A&A 408, 905-913 (2003)
DOI: 10.1051/0004-6361:20031016
A. Cappi1 - C. Benoist2 - L. N. da Costa3 - S. Maurogordato4
1 -
INAF, Osservatorio Astronomico di Bologna, via Ranzani 1, 40127
Bologna, Italy
2 -
CERGA, Observatoire de la Côte d'Azur, BP 4229, Le Mont-Gros, 06304 Nice
Cedex 4, France
3 -
European Southern Observatory, Karl Schwartzschildsrtrae 2, 85748
Garching bei München, Germany
4 -
CERGA, CNRS, Observatoire de la Côte d'Azur, BP 4229, Le Mont-Gros, 06304
Nice Cedex 4, France
Received 21 February 2003 / Accepted 12 June 2003
Abstract
The most luminous galaxies in the blue passband have a larger
correlation amplitude than L* galaxies. They do not
appear to be preferentially located in rich clusters or groups,
but a significant fraction of them seem to be in systems which
include fainter members.
We present an analysis of fields centered on 18 Very
Luminous Galaxies (
)
selected from the Southern Sky Redshift
Survey 2, based on new observations and public data of the 2dF Galaxy
Redshift Survey; we present also additional data on a CfA VLG and on
Arp 127.
We find that all the selected VLGs are physically associated with fainter
companions. Moreover, there is a relation between the VLG morphology
(early or late) and the dynamical properties of the system, which reflects
the morphology-density relation. 6 out of the 18 SSRS2
VLGs are early type galaxies: 2 are in the center of rich Abell clusters
with velocity dispersion
km s-1,
and the other 4 are in poor clusters or groups with
.
The VLG extracted from the CfA catalog is also an elliptical in a
Zwicky cluster.
The remaining 2/3 of the sample are late-type VLGs,
generally found in poorer systems with a larger spread
in velocity dispersion, from
100 up to
750 km s-1.
The low velocity dispersion, late-type VLG dominated systems
appear to be analogous to our own Local Group.
The possibile association of VLG systems with dark matter halos with mass
comparable to rich groups or clusters, as suggested by the comparable
correlation amplitude, would imply significant differences in the
galaxy formation process.
This work also shows that observing fields around VLGs represents an
effective way of identifying galaxy systems which are not selected through
other traditional techniques.
Key words: cosmology: observations - galaxies: distances and redshifts - galaxies: kinematics and dynamics
From the analysis of the Southern Sky Redshift Survey 2
(SSRS2, da Costa et al. 1994), we have found that the amplitude
of galaxy clustering increases significantly as a function of
galaxy luminosity,
but only when L > L* (Benoist et al. 1996;
see also Willmer et al. 1998); moreover, the analysis of
high-order moments shows that the bias is not linear, without a
significant dependence on scale (Benoist et al. 1999),
analogous to the bias between clusters and galaxies
(Cappi & Maurogordato 1995).
We have also found that the clustering amplitude of the most
luminous galaxies in the sample,
having absolute magnitude
(i.e.
), which
we defined as Very Luminous Galaxies (VLGs),
is similar to that of clusters, with
a correlation length
h-1 Mpc.
From the analysis of the 2dF Galaxy Redshift Survey (2dFGRS)
Norberg et al. (2001) have confirmed the reality of luminosity segregation
for galaxies more luminous than L*, even if their most luminous galaxies
show a correlation amplitude not as high as the SSRS2 VLGs.
The large value of the VLG correlation function could be explained if VLGs were in clusters, as originally suggested by Hamilton (1984): in this case, most of them should be luminous ellipticals. However, in our statistical analysis of the SSRS2 VLGs (Cappi et al. 1998, Paper I) we have shown that the fractions of the different morphological types are comparable to lower luminosity samples, and that most of the VLGs are not in rich clusters. Only a minority of VLGs were found in known groups, but in most cases our visual inspection of the Digitized Sky Survey images revealed the presence of fainter companions, often with signs of interaction.
In fact, if VLGs are neither in clusters nor in rich groups, they can nevertheless be associated with poorer systems. In biased galaxy formation (Kaiser 1984; Bardeen et al. 1986) more massive halos, which represent rare fluctuations of the matter density field, have a larger correlation amplitude. This suggests an association of VLGs to high density peaks; the fact that they are dominant galaxies in poor systems with much fainter galaxies can have interesting implications, concerning for example the efficiency of galaxy formation or the overabundance of predicted subhalos relative to the observed dwarf satellites of the Milky Way and M 31 (see e.g. Moore et al. 1999): for this reason, it would be useful to have a statistical sample of galaxy systems similar to our own Local Group.
Unfortunately the properties of poor galaxy systems, especially those comparable to the Local Group, are not well known. Zabludoff & Mulchaey (2000) have studied a sample of six nearby poor groups, finding evidence for a different luminosity function, with an increasing dwarf to giant galaxy ratio with the mass density of the system. More generally, Zabludoff & Mulchaey (1998, 2000) have examined the properties of 12 poor groups of galaxies with PSPC images: 9 of them have diffuse X-ray emission and a bright, central elliptical galaxy.
Our approach is complementary, as it selects another class of poor systems. In fact, a main problem is the bias on the properties of the selected galaxy groups due to the adopted selection criteria. A selection algorithm defines a priori the properties of the systems: well known examples are Abell clusters (Abell 1958) and Hickson compact groups (Hickson 1982). The introduction of automated methods can give a more objective selection, but it is obviously impossible to recover a system if only its most luminous member is present in the original photometric catalogue. Moreover, the typical friends-of-friends algorithms used to select "galaxy groups" require the detection of at least three neighbouring galaxies above the limiting magnitude of the catalogue (see e.g. White et al. 1999): this means that many groups are classified as "binaries''. It is clear that the problem becomes critical when going towards poorer and more distant systems, with increasing contamination and spurious detections.
Let us take the best example of
VLG system, i.e. our Local Group, which contains two VLGs: M 31 and
our Milky Way (with respectively MV=-21.2 and MV=-20.9,
see van den Bergh 1999 and references therein), and
is usually considered as a "typical group''.
If this is true, it is surely not reflected in group
catalogs, for a simple reason: VLGs are rare galaxies. For example,
the third brightest galaxy of the Local Group M 33 (with an absolute magnitude
MV=-18.9) would become fainter than mV=15.5 (i.e. fainter than
the limit of the SSRS2) already at
.
Therefore we do not know if the properties of
our Local Group are really "typical'', and only
looking deeper at VLG fields we can expect to find other groups
similar to our own.
In order to construct a statistical sample including, among others, also systems comparable to our Local Group, we have decided to investigate the environment of the VLGs listed in our catalogue defined in Paper I, which represent a volume-limited sample. The first step is to measure redshifts of fainter galaxies in the field of VLGs and determine the membership and velocity dispersion of the systems: in this paper we discuss data concerning the fields of 19 VLGs. In Sect. 2 we define our sample, with the VLG fields we observed at the Observatoire de Haute Provence and the selection of galaxies around VLGs extracted from the 2dFGRS; Sect. 3 presents the individual properties of the systems, while in Sect. 4 we discuss the relation between the VLGs and their environment. Our conclusions are in Sect. 5. In Appendix A we also discuss Arp 127, a pair identified in our preliminary selection as possibly including a VLG, and in Appendix B we give positions, magnitudes and redshifts of 2dFGRS galaxies in our VLG systems.
Three VLGs were selected from our catalogue of VLGs (see Table 1 in Paper I), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller & Huchra 1989); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue, which has an overlap with the SSRS2. While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I.
At the Observatoire de Haute-Provence we could observe only galaxies
at
,
while SSRS2 galaxies are south of
.
Among the 12 VLGs in our catalogue which satisfied
this declination constraint, we chose three VLGs around which
an inspection of DSS images had revealed the presence
of galaxies fainter
than the VLG but still bright enough to get a useful spectrum at
the 1.93 m telescope.
The selected VLGs are VLG 061, VLG 068 and VLG 074.
In order to cover the whole night, we included also
a VLG galaxy selected from the CfA catalogue (VLG 0716+5323), and Arp 127,
a galaxy we had included in a preliminary version of the VLG catalogue but
finally excluded for its discrepant redshift and the consequent uncertainty
on its absolute magnitude. This system is presented in Appendix A.
Our observations were carried out in 1997 at the 1.93 m telescope
with the Carelec spectrograph in long slit mode at the Cassegrain focus.
The grating dispersion was 260 Å/mm, corresponding to 7 Å with the
pixels of the Tektronix CCD.
Data reduction was performed with IRAF; calibrations were done
using the OHP He-Ar lamps.
Redshifts were measured with
xcsao in the rvsao package, using 5 star templates and
attributing to each galaxy the redshift given by the best-fitting template
(i.e. the one with the highest R parameter, see Tonry & Davis 1979).
One velocity standard star and one galaxy with velocity
measured from HI observations were also observed and used as a check of the
zero-point calibration, cross-correlating them with a subset of our spectra
and with our templates:
in both cases, the redshifts were consistent within 10 km s-1.
Positions and redshifts of the observed galaxies are listed in Table 1.
Iden. | RA (J2000) | Dec (J2000) | Vh (km s-1) | Error | Notes |
VLG 061 | 02 30 42.7 | -02 56 21 | 5719 | 31 | |
1 | 02 30 32.1 | -02 53 07 | 5950 | 24 | Emission lines |
2 | 02 30 44.7 | -02 53 58 | 5488 | 36 | |
3 | 02 30 46.4 | -02 57 06 | 5561 | 28 | |
4 | 02 30 47.6 | -02 54 32 | 5870 | 20 | Emission lines |
5 | 02 30 48.9 | -02 56 46 | 5189 | 91 | |
6 | 02 31 11.6 | -02 56 35 | 5847 | 31 | m=15.76 |
7 | 02 30 21.9 | -02 59 07 | 12 498 | 56 | |
VLG 068 | 03 25 11.5 | -06 10 52 | 9933 | 48 | V=10 107 m=13.97 |
MRK 0609 | 03 25 25.3 | -06 08 38 | 10 264 | 57 | V=10236 |
MRK 0610 | 03 25 31.4 | -06 07 43 | 10 408 | 55 | V=10301 |
VLG 074a | 04 08 07.4 | -08 49 45 | 9930 | 50 | NGC 1516A |
VLG 074b | 04 08 08.2 | -08 50 06 | 9864 | 45 | NGC 1516B |
1 | 04 07 45.3 | -08 44 26 | 10 073 | 37 | |
2 | 04 07 59.0 | -08 50 24 | 36 482 | 61 | |
3 | 04 08 00.3 | -08 49 24 | 46 248 | 65 |
![]() |
4 | 04 08 06.4 | -08 48 04 | 36 342 | 101 | |
5 | 04 08 12.1 | -08 56 11 | 42 342 | 95 | |
6 | 04 08 21.1 | -08 47 20 | 36 254 | 45 | |
VLG 0716+5323 | 07 16 41.2 | 53 23 09 | 19 069 | 41 | m=14.0, V=19307, X-ray |
1 | 07 16 19.9 | 53 21 51 | 137 | 17 | Star |
2 | 07 16 21.2 | 53 21 59 | 19 048 | 32 | |
3 | 07 16 24.4 | 53 21 37 | 19 573 | 25 | |
4 | 07 16 32.0 | 53 23 45 | 18 330 | 44 | |
5 | 07 16 38.1 | 53 15 38 | 19 781 | 47 | |
6 | 07 16 40.0 | 53 22 23 | 19 904 | 43 | |
7 | 07 16 43.1 | 53 22 55 | 20 522 | 73 | |
8 | 07 16 47.9 | 53 22 45 | 19 066 | 57 | |
9 | 07 17 29.2 | 53 24 45 | 19 043 | 42 |
Part of the SSRS2 region is covered by the 2dFRS
(see Colless et al. 2001), and we searched for
galaxies around VLG positions
in the presently available public catalogue (the "100k''
catalogue,
including more than 102 000 redshifts).
The limiting magnitude of the 2dFGRS is bJ=19.45;
within the maximum distance defined by the SSRS2 VLG volume-limited sample
(0.065), the 2dFGRS is volume-limited at M=-17
(of course the field incompleteness has to be taken into account).
We selected all galaxies in the 2dFGRS within a projected separation less than
1.5h-1 Mpc and a velocity difference less than 1500 km s-1 with respect to the
SSRS2 VLGs. The velocity cut was chosen to limit foreground and background
contamination, but large enough to include also marginal members.
We also applied a 3-
clipping (see e.g. Yahil & Vidal 1977) to the
velocity distribution.
The chosen value of the projected radius corresponds to one Abell radius and
it is also used as a criterion for determining the Local Group membership
(van den Bergh 1999). We found data for 19 VLG fields: in 4 cases
(VLG 003, VLG 008, VLG 054, VLG 075) we could retrieve only one redshift
(in addition to the VLG) with our selection limits.
Such cases deserve a more careful study and we will not include them in the
present work. We simply note here that VLG 075 is in a group
identified in the Las Campanas Redshift Survey (Tucker et al. 2000).
In the other 15 fields we could obtain at least 5 redshifts
(reduced to 3 by the 3
clipping in the case of VLG 022).
The images of the fields centered on the selected VLGs
(30 arcmin size in )
were retrieved from the
Digitized Sky Survey and are shown in Figs. 1
and 2.
In Appendix B and in tables available in electronic
form we give positions and redshifts of the 2dFGRS galaxies selected
according to the criteria defined above.
We have calculated the mean redshift and the velocity dispersion for each
VLG system; the main properties are shown in Table 2, where we
list in Col. (1) the VLG number, in Col. (2) the VLG morphological type,
in Col. (3) the total number of galaxies after applying
the 3-
clipping and used for measuring the mean redshift and velocity
dispersion, in Col. (4) the mean heliocentric redshift
with its error, in Col. (5) the velocity dispersion,
in Col. (6) the system type, when available from the literature.
With respect to the known systems listed in Table 2 of our Paper I, we could associate other 8 VLGs to galaxy systems, and increase the number of measured velocity dispersions: in fact only VLG 086 (in an Hickson compact group) and VLG 108 (in the ACO cluster A4038) had already an estimate of the velocity dispersion.
Ident. | Type | Nz | ![]() |
![]() |
System Type |
14 | Sbc | 14 |
![]() |
747 -114 +204 | Triplet |
22 | S0 | 3 |
![]() |
![]() |
SCG55 |
31 | D | 15 |
![]() |
720 -107 +188 | A151 |
40 | S | 10 |
![]() |
724 -127 +256 | -- |
43 | Sb | 15 |
![]() |
468 -72 +123 | -- |
45 | S | 21 |
![]() |
464 -62 +97 | -- |
48 | Sbc | 20 |
![]() |
378 -53 +82 | Binary |
53 | S0 | 33 |
![]() |
360 -41 +57 | -- |
61 | SB(rs)c | 7 |
![]() |
318 -67 +177 | -- |
68 | S Sy1 | 3 |
![]() |
![]() |
SSRS2 group |
69 | SB(s)b p | 8 |
![]() |
158 -46 +79 | Binary |
74 | S | 3 |
![]() |
![]() |
Binary |
83 | E | 31 |
![]() |
319 -38 +53 | S0983 |
86 | SB(s)bc p:Sy | 37 |
![]() |
669 -68 +96 | HCG91 |
93 | Sb | 15 |
![]() |
550 -83 +144 | -- |
94 | SAB(rs)p | 39 |
![]() |
413 -43 +59 | EDCC155 |
108 | cD | 114 |
![]() |
659 -41 +49 | A4038 |
109 | E | 13 |
![]() |
297 -52 +89 | S1155 |
VLGN 0716+5323 | E | 9 |
![]() |
609 +234 -109 | Z1261 |
In Fig. 3 we show the velocity histograms of the systems with at least 10 measured redshifts. The redshift of the VLG is indicated by a dashed line.
From Table 2, and also taking into account the 4 VLGs not included in this selection, it appears that all VLGs have companions. This is not so surprising, given the known correlation between galaxies, and confirms the idea that there are no truly "isolated'' galaxies. Moreover, it is quite striking that in the literature 6 out of the 18 SSRS2 VLGs were not associated to any system, while other 3 were classified simply as binaries: for example, VLG 048 belongs to a system for which we could collect 15 new redshifts from the 2dFGRS. Such a high number of nearby galaxy systems which were not previously identified neither in the optical nor in the X-ray reminds us how poorly known the low-mass end of galaxy systems is. Therefore it is interesting to examine in more detail the nature and environment in which VLGs are found. In the following, we briefly describe the main properties of the selected VLGs and their systems.
In Paper I we have shown that the correlation function of VLGs approaches that of clusters. Various galaxies discussed above (VLG 045, VLG 048, VLG 053) are within the Pisces-Cetus Supercluster, which appears as a prominent feature near the limiting depth of the SSRS2 volume-limited sample of VLGs (the presence of this structure might explain the excess of the VLG correlation amplitude measured in the SSRS2 with respect to the 2dFGRS). The Pisces-Cetus supercluster is well traced by Abell and ACO clusters (Tully 1986), but none of our VLGs is a member of those clusters. The VLG correlation function is large because VLGs trace large-scale fluctuations just as clusters do, not because they are in rich clusters.
Another interesting issue is the luminosity function of the VLG systems.
In principle, merging should have played a major role in the formation
of the elliptical VLGs, and the luminosity function of the associated system
might be different from those dominated by a spiral VLG.
As a preliminary test, we have estimated the composite luminosity
functions of early and late VLG dominated systems, excluding
both rich clusters and systems with probable field contamination. In this rough
comparison, we assume that selection effects are the same for the two types
of systems.
We have normalized numbers to the total number of galaxies in the two samples
(66 for spiral VLG and 71 for elliptical VLG systems).
In deriving absolute magnitudes, we applied the mean
correction formula
K = 0.03 z /(0.01+z4) adopted by Norberg et al. (2001); at the distances
of SSRS2 VLGs (
), it is consistent with the correction adopted
for the SSRS2 (da Costa et al. 1994; K = 3z). As apparent from
Fig. 4, taking into account the small
number of objects in our samples we cannot find significant differences between
the two luminosity functions to M=-17, the absolute limiting magnitude at
which galaxies around SSRS2 VLGs could still be detected in the 2dFGRS.
![]() |
Figure 4:
Normalized luminosity function of systems with an early type VLG
(red squares) and a late type VLG (blue triangles), with Poissonian
![]() |
There is however a difference when looking at the morphology
of the central VLG and the velocity dispersion of the associated system.
It is not surprising that
the VLGs which are at the center of clusters are giant ellipticals;
these clusters have
km s-1 and
an associated X-ray emission at a temperature consistent with their
velocity dispersion.
Other 3 systems including an early type VLG
(one S0 and two ellipticals)
have velocity dispersions in the range 300-350 km s-1,
and might be considered the low-mass end of galaxy clusters.
The remaining S0 in the sample is in a compact group with a small velocity
dispersion (
140 km s-1).
The systems dominated by a spiral VLG have a large spread
in velocity dispersion: but as we have seen from the velocity histograms,
those with the largest
velocity dispersions (700 km s-1), VLG 014, VLG 040 and VLG 086,
are probably affected by field contamination.
Moreover, for these systems no
extended X-ray emission is reported in the on-line databases.
Within the limits of the small statistics and lack of completeness, we can conclude that VLGs are in a qualitative agreement with the morphology-density relation: in clusters and rich groups we find only early type VLGs, while among systems originally classified as binaries or triplets, and those with the lowest velocity dispersions (with the exception of the S0 VLG 022) the VLG is a late-type.
The nearby systems we have observed at OHP have lower velocity dispersions,
and have probably also a lower richness but the limiting apparent magnitude
is also brighter for these systems.
The system more similar to our own Local Group is the one associated to
VLG 069. It has 10 galaxies with measured redshifts and
:
even if this is still not a complete sample, the number is comparable to
the Local Group, where we find 10 galaxies with
.
VLG 069 is the main member of a binary system, as Andromeda and the
Milky Way; moreover, the VLG 069 system has also a relatively low velocity
dispersion,
km s-1, still somewhat higher than
the velocity dispersion of the Local Group,
km s-1 (van den Bergh 1999, 2000), which is indeed lower than
the observed range of our VLG systems. However, our observational errors
would not allow us to measure accurately such a low velocity dispersion.
Our optical classification of VLG systems can be compared to the X-ray based classification of galaxy groups by Zabludoff & Mulchaey (1998), who distinguish groups with a bright, central elliptical galaxy and smooth X-ray emission from the hot IGM, and groups without X-ray emission, a few bright late-type galaxies with fainter members, like our Local Group. Our systems with an early-type VLG have generally velocity dispersion and richness comparable to the values found by ZM98 for their 9 poor groups with diffuse X-ray emission. They also find that the 3 groups without X-ray emission have a lower number of members, which seems also consistent with what we find. Zabludoff (2000) has suggested the possibile existence of a third class of groups in a transition phase, but it has still to be demonstrated that the differences between the two classes might be due to evolution instead of their different formation processes.
The number density of galaxies is dominated by faint, small systems.
As an example, let us assume a Schechter luminosity function
with
M* bJ=-19.6,
and
(Zucca et al. 2000).
The fraction of galaxies brighter than L* is in fact less than
2% of all galaxies with
.
The brightest galaxies with
are only 3 out of 10 000.
Among these galaxies, we find M 31 and probably the Milky Way
(see e.g. van den Berg 1999), which are therefore not typical galaxies,
but very special systems.
Nevertheless, when looking at the luminosity (mass) density,
the contribution of Very Luminous
Galaxies (VLGs) with
to the luminosity
density increases to 1.6% and that of
M* galaxies to nearly 30%. VLGs are extremely interesting
from the point of view of galaxy formation and large-scale structure.
They are visible at large distances (
h-1 Mpc
at the limiting magnitude of the SSRS2 mB=15.5)
and their distribution is biased with
respect to galaxies of lower luminosity.
There is a common misconception according to which optically very luminous galaxies selected with a large correlation amplitude are early-type galaxies in clusters. In this work we have shown that, at least choosing galaxies in the blue passband, this is not the case. We have presented our observations and 2dFGRS data concerning fields centered on SSRS2 VLGs: we have found clear evidence that VLGs are the brightest members of galaxy systems which can escape standard group finding methods, except of course for the minority of early-type VLGs in rich groups or clusters. VLGs have clustering properties similar to clusters, but most of them are in systems with a galaxy population comparable to loose groups, and some of them are probably comparable to our Local Group. The large correlation amplitude suggests that VLGs are in high density regions; most of them, being spirals, cannot have accreted more than a few percent of their mass through major merging episodes (Tóth & Ostriker 1992), so we have to suppose that these systems already formed with a large, central massive galaxy and low mass companions. On the other hand, the merging of two late-type VLGs could evolve into an early type system, analogously to what was suggested for poor groups by Zabludoff & Mulchaey (2000).
Other recent works appear to confirm the general properties of VLGs which we have found from the analysis of the SSRS2. Giuricin et al. (2001) have analysed the Nearby Optical Galaxy sample, finding a similar trend for the luminosity segregation, and that only 10% of their VLGs reside in clusters; they also find that, while the fraction of very luminous early-type galaxies is larger than the corresponding fraction for the total sample, it is still only 29%, less than than the fraction of Scd galaxies (39%). Moreover, from the analysis of the 2dFGRS Norberg et al. (2002) confirm that "luminosity, and not type, is the dominant factor in determining how the clustering strength of the whole galaxy population varies with luminosity''.
The amount of mass associated to VLG systems is still an open question. For example, the lower correlation amplitude for VLGs found in the 2dFGRS would indicate that VLGs are associated to dark halos less massive than typical halo clusters. The increase in local overdensity of galaxies around VLGs should also be better determined. In a recent paper Hogg et al. (2003) analyse the Sloan Digital Sky Survey and find the intriguing results that blue luminous galaxies with L < 3 L* are not apparently found in overdensities, but VLGs have even larger luminosities.
Therefore only further and deeper observations devoted to the detailed study of VLGs, determining the luminosity function of these systems and the dynamics of satellites around the VLGs, together with observations in redder passbands (more representative of the mass of the systems) will shed more light on the properties of VLGs and their environment, and their implications for galaxy formation and evolution.
Acknowledgements
This work has been partially supported by the Italian Space Agency grants ASI-I-R-105-00 and ASI-I-R-037-01, and by the Italian Ministery (MIUR) grant COFIN2001 "Clusters and groups of galaxies: the interplay between dark and baryonic matter". We thank the referee, Florence Durret, for her careful reading of the manuscript and useful comments.
Iden. | RA (2000) | Dec (2000) | Vh (km s-1) | Error | Bt Notes |
NGC 0191 | 00 38 59.3 | -09 00 09 | 6076 | 32 | 12.5 [13.68] |
IC 1563 | 00 39 00.2 | -09 00 53 | 6138 | 39 | 14.74 [14.39] |
0039-0931 | 00 39 02.0 | -09 00 31 | 13 652 | 141 |
The Arp 127 pair (Arp 1966) is made by NGC 0191, a spiral classified as
SAB(rs)c: pec, and IC 1563, an S0 pec sp. A third, more compact object
is seen among the two galaxies (see Fig. A.1). According to
the literature, the redshifts of NGC 0191 and
IC 1563 are respectively
km s-1 and
km s-1
(Huchra et al. 1993), a surprising difference given the apparent signs of
interactions; for this reason IC 1563 was not included in our final catalogue,
even if according to the quoted redshift and the
apparent magnitude (m = 14.74) it should be considered a VLG.
Our measurements for NGC 0191 and IC 1563 are reported in Table A.1, and show
that there is no discrepancy:
the binary system Arp 127 is at
km s-1, and the two galaxies have
a velocity difference of only
60 km s-1 -, i.e. they have the same
velocity taking into account the errors.
These two galaxies are clearly interacting, as shown by the tidal distortion
in NGC 0191.
We suggest that the redshift of 13 652 km s-1 should be attributed to the round object between the two galaxies. In fact Beers et al. (1991) report that value for the redshift giving the coordinates of the round object, but identify it as IC 1563, while Huchra et al. (1993) give the approximate coordinates of the Arp 127 system for both NGC 0191 and IC 1563. The velocity of the round object is in the lower part of the velocity range of the A85 galaxy cluster (see Durret et al. 1998) and at an angular distance of 44 arcmin from its center, and it might be a galaxy member of the cluster.
The new redshift for IC 1563 means that this galaxy has M=-19.2, i.e. it is a typical M* galaxy and not a VLG. In Table A.1 we report also the photometric observations of Reshetnikov & Combes (1996).
![]() |
Figure 1:
Finding charts of the VLG fields observed at OHP
(the scale is approximately
![]() |
![]() |
Figure 2:
Finding charts of the VLG fields selected from the 2dFGRS
(the scale is approximately
![]() |
In the following tables we list the 2dFGRS galaxies which we have selected as members of VLG systems. We give in Col. (1) our identification number, in Cols. (2) and (3) respectively right ascension and declination, in Col. (4) the bJ magnitude, and in Col. (5) the redshift.
We have listed the 2dFGRS data on the VLG when available, otherwise we have reported the SSRS2 data.
We could compare magnitudes and redshifts of the 2dFGRS and SSRS2 for
5 VLGs with 2dFGRS data (VLG 014, VLG 022, VLG 043, VLG 045, VLG 048, VLG 109):
we find an average velocity difference
<V (2dF) - V (SSRS2)> = 118 km s-1 with an rms of 155 km s-1 and
an average magnitude difference
<bJ (2dF) - mB (SSRS2)> =
0.20, with an rms of 0.46.
The magnitude difference is consistent with the
zero-point shift
expected between the blue magnitudes of the SSRS2
(Alonso et al. 1993, 1994; da Costa et al. 1994)
and the APM bJ magnitudes on which the 2dFGRS is based
(Maddox et al. 1990, 1990, 1996). Note that for bright galaxies,
magnitudes are
not very precise: the APM bJ magnitudes have a precision of
0.2 in the range 17-19.5 but are significantly affected by saturation at
magnitudes brighter than bJ = 16 (Norberg et al. 2002).
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 00 49 16.58 | -27 15 02.3 | 17.04 | 0.03514 | |
2 | 00 49 32.12 | -27 40 00.1 | 18.14 | 0.04093 | |
3 | 00 49 45.62 | -27 45 15.2 | 16.65 | 0.04012 | |
4 | 00 49 57.81 | -26 55 11.7 | 18.86 | 0.04342 | |
5 | 00 50 20.18 | -27 47 36.3 | 17.41 | 0.03942 | |
6 | 00 50 21.56 | -27 37 15.5 | 18.74 | 0.04076 | |
7 | 00 51 03.74 | -27 41 06.2 | 17.43 | 0.03996 | |
8 | 00 51 27.98 | -27 38 24.5 | 16.89 | 0.04005 | |
9 | 00 52 15.02 | -27 19 41.4 | 15.17 | 0.03983 | VLG014 |
10 | 00 52 15.58 | -27 01 35.9 | 18.13 | 0.03534 | |
11 | 00 52 15.64 | -27 20 58.1 | 15.62 | 0.04005 | |
13 | 00 52 25.52 | -26 59 17.6 | 16.96 | 0.03553 | |
13 | 00 52 40.97 | -27 15 51.2 | 18.21 | 0.03498 | |
14 | 00 53 11.23 | -26 47 31.7 | 19.32 | 0.03946 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 00 58 52.33 | -28 18 11.9 | 15.64 | 0.05753 | VLG022 |
2 | 00 58 55.81 | -28 19 30.2 | 16.53 | 0.05703 | |
3 | 01 00 58.93 | -28 21 39.9 | 19.28 | 0.05640 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 01 07 17.22 | -15 04 48.0 | 18.55 | 0.05560 | |
2 | 01 07 41.81 | -14 54 56.7 | 18.06 | 0.05044 | |
3 | 01 08 09.82 | -15 12 18.7 | 17.13 | 0.05197 | |
4 | 01 08 16.05 | -14 52 07.8 | 17.05 | 0.05272 | |
5 | 01 08 30.64 | -14 57 04.7 | 16.07 | 0.05112 | |
6 | 01 08 32.40 | -15 03 10.4 | 18.21 | 0.05184 | |
7 | 01 08 32.44 | -15 08 54.6 | 18.26 | 0.05371 | |
8 | 01 08 50.70 | -15 24 32.2 | 14.36 | 0.05326 | VLG031; data from SSRS2 |
9 | 01 09 40.52 | -14 55 50.5 | 17.47 | 0.05813 | |
10 | 01 10 15.95 | -15 18 17.3 | 17.28 | 0.05563 | |
11 | 01 10 20.67 | -15 18 08.1 | 17.44 | 0.05439 | |
12 | 01 10 21.68 | -15 15 22.1 | 18.09 | 0.05634 | |
13 | 01 10 25.17 | -15 15 24.8 | 15.39 | 0.05666 | |
14 | 01 10 26.38 | -15 18 57.4 | 17.59 | 0.05309 | |
15 | 01 10 27.46 | -15 06 43.1 | 17.58 | 0.04893 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 01 37 40.78 | -28 37 01.9 | 16.83 | 0.04254 | |
2 | 01 38 20.37 | -28 38 58.5 | 17.61 | 0.04307 | |
3 | 01 38 40.39 | -28 57 17.6 | 19.23 | 0.04067 | |
4 | 01 38 56.46 | -28 35 08.7 | 18.96 | 0.04261 | |
5 | 01 38 59.71 | -28 34 21.2 | 14.64 | 0.04212 | VLG040; data from SSRS2 |
6 | 01 39 21.29 | -29 00 42.2 | 17.28 | 0.04205 | |
7 | 01 41 07.26 | -29 07 42.7 | 18.16 | 0.03683 | |
8 | 01 41 47.60 | -28 12 26.4 | 19.37 | 0.03812 | |
9 | 01 41 48.65 | -28 31 28.7 | 17.00 | 0.03724 | |
10 | 01 41 55.43 | -28 32 53.0 | 15.77 | 0.03768 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 01 38 44.44 | -27 50 47.4 | 16.50 | 0.05666 | |
2 | 01 39 17.85 | -27 49 05.0 | 17.17 | 0.05702 | |
3 | 01 39 21.51 | -27 48 47.1 | 19.21 | 0.05596 | |
4 | 01 39 36.50 | -28 25 41.6 | 19.14 | 0.05888 | |
5 | 01 39 51.04 | -27 48 51.9 | 19.00 | 0.05674 | |
6 | 01 39 57.12 | -27 57 21.7 | 15.63 | 0.05640 | VLG043 |
7 | 01 40 03.08 | -27 59 04.0 | 18.05 | 0.05652 | |
8 | 01 40 31.09 | -28 04 36.2 | 19.14 | 0.05924 | |
9 | 01 40 39.96 | -27 28 58.6 | 18.82 | 0.05372 | |
10 | 01 40 55.41 | -27 49 40.2 | 18.62 | 0.05915 | |
11 | 01 41 30.07 | -27 46 31.8 | 17.52 | 0.05704 | |
12 | 01 41 37.09 | -27 45 33.0 | 18.61 | 0.05658 | |
13 | 01 41 42.11 | -27 40 18.1 | 17.03 | 0.05687 | |
14 | 01 41 44.35 | -28 07 23.1 | 19.43 | 0.05319 | |
15 | 01 42 19.91 | -27 59 36.8 | 18.75 | 0.05674 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 01 48 02.03 | -28 49 30.2 | 19.00 | 0.05580 | |
2 | 01 48 37.65 | -29 03 18.1 | 18.34 | 0.06024 | |
3 | 01 49 00.27 | -28 36 28.9 | 17.32 | 0.05612 | |
4 | 01 49 05.17 | -28 33 57.5 | 17.00 | 0.05547 | |
5 | 01 49 12.19 | -28 37 10.2 | 18.86 | 0.05607 | |
6 | 01 49 22.26 | -28 57 38.4 | 18.04 | 0.05604 | |
7 | 01 49 40.19 | -29 15 21.7 | 19.04 | 0.05552 | |
8 | 01 50 05.55 | -28 49 54.0 | 18.56 | 0.05576 | |
9 | 01 50 06.99 | -28 49 17.0 | 18.36 | 0.05756 | |
10 | 01 50 08.49 | -28 45 46.1 | 18.20 | 0.05769 | |
11 | 01 50 14.15 | -28 52 18.0 | 14.96 | 0.05759 | VLG045 |
12 | 01 50 20.74 | -29 05 32.0 | 18.83 | 0.05736 | |
13 | 01 50 43.56 | -28 58 56.4 | 17.04 | 0.05606 | |
14 | 01 50 44.60 | -29 11 10.0 | 17.92 | 0.06084 | |
15 | 01 51 00.56 | -28 54 27.9 | 16.66 | 0.05802 | |
16 | 01 51 01.84 | -29 15 35.9 | 18.64 | 0.05592 | |
17 | 01 51 04.92 | -28 59 50.8 | 19.41 | 0.05723 | |
18 | 01 51 11.10 | -28 54 42.2 | 17.54 | 0.05622 | |
19 | 01 51 32.85 | -28 29 32.6 | 18.04 | 0.05681 | |
20 | 01 51 35.00 | -28 55 42.8 | 18.70 | 0.06092 | |
21 | 01 51 39.92 | -28 30 14.8 | 19.09 | 0.05707 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 01 53 13.63 | -27 54 33.2 | 19.06 | 0.05883 | |
2 | 01 53 16.97 | -27 49 32.7 | 17.14 | 0.06007 | |
3 | 01 53 34.87 | -28 34 07.0 | 17.54 | 0.05741 | |
4 | 01 53 55.02 | -28 14 37.4 | 19.32 | 0.05816 | |
5 | 01 54 11.90 | -28 23 02.1 | 17.01 | 0.05745 | |
6 | 01 54 12.78 | -27 51 57.1 | 16.90 | 0.06024 | |
7 | 01 54 13.11 | -27 52 19.7 | 17.94 | 0.05717 | |
8 | 01 54 26.25 | -27 47 43.0 | 18.43 | 0.06103 | |
9 | 01 54 27.30 | -27 51 08.0 | 19.30 | 0.06021 | |
10 | 01 54 29.09 | -28 27 22.4 | 17.76 | 0.05686 | |
11 | 01 54 39.87 | -27 59 20.8 | 18.40 | 0.06010 | |
12 | 01 54 41.67 | -28 10 10.2 | 19.31 | 0.05614 | |
13 | 01 54 48.16 | -28 11 45.5 | 19.13 | 0.05954 | |
14 | 01 54 48.72 | -28 08 56.8 | 15.66 | 0.05726 | VLG048 |
15 | 01 55 03.18 | -28 12 57.9 | 18.96 | 0.05750 | |
16 | 01 55 09.03 | -27 41 35.3 | 19.45 | 0.05734 | |
17 | 01 55 15.56 | -28 11 37.6 | 18.81 | 0.05818 | |
18 | 01 55 39.26 | -27 53 56.5 | 19.10 | 0.05897 | |
19 | 01 55 49.42 | -28 00 13.2 | 17.53 | 0.05813 | |
20 | 01 56 35.77 | -27 55 39.7 | 19.32 | 0.05789 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 02 11 25.59 | -26 49 51.0 | 17.93 | 0.05572 | |
2 | 02 11 48.77 | -26 35 24.5 | 18.28 | 0.05744 | |
3 | 02 12 07.18 | -26 46 18.8 | 16.03 | 0.05566 | |
4 | 02 12 07.92 | -26 49 38.9 | 17.72 | 0.05555 | |
5 | 02 12 27.64 | -26 38 18.4 | 18.76 | 0.05903 | |
6 | 02 12 36.11 | -26 30 03.9 | 17.25 | 0.05513 | |
7 | 02 12 36.71 | -26 38 29.8 | 18.46 | 0.05650 | |
8 | 02 12 40.02 | -26 29 11.6 | 18.10 | 0.05770 | |
9 | 02 12 40.28 | -26 45 21.8 | 19.04 | 0.05890 | |
10 | 02 12 43.66 | -26 09 50.9 | 17.70 | 0.05882 | |
11 | 02 12 44.45 | -26 27 28.1 | 19.16 | 0.05765 | |
12 | 02 12 49.00 | -26 27 35.0 | 15.16 | 0.05695 | VLG053; data from SSRS2 |
13 | 02 12 51.77 | -26 24 39.8 | 18.56 | 0.05715 | |
14 | 02 12 52.89 | -26 47 58.4 | 15.15 | 0.05634 | |
15 | 02 12 53.46 | -26 39 42.3 | 18.70 | 0.05724 | |
16 | 02 12 54.13 | -26 25 20.2 | 17.02 | 0.05721 | |
17 | 02 12 57.90 | -26 42 24.9 | 18.37 | 0.05536 | |
18 | 02 13 04.47 | -26 40 04.4 | 18.56 | 0.05652 | |
19 | 02 13 08.44 | -26 30 11.9 | 18.62 | 0.05749 | |
20 | 02 13 27.83 | -26 48 41.7 | 18.38 | 0.05891 | |
21 | 02 13 31.14 | -26 25 39.3 | 19.21 | 0.05916 | |
22 | 02 13 35.09 | -26 34 47.2 | 17.00 | 0.05752 | |
23 | 02 13 38.35 | -26 50 23.4 | 19.34 | 0.05890 | |
24 | 02 13 45.41 | -26 49 17.1 | 18.78 | 0.05958 | |
25 | 02 13 46.08 | -26 46 12.7 | 17.96 | 0.05881 | |
26 | 02 14 02.66 | -26 27 38.3 | 16.82 | 0.05832 | |
27 | 02 14 06.69 | -26 31 21.9 | 18.30 | 0.05605 | |
28 | 02 14 07.28 | -26 29 43.4 | 18.80 | 0.05658 | |
29 | 02 14 22.41 | -26 39 48.9 | 16.69 | 0.05909 | |
30 | 02 14 33.71 | -26 28 02.9 | 18.24 | 0.05676 | |
31 | 02 14 46.39 | -26 35 14.0 | 18.70 | 0.05941 | |
32 | 02 14 51.04 | -26 39 37.1 | 15.77 | 0.05784 | |
33 | 02 14 58.37 | -26 16 18.9 | 18.87 | 0.05661 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 03 29 13.06 | -28 07 47.8 | 19.37 | 0.03771 | |
2 | 03 29 20.35 | -28 09 10.5 | 18.78 | 0.03778 | |
3 | 03 29 20.92 | -28 08 00.9 | 14.22 | 0.03773 | |
4 | 03 29 32.13 | -28 09 35.4 | 16.55 | 0.03818 | |
5 | 03 29 56.13 | -28 46 14.5 | 14.09 | 0.03647 | companion of the VLG? |
6 | 03 29 56.79 | -28 46 29.8 | 13.95 | 0.03687 | VLG069; data from SSRS2 |
7 | 03 29 58.84 | -28 43 35.5 | 15.23 | 0.03830 | |
8 | 03 30 11.98 | -28 59 49.0 | 19.20 | 0.03778 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 21 58 44.19 | -19 05 08.0 | 17.22 | 0.05913 | |
2 | 21 58 49.05 | -19 09 46.3 | 18.51 | 0.05877 | |
3 | 21 58 55.66 | -19 03 13.7 | 19.04 | 0.05817 | |
4 | 21 58 57.89 | -19 20 14.5 | 17.03 | 0.05751 | |
5 | 21 59 10.30 | -19 17 13.3 | 17.78 | 0.05682 | |
6 | 21 59 10.32 | -19 24 23.5 | 18.91 | 0.05777 | |
7 | 21 59 19.18 | -19 22 53.1 | 15.76 | 0.05814 | |
8 | 21 59 31.49 | -19 06 59.1 | 18.34 | 0.05715 | |
9 | 21 59 36.35 | -19 22 03.7 | 18.45 | 0.05788 | |
10 | 21 59 40.51 | -19 10 40.1 | 18.32 | 0.05752 | |
11 | 21 59 43.73 | -19 16 26.5 | 19.16 | 0.05901 | |
12 | 21 59 48.86 | -19 20 01.8 | 18.14 | 0.05814 | |
13 | 21 59 52.95 | -19 04 50.0 | 18.70 | 0.05691 | |
14 | 21 59 56.81 | -19 06 06.6 | 19.01 | 0.05808 | |
15 | 22 00 04.31 | -19 09 58.3 | 19.18 | 0.05778 | |
16 | 22 00 05.40 | -19 12 16.0 | 15.48 | 0.05858 | VLG083; data from SSRS2 |
17 | 22 00 07.52 | -19 12 38.5 | 17.93 | 0.05731 | |
18 | 22 00 10.74 | -19 02 48.0 | 18.20 | 0.05872 | |
19 | 22 00 13.16 | -18 50 12.4 | 19.19 | 0.05848 | |
20 | 22 00 22.42 | -18 43 14.8 | 18.99 | 0.05777 | |
21 | 22 00 24.22 | -19 09 11.0 | 16.90 | 0.05830 | |
22 | 22 00 49.05 | -19 00 57.6 | 17.65 | 0.05588 | |
23 | 22 00 55.20 | -19 19 58.5 | 18.74 | 0.05701 | |
24 | 22 00 56.22 | -19 09 11.8 | 19.15 | 0.05646 | |
25 | 22 01 04.69 | -19 01 04.6 | 16.84 | 0.05713 | |
26 | 22 01 28.62 | -19 23 53.1 | 17.34 | 0.05860 | |
27 | 22 01 34.80 | -19 26 41.1 | 18.37 | 0.05715 | |
28 | 22 01 43.74 | -19 19 19.4 | 17.46 | 0.05709 | |
29 | 22 01 56.98 | -19 22 54.9 | 17.99 | 0.05755 | |
30 | 22 02 05.65 | -19 23 45.2 | 17.24 | 0.05694 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 22 03 38.55 | -27 58 32.7 | 18.02 | 0.02329 | |
2 | 22 03 41.79 | -27 56 07.2 | 15.03 | 0.02014 | |
3 | 22 03 45.74 | -27 47 52.5 | 15.50 | 0.02327 | |
4 | 22 03 54.11 | -27 51 30.5 | 19.14 | 0.02155 | |
5 | 22 04 03.25 | -27 29 38.5 | 16.18 | 0.02316 | |
6 | 22 04 57.79 | -28 05 18.4 | 19.01 | 0.02291 | |
7 | 22 06 14.11 | -27 57 14.8 | 14.32 | 0.02400 | |
8 | 22 06 21.29 | -27 35 22.0 | 17.69 | 0.02014 | |
9 | 22 06 34.06 | -27 59 30.8 | 14.99 | 0.02287 | |
10 | 22 06 36.75 | -27 48 05.3 | 18.89 | 0.02312 | |
11 | 22 06 38.17 | -27 57 24.7 | 17.65 | 0.02331 | |
12 | 22 07 27.04 | -27 55 34.9 | 18.67 | 0.02309 | |
13 | 22 07 33.04 | -27 44 51.8 | 18.98 | 0.02066 | |
14 | 22 07 57.11 | -28 15 01.2 | 16.43 | 0.02593 | |
15 | 22 08 12.28 | -27 05 56.1 | 16.83 | 0.01956 | |
16 | 22 08 26.36 | -28 13 07.7 | 19.21 | 0.02689 | |
17 | 22 08 33.09 | -27 56 12.1 | 18.88 | 0.02331 | |
18 | 22 08 50.20 | -26 54 05.3 | 18.25 | 0.01885 | |
19 | 22 09 07.45 | -27 48 22.8 | 14.19 | 0.02298 | |
20 | 22 09 07.68 | -27 48 34.1 | 13.05 | 0.02279 | VLG086; data from SSRS2 |
21 | 22 09 13.08 | -27 34 03.9 | 15.70 | 0.02352 | |
22 | 22 09 14.08 | -27 46 57.1 | 14.66 | 0.02431 | |
23 | 22 09 14.28 | -27 24 11.8 | 14.98 | 0.02373 | |
24 | 22 09 16.29 | -27 43 50.0 | 15.09 | 0.02398 | |
25 | 22 09 38.77 | -27 33 18.2 | 19.00 | 0.02481 | |
26 | 22 09 43.74 | -27 35 56.1 | 18.48 | 0.02359 | |
27 | 22 09 47.10 | -26 53 02.7 | 18.91 | 0.02141 | |
28 | 22 09 50.52 | -27 32 06.0 | 15.18 | 0.02450 | |
29 | 22 09 52.15 | -27 37 53.8 | 19.03 | 0.02586 | |
30 | 22 11 52.69 | -27 18 45.2 | 19.15 | 0.02410 | |
31 | 22 12 20.97 | -27 29 17.1 | 15.93 | 0.02374 | |
32 | 22 12 29.62 | -27 54 17.8 | 18.65 | 0.02740 | |
33 | 22 13 23.04 | -27 56 01.9 | 18.34 | 0.02404 | |
34 | 22 13 23.52 | -27 13 10.6 | 14.00 | 0.02375 | |
35 | 22 13 28.77 | -28 07 17.6 | 19.05 | 0.02691 | |
36 | 22 13 56.58 | -27 30 31.3 | 17.21 | 0.01765 | |
37 | 22 14 39.41 | -27 27 52.0 | 13.97 | 0.01789 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 22 29 45.57 | -30 28 30.1 | 18.88 | 0.05894 | |
2 | 22 29 49.89 | -30 12 24.9 | 18.62 | 0.05316 | |
3 | 22 29 50.60 | -30 31 02.9 | 14.73 | 0.05356 | VLG093; data from SSRS2 |
4 | 22 29 55.77 | -30 32 39.7 | 18.06 | 0.05389 | |
5 | 22 30 11.21 | -30 21 19.5 | 19.32 | 0.05700 | |
6 | 22 30 15.05 | -30 47 03.4 | 18.35 | 0.05868 | |
7 | 22 30 17.94 | -30 44 42.8 | 17.93 | 0.05788 | |
8 | 22 30 21.04 | -30 51 48.2 | 19.14 | 0.05832 | |
9 | 22 30 23.39 | -30 40 56.3 | 18.69 | 0.05686 | |
10 | 22 30 29.91 | -30 59 31.5 | 18.07 | 0.05709 | |
11 | 22 30 36.86 | -30 16 37.8 | 19.21 | 0.05513 | |
12 | 22 30 37.17 | -30 37 41.3 | 17.81 | 0.05815 | |
13 | 22 30 41.06 | -30 26 09.7 | 18.83 | 0.05492 | |
14 | 22 30 50.02 | -30 24 01.5 | 19.06 | 0.05778 | |
15 | 22 31 02.16 | -30 43 12.8 | 18.28 | 0.05793 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 22 29 36.48 | -25 01 38.5 | 17.52 | 0.03260 | |
2 | 22 29 42.08 | -25 27 31.0 | 19.13 | 0.03231 | |
3 | 22 30 04.41 | -24 59 05.2 | 17.98 | 0.03186 | |
4 | 22 30 07.11 | -24 58 22.4 | 14.56 | 0.03116 | |
5 | 22 30 12.09 | -25 18 47.6 | 19.25 | 0.03302 | |
6 | 22 30 23.82 | -25 28 10.0 | 18.24 | 0.03317 | |
7 | 22 30 35.88 | -24 36 56.9 | 17.77 | 0.03363 | |
8 | 22 30 44.70 | -25 43 14.6 | 18.85 | 0.03620 | |
9 | 22 30 57.29 | -25 10 45.9 | 15.75 | 0.03384 | |
10 | 22 31 02.76 | -25 20 34.8 | 15.12 | 0.03296 | |
11 | 22 31 17.61 | -24 58 07.8 | 19.26 | 0.03129 | |
12 | 22 31 17.97 | -24 43 58.5 | 15.98 | 0.03410 | |
13 | 22 31 27.37 | -25 15 41.5 | 18.41 | 0.03502 | |
14 | 22 31 31.09 | -25 53 13.0 | 15.03 | 0.03458 | |
15 | 22 31 32.05 | -25 25 12.9 | 15.79 | 0.03376 | |
16 | 22 31 41.06 | -25 13 36.6 | 16.67 | 0.03378 | |
17 | 22 31 41.66 | -25 30 21.0 | 18.84 | 0.03589 | |
18 | 22 31 49.74 | -25 26 28.5 | 16.57 | 0.03190 | |
19 | 22 31 55.43 | -25 30 39.9 | 17.04 | 0.03163 | |
20 | 22 31 58.81 | -25 21 39.3 | 15.40 | 0.03617 | |
21 | 22 31 59.49 | -25 32 55.6 | 16.05 | 0.03310 | |
22 | 22 32 03.77 | -25 38 47.8 | 18.83 | 0.03435 | |
23 | 22 32 07.45 | -25 24 53.4 | 18.35 | 0.03132 | |
24 | 22 32 08.10 | -25 23 51.0 | 13.92 | 0.03409 | VLG094; data from SSRS2 |
25 | 22 32 11.88 | -26 00 19.7 | 18.77 | 0.03234 | |
26 | 22 32 13.43 | -25 23 27.7 | 16.52 | 0.03406 | |
27 | 22 32 17.26 | -25 13 57.4 | 16.99 | 0.03179 | |
28 | 22 32 17.77 | -25 18 49.4 | 18.46 | 0.03668 | |
29 | 22 32 25.17 | -25 20 33.0 | 18.53 | 0.03347 | |
30 | 22 32 26.99 | -25 25 35.3 | 15.76 | 0.03632 | |
31 | 22 32 33.25 | -25 16 29.4 | 17.15 | 0.03415 | |
32 | 22 32 55.19 | -26 02 16.9 | 18.10 | 0.03246 | |
33 | 22 34 29.62 | -25 43 07.3 | 15.20 | 0.03330 | |
34 | 22 34 49.05 | -25 14 29.0 | 16.51 | 0.03396 | |
35 | 22 34 49.93 | -25 36 01.7 | 17.20 | 0.03463 | |
36 | 22 35 10.71 | -25 02 56.7 | 16.75 | 0.03465 | |
37 | 22 35 18.30 | -25 06 56.8 | 15.76 | 0.03323 | |
38 | 22 35 26.06 | -25 04 29.3 | 14.65 | 0.03409 | |
39 | 22 35 39.69 | -25 06 35.8 | 18.45 | 0.03474 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 23 43 15.45 | -28 14 26.7 | 17.35 | 0.02836 | |
2 | 23 43 23.27 | -28 11 17.9 | 17.80 | 0.02845 | |
3 | 23 43 35.67 | -28 06 04.0 | 16.67 | 0.02974 | |
4 | 23 44 22.30 | -28 11 44.6 | 17.69 | 0.02787 | |
5 | 23 44 38.81 | -27 39 34.5 | 15.93 | 0.03031 | |
6 | 23 45 03.76 | -27 59 11.9 | 17.99 | 0.02987 | |
7 | 23 45 03.84 | -27 20 41.4 | 16.80 | 0.02782 | |
8 | 23 45 16.64 | -27 18 57.1 | 18.02 | 0.02784 | |
9 | 23 45 28.01 | -27 57 49.0 | 16.63 | 0.03058 | |
10 | 23 45 32.63 | -27 37 21.8 | 19.36 | 0.02647 | |
11 | 23 45 34.49 | -28 10 48.0 | 17.67 | 0.02811 | |
12 | 23 45 40.30 | -27 51 48.8 | 16.91 | 0.02876 | |
13 | 23 45 41.19 | -27 48 27.8 | 17.65 | 0.03093 | |
14 | 23 45 52.57 | -28 02 53.0 | 17.86 | 0.03008 | |
15 | 23 45 55.71 | -28 13 52.1 | 18.53 | 0.02636 | |
16 | 23 46 00.76 | -27 53 44.3 | 17.30 | 0.02871 | |
17 | 23 46 16.09 | -27 30 37.3 | 15.99 | 0.02933 | |
18 | 23 46 22.83 | -28 00 18.4 | 15.34 | 0.02696 | |
19 | 23 46 38.39 | -28 15 11.4 | 16.81 | 0.02665 | |
20 | 23 46 41.44 | -27 58 04.4 | 18.95 | 0.02947 | |
21 | 23 46 43.40 | -27 56 01.9 | 18.23 | 0.03097 | |
22 | 23 46 44.02 | -27 50 29.2 | 17.93 | 0.03259 | |
23 | 23 46 45.76 | -27 49 23.7 | 18.60 | 0.03180 | |
24 | 23 46 47.33 | -27 33 21.2 | 17.88 | 0.02878 | |
25 | 23 46 49.87 | -28 10 08.9 | 16.02 | 0.03251 | |
26 | 23 46 50.07 | -27 57 29.1 | 17.96 | 0.03142 | |
27 | 23 46 53.00 | -27 34 47.8 | 16.68 | 0.03142 | |
28 | 23 46 54.99 | -28 21 42.6 | 15.62 | 0.02425 | |
29 | 23 46 58.15 | -28 02 55.6 | 17.71 | 0.02706 | |
30 | 23 47 11.34 | -28 14 25.5 | 18.00 | 0.02472 | |
31 | 23 47 12.08 | -27 55 48.4 | 15.98 | 0.02963 | |
32 | 23 47 13.29 | -28 01 03.0 | 16.63 | 0.03345 | |
33 | 23 47 14.15 | -28 01 48.9 | 17.72 | 0.02826 | |
34 | 23 47 14.39 | -28 11 35.7 | 16.62 | 0.02922 | |
35 | 23 47 14.80 | -27 57 27.9 | 14.65 | 0.02884 | |
36 | 23 47 17.39 | -28 13 37.9 | 18.08 | 0.03289 | |
37 | 23 47 20.14 | -28 03 46.7 | 17.08 | 0.02787 | |
38 | 23 47 22.36 | -27 58 32.6 | 16.79 | 0.02475 | |
39 | 23 47 23.22 | -28 07 09.0 | 16.36 | 0.03283 | |
40 | 23 47 27.39 | -27 27 56.1 | 16.80 | 0.02838 | |
41 | 23 47 28.56 | -28 06 33.3 | 14.76 | 0.02792 | |
42 | 23 47 28.84 | -28 08 08.3 | 14.81 | 0.02799 | |
43 | 23 47 30.17 | -27 39 44.0 | 15.43 | 0.02887 | |
44 | 23 47 30.63 | -28 02 35.5 | 17.28 | 0.02780 | |
45 | 23 47 30.77 | -27 56 05.3 | 18.56 | 0.02733 | |
46 | 23 47 31.80 | -28 06 26.1 | 16.43 | 0.02783 | |
47 | 23 47 34.67 | -28 09 16.0 | 17.62 | 0.03218 | |
48 | 23 47 38.14 | -27 44 45.2 | 18.45 | 0.03141 | |
49 | 23 47 41.98 | -28 04 51.4 | 19.36 | 0.03049 | |
50 | 23 47 42.10 | -28 07 33.8 | 17.25 | 0.02946 | |
51 | 23 47 42.33 | -27 59 54.0 | 17.56 | 0.02943 | |
52 | 23 47 44.71 | -27 29 13.9 | 14.86 | 0.02976 | |
53 | 23 47 45.00 | -28 08 27.0 | 13.78 | 0.02916 | VLG108; data from SSRS2 |
54 | 23 47 45.53 | -27 49 49.3 | 17.98 | 0.03149 | |
55 | 23 47 47.16 | -28 08 06.5 | 17.61 | 0.02699 | |
56 | 23 47 49.34 | -28 17 28.7 | 17.92 | 0.02979 | |
57 | 23 47 49.54 | -28 05 12.4 | 17.31 | 0.03214 | |
58 | 23 47 49.54 | -28 12 13.8 | 16.99 | 0.03178 | |
59 | 23 47 50.41 | -28 09 08.8 | 17.74 | 0.03289 | |
60 | 23 47 52.55 | -28 06 13.8 | 18.45 | 0.03336 | |
61 | 23 47 55.83 | -28 14 25.8 | 18.66 | 0.03174 | |
62 | 23 47 58.53 | -27 56 11.5 | 18.94 | 0.03119 | |
63 | 23 48 00.86 | -28 09 22.9 | 19.18 | 0.03220 | |
64 | 23 48 03.81 | -27 53 01.7 | 18.39 | 0.03051 | |
65 | 23 48 05.68 | -27 43 42.6 | 19.04 | 0.02868 | |
66 | 23 48 11.40 | -27 55 58.6 | 18.54 | 0.03402 | |
67 | 23 48 20.23 | -27 55 11.6 | 18.26 | 0.03406 | |
68 | 23 48 26.86 | -27 51 20.1 | 17.41 | 0.02998 | |
69 | 23 48 27.14 | -27 47 44.5 | 18.97 | 0.03304 | |
70 | 23 48 40.31 | -27 52 31.3 | 18.78 | 0.03192 | |
71 | 23 48 48.75 | -27 41 58.5 | 17.98 | 0.03400 | |
72 | 23 48 54.69 | -27 49 03.6 | 17.13 | 0.03410 | |
73 | 23 49 05.07 | -27 44 47.4 | 18.94 | 0.02661 | |
74 | 23 49 05.47 | -28 50 12.3 | 18.87 | 0.02953 | |
75 | 23 49 11.19 | -27 39 06.2 | 18.05 | 0.02890 | |
76 | 23 49 21.48 | -28 32 30.2 | 16.60 | 0.02913 | |
77 | 23 49 33.91 | -28 27 25.6 | 18.22 | 0.02695 | |
78 | 23 49 44.75 | -28 15 41.9 | 17.65 | 0.02861 | |
79 | 23 49 44.76 | -28 00 20.0 | 18.30 | 0.03121 | |
80 | 23 49 51.09 | -27 57 01.2 | 14.54 | 0.02996 | |
81 | 23 49 57.42 | -27 58 49.0 | 18.05 | 0.03364 | |
82 | 23 50 00.20 | -28 11 26.1 | 17.02 | 0.03199 | |
83 | 23 50 00.69 | -27 55 46.3 | 19.22 | 0.03025 | |
84 | 23 50 06.33 | -27 25 46.2 | 18.79 | 0.03349 | |
85 | 23 50 20.04 | -27 38 49.0 | 17.57 | 0.02885 | |
86 | 23 50 21.56 | -28 20 36.1 | 18.60 | 0.02506 | |
87 | 23 50 24.70 | -27 56 25.8 | 15.42 | 0.02916 | |
88 | 23 50 27.55 | -28 20 23.2 | 18.53 | 0.02739 | |
89 | 23 50 30.75 | -27 32 13.1 | 16.91 | 0.03411 | |
90 | 23 50 35.11 | -27 47 45.2 | 15.62 | 0.02959 | |
91 | 23 50 35.65 | -28 07 42.8 | 16.59 | 0.02858 | |
92 | 23 50 37.30 | -28 35 54.3 | 18.28 | 0.02799 | |
93 | 23 50 37.95 | -28 26 04.5 | 14.86 | 0.02839 | |
94 | 23 50 53.02 | -28 03 29.9 | 17.44 | 0.02771 | |
95 | 23 51 00.47 | -27 56 17.1 | 15.82 | 0.02982 | |
96 | 23 51 02.82 | -27 47 51.3 | 16.78 | 0.02912 | |
97 | 23 51 03.64 | -28 21 00.8 | 16.41 | 0.02757 | |
98 | 23 51 06.50 | -28 09 05.5 | 18.04 | 0.02742 | |
99 | 23 51 07.01 | -27 48 44.0 | 17.61 | 0.02978 | |
100 | 23 51 11.37 | -28 06 06.2 | 19.29 | 0.02951 | |
101 | 23 51 19.10 | -27 58 27.8 | 15.45 | 0.03360 | |
102 | 23 51 24.97 | -28 35 44.8 | 17.11 | 0.02897 | |
103 | 23 51 25.67 | -28 28 51.1 | 17.39 | 0.02705 | |
104 | 23 51 26.91 | -28 03 07.9 | 17.28 | 0.03219 | |
105 | 23 51 35.63 | -28 17 13.5 | 17.48 | 0.02817 | |
106 | 23 51 36.69 | -28 21 53.2 | 14.40 | 0.02758 | |
107 | 23 51 39.58 | -28 35 32.1 | 16.65 | 0.02789 | |
108 | 23 51 41.85 | -28 04 26.7 | 18.91 | 0.03285 | |
109 | 23 51 48.02 | -28 18 46.9 | 17.55 | 0.02933 | |
110 | 23 51 50.29 | -28 17 37.6 | 17.21 | 0.02777 | |
111 | 23 51 50.36 | -27 57 55.1 | 15.11 | 0.02927 | |
112 | 23 51 54.42 | -27 55 48.3 | 14.55 | 0.02921 | |
113 | 23 51 54.55 | -27 59 03.6 | 18.22 | 0.03317 | |
114 | 23 52 02.00 | -28 11 34.5 | 17.41 | 0.03109 |
Iden. | RA (J2000) | DEC (J2000) | bJ | Redshift | |
1 | 23 47 48.41 | -28 56 38.9 | 18.62 | 0.04815 | |
2 | 23 47 56.85 | -29 18 08.3 | 17.82 | 0.04885 | |
3 | 23 49 21.95 | -29 10 22.2 | 17.46 | 0.04869 | |
4 | 23 49 39.21 | -28 56 30.1 | 16.53 | 0.04731 | |
5 | 23 49 44.29 | -29 16 23.6 | 19.05 | 0.05044 | |
6 | 23 49 52.57 | -28 49 41.2 | 18.51 | 0.04989 | |
7 | 23 50 13.62 | -29 00 32.3 | 14.31 | 0.04973 | VLG 109 |
8 | 23 50 15.62 | -29 08 09.2 | 15.08 | 0.05062 | |
9 | 23 50 16.65 | -28 59 50.2 | 18.88 | 0.05058 | |
10 | 23 50 26.60 | -29 06 16.6 | 18.71 | 0.04857 | |
11 | 23 50 34.41 | -29 02 03.2 | 17.16 | 0.04920 | |
12 | 23 50 36.89 | -29 06 58.4 | 16.80 | 0.04977 | |
13 | 23 50 43.89 | -28 57 24.8 | 16.11 | 0.04778 |