A&A 484, 655-670 (2008)
DOI: 10.1051/0004-6361:20078361
P. Focardi1 - V. Zitelli2 - S. Marinoni1,3
1 - Dipartimento di Astronomia, Universitá di Bologna, Italy
2 -
INAF - OABO, Via Ranzani 1, 40127 Bologna, Italy
3 -
Fundacion Galileo Galilei & TNG, PO Box 565 S/C de la Palma,
Tenerife, Spain
Received 26 July 2007 / Accepted 8 March 2008
Abstract
Context. The role played by interaction on galaxy formation and evolution continues to be debated. Several questions remain open, among them whether, and to what extent, galaxy interaction induce nuclear activity, as theoretical predictions, so far, have not been adequately supported by observations. Part of the uncertainty affecting the observational results is likely to be due to the limited sizes and the inhomogeneity of the samples.
Aims. Galaxy pairs are ideal sites in which to investigate the role of interaction on nuclear activity, since the proximity, in redshift and in projected separation, between members make interaction and encounters highly probable. For this reason we have undertaken a spectroscopic survey of a large homogeneous sample of galaxy pairs (UZC-BGP) selected applying an objective neighbour search algorithm to a 3D galaxy catalog (UZC).
Methods. We present the results of the nuclear spectral classification, performed using standard diagnostic diagrams, of 48 UZC-BGPs, which represents more than half of the whole sample and has an excellent morphological match with it.
Results. The fraction of emission line galaxies in our pair sample is large, especially among spirals where it reaches 84% and 95%, for early and late spirals. Star Burst (SB) is the most frequent type of nuclear activity encountered (30% of galaxies), while AGNs (Active Galactic Nuclei) make only 19%. The fractions increase to 45% and 22% when considering only spirals. Late spirals are characterized by both an unusual increase (35%) of AGN activity and high luminosity (44% have
). LLAGNs (Low Luminosity AGNs) are only 8% of the total number of galaxies, but this kind of activity could be present in another 10% of the galaxies (LLAGN candidates). If confirmed, these candidates would make LLAGNs constitute a significant fraction of the whole AGN (LLAGN + AGN) population, and raise the AGN population as a whole to 37%. Absorption line galaxies reside mostly (61%) in S0 galaxies and display the lowest B luminosity in the sample; only 18% of them have
,
but together with LLAGNs (candidates included) they are the most massive galaxies in the sample. Intense-SB nuclei are found in galaxy pairs with galaxy-galaxy projected separation of up to
160 h-1 kpc suggesting that in bright isolated galaxy pairs interaction may be at work and effective up to that distance.
Conclusions. AGNs are characterized by an advanced morphological type while the SB phenomenon occurs with the same frequency in early and late spirals. Whether and how these unusual characteristics relate to the pair environment needs to be further investigated. LLAGNs and LLAGN candidates do not always show similar properties; the former are more luminous in B, richer in early-type (E-S0s) galaxies, and half of them are hosted in galaxies showing visible signs of interaction with fainter companions. This last finding suggests that minor interactions might be a driving mechanism for a fraction of LLAGNs. The differences between LLAGNs and LLAGN candidates might confirm the heterogeneous nature of this class of objects.
Key words: galaxies: active - galaxies: interactions
The role played by interactions; on galaxy formation and evolution remains hotly debated, involving both the ``far'' and ``local'' universe. Hierarchical models of galaxy formation invoke a regular occurrence of interaction and merging phenomena, which are expected to increase with redshift (Gottlober et al. 2001; Governato et al. 1999) and affect morphologies, gas distribution and the population of galaxies (Dubinski et al. 1996; Mihos & Hernquist 1996). Evolution of the merging rate with z has been estimated using close galaxy pairs, but results are conflicting (Carlberg et al. 1994; Le Fevre et al. 2000; Bundy et al. 2000; Zepf & Koo 1989), which is not unexpected due to differences in sample depths, observational techniques and selection criteria (Patton et al. 2000). Interaction and mergers are less frequent in the ``local'' universe, but can be analysed in more detail. Nearby galaxy systems can be investigated at faint luminosity, on a wide spatial scale and with a better knowledge of the surrounding environment. However, even ``locally'' theoretical expectations have not found adequate support from observational data. Galaxy interaction should be extremely effective in redistributing large amounts of material towards the galaxy central regions, giving rise, in this way, to violent bursts of star formation (Barnes & Hernquist 1991). Tidal interaction between galaxies is expected to induce instabilities in the discs, able to generate galaxy bar formation, which, producing an inflow of gas towards the galaxy central regions, may even activate the AGN phenomenon (Noguchi 1988; Barnes & Hernquist 1991). However, observations concerning the amount and level of nuclear activity in nearby interacting systems so far have produced conflicting results neither able to confirm nor to definitely rule out theoretical expectations. In fact, eventhough, starting with Larson & Tinsley (1988), there has been growing evidence of an increase in star formation in interacting galaxy systems (e.g. Kennicutt et al. 1987; Kennicutt & Keel 1984; Keel 1996,1993; Barton et al. 2000; Donzelli & Pastoriza 1997), a one-to-one correlation between galaxy-galaxy interaction and star formation remains unclear. Such a correlation holds only for an extremely limited number of objects (ULIRGs, Sanders & Mirabel 1996) which show a fraction of interacting galaxies nearly close to 100% (Borne et al. 1999; Sanders et al. 1988), while there are several interacting systems with no sign of star formation. The situation becomes even more complex and controversial for the so-called AGN-interaction paradigm for which conflicting results have been given so far (Dahari 1985; Kelm et al. 2004; De Robertis et al. 1998; Fuentes-Williams & Stocke 1988; Rafanelli et al. 1995; Schmitt 2001; MacKenty 1989; Keel et al. 1985; Kelm et al. 1998). However a large part of this contradiction is likely to be due to inhomogeneities among the analyzed samples which are often small, have been selected by different methods and criteria, and may be biased towards or against certain kind of systems.
Galaxy pairs are ideal sites to investigate the role of interaction on nuclear activity since proximity in redshift and in projected separation make interaction and encounters between member galaxies highly probable. The recent availability of a large and complete nearby 3D galaxy catalog (UZC, Falco et al. 1999) has made it feasible to select a volume-limited sample of 89 Bright Galaxy Pairs (UZC-BGP, Focardi et al. 2006, hereafter Paper I) which does not suffer from velocity/distance biases or contamination by projection effects. At variance with previous available nearby pair samples (KPG, Karachentsev 1972; RR, Reduzzi & Rampazzo 1995), the first selected visually from the POSS plates, the second applying KPG criteria to the ESO-LV catalog (Lauberts & Valentijn 1989), the UZC-BGP sample has been selected by means of an objective neighbour search algorithm (Focardi & Kelm 2002) applied to the UZC catalog; it is thus complete, homogeneous and contains pairs which are already close in 3D space.
The analysis of UZC-BGP, based on available data (Paper I), has allowed us to show that ellipticals are extremely rare and underluminous (in B), while late spirals (>Sc) are overluminous. This finding confirms previous claims (Kelm & Focardi 2004) linking the formation of bright ellipticals to group/cluster environment and suggest that galaxy-galaxy interactions might be responsible for the blue luminosity enhancement of disk galaxies through SF phenomena. This last suggestion found support in the strong FIR emission displayed by a significant fraction of early spirals, mostly belonging to interacting pairs.
Very little is available (see Paper I) concerning nuclear activity type in UZC-BGP; we have thus undertaken a spectroscopic survey of the sample. The survey is currently still ongoing (now 85% complete). In this paper we present results and analysis for 48 UZC-BGPs which constitute more than half of the whole sample and have an excellent morphological match with it.
The sample is presented in Sect. 2; in
Sect. 3 we show the results of our nuclear activity classification based on standard
diagnostic diagrams; in
Sect. 4 we analyze and compare the characteristics of galaxies
having different nuclear activity type; in Sect. 5 we look for
a possible link between nuclear activity and interaction strength. The conclusions
are drawn in Sect. 6. As in Paper I, a Hubble constant
of
km s-1 Mpc-1 is assumed throughout.
The sample contains 48 galaxy pairs, which represent more than half (54%) of UZC-BGP sample. The latter
is a volume-limited sample
of galaxy pairs
selected from the UZC catalog applying an adapted version of
the neighbour search algorithm of Focardi & Kelm (2002).
The environment of each UZC galaxy with
,
km s-1 and
;
has been explored in a surronding area characterized by two
projected dimensions (
kpc and
Mpc)
and a radial velocity ``distance'' (
km s-1).
Galaxies having only one bright neigbour (
)
within
and
and no other ones up to
(and within
)
were included in the UZC-BGP sample.
The adopted value for
(galaxy-galaxy projected distance) accounts for possible large haloes linked to bright
galaxies (Zaritsky et al. 1997; Bahcall et al. 1995).
The
value for
is
large enough to not induce an artificial
cut in the relative velocities of galaxies in pairs (within
)
and to prevent contamination by
galaxy groups/clusters (up to
). The value for
(large scale
isolation radius) was chosen to ensure the absence of luminous companions on group/cluster typical scales.
The lower limit in radial velocity was fixed to
reduce distance uncertainities due to peculiar motions and to prevent contamination
by the Virgo complex, while the upper limit was set to guarantee
sampling of the UZC luminosity function just below L* (Cuesta-Bolao & Serna 2003).
A limit in
was imposed to minimize the effects of galactic
absorption.
Table 1: The E+E pairs.
Unlike other galaxy pair samples selected from 3D catalogs (Alonso et al. 2004; Barton et al. 2000)
that are magnitude limited and contain pairs belonging to any kind of large scale environment,
UZC-BGP is particularly suited to investigate the mutual effects of two
bright close companions, isolated on the typical group/cluster scale. Minor companions,
which might have failed to enter either the UZC (
)
or UZC-BGP (
)
luminosity limit,
could be present in the local (within
)
or distant (within
)
environment but are not expected to play
a role comparable to that of the two massive galaxies in the pair.
UZC-BGP
galaxies are rather bright and, since luminosity relates to mass although not in an obvious way,
are rather massive
too.
(Further details on the UZC-BGP sample can be found in Paper I).
Following Karachentsev (1972), galaxy pairs can be classified on the basis of their morphology in E+E, S+S and E+S pairs. E+E pairs contain only early-type galaxies (E+S0s), S+S pairs only spirals and E+S pairs both types. The sample we present here is a fair representation of the whole UZC-BGP as it contains 6 E+E (12%), 23 S+S (48%) and 19 E+S (40%) pairs, which are remarkably similar to the ones of the whole UZC-BGP sample (13%, 48% and 39%).
Two dimensional long slit spectra have been acquired with BFOSC
(the Bologna Faint Object Spectrograph and Camera) at the 152 cm
telescope (of Bologna University) in Loiano (Italy). Spectral coverage is
4000-8500 Å with an average resolution of about 4 Å. The
slit was positioned over the nucleus of each galaxy and its width was
set either at 2'' or at 2.5'' (depending on seeing conditions), which
corresponds to the galaxy nuclear region (about 500 h-1 pc
at the average redshift of our sample). The data
reduction was performed with IRAF. After standard CCD (flat field
and bias) correction, we extracted the spectra, calibrated them in
wavelength, identified the emission lines and measured their EW.
Spectral extraction was limited to the 4-5 central pixels,
corresponding to
2''-2.5'' at the detector scale. We set the
continuum level in the close neighborhood of each emission line (on
both sides) and when the emission (H
and/or H
)
was affected by the presence of an underlaying strong absorption
line, we set the continuum at the bottom of the emission line, to
minimize the effect of the absorption.
Galaxies in E+E, S+S
and E+S pairs are listed respectively in Tables 1-3. In each
table we give the galaxy name, (Col. 1), the UZC-BGP
identifier (Col. 2), morphological classification (type) and
type code (T) (both from LEDA, Cols. 3 and 4), and emission lines
identified in each spectrum, if any (Col. 5). We have identified
only lines with
;
very few lines, however, are characterized by such a low signal, and
the vast majority has, on average,
.
Morphology is very well defined for 86% (83/96) of the galaxies, is less
defined for 13 galaxies and, in these last cases the morphological classification (Col. 3)
is followed by a question mark.
Table 2: The S+S pairs.
Table 3: The E+S pairs.
Inspection of Tables 1 to 3 provides evidence that emission
line galaxies are extremely rare in E+E, overabundant in S+S and rather
frequent (more than
half of the galaxies) in E+S pairs. There are 3 galaxies with emission
lines in the E+E pairs representing 25% of the total number of galaxies, 39 emission line galaxies in the
S+S (85%) and 26 in the E+S (68%) pairs. The different fractions are obviously related to the different
morphological content of the pairs and this is clearly illustrated in Fig. 1,
whose 4 panels
show the morphological distribution of galaxies in the whole sample
(upper left), E+E (upper right), S+S (lower left) and E+S (lower
right) pairs. Morphology is represented, on the x axis, by
the type code T (Col. 4 in each table), which is a numerical
parametrization of the morphological type, introduced by de Vaucouleurs & de Vaucouleurs (1964). According to this parametrization, early-type galaxies
(E and S0s) have T < 0 (E in general T < -3), while late spirals
(>Sbc) have, on average, .
The increase in emission line
galaxies with morphology is clearly evident in all pair samples
containing spiral galaxies (panels 1, 3 and 4 of Fig. 1) and
especially in panels 1 and 4 which show the more frequent
occurrence of emission features in spiral than in E-S0 galaxies.
The much higher occurrance of emission line galaxies among spirals than among early-type (E-S0s) galaxies is not unexpected as emission features occur more frequently in gas rich than in gas poor galaxies; however the two lower panels of Fig. 1 show that our sample is characterized by a morphological content which is never more advanced than T=6 (corresponding roughly to Sc galaxies). The frequency of emission lines among spirals attains the maximum value for morphologies more advanced than Sc as the the ratio of the current SFR (Star Formation Rate) to the average past one increases from about 0.01 in Sa to 1 in Sc-Irr galaxies (Kennicutt et al. 1994). The large number of emission lines occurring among early spirals in our sample might thus be partly induced by interaction.
The two lower panels of Fig. 1 show clearly that the fraction of emission galaxies is much lower in E+S than in S+S pairs simply because of the large number of early-type (E-S0s) galaxies in E+S pairs. In this last sample, 11 of the 12 galaxies with only absorption lines in their spectrum are early-type galaxies, implying that the fractions of early-type galaxies and spirals with emission lines are 42% (8/19) and 95% (18/19) respectively. If we compare the last fraction with the fraction (85%) of emission line galaxies in S+S we see that both E+S and S+S pairs have an equally high probability of hosting an emission line spiral.
Figure 2 shows the absolute magnitude (
)
distribution of ellipticals (T < -3, upper left), S0s (
,
upper right), and early (
,
lower left) and
late (
,
lower right) spirals. (MB has been derived
from B which is available in LEDA, Paturel et al. 2003, for 95/96
galaxies of our sample.)
In analogy with Fig. 1
the continuous distribution refers to the whole sample, the hatched
one to galaxies with emission lines. The lower panels of Fig. 2
reveal the extremely large fraction of emission line galaxies
in early and late spirals: 84% (37/44) and 95% (19/20), respectively.
Curiously, ellipticals (upper left) also appear often
(67%) in emission line galaxies, but the
statistics are too low
and do not allow us to draw definitive conclusions on this
point. S0 galaxies, instead, are abundant in our sample
(22/96) and appear to host a much more limited fraction (23%)
of emission line galaxies. From Fig. 2 we see that our sample is
numerically dominated by early spirals (47%), has an almost equal
content of late spirals (21%) and S0s (23%) and contains a
limited fraction (9%) of ellipticals. In terms of luminosity
(MB) S0s are characterized by more ``faint''
galaxies; about half of them (12/22, 55%) have
.
There are no ellipticals with
MB larger than that value, while early and late spirals
(with
)
represent,
respectively, 25% and 15% of each population.
Further
investigation is required to establish whether the population of low
luminosity S0s is typical of bright galaxy pairs and whether the lack of
emission features in these galaxies is related to their low luminosity.
Figure 3 shows the distribution of galaxy-galaxy projected distance
(,
upper panels) and velocity separation (
,
lower
panels) for E+E, S+S and E+S pairs. The continuous distribution
indicates the whole sample, the dashed distributions indicate pairs
having at least one member with an emission line spectrum (double dash)
and pairs in which both members have emission lines (single dash).
The fraction of pairs having both members ``active'' is clearly larger
in S+S (78%, 18/23) than in E+S (42%, 8/19). This difference is
caused by the early-type galaxy content of the E+S pairs. The
fractions become similar (91% and 95%) when considering
S+S and E+S pairs in which at least one member has an emission line
spectrum.
Previous work (Alonso et al. 2004; Barton et al. 2000)
has claimed an increase
in emission line galaxies in pairs with decreasing member projected distances.
In our sample the fraction of emission line galaxies in E+S and S+S pairs
is so high,
at all member distances, that we hardly see such an effect.
We stress however that UZC-BGP is a volume limited sample of bright
isolated galaxy pairs quite different from the magnitude limited samples
of close pairs belonging to any kind of environment, as in the
samples in which Barton et al. (2000) and Alonso et al. (2004)
observed a distance effect. The very large fraction of emission
line galaxies in our sample at all pair distances may
indicate that in isolated pairs of luminous (
)
galaxy interaction is at work and is effective up to 200 h-1 kpc. Both Barton et al. (2000) and Alonso et al. (2004)
find emission line enhancement on a much smaller scale (
30 h-1 kpc). Their result is likely to indicate that when
galaxy pairs are surrounded by companions of comparable luminosity,
galaxy-galaxy interaction becomes effective only at very small
distances. Our result indicates that fainter companions which
may be present in some UZC-BGP systems in the close (200 h-1) kpc and/or distant (1 h-1) Mpc surrounding area do
not play a role comparable to that of luminous member
galaxies.
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Figure 1: Relation between pair morphology and the presence of emission lines in the member galaxy spectra. The continuous histogram shows the morphological distribution of the whole galaxy pair sample ( upper left), and of E+E ( upper right), S+S ( lower left) and E+S ( lower right) pairs. Dashed histograms indicate the morphological distribution of galaxies with the emission line spectrum in each sample. |
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Figure 2: Absolute magnitude (MB) distribution of galaxies, of different morphological types, having or not having emission lines in their spectra. Continuous distribution refer to the whole samples, hatched one to galaxies with emission lines. |
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Figure 3:
Relation between the presence of
emission lines in the galaxy spectra and dynamical parameters
of the pairs. The upper panels show the galaxy-galaxy projected distance (![]() ![]() |
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The lower panels of Fig. 3 indicate a ``dynamical'' difference between pairs
containing only spirals (middle panel) and pairs containing either both
(left panel) or at least one (right panel) early-type galaxy, the
former being characterized by a narrower
distribution than the latter ones
(KS confidence level 93.9% and 99.9% respectively).
This difference (already outlined in Paper I) suggests that E+S and E+E pairs might
be embedded within large loose structures as
their broader
distribution indicates the presence of a larger potential
well. In this framework the emission spectrum of the 3
early-type galaxies belonging to the E+E pairs could arise from infalling of these
galaxies within a loose group as suggested from their large
value. We have checked
this hypothesis and found that neither UZC-BGP 51 nor UZC-BGP 77 are part of any
known galaxy group. However, inspection of available (LEDA) redshifts of galaxies in the
environment surrounding both pairs show that UZC-BGP 51 might be part of a loose galaxy group which
possibly could be infalling on the nearby (4 h-1 Mpc) Coma cluster. UZC-BGP 77A
(NGC 6018) might be infalling on a galaxy loose group having the same radial velocity as UZC-BGP 77B
(NGC 6021). More investigation is required to confirm our hypothesis.
To classify nuclear activity in our galaxy sample, we have made use of the
standard diagnostic diagrams (Veilleux 2002; Baldwin et al. 1981; Veilleux & Osterbrock 1987),
also known as the BPT diagrams,
which have proved to be an extremely
efficient method to distinguish the different types of activity encountered
in emission line galaxies (Gonçalves et al. 1999; Véron et al. 1997; Veilleux et al. 1995).
Moreover, being based on ratios of emission lines which are very close in wavelength they
are almost unaffected by reddening corrections (Veilleux & Osterbrock 1987).
The diagnostic diagrams relate [OIII]5007/H
to
[NII]6583/H
,
[SII]
(6717+6731)/H
and [OI]6300/H
.
Of the 68 galaxies with emission spectra (cf. Tables 1-3), 24 allowed us to create from one to three of the abovementioned
standard diagnostic diagrams. These galaxies are listed in Table 4,
in order of decreasing number of diagnostic diagrams, i.e. the first
14 galaxies have all line ratios measured, the subsequent 8 galaxies
only three line ratios and the remaining 2 only two. Table 4
reports for these galaxies, the UZC-BGP identifier (Col. 1), pair/galaxy
morphology (Col. 2, galaxy morphology is underlined in cases of
mixed pair morphology), line ratios and errors (Cols. 3-6). Each
line ratio has been obtained by averaging line ratios obtained
independently by each of us and the associated error represents the
standard deviation ().
The vast majority
(20/24) of galaxies listed in Table 4 belong to the S+S pair sample
and the remaining 4 are spirals, implying that there are
no early-type galaxies in our sample showing at least 4 emission lines.
Table 4: Spectral line ratios for standard diagnostic diagrams (DDs 1, 2 and 3).
The Log([OIII]5007/H)
versus
log([NII]6583/H
)
diagnostic diagram (hereafter DD1), for all
the galaxies listed in Table 4, is shown in Fig. 4. Different
symbols indicate different nuclear activity according to Veilleux &
Osterbrock (1987) empirical classification (hereafter VO87)
which separates high from low excitation galaxies (Seyfert 2 from LINERs
and HII galaxies from SBs) based on a [OIII]5007/H
value of 3 and LINER from SBs based on a
[NII]6583/H
value of 0.6.
According to VO87, our sample contains one Seyfert 2 galaxy
(triangle), two LINERs (squares) and 21 SBs (circles). The Sy 2
(UZC-BGP 83A) and the LINERs (UZC-BGP 28A and 69B) are identified in Fig. 4.
On the same diagram we show two curves, the solid one to the left
is the Kauffman et al. (2003) sequence (hereafter Kauff03), the dotted
one to the right is the Kewley et al.
(2001) sequence (hereafter Kew01). Both sequences are supposed to
separate SB from AGNs. Kauff03
is an empirical sequence that has been derived from
a very large sample (22 000) of SDSS emission line galaxies,
while Kew01
is a theoretical sequence derived using a wide set of models
accounting for photoionization and
stellar population synthesis.
Figure 4 shows that there are 8 galaxies
falling between the Kauff03 and Kew01
sequences.
These galaxies, ordered by decreasing value of [OIII]5007/H
,
are
UZC-BGP 81A, 66A, 24A, 5A, 44A, 69B (a LINER according to VO87), 2A and 81B and are
indicated in Fig. 4. Two of these galaxies (UZC-BGP 81A and 66A) may fall just below
the Kauff03 sequence taking into account the error associated with the [OIII]5007/H
measurement,
while another one (UZC-BGP 81B) could move
from just above the sequence to the sequence itself.
One further galaxy (UZC-BGP 74A) is identified in Fig. 4 as,
although it lies, in this diagram, well below the Kauff03 sequence, it
occupies the LINER region
of Fig. 6.
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Figure 4:
Log ([OIII]5007/H![]() ![]() |
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Figure 5:
Log ([OIII]5007/H![]() ![]() |
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Figure 5 shows that, according to the Kew01 and Kew06 classification, only one
galaxy (UZC-BGP 28A) would be classified as a LINER. All the others would be
SB, although UZC-BGP 83A (Sy 2 following the VO87 scheme) lies just below the
Kew01 sequence and would move exactly on to it if one lets
[OIII]5007/H
attain its maximum possible value (within the error).
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Figure 6:
Log ([OIII]5007/H![]() ![]() |
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Figure 6 shows the log ([OIII]5007/H)
versus
log ([OI]6300/H
)
diagram (hereafter DD3) for the
14 galaxies in Table 4 with those measured line ratios.
Symbols indicate different nuclear activity type according to the VO87 scheme that
separates Sy 2 from SB and LINERs based on a value of [OIII]5007/H
of 3 and
requires a value of
[OI]6300/H
for Sy 2 and
0.17 for LINERs.
Here the dotted curve and line correspond to Kew01 and Kew06 sequences
separating SB from AGNs and Sy 2 from LINERs respectively.
We indicate, in this plot, the galaxies lying above the Kew01 curve and 3 (over 8) galaxies lying in the Kauff03 Kew01 region of DD1 (Fig. 4).
Two galaxies (UZC-BGP 28A and 74A) occupy the Kew01-Kew06 LINER region,
one (UZC-BGP 83A) the Sy 2 region. This classification is confirmed by VO87.
One galaxy in Fig. 6 (UZC-BGP 74B) could move from the SB locus to the Kew01 SB/AGN separation
curve when taking into account the error associated with the [OI]6300/H
measurement. This galaxy is very close to UZC-BGP 24A (its right),
but we have not indicated it in Fig. 6, as it occupies the SB region both in DD1 and DD2 (Figs. 4 and 5).
Table 5: Spectral line ratios for DD4.
The spectral analysis of the 24 emission line galaxies listed in Table 4
allow us to unambiguously classify 14 of them, as for these galaxies
all the different classification schemes (V087, Kauff03 and Kew01-06)
give consistent results on the 3 diagnostic
diagrams. Of the remaining 10 galaxies 8 lie above the Kauff03 sequence and
below the Kew01 in DD1. One of these 8 (UZC-BGP 44A) has only DD1 available,
4 also have DD2, and 3 have both DD2 and DD3 available. The VO87 and Kew01 classification
schemes agree on SB activity in the other diagnostic diagrams for 6 of the 7 galaxies having
either both DD2 and DD3 or only DD2 available; only UZC-BGP 69B is classified
(in DD2) as a LINER in the VO87 scheme and as a SB in the Kew01 one.
The 2 other ``difficult'' cases are UZC-BGP 83A and 74A. The first one is a Sy 2 in
both DD1 and DD3, for all classification schemes, but in DD2 is a SB,
according to Kew01 (although it lies very
close to the SB/AGN border and would lie exactly on it if [OIII]5007/H
attains its
maximum permitted value within the error), and a Sy 2 according to VO87. More ``difficult'' is the case of
UZC-BGP 74A which is
a LINER in DD3 (for both Kew01 and VO87) and a SB in DD1 and DD2
for all classification schemes.
Galaxies displaying different kinds of nuclear activity in different diagnostic diagrams should be classified as composite objects (Kewley et al. 2006). However, in order to avoid a double classification (e.g. SB/AGN, Sy2/SB, LINER/SB) we have assigned to each galaxy the ``most frequent'' classification according to the different schemes applied to the 3 diagnostic diagrams. However, we record each classification scheme in each diagnostic diagram in Table 6, which summarizes the results of our spectral analysis.
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Figure 7:
Log EW([NII]6583) versus log ([NII]6583/H![]() |
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A large fraction of the emission line galaxies (31/68) have well defined
H
and [NII] lines but do not show [OIII] and/or
H
features and thus does not allow us to use the standard
diagnostic diagrams. For these galaxies, listed in Table 5, the
activity type can be classified (Coziol et al. 1998) comparing the
EW of the [NII]6583 feature with the ratio of [NII]6583 to
H
.
These values are listed in Table 5, together with
their errors, which, similarly to Table 4, represent
the average of 3 measures obtained independently by each of us and
the associated
.
The underlined morphology in Col. 2 indicates, as in
Table 4, the ``rough'' galaxy morphology when the galaxy pair is of mixed (E+S) type.
Following Coziol et al. (1998) we have classified the 31 galaxies listed in Table 5
as SB if they have
/H
and
;
AGN and LLAGN if they have
/H
and log EW([NII]
or <0.5.
The lines which separate the loci of SB, AGN and LLAGN
are represented in Fig. 7 which shows the log EW([NII]6583) versus log ([NII]6583/H
)
diagram (hereafter DD4)
for the 31 galaxies listed in Table 5 (filled circles). Among these galaxies
we have identified the seven
showing the largest value of [NII]6583/H
.
This
behaviour is due to the presence of a strong H
feature
in absorption depressing the emission feature and resulting in an
enhanced [NII]6583/H
ratio. From Fig. 7 we see that only one galaxy (UZC-BGP 36A) could have its classification
changed (from AGN to LLAGN) when taking into account the error associated with EW([NII]6583)
The classification scheme adopted by Coziol et al. (1998) is empirical and might, thus, be questioned.
For this reason we also show, on the same plot (Fig. 7), the 24 galaxies (open symbols) listed in Table 4 that we have
classified with one or more standard diagnostic diagrams. The different symbols
indicate (as in Figs. 4-6) different nuclear activity.
From Fig. 7 we see that for low values of EW([NII]6583) (log EW([NII]
)
the Coziol classification scheme
holds, since all galaxies classified as SB (open circles) occupy the SB region of the diagram, whereas
for larger values of EW([NII]6583) there are SBs in the AGN region and
AGN in the SB ones
. The agreement between Coziol and
the standard classification, occurring at low values of EW([NII]6583)
where SBs from Tables 4 and 5 overlap, increases our confidence in this classification scheme.
Of the remaining 13 galaxies with emission lines (cf. Tables 1-3), 10 show only the [NII]6583 emission feature and thus, according
to Coziol et al. (1998), we have classified them as LLAGN candidates,
while 3 show only H
in emission and have not been
classified.
Table 6: Nuclear activity classification.
Table 6 summarizes the nuclear activity classification for 65/68 emission line galaxies of our sample. The classification has been
performed on the basis of one or more diagnostic diagrams for 55 galaxies and on the presence of the unique emission feature
[NII]6583, for 10 of them, that following Coziol et al. (1998) we have classified as LLAGN candidates. Three galaxies
(UZC-BGP 17A, 80A and 82B) show only H
in emission and thus
could not be classified and included in Table 6. As well as the UZC-BGP
identifier (Col. 1) and pair/galaxy morphology (Col. 2, as in
Tables 4 and 5, galaxy morphology is underlined in E+S pairs), Table 6
lists the classification derived from DD1, DD2 and DD3
(Cols. 3-5), according to VO87 (first subcolumn), Kew01
(second subcolumn) and Kauff03 (third subcolumn, only for DD1).
In Col. 6 the classification into AGN, SB or LLAGN, according to
DD4, is given. Column 7 reports the classification that we have
adopted for each galaxy (LL stands for LLAGN candidate, based on
the unique presence of the [NII]6583 feature).
Finally,
Col. 8 reports the activity type classification available for 11 galaxies from NED.
Comparison of Col. 7 with Col. 8 shows a very good agreement between our classification
and the available one. The agreement is very good
also for the cases in which we have adopted the ``majority'' classification
criterion (UZC-BGP 2A, 5A and 83A) and when the classification has been based only on H
and [NII]6583 (UZC-BGP 18A and 37A). Only for UZC-BGP 79A (NGC 6251) could we not confirm the Sy 2
nature as
we did not detect H
(cf. Table 3) at our imposed
threshold limit for emission lines (
).
From Table 6 we see that among the 65 galaxies with classified nuclear activity, 29 are SB, 18 AGN (including 2 LINERs and 1 Sy 2), 8 LLAGN and 10 LLAGN candidates. SB is the most common kind of nuclear activity encountered in our sample (30% of galaxies display it), while AGN is limited to a smaller fraction (19%) of galaxies. SBs are more commonly found in S+S pairs than AGNs. There are 23/29 SB galaxies and 10/18 AGNs in S+S pairs (these last 10 include the 2 LINERs and the Sy 2), which implies a fraction of SB and AGN per spiral galaxy in S+S pairs of 50% and 22% respectively. The remaining 6 SBs are all hosted in the spiral member of E+S pairs, while the 8 AGNs are equally divided between spirals and early-type galaxies, one (UZC-BGP 77A) of these last being hosted in an E+E pair. As a whole the fractions of SB and AGNs per spiral galaxy are 45% and 22% respectively. LLAGNs, instead, are exclusively found in E+S pairs and in half (4/8) of the cases this kind of activity is displayed by the early-type galaxy member of the pair. The distribution of LLAGN candidates (LL in Col. 7 of Table 6) appears somewhat different from the LLAGN one; there are 3/10 LL in S+S pairs and of the remaining 7 LL only 3 are early-type galaxies. It is difficult to state whether the difference between LLAGNs and LLAGN candidates confirms previous findings (Ho et al. 1994) concerning the heterogenous nature of LLAGNs, as our classification of LLAGN candidates has been based on the presence of the [NII]6583 feature alone.
![]() |
Figure 8: Luminosity (MB) and morphology (T) distribution of absorption line galaxies, SBs, AGNs, LLAGNs and LLAGN candidates. The dashed distributions in the right panels indicate morphological distribution of the brightest 20% galaxies in each sample. In the AGN panels the positions are indicated of the 2 LINERs (squares) and the Sy 2 (triangle) which have not been included in the histograms. |
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Figure 8 shows the luminosity (MB) and morphology (T)
distribution of absorption line galaxies, SBs, AGNs, LLAGNs
and LLAGN candidates.
MB has been derived from BT which is available in LEDA for all but one LLAGN galaxy (UZC-BGP 10B).
The dashed histogram in the morphological distribution (right panels) refers to the 20%
brightest galaxies in each sample. In AGN panels magnitudes and types are also indicated of
the two LINERs (squares) and the Sy 2 (triangle) which have not been included in the histograms.
Examining the left panels of Fig. 8 we see that galaxies displaying the largest B luminosity are LLAGNs,
most (71%) of them have
,
a fraction to be compared with 55% of
LLAGN candidates, 44% of AGNs (LINERs and Sy 2 included), 35% of SBs and 18% of absorption line galaxies.
These last ones are of particularly low B luminosity, quite unsual for passive galaxies which are, in general,
much more luminous star forming ones (Kelm et al. 2005). Curiously, in our sample,
absorption line galaxies and SBs have a rather similar luminosity distribution which derives from an almost
``opposite'' morphological content.
Further investigation is needed to understand
if and how this population of low luminous early-type passive galaxies is connected to the pair environment or if it is a
more general
characteristics of low density large scale environments.
The right panels of Fig. 8 show that absorption line galaxies
are dominated by S0s (
)
and that very few of these galaxies display nuclear activity;
ellipticals
(T < -3), instead, show a much higher rate of nuclear activity and in some cases (AGNs and LLAGNs) are even among
the 20% brightest
galaxies in each sample. Thus, low B luminosity coupled with the absence of emission features
seems to characterize more S0s than ellipticals, which, however, are much rarer than S0s in our sample.
The morphological distribution of SBs is rather flat as is the distribution of the brightest 6
among them. The first luminosity ranked (
)
SB is a late spiral (UZC-BGP 9B)
and the second one (
)
UZC-BGP 2A, is an early spiral.
The median type of the SB morphological distribution is 2.95 (corresponding to Sb) while Ho et al. (1997)
find a median value of 5 (corresponding to Sc) for their sample of galaxies with nuclear SB activity.
Our sample is surely early spiral dominated but we could arrive at a larger median value of T if we had
more late spirals among the SBs. In our sample the fractions of early and late spiral
SBs are similar (19/44 and 9/20), while Ho et al. (1997) report fractions of 38% and 82%.
However, if we separate 4-line SBs
(i.e. SB classified on the basis of at least 4 emission lines) from 2-line SBs (classified
based on H
and [NII]6583 features) we find both a B luminosity increase
(63% of these galaxies has
)
and a more advanced morphological type (median T = 3.95).
The morphological distribution of AGNs is rather advanced, the median value is 2.55 (Sab)
compared with 1 (
Sa) of Ho et al. (1997). AGNs are spread all over the morphological
range and the 3 brightest AGNs reflect this behaviour too. The brightest
(
)
AGN is UZC-BGP 79A, an elliptical galaxy
(NGC 6251) classified as Sy 2
(NED) showing, in our spectrum, H
emission well below our adopted S/N threshold
(see also Sect. 3). The other two brightest
galaxies both have
and advanced morphological type. The LINERs and the Sy 2, whose positions are
represented
with two squares and a triangle, display a modest luminosity. The morphological type of
the LINERs is quite advanced too; for comparison Ho et al. (1997) give a median value of 1.
LLAGNs and LLAGN candidates are distributed over the whole morphological range, but their T morphological and luminosity distributions are somewhat different, LLAGN candidates displaying more faint galaxies and spirals.
![]() |
Figure 9:
H![]() ![]() |
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The EW of the H
emission line of galaxies classified as SB (upper panels),
AGN (lower left) and LLAGNs (lower right) is shown in Fig. 9. The upper left and right panels refer
respectively to 4-line SBs and 2-line SBs. The squares in the AGN panel indicate the position
that would be occupied by the two LINERs, not included in the histogram. The position of the Sy 2
is not marked as it would far to the right in this plot. This galaxy has the largest (117.43 Å)
H
EW of the whole sample.
The median values of the distribution of H
EW of 4-line
SBs, 2-line SBs, AGNs and LLAGNs are respectively 45.17 Å,
16.48 Å, 8.77 Å (9.67 Å including the Sy 2 and the
LINERs) and 1.33 Å. For comparison Miller et al. (2003)
report, for a large sample of SDSS galaxies having a luminosity
similar to ours but belonging to any environment, median
values of the H
EW of 26 Å, 14 Å and 3 Å for 4-line SBs, 2-line SBs and AGNs respectively. Thus, while
the 2-line SBs display similar values of the median H
EW, both 4-line SBs and 2-line AGNs show larger values in ours
than in the Miller et al. (2003) sample. However, the criterion
adopted by Miller et al. (2003) to classify 2-line AGNs is more
conservative than the one adopted by us, as they required log
([NII]/H
.
Application of their criterion to
our data causes exclusion of 6 2-line AGNs (belonging, obviously,
to the large value tail of H
EW) and reduces the
median value of 2-line AGNs, in our sample, to 4.94 a value
which is similar to but still exceeds (1.6 times) the one reported
by Miller et al. (2003). The excess, however, disappears
if we include LLAGNs in our AGN sample, as the median value of
H
EW drops to 2.34 Å, which is below the value
(3 Å) reported by Miller et al. (2003).
The inclusion of LLAGNs among AGNs is justified since Miller et al. (2003) state that
a significant population of their 2-line AGNs are LLAGNs, although they
do not say how many LLAGNs enter their AGN sample. Since LLAGNs are characterized by lower
values of H
EW than AGNs, the H
EW of an AGN sample also including
LLAGNs will reflect the relative amount of the two populations
entering the sample. For this reason we do not expect exact coincidence between
the value that we derive in our sample and the one reported by Miller et al. (2003)
and we consider the agreement between the two values to be quite good.
Thus only 4-line SB in our sample display a median H
EW
that is significantly larger than the one reported by Miller et al. (2003)
and which cannot be attributed to instrumental effects as we find no correlation between
the measured H
EW and the S/N of the spectra.
In star forming galaxies the increase of H
EW relates to the star formation rate
(SFR, Kennicutt et al. 1987; Kennicutt & Kent 1983).
Thus the larger values displayed by 4-line SB galaxies in our
sample
compared to the ones of Miller et al. (2003) supports the interaction - SB scenario.
In this framework Barton et al. (2000) found a significant increase of H
EW with decreasing
galaxy-galaxy projected distance for SB galaxies in a magnitude limited sample of galaxy pairs. The
correlation holds over
a limited projected distance range (from 5 h-1 to 40 h-1 kpc) over which the
H
EW decreases from about 150 Å to 50 Å.
Figure 9 shows that there are no SBs in our sample with an H
EW larger than 85 Å; that value
is reached only by one galaxy (UZC-BGP 83B) whose projected distance from its companion (the only Sy 2 that we
detected in our sample) is 19 h-1 kpc, which is small but not the smallest in the sample.
The two SBs showing the smallest projected distance (3 h-1 kpc) in our sample
belong to the same pair (UZC-BGP 74) and show
an H
EW of 58.94 and 57.30 Å respectively.
Half (15/29) of the SBs in our sample display a value of
H
Å, which is supposed to separate normal from intense SB activity (Kennicutt & Kent 1983).
None of these intense-SB galaxies is found in pairs with a projected galaxy
separation (
)
larger than 160 h-1and 3 of them show
.
There are no other SBs with
,
while for
only 2 SBs are found (with an average value of H
EW of 21.89 Å).
We cannot confirm the anticorrelation between H
EW and
galaxy-galaxy projected distance found by Barton et al. (2000), which is not
surprising since our sample is quite different from theirs and we
have few (9) galaxy pairs characterized by small (
50 h-1 kpc) galaxy-galaxy separation. The lack of a clear
anticorrelation in our sample might indicate that for bright
isolated galaxies
in pairs, interaction is at work and is effective up to 160 h-1 kpc.
![]() |
Figure 10: MH distribution of galaxies with absorption spectra ( upper left) and classified as SB ( upper right), AGN ( lower left) and LLAGN ( lower right). The continuous distribution in the upper right panel represents the whole SB population, the dashed histogram 2-line SBs. As in Fig. 8 we have marked in the AGN panel ( lower left) the position of the 2 LINERs (squares) and the Sy 2 (triangle) which have not been included in the histogram. In the lower right panel the continuous and dashed line refer respectively to LLAGNs and LLAGN candidates. |
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Table 7: The mass of galaxies with different nuclear activity type.
Figure 10 shows the MH distribution of galaxies in our sample showing absorption lines (upper left) and classified as SB (upper right), AGN (lower left) and LLAGN/LLAGN candidates (lower right, continuous/dashed histogram). The continuous distribution in the upper right panel refers to the whole SB population, the dashed histogram to 2-line SBs. MH has been derived from 2MASS data available for all but 6 galaxies in our sample, which are 3 SBs (UZC-BGP 29B 49A and 74B), 2 absorption line galaxies (UZC-BGP 49B and 58B) and 1 LLAGN (UZC-BGP 26B). At variance with Fig. 8 in which galaxies display rather similarly large B luminosity distributions, Fig. 10 shows that only SBs have a broad MHdistribution extending over 4 mag; in all the other cases galaxies are concentrated in a 2 mag range. The only exception is AGNs whose distribution, however, appear broad due to the presence of only two galaxies: the faintest and the brightest, in H, of the whole sample. The faintest (
The luminosity in H relates to the galaxy mass within the optical radius of disc galaxies (
),
a quantity that can be derived through the relationship log (
/
(Gavazzi et al. 1996).
Adopting
(Allen 1973) we have calculated
for all the disc galaxies (i.e. ellipticals
excluded)
in the sample having H magnitude available.
The results are summarized in Table 7 where we indicate for each
activity type (Col. 1), the total number of galaxies (
)
(Col. 2), the number of galaxies (NH) having H magnitude
available (Col. 3) and the number of galaxies (
)
for which we have derived the galaxy mass (
), (Col. 4).
In Col. 5 we give the minimum and maximum value of the mass for
each distribution (
)
and in Col. 5 the median
value of each distribution (med (
)). With the term none
(first row of Col. 1) we indicate galaxies with absorption lines
only in their spectrum. Since the nature of S0 galaxies is somewhat
questioned and since among them there might be some misclassified
ellipticals we have also computed
for spiral galaxies
only. The results, only if different from values reported in
Cols. 3-5, are shown in Cols. 6-8 in which we
indicate the number of spiral galaxies (
), minimum and
maximum value
of the mass (
)
and median value of the mass distribution (med
(
)).
The exclusion of S0s does not significantly change the results as the
mass ranges remain the same in all but the sample of absorption
line galaxies, and median values display, consequently, modest
changes (only for LLAGNs and LLAGN candidates).
Absorption line galaxies, LLAGNs and LLAGN candidates display higher values of the mass, and SB the lowest, as this is the
only population with a median value of the mass distribution below 10
.
However, if we
separate 2-line SBs from 4-line SBs the median value of the first ones increases to
and the mass range narrows (between
and
), while the second ones
display a mass range between
and
and a median value of
.
AGNs appear characterized by a wide mass distribution too, which is induced by the presence of an extremely
low mass galaxy (UZC-BGP 24B, see also Fig. 10 and relative comments). Exclusion of this galaxy from the AGN
sample would raise the minimum mass to
(still below the minimum for absorption line
galaxies, LLAGNs and LLAGN candidates) and the median value to
.
Kauffmann et al. (2003) have shown that AGNs reside only in galaxies with masses
,
a value that should be scaled to
to account for the different values of H0 adopted by us
and by them. Table 7 shows that, due to the imposed criterion on luminosity (see also Sect. 2),
all galaxies
in our sample
have masses above the Kauffmann et al. (2003) value and we are thus unable to confirm
their finding.
![]() |
Figure 11: Color magnitude diagram (B-H vs. MH) for galaxies with absorption spectra ( upper left) and classified as SBs ( upper right), AGNs ( lower left), LLAGNs and LLAGN candidates ( lower right). Filled and empty circles and triangles indicate, in each panel, ellipticals, S0s, early and late spirals. In the SB panel ( upper right) the previously defined symbols indicate the morphological classification of 4-line SBs, while filled and empty squares indicate early and late spirals of 2-line SBs. In the AGN panel ( lower left) filled and empty squares indicate the 3 galaxies classified respectively as LINERs and Sy 2. In the LLAGNs/LLAGN candidates panel ( lower right) the standard symbols (filled/open circles/triangles) distinguish LLAGN morphological types while we have used filled/open squares to indicate LLAGN candidate ellipticals and S0s and filled/empty stars to indicate early/late spirals. |
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Figure 11 illustrates the Color Magnitude (CM) diagram (B-H vs. MH) for galaxies with absorption spectra (upper left) and classified as SB (upper right), AGN (lower left), LLAGN and LLAGN candidates (lower right). We distinguish, for each activity class, different morphological types. Filled and empty circles indicate ellipticals and S0s, while filled and empty triangles stand for early and late spirals. This holds for the absorption line galaxies, 4-line SBs (although this class of objects does not contain early-type galaxies), AGNs and LLAGNs. Concerning 2-line SBs (upper right panel), early and late spirals are indicated as filled and empty squares, while for LLAGN candidates (lower right panel) we have adopted filled and empty squares to indicate E and S0s and filled and empty stars to indicate early and late spirals. In the AGN panel (lower left) empty and filled squares indicate the Sy 2 and LINER location (all three are early spirals).
Absorption line galaxies (upper left panel of Fig. 11) occupy a well
defined ``red-bright'' region in the CM diagram, with the exception
of UZC-BGP 8A (NGC 800) which is the only late type spiral with an
absorption spectrum in our sample. The absence of a trend for
absorption line galaxies in the CM diagram must be attributed to the
large group of S0s (empty circles) that dominates this population.
Early spirals with an absorption spectrum (filled triangles)
follow the expected trend and become more H luminous as they become
redder (B-H increasing). SB galaxies (upper right panel) follow a
much better defined sequence which holds over a wide range of
luminosities. The high proportion of filled vs. empty symbols
indicates the dominance of early spirals among this class of objects.
The faint luminosity region is mostly occupied by a population
of early spirals which, besides being quite faint (
), are also exceptionally
``blue'' (
).
As expected (cf. Fig. 9), early and late spirals classified as 2-line SBs (filled and empty squares) occupy the high H luminosity
``red'' region of the diagram. They too follow the general SB trend. The AGN panel shows the absence of a
trend and all but 2 (the brightest and the faintest) AGNs are concentrated in a narrow
region which resembles the absorption line galaxy ``cloud'' but is characterized by a bluer color
and a somewhat fainter H luminosity. The AGN ``cloud'' is made up of two different regions
characterized by similar H luminosity and different color. The separation of the two AGN regions
occurs at
,
which is also the value below which almost no absorption line galaxies are found
and where most SB galaxies reside. Also LLAGN and all but one LLAGN candidates
occupy a well defined region in the CM diagram which is brighter than the ones occupied by absorption line
galaxies and AGNs and has a color in between the two.
Figure 11 indicates that absorption line galaxies, SBs, AGNs and LLAGNs
occupy rather distinct regions in this CM diagram so that it would possible to
distinguish SB from absorption line galaxies on the basis of their location in this diagram.
The AGN location is in between the previous two, but is almost completely separated from LLAGN and LLAGN candidates.
This is an interesting finding that should be verified on galaxy samples in different environments.
There are cases in which galaxy interaction produces ``visible'' effects such as morphological distortions, bridges and tidal tails. However, the detection of those features depends on the sensitivity of the instrument to low surface brightness structures and is thus strongly affected by seeing, depth and redshift. Moreover morphological distortions are short lived phenomena (100 Myr) and tidal tails appear only in prograde disk encounters (Toomre & Toomre 1972). Thus a selection of systems based on the presence of ''visible'' signs of interaction would lead to a fraction of interacting pairs being missed. However, pairs showing interaction can be used to test the pair sample as a whole, as differences that might be present in the content and type of nuclear activity between these systems and the whole pair sample could bring into question the interaction status of galaxy pairs.
Careful inspection of DSS images of all pairs in our sample allowed
us to identify 9 pairs in which interaction is detected
between the members. These pairs are listed in Table 8, where we
give, for each of them, identifier (Col. 1), pair/galaxy
morphology (Col. 2; as in Tables 4-6 galaxy morphology of
the active member is underlined in E+S pairs), nuclear
activity type (Col. 3; - indicates absence of nuclear activity)
and H
EW
(Col. 4; only if the galaxy is active).
Table 8: UZC-BGPs showing interaction between members.
Table 9: UZC-BGP galaxies interacting with fainter companions.
Among the 48 galaxy pairs of our sample only 9 (listed in Table 8) are characterized by
signs of interaction between
their members. Table 8 shows that this happens more
frequently in S+S (6/23) than in E+S (3/19) pairs and that in these
last cases interaction is never able to induce emission activity in the early
type member of the pair. On the other hand interaction does
not appear to be able to induce nuclear activity in 2 galaxies
belonging to the S+S pairs either. All kinds of activities are found in
pairs listed in Table 8; visible interaction thus does not appear to
be responsible for activation of a particular kind of nuclear
activity. In Table 8 there are 7 SB galaxies, 3 AGNs (Sy 2 included), 1 LLAGN, 2 LLAGN candidates
and 5 galaxies with absorption spectra. This implies fractions of activity type per galaxy of 39%, 17%,
6%, 11% and 28% which are remarkably similar to the ones
for the whole sample (30%, 19%, 8%, 11% and 30%). Five of the SBs in Table 8
are 4-line SBs, two (UZC-BGP 8A and 49A) are 2-line SBs. Thus also the fraction of 2 to 4-line SBs
in these pairs agrees remarkably well with the fraction in the whole sample (8/21). From Col. 5
of Table 8 we can derive the median value of H
EW of 4-line and 2-line SB respectively
58.94 Å and 16.49 Å, again very similar to the ones derived for the whole sample (cf. Sect. 4).
The similarity in terms of amount, type and characteristics of the nuclear activity between
these 9 pairs and the whole sample
supports the hypothesis that galaxy-galaxy interaction between bright galaxies
in isolated pairs is at work and effective.
Since UZC-BGP is a volume-limited sample, interaction may
even occur between one pair member and a faint companion that has
gone undetected either because of the UZC catalog magnitude limit (
)
or the UZC-BGP luminosity limit (
). This happens for 9 galaxies, belonging to 8 distinct
pairs, which we list in Table 9. For each galaxy we give
identifier
(Col. 1), pair/galaxy morphology (Col. 2; as in Table 8 galaxy morphology is underlined in case
of E+S), activity type (Col. 3; - means no activity), H
EW, identificator
of the companion (Col. 5).
Among these faint companions only two (NGC 1588 and NGC 2751)
interacting respectively with UZC-BGP 16A and 20B have failed
the luminosity limit of UZC-BGP, in all other cases companions were too faint
to be included in the UZC catalog.
Table 10: UZC-BGPs with absorption line spectra in both members.
At variance with Table 8, Table 9 shows that most (7/9) of the galaxies interacting with fainter companions belong to E+S pairs. Five galaxies in Table 9 are early-type, two of them (UZC-BGP 5B and 16A) display no activity and the remaining three (UZC-BGP 10A, 20B and 26B) show LLAGN activity. This last one is the most frequent kind of activity of galaxies in Table 9. The fraction of LLAGNs among the galaxies of Table 9 is 44% (to be compared with 8% in the whole sample). The excess of LLAGNs could indicate minor galaxy interaction (Woods & Geller 2007) as a driving mechanism for this kind of activity. Interestingly, the interacting LLAGNs of Table 9 are all found in E+S pairs which we expected (cf. Fig. 3 and discussion) to be the bright core of a looser structure. The presence of a fainter close companion confirms both our expectation and previous finding (Coziol et al. 1998, 2000; Martinez et al. 2006) that LLAGN is the most common kind of activity in Compact Groups. Further investigation is needed since no detailed analysis concerning the link between LLAGN activity and interaction has been carried out so far.
Finally, if interaction plays a major role in activating nuclear
activity, passive galaxies in galaxy pairs should not display evident
interaction. There are 7 pairs in our sample with both members
passive. They are listed in Table 10 where we give, the pair
identifier (Col. 1), morphology (Col. 2) and, in Col. 3,
we indicate if interaction occurs between pair members or with a
faint companion. Only one galaxy (UZC-BGP 23A) interacts with a
faint companion (NGC 2988, which was not included in the UZC catalog).
The sample is dominated by E+E pairs (4/7), 3 of which show
interaction patterns, the remaining 2 S+S and E+S pairs do not show
interaction at all. There is interaction and no activity
only in the 3 E+E pairs, which is somewhat encouraging for the
interaction-activity scenario as galaxy interaction will
produce larger effects in gas rich than in gas poor galaxies,
while the 2 S+S pairs are characterized by large values (159 and
183 h-1 kpc) of
(cf. Fig. 3, upper middle panel) in
our sample. This confirms our previous finding on H
EW
and suggest that in the UZC-BGP sample interaction is at work and
effective up to 160 h-1 kpc.
To investigate the role of galaxy interaction on nuclear activity we performed a detailed spectroscopical analysis on 48 galaxy pairs which represent more than half of the whole UZC-BGP sample and have an excellent morphological match with it.
We found an extremely large fraction of emission line galaxies in our sample, particularly among early (84%) and late (95%) spirals.
Classification and analysis of spectral activity, performed by means of standard diagnostic diagrams,
allowed us to show that SB is the most frequent (30% of galaxies) kind of activity in our sample.
It occurs exclusively in spiral galaxies with a frequency of the SB phenomenon
among spirals of 45%. The blue luminosity distribution of these SB is not particularly
high as 67% have
.
While SB are preferentially found in S+S pairs, AGN are almost equally found in S+S and in E+S pairs
although in most cases (82%) this kind of activity is displayed by a spiral galaxy. AGN
in our sample show rather advanced
morphological distribution characterized by a high blue luminosity. The fraction of AGNs
in late spirals is 35% and late spirals hosting AGNs have an average
.
SBs display enhanced H
EW, an effect which relates to star formation and
might thus be related to pair environment. Star formation is intense in half of the SB
galaxies in our sample. Intense-SBs have galaxy-galaxy separations up to 160 h-1 kpc
implying that interaction may be effective in isolated pairs of bright galaxies up to that distance.
Absorption line galaxies, SBs, AGNs and LLAGNs (candidates included) occupy rather distinct locations in the B-H vs. MH diagram, a characteristics which reflects the different distribution in B and H luminosity of each sample. Galaxy masses, estimated using the H luminosity, are high for absorption line galaxies and LLAGNs (as a whole), low for SBs and ``intermediate'' for AGNs
All LLAGNs reside in E+S and are equally distributed between early type galaxies and spirals. We have shown that half of them are hosted in galaxies displaying signs of interaction with fainter companions, which suggests that minor interaction might be a driving mechanism in some fraction of LLAGNs. LLAGN has been claimed to be a heterogenous class of objects: our previous finding concerning only half of the whole LLAGN population, coupled with the quite different behaviour in terms of blue luminosity and morphological content of LLAGN candidates, appears to confirm that claim.
Acknowledgements
This work was supported by MIUR. P.F. acknowledges financial support from the contract ASI-INAF I/023/05/0. S.M. acknowledges a fellowship by INAF-OAB. This research has made use of the NASA/IPAC Extragalactic Database (NED) and of the Hyperleda Database (http://leda.univ-lyon1.fr/). We thank the anonymous referee whose comments and criticism greatly improved the paper.