103816 100640.3+121900 100703.6+160440 100704.5+050025 100707.2+155902 100719.8+102143 100724.1+051931 100806.9+022043 100810.3+022748 100828.0+121823 100917.4+052414 101020.5+074513 101241.3+030746 101249.1+070612 101331.3+032230 101332.3+010601 101345.7+032530 101358.9+070126 101414.9+032759 101555.0+024109 101559.5+064816 101659.0+034235 101702.3+033846 101709.0+042040 101711.9+041949 101803.7+041835 101901.5+211702 101904.6+171100 102117.3+193906 102138.9+005400 102144.8+180520 102322.5+195452 102327.0+195354 102330.6+195154 102440.1+144523 102504.8+170949 102546.4+053909 102553.1+142148 102628.4+202859 102641.8+035143 102827.2+081026
(3)
(4)
1589 1855 1946 1763 993 1135 1823 1512 1651 1906 1958 1544 944 914 1060 1394 1329 67 1534 700 360 1414 1760 1873 125 1512 1090 1140 1364 1145 1952 1148 1037 1041 1081 1438 1033 862 1115 1148 1130 972 1846 1227 495 135 1081 1197 1039 1240 623 966 1225 1054 1961 1317
2141 2401 2493 2308 1507 1694 2374 2050 2204 2348 2399 2098 1473 1466 1617 1898 1822 533 2073 1167 866 1951 2314 2426 619 2050 1614 1691 1893 1695 2514 1698 1566 1591 1636 1969 1582 1412 1661 1694 1676 1401 2307 1670 1060 590 1522 1638 1480 1720 1086 1506 1708 1491 2511 1842
(5) 14.82 14.29 15.24 17.02 18.02 17.84 18.20 17.82 18.71 16.30 14.45 17.65 15.81 18.47 17.26 17.0 19.24 16.2 17.3 15.39 13.74 18.05 16.52 15.55 11.16 17.5 18.12 13.07 16.25 14.50 19.0 11.42 14.61 11.25 16.10 17.84 17.37 17.12 17.36 16.8 19.0 15.4 18.12 14.17 17.5 17.2 17.32 12.34 11.55 14.46 11.70 16.17 14.20 14.72 13.91 18.9
17
(6)
(7)
(8)
338
45.3
TFb
120 266
40.0 46.4
TF TF
42
10.5
TF
258 26 34 53 61
0.02 11.3
rgb TF
5.60
rgb
83
0.25 37.5
rgb TFb
200 147 128
22.5 30.3 17.9
sbf tf TF
193 211 452 141 94
31.6 18.8 27.0 30.6
TFb SN TFb TFb
33 56 34 78
400 167 99 221 268 244 91
17.8
TF
24.8
TF
32.0
tf
2.0
txt
23.7 22.2 36.2 7.9 28.4 27.6 31.8 35.5
sbf TF TF tf TF TF tf tf
(9)
(10)
dE Scd Sm Sm BCD Sdm Im BCD Ir Sm S0em Im BCD Ir Ir Sc Ir Sph Ir Im Im Ir BCD dE Sph Sd Ir S0em Sd Sm Ir S0a Scd Sa Sm Im Im BCD Ir Im Ir Sm BCD Sd Ir Im dE E Sab Sm Im Sd Sbc Sbc Sd Ir
Ark 227 UGC 5376 UGC 5376 UGC 5376
UGC 5376
UGC 5403 UGC 5403
NGC 3166
Milky Way
Milky Way
NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3166 NGC 3227
NGC 3227 NGC 3227 NGC 3227 UGC 5646
UGC 5646 NGC 3227 NGC 3246
(1)
(2)
UGC 05675 UGC 05677 PGC 1214845 AGC 208394 VIII Zw081 AGC 202218 SDSS J10304 AGC 205156 UGC 05708 SDSS J10313 AGC 202244 AGC 204139 SDSS J10331 AGC 202016 AGC 205161 NGC 3279 AGC 202248 LeG 03 NGC 3299 AGC 205165 FGC 125a AGC 200499 AGC 208397 UGC 05797 LeG 05 LeG 06 AGC 208399 UGC 05812 AGC 205078 AGC 203080 FS 04 NGC 3338 AGC 203082 UGC 05832 AGC 205268 AGC 200543 NGC 3346 NGC 3351 AGC 205445 PGC 1174229 LeG 13 AGC 205270 PGC 3090074 NGC 3365 LeG 14 LeG 17 NGC 3368 LeG 18 KK 94 LeG 21 NGC 3370 DDO 88 NGC 3377 NGC 3379 NGC 3384 NGC 3389
102830.0+193345 102838.2+033338 102843.0+020349 102843.8+044404 102848.1+041403 102855.8+095144 103044.3+060734 103052.9+122648 103113.2+042819 103137.3+043422 103140.8+135005 103201.3+042046 103316.2+181311 103319.2+101122 103405.5+154650 103442.8+111149 103456.1+112932 103548.9+082853 103624.0+124224 103704.8+152015 103728.7+122346 103808.0+102251 103858.1+035227 103925.2+014307 103942.9+123805 103955.6+135434 104010.7+045432 104056.5+122818 104126.1+070216 104141.0+134930 104200.3+122006 104207.6+134449 104226.5+135726 104248.5+132736 104252.4+134428 104305.5+133040 104338.9+145218 104357.7+114213 104435.3+135623 104456.3+004427 104457.5+115458 104509.8+152700 104602.8+193216 104612.6+014848 104614.2+125737 104641.3+121938 104645.7+114911 104653.2+124440 104656.8+125957 104700.8+125735 104704.0+171625 104722.4+140412 104742.4+135908 104749.6+123454 104816.9+123746 104827.9+123159
(3)
(4)
983 963 1860 992 1967 1024 458 762 987 1013 1141 957 1107 1270 1081 1236 1020 987 453 586 1178 1009 573 511 629 863 561 857 999 1127 621 1157 1133 1070 1001 1111 1135 624 490 1412 734 1083 1197 789 749 880 740 488 684 696 1153 431 536 774 556 1159
1427 1515 2420 1538 2515 1538 996 1259 1534 1560 1629 1505 1562 1783 1555 1742 1524 1511 949 1063 1676 1521 1124 1074 1125 1350 1106 1355 1532 1615 1119 1646 1620 1561 1490 1601 1615 1127 977 1979 1235 1559 1642 1351 1243 1378 1242 983 1178 1190 1615 917 1023 1270 1052 1656
(5)
(6)
(7)
(8)
(9)
(10)
16.66 15.07 17.66 19.0 15.76 16.71 16.80 18.6 14.37 16.27 16.5 18.42 17.57 19.10 17.90 13.93 17.5 17.3 13.30 16.4 17.4 14.40 19.7 14.30 16.80 18.30 20.0 15.50 19.0 17.46 15.7 11.44 17.8 14.31 17.4 16.2 12.59 10.60 16.4 17.12 17.36 17.14 16.57 13.18 18.70 17.0 10.10 18.90 17.5 18.60 12.29 14.40 11.20 10.23 10.89 12.51
72
27.3 22.0
TF tf
NGC 3227
26.9 11.7 7.8 10.4 21.3
TF TF tf tf TF
34.3
TF
32.2 10.4 10.4 10.4 10.4 25.0 36.5 26.2
tf mem mem mem mem TF TF tf
10.4 10.4 20.9 10.4
mem mem tf mem
36 339 41 102
10.4 24.9 17.5 18.6
mem tf TF TF
70 162 270
18.1
TF
10.05 10.4
cep mem
24 51
11.3
TF
234
18.2 10.4 10.4 10.42 10.4 10.4 10.4 27.50 7.73 10.91 11.12 11.38 32.8
tf mem mem cep mem mem mem cep rgb sbf sbf sbf SN
Sm Sd BCD Ir BCD Im Ir BCD Sd BCD Im Ir Ir Ir Ir Scd Ir Sm Sm Im Sd BCD Ir BCD dE Ir Ir Sm Ir dE Sm Sc Ir Scd BCD Im Scd Sb Sph Im Ir BCD dE Sd Sph Sph Sab Ir Tr Ir Sbc Im E E S0 Sc
18
27 104 39 27 21 169 102 68 32 114 347 62 70 112 27 59 178 33 47 21 23 56 32
343 38
46
266
NGC 3246
NGC 3379 UGC 5708 UGC 5708
NGC 3379 NGC 3379 NGC 3379 NGC 3379
NGC 3379 NGC 3379 NGC 3379 NGC 3338 NGC 3379 NGC 3338 NGC 3338 NGC 3338 NGC 3338 NGC 3338 NGC 3338 NGC 3379 NGC 3379 NGC 3379
NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379 NGC 3379
(1)
(2)
AGC 200596 Mrk 1263 AGC 200600 UGC 05923 AGC 200603 PGC 032376 AGC 202253 AGC 205197 AGC 205313 AGC 205198 LSBGL1-134 UGC 05944 UGC 05945 UGC 05947 UGC 05948 NGC 3412 NGC 3423 LeG 26 AGC 205540 KKH 64 UGC 05974 SDSS J10514 AGC 205544 AGC 202456 PGC 032630 UGC 05989 SDSS J10523 MGC 0013223 PGC 032664 NGC 3443 PGC 135768 SDSS J10531 PGC 032687 NGC 3447 NGC 3447b UGC 06014 SDSS J10540 UGC 06022 NGC 3454 NGC 3455 NGC 3457 AGC 202033 PGC 1533359 UGC 06035 PGC 032833 PGC 032843 LSBC D640-1 Mrk 1271 AGC 202035 SDSS J10561 SDSS J10563 AGC 202260 CGCG 095-78 AGC 205278 NGC 3485 NGC 3489
104853.7+140728 104856.8+121142 104859.7+105007 104907.6+065502 104917.1+122519 104918.4+122242 104926.7+121528 104942.8+134941 104947.9+123626 105001.8+134705 105008.9+011554 105019.0+131621 105025.5+173351 105030.4+193839 105038.2+154548 105053.3+132444 105114.4+055024 105121.1+125057 105131.3+140653 105132.1+032718 105135.0+043459 105148.7+194606 105204.7+150149 105219.5+110235 105221.4+175607 105231.8+194732 105234.9+170842 105240.6-000116 105248.6+000204 105300.1+173426 105303.3+022937 105314.5+175028 105318.9+023736 105323.9+164630 105329.6+164710 105342.7+094339 105400.0+094952 105415.4+174837 105429.2+172040 105431.1+171705 105448.6+173716 105503.6+140515 105506.7+172746 105529.0+170830 105539.2+022345 105544.4+170018 105555.8+122019 105609.1+061022 105613.9+120040 105619.9+170506 105638.6+172301 105738.2+135844 105802.2+193019 105852.4+140747 110002.4+145029 110018.6+135404
(3)
(4)
400 1171 1782 538 1234 1200 1188 1190 626 1168 1405 928 1008 1137 987 697 825 483 691 881 859 1276 692 669 1182 1016 928 1569 1607 1009 854 1052 866 940 971 965 1023 848 977 978 1025 1968 1035 947 829 1018 699 837 840 830 818 1078 538 548 1301 538
885 1670 2290 1071 1731 1698 1686 1677 1122 1656 1969 1419 1468 1581 1460 1187 1364 977 1176 1433 1405 1719 1171 1175 1639 1458 1391 2139 2177 1468 1411 1509 1423 1405 1436 1480 1537 1305 1438 1439 1484 2453 1495 1409 1386 1481 1196 1373 1339 1293 1278 1563 982 1032 1779 1023
(5) 15.66 15.70 16.25 14.41 15.72 18.0 17.5 19.0 18.0 17.18 17.38 15.27 14.7 14.92 16.65 11.44 11.61 16.9 18.0 16.5 14.82 18.24 17.1 16.2 15.20 14.41 18.26 17.8 15.75 14.83 17.46 17.57 15.95 14.46 14.3 15.2 17.54 16.4 13.71 14.31 13.6 18.9 16.90 15.44 16.48 15.32 18.40 14.81 16.9 18.52 18.20 17.50 15.6 17.3 12.67 11.06
19
(6)
(7)
(8)
125 120 142 68
34.2 38.4 22.3 14.2
TF TF tf TF
42 30 53
124 70 106 156
74
126
12.1 19.1
TF TF
11.07 22.8 10.4 26.3 11.3 19.5 10.4 10.4 23.1 27.2
sbf TF TF TFb sbf TF mem mem TF tf
10.4 10.4
mem mem
16.1
TF
89
20.8 22.0
TF tf
78
18.6
TF
94
17.0
TF
86
31.8 27.6 29.0 20.7
TF tf tf sbf
72
21.7
TF
22 128 30
10.4 23.3 10.4
mem TF mem
92 62 36 135 113
28.8 11.7 11.8
TFb TF TF
12.08
sbf
(9)
(10)
dE BCD Sm S0em Sm Ir BCD Ir Im BCD Sm Sph Im Im Im S0 Scd Sph Ir Im Sd BCD Sph Sph dS0 Sm Ir Ir BCD Scd Im Im Sm Sm Im Sm BCD Sm Sc Sb E Ir Im Im Im BCD Ir BCD Im Im BCD Im Im Ir Sb S0a
NGC 3379
NGC 3379 NGC 3379 NGC 3379
NGC 3379 NGC 3607
NGC 3379 NGC 3423 NGC 3379 NGC 3379 NGC 3423 NGC 3423 NGC 3379 NGC 3379
NGC 3607 PGC 032664 PGC 032664 NGC 3607 PGC 032687 NGC 3607 PGC 032687 NGC 3607 NGC 3607
NGC 3607 NGC 3607 NGC 3607 NGC 3607 NGC 3607 NGC 3607 NGC 3607 NGC 3379 NGC 3423 NGC 3379 NGC 3607 NGC 3607
NGC 3379 NGC 3379
(1)
(2)
UGC 06083 SDSS J11004 UGC 06095 NGC 3495 UGC 06112 NGC 3501 AGC 202040 NGC 3507 AGC 215256 AGC 219117 AGC 210023 KK SG 20 SDSS J11045 PGC 033523 UGC 6145 NGC 3521 UGC 06151 AGC 213757 PGC 1558217 NGC 3524 AGC 215262 SDSS J11065 NGC 3526 UGC 06169 UGC 06171 UGC 06181 PGC 033816 NGC 3547 AGC 210111 AGC 213064 PGC 033959 UGC 06233 SDSS J11114 KK 98 PGC 087259 IC 0676 UGC 06248 AGC 213796 PGC 034135 AGC 215280 PGC 1257521 AGC 215240 AGC 219197 PGC 1219195 AGC 215282 NGC 3592 NGC 3593 AGC 202256 NGC 3596 AGC 215281 NGC 3599 AGC 215284 AGC 212132 PGC 034407 PGC 1224534 NGC 3605
110023.8+164132 110047.2+165256 110104.4+190600 110116.2+033741 110235.2+164406 110247.3+175922 110301.8+080253 110325.4+180810 110326.4+160059 110346.7+083419 110426.4+114522 110440.2+000329 110456.8+173830 110532.5+173823 110535.0-015149 110548.6-000209 110556.3+194931 110559.6+072225 110627.3+182324 110632.1+112307 110635.3+121348 110651.1+173003 110656.7+071026 110703.4+120336 110710.1+183412 110746.6+193258 110923.2+105003 110955.9+104314 111025.2+100733 111054.5+093719 111054.9+010531 111128.3+065427 111147.0+185126 111215.7+164514 111231.7+161723 111239.8+090321 111251.8+101200 111252.7+075519 111300.2+075143 111316.3+152428 111350.6+034342 111350.8+095739 111355.2+040619 111405.2+021155 111425.2+153202 111427.3+171536 111437.0+124904 111445.0+123851 111506.2+144713 111516.2+144155 111527.0+180637 111532.4+143438 111626.1+042011 111635.3+180706 111642.1+022149 111646.7+180102
(3)
(4)
811 1022 1002 944 909 1012 1194 862 1102 1575 629 636 798 898 546 598 1227 1472 1130 1216 1461 830 1259 1405 1092 1060 1404 1438 1167 1414 802 1398 856 1092 1127 1272 1134 1242 1233 1351 2081 1457 1430 1179 731 1180 489 490 1063 962 726 1002 932 828 1415 548
1276 1485 1448 1494 1373 1466 1717 1315 1571 2095 1128 1203 1254 1354 1122 1165 1666 1999 1580 1717 1956 1287 1787 1901 1541 1501 1908 1942 1675 1925 1362 1926 1301 1553 1591 1786 1641 1763 1754 1822 2626 1965 1973 1732 1200 1636 977 980 1537 1437 1175 1478 1473 1277 1966 998
(5)
(6)
(7)
(8)
(9)
(10)
15.29 18.13 16.31 12.42 14.79 13.61 18.10 12.07 16.88 18.72 16.4 17.5 17.43 14.89 16.50 9.80 14.90 17.49 17.46 13.36 18.2 18.52 13.86 14.56 15.13 15.54 15.27 13.20 15.98 15.52 15.88 14.66 17.72 17.40 16.89 13.52 16.7 17.5 15.28 18.2 17.7 18.55 16.80 17.12 16.84 14.46 11.86 17.50 11.79 18.1 12.88 17.84 15.95 15.40 18.13 13.16
146
27.2
TF
94
29.4 18.5 25.7 24.3 37.6
TF tf TF tf TFb
Sbc Im Im Scd Sd Scd Ir Sb Ir Ir Im Ir dEem dEem Ir Sbc Sm BCD Sdm S0 Ir Sph Scd Sbc Sdm Sm Sm Sbc Ir BCD Im S0em Sm Tr dE S0em Sm BCD Sdm Ir BCD BCD BCD Sm Im Sc S0a Ir Sc Ir S0 Ir Sdm S0 dE E
NGC 3607 NGC 3607 NGC 3607
20
152 96 105 68 44 25
37.5
TF
10.3 10.7
TF mem
41 441
10.7 10.7
TF TF
57 66
30.4
TF
196 241 146
20.8 34.6 29.5
TF TF TF
66 204 60 124 71 212
28.7 18.7 31.4 16.2 34.8
tf TF TF TF TF
63
177 26 78 118 93 34 63
20.0
TF
25.6 22.7
TF TF
19.5 20.3
TF TF
27 254 42 118
23 155
25.7 10.8 11.0
tf tf tf
20.4
sbf
39.8
TF
20.5
sbf
NGC 3607 NGC 3607 NGC 3607
NGC 3379 NGC 3521 NGC 3607 NGC 3607 NGC 3521 NGC 3521
NGC 3607
NGC 3607 NGC 3607 NGC 3547 NGC 3547
NGC 3607 NGC 3607
PGC 34135 PGC 34135
NGC 3640
NGC 3627 NGC 3627 NGC 3596 NGC 3596 NGC 3607 NGC 3596 NGC 3607 NGC 3607
(1)
(2)
UGC 06296 NGC 3607 NGC 3608 IC 2684 AGC 215186 AGC 215241 UGC 06300 UGC 06306 NGC 3611 PGC 034493 PGC 1513499 PGC 034522 AGC 213006 IC 2703 UGC 06320 PGC 086629 UGC 06324 PGC 1192339 SDSS J11185 NGC 3623 AGC 215286 AGC 202257 AGC 215354 AGC 213074 PGC 034653 AGC 215287 PGC 3288593 UGC 06341 PGC 1234729 NGC 3626 NGC 3627 UGC 06345 NGC 3628 NGC 3630 PGC 1553459 SDSS J11210 NGC 3640 NGC 3641 NGC 3643 PGC 1534499 SDSS J11214 PGC 1519262 SDSS J11215 SDSS J11220 SDSS J11221 IC 2763 AGC 219200 IC 2767 AGC 213511 AGC 213436 AGC 219201 IC 2781 NGC 3655 IC 2782 AGC 215290 PGC 086673
111651.1+174754 111654.5+180307 111658.9+180855 111701.0+130557 111701.2+043944 111702.7+100836 111717.0+161938 111727.4+043616 111730.1+043319 111738.2+174905 111748.4+163824 111758.0+172629 111803.9+101440 111805.1+173858 111817.3+185049 111821.4+174151 111822.1+184418 111826.9+012121 111850.5+034549 111855.8+130535 111912.7+141940 111914.4+115707 111915.9+141725 111928.1+093544 111933.2+030053 111945.1+153008 111954.0+005019 112000.6+181538 112003.1+024123 112003.8+182125 112015.0+125928 112015.6+023133 112016.9+133520 112017.0+025751 112045.0+181310 112106.9+032807 112106.9+031405 112108.8+031140 112125.0+030050 112125.1+173037 112140.3+193643 112148.0+165247 112151.4+032418 112204.1+033652 112211.1+043942 112218.5+130354 112220.0+035356 112223.2+130440 112223.4+114738 112224.0+125846 112231.4+053129 112250.7+122041 112254.7+163524 112255.4+132628 112259.1+122738 112259.4+172826
(3)
(4)
862 829 1113 451 1279 1614 948 1579 1447 1181 851 691 806 862 1016 937 958 770 1513 671 867 719 659 843 1070 1209 1488 1530 1460 1382 590 1419 709 1317 1364 1326 1118 1600 1569 865 1043 1399 1044 1259 1131 1433 1124 942 1430 491 1405 1406 1355 727 1475 1268
1313 1278 1562 937 1818 2119 1410 2118 1986 1632 1311 1145 1310 1314 1459 1389 1402 1326 2056 1156 1343 1212 1135 1351 1617 1676 2046 1977 2008 1828 1075 1968 1190 1864 1811 1870 1663 2145 2115 1317 1478 1855 1588 1801 1668 1917 1665 1425 1922 975 1936 1894 1813 1208 1962 1719
(5) 14.18 10.93 11.57 16.2 18.51 17.72 15.77 17.4 12.85 15.56 17.18 15.05 18.33 15.70 13.83 17.6 14.77 18.07 18.4 10.14 18.0 17.35 17.40 17.43 16.0 16.8 19.09 16.06 17.98 11.81 9.74 14.07 9.97 12.90 16.61 18.0 11.33 14.12 14.65 16.46 16.55 17.12 17.34 18.40 17.83 15.15 19.0 17.06 17.6 16.7 18.9 17.0 12.32 15.12 17.9 17.72
21
(6)
25 66 120
(7)
(8)
(9)
(10)
24.4 22.8 22.9 10.3
tf sbf sbf mem
NGC 3607 NGC 3607 NGC 3607 NGC 3627 NGC 3640
44.4
TFb
Scd S0 E Tr Ir Sdm dEem Ir Sa S0a Im dE Ir dE Sm Ir S0e? Ir Ir Sa Ir Ir BCD Ir Sm Sm Ir Sdm Ir Sa Sb Sm Sb S0 BCD Ir E E S0a dE Ir Ir Ir dE dE Sdm Ir Im BCD dEem Ir Im Sc Sph Ir Ir
108 375
55
25.0
TF
493 28 51 51
12.8 11.7 11.7 10.4 20.6
tf TF TFb mem TF
103
40.5
TF
88
23.4
TF
369 107 458
20.00 10.28 12.3 12.2 28.9
sbf cep TF tf tf
27.0 26.7
sbf sbf
24.8
TF
132 28 92 61 24 72
42 60
28.8 10.3
TF mem
27.6 30.9
TF tf
18.8 29.8
TF TF
NGC 3607 NGC 3611 NGC 3611
NGC 3607 NGC 3627 NGC 3607 NGC 3607 NGC 3607 NGC 3607
NGC 3627 NGC 3627 NGC 3627 NGC 3627 NGC 3640
NGC 3626 NGC 3626 NGC 3627 NGC 3627 NGC 3640 NGC 3640 NGC 3640 NGC 3640 NGC 3640 NGC 3607 NGC 3607 NGC 3626 NGC 3640 NGC 3640 NGC 3640 NGC 3640 NGC 3627 NGC 3627
NGC 3626 NGC 3627 NGC 3626
(1)
(2)
AGC 215414 PGC 1509123 PGC 034965 IC 2787 IC 2791 KK 103 NGC 3659 SDSS J11240 NGC 3664 NGC 3664A NGC 3666 AGC 215142 PGC 035087 AGC 214317 PGC 035096 PGC 1502483 AGC 214318 IC 0692 AGC 219119 AGC 214319 NGC 3681 AGC 215296 AGC 219202 IC 2828 NGC 3684 AGC 219203 NGC 3686 SDSS J11280 NGC 3691 NGC 3692 AGC 213939 KK 104 PGC 1164263 PGC 3123526 AGC 213091 PGC 3287557 PGC 035426 NGC 3705 PGC 3090344 KKH 68 AGC 215303 Leo V PGC 035565 PGC 1228108 PGC 3291243 PGC 1598409 AGC 215306 AGC 215248 KK 107 IC 2934 KKH 69 SDSS J11345 AGC 213169 PGC 3291071 PGC 1209232 UGC 06578
112311.1+134220 112313.9+162711 112318.8+035719 112319.1+133747 112337.6+125345 112341.1+191626 112345.4+174906 112408.5+034404 112424.3+031930 112425.0+031317 112426.1+112031 112444.5+151632 112501.8+170509 112505.4+040716 112510.8+165304 112529.0+161019 112540.0+044036 112553.5+095914 112603.4+080432 112608.3+040345 112629.8+165148 112655.2+145003 112710.9+050856 112711.0+084352 112711.2+170149 112728.9+053702 112743.9+171327 112806.2+175913 112809.4+165514 112824.3+092427 112824.3+060704 112851.2+181658 112922.6+002220 112930.0+031343 112934.6+104836 112945.6+003425 112954.5+162546 113007.5+091636 113026.2+171957 113053.3+140846 113108.8+133414 113109.6+021312 113201.9+143639 113244.1+022825 113306.9+012051 113319.1+193551 113350.1+144929 113350.9+140315 113416.2+170947 113419.6+131917 113453.3+110112 113456.5+161452 113518.4+045717 113530.2+015944 113543.0+015325 113636.8+004858
(3)
(4)
746 1004 1415 576 530 1789 1173 1587 1203 1147 917 1008 1093 1421 903 706 1398 1008 1410 1351 1124 788 1348 886 1048 1345 1043 902 970 1576 1389 1200 1490 1329 600 922 951 868 1064 751 875 -7 1002 882 1466 1320 1007 808 941 1069 742 1020 1226 1440 1410 915
1225 1463 1955 1055 1014 2226 1621 2128 1746 1690 1411 1475 1546 1959 1358 1166 1933 1510 1924 1889 1578 1257 1879 1396 1501 1873 1494 1347 1423 2081 1914 1642 2046 1870 1095 1476 1407 1373 1513 1223 1351 538 1470 1425 2015 1750 1472 1279 1389 1545 1233 1474 1754 1984 1954 1464
(5)
(6)
(7)
(8)
(9)
(10)
18.0 18.37 16.20 15.70 17.15 17.60 12.92 18.13 13.31 16.19 12.70 16.9 17.35 17.83 16.12 16.88 18.06 14.23 18.7 17.24 12.42 19.12 19.1 15.03 12.31 18.8 12.00 18.19 12.64 13.14 17.55 17.10 18.69 17.92 17.74 18.94 17.61 11.76 16.41 17.8 17.90 17.6 16.75 17.45 18.98 17.23 17.46 17.91 17.21 15.6 17.6 17.87 18.4 19.10 18.31 15.2
27
11.1
TF
22
10.3 10.3
mem mem
NGC 3627 NGC 3607 PGC 34965 NGC 3627 NGC 3627
26.5
tf
26.3 19.3 39.1
TF tf TFb
17.2 20.6 17.4
TF TF TF
Ir dE dE dE Ir Sph Sd dE Sm Sm Sbc Sdm Im Im Im BCD BCD BCD Ir Im Sab Ir Ir BCD Sbc Ir Sbc Im Sbc Sb Ir Ir Ir BCD Ir Ir Im Sab dEem? Ir Im Sph Sdm Ir Ir Im Im Im Ir Im Ir Ir Ir Ir BCD Im
22
84 255 123 130
123 95 35 49 44 70 80
14.2 23.8
TF tf
18.6
tf
408 45 62
28.3 36.0 17.8 23.7
tf tf TF TF
345
18.4
tf
22 32
8.5 13.0 0.18 39.6
TF TF rgb TF
64 19
29.0
TF
61 22
11.1 7.4
TF TF
37
20.2
TF
90
18.1
TF
28
115
NGC 3686 NGC 3640 NGC 3640 NGC 3607 NGC 3686 PGC 34965 NGC 3607
NGC 3686 NGC 3627 NGC 3705 NGC 3686 NGC 3686 NGC 3686 NGC 3686
NGC 3686
NGC 3686 NGC 3705 NGC 3686 NGC 3627 NGC 3627 Milky Way
NGC 3627
NGC 3627
(1)
(2)
AGC 213155 HIPASS J113 UGC 06594 NGC 3773 PGC 1170677 PGC 1191771 PGC 1597887 IC 0718 IC 0719 AGC 215137 NGC 3810 UGC 06655 UGC 06669 PGC 1218595 UGC 06670 KDG 79 AGC 213333 PGC 1519757 KKH 72 SDSS J11470 PGC 2806928 SDSS J11484 PGC 1528400 SDSS J11493 SDSS J11495 Mrk 750 AGC 210835 AGC 213174 KIG 0506 SDSS J11530 PGC 166116 IC 0745 AGC 215145 SDSS J11544 PGC 3291881 KIG 0511 UGC 06903 PGC 135785 PGC 1218832 PGC 1218144 PGC 1488625 AGC 213178 PGC 3291730 AGC 210968
113708.8+131504 113728.7+182436 113737.1+163322 113813.0+120644 113817.4+003648 113901.1+012012 113908.9+193500 113952.8+085229 114018.5+090035 114056.7+140428 114058.8+112816 114150.6+155825 114218.7+145944 114228.4+021050 114229.4+182000 114310.5+141327 114327.0+112354 114440.7+165359 114454.1+020951 114707.0+030623 114816.4+183833 114843.1+171053 114905.6+171521 114931.0+151539 114957.1+161744 115002.7+150124 115055.9+143542 115104.8+051446 115201.9+135243 115300.3+160230 115401.6+164324 115412.3+000812 115412.5+122606 115449.3+064234 115501.8+013900 115504.9+014311 115536.9+011414 115722.4+014653 115725.1+021116 115735.2+021004 115840.4+153534 115900.8+044011 115909.2+012938 115933.8+135315
(3)
(4)
855 844 925 849 773 1429 1624 1836 1686 776 857 635 906 1623 820 894 763 794 839 844 879 988 519 744 1080 635 893 1324 879 826 875 951 880 1209 1627 1116 1719 1811 839 796 454 1446 1989 1330
1329 1280 1375 1330 1322 1974 2050 2338 2186 1242 1341 1087 1365 2161 1254 1358 1246 1237 1376 1374 1307 1426 957 1196 1524 1088 1349 1839 1339 1270 1313 1491 1348 1713 2159 1647 2252 2340 1366 1323 896 1958 2518 1784
(5)
(6)
(7)
(8)
(9)
(10)
17.50 18.5 14.92 13.51 16.87 16.89 18.59 14.67 13.89 16.5 11.27 14.93 16.65 18.57 13.39 17.4 16.71 17.23 18.0 18.03 17.8 17.93 18.49 17.8 18.13 15.76 16.66 17.92 15.79 19.0 17.37 14.11 18.5 18.52 18.82 15.5 14.09 17.70 17.97 16.49 18.39 17.20 19.09 15.2
40
14.8
TF
NGC 3810
108
18.9 17.1
tf TF
Sd Ir Scd BCD Ir Im Ir Sdm S0 Scd Sc BCD Im Sm Sd Sm BCD BCD Ir Ir Im Ir dE dE Ir BCD Im BCD Sm Ir Ir Eem Ir Ir Ir Sm Sc Ir BCD Sdm Im BCD Im Sm
23
156 294 110 249 54 65
27.9 28.6 35.3 18.3
TF tf TF tf
20.1
TF
194 85 64
18.1 18.7 20.3
TF TFb TF
47 52
13.6 11.6
TF TF
79
18.3
TF
32
18.3 17.1
sbf TF
26.8
TF
32
112 177
58
19.4
TF
57
11.3
TF
NGC 3810
NGC 3810
NGC 3810 NGC 3810
PGC 1218144 PGC 1218144
