A&A 396, 449-461 (2002)
DOI: 10.1051/0004-6361:20021403
G. Gavazzi 1 - A. Boselli 2 - P. Pedotti 1 - A. Gallazzi 1 - L. Carrasco 3,4
1 - Università degli Studi di Milano-Bicocca, Piazza delle scienze 3, 20126 Milano, Italy
2 -
Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille
Cedex 12, France
3 -
Instituto Nacional de Astrofísica, Optica y Electrónica,
Apartado Postal 51. C.P. 72000 Puebla, Pue., México
4 -
Observatorio Astronómico Nacional, UNAM, Apartado Postal 877, C.P. 22860, Ensenada B.C., México
Received 31 July 2002 / Accepted 20 September 2002
Abstract
H+[NII] imaging observations of 369 late-type (spiral) galaxies in the Virgo cluster and in
the Coma/A1367 supercluster are analyzed, covering 3 rich nearby clusters (A1367, Coma and Virgo)
and nearly isolated galaxies in the Great-Wall.
They constitute an optically selected sample (mp<16.0) observed with
completeness.
These observations provide us with the current (T<107 yrs) star formation
properties of galaxies that we study as a function of
the clustercentric projected distances (
). The expected decrease of the star formation rate (SFR),
as traced by the H
EW,
with decreasing
is found only when galaxies brighter than
are considered. Fainter objects
show no or reverse trends.
We also include in our analysis Near Infrared data, providing information on the old (T>109 yrs)
stars. Put together, the young and the old stellar indicators give the ratio of
currently formed stars over the stars formed in the past, or "birthrate'' parameter b. For the considered galaxies
we also determine the "global gas content'' combining HI with CO observations. We define the
"gas deficiency'' parameter as the logarithmic difference between the gas content of isolated galaxies
of a given Hubble type and the measured gas content.
For the isolated objects we find that b decreases with increasing NIR luminosity.
In other words less massive galaxies are currently forming stars at a higher rate than
their giant counterparts which experienced most of their star formation activity at earlier
cosmological epochs.
The gas-deficient objects, primarily members of the Virgo cluster, have a birthrate significantly lower than
the isolated objects with normal gas content and of similar NIR luminosity.
This indicates that the current star formation is regulated by the gaseous content of spirals.
Whatever mechanism (most plausibly ram-pressure stripping) is responsible for the pattern of gas
deficiency observed in spiral galaxies members of rich clusters, it also produces the observed quenching of the
current star formation.
A significant fraction of gas "healthy'' (i.e. with a gas deficiency parameter less than 0.4)
and currently star forming galaxies
is unexpectedly found projected near the center of the Virgo cluster. Their average Tully-Fisher distance
is found approximately one magnitude further away (
31.77) than the distance of their gas-deficient counterparts
(
30.85), suggesting that the gas healthy objects belong to a cloud projected onto the cluster center,
but in fact lying a few Mpc behind Virgo, thus unaffected by the dense IGM of the cluster.
Key words: galaxies: photometry - galaxies: clusters: individual: Virgo
A significant trend of the global star formation rate (SFR) of galaxies with the projected
clustercentric distance from rich clusters of galaxies is well documented in the local universe
(
0.05<z<0.1). The mean SFR, as traced by the equivalent width of the H
line (Kennicutt 1989),
is found to decrease with decreasing distance from rich clusters (Lewis et al. 2002).
This pattern is dominated by the "morphology segregation'' effect (Dressler 1980), i.e.
there are more
elliptical and spheroidal galaxies with little or no current star formation
than the star forming galaxies in the center of rich clusters. What physical mechanism
(nature vs. nurture) is responsible for the morphological transformation taking place in
the densest environments is however not yet fully understood. To shed light on the various
possibilities, i.e. galaxy harassment (Moore et al. 1996, 1998), tidal stirring (Mayer et al. 2001)
or ram pressure stripping (Gunn & Gott 1972), it is crucial to establish observationally if,
beside the morphology segregation,
galaxies of a given morphological type, namely the spirals, are affected by a systematic SFR decrease
toward the center of nearby clusters.
If on the one hand Kennicutt (1983) found that spirals in the Virgo cluster
have their mean SFR as much as a factor of two lower than isolated galaxies,
Gavazzi et al. (1998) did not confirm this evidence in the Coma and A1367 clusters.
Moreover Iglesias-Paramo et al. (2002) found that the shape of the H
luminosity function of these two clusters does not differ significantly from the one
of isolated galaxies.
The result of Kennicutt (1983) was based on only a dozen giant galaxies with
H
measurements from aperture photometry,
thus requiring a confirmation on a larger sample with modern imaging data.
With the aim of solving this riddle we undertook an H
imaging survey
of two optically complete samples of galaxies.
The first is composed of nearly isolated objects selected from the CGCG
(Zwicky et al. 1961-68) in the bridge between Coma and A1367,
which we observed down to the limit of 15.7 mag. This constitutes our reference sample of non-cluster objects.
The cluster sample is focused on A1367, the Coma and the Virgo clusters.
We took H
imaging observations of these regions (Gavazzi et al. 1998; Gavazzi et al.
2002a, Paper I of this series; Boselli & Gavazzi 2002, Paper II;
Boselli et al. 2002b, Paper III). Our own observations were complemented with data taken from
the literature (Kennicutt & Kent 1983; Romanishin 1990; Gavazzi et al. 1991; Young et al.
1996; Koopmann et al. 2001).
Furthermore we performed a NIR imaging survey of the same regions (Gavazzi et al. 2000b and references therein), providing information on the old stars.
In the present paper we combine H
with NIR measurements to study
the young and the old components of the stellar population integrated over the
whole galaxy and we analyze the
properties of the stars as a function of the clustercentric projected distance, of the luminosity and
of the global gas content.
We postpone to a forthcoming paper the morphological aspects of the analysis related to
the spatial distribution of the young/old stars.
The present paper is organized as follows:
in Sect. 2 we briefly present the new H
imaging observations of 13 galaxies.
The sample used in the present investigation is illustrated in Sect. 3.
After defining the "birth-rate'' parameter (Sect. 4.1) and the "gas-deficiency'' parameter (Sect. 4.2),
we analyze in Sect. 5.1 the clustercentric dependence of the current star formation rate.
In Sects. 5.2 and 5.3 we study
the current star formation properties of galaxies in 3 local clusters
as a function of their global luminosity and gaseous properties.
The conclusions are briefly discussed in Sect. 6 and summarized in Sect. 7.
Narrow band imaging in the H
emission line (
= 6562.8 Å) of 13 galaxies was
obtained in March 20, 2002, using the 2.1 m telescope at San Pedro
Martir Observatory (SPM) (Baja California, Mexico).
The target galaxies are listed in Table 3 as follows:
The reduction of the CCD frames follows a procedure identical to the one
described in previous papers of this series (e.g. Gavazzi et al. 2002), based on the IRAF
STSDAS
reduction packages, and it will be briefly summarized here.
To remove the detector response each image was
bias subtracted and divided by the median of several flat field exposures obtained on
empty regions of the twilight sky.
Cosmic rays were removed either
using the task COSMICRAY in IRAF or manually by direct inspection of the frames.
The sky background was determined in each frame in concentric object-free regions
around the galaxies and then subtracted from the flat-fielded images.
The typical uncertainty on the mean background is estimated
10% of the rms in the individual pixels. This represents the dominant source of
error in low S/N regions.
H
fluxes and equivalent widths are estimated subtracting the contribution of the continuum
from the ON-band measurements.
As the continuum was estimated using the broad band r filter, which in fact includes the
H
and [NII] lines, the corrected fluxes and equivalent widths are computed
according to Eqs. (1) and (2) of Paper III, and their uncertainties
are given by:
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(1) |
![]() |
(2) |
Galaxies with substantial
structure are given in Fig. 14. The contours of the OFF frames are
superposed to the NET (ON-OFF) frames (grey-scale).
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Figure 1:
Sky distribution of the 312 spiral galaxies brighter than
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Figure 2:
Sky distribution of the 256 spiral galaxies brighter than
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Including the new observations presented in this paper, this work comprises
H
and NIR (H band) imaging observations of 369 late-type galaxies belonging to
the Virgo cluster and to the Coma supercluster region.
The Virgo cluster galaxies were selected from the Virgo Cluster
Catalogue (VCC) of Binggeli et al. (1985), with
,
Hubble type later than S0a (as given in the VCC) and
classified as cluster members, possible members or belonging to the
W, W', M clouds or to the southern extension (Binggeli et al. 1985, 1993; see also
Gavazzi et al. 1999a) matching V<3000
(see Fig. 1).
The late-type (> S0a) galaxies in the Coma supercluster region
(
;
)
were selected from the CGCG catalogue (
)
(Zwicky et al. 1961-68)
and include members to the Coma Supercluster according to Gavazzi et al. (1999b) (see Fig. 2).
Table 1 gives the details of the sample completeness in the two studied regions.
The Coma supercluster members are divided in cluster (A1367+A1656) members, members
to groups and pairs (see Gavazzi et al. 1999b) and strictly isolated
supercluster objects (with projected separations >300 kpc).
The H
observations were taken either from the present series of papers (Papers I, II, III, IV, primarily
devoted to the Virgo cluster), from Gavazzi et al. (1991, 1998) (containing mostly observations
of the Coma supercluster region) or from
Kennicutt & Kent (1983), Kennicutt et al. (1984), Romanishin (1990),
Koopmann et al. (2001) (see detailed references in Table 4).
The NIR observations were taken from the series of papers "Near-infrared H surface photometry of galaxies'' (Gavazzi et al. 1996a,b, 2000a; Boselli et al. 1997; Boselli et al. 2000 and from Gavazzi et al. 2001). Total asymptotic H band magnitudes were obtained by Gavazzi et al. (2000b) and by Gavazzi et al. (2001).
As listed in Table 1 the combined NIR+ H
observations cover more than
60% of the targets in all regions (except Coma supercluster groups+pairs), thus our data can
be considered as representative of the late-type galaxies in the studied regions.
region |
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with NIR | with NIR & H![]() |
Compl. |
Virgo | 323 | 271 | 205 | 63% |
Coma S. (Clusters) | 72 | 72 | 54 | 75% |
Coma S. (Grps+Prs) | 67 | 67 | 27 | 40% |
Coma S. (Isolated) | 119 | 83 | 83 | 69% |
Tot. | 568 | 480 | 356 | 63% |
The analyzed galaxies are listed in Table 4 as follows:
and NIR observations provide us with information on
stellar populations with different time scales:
107 yrs the former
and
1010 yrs the latter. The two quantities combined give the ratio
of the current SFR to the average past SFR or
the birthrate parameter b, as defined by Kennicutt et al. (1994).
Following Boselli et al. (2001), we use the Near Infrared luminosity
as
a tracer of the global mass of old stars, assuming that disk galaxies have a constant
within their optical radius
(Gavazzi et al. 1996c). Thus we write the adimensional parameter b as:
![]() |
(3) |
![]() |
(4) |
is the dark matter contribution at the optical radius, i.e. within the
B band isophote, that we assume
0.5, as in Kennicutt et al. (1994).
R=0.3 (Kennicutt et al. 1994) is the fraction of gas that stars re-injected
through stellar winds into the interstellar medium during their lifetime,
that we assume
12 Gyrs.
If we assume that galaxies evolved as "closed'' systems following
an exponential
Star Formation History (SFH), with a characteristic decay time
since their epoch of formation (
), their birthrate parameter
can be computed analytically (see Boselli et al. 2001) as:
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(5) |
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(6) |
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(7) |
Although b and
EW have distinct dimensions, they are strongly correlated quantities.
In fact they are operationally obtained in a similar way: b is computed by normalizing the
line intensity
to the NIR continuum intensity, while the equivalent width is divided by the continuum intensity underlying the
line. This is shown in Fig. 3 which can be
directly compared with Fig. 4 of Kennicutt et al. (1994).
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Figure 3:
The relation between the birthrate parameter and the
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For galaxies in our sample we estimate the "global gas content''
.
is available for most (95%) targets by direct 21 cm observations
(see Scodeggio & Gavazzi 1993; Hoffman et al.
1996, and references therein).
The mass of molecular hydrogen can be estimated from the measurement
of the CO (1-0) line emission, assuming a conversion factor (X)
between this quantity and the
surface density.
X is known to vary in the
range 1020 to 1021 [mol cm-2 (K km s-1)-1]
from galaxy to galaxy, according to their metallicity and UV radiation field. We adopt the empirical calibration
as a function of the H band luminosity:
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(8) |
The contribution of He, not directly observable, is estimated as
30% of
(see Boselli et al. 2002a).
We define the "gas deficiency'' parameter
as the logarithmic difference between
of a reference sample of isolated
galaxies and
actually observed in individual objects (in full analogy with
the definition of HI deficiency by Giovanelli & Haynes 1985).
Using a procedure similar to the one adopted by Haynes and Giovanelli (1984)
we find that the gas content of 72 isolated objects
in the Coma Supercluster correlates with
their linear optical diameter (D):
,
where a and b are weak functions of the Hubble type, as listed in Table 2.
are listed in Col. 7 of Table 4.
Histograms of the
parameter are given in Fig. 4 for the Coma isolated objects and for the Virgo galaxies. Isolated objects have
,
while Virgo galaxies have significantly positive
.
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Figure 4:
Histograms of the
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The
EW of galaxies is known to increase systematically along the Hubble sequence,
from virtually zero for the early types (E-S0) to several hundred Å for the latest types (Kennicutt 1998). A weak trend is confirmed when data
limited to the Virgo spiral galaxies included in this work are used, as shown in Fig. 5.
However the scatter in each of the morphological type bins is as much as an order of magnitude,
even though the scatter is somewhat reduced when gas deficient galaxies are excluded.
The Hubble type alone does not account for the star formation properties of galaxies in this cluster.
To shed light on other possible dependences we will analyze how the SFR varies as a function of
the projected clustercentric distance (Sect. 5.1), of the luminosity (Sect. 5.2)
and of the gaseous content of galaxies (Sect. 5.3).
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Figure 5:
The distribution of
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Lewis et al. (2002) analyzed the dependence of the galaxy SFR on the projected distance from clusters in the 2dF survey. Their volume limited samples comprise galaxies of all morphological types with 0.05<z<0.1, brighter than Mb<-19. They showed with high statistical significance that the median SFR of galaxies decreases with decreasing projected distance from clusters.
It would be interesting to compare these intermediate distance clusters
with the 3 local clusters analyzed in this work, however a direct comparison
cannot be carried out because data of early-type galaxies are not in our possession.
The dependence of the
EW on the clustercentric distance in units of virial radii
can be analyzed only for the late-types galaxies, bearing in mind that our completeness is 60%.
We compute
(Girardi et al. 1998)
for the 3 clusters assuming
= 775, 840, 925
for Virgo, A1367 and Coma respectively.
The combined Coma and A1367 clusters (with Mb<-19) are shown in Fig. 6 enbedded in the Coma supercluster
that we trace out to large clustercentric radial distances.
We find a significant inner decrease only of the 25th percentile of the
EW
distribution. Both the median and the 75th percentile instead increase inwards.
We find it unlikely that the
EW distribution is biased toward high values due to incompleteness,
since for the Coma+A1367 clusters our survey covers 75% of the sample.
These clusters are inhabited by strong
emitters
to which the attention has been drawn by several authors. These include the "blue galaxies in the Coma cluster''
of Bothun & Dressler (1986) and the blue galaxy sample observed with ISO by Contursi et al. (2001).
Many (13) galaxies with
EW in excess of 50 Å are found both in the inner regions (
)
and at intermediate distances (
)
from the observed clusters.
Noticeably these galaxies are near the faint limit of our survey (
-19.5<Mb<-19 mag).
For the Virgo cluster we separate the bright sample
(Mp<-19), with a luminosity cutoff and
completeness similar to the Coma supercluster (75%),
from the total sample
(Mp<-15) and we show the two radial dependences separately in Fig. 7.
The bright sample shows an inner decrease of the SFR. For the total sample this
pattern no longer holds true. The Virgo cluster contains 24 galaxies with
EW in excess of 50 Å
(11 are BCDs), the majority (14/24 objects) being fainter than -17.1 mag.
Because of their low optical luminosity
the strong
emitters belonging to Virgo would have all escaped detection in
the 2dF survey.
We conclude that, beside morphology segregation, the three local clusters analyzed in this work
do not show a clear radial trend of the SFR distribution. The presence of the radial trend depends purely
on a luminosity cutoff, which varies cluster to cluster between -17 and -19 mag.
While spiral galaxies brighter than this cutoff luminosity have lower than average SFR at
the cluster centers, galaxies fainter than this limit have SFR independent from the clustercentric projected distances.
This is consistent with the idea that infall of small galaxies is occurring onto
rich clusters at the present cosmological epoch.
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Figure 6:
The distribution of
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Figure 7:
The distribution of
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Figure 8:
The relation between the birthrate parameter and the NIR
luminosity (mass) for the Coma supercluster galaxies. Galaxies in
the Coma+A1367 clusters are represented with empty symbols, filled
symbols are non-cluster galaxies.
The dotted line represents the expected b as a function of ![]() |
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Since, as concluded in the previous section, the present star formation rate of galaxies
near the center of the studied clusters is a luminosity sensitive parameter, it is compelling
to proceed to a systematic investigation of the luminosity dependence of the star formation properties.
To this aim it is adequate to analyze the luminosity dependence of the birthrate parameter b (see Sect. 4.1).
The most appropriate luminosity indicator, which we will adopt hereafter, is the NIR (H band) luminosity. This
parameter traces at best the dynamical mass (within the optical disk) of spiral galaxies,
as concluded by Gavazzi et al. (1996c), who found
.
The dependence of the b parameter on ,
given in Fig. 8,
shows that the star formation history of spiral galaxies in the
Coma supercluster region is in almost inverse proportionality with
the system luminosity (mass). The most massive spirals (
)
have their b parameter as much as 100 times lower than less luminous
(giant) galaxies (
). This confirms previous claims that the
current SFR, as derived from the
EW, anti-correlates with
the system mass (Gavazzi et al. 1998).
Furthermore Fig. 8 shows that there is not a significant
difference between the SFH of galaxies in the rich Coma+A1367
clusters and of relatively isolated objects in the same supercluster,
in agreement with Gavazzi et al. (1998).
Both results are however biased by selection effects.
The Coma supercluster galaxies were selected optically in the blue
(photographic) band (
). The selected targets were observed "a posteriori''
in
and in the NIR, therefore at any given
only
galaxies bluer than a certain threshold are sampled. In other words
the B selection biases against faint-red galaxies, according to the relation between B-H
and the infrared luminosity represented by Eq. (9) (see Scodeggio et al. 2002).
This, combined with the fact that
b correlates with the B-H color (see Eq. (10)), introduces a selection effect
in the b vs.
plane
(see Eq. (11)).
These empirically determined relations are:
Type | a | b | R2 |
Sa-Sb | 7.62 | 1.55 | 0.75 |
Sbc-Sc | 7.48 | 1.68 | 0.75 |
Scd-Irr | 7.74 | 1.49 | 0.77 |
VCC/CGCG | NGC/IC | UGC |
![]() |
Dec |
![]() |
Vel |
![]() |
![]() |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
343 | 3148 | - | 121921.68 | 075213.8 | 15.1 | 2479 | 20 | 0.79 |
841 | - | - | 122547.40 | 145711.4 | 15.6 | 501 | 20 | 0.66 |
15031 | 4771 | 8020 | 125321.85 | 011613.5 | 13.3 | 1119 | 15 | 0.85 |
15049 | 4845 | 8078 | 125801.33 | 013430.3 | 12.9 | 1097 | 15 | 0.85 |
15055 | 4904 | 8121 | 130058.89 | -000142.4 | 13.2 | 1174 | 15 | 0.85 |
41041 | 4116 | 7111 | 120736.33 | 024133.1 | 13.0 | 1309 | 15 | 0.85 |
43028 | 4688 | 7961 | 124746.67 | 042005.3 | 14.5 | 984 | 15 | 0.84 |
43034 | 4701 | 7975 | 124911.87 | 032324.5 | 13.1 | 727 | 15 | 0.79 |
43054 | 4765 | 8018 | 125314.52 | 042749.4 | 13.0 | 725 | 15 | 0.79 |
69036 | 4067 | 7048 | 120411.46 | 105114.8 | 13.2 | 2424 | 15 | 0.8 |
100015 | 4758 | 8014 | 125244.16 | 155050.9 | 14.1 | 1240 | 15 | 0.85 |
157075 | - | - | 115940.06 | 263248.7 | 15.7 | 6694 | 15 | 0.77 |
160121 | - | 8161 | 130329.11 | 263300.8 | 15.5 | 6676 | 20 | 0.77 |
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Figure 9:
The relation between the birthrate parameter and the NIR luminosity (mass)
for the Virgo galaxies. Empty symbols represent galaxies with normal gas content (
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Figure 10:
The relation between the birthrate parameter and the NIR luminosity (mass)
for Virgo+Coma galaxies with normal gas content (
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The selection effect mentioned above affects the Virgo sample
to a much lesser extent, because Virgo is 3.7 mag closer than Coma.
When we consider the Virgo galaxies alone in Fig. 9
we include dwarf systems with
fainter by almost 2 orders of magnitudes with respect to Coma.
The scatter of the b vs.
relation increases considerably because
the large majority of faint Virgo objects have b lower than Coma. This is
in agreement with Kennicutt (1983) who found evidence for significant
deficiency in 12 Virgo galaxies with respect to isolated galaxies.
Galaxies with b as low as the ones in Virgo might exist in the Coma+A1367 clusters as well,
but are not observed because of the previously mentioned observational bias.
Thus we conclude that, at any given mass, spirals belonging to the Virgo cluster
have their present star formation activity significantly lower than
isolated galaxies.
It remains to be explained why. The first thing to explore is whether their gaseous content is sufficient for fueling the star formation. Cluster spirals are in fact known to suffer from HI deficiency (Giovanelli & Haynes 1985; Solanes et al. 2001), a pattern that is interpreted in the framework of the ram pressure mechanism (Gunn & Gott 1972).
When galaxies are separated according to their
gas deficiency parameter (see Fig. 9), we recognize that, at any given ,
galaxies with "normal'' gas content (
)
(open symbols)
have their b parameter significantly higher than gas "deficient'' objects.
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Figure 11:
Histograms of the residual
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Figure 12:
The relation between
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Figure 10 is restricted to the non deficient galaxies of both the Virgo and Coma regions.
In this and in the previous figures the dotted curve represents
i.e.
the b vs.
relation expected from the closed-box scenario, in the
assumption that
is inversely proportional to
according to Eq. (6).
Galaxies in Fig. 10 are found in relatively good agreement with
,
in other words their residuals
are small.
This is evidenced in the histograms of Fig. 11 where the distribution
of the residuals
is given separately for the
Coma galaxies, for the Virgo galaxies and for the subsample of the Virgo
galaxies with normal gas content (
). Large negative residuals,
implying a factor of 3 lower SFR,
are associated with significantly gas deficient galaxies. It is concluded that,
at any given luminosity,
the principal parameter regulating the current star formation activity in cluster spirals is the
availability of gas at their interior.
This is further evidenced in Fig. 12, where
is plotted against the gas deficiency parameter,
showing a significant linear anti-correlation:
-
.
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Figure 13: The distribution of the "quenched" (empty symbols) and "healthy" (filled symbols) galaxies in the Virgo cluster. Positions of M87 and M49 are shown by crosses. |
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We have shown that a large fraction of late-type galaxies in the Virgo cluster
have their current star formation rate significantly quenched with respect to
isolated objects. These systems coincide with the Virgo gas deficient galaxies.
Since the "gas'' deficiency parameter is dominated by
the HI phase (H2 contributes only to 15% of the HI), it is concluded that, to the first order,
the star formation properties of galaxies in the Virgo cluster are determined by
the pattern of HI deficiency.
As earlier recognized by Kennicutt (1998), this is a somewhat surprising result,
because the typical scales of HI and of star formation are
very different in disk galaxies. HI reservoirs extend some 2
the scale where the star formation takes place
(Cayatte et al. 1994). We will re-examine this issue in more details in our forthcoming
paper dedicated to the morphology of the star formation regions in galaxies,
where a comparison between the scale-length of
,
and
will be
carried on specifically.
Limiting ourself to the global quantities, they indicate that
infall of HI gas occurs in the disks on time scales similar to the star formation time.
If the gas replenishment fails, because the HI reservoir is reduced by some
ablation mechanism (e.g. ram pressure), the star formation
adjusts itself to significantly lower rates.
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Figure 14:
Newly observed galaxies with substantial
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Figure 14: Continued. |
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Figure 14: Continued. |
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Galaxies with
and
("quenched'') are plotted in Fig. 13 with
empty symbols, together with their "healthy'' counterparts (filled symbols).
Beside a marginal clustering of deficient objects around M 87 (cluster A) and M 49 (cluster B)
the two populations appear mixed in position. There is for example a considerable fraction
of "healthy'' objects projected onto the center of cluster A.
However Virgo is known to be a complex dynamical entity, composed by the main cluster (A)
a secondary cluster (B), several Mpc behind A, and a number of clouds at approximately the
distance of A, but with significantly discrepant velocities, suggesting infall (see Gavazzi et al. 1999a).
By considering galaxies with projected angular separation <3.7 deg from M 87
we isolate 68 bona fide members of cluster A. We divide them into 48 "quenched'' and 20 "healthy''.
For a considerable fraction (22/48 and 13/20 respectively) their distance is available from Gavazzi et al. (1999a)
based on the H band Tully-Fisher relation (Tully & Fisher 1977) (distances of few galaxies whose H magnitudes were not yet available to
Gavazzi et al. 1999a were recomputed by us).
To our surprise we find that, while the average distance modulus of the deficient objects (
30.85)
is in perfect agreement with the distance modulus of cluster A as a whole (
30.82)
(Gavazzi et al. 1999a), the distance modulus of the non-deficient
galaxies projected onto A is
31.77 on average, thus
almost one mag more distant.
It is thus concluded that "healthy'' spirals projected onto the
Virgo center belong in fact to a background cloud with a distance comparable with that of cluster B. This cloud has not yet entered the dense environment of cluster A.
Acknowledgements
This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Virgo | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
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ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
VCC0001 | VM | BCD | 5.63 | 12.75 | 32 | - | 12 | -13.46 | 11 |
VCC0010 | VM | BCD | 5.35 | 12.76 | 32 | 0.34 | 31 | -12.98 | 6 |
VCC0017 | VM | Im | 5.43 | 14.12 | 32 | 0.26 | 105 | -12.78 | 9 |
VCC0025 | VM | Sc | 6.10 | 9.96 | 32 | -0.15 | 58 | -11.50 | 11 |
VCC0047 | VM | Sa | 4.62 | 10.70 | 32 | 0.79 | 16 | -12.84 | 11 |
VCC0058 | VM | Sb | 4.48 | 10.51 | 32 | 0.15 | 15 | -12.31 | 11 |
VCC0066 | VN | Sc | 4.68 | 9.01 | 17 | -0.06 | 23 | -11.45 | 1 |
VCC0067 | VM | Sc | 4.66 | 11.27 | 32 | 0.36 | 27 | -12.49 | 7 |
VCC0073 | VW | Sb | 6.92 | 9.47 | 32 | 0.42 | 11 | -12.19 | 11 |
VCC0081 | VN | Sc | 4.85 | 12.78 | 17 | -0.19 | 21 | -13.06 | 11 |
VCC0083 | VN | Im | 4.69 | 12.98 | 17 | 0.81 | 8 | -13.73 | 6 |
VCC0087 | VN | Sm | 5.17 | 13.66 | 17 | 0.39 | 20 | -12.89 | 7 |
VCC0089 | VM | Sc | 4.28 | 9.31 | 32 | 0.00 | 20 | -11.73 | 1 |
VCC0092 | VN | Sb | 4.84 | 7.06 | 17 | 0.30 | 9 | -11.33 | 7 |
VCC0097 | VM | Sc | 4.20 | 9.60 | 32 | 0.13 | 14 | -12.13 | 11 |
VCC0120 | VW | Scd | 7.70 | 10.42 | 32 | 0.18 | 54 | -11.87 | 11 |
VCC0131 | VN | Sc | 4.17 | 10.76 | 17 | 0.24 | 23 | -12.48 | 11 |
VCC0144 | VW | BCD | 7.66 | 12.95 | 32 | 0.07 | 144 | -12.19 | 12 |
VCC0145 | VN | Sc | 3.84 | 9.61 | 17 | 0.22 | 7 | -11.84 | 7 |
VCC0152 | VN | Scd | 4.69 | 9.77 | 17 | 0.39 | 9 | -12.59 | 7 |
VCC0157 | VN | Sc | 3.99 | 8.35 | 17 | 0.42 | 20 | -11.43 | 1 |
VCC0159 | VW | Im | 5.54 | 13.23 | 32 | 0.57 | 19 | -13.16 | 7 |
VCC0162 | VN | Sd | 4.06 | 11.48 | 17 | 0.48 | 30 | -12.83 | 11 |
VCC0167 | VN | Sb | 3.72 | 6.69 | 17 | 0.66 | 3 | -11.32 | 7 |
VCC0199 | VW | Sa | 6.05 | 8.86 | 32 | 0.84 | 10 | -12.04 | 11 |
VCC0213 | VN | BCD | 3.60 | 11.52 | 17 | 0.66 | 24 | -12.62 | 12 |
VCC0221 | VW | Sc | 9.35 | 11.23 | 32 | 0.54 | 53 | -11.87 | 11 |
VCC0222 | VW | Sa | 6.19 | 8.73 | 32 | 0.91 | 2 | -12.55 | 7 |
VCC0226 | VN | Sc | 4.42 | 8.89 | 17 | -0.34 | 6 | -12.23 | 1 |
VCC0234 | VW | Sa | 6.59 | 9.23 | 32 | 1.40 | 14 | -12.11 | 7 |
VCC0267 | VB | Sbc | 6.55 | 10.92 | 23 | 0.16 | 11 | -12.63 | 7 |
VCC0307 | VN | Sc | 3.55 | 7.20 | 17 | 0.04 | 29 | -10.76 | 7 |
VCC0318 | VW | Scd | 4.57 | 12.97 | 32 | 0.04 | 51 | -12.46 | 11 |
VCC0324 | VS | BCD | 9.01 | 11.83 | 17 | 0.70 | 57 | -12.27 | 12 |
VCC0328 | VN | Im | 2.88 | 14.66 | 17 | 0.73 | 20 | -13.62 | 9 |
VCC0341 | VB | Sa | 6.90 | 8.70 | 23 | 0.94 | 2 | -12.66 | 7 |
VCC0343 | VA | Sd | 5.33 | 13.17 | 23 | 0.97 | 15 | -13.37 | T.W. |
VCC0382 | VW | Sc | 7.55 | 9.31 | 32 | -0.27 | 31 | -11.58 | 7 |
VCC0393 | VB | Sc | 5.39 | 10.58 | 23 | 0.48 | 25 | -12.14 | 11 |
VCC0410 | VN | BCD | 2.57 | 16.37 | 17 | 0.61 | 77 | -13.25 | 6 |
VCC0446 | VB | BCD | 6.52 | 13.40 | 23 | 1.11 | 17 | -13.43 | 7 |
VCC0459 | VA | BCD | 5.74 | 12.72 | 17 | 0.27 | 47 | -12.61 | 12 |
VCC0460 | VA | Sa | 6.42 | 7.60 | 17 | 1.02 | 2 | -11.65 | 1 |
VCC0465 | VN | Sc | 2.49 | 9.86 | 17 | 0.27 | 57 | -11.43 | 11 |
VCC0483 | VA | Sc | 3.16 | 8.49 | 17 | 0.17 | 31 | -11.41 | 7 |
VCC0491 | VN | Scd | 2.41 | 10.99 | 17 | 0.02 | 74 | -11.67 | 4 |
VCC0492 | VB | Sa | 7.36 | 9.68 | 23 | 1.46 | 6 | -12.54 | 11 |
VCC0497 | VA | Sc | 3.13 | 8.11 | 17 | 0.46 | 15 | -11.66 | 7 |
VCC0508 | VS | Sc | 8.22 | 7.09 | 17 | -0.02 | 34 | -10.58 | 1 |
VCC0513 | VS | BCD | 10.28 | 12.33 | 17 | 1.24 | 47 | -12.67 | 12 |
VCC0524 | VB | Sbc | 3.98 | 9.54 | 23 | 1.49 | 5 | -12.32 | 7 |
Virgo | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
![]() |
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ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
VCC0530 | VA | Im | 4.01 | 15.02 | 17 | 1.26 | 3 | -14.06 | 9 |
VCC0534 | VB | Sa | 5.66 | 9.95 | 23 | 1.56 | 8 | -12.54 | 11 |
VCC0559 | VA | Sab | 3.74 | 8.99 | 17 | 1.04 | 2 | -12.66 | 7 |
VCC0562 | VA | BCD | 2.02 | 15.75 | 17 | 0.85 | 84 | -12.82 | 6 |
VCC0576 | VB | Sbc | 3.65 | 9.61 | 23 | 0.16 | 14 | -12.29 | 11 |
VCC0596 | VA | Sc | 3.93 | 6.69 | 17 | 0.47 | 18 | -10.81 | 7 |
VCC0613 | VS | Sa | 7.39 | 8.67 | 17 | 0.54 | 6 | -12.20 | 11 |
VCC0620 | VA | Sm | 1.99 | 13.02 | 17 | 0.83 | 27 | -13.64 | 7 |
VCC0630 | VA | Sd | 2.11 | 9.77 | 17 | 1.20 | 7 | -12.57 | 7 |
VCC0641 | VB | BCD | 6.82 | 13.87 | 23 | 0.55 | 19 | -13.51 | 7 |
VCC0655 | VA | BCD | 5.44 | 10.66 | 17 | 0.68 | 6 | -12.73 | 12 |
VCC0656 | VB | Sb | 5.72 | 9.34 | 23 | 0.40 | 9 | -12.06 | 7 |
VCC0664 | VA | Sc | 1.73 | 12.24 | 17 | 0.70 | 101 | -11.92 | 7 |
VCC0667 | VB | Sc | 5.49 | 10.76 | 23 | 0.75 | 9 | -12.77 | 11 |
VCC0688 | VB | Sc | 4.90 | 11.00 | 23 | 0.63 | 9 | -12.82 | 11 |
VCC0692 | VA | Sc | 1.67 | 10.44 | 17 | 0.78 | 16 | -12.27 | 13 |
VCC0697 | VB | Sc | 5.60 | 11.05 | 23 | 0.80 | 14 | -12.61 | 7 |
VCC0699 | VB | Pec | 6.02 | 10.93 | 23 | 0.27 | 42 | -12.22 | 11 |
VCC0713 | VB | Sc | 4.18 | 9.81 | 23 | 1.44 | 8 | -12.52 | 11 |
VCC0768 | VA | Sc | 4.83 | 12.30 | 17 | 0.41 | 43 | -12.63 | 11 |
VCC0785 | VS | Sa | 7.59 | 8.41 | 17 | 0.28 | 8 | -11.99 | 11 |
VCC0787 | VB | Scd | 6.79 | 11.08 | 23 | 0.48 | 31 | -12.31 | 12 |
VCC0792 | VB | Sab | 2.73 | 8.55 | 23 | 0.86 | 10 | -12.44 | 7 |
VCC0793 | VA | Im | 1.50 | 15.29 | 17 | 0.59 | 2 | -14.36 | 12 |
VCC0801 | VA | ? | 4.28 | 9.63 | 17 | -0.28 | 69 | -11.52 | 7 |
VCC0802 | VA | BCD | 1.71 | 14.64 | 17 | 0.77 | 36 | -13.49 | 12 |
VCC0827 | VB | Sc | 5.33 | 9.85 | 23 | 0.18 | 26 | -12.05 | 11 |
VCC0836 | VA | Sab | 1.26 | 8.21 | 17 | 0.73 | 15 | -11.47 | 7 |
VCC0841 | VA | BCD | 2.84 | 13.65 | 17 | 0.99 | 29 | -13.08 | T.W. |
VCC0848 | VB | BCD | 6.70 | 13.35 | 23 | 0.13 | 26 | -13.00 | 12 |
VCC0849 | VB | Sbc | 2.29 | 10.74 | 23 | 0.40 | 23 | -12.10 | 4 |
VCC0851 | VB | Sc | 4.99 | 10.71 | 23 | 0.38 | 20 | -12.35 | 11 |
VCC0857 | VA | Sb | 5.94 | 8.23 | 17 | 0.66 | 12 | -11.77 | 7 |
VCC0865 | VA | Sc | 3.48 | 10.33 | 17 | 0.51 | 34 | -11.92 | 7 |
VCC0873 | VA | Sc | 1.36 | 8.58 | 17 | 0.26 | 16 | -11.76 | 12 |
VCC0874 | VA | Sc | 3.96 | 9.63 | 17 | 0.42 | 3 | -12.73 | 7 |
VCC0905 | VB | Sc | 3.68 | 11.07 | 23 | 0.47 | 39 | -12.44 | 7 |
VCC0912 | VA | Sbc | 1.07 | 9.91 | 17 | 0.74 | 8 | -12.36 | 7 |
VCC0921 | VS | Sbc | 8.49 | 10.44 | 17 | 0.61 | 38 | -11.83 | 11 |
VCC0938 | VS | Sc | 4.58 | 10.20 | 17 | 0.52 | 20 | -12.04 | 4 |
VCC0939 | VB | Sc | 3.65 | 10.53 | 23 | 0.37 | 24 | -12.17 | 4 |
VCC0950 | VA | Sm | 1.28 | 12.98 | 17 | 0.23 | 23 | -13.40 | 11 |
VCC0957 | VS | Sc | 9.94 | 9.77 | 17 | 0.08 | 40 | -11.55 | 1 |
VCC0958 | VA | Sa | 2.82 | 8.03 | 17 | 0.22 | 7 | -12.50 | 7 |
VCC0971 | VB | Sd | 6.57 | 11.46 | 23 | 0.17 | 29 | -12.47 | 11 |
VCC0975 | VB | Scd | 5.21 | 11.06 | 23 | 0.39 | 26 | -12.44 | 4 |
VCC0979 | VB | Sa | 3.10 | 8.95 | 23 | 1.20 | 9 | -12.02 | 7 |
VCC0980 | VA | Scd | 3.61 | 12.45 | 17 | 0.88 | 40 | -12.60 | 11 |
VCC0984 | VA | Sa | 0.94 | 9.26 | 17 | 1.95 | 1 | -12.97 | 7 |
VCC0995 | VA | Sc | 1.75 | 13.03 | 17 | -0.13 | 31 | -12.79 | 7 |
VCC1002 | VB | Sc | 6.19 | 9.65 | 23 | 0.53 | 9 | -11.91 | 7 |
VCC1011 | VS | Sdm | 4.82 | 12.30 | 17 | 0.78 | 13 | -13.22 | 11 |
VCC1043 | VA | Sb | 0.97 | 7.27 | 17 | 0.75 | 6 | -11.57 | 13 |
Virgo | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
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ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
VCC1110 | VA | Sab | 4.73 | 7.13 | 17 | 0.93 | 2 | -12.10 | 13 |
VCC1118 | VB | Sc | 3.18 | 10.02 | 23 | 0.67 | 17 | -12.14 | 11 |
VCC1126 | VA | Sc | 2.66 | 9.39 | 17 | 1.48 | 11 | -12.35 | 11 |
VCC1145 | VS | Sb | 8.83 | 7.96 | 17 | 0.55 | 11 | -11.53 | 7 |
VCC1179 | VB | BCD | 2.43 | 13.25 | 23 | 1.25 | 20 | -13.17 | 6 |
VCC1189 | VS | Sc | 5.63 | 11.42 | 17 | 0.43 | 20 | -12.47 | 7 |
VCC1190 | VB | Sa | 3.66 | 8.27 | 23 | 2.07 | 3 | -12.29 | 7 |
VCC1193 | VS | Sc | 4.71 | 11.35 | 17 | 0.18 | 31 | -12.38 | 11 |
VCC1200 | VA | Im | 1.63 | 12.58 | 17 | 1.46 | 16 | -13.56 | 7 |
VCC1205 | VS | Sc | 4.58 | 10.23 | 17 | 0.05 | 11 | -12.30 | 7 |
VCC1290 | VS | Sb | 8.14 | 9.78 | 17 | 0.07 | 30 | -11.89 | 11 |
VCC1313 | VA | BCD | 0.35 | 15.60 | 17 | 0.38 | 291 | -12.79 | 12 |
VCC1330 | VS | Sa | 4.31 | 9.22 | 17 | 1.04 | 4 | -12.48 | 11 |
VCC1356 | VA | BCD | 0.91 | 13.10 | 17 | 0.43 | 43 | -13.00 | 11 |
VCC1374 | VA | BCD | 2.48 | 12.41 | 17 | 0.59 | 49 | -12.48 | 6 |
VCC1375 | VS | Sc | 8.45 | 11.17 | 17 | 0.09 | 28 | -11.49 | 7 |
VCC1379 | VA | Sc | 4.46 | 9.95 | 17 | 0.30 | 36 | -11.72 | 11 |
VCC1393 | VA | Sc | 2.74 | 10.87 | 17 | 0.43 | 38 | -12.10 | 11 |
VCC1401 | VA | Sbc | 2.05 | 6.60 | 17 | 0.41 | 6 | -11.28 | 7 |
VCC1410 | VA | Sm | 4.31 | 12.11 | 17 | 0.75 | 35 | -12.66 | 11 |
VCC1411 | VA | Pec | 0.65 | 13.83 | 17 | 0.53 | 2 | -14.32 | 11 |
VCC1412 | VA | Sa | 1.25 | 8.22 | 17 | 1.60 | 2 | -12.32 | 7 |
VCC1419 | VA | S.. | 1.08 | 10.39 | 17 | 1.77 | 5 | -13.02 | 7 |
VCC1426 | VA | Im | 0.63 | 13.13 | 17 | 1.24 | 6 | -13.88 | 11 |
VCC1437 | VS | BCD | 3.25 | 12.21 | 17 | 0.43 | 13 | -13.19 | 12 |
VCC1450 | VA | Sc | 1.72 | 10.85 | 17 | 0.65 | 69 | -11.69 | 7 |
VCC1486 | VA | S.. | 1.19 | 12.05 | 17 | 0.93 | 11 | -13.14 | 7 |
VCC1508 | VS | Sc | 3.79 | 9.73 | 17 | -0.09 | 40 | -11.58 | 11 |
VCC1516 | VS | Sbc | 3.29 | 9.93 | 17 | 0.51 | 10 | -12.19 | 13 |
VCC1532 | VA | Sc | 3.06 | 10.68 | 17 | 1.00 | 17 | -12.35 | 11 |
VCC1540 | VS | Sb | 9.77 | 7.27 | 17 | -0.18 | 20 | -11.15 | 7 |
VCC1552 | VA | Sa | 1.08 | 9.07 | 17 | 1.66 | 2 | -12.78 | 7 |
VCC1554 | VS | Sm | 5.99 | 9.79 | 17 | -0.13 | 75 | -11.35 | 13 |
VCC1555 | VS | Sc | 4.28 | 7.64 | 17 | 0.23 | 17 | -11.06 | 7 |
VCC1557 | VS | Scd | 10.10 | 11.74 | 17 | 0.64 | 23 | -12.69 | 11 |
VCC1562 | VS | Sc | 10.24 | 7.78 | 17 | 0.18 | 20 | -11.17 | 7 |
VCC1569 | VA | Scd | 1.43 | 13.51 | 17 | 1.28 | 13 | -13.42 | 7 |
VCC1575 | VS | Sm | 5.32 | 11.27 | 17 | 0.35 | 13 | -12.68 | 7 |
VCC1581 | VS | Sm | 6.17 | 12.69 | 17 | 0.30 | 6 | -13.41 | 11 |
VCC1585 | VA | Im | 2.99 | 13.54 | 17 | 0.23 | 21 | -13.04 | 9 |
VCC1588 | VA | Scd | 3.31 | 9.43 | 17 | 0.74 | 3 | -12.51 | 7 |
VCC1615 | VA | Sb | 2.38 | 7.28 | 17 | 0.59 | 3 | -11.78 | 1 |
VCC1624 | VS | Sc | 9.43 | 10.35 | 17 | 0.80 | 11 | -12.62 | 11 |
VCC1654 | VA | Im | 2.79 | 14.22 | 17 | 0.48 | 20 | -13.52 | 11 |
VCC1673 | VA | Sc | 1.80 | 8.22 | 17 | 0.27 | 15 | -11.80 | 7 |
VCC1675 | VS | Pec | 4.56 | 12.56 | 17 | 1.40 | 4 | -13.80 | 11 |
VCC1676 | VA | Sc | 1.82 | 7.70 | 17 | 0.34 | 19 | -11.54 | 7 |
VCC1678 | VS | Sd | 5.94 | 12.52 | 17 | 0.18 | 51 | -12.52 | 7 |
VCC1686 | VA | Sm | 1.68 | 11.25 | 17 | 0.90 | 44 | -12.12 | 11 |
VCC1690 | VA | Sab | 1.65 | 7.02 | 17 | 0.80 | 2 | -11.82 | 7 |
VCC1696 | VA | Sc | 2.35 | 8.59 | 17 | 0.55 | 12 | -11.86 | 4 |
VCC1699 | VS | Sm | 5.68 | 12.47 | 17 | 0.36 | 24 | -12.80 | 11 |
VCC1725 | VS | BCD | 4.19 | 12.13 | 17 | 0.87 | 48 | -12.56 | 12 |
Virgo | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
![]() |
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ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
VCC1726 | VS | Sdm | 5.55 | 12.96 | 17 | 0.34 | 34 | -12.75 | 7 |
VCC1727 | VA | Sab | 1.78 | 6.77 | 17 | 0.45 | 4 | -11.22 | 1 |
VCC1730 | VS | Sc | 7.23 | 9.02 | 17 | 0.72 | 4 | -12.42 | 7 |
VCC1757 | VA | Sa | 1.96 | 10.81 | 17 | 1.57 | 7 | -12.78 | 11 |
VCC1758 | VS | Sc | 4.87 | 11.97 | 17 | 0.59 | 17 | -12.87 | 11 |
VCC1760 | VS | Sa | 8.29 | 8.74 | 17 | 1.03 | 5 | -12.26 | 7 |
VCC1789 | VS | Im | 7.74 | 12.95 | 17 | 0.91 | 16 | -13.20 | 11 |
VCC1791 | VS | BCD | 4.90 | 12.17 | 17 | 0.23 | 72 | -12.37 | 11 |
VCC1811 | VE | Sc | 3.64 | 9.92 | 17 | 0.28 | 11 | -12.23 | 1 |
VCC1868 | VE | Scd | 2.59 | 9.74 | 17 | 1.02 | 3 | -13.13 | 7 |
VCC1918 | VS | Im | 7.23 | 14.49 | 17 | 0.56 | 15 | -13.85 | 11 |
VCC1923 | VS | Sbc | 8.91 | 9.98 | 17 | 0.47 | 36 | -11.73 | 11 |
VCC1929 | VE | Scd | 3.48 | 10.78 | 17 | 0.57 | 12 | -12.71 | 7 |
VCC1931 | VE | Im | 3.02 | 13.04 | 17 | 0.45 | 36 | -13.28 | 7 |
VCC1932 | VE | Sc | 3.45 | 9.52 | 17 | 0.38 | 16 | -12.13 | 7 |
VCC1943 | VE | Sb | 3.06 | 8.90 | 17 | 0.31 | 24 | -11.74 | 7 |
VCC1952 | VE | Im | 5.62 | 14.60 | 17 | 0.29 | 32 | -13.57 | 9 |
VCC1955 | VE | BCD | 3.02 | 11.16 | 17 | 1.18 | 9 | -13.05 | 12 |
VCC1972 | VE | Sc | 3.21 | 8.38 | 17 | 0.12 | 16 | -11.51 | 4 |
VCC1987 | VE | Sc | 3.28 | 7.90 | 17 | -0.18 | 30 | -11.14 | 4 |
VCC1992 | VE | Im | 3.27 | 14.10 | 17 | 0.23 | 24 | -13.16 | 9 |
VCC2023 | VE | Sc | 3.70 | 11.62 | 17 | 0.12 | 27 | -12.36 | 11 |
VCC2033 | VE | BCD | 5.42 | 13.06 | 17 | 1.06 | 13 | -13.27 | 12 |
VCC2034 | VE | Im | 4.36 | 13.23 | 17 | 0.72 | 2 | -14.40 | 12 |
VCC2037 | VE | BCD | 4.37 | 12.55 | 17 | 1.24 | 15 | -13.42 | 7 |
VCC2058 | VE | Sc | 4.34 | 8.37 | 17 | 0.72 | 13 | -11.58 | 1 |
VCC2066 | VE | ? | 4.49 | 9.28 | 17 | 0.89 | 6 | -12.43 | 7 |
VCC2070 | VE | Sa | 5.82 | 7.68 | 17 | 0.21 | 6 | -11.78 | 4 |
Z013046 | VZ | Sa | 12.53 | 8.93 | 17 | 0.36 | 17 | -11.90 | 10 |
Z014062 | VZ | Scd | 12.01 | 10.47 | 17 | 0.11 | 15 | -12.52 | 4 |
Z014063 | VZ | Sc | 12.29 | 7.61 | 17 | 0.41 | 32 | -11.04 | 7 |
Z014110 | VZ | Sc | 12.81 | 9.23 | 17 | -0.21 | 34 | -11.43 | 1 |
Z015031 | VZ | Sc | 12.44 | 9.2 | 17 | 0.52 | 16 | -12.11 | T.W. |
Z015049 | VZ | Sb | 12.74 | 8.13 | 17 | 1.24 | 11 | -11.89 | T.W. |
Z015055 | VZ | Sc | 14.5 | 9.46 | 17 | 0.33 | 28 | -11.89 | T.W. |
Z041041 | VZ | Scd | 11.28 | 9.88 | 17 | 0.00 | 40 | -11.77 | T.W. |
Z043028 | VZ | Sc | 9.08 | 10.74 | 17 | 0.21 | 60 | -11.82 | T.W. |
Z043034 | VZ | Sc | 10.08 | 10.07 | 17 | -0.05 | 51 | -11.77 | T.W. |
Z043041 | VZ | Sc | 8.51 | 9.62 | 17 | -0.21 | 66 | -11.29 | 4 |
Z043054 | VZ | Scd | 9.67 | 10.97 | 17 | 0.00 | 71 | -11.90 | T.W. |
Z043071 | VZ | Sc | 10.18 | 9.25 | 17 | -0.54 | 43 | -11.37 | 1 |
Z043093 | VZ | Sc | 12.34 | 8.87 | 17 | 0.07 | 40 | -11.25 | 1 |
Z069036 | VZ | Sb | 6.7 | 10.38 | 17 | 0.33 | 19 | -12.32 | T.W. |
Z071060 | VZ | Sd | 5.16 | 9.87 | 17 | 0.12 | 44 | -11.92 | 7 |
Z098044 | VZ | Sa | 4.87 | 8.78 | 17 | 1.20 | 7 | -11.91 | 13 |
Z099098 | VZ | Sc | 10.22 | 11.69 | 17 | -0.43 | 18 | -12.02 | 1 |
Z100004 | VZ | Sc | 5.07 | 8.25 | 17 | -0.11 | 20 | -11.27 | 1 |
Z100015 | VZ | Scd | 6.34 | 10.13 | 17 | 0.44 | 37 | -12.06 | T.W. |
Coma/A1367 supercluster | |||||||||
Z097005 | Iso | Sc | 2.74 | 12.41 | 81 | -0.18 | 39 | -12.66 | 11 |
Z097026 | Prs | Pec | 1.77 | 11.65 | 83 | -0.38 | 83 | -12.18 | 11 |
Z097027 | Prs | Sc | 1.77 | 11.84 | 88 | 0.37 | 22 | -12.69 | 11 |
Coma/A1367 supercluster | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
![]() |
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![]() |
ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
Z097062 | A1367 | Pec | 0.53 | 12.94 | 91 | 0.34 | 37 | -13.13 | 11 |
Z097063 | A1367 | Pec | 0.55 | 13.56 | 91 | 0.18 | 22 | -13.42 | 11 |
Z097064 | A1367 | S.. | 0.58 | 12.41 | 91 | 0.20 | 1 | -14.77 | 11 |
Z097068 | A1367 | Sbc | 0.55 | 11.26 | 91 | -0.25 | 41 | -12.30 | 1 |
Z097072 | A1367 | Sa | 0.44 | 11.36 | 91 | 0.32 | 5 | -13.23 | 2 |
Z097073 | A1367 | Pec | 0.37 | 13.19 | 91 | 0.00 | 111 | -12.60 | 11 |
Z097076 | A1367 | Sb | 0.36 | 11.39 | 91 | 1.39 | 1 | -14.08 | 11 |
Z097079 | A1367 | Pec | 0.33 | 13.15 | 91 | 0.10 | 129 | -12.61 | 11 |
Z097087 | A1367 | Pec | 0.20 | 11.01 | 91 | 0.14 | 77 | -12.07 | 5 |
Z097091 | A1367 | Sa | 0.27 | 11.07 | 91 | -0.05 | 23 | -12.66 | 14 |
Z097092 | A1367 | Sbc | 0.38 | 12.57 | 91 | 0.04 | 28 | -13.10 | 1 |
Z097093 | A1367 | Pec | 0.09 | 12.90 | 91 | 0.47 | 9 | -13.47 | 5 |
Z097102 | A1367 | Sa | 0.40 | 11.40 | 91 | 0.44 | 2 | -13.66 | 5 |
Z097114 | A1367 | Pec | 0.11 | 13.19 | 91 | - | 36 | -13.19 | 14 |
Z097120 | A1367 | Sa | 0.10 | 10.55 | 91 | 0.45 | 4 | -12.93 | 2 |
Z097122 | A1367 | Pec | 0.38 | 11.74 | 91 | 0.43 | 46 | -12.53 | 2 |
Z097129N | A1367 | Sb | 0.22 | 9.77 | 91 | -0.37 | 14 | -12.23 | 5 |
Z097129S | A1367 | Sbc | 0.22 | 11.91 | 91 | - | 17 | -13.08 | 5 |
Z097138 | A1367 | Pec | 0.38 | 13.92 | 91 | -0.13 | 64 | -12.77 | 5 |
Z097149 | A1367 | S.. | 0.93 | 11.68 | 91 | 0.23 | 13 | -13.26 | 3 |
Z097168 | Iso | S.. | 1.81 | 12.41 | 80 | 0.42 | 78 | -13.00 | 8 |
Z098002 | Iso | Sb | 2.32 | 13.13 | 82 | 0.12 | 34 | -12.76 | 8 |
Z098013 | Iso | Sc | 3.49 | 11.73 | 92 | -0.10 | 35 | -12.58 | 5 |
Z098016 | Iso | Sc | 4.12 | 12.12 | 86 | 0.17 | 31 | -12.70 | 5 |
Z098023 | Prs | Sb | 4.53 | 11.58 | 92 | - | 11 | -13.00 | 5 |
Z098041 | Grp | Sc | 4.66 | 11.86 | 97 | 0.70 | 66 | -12.18 | 3 |
Z098046 | Grp | Sa | 4.75 | 10.66 | 97 | 0.21 | 8 | -12.76 | 3 |
Z098058 | Iso | Sbc | 5.50 | 10.70 | 96 | 0.00 | 11 | -12.70 | 5 |
Z098081 | Prs | Sa | 6.52 | 11.57 | 96 | - | 14 | -12.86 | 5 |
Z098085 | Prs | Sc | 6.64 | 12.05 | 94 | -0.04 | 29 | -12.50 | 3 |
Z098116 | Iso | Sc | 7.33 | 11.87 | 83 | -0.25 | 39 | -12.34 | 5 |
Z100005 | Iso | Pec | 9.85 | 10.66 | 88 | 0.32 | 19 | -12.54 | 3 |
Z100012 | Iso | Pec | 10.10 | 12.47 | 86 | -0.04 | 39 | -12.89 | 5 |
Z101033 | Iso | Sc | 9.80 | 12.29 | 89 | 0.14 | 16 | -13.34 | 11 |
Z101049 | Iso | Sbc | 10.09 | 11.49 | 95 | -0.23 | 10 | -12.88 | 11 |
Z101054 | Iso | Sab | 12.05 | 10.75 | 88 | -0.04 | 11 | -12.61 | 5 |
Z127005 | Iso | Sbc | 3.04 | 12.22 | 91 | 0.05 | 26 | -12.82 | 5 |
Z127018 | Iso | Sb | 3.06 | 12.33 | 92 | - | 16 | -12.89 | 3 |
Z127025S | Prs | Sbc | 2.74 | 11.20 | 94 | -0.02 | 22 | -12.39 | 2 |
Z127025N | Prs | Sc | 2.76 | 11.73 | 95 | - | 21 | -12.70 | 3 |
Z127026 | Iso | Sbc | 6.01 | 11.30 | 91 | -0.16 | 15 | -12.70 | 11 |
Z127033 | Iso | Sc | 5.02 | 11.46 | 84 | 0.06 | 10 | -12.96 | 5 |
Z127035 | Iso | Sa | 4.13 | 11.21 | 91 | 0.29 | 10 | -12.93 | 5 |
Z127037 | Iso | Pec | 5.19 | 12.90 | 82 | -0.00 | 47 | -12.77 | 5 |
Z127038 | Iso | Sc | 2.91 | 10.54 | 92 | -0.18 | 16 | -12.27 | 2 |
Z127039 | Iso | Sbc | 3.20 | 12.16 | 92 | - | 48 | -12.54 | 3 |
Z127049 | A1367 | Pec | 0.87 | 11.93 | 91 | 0.29 | 57 | -12.84 | 8 |
Z127050 | Grp | Sbc | 1.26 | 11.38 | 93 | 0.00 | 16 | -12.53 | 2 |
Z127052 | A1367 | Sa | 0.71 | 9.79 | 91 | 0.27 | 4 | -12.70 | 5 |
Z127053 | Iso | Sbc | 4.18 | 11.33 | 85 | -0.10 | 17 | -12.74 | 5 |
Z127054 | Grp | Sb | 1.02 | 10.62 | 93 | 0.10 | 4 | -12.81 | 5 |
Z127055 | Iso | Pec | 1.55 | 12.06 | 89 | - | 41 | -12.74 | 8 |
Z127061 | Iso | Sc | 5.24 | 12.99 | 79 | -0.12 | 29 | -12.70 | 11 |
Coma/A1367 supercluster | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
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ref. |
deg | mag | Mpc | ![]() |
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|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
Z127071 | Grp | Pec | 2.02 | 12.83 | 93 | 0.22 | 52 | -12.71 | 3 |
Z127082 | Grp | Sc | 2.20 | 11.39 | 93 | 0.11 | 22 | -12.59 | 2 |
Z127095 | Grp | Sc | 2.29 | 10.55 | 93 | 0.03 | 15 | -12.36 | 2 |
Z127100 | Grp | Sb | 2.37 | 11.05 | 93 | 0.06 | 10 | -12.87 | 2 |
Z128003 | Iso | Pec | 5.05 | 11.61 | 86 | -0.07 | 41 | -12.48 | 3 |
Z128015 | Prs | Sb | 5.01 | 11.96 | 91 | - | 21 | -12.78 | 5 |
Z128016 | Iso | S.. | 5.32 | 12.07 | 88 | -0.13 | 35 | -12.69 | 3 |
Z128021 | Iso | Sbc | 7.19 | 10.95 | 94 | 0.03 | 16 | -12.68 | 5 |
Z128023 | Grp | Sa | 5.08 | 10.70 | 97 | -0.16 | 17 | -12.43 | 3 |
Z128049 | Iso | Sc | 8.58 | 11.31 | 86 | 0.41 | 20 | -12.85 | 3 |
Z128063 | Prs | Sa | 7.56 | 11.07 | 90 | 0.19 | 4 | -13.28 | 3 |
Z128072 | Iso | Pec | 9.20 | 12.26 | 91 | - | 37 | -12.81 | 5 |
Z128073 | Iso | Sb | 9.52 | 11.29 | 92 | -0.02 | 16 | -12.63 | 5 |
Z128080 | Iso | Sb | 9.34 | 11.76 | 98 | -0.13 | 24 | -12.67 | 3 |
Z128087 | Iso | Sc | 8.02 | 11.55 | 89 | 0.20 | 14 | -12.83 | 5 |
Z128089 | Iso | Sa | 9.15 | 10.76 | 91 | 0.40 | 9 | -12.78 | 5 |
Z129004 | Iso | S.. | 8.82 | 12.04 | 91 | - | 34 | -12.77 | 5 |
Z129020 | Iso | Sb | 7.99 | 10.94 | 87 | 0.15 | 10 | -12.81 | 5 |
Z129021 | Iso | S.. | 7.60 | 11.83 | 89 | -0.96 | 24 | -12.72 | 3 |
Z129022 | Iso | Sab | 5.96 | 10.63 | 93 | -0.10 | 8 | -12.63 | 3 |
Z130003 | Iso | Sb | 6.17 | 11.01 | 95 | - | 19 | -12.60 | 5 |
Z130005 | Iso | Sbc | 5.77 | 12.24 | 94 | 0.22 | 40 | -12.69 | 11 |
Z130006 | Iso | Sbc | 2.35 | 11.45 | 87 | -0.04 | 32 | -12.59 | 5 |
Z130008 | Iso | Sc | 2.89 | 11.89 | 97 | -0.41 | 49 | -12.37 | 2 |
Z130014 | Iso | Sbc | 4.07 | 11.36 | 94 | 0.05 | 20 | -12.64 | 3 |
Z130021 | Iso | Sa | 4.31 | 11.57 | 95 | 0.16 | 28 | -12.54 | 5 |
Z130025 | Iso | Sa | 7.10 | 11.18 | 93 | 0.17 | 1 | -14.26 | 11 |
Z130026 | Prs | Sc | 8.34 | 11.59 | 91 | 0.02 | 18 | -12.67 | 11 |
Z130029 | Prs | Sc | 8.40 | 11.35 | 90 | - | 54 | -12.31 | 11 |
Z131008 | Iso | Sbc | 9.48 | 11.16 | 79 | -0.03 | 27 | -12.67 | 11 |
Z131009 | Iso | Sc | 7.40 | 12.39 | 100 | 0.05 | 27 | -12.74 | 5 |
Z157012 | Iso | Sbc | 9.08 | 12.40 | 91 | -0.18 | 30 | -12.65 | 3 |
Z157032 | Iso | Sa | 9.78 | 9.79 | 91 | 0.78 | 1 | -13.75 | 5 |
Z157035 | Iso | Sb | 10.57 | 10.34 | 83 | -0.18 | 19 | -12.09 | 3 |
Z157044 | Iso | Pec | 7.14 | 12.86 | 88 | - | 40 | -13.00 | 5 |
Z157062 | Iso | Pec | 11.64 | 14.53 | 92 | 0.12 | 77 | -12.87 | 11 |
Z157064 | Iso | Sb | 9.71 | 11.72 | 85 | -0.02 | 11 | -12.79 | 5 |
Z157075 | Iso | Sc | 7.58 | 12.97 | 89 | 0.18 | 29 | -13.14 | T.W. |
Z158009 | Prs | Sb | 12.24 | 10.77 | 100 | 0.11 | 17 | -12.41 | 3 |
Z158010 | Prs | Sbc | 12.23 | 12.07 | 105 | 0.19 | 22 | -12.89 | 3 |
Z158036 | Iso | Sb | 8.89 | 10.24 | 87 | -0.17 | 11 | -12.51 | 5 |
Z158038 | Iso | Sab | 11.23 | 11.66 | 90 | 0.23 | 23 | -12.68 | 3 |
Z158054 | Iso | Pec | 9.86 | 12.01 | 102 | -0.02 | 72 | -12.35 | 3 |
Z158081 | Iso | Pec | 9.15 | 11.85 | 90 | 0.02 | 24 | -12.80 | 3 |
Z158105 | Iso | Sbc | 7.93 | 11.50 | 91 | -0.12 | 17 | -12.71 | 5 |
Z159008 | Iso | Sb | 6.71 | 10.98 | 98 | 0.03 | 24 | -12.44 | 5 |
Z159031 | Prs | Sa | 5.09 | 11.55 | 100 | -0.02 | 9 | -12.99 | 3 |
Z159033 | Iso | Sa | 4.98 | 10.85 | 102 | 0.65 | 2 | -13.50 | 5 |
Z159037 | Iso | Sab | 4.86 | 11.50 | 97 | -0.13 | 44 | -12.42 | 11 |
Z159040 | Iso | Sa | 5.14 | 12.20 | 93 | -0.19 | 26 | -12.69 | 3 |
Z159059 | Iso | Sab | 3.73 | 12.15 | 100 | -0.26 | 61 | -12.34 | 5 |
Z159061 | Iso | Sbc | 4.77 | 11.18 | 93 | 0.29 | 4 | -13.26 | 5 |
Z159071 | Iso | Sc | 3.43 | 12.78 | 92 | - | 32 | -12.84 | 11 |
Coma/A1367 supercluster | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
![]() |
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ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
Z159072S | Prs | Pec | 4.06 | 10.84 | 88 | 0.01 | 12 | -12.77 | 11 |
Z159072N | Prs | Pec | 4.07 | 10.85 | 88 | 0.09 | 4 | -13.30 | 11 |
Z159076 | Iso | Sbc | 3.27 | 11.08 | 90 | 0.30 | 15 | -12.61 | 2 |
Z159090 | Prs | Sc | 2.05 | 12.25 | 111 | -0.47 | 22 | -12.83 | 2 |
Z159091 | Iso | S.. | 2.17 | 11.74 | 86 | -0.19 | 6 | -13.34 | 3 |
Z159095 | Iso | Sbc | 3.60 | 11.23 | 91 | -0.20 | 4 | -13.32 | 5 |
Z159096 | Iso | Sc | 3.82 | 12.10 | 82 | 0.08 | 22 | -12.76 | 5 |
Z159097 | Iso | Pec | 1.98 | 12.22 | 86 | - | 18 | -13.15 | 5 |
Z159101 | Coma | Pec | 1.67 | 13.50 | 96 | 0.14 | 64 | -12.78 | 5 |
Z159102 | Coma | Sab | 1.60 | 10.60 | 96 | -0.22 | 31 | -12.28 | 5 |
Z160001 | Coma | Sb | 1.66 | 12.34 | 96 | 0.10 | 15 | -13.17 | 11 |
Z160005 | Iso | Sb | 2.07 | 10.47 | 84 | 0.01 | 3 | -13.35 | 5 |
Z160009 | Coma | S.. | 1.25 | 11.44 | 96 | - | 6 | -13.46 | 11 |
Z160020 | Coma | Pec | 0.90 | 13.36 | 96 | 0.08 | 33 | -12.84 | 5 |
Z160025 | Coma | Sa | 1.25 | 10.35 | 96 | 1.03 | 2 | -13.29 | 5 |
Z160026 | Coma | Sc | 1.03 | 12.53 | 96 | 0.20 | 35 | -12.87 | 5 |
Z160032 | Coma | Sb | 1.64 | 11.69 | 96 | 0.52 | 10 | -13.05 | 5 |
Z160055 | Coma | Sab | 0.48 | 10.91 | 96 | 0.39 | 31 | -12.34 | 14 |
Z160058 | Coma | Sbc | 0.82 | 11.87 | 96 | 0.22 | 22 | -12.82 | 2 |
Z160064 | Coma | Pec | 0.77 | 12.79 | 96 | 0.32 | 67 | -12.94 | 5 |
Z160067 | Coma | Pec | 0.85 | 13.16 | 96 | -0.21 | 78 | -12.67 | 5 |
Z160073 | Coma | Pec | 0.38 | 12.50 | 96 | 0.43 | 23 | -12.98 | 5 |
Z160076 | Coma | Sc | 0.65 | 13.64 | 96 | -0.23 | 47 | -12.83 | 5 |
Z160086 | Coma | Pec | 0.37 | 13.18 | 96 | 0.76 | 41 | -13.04 | 5 |
Z160088 | Coma | Sb | 1.05 | 11.12 | 96 | 0.20 | 16 | -12.65 | 5 |
Z160095 | Coma | Sb | 0.35 | 9.50 | 96 | 0.72 | 4 | -12.66 | 5 |
Z160096N | Coma | Pec | 1.37 | 11.36 | 96 | 0.02 | 39 | -12.51 | 3 |
Z160098 | Coma | Pec | 0.77 | 12.04 | 96 | 0.17 | 22 | -12.95 | 5 |
Z160102 | Coma | Sab | 1.14 | 11.13 | 96 | 0.13 | 6 | -12.63 | 2 |
Z160106 | Coma | Pec | 0.59 | 10.84 | 96 | 0.33 | 20 | -12.98 | 2 |
Z160108 | Coma | Pec | 0.56 | 12.90 | 96 | 0.45 | 37 | -13.00 | 11 |
Z160121 | Coma | Sb | 1.64 | 11.21 | 96 | 0.05 | 21 | -12.93 | T.W. |
Z160127 | Coma | Sc | 1.21 | 13.29 | 96 | -0.01 | 67 | -12.53 | 5 |
Z160128 | Coma | Pec | 1.29 | 13.67 | 96 | - | 87 | -12.65 | 5 |
Z160137 | Coma | Sa | 1.77 | 10.57 | 96 | 0.00 | 11 | -12.51 | 2 |
Z160139 | Coma | Pec | 1.71 | 13.26 | 96 | -0.04 | 51 | -12.58 | 5 |
Z160141 | Coma | Pec | 1.61 | 12.51 | 96 | 0.39 | 30 | -13.08 | 11 |
Z160148 | Iso | Sa | 1.99 | 10.73 | 80 | 0.11 | 7 | -12.83 | 2 |
Z160151 | Iso | Pec | 2.48 | 12.57 | 83 | 0.40 | 28 | -12.87 | 3 |
Z160152 | Iso | Sb | 2.36 | 10.85 | 75 | 0.02 | 17 | -12.32 | 2 |
Z160156 | Prs | Sa | 2.91 | 10.98 | 97 | 0.23 | 10 | -12.81 | 3 |
Z160168 | Iso | Sc | 4.19 | 10.87 | 100 | -0.34 | 15 | -12.50 | 5 |
Z160182 | Iso | Sab | 3.97 | 11.13 | 93 | 0.11 | 12 | -12.72 | 3 |
Z160192 | Iso | Sb | 4.27 | 10.49 | 88 | -0.12 | 2 | -13.20 | 5 |
Z160213 | Coma | Pec | 0.24 | 13.07 | 96 | -0.08 | 57 | -12.87 | 7 |
Z160252 | Coma | Pec | 0.18 | 12.37 | 96 | 0.10 | 37 | -12.88 | 14 |
Z160257 | Coma | Sa | 0.27 | 10.55 | 96 | 0.69 | 6 | -12.93 | 2 |
Z160260 | Coma | Sa | 0.30 | 10.29 | 96 | 0.50 | 11 | -12.61 | 14 |
Z161040 | Iso | Sc | 5.42 | 12.73 | 97 | 0.09 | 21 | -13.18 | 11 |
Z161052 | Iso | Pec | 6.15 | 12.55 | 94 | -0.57 | 44 | -12.67 | 11 |
Z161054 | Iso | Sa | 6.62 | 12.84 | 90 | - | 43 | -12.73 | 11 |
Z161063 | Iso | Sbc | 6.83 | 12.62 | 95 | -0.05 | 22 | -12.89 | 5 |
Z161069 | Iso | Sb | 7.22 | 11.15 | 95 | -0.30 | 24 | -12.46 | 7 |
Coma/A1367 supercluster | |||||||||
Gal | Agg | Type | ![]() |
H | Dist. |
![]() |
![]() |
![]() |
ref. |
deg | mag | Mpc | ![]() |
![]() |
|||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
Z161071 | Iso | Pec | 7.40 | 13.22 | 64 | -0.16 | 48 | -12.55 | 3 |
Z161073 | Iso | Sb | 7.55 | 10.31 | 97 | -0.21 | 4 | -12.83 | 3 |