Issue |
A&A
Volume 511, February 2010
|
|
---|---|---|
Article Number | A12 | |
Number of page(s) | 12 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200811013 | |
Published online | 23 February 2010 |
Revisiting the low-luminosity galaxy population of the NGC 5846 group with SDSS
P. Eigenthaler - W. W. Zeilinger
Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Vienna, Austria
Received 22 September 2008 / Accepted 26 November 2009
Abstract
Context. Low-luminosity galaxies are known to
outnumber the bright galaxy population in poor groups and clusters of
galaxies. Yet, the investigation of low-luminosity galaxy populations
outside the Local Group remains rare and the dependence on different
group environments is still poorly understood. Previous investigations
have uncovered the photometric scaling relations of early-type dwarfs
and a strong dependence of morphology with environment.
Aims. The present study aims to analyse the
photometric and spectroscopic properties of the low-luminosity galaxy
population in the nearby, well-evolved and early-type dominated
NGC 5846 group of galaxies. It is the third most massive
aggregate of early-type galaxies after the Virgo and Fornax clusters in
the local universe. Photometric scaling relations and the distribution
of morphological types as well as the characteristics of emission-line
galaxies are investigated.
Methods. Spectroscopically selected low-luminosity
group members from the Sloan Digital Sky Survey with cz<3000 km s-1
within a radius of Mpc
around NGC 5846 are analysed. Surface brightness profiles of
early-type galaxies are fit by a Sérsic model
r1/n.
Star formation rates, oxygen abundances, and emission characteristics
are determined for emission-line galaxies.
Results. Seven new group members showing no entry in
previous catalogues are identified in the outer (>
)
parts of the system. Several photometric scaling relations for dEs as
well as the morphology-density relation for dwarf galaxies are
reproduced. The correlation between host and satellite morphologies in
poor groups of galaxies is also confirmed. Nucleated dwarfs are found
to be located in the vicinity to the brightest ellipticals in the
group. Only two faint galaxies exhibit fine structure. Emission-line
dwarfs show no interaction-induced activity.
Key words: galaxies: clusters: individual: NGC 5846 group - galaxies: dwarf - galaxies: photometry - methods: data analysis
1 Introduction
Redshift surveys indicate that most galaxies in the nearby
universe are located in poor groups
(Tully & Fisher 1988).
These aggregates not only consist of the ordinary bright Hubble types
but also a low-luminosity
dwarf galaxy population outnumbering their brighter counterparts by
far. Previous observations studying the distribution and
morphological properties of these low-luminosity galaxy populations
have mainly focused on large-scale
structures, e.g., the Virgo and Fornax clusters (Sandage & Binggeli 1984;
Ferguson 1989),
which are representative of high-density
environments. In contrast, poor groups serve as ideal laboratories for
studying the environmental dependence of the
properties of low-luminosity galaxy populations in a low-density
environment where galaxy interactions, mergers, and the
coalescence of individual galaxies are the primary physical processes.
However, the acquisition of high quality photometry and spectroscopy
of low-luminosity galaxies is challenging. Only the Local Group and a
few other nearby galaxy aggregates have
been investigated in detail to analyse the connection between
low-luminosity galaxies and their environment
(Grützbauch
et al. 2009; Karachentsev et al. 2002;
Jerjen
et al. 2000; Côté et al. 1997). Because CDM
cosmology proposes the hierarchical growth of galaxies by means of
mergers, poor groups are commonly classified on the basis of their
optical morphologies (Zabludoff 1999).
Spiral
dominated aggregates represent unevolved systems in this scenario,
while aggregates containing tidal signatures and
evidence of the formation of tidal dwarf galaxies mark an intermediate
stage (Temporin et al. 2003).
Groups dominated
by early-type morphologies represent an advanced phase of coalescence.
Dynamically, these well-evolved aggregates are more
likely to be virialised systems than groups with a higher spiral
fraction. The dwarf-to-giant ratio (DGR) is
expected to increase with time because the bright, massive galaxies are
more affected by mergers than their
faint counterparts (Zabludoff
& Mulchaey 1998). However, the number of faint
galaxies in groups and clusters is puzzling.
The
CDM
cosmology predicts more dwarfs than observed, an issue widely referred
to as the missing satellite problem
(Klypin et al. 1999).
This paper focuses on the low-luminosity galaxy population of
the X-ray bright galaxy group around the giant elliptical
NGC 5846 in
the Local Supercluster. The group was first catalogued in de Vaucouleurs (1975). Since
then, the system
has appeared in many similar catalogues (Garcia 1993; Geller
& Huchra 1983). Zabludoff
& Mulchaey (1998) identified 13 dwarfs in the
central region of the system. Mahdavi
et al. (2005), hereafter [MTT05], identify group
members including 83 spectroscopically confirmed ones. Carrasco et al. (2006)
discovered 16 additional low surface
brightness dwarfs. The NGC 5846 group of galaxies is located
at a distance of 26.1 Mpc in the Virgo III cloud of
galaxies,
a major component of the Local Supercluster (Tully
1982). Being an elongated structure extending from the Virgo
cluster out
from the Supergalactic Plane, this cloud contains about
40 luminous galaxies, the NGC 5846 system being the
largest aggregate in the region. The NGC 5846 group is the
most massive of only three dense groups (NGC 4274,
NGC 5846, and M96) in the Local Supercluster that are
dominated by elliptical and lenticular galaxies, and is the
third most massive aggregate of early-type galaxies (after the Virgo
and Fornax clusters) in the local
universe. With an average galaxy density
of
Mpc-3
compared to
Mpc-3
for the Local Group and
Mpc-3
for the central regions of the Virgo cluster, the NGC 5846
system also represents one of the densest galaxy environments found for
poor groups. The group is dominated by early-type galaxies with a
massive central elliptical surrounded by a symmetric X-ray halo. The
large early-type fraction, the prevalence
of dwarf galaxies together with the strong, and extended diffuse X-ray
emission indicate that the NGC 5846 group is an evolved
system. The group consists of two smaller aggregates around the two
brightest ellipticals NGC 5846 and NGC 5813.
MTT05 determine the group virial mass to be
by
means of the median virial mass estimator proposed by Heisler et al. (1985) and
derive a velocity dispersion of 322 km s-1.
The goals of this work are to study new faint members using
the Sloan Digital Sky
Survey (DR4)
(Adelman-McCarthy et al. 2006)
to extend the list of known group members and study photometric scaling
relations, the distribution of morphological
types, as well as the spectroscopic properties of the low-luminosity
galaxy population. The paper is organized as follows.
Section 2
provides a brief overview on the sample selection and data analysis
procedures. Section 3 focuses on the low-luminosity galaxy
population and presents the photometric and spectroscopic data of all
individual objects. Finally, our
results are summarized and discussed in Sect. 4. A group
distance of 26.1 Mpc based on the work of MTT05 is
used
throughout this paper corresponding to a distance modulus of m-M=32.08.
The systemic velocity of the group is assumed to be represented
by that of NGC 5846, which is vr=1710 km s-1.
To separate between dwarf and bright galaxies, an
absolute magnitude of
is used (Ferguson &
Binggeli 1994) except when otherwise stated. Total magnitudes
presented in
this work are SDSS model magnitudes
.
2 Sample selection and data analysis
To extend the existing sample of low-luminosity galaxies in the
NGC 5846 system, we searched in the SDSS database for all
galaxies
with cz<3000 km s-1
within a radius of Mpc,
similar to the second turnaround radius r2t=1.85
presented by MTT05
.
Galaxies beyond these limits are
very likely to be either field or background objects. The query
resulted in a total sample of 74
galaxies, 19 bright objects and 55 dwarfs (see Table 1 and Fig. 1) with seven objects
found in the outer
parts (>
)
of the system that have no entry in previous catalogues. Though
slightly fainter than
,
UGC 9751 and UGC 9760 are listed as bright members
because of their classification as Scd and Sd in NED
.
Corrected FITS frames (bias subtracted, flat-fielded, and
cleaned of bright stars) were extracted from the SDSS for
these 55 dwarfs in the ,
,
and
bands
. SDSS model magnitudes
were adopted from the database for each individual galaxy and
transformed to the
Johnson-Morgan-Cousins B band by means of
transformation equations from Smith
et al. (2002). Absolute magnitudes were
derived assuming an average extinction value of
from Schlegel et al. (1998)
for the entire galaxy population. An isophote
analysis was carried out for the dE subsample using the ellipse
task within the IRAF stsdas
package to fit ellipses to the galaxy images and measure the deviations
from purely elliptical isophote
shapes. A detailed description of the procedure is given by Jedrzejewski (1987). The
analysis resulted in surface
brightness profiles and the harmonic content of the isophotes. A Sérsic (1968) law
with an effective radius
,
an effective surface brightness
,
and a shape
parameter n as free parameters was fit to each
object. The quantity bn
is a function of n and chosen so
that half the galaxy luminosity is located within the effective radius
.
The fitting was carried out using a Levenberg-Marquardt algorithm until
a minimum in
was
achieved, yielding the parameters n,
,
and
with the corresponding uncertainties. The
innermost parts of the surface brightness profiles (
1.4 arcsec)
have not been taken into account
for the fitting procedure to avoid the effects of seeing. Central
surface brightnesses
were derived from the fit. The results of the isophote analysis are
presented in
Table 2.
Sérsic models were subtracted from the original images yielding
residual frames that were
investigated for photometric substructures. In addition to the
photometric data, wavelength and flux-calibrated
spectra (sky subtracted and corrected for telluric absorption) were
examined for all sample galaxies. The
spectra cover a wavelength range of
Å
and were checked for spectral lines in both emission
and absorption. Identified spectral lines were fit by Gaussians
yielding central wavelengths and full widths at
half maximum (FWHM). The derived central wavelengths were subsequently
used to verify SDSS redshifts.
Table 1:
Galaxies within 2
around NGC 5846 as studied in this work.
3 The low-luminosity galaxy population
![]() |
Figure 1:
Projected spatial distribution of NGC 5846 group members as
studied in this work. Filled triangles indicate
bright members, while open ones represent the low-luminosity galaxies.
Numbers refer to the galaxy identification of Table 1. The circle shows
the 2 |
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![]() |
Figure 2:
Colour-magnitude diagram of NGC 5846 group members. Numbers as
in Fig. 1.
The dashed line indicates
the red-sequence linear fit to bright galaxies and early-type dwarfs: |
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![]() |
Figure 3: Sérsic shape parameter versus absolute blue magnitude of early-type galaxies in the NGC 5846 group. Open symbols represent dwarf ellipticals, while filled triangles show bright ellipticals. The horizontal lines indicate exponential and de Vaucouleurs r1/4 laws. |
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Table 1 lists the NGC 5846 galaxy group sample studied in this work. Morphological types for dwarfs were classified by the visual inspection of SDSS images and spectra. Objects with a smooth light distribution and exponential profiles were classified as dEs. The dE ellipticity was determined from the isophote analysis. Dwarfs showing a blue patchy appearance and emission lines were classified as dIrrs. Morphological types for bright galaxies were taken from NED. Dwarfs are identified with increasing projected radial distance from NGC 5846.
We extend previous group member lists with seven new objects
in the outer parts (>
)
of the system
that have no entry in previous catalogues. Despite exhibiting slightly
brighter values than
,
some
galaxies were classified as dwarfs because of their nearly exponential
surface brightness profiles or their
compactness. Thirty-five dwarfs (
63%) were identified as dEs according to their
optical
appearance and red colours
.
Eighteen objects (
32%)
are dwarf irregulars with a patchy,
blue optical appearance and emission lines, both indicative of ongoing
star formation. Three galaxies (
1%) exhibit
photometric fine structure and sizes that are in-between those of dwarf
and bright galaxies. Eleven dwarfs (
31% of the dEs) are
found to be nucleated on the basis of the analysis of their surface
brightness profiles.
Our list of nucleated dwarfs is almost identical to the list
obtained by MTT05 with exception of only three objects classified
differently. Taking the Schechter luminosity function derived by MTT05,
we conclude that with an absolute magnitude
of
for our faintest object, our sample consists of at most 34% of the
total number of galaxies expected
in the system to a limiting magnitude of
.
Our sample yields a dwarf-to-giant-ratio (DGR) of
3 as lower
limit. Following
the photometric dwarf classification of MTT05, this value could rise to
12,
confirming that the NGC 5846 group is indeed one of the
richest groups in the Local Supercluster.
The projected spatial distribution of all investigated
galaxies is illustrated in Fig. 1. The distribution
indicates two substructures of the system around the two brightest
ellipticals NGC 5846 and NGC 5813. A third,
much smaller subgroup can be discerned around UGC 9760, which in
contrast to the NGC 5846 and NGC 5813 aggregates, has
no noteworthy X-ray counterpart. We present in Fig. 2 a colour-magnitude
diagram for the studied
group galaxy population. The diagram indicates the prevalence of an
early-type dwarf morphology and the continuation
of a red sequence similar to that found in galaxy clusters (Gladders et al. 1998)
into the dwarf regime. Figure 3 shows the
relation consisting of our dE sample as well as the bright galaxies
classified as ellipticals in NED. Sérsic shape
parameters of the low-luminosity galaxy population show a mean value of
n=1.19 with a scatter of
representing
nearly exponential surface brightness profiles as expected for dwarf
ellipticals. Three dwarfs
(N5846_10, N5846_15, N5846_43) show comparatively large error bars of
the shape parameter because of their faintness or contamination of
their
surface brightness profiles by a central nucleus. Our data confirm the
trend of more luminous galaxies having higher shape
parameters, thus a steeper surface brightness profile than the less
luminous objects. Interestingly there are no objects
with intermediate Sérsic parameters between 2<n<3.
NGC 5813 shows a comparatively high shape parameter around
.
3.1 Scaling relations
When addressing the question of the influence of the environment on the
evolution of galaxies, scaling relations of
the photometric properties of early-type galaxies are a useful tool.
However, the environment does not
seem to affect all early-type systems in a similar way. The fundamental
plane of bright ellipticals is found to be almost independent
of environment, while dwarf ellipticals exhibit a stronger
environmental dependence (Peterson & Caldwell 1993;
Nieto
et al. 1990). Elliptical galaxies and bulges are
known to exhibit a tight correlation in the
plane such that higher surface brightnesses
correspond to lower total luminosities (Kormendy et al. 2009; Kormendy 1985).
Dwarf galaxies exhibit an opposite trend, being a
distinct class of objects with possibly different formation and
evolution histories. Binggeli
& Jerjen (1998), hereafter
[BJ98] investigated the
plane for Virgo cluster early-type dwarfs and confirm this
trend. Figure 4(a)
shows the
plane for our dEs and the relationship
determined by BJ98 (dash-dotted line) for their sample of Virgo dwarf
ellipticals (assuming a Virgo distance of 16.5 Mpc
corresponding
to a distance modulus of
31.09).
The figures Figs. 4(b)-(f)
focus on
,
,
,
,
and ellipticity
.
Sérsic shape parameters used here should
not be compared directly with those of BJ98, because
.
The parameter r0 is the
scale radius
of the Sérsic model
.
Table 2
presents the corresponding values of the
isophote analysis. Objects with larger errors than the data itself are
not listed.
Our data in the
plane are in agreement with the work of BJ98. One object falling
outside
the
limit is N5846_01, which has a comparatively too high surface
brightness according to its luminosity (see
Sect. 3.2).
In the
plane, our data show a larger scatter
.
Compared to the dwarf
sample of the Virgo cluster, our dwarfs agree with the Virgo dwarf
relation, however. Our sample also confirms a trend between shape
parameter
n and scale radius r0
with smaller objects exhibiting higher shape parameters. Again N5846_01
is the only object in our sample to
fall away from the trend. The scale radius r0
is also strongly correlated with the central surface brightness as
seen in the
plane. The NGC 5846 dwarfs follow the relation obtained for
the Virgo dwarfs with a
lower scatter in magnitude (
mag arcsec-2)
than that measured by BJ98, who derive a value of
mag arcsec-2.
As for BJ98, we also derived the best-fit linear combination between
shape parameter n, central surface brightness
,
and absolute B band magnitude with a scatter of
mag.
Finally, we also checked whether a correlation exists
between shape parameter n and ellipticity. There is
a slight trend of flattened objects showing shallower surface
brightness profiles.
![]() |
Figure 4:
Photometric scaling relations of the low-luminosity galaxy population
in the NGC 5846 group. In panels
a)- d), dash-dotted lines
are the relations of the Virgo cluster early-type dwarfs from BJ98
assuming a distance to the
Virgo cluster of 16.5 Mpc. The scatter in our data
with respect to the BJ98 relations is given in the lower left corner of
each
panel. One- |
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The structural properties of early-type systems can in
addition be investigated by the Hamabe
& Kormendy (1987)
relation, a photometric projection of the fundamental plane of galaxies
relating the logarithm of effective radii and
effective surface brightnesses linearly (Ziegler et al. 1999; di Serego
Alighieri et al. 2005). This relation divides
early-type systems into regular
and bright classes separated at the effective
radius of kpc
(Capaccioli et al. 1992).
In hierarchical
evolution scenarios, regular galaxies are understood to be the
progenitors of bright ones that evolve through successive
mergers along the Hamabe-Kormendy relation (Capelato
et al. 1995). However, the numerical simulations of Evstigneeva et al. (2004)
suggest that
low mass systems such as dwarf galaxies can only follow this scenario
when a large amount of dissipation is involved.
Figure 5
shows the Hamabe-Kormendy relation for the faint galaxy population of
our work. Open
squares are dwarfs from X-ray faint and X-ray bright groups studied by Khosroshahi et al. (2004).
All faint galaxies of
our sample are regular systems with similar properties to those of the
dwarfs from Khosroshahi
et al. (2004): this suggests that there is no
strong difference in structural properties of the early-type dwarfs
between the NGC 5846 group and other group environments.
Again,
N5846_01 is the only dwarf clearly separated from the main cloud of
dEs.
Table 2: Surface photometry of the low-luminosity galaxy sample.
3.2 Comments on individual objects
Most of the dwarfs investigated do not have any photometric or
spectroscopic peculiarities, although a few galaxies in the sample
deserve a closer examination. Figure 6 presents all objects
that clearly exhibit fine structure in their optical appearance
with
band images and residual frames shown for each galaxy. Because of their
relatively large angular diameters, the sizes of
these objects are in-between those of dwarf and bright galaxies.
![]() |
Figure 5:
|
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N5846_01 is the closest dwarf elliptical to
NGC 5846 with a much higher central surface brightness than
the remainder of our dwarfs.
Furthermore it is the reddest galaxy in our low-luminosity galaxy
sample. With an average effective radius of only pc
in all studied passbands, this object is also the most compact of our
sample. Because of its visual appearance and close
proximity to NGC 5846, MTT05 suggested that N5846_01 has
probably been affected by tidal stripping and should therefore
be classified instead as an ultra compact dwarf. This idea is also
supported by the nearby object NGC 5846A exhibiting a
similar morphological appearance. Indeed, NGC 5846A is an
extremely rare compact elliptical similar to
M 32, which is the prototypical
object of this class. Thus, N5846_01 is perfectly consistent with a
scenario in which the structural differences of compact
ellipticals and ordinary dEs are produced when the compacts form within
the potential well of another massive galaxy, whereas dEs
evolve as isolated systems (Burkert 1994).
N5846_07 is classified as an S0/a galaxy by
MTT05 and was originally considered as an almost certainly background
object in
their sample because of its optical appearance. Spectroscopy however
confirmed its group membership. Assuming the group distance to be
26.1 Mpc, the galaxy has a
projected diameter of kpc,
which implies that the galaxy size is in-between those of bright and
dwarf galaxies. The
spectrum of N5846_07 uncovers strong H
emission and weaker H
,
[N II], and [S II]
features, which are indicative of ongoing
star formation. Two spiral arms are identified in the optical image,
which could also be interpreted as signatures of ongoing
interaction with the nearby irregular dwarf N5846_08, only 21kpc away.
N5846_41/42 are two large HII regions of
the irregular dwarf KKR15 (Karachentseva et al. 1999;
Huchtmeier
et al. 2000), which are
classified as individual galaxies in SDSS. The host galaxy shows an
extremely blue colour, the majority of its light originating in the two
HII regions. The brighter component, N5846_41, is the bluest object of
our sample. Because of the high concentration of its light,
N5846_41/42 has by far the highest S/N ratio
of all spectra in our sample. Besides the usual H,
H
,
[O III], [N II],
and
[S II] features, both spectra
also exhibit the weaker Balmer lines H
,
H
,
and H
along with the more
uncommon HeI
5875.6,
[Ne III]
3868.7, and Ar III
7135.8
transitions. Of all emission-line galaxies in
our sample, N5846_41/42 has the lowest oxygen abundance with an average
value of
O/H)=7.68
(see Sect. 3.4).
N5846_54 and N5846_55
were both classified as S0 galaxies in the MTT05 sample and are the
only objects of our work that
have photometric substructures. With projected linear sizes of
and 7 kpc, respectively, these objects have, as for
N5846_07, sizes that are in-between those of dwarf and bright galaxies.
The surface brightness profile of N5846_55 exhibits a rather flat
gradient out
to 14 arcsec, wherefrom the light distribution falls far more
steeply, indicative of a possible bar feature (Gadotti
et al. 2007).
Spectroscopically, both galaxies exhibit ongoing star formation.
3.3 Spatial distribution of morphological types
We studied the morphology distribution for the low-luminosity galaxy
population in the NGC 5846 system for both the early- and
late-type
populations. Figure 7
illustrates the clustering of both the dE and dIrr samples with the
projected number
density shown separately for each morphological type. The diagram
displays the same field of view presented in
Fig. 1.
Density contours were created using a grid with a spatial resolution of
.
The segregation between early- and late-type low-luminosity galaxies in
the NGC 5846 system is clearly evident: dwarf
ellipticals are found predominantly in the vicinity of bright galaxies,
while irregular systems are clearly detached from this distribution
and diffusely arranged in the outer regions of the group. Morphology
shows also a strong correlation with the projected number density.
Early-type dwarfs populate the high-density regions around
NGC 5846 and NGC 5813, while irregulars show
comparatively low
agglomeration. Moreover, the satellite morphologies resemble the
morphology of their elliptical hosts (NGC 5846 and
NGC 5813). Similar
results were found by Weinmann
et al. (2006), who, on the basis of a large sample
of SDSS groups, inferred that the satellite morphologies
in groups correlate strongly with the morphology of the central host
galaxy. In terms of the radial morphology distributions,
Fig. 7
indicates that the projected number density of the early-type
population exhibits a much steeper
radial gradient than the irregular subsample. In addition to the
optical picture, the diffuse X-ray component also correlates spatially
with the early-type dwarf distribution (see MTT05); this component
should represent the dark matter potentials of the group. We also
studied the distribution
of nucleated dwarfs within the NGC 5846 system shown in
Fig. 8.
With the exceptions of two objects, all nucleated dwarfs
are found to be in the vicinity (
260 kpc) of NGC 5846 and
NGC 5813. Research on the distribution of nucleated dwarfs in
the
Virgo cluster has also shown that these nuclei are predominantly found
in the central regions of the cluster and not in the cluster
outskirts (Binggeli &
Cameron 1991). Oh & Lin
(2000) argued that this could be explained by assuming the
nuclei to be the result
of the orbital decay of globular clusters. By means of a series of
numerical simulations, they showed that dwarf
galaxies exposed to a little external tidal perturbation dynamical
friction can reproduce the significant orbital decays of
globular clusters and the formation of compact nuclei within a Hubble
time. Thus, a larger fraction of nucleated dwarfs is
expected in the centres of galaxy clusters, where the extragalactic
tidal perturbation tends to preserve the integrity of dwarf
galaxies, unlike in the outskirts, where this perturbation tends to be
disruptive.
![]() |
Figure 6:
Modeling of faint galaxies with significant fine structure. Figures
show SDSS |
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3.4 Emission-line dwarfs
Fluxes measured from H,
H
,
[N II]
6548.1, 6583.4 Å, [O III]
4958.9,
5006.8 Å, and [S II]
6717.0,
6731.3 Å spectral lines and star formation rates and
oxygen abundances were measured for
dwarfs showing emission lines in their spectra. The data are presented
in Table 3.
Star formation rates (SFRs)
were derived by means of H
fluxes using the Kennicutt (1998)
relation:
.
H
extinction was taken
into account using an average extinction value of
mag based on
Kennicutt (1983) and Niklas et al. (1997). In
addition, Galactic extinction
mag
was also taken into
account so that a total extinction value of 1.10 mag for H
was allowed. Errors in the star formation
rates were estimated by assuming H
photon noise to be the dominant error source. Star formation rates of
galaxies
exhibiting H
fluxes with S/N<15 are
not listed in Table 3.
Emission
characteristics were analysed by calculating the
line flux
ratios
,
,
and
according to
Veilleux &
Osterbrock (1987). Oxygen abundances were estimated using
the N2 index (
)
method as
defined by Denicoló et al.
(2002):
.
Extinction and reddening effects
and particular absorption components related to H
and H
can considerably affect line flux
measurements. A correction was applied to the emission-line galaxies by
taking H
extinction into account and
assuming a Balmer decrement of H
/H
for HII region-like galaxies (Veilleux
& Osterbrock 1987) to consider H
extincion
too.
![]() |
Figure 7: Clustering properties of both early and late-type dwarfs of the NGC 5846 system. Contours are linearly spaced and show the projected number density of the distinct morphological populations. Triangles refer to bright group members. The values indicate the number of galaxies per 0.25 square degree. |
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![]() |
Figure 8: Distribution of nucleated dwarfs in the NGC 5846 group. Black triangles are bright group members, open triangles dEs without nucleus. Diamonds show nucleated dwarfs, concentrated around NGC 5846 and NGC 5813 (circles indicate a radius of 260 kpc). |
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![$\textrm{[N~\begin{tiny}II\end{tiny}]}~\lambda6583/\textrm{H$\alpha$ }$](/articles/aa/full_html/2010/03/aa11013-08/img91.png)
![$\textrm{[S~\begin{tiny}II\end{tiny}]}~(\lambda6716+\lambda6731)/\textrm{H$\alpha$ }$](/articles/aa/full_html/2010/03/aa11013-08/img93.png)
4 Discussion and conclusions
We have undertaken an analysis of the photometric and spectroscopic
properties of the low-luminosity galaxy population of the
NGC 5846
group of galaxies located in the Virgo III Cloud of galaxies in the
Local Supercluster. This group is of particular
interest because it is the most massive of only three dense groups
(NGC 4274, NGC 5846, and M96) in the Local
Supercluster
that are dominated by elliptical and lenticular galaxies, and is the
third most massive aggregate of early-type galaxies
(after the Virgo and Fornax clusters) in the local universe. Of the 19
bright galaxies in our sample, E and S0 galaxies
constitute 58%.
Seven new group members in the outer regions (>
)
of the group have been identified using
SDSS and NED redshifts, complementing existing member catalogues.
The dwarf-to-giant-ratio (DGR) of the NGC 5846 system
is high: our sample of spectroscopically determined group members
yields a DGR of
3. Taking
into account the photometric classification of group members to
by MTT05 this value could rise to
12. Ferguson & Sandage (1991)
demonstrated that the DGR increases with the richness of a group and
corresponds to an early-type-dwarf-to-giant-ratio (EDGR) (i.e.,
dE+dE,N+dS0 to E+S0) of 5.77 for the Virgo cluster and 3.83 for the
Fornax cluster to
.
For the
Coma cluster, Secker &
Harris (1996) state an EDGR of
to
.
Our data yield an EDGR of 2.69 for the NGC 5846 system to
our faintest dwarf (
). This value shows that the
NGC 5846 system has fewer early-type dwarfs per giant
early-type galaxy than
clusters but still a much larger EDGR than other groups (Leo: 1.48,
Dorado: 1.44, NGC 1400: 2.08; all down to
,
see
Ferguson & Sandage 1991),
indicating that NGC 5846 is indeed one of the more massive
aggregates in the Local Supercluster.
A colour-magnitude diagram of the investigated group members contains a red sequence displaying the well-known trend of early-type galaxies exhibiting redder colours (higher metallicities) at higher luminosities (Caldwell 1983). In contrast, irregular dwarfs do not form a sequence but show a large spread in colours. There is no evident segregation between bright galaxies and dwarfs.
Photometric scaling relations have been studied for early-type
dwarfs and compared with the relations derived by BJ98 for Virgo
cluster dwarf ellipticals. If bright ellipticals and early-type dwarfs
share a similar evolution, a continous
sequence in scaling relations with respect to the galaxy luminosity
would be expected. It is known that in the
surface-brightness-luminosity ()
plane (Kormendy
et al. 2009; Kormendy 1985), early-type
dwarfs and bright ellipticals follow
different trends, implying that dwarf galaxies are a distinct class of
objects that have followed different evolutionary paths to ordinary
ellipticals. Our data match the trends of Virgo cluster dEs suggesting
a similar structure and
origin of the dwarfs in both the Virgo cluster and the
NGC 5846 group. However, one special object falling off the
main
cloud of early-type dwarfs is N5846_01. It is the closest dwarf to
NGC 5846 and shows a comparatively high surface
brightness and compactness compared to the other dwarfs investigated.
In the
plane, the
object lies outside the
limit
compared to the relation of BJ98. Owing to its proximity to
NGC 5846, the galaxy has probably been affected by tidal
stripping and can therefore be classified as an
ultra compact dwarf. This idea is also supported by the nearby object
NGC 5846A, the elliptical companion
to NGC 5846, having a similar morphological appearance, though being
too bright to be considered as a dwarf. Indeed, NGC 5846A is
one of the extremely rare compact ellipticals
like M 32, the prototype of this class. N5846_01 confirms the
idea that the structural differences of compact ellipticals and
ordinary dEs can be explained if the compacts formed
within the potential well of another massive galaxy, whereas dEs
evolved as isolated systems (Burkert
1994). Our data also show
that early-type dwarfs with high ellipticity tend to have shallower
surface brightness profiles. We also checked the
location of the NGC 5846 low-luminosity galaxy population in
the
plane with respect to the Hamabe-Kormendy relation, which is a
photometric projection of the fundamental plane of galaxies relating
the logarithm
of effective radii and effective surface brightnesses linearly. The
NGC 5846 dwarfs are regular galaxies
according to the classification of Capaccioli
et al. (1992), indicating that these systems are the
building blocks of more
massive galaxies, in agreement with
CDM cosmology. Moreover, the
dwarfs are comparable to the dwarfs from
X-ray dim and X-ray bright groups studied by Khosroshahi
et al. (2004).
Scaling relations for dwarf ellipticals are not the only means
of studying their origin and evolution. The study of morphological
segregation within
clusters and groups also provides the opportunity to test the formation
and environmental dependence of the faint
galaxy population. The well-known morphology-density relation (Dressler 1980) is not only
restricted to the normal
Hubble types but is also found to apply to dwarf galaxies (Binggeli et al. 1987).
This relation has been investigated in
detail in our immediate vicinity, the Local Group (Grebel
1999). We confirm this morphology-density relation for dwarf
galaxies in the NGC 5846 system. While early-type dwarfs are
concentrated around the two massive ellipticals
NGC 5846 and NGC 5813, objects of irregular type are
more randomly distributed and found predominantly in
the outer regions. This morphological segregation could be explained by
gas stripping due to the infall of the dwarfs towards
the group centre. This scenario was also investigated by Weinmann et al. (2006)
and Park et al. (2008),
who inferred that
satellite morphologies in groups tend to be similar to those of their
hosts. Because of the comparatively high density of the
NGC 5846 system and the hot and dense halo gas present around
NGC 5846 and NGC 5813, the
dependence of the satellite morphology on host morphology can be
interpreted by the hydrodynamic and radiative interaction of
the hot X-ray gas of the two host galaxies with their surrounding
satellites. We have also checked the distribution of nucleated
dwarfs in the NGC 5846 system with respect to non-nucleated
ones. Interestingly, nearly all dwarfs that contain a nucleus
superimposed on their underlying smooth surface brightness profile are
found in the vicinity of NGC 5846 and NGC 5813
within a radius of 260 kpc.
This is in agreement with the work of Binggeli
& Cameron (1991) for the Virgo
cluster, who show that dwarfs located near the centre of the cluster
are mostly nucleated while those in the outskirts are
non-nucleated. Assuming that the formation of the nuclei is related to
the orbital decay of globular clusters, Oh
& Lin (2000) argued
that this could be explained by extragalactic tidal perturbation, which
tends to preserve the integrity of dwarf galaxies at cluster
centres but tends to disrupt dwarf galaxies in their outskirts.
Table 3: Spectral properties of emission-line dwarfs.
![]() |
Figure 9: Classification of emission-line galaxies in the NGC 5846 group according to Veilleux & Osterbrock (1987). The line separates HII region-like galaxies from AGNs. All measured objects show flux ratios explained by simple photoionization. |
Open with DEXTER |
Only two objects of the low-luminosity galaxy population
exhibit photometric fine structure. These galaxies exhibit ongoing star
formation and
diameter sizes that are in-between those of dwarf and bright galaxies.
This lack of photometric peculiarities in the low-luminosity galaxy
population
emphasises that the NGC 5846 system is an old, well-evolved
aggregate, where no recent interactions between individual members
have occurred. Emission characteristics and star formation rates of the
irregular dwarfs exhibit typical values for
low-luminosity galaxies, additionally supporting the idea of a system
that does not exhibit recent activity that is enhancing star formation.
Oxygen abundances have been derived indirectly via the N2
index method proposed by
Denicoló et al. (2002).
Our abundances show a large scatter (
dex) with respect to
the metallicity-luminosity relation of
Richer & McCall (1995)
due to the intrinsic scatter in the N2
method itself. Nevertheless, all objects outside 1
confidence intervals
lie above the metallicity-luminosity relation, indicating a
comparatively high oxygen abundance for irregular dwarfs in the
NGC 5846 group.
Our study of the low-luminosity galaxy population of the NGC 5846 group has found that the dwarf galaxies in this massive group match the trends observed for dwarf galaxies in other aggregates, which implies that they have similar formation and evolution scenarios. The spatial distribution of morphological types suggests that the structural properties of dwarf galaxies are clearly dependent on the location within the group. The structural properties of the dwarfs confirm the evolved state of the system. The group remains unusual because of predominant early-type morphology of its members, the strong X-ray emission, and the high dwarf-to-giant-ratio compared to other groups.
![]() |
Figure 10:
Oxygen abundances versus abolute B magnitudes of NGC 5846
irrgeluar dwarfs. The abundances were determined
indirectly using the N2
method as proposed by Denicoló
et al. (2002). The dash-dotted line shows the
metallicity-luminosity relation of
Richer & McCall (1995).
One- |
Open with DEXTER |
We acknowledge the useful comments from the anonymous referee which helped to improve the paper. We are also very grateful to the language editor, Claire Halliday, for her careful reading of the manuscript. P.E. has been supported by the University of Vienna in the frame of the Initiativkolleg (IK) The Cosmic Matter Circuit I033-N. This work has made use of the astronomical data reduction software IRAF which is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy Inc., under cooperative agreement with the National Science Foundation.
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Footnotes
- ... density
- Densities taken from the Nearby Galaxies Catalog (Tully & Fisher 1988), see Tully (1988) for details.
- ... magnitudes
- SDSS model magnitudes are based on a matched galaxy model that provides an optimal measure of the flux of a galaxy. The code fits a deVaucouleurs profile as well as an exponential profile to the two-dimensional image. The best-fit model is stored as the model magnitude.
- ... MTT05
- Bound group members decouple from the Hubble flow at first turnaround, i.e., the zero-velocity surface around the group (Sandage 1986), begin to collapse, and again expand to a radius of second turnaround, finally oscillating and exchanging kinetic energy with other group members (Bertschinger 1985).
- ... NED
- http://nedwww.ipac.caltech.edu/
- ... bands
- See Fukugita et al. (1996) for a description of the SDSS photometric system.
- ... radius
- The exact relation between nand bn
is derived by
, where
and
are the complete and incomplete gamma functions, respectively. A good approximation is bn=1.9908n-0.3118 for
, which has been used in this work.
All Tables
Table 1:
Galaxies within 2
around NGC 5846 as studied in this work.
Table 2: Surface photometry of the low-luminosity galaxy sample.
Table 3: Spectral properties of emission-line dwarfs.
All Figures
![]() |
Figure 1:
Projected spatial distribution of NGC 5846 group members as
studied in this work. Filled triangles indicate
bright members, while open ones represent the low-luminosity galaxies.
Numbers refer to the galaxy identification of Table 1. The circle shows
the 2 |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Colour-magnitude diagram of NGC 5846 group members. Numbers as
in Fig. 1.
The dashed line indicates
the red-sequence linear fit to bright galaxies and early-type dwarfs: |
Open with DEXTER | |
In the text |
![]() |
Figure 3: Sérsic shape parameter versus absolute blue magnitude of early-type galaxies in the NGC 5846 group. Open symbols represent dwarf ellipticals, while filled triangles show bright ellipticals. The horizontal lines indicate exponential and de Vaucouleurs r1/4 laws. |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Photometric scaling relations of the low-luminosity galaxy population
in the NGC 5846 group. In panels
a)- d), dash-dotted lines
are the relations of the Virgo cluster early-type dwarfs from BJ98
assuming a distance to the
Virgo cluster of 16.5 Mpc. The scatter in our data
with respect to the BJ98 relations is given in the lower left corner of
each
panel. One- |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
|
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Modeling of faint galaxies with significant fine structure. Figures
show SDSS |
Open with DEXTER | |
In the text |
![]() |
Figure 7: Clustering properties of both early and late-type dwarfs of the NGC 5846 system. Contours are linearly spaced and show the projected number density of the distinct morphological populations. Triangles refer to bright group members. The values indicate the number of galaxies per 0.25 square degree. |
Open with DEXTER | |
In the text |
![]() |
Figure 8: Distribution of nucleated dwarfs in the NGC 5846 group. Black triangles are bright group members, open triangles dEs without nucleus. Diamonds show nucleated dwarfs, concentrated around NGC 5846 and NGC 5813 (circles indicate a radius of 260 kpc). |
Open with DEXTER | |
In the text |
![]() |
Figure 9: Classification of emission-line galaxies in the NGC 5846 group according to Veilleux & Osterbrock (1987). The line separates HII region-like galaxies from AGNs. All measured objects show flux ratios explained by simple photoionization. |
Open with DEXTER | |
In the text |
![]() |
Figure 10:
Oxygen abundances versus abolute B magnitudes of NGC 5846
irrgeluar dwarfs. The abundances were determined
indirectly using the N2
method as proposed by Denicoló
et al. (2002). The dash-dotted line shows the
metallicity-luminosity relation of
Richer & McCall (1995).
One- |
Open with DEXTER | |
In the text |
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