11institutetext: INAF - Osservatorio Astrofisico di Torino, Strada
Osservatorio 20, I-10025 Pino Torinese, Italy 22institutetext: INAF -
Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti
93/3, 40129 Bologna, Italy 33institutetext: Dipartimento di Fisica e
Astronomia, Università di Bologna, Via P. Gobetti 93/2

# The LOFAR view of massive early-type galaxies:
Transition from radio AGN to host emission.

A. Capetti 11 M. Brienza 2233

We extend the study of the radio emission in early-type galaxies (ETGs) in the
nearby Universe (recession velocity $<7,500$ $\rm{\,km\,s}^{-1}$) as seen by
the 150 MHz Low-Frequency ARray (LOFAR) observations and extend the sample
from giant ETGs to massive ($\sim 6\times 10^{10}-3\times 10^{11}{\rm
M}_{\odot}$) ETGs (mETGS) with $-25<M_{K}<-23.5$. Images from the second data
release of the LOFAR Two-metre Sky Survey were available for 432 mETGs, 48% of
which are detected above a typical luminosity of $\sim 3\times 10^{20}\>{\rm
W}\,{\rm Hz}^{-1}$. Most (85%) of the detected sources are compact, with sizes
$\lesssim 4$ kpc. The radio emission of 31 mETGs is extended on scales ranging
from 2 to 180 kpc (median 12 kpc). In several cases, it is aligned with the
host galaxy. We set a limit of $\lesssim$1% to the fraction of remnant or
restarted objects, which is $\lesssim$16% of the extended sources.

We found that the properties of the radio sources are connected with the
stellar mass of the ETGs (the median radio power, the fraction of extended
radio sources, and the link with the large-scale environment). However, these
results only describe statistical trends because the radio properties of
sources of similar stellar mass and environment show a large spread of radio
properties. These trends break at the lowest host luminosities
($M_{K}>-24.5$). This effect is strengthened by the analysis of even less
massive ETGs, with $-23.5<M_{K}<-21.5$. This suggests that at a mass of $\sim
2\times 10^{11}{\rm M}_{\odot}$ , a general transition occurs from radio
emission produced from radio-loud active galactic nuclei (AGN) to processes
related to the host galaxy and (or) radio quiet AGN. At this luminosity, a
transition in the stellar surface brightness profile also occurs from Sérsic
galaxies to those with a depleted stellar core, the so-called core galaxies.
This finding is in line with previous results that indicated that only core
galaxies host radio-loud AGN.

###### Key Words.:

galaxies: active – galaxies: jets

##  1 Introduction.

Radio-mode feedback, that is, the interplay between the transfer of energy and
matter from relativistic jets to the external medium and the accretion
powering active galactic nuclei (AGNs), is an essential ingredient in the
evolution of galaxies (e.g., Fabian 2012). The energy injected by relativistic
jets is thought to quench star formation and produce the exponential cutoff at
the bright end of the galaxy luminosity function (Croton et al., 2006).
Powerful radio sources are almost invariably associated with early-type
galaxies (ETGs) with high black hole masses, $M_{\rm SMBH}\gtrsim
10^{8}M_{\odot}$ (Baldi et al., 2010; Chiaberge & Marconi, 2011). In order to
understand how radio-mode feedback operates, it is necessary to explore the
properties and the origin of the radio emission in massive ETGs to study their
morphology and to explore their duty cycle.

In recent years, the advent of new-generation radio facilities has allowed
major progress in this field, especially because much lower flux limits than
previously accessible could be explored. For example, it has become clear that
the extended and powerful radio galaxies (hundreds of kiloparsec, kpc, with
L$\gtrsim 10^{24}$ W Hz-1), which dominated the historical 3C and B2 radio
samples, clearly represent only a small part of the entire radio AGN
population. The bulk of radio AGN instead has low radio powers and sizes
smaller than a few kpc (e.g., Best et al. 2005b; Baldi et al. 2015; Hardcastle
et al. 2019). In analogy to the historical radiogalaxy classification into FRI
or FRII ( Fanaroff & Riley (1974)), this population of compact radio sources
was named FR0s. It is still debated why most radio sources do not develop
large-scale jets, but it is likely due to a combination of different intrinsic
properties of the black hole (e.g., mass and spin) and the mass of the host,
its environment, and the jet duty cycle.

Even the classical FRI/FRII dichotomy (low power/edge-darkened versus high-
power/edge-brightened radio galaxies) has recently started to be questioned.
Large samples of extended sources at high sensitivity have indeed shown that
there is a very large overlap in luminosity for the two morphologies. In
particular, a population of low-power FR IIs was revealed (e.g., Capetti et
al. 2017; Mingo et al. 2019, 2022). They appear to be associated with lower-
mass hosts and reach radio luminosities lower by three orders of magnitude of
the traditional FR break ($\sim 10^{25}$ W Hz-1 at 1.4 GHz Ledlow & Owen
1996). Two main scenarios have long been discussed in the literature to
explain the difference between FRI and FRII morphology. The first scenario
suggests that FRIs live in more massive galaxies and denser environments,
which are able to decelerate their jets with respect to FRIIs. The second
scenario suggests instead that there is a more intrinsic difference in the jet
formation of these two classes of sources, or that it might be related to a
different accretion process (radiatively efficient versus radiatively
inefficient). However, while the large predominance of FRI radio galaxies seem
to be associated with radiatively inefficient accretion, FRII sources can
clearly be both: Up to 65% of the luminous FRIIs (L${}_{150}\gtrsim 10^{26}$ W
Hz-1) are radiatively inefficient (e.g., Miraghaei & Best 2017; Mingo et al.
2022.)

To explore all this further, in Capetti et al. (2022), hereafter Paper I, we
studied the properties and the origin of the low-frequency radio emission in
the most luminous giant ETGs (gETGs) in the local Universe (recession velocity
$\rm\leq 7,500\ km\ s^{-1})$. Low-Frequency ARray (LOFAR, Shimwell et al.
2017) observations at 150 MHz that were obtained as part of the LOFAR Two-
metre Sky Survey (LoTSS) were available for 188 out of the 489 selected
galaxies at the time of this analysis. We confirmed the positive correlation
between the stellar luminosity of gETGs and their median radio power that has
been reported by previous studies (Colla et al., 1975; Fanti et al., 1978;
Sadler et al., 1989; Wrobel, 1991; Wrobel & Heeschen, 1991; Best et al.,
2005a; Brown et al., 2011; Sabater et al., 2019) and also the very wide spread
of the radio luminosity (several orders of magnitude) at a given host mass.
Two-thirds of the detected gETGs are compact, with sizes $\lesssim 4$ kpc.
This confirms the prevalence of compact radio sources in nearby ETGs (Capetti
et al., 2017). The radio emission of 46 (24%) gETGs is extended, with sizes up
to $\sim$300 kpc, and at least 80% of these have a Fanaroff & Riley (1974)
type I morphology. Based on the morphology and spectral index of the extended
sources, we classified $\sim$30% of them as candidate remnant or restarted
sources. Optical spectroscopy (available for 44 gETGs) indicates that the
nuclear gas in 7 gETGs is ionized by young stars, which suggests a
contribution to their radio emission from star-forming regions. Although all
the 25 most luminous ($M_{K}<-25.8$) gETGs are detected at 150 MHz, they are
not all currently turned on: At least 4 of them are remnant sources, and at
least one source is likely powered by star formation.

We here extend our analysis to less massive ETGs (mETGs) with
$-23.5<M_{K}<-25$ in the same redshift range (see below for the details of the
sample selection). The selected galaxies lie above the exponential cutoff of
the near-infrared luminosity function of local ETGs, which occurs at
$M_{K}\sim$ -22.3 (see, e.g., Bell et al. 2003). ETGs can be separated into
two classes based on their surface brightness profile (SBP): The SBPs of
Sérsic galaxies (SGs) are well represented by a single Sérsic function
(Sersic, 1968), while it deviates in core-Sérsic galaxies (CSGs) from a Sérsic
law in that the core is partially depleted (Graham et al., 2003; Trujillo et
al., 2004; Scott et al., 2013). SGs are less luminous than CSGs. The
transition occurs at $M_{K}\sim-24.5$ (Capetti & Balmaverde, 2006), although
the two classes coexist at luminosities $-23.5\gtrsim M_{K}\gtrsim-25$ .
Capetti & Balmaverde found that the radio-loudness of AGN that are hosted by
ETGs is univocally related to the brightness profile of the host: CSGs
invariably host radio-loud nuclei, while SGs are associated with radio-quiet
nuclei. The gETGs are expected to be CSGs based on their luminosity, while the
mETGs straddle the luminosity separation between the two classes. Therefore,
the sample of ETGs we study in this work covers the crucial mass range in
which the transition between SGs and CSGs (and radio-loud/radio-quiet AGN)
occurs.

We also consider a sample of even less massive ETGs (lmETGs) with
$-21.5<M_{K}<-23.5$ in our study. The sample corresponds to a mass range of
$\sim 0.8\times 10^{10}-6\times 10^{10}{\rm M}_{\odot}$. The lmETGs are
thought to be all SGs based on their near-infrared luminosity.

Figure 1: Distribution in the $cz$ vs. absolute magnitude plane of the lmETG
sample. The empty region in the bottom right corner is due to the threshold of
the 2MASS sample we used for the near-infrared selection of these galaxies.

Figure 2: Distributions of absolute K-band magnitude (left) and recession
velocity (right) for the three ETG samples. The red histograms show the gETGs
studied in Paper I (the dashed histogram in the left panel represents the
gETGs included in the LoTSS DR2 area, the same region in which the mETGs and
lmETGs were selected), the black histogram shows the mETGs sample, and the
blue histogram represents the lmETGs. The lmETG sample is not complete, and
this is clearly seen in the reduced number of galaxies below $M_{K}>-23.5$ and
for $v\gtrsim 6000$ $\rm{\,km\,s}^{-1}$.

The properties of radio-AGN are also likely to be affected by the large-scale
environment. Best et al. (2007) studied the connection between environment and
radio activity in nearby groups ($z<0.1$) identified in observations of the
Sloan Digital Sky Survey (SDSS, York et al. 2000) by Von Der Linden et al.
(2007). They found that brightest group and cluster galaxies (BCGs) are more
likely to host a radio-loud AGN than galaxies of the same stellar mass. Within
$\sim$20% of the virial radius, cluster galaxies exhibit an enhanced
likelihood of radio-loud AGN activity. Croston et al. (2019) found that only
10% of the radio AGN are located in halos with $M>10^{14}M_{\odot}$. Within
this population, they found that the radio luminosity of the brightest AGN
depends on the richness, and that the radio luminosity negatively depends on
the distance from the cluster center. These results indicate that the nuclear
activity is related to the large-scale environment and not to the host stellar
mass alone.

Capetti et al. (2020) explored the properties of the large-scale environment
of the compact FR 0 radio galaxies associated with nearby ($z<0.05$) ETGs.
They reported that FR 0s are located in regions with an average galaxy density
that was lower by a factor of two than for FR Is. This difference is driven by
the large fraction (63%) of FR 0s that are located in groups formed by fewer
than 15 galaxies. FR Is rarely (17%) inhabit an environment like this. The
authors interpreted the differences in environment between FR 0s and FR Is as
due to an evolutionary link between local galaxies density, black hole spin,
jet power, and extended radio emission. The analysis of the environment of
local ETGs can be used to test these conclusions and strengthen their
statistical significance.

The paper is organized as follows: In Sect. 2 we describe the sample of the
selected sources and the available radio observations with LOFAR and from
surveys at 1.4 GHz. In Sect. 3 we present the main results for the mETGs,
including a description of the radio morphology and spectral shape. The
connection between radio properties and environment is the subject of Sect. 4.
The information available for the mETGs from optical spectroscopy are
described in Sect. 5. In Sect. 6 we draw a comparison of the properties of
gETGs and mETGs. The analysis is then extended to even lower-mass ETG in Sect.
7, which are used to set our results on a firmer basis. In Sect. 8 we discuss
the results, which are summarized in Sect. 9, where we also draw our
conclusions.

##  2 Sample selection and the LOFAR observations.

Figure 3: Distribution of the 150 MHz luminosity of the three samples of ETGs:
(top) lmETGs, (middle) mETGs, and (bottom) the gETGs studied in Paper I. The
dashed histograms correspond to the upper limits of the undetected sources.

Figure 4: Three examples of mETGs with extended radio emission, representative
of the main morphological classes: (left) cospatial radio and optical
emission, (center) jetted source, (right) diffuse radio source. The LOFAR
images at 150 MHz are superposed to the optical images from Pan-STARRS. The
lowest contours are drawn at three times the local r.m.s. (see Table
LABEL:tab). Images of all 31 extended sources are shown in the Appendix B.

In Paper I we selected the galaxies that are included in the 2MASS Redshift
Survey Huchra et al. (2012) by requiring a declination DEC $>0^{\circ}$, a
Hubble type $T\leq 0$, a total absolute magnitude $M_{K}<-25$, and a recession
velocity (corrected for the effects of the Virgo cluster, the Great Attractor,
and the Shapley supercluster; Mould et al. 2000) $v<7500$ $\rm{\,km\,s}^{-1}$.
We here extend the analysis to less massive ETGs by requiring a total absolute
magnitude in the $-23.5<M_{K}<-25$ range. The magnitude limit of the 2MASS
survey, $K=11.75$, translates into a threshold in the absolute of
$M_{K}=-23.45$ at $v=7500$ $\rm{\,km\,s}^{-1}$: The selected sources form a
complete volume-limited sample. By using the relation between the dynamical
mass and K-band absolute magnitude (log $M_{*}=10.58-0.44\times(M_{Ks}+23)$;
Cappellari 2013), the mETG masses lie in the range of $\sim 6\times
10^{10}-3\times 10^{11}{\rm M}_{\odot}$, while we considered in Paper I all
the available LoTSS pointings (including DR1 data and proprietary data).
Considering the higher space density of lower-mass ETGs, we can now limit
ourselves to the 432 galaxies that are located in the area covered by the
second LoTSS data release (DR2; Shimwell et al. 2022) as they form a
sufficiently large sample for this statistical study. Furthermore, the DR2
images are deeper than those obtained from individual LoTSS pointings. Two
additional sources are superposed to the lobes of bright nearby sources, and
they were dropped from the sample at this stage.

In the same DR2 area there are 158 lmETGs. The magnitude limit of the 2MASS
survey, $K=11.75$, translates into a threshold in the absolute of
$M_{K}=-23.45$ at $v=7500$ $\rm{\,km\,s}^{-1}$: Unlike the gETGs and mETGs,
the lmETGs sample is not complete (see Fig. 1 where we present the
distribution of the lmETGs in the $cz$ versus absolute magnitude plane).

Figure 2 shows the distributions in redshift and absolute K-band magnitude of
all the ETGs considered in this study. The combined sample of mETGs and gETGs
covers a range of a factor $\sim 100$ in near-infrared luminosity.

The LoTSS DR2 includes 27% of the northern sky with a median rms sensitivity
of 83 $\mu$Jy/beam. DR2 provides fully calibrated mosaics at a resolution with
a full width at half maximum (FWHM) $\sim 6\arcsec$, catalogs, and pipeline
products. The flux density scale has an accuracy of approximately 10%.

##  3 The radio properties of mETGs.

We estimated the rms of each image of the mETGs in various regions, usually
centered 45$\arcmin$ away from the source of interest. The median rms is
88$\mu$Jy/beam, similar to the value measured over the whole DR2. The radio
flux density of the sources is available from the released catalog, but
several galaxies have large-scale and complex radio structures that are not
always fully included in the catalog measurement. For these objects, we
measured the flux densities directly from the images and included the whole
source emission within the 3$\sigma$ isophote. We obtained a detection at
$>5\sigma$ significance for 208 (48%) of the sources of the sample.

The measurements at 1.4 GHz were obtained from the Faint Images of the Radio
Sky at Twenty centimeters survey (FIRST; Becker et al. 1995; Helfand et al.
2015) or from the National Radio Astronomy Observatory Very Large Array Sky
Survey (NVSS; Condon et al. 1998). The FIRST area contains 219 galaxies, 45 of
which are detected by this survey above the 5$\sigma$ level. For the
undetected sources, we estimated upper limits at five times the local noise,
typically $\sim 0.14$ mJy beam-1. For the 102 galaxies outside the FIRST area,
we collected the NVSS measurements; 37 of these sources have an NVSS
detection. For the remaining 65 sources, we adopted a limit of 2 mJy. For the
extended galaxies (defined as described in Section 3) we measured the NVSS
flux densities in the same region as was used for the LOFAR images.

The LOFAR observations did not detect 224 mETGs at a 5$\sigma$ significance
(52%). The corresponding limits to the radio luminosity range from
$\sim$3$\times 10^{19}$ to $\sim 3\times 10^{21}\>{\rm W}\,{\rm Hz}^{-1}$,
with a median of 3$\times 10^{20}\>{\rm W}\,{\rm Hz}^{-1}$. The luminosity
distribution at 150 MHz of the mETGs covers a wide range in power from $\sim
4\times 10^{19}\>{\rm W}\,{\rm Hz}^{-1}$ to $\sim 2\times 10^{24}\>{\rm
W}\,{\rm Hz}^{-1}$ and is compared to that obtained for the gETGs in Figure 3.
The mETGs have a lower median power than the gETGs, which extend to a higher
radio power.

We defined the 31 sources in which the 3$\sigma$ level isophote extends to a
radius of at least 15″(about twice the beam FWHM) as extended objects. Their
images are presented in Appendix B. In Figure 4 we show three examples that
are representative of the main morphological classes. The sizes of the
extended sources range from 2.2 to 180 kpc, with a median of 12 kpc.

In 5 galaxies with extended radio structures, optical and radio emission are
closely cospatial (see Appendix B for a morphological description of the
individual sources), and the radio emission is elongated along the same axis
as the host galaxy in another 6 cases. This suggests that the radio emission
is not produced by an AGN in these 11 galaxies, but is due to processes
related to the host, such as free-free emission in star-forming regions and
cosmic rays accelerated by supernova explosions (see, e.g., Tabatabaei et al.
2017). Nine sources have an elongated morphology that suggests the presence of
jets. The radio emission of four mETGs is instead diffuse and lacks a central
component, while one has a ring-like structure. The radio structure of the
remaining six sources is unclear because they are barely resolved.

The remaining 177 mETGs are unresolved or marginally resolved. The limit to
their sizes is $\lesssim 4$ kpc. These compact sources represent 85% of the
detected sources and 41% of the whole sample. The fraction of detected sources
(and of those with extended emission) among the mETGs decreases with
decreasing near-infrared host luminosity (see Table 1).

In Figure 5 we compare the flux densities at 150 MHz and 1.4 GHz of the radio
sources associated with the mETGs. The compact objects show a large spread in
their spectral slopes, $-0.5<\alpha_{150,1400}<1.2$, with the spectral indices
$\alpha$ defined as $F_{\nu}\propto\,\nu^{-\alpha}$. but the range could be
even wider considering the lower limits. Most extended sources have
$0.5<\alpha_{150,1400}<1.0$, which is typical of currently active objects.
Three of them (namely, NGC 3619, NGC 4148, and NGC 6211) have flatter spectral
indices ($0.0<\alpha_{150,1400}<0.5$): These are all core-dominated sources,
and their spectrum is determined by the (likely flat spectrum) central
component.

In Paper I we defined as candidate remnant and restarted sources (RRS) those
with 1) a bright small-scale radio structure accompanied by large-scale
diffuse emission (restarted sources) or 2) a radio spectral index
$\alpha_{150,1400}>1.2$ and lack of a central component (remnant sources).
Using the same definition, we find in the sample of mETGs one candidate
restarted source, CGCG499-084. Its radio emission is dominated by two diffuse
tails extending over $\sim$180 kpc and by a central compact bright region. The
overall spectral index is $\alpha_{150,1400}=1.14$, suggesting that the radio
tails are remnants of a previous phase of activity. The limits to the radio
spectral index for two extended sources (namely, CGCG 311-017 and NGC 7276)
are $\alpha_{150,1400}>1.34$ and $\alpha_{150,1400}>1.35$, respectively, and
we consider them as candidate remnant sources. Three more extended sources are
not detected at 1.4 GHz either (namely, NGC 2521, UGC 1022, and UGC 1503). The
lower limits to their spectral slopes are in the $\alpha_{150,1400}>0.54-0.96$
range, which means that they are not necessarily remnant sources. However,
they are all characterized by a diffuse radio structure, which supports this
interpretation. Overall, we set an upper limit of $\lesssim$16% to the
fraction of RRSs among the mETGs with extended radio emission and of
$\lesssim$1% for the whole sample.

Figure 5: Comparison of the flux densities at 150 and 1400 MHz for the mETGs.
The small red dots mark the upper limits for the sources that are not detected
at 1.4 GHz. The two clusters of upper limits correspond to the sources that
are undetected by either the FIRST or the NVSS. The two black crosses
represent the typical errors on the flux density measurements, which are $\sim
10$% on $F_{150}$ and $\sim 30$% and $\sim 5$% for high and low values of
$F_{1400}$, respectively. The blue diamonds mark the extended sources at 150
MHz. The lines represent the loci of constant spectral index. Figure 6:
Absolute K-band magnitude vs. the luminosity at 150 MHz. The red symbols show
the gETGs ($M_{K}<-25.0$), and the black symbols show the mETGs
($-25.0<M_{K}<-23.5$). The small dots mark the upper limits of the undetected
objects. The large green dots represent the median radio luminosity in six
bins of absolute magnitude, and the green line is the best linear fit to the
four brightest galaxies bins.  Figure 7: Fraction of galaxies that host a
radio source above a given luminosity limit. The samples of mETGs and gETGs
are split into six bins with a K-band luminosity that are 0.5 magnitude wide.
The galaxies in the first bin have $-23.5>M_{K}>-24.0$ (green histogram), and
the following bins correspond to the red, blue, black, gray, and orange
histograms. The solid histograms correspond to the detected sources, and the
dashed histograms include the upper limits and represent the lower and upper
envelope of the distribution, respectively. The circles represent the median
value of the undetected sources obtained with the stacking technique. Figure
8: Comparison of the distributions of the 150 MHz luminosity of the mETGs in
the two least massive bins. The dashed histograms represent the upper limits
for the undetected sources.

In Figure 6 we compare the near-infrared and radio luminosity of the mETGs and
gETGs. The radio power shows a spread of about four orders of magnitude at a
given host luminosity. We estimated the median luminosity,
$\overline{L}_{150}$, of the mETGs by splitting the sample into three bins of
absolute magnitude, each 0.5 mag wide, and by using the stacking technique
(e.g., White et al. 2007). By performing a filtering of the images of the
three subsamples in the luminosity domain, we measured the values of
$\overline{L}_{150}$ reported in Tab. 1. The median $L_{150}$ increases with
stellar luminosity. A linear fit, estimated using the Python procedure
polyfit, to the median $L_{150}$ in the four brightest bins of $M_{K}$ (i.e.,
also including the gETGs) returns log $L_{150}=(-0.96\pm
0.02)\times(M_{K}+25.5)+(21.79\pm 0.01)$. The faintest galaxies show an excess
with respect to the general trend. In particular, the measured median
luminosity for the galaxies with $-23.5<M_{K}<-24.0$ is log$L_{150}=20.58\pm
0.04$. This value is higher by a factor of about three than the extrapolation
of the correlation, which predicts log$L_{150}=20.10\pm 0.03$.

Figure 9: Comparison of the number of group members, $N_{\rm mb}$, for the
gETGs (left) and mETGs (right). In each subsample, we separately consider the
sources based on their radio properties. The 34 mETGs with $N_{\rm mb}>65$ (22
undetected, 10 compact, and 2 extended), all belonging to the Coma cluster,
are not shown for more clarity. Similarly, there are 9 gETGs with $N_{\rm
mb}>65$ (3 undetected, 5 compact, and one extended).

Figure 7 reports the fraction of ETGs hosting a radio source with a power
higher than a given radio power in various bins of near-infrared absolute
magnitude. These functions are fully determined down to the luminosity at
which we encounter the first upper limit. Below this value, the presence of
undetected sources produces two branches that represent the lower and upper
envelope of the true distribution. This analysis can be extended to lower
luminosities with the stacking technique, which enables us to estimate the
median power of the undetected sources. We find a power of log L150=20.57 at
the 81th percentile, log L150=20.34 at the 71th percentile, and log L150=20.12
at the 71th percentile for the three luminosity bins of the mETGs. Overall,
this analysis confirms that the more massive galaxies have a higher
probability to host a radio luminosity above a given threshold. However, this
trend is not seen at the lowest near-infrared luminosities because the mETGs
in the two lower-luminosity bins show very similar distributions. This is
clearly seen in Fig. 8, where we compare the distributions of the 150 MHz
luminosity of the least massive mETGs. In addition, the slopes of the
distributions generally increase with decreasing $L_{K}$. This effect is
likely due to the cutoff in the power law that describes these distributions,
which occur at a radio power that moves to lower $L_{150}$ for lower $L_{K}$.

##  4 Large-scale environment and radio activity in mETGs and gETGs.

We explored the connection between the large-scale environment and the radio
properties of both ETG samples. We used the galaxy group catalog built from
the 2MASS Redshift Survey by Tully (2015) to identify those associated with
each ETG of our sample. We report the number of group members from Tully
(2015), $N_{\rm mb}$, for each galaxy in Tables LABEL:tab and C.1. Figure 9
shows the distributions of $N_{\rm mb}$ for the gETGs and the mETGs,
considering extended, compact, and undetected sources separately.

Table 1: Properties of mETGs versus gETGs.

|  | $\overline{M}_{K}$ | log $\overline{M_{\odot}}$ | Detected | Compact | Extended | log $\overline{L}_{150}$
---|---|---|---|---|---|---|---
|  |  |  |  | Detected | Total |  |
| -26.0$<M_{K}<$-26.5 | -26.22 | 12.0 | 100% | 55% | 55% | 45% | 22.47
gETGs | -25.5$<M_{K}<$-26.0 | -25.67 | 11.7 | 91% | 63% | 57% | 34% | 21.97
| -25.0$<M_{K}<$-25.5 | -25.17 | 11.5 | 70% | 74% | 52% | 18% | 21.45
| -24.5$<M_{K}<$-25.0 | -24.70 | 11.3 | 64% | 84% | 54% | 10% | 21.02
mETGs | -24.0$<M_{K}<$-24.5 | -24.26 | 11.1 | 42% | 86% | 36% | 6% | 20.69
| -23.5$<M_{K}<$-24.0 | -23.74 | 10.9 | 43% | 86% | 37% | 6% | 20.58

Columns 1 and 2: Range and median value of infrared absolute magnitude. Column
3: Fraction of sources detected at 150 MHz. Columns 4 and 5: Fraction of
compact sources in the detected sources and in the whole bin. Column 6:
Fraction of extended sources. Column 7: Median radio luminosity.

The radio morphology and $N_{\rm mb}$ in gETGs are strongly connected. The
median $N_{\rm mb}$ value for the extended sources is $\overline{N}_{\rm
mb}$=13, for the compact sources, it is $\overline{N}_{\rm mb}$=7, and for the
undetected sources, it is $\overline{N}_{\rm mb}$=3. The Kolmogorov-Smirnov
test indicates that the $N_{\rm mb}$ distributions for the three subsamples
are all significantly different. The Kolmogorov-Smirnov test returns a
probability of P=0.042 when the extended and the compact sources are compared,
P=5$\times 10^{-5}$ for the comparison between extended and undetected
sources, and P=0.013 for the compact and the unresolved sources. For the
mETGs, the median value for all classes is $\overline{N}_{\rm mb}$=4, and
their distributions are not statistically different at a 5% confidence level.

Capetti et al. (2020) compared the large-scale environment of the compact FR 0
radio galaxies with those with a FR I morphology. They found that FR 0s are
located in a poorer environment, 63% of them living in groups formed by less
than 15 galaxies, compared to only 17% of the FR Is. Their analysis is based
on the number of cosmological neighbors, $N_{\rm cn}^{1000}$, i.e., galaxies
lying within a region of projected radius of 1 Mpc and having a spectroscopic
redshift differing by less than 0.005 from the radio galaxy, based on SDSS
data.

The gETGs sample is only partially covered by the SDSS survey and this method
cannot be applied. To put the present result into context we estimated $N_{\rm
cn}^{1000}$ and $N_{\rm mb}$ for the 78 gETGs with available SDSS spectra. The
number of companions estimated by the two methods shows a strong correlation,
with $N_{\rm cn}^{1000}\sim 2\times N_{\rm mb}$, the larger number of
cosmological neighbors being due to the fact that the SDSS data reach lower
magnitudes with respect to 2MASS.

After applying a factor two correction to the galaxy members of each system,
following the aforementioned analysis, we find that the fractions of gETGs
located in 2MASS groups with less than eight members are 28% and 53% for the
extended and compact sources, respectively, in substantial agreement with the
previous analysis.

The link between the radio morphology of the gETGs and large-scale galaxy
densities translates into a similar connection between radio luminosity and
environment, likely due to the fact that the extended sources are generally
those of higher radio power. The median luminosities at 150 MHz are $4.2\times
10^{20},12.6\times 10^{20}$, and $19.5\times 10^{20}\>{\rm W}\,{\rm Hz}^{-1}$,
for galaxies with $N_{\rm mb}\leq 10$, $10<N_{\rm mb}\leq 30$, and $N_{\rm
mb}>30$, respectively.

Furthermore, the galaxy densities around compact sources is higher than in
undetected ones. For the compact gETGs we find a median
$\overline{L}_{150}=5.0\times 10^{21}\>{\rm W}\,{\rm Hz}^{-1}$ while the
stacking analysis indicates that this value for the undetected sources is
$5.1\times 10^{20}\>{\rm W}\,{\rm Hz}^{-1}$. This effect does not stem from
the dependence on the host luminosity, because these two classes have very
similar median values ($\overline{M}_{K}=-25.33$ and $\overline{M}_{K}=-25.19$
for the compact and undetected sources, respectively). These results indicate
that the large scale environment plays an important role in setting the
morphology and the luminosity of the radio sources associated with ETGs.

As already mentioned, these results apply only to the gETGs. No link between
environment and radio properties is seen for the mETGs.

##  5 Optical spectroscopic properties of mETGs.

Figure 10: Optical spectroscopic diagnostic diagrams for the mETGs with
available SDSS spectra. We adopted a conservative threshold of S/N$>$5 for the
lines detection. The solid lines are from Kewley et al. (2006) and separate
S.F. galaxies, LINER, and Seyfert; in the first panel, the region between the
two curves is populated by the composite galaxies. Triangles are used to mark
upper or lower limits. The blue symbols represent mETGs located within the
region populated by S.F. galaxies in the [S II]/H$\alpha$ vs. [O III]/H$\beta$
diagram.

Optical spectra can be used to identify the gas ionization mechanism by
measuring the ratios of selected emission lines (e.g. Heckman 1980; Baldwin et
al. 1981; Veilleux & Osterbrock 1987; Kewley et al. 2006). We used the fluxes
of the diagnostic optical emission lines from the MPA-JHU added value catalog
of SDSS spectral measurements.111available at http://www.mpa-
garching.mpg.de/SDSS/DR7/ SDSS spectra are available for 158 of the ETGs of
our sample, but only in 73 of these spectra it is possible to measure a
sufficient number of emission lines (at a significance $>5\sigma$) to locate
them in the diagnostic diagrams, see Figure 10. Their spectral classification
is reported in Table LABEL:tab. Three ETGs in the [O III]/H$\beta$ versus [S
II]/H$\alpha$ diagram fall into the region of Seyferts, and 45 of them are
among the LINERs. The remaining 25 (34 %) are compatible with a classification
as star-forming (S.F.)

The 25 S.F. candidates span the whole range of near-infrared luminosity with a
median of $M_{K}=-24.0$, which is slightly lower than the median for the whole
sample. Most S.F. candidates (20 out of 25) are detected by LOFAR with
luminosities in the range $L_{150}=1.7\times 10^{21}-6\times 10^{22}$ W Hz-1
(median $L_{150}=5\times 10^{21}$ Hz-1). All but two (MCG+10-12-141 and UGC
09473) are compact sources.

By adopting the relation from Gürkan et al. (2018), we translated the radio
luminosities at 150 MHz of the S.F. candidates detected by LOFAR into a star
formation rate (SFR). We obtained a range between 0.2 and 4.3 M⊙yr-1 (median
0.4 M⊙yr-1).

The masses of the 25 S.F. candidates are in the range of $\sim 6\times
10^{10}-2\times 10^{11}{\rm M}_{\odot}$ . The values for the specific SFR
(sSFR) are $0.6-30\times 10^{-12}{\rm yr}^{-1}$ . The median value (including
the sources not detected at 150 MHz) is $2.5\times 10^{-12}{\rm yr}^{-1}$.

From the point of view of the radio spectra, only eight of the S.F. candidates
are detected in the surveys at 1.4 GHz, and the resulting spectral slopes are
in the range of $\alpha_{150}^{1400}=0.31-0.90$ , with a median of
$\alpha_{150}^{1400}=0.70$ that is consistent with the low-frequency radio
slope of S.F. galaxies ($\alpha=0.59$, Klein et al. 2018).

##  6 Extending the study to lower-mass ETGs.

The results of the previous sections show several trends linking the radio
properties to the host luminosity. In particular, we found an increase in
median radio luminosity with the host mass. While this trend in the brightest
galaxies is well described by $L_{150}\propto L_{K}^{2.6}$, the $L_{150}$
versus $L_{K}$ flattens in the faintest galaxies. However, this effect is not
well defined. It is only visible in the $-24.5<M_{K}<-23.5$ luminosity range.
The lmETGs sample can be used to place this result on a stronger basis.

The luminosity distribution at 150 MHz of the 55 detected lmETGs covers a wide
range in power, from $\sim 3\times 10^{19}\>{\rm W}\,{\rm Hz}^{-1}$ to $\sim
10^{23}\>{\rm W}\,{\rm Hz}^{-1}$ (see Figure 3). One hundred and three lmETGs
are not detected by the LOFAR observations, and the median limit to their
radio luminosities is 2.5$\times 10^{20}\>{\rm W}\,{\rm Hz}^{-1}$. The
fraction of detected lmETGs is smaller than that measured in the samples of
more massive ETGs. It is 35%, 48%, and 78% for the lmETGs, mETG, and gETGs,
respectively. We list the main properties of the lmETG sample in Table
LABEL:tablm .

In Figure 11 we compare the near-infrared and radio luminosity of the three
samples. As we found for the more massive ETGs, the radio power of lmETGs is
spread widely, about four orders of magnitude) at a given host luminosity. By
including the lmETGs, we confirm that the median radio luminosity decreases at
lower stellar luminosity. We estimated the median luminosity,
$\overline{L}_{150}$, of the lmETGs by splitting the sample into four bins of
absolute magnitude, each 0.5 mag wide, and using the stacking technique. The
stacking analysis only returns a robust measurement for the two bins including
the brightest galaxies. We obtained log $\overline{L}_{150}=20.28$ and 20.12
for $-22.5>M_{K}>-23.0$ and $-23.0>M_{K}>-23.5$, respectively. Similarly to
the lower-mass mETGs, the lmETGs show an excess with respect to the trend
measured at the highest masses. The overall connection between $L_{150}$ and
near-infrared luminosity $L_{K}$ is well described by log
$L_{150}\sim$log$L_{K}^{2.6}$ for $M_{K}\lesssim-24.5,$ while it flattens to a
slope of 1.03 for the four bins including the less luminous ETGs. From a
linear fit, we obtain log $L_{150}=(-0.41\pm 0.04)\times(M_{K}+23.5)+(20.41\pm
0.04)$.

Figure 11: Absolute K-band magnitude vs. luminosity at 150 MHz. The red
symbols are the gETGs ($M_{K}<-25.0$), the black symbols are the mETGs
($-25.0<M_{K}<-23.5$), and the blue symbols are the lmETGs
($-23.5<M_{K}<-21.5$). The small dots mark the upper limits of the undetected
objects. The large green dots represent the median radio luminosity in eight
bins of absolute magnitude, and the solid (dashed) green line represents the
best linear fit to the four brightest (faintest) galaxies bins.

Another effect shown by the ETGs is the dependence of the morphology of the
radio sources on the host mass. In this respect, the morphologies of the radio
sources associated with the lmETGs are significantly different from those seen
in the brighter ETGs. In the gETGs, we found 42 (out of 188) extended sources,
at least 80% of which having a class I Fanaroff & Riley (1974) morphology. The
fraction of sources with a jetted morphology in mETGs is strongly reduced.
Only nine out of 432 galaxies ($\sim 2\%$) are jetted, while the morphology of
none of the lmETGs is indicative of collimated jets. Only 4 (out of 158)
lmETGs satisfy the definition of an extended radio source. In all four cases,
the radio emission is diffuse and cospatial with the host galaxy.

While most radio sources in the gETGs and mETGs are compact or barely
resolved, the most common morphology in lmETGs is a diffuse emission. To draw
a more quantitative comparison, we show in Fig. 12 the distribution of the
radio source extension (obtained by fitting a two-dimensional Gaussian profile
as reported in the DR2 catalog) versus the flux density at 150 MHz for the
lmETGs and the mETGs split into two bins of absolute magnitude. Overall, there
is a clear trend of increasing radio source size for lower-mass ETGs. More
quantitatively, 51% of the lmETGs have measured angular sizes between $\sim
10\arcsec$ and $\sim 25\arcsec$, corresponding to deconvolved linear sizes of
$\sim 4-12$ kpc. Conversely, for the two luminosity bins of mETGs, the
fractions are 36% and 14%.

Figure 12: Distribution of the radio sources extension vs. flux density at 150
MHz for the lmETGs (top) and the mETGs, split into two bins of near-infrared
luminosity (middle and bottom). The dashed green lines mark the 6″ resolution
of the LoTSS images.

##  7 Discussion.

The study of a volume-limited sample of ETGs covering a factor $\sim 100$ in
host luminosity indicates that several physical parameters show a positive
correlation with the stellar luminosity.

  * •

1) The fraction of galaxies detected by LOFAR increases with increasing
$L_{K}$: While the more luminous gETGs (with $-26.0<M_{K}<-26.5$) are all
detected at 150 MHz, this fraction decreases to $\sim$40% for the least
luminous mETGs and to 35% for lmETGs.

  * •

2) The fraction of extended radio sources decreases from 45% in the more
massive gETGs to 6% in the less massive mETGs. While the extended sources in
gETGs have a median size of 57 kpc, this value is 12 kpc in the mETGs. At
least 80% of the extended gETGs have a FR I class morphology, which clearly
indicates jets. Only 9 mETGs ($\sim$ 2%) are likely jetted sources, six of
which lie in the brightest host luminosity bin. The radio emission is
cospatial (or aligned) with the optical emission in 11 mETGs, suggesting a
prevalence of processes at the origin of the radio emission related to the
host galaxies. None of the lmETGs has a morphology indicative of the presence
of collimated jets. Only 4 (out of 158) lmETGs satisfy the definition of an
extended radio source, and in all cases, the radio emission is diffuse and
cospatial with the host galaxy.

  * •

3) The median radio luminosity shows an increasing trend with the host
luminosity. When only the brightest galaxies are considered, this trend is
well described by $L_{150}\propto L_{K}^{2.6}$. The faintest galaxies instead
show a much shallower, almost linear, dependence on $L_{K}$. This is
interpreted as due to the transition from an AGN- to host-dominated radio
emission.

  * •

4) The fraction of candidate RRSs among the gETGs is $\sim 7\%$. This is $\sim
28\%$ of those with extended emission. Conversely, we find only one candidate
restarted source among the mETGs and two sources with a spectral index higher
than 1.2, which are therefore candidate remnants. Three additional extended
sources that are not detected at 1.4 GHz might be remnant sources. This
interpretation is supported by their diffuse morphology. However, the limits
to their spectral slopes are all well below the 1.2 threshold. Overall, we set
an upper limit of $\lesssim 1\%$ to the fraction of RRSs in the mETG sample,
which is $\lesssim$16% of those with extended emission. This is lower than in
gETGs. However, when we only consider the mETGs with a jetted morphology, this
fraction increases significantly.

  * •

5) The source radio morphology and the large-scale environment of gETGs are
connected. The extended (and more powerful radio sources) are found in regions
of higher galaxy density than the compact and undetected sources. This effect
is absent for the mETGs.

To summarize, the median radio power, the fraction of the detected sources,
and the fraction (and size) of the jetted sources all depend on the host
luminosity. The fraction of RRS is also related to the host mass because it
decreases from $\sim 7\%$ in the gETGs to $<1\%$ in the mETGs. These same
parameters are also related to the large-scale environment: We find a
connection between the large-scale galaxy density and the presence of extended
radio emission and its luminosity. This effect is seen only in the gETGs and
in the most massive mETGs. However, these results only describe statistical
trends. Even when we consider sources of similar stellar mass and environment,
for example, a wide spread in radio luminosity is found. This implies that
additional physical quantities such as the accretion rate and the source age
are likely to be involved in setting the level of radio activity. In addition,
as we already argued in Paper I, compact and extended radio sources differ in
their jet properties. The compact sources might be produced by slower jets
because of a lower black holes spin.

These trends break at the lowest near-infrared luminosity. While at high mass,
the $L_{150}$ versus $L_{K}$ relation is well described by a power law with an
index of $\sim 2.6$, at lower masses, the index decreases to $\sim 1$. In
addition, while the more massive ETGs are mostly associated with point-like or
jetted radio sources, in the least luminous galaxies, these are often diffuse
and extended on a scale of $\sim 4-12$ kpc. These results suggest that in the
less massive galaxies probed by our study, the dominant process at the origin
of the radio emission is not associated with a radio-loud AGN, but with the
host galaxy. This interpretation is supported by the significant fraction of
mETGs and lmETGs in which the radio emission is aligned (or cospatial) with
the host galaxy. In these sources, the radio emission is likely to be
dominated by processes related to the host galaxies such as young stars and
supernovae. The fraction of mETGs in which the optical spectra indicate that
the nuclear gas is ionized by young stars is $\sim 16\%$, similar to what we
found for the gETGs. The star formation rate, which is derived by ascribing
the radio emission to young stars, is similar for two luminosity classes of
ETGs, but the specific SFR is about three times higher in mETGs than in gETGs
because their mass is lower. However, the SDSS spectra cover a nuclear region
of less than 1 kpc in radius, and they are not representative of the whole
galaxy. The only two sources where the extended emission is cospatial (or
aligned) with the host and with an available SDSS spectra are one Seyfert and
one LINER. This suggests that the radio emission in low-mass ETGs might also
be powered by a radio-quiet AGN.

The transition between radio sources that are dominated by a radio-loud AGN to
host galaxy processes (or radio-quiet AGN) occurs at a mass that is similar to
the mass at which ETGs change their stellar brightness profile from a pure
Sérsic law to a core-Sérsic law. As already mentioned in the Introduction, the
different brightness profiles correspond to the dichotomy between radio-loud
and radio-quiet AGN: Radio-loud AGN are only hosted by core galaxies, while
radio-quiet AGN are found only in Sérsic galaxies.

##  8 Summary and conclusions

We explored the radio properties of ETGs in the local Universe (recession
velocity $<7,500$ $\rm{\,km\,s}^{-1}$) as seen by LOFAR observations at 150
MHz. In Paper I we considered 188 giant ETGs with $M_{K}<-25$, while here we
analyzed the mETGs, which have a near-infrared luminosity in the
$-23.5>M_{K}>-25$ range, that is, with a mass $6\times 10^{10}\lesssim
M_{*}\lesssim 3\times 10^{11}{\rm M}_{\odot}$. We also considered even less
luminous galaxies, the lmETGs, down to $M_{K}=-21.5$. The combined volume-
limited sample covers an interval of a factor $\sim 100$ in stellar mass.

The fraction of sources detected above a typical luminosity of $\sim 3\times
10^{20}\>{\rm W}\,{\rm Hz}^{-1}$ decreases from 78% of the gETGs to $\sim
48\%$ of the mETGs and $\sim 35\%$ of the lmETGs. Of the 31 mETGs with a radio
emission that extends over at least 15″, only a minority (9, representing
$\sim$ 2% of the whole sample) have a morphology suggesting the presence of
collimated jets. This fraction is $\sim$ 20% for the gETGs. No jetted source
is found among the lmETGs. Although we observed mETGs with extended radio
emission (with a median size of $\sim 12$ kpc), the majority of them ($\sim
85\%$ of the detected sources) is unresolved, with a characteristic limit to
their size of $\sim$ 4 kpc. This strengthen previous results that compact FR 0
radio sources represent the dominant population of radio galaxies in the
nearby Universe.

Our study confirms the strong connection between the radio properties and the
host mass: 1) the positive correlation between the stellar luminosity and the
median radio power, 2) the fraction of compact sources that increases with
decreasing host mass, 3) the high incidence of jetted sources among the most
massive ETGs (about 20%), and their scarcity ($\sim 2\%$) among the least
massive ones.

However, the trends above break for the least luminous ETGs. The extension of
the study to even less massive ETGs, the lmETGs, which reach masses as low as
$\sim 0.8\times 10^{10}{\rm M}_{\odot}$, shows that while at high mass, the
log $L_{150}\sim$log$L_{K}$ relation is well described by a power law with an
index of $\sim 2.6$, at lower masses, the index decreases to $\sim 1$.
Combined with the radio morphology of the less massive ETGs, which is often
aligned with the optical axis, this result suggests that we are observing the
transition from the population of the most massive ETGs, $M_{*}\gtrsim 2\times
10^{11}{\rm M}_{\odot}$, in which the dominant process of radio emission can
be associated with a radio loud AGN, to host-dominated sources. At
approximately this mass, the stellar surface brightness profile also
transitions from Sérsic galaxies to those with a depleted stellar core.
Previous studies have shown that only core galaxies host radio-loud AGN. This
is in line with the the present analysis.

The selection of a complete sample based only on stellar luminosity is
optimally suited to exploring the duty cycle of the radio activity in ETGs. We
are now in the position to further constrain the energy output of radio-loud
AGN. The mETGs showing extended radio emission include a candidate restarted
source, with a bright central region associated with two low-brightness tails,
and two galaxies are characterized by a steep radio spectral index
($\alpha_{150}^{1400}\sim 1.35$) that are likely remnant sources. Three
additional extended sources have a diffuse morphology: They are not detected
in the surveys at 1.4 GHz and should be considered candidate remnant sources.
Overall, by considering the mETGs and gETGs samples, based on a combination of
morphology an spectral index, we isolated 19 restarted and remnant (or
candidate remnant) sources. With multiband radio observations, we will be able
to estimate the timescale of the various activity phases.

###### Acknowledgements.

MB acknowledges financial support from the agreement ASI-INAF n. 2017-14-H.O,
from the PRIN MIUR 2017PH3WAT “Blackout” and from the ERC-Stg “MAGCOW”, no.
714196. LOFAR, the Low Frequency Array designed and constructed by ASTRON, has
facilities in several countries, which are owned by various parties (each with
their own funding sources), and are collectively operated by the International
LOFAR Telescope (ILT) foundation under a joint scientific policy. The ILT
resources have benefited from the following recent major funding sources:
CNRS-INSU, Observatoire de Paris and Université d’Orléans, France; BMBF, MIWF-
NRW, MPG, Germany; Science Foundation Ireland (SFI), Department of Business,
Enterprise and Innovation (DBEI), Ireland; NWO, The Netherlands; the Science
and Technology Facilities Council, UK; Ministry of Science and Higher
Education, Poland; The Istituto Nazionale di Astrofisica (INAF), Italy. Part
of this work was carried out on the Dutch national e-infrastructure with the
support of the SURF Cooperative through grant e-infra 160022 & 160152\. The
LOFAR software and dedicated reduction packages on
https://github.com/apmechev/GRID_LRT were deployed on the e-infrastructure by
the LOFAR e-infragrop, consisting of J. B. R. (ASTRON & Leiden Observatory),
A. P. Mechev (Leiden Observatory) and T. Shimwell (ASTRON) with support from
N. Danezi (SURFsara) and C. Schrijvers (SURFsara). The Jülich LOFAR Long Term
Archive and the German LOFAR network are both coordinated and operated by the
Jülich Supercomputing Centre (JSC), and computing resources on the
supercomputer JUWELS at JSC were provided by the Gauss Centre for
supercomputing e.V. (grant CHTB00) through the John von Neumann Institute for
Computing (NIC). This research made use of the University of Hertfordshire
high-performance computing facility and the LOFAR-UK computing facility
located at the University of Hertfordshire and supported by STFC
(ST/P000096/1), and of the Italian LOFAR IT computing infrastructure supported
and operated by INAF, and by the Physics Department of Turin University (under
an agreement with Consorzio Interuniversitario per la Fisica Spaziale) at the
C3S Supercomputing Centre, Italy. The Pan-STARRS1 Surveys (PS1) and the PS1
public science archive have been made possible through contributions by the
Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project
Office, the Max-Planck Society and its participating institutes, the Max
Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for
Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham
University, the University of Edinburgh, the Queen’s University Belfast, the
Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory
Global Telescope Network Incorporated, the National Central University of
Taiwan, the Space Telescope Science Institute, the National Aeronautics and
Space Administration under Grant No. NNX08AR22G issued through the Planetary
Science Division of the NASA Science Mission Directorate, the National Science
Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand
University (ELTE), the Los Alamos National Laboratory, and the Gordon and
Betty Moore Foundation.

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##  Appendix A Properties of the mETG sample.

Table 2: Radio properties of the sample Name | R.A. | DEC. | v | MK | rms | F150 | L150 | Morph. | F1.4 | SDSS | $N_{\rm mb}$
---|---|---|---|---|---|---|---|---|---|---|---
NGC7805 | 0.3616 | 31.4337 | 4766 | -24.10 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |  | — |  | 4
NGC0005 | 1.9537 | 35.3623 | 5062 | -23.74 | 0.17 |  $<$ 0.8 |  $<$ 20.73 |  | — |  | 1
NGC7836 | 2.0068 | 33.0707 | 4854 | -24.00 | 0.09 | 43.0 | 22.41 | E | 9.2 |  | 6
NGC0016 | 2.2679 | 27.7294 | 3097 | -24.52 | 0.13 |  $<$ 0.7 |  $<$ 20.21 |  | — |  | 1
NGC0006 | 2.3862 | 33.3087 | 4919 | -24.88 | 0.08 | 4.7 | 21.46 | C | — |  | 6
NGC0042 | 3.2348 | 22.1003 | 5876 | -24.58 | 0.10 | 1.9 | 21.23 | C | — |  | 2
NGC0043 | 3.2531 | 30.9153 | 4728 | -24.78 | 0.10 |  $<$ 0.5 |  $<$ 20.44 |  | — |  | 3
UGC00130 | 3.4872 | 30.8830 | 4724 | -23.62 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |  | — |  | 3
CGCG499-084 | 3.5528 | 28.5451 | 7023 | -24.11 | 0.10 | 122.9 | 23.19 | E | 9.7 |  | 4
CGCG478-044 | 3.5536 | 22.7665 | 6064 | -23.92 | 0.10 |  $<$ 0.5 |  $<$ 20.67 |  | — |  | 1
CGCG499-087 | 3.8068 | 31.5009 | 6551 | -24.14 | 0.11 |  $<$ 0.6 |  $<$ 20.79 |  | — |  | 1
UGC00146 | 3.9329 | 27.4444 | 7356 | -24.64 | 0.16 |  $<$ 0.8 |  $<$ 21.03 |  | — |  | 1
ARK003 | 3.9691 | 19.7743 | 6353 | -23.86 | 0.10 |  $<$ 0.5 |  $<$ 20.73 |  | — |  | 1
CGCG499-098 | 4.2610 | 29.9424 | 6818 | -24.33 | 0.09 |  $<$ 0.4 |  $<$ 20.73 |  | — |  | 21
CGCG499-102 | 4.4959 | 29.4697 | 6751 | -24.30 | 0.08 |  $<$ 0.4 |  $<$ 20.68 |  | — |  | 21
NGC0072A | 4.6431 | 30.0363 | 6606 | -23.64 | 0.09 |  $<$ 0.5 |  $<$ 20.71 |  | — |  | 21
IC1541 | 5.0081 | 21.9997 | 5815 | -23.74 | 0.08 |  $<$ 0.4 |  $<$ 20.56 |  | — |  | 18
CGCG457-008 | 5.2157 | 21.5366 | 5814 | -23.76 | 0.09 |  $<$ 0.5 |  $<$ 20.60 |  | — |  | 18
NGC0079 | 5.2619 | 22.5665 | 5385 | -24.25 | 0.09 |  $<$ 0.4 |  $<$ 20.51 |  | — |  | 18
NGC0085 | 5.3565 | 22.5117 | 6087 | -23.84 | 0.10 |  $<$ 0.5 |  $<$ 20.69 |  | — |  | 18
NGC0086 | 5.3690 | 22.5564 | 5488 | -23.55 | 0.09 |  $<$ 0.4 |  $<$ 20.54 |  | — |  | 18
IC1548 | 5.4799 | 22.0064 | 5638 | -23.55 | 0.09 | 0.9 | 20.87 | C | — |  | 18
CGCG500-007 | 5.5668 | 30.2474 | 6334 | -23.72 | 0.08 |  $<$ 0.4 |  $<$ 20.61 |  | — |  | 21
NGC0096 | 5.5738 | 22.5462 | 6068 | -23.78 | 0.09 | 0.9 | 20.93 | C | — |  | 18
NGC0097 | 5.6250 | 29.7453 | 4698 | -24.68 | 0.09 |  $<$ 0.4 |  $<$ 20.39 |  | — |  | 1
IC1550 | 6.1152 | 38.1856 | 5834 | -24.32 | 0.08 |  $<$ 0.4 |  $<$ 20.53 |  | — |  | 1
UGC00330 | 8.4243 | 39.5448 | 5793 | -24.05 | 0.12 |  $<$ 0.6 |  $<$ 20.71 |  | — |  | 1
UGC00375 | 9.4328 | 25.6402 | 7235 | -24.57 | 0.09 |  $<$ 0.4 |  $<$ 20.77 |  | — |  | 1
NGC0183 | 9.6225 | 29.5112 | 5303 | -24.74 | 0.10 | 1.5 | 21.03 | C | — |  | 6
UGC00411 | 9.8733 | 25.6434 | 4586 | -23.75 | 0.10 |  $<$ 0.5 |  $<$ 20.41 |  | — |  | 3
CGCG500-074 | 10.6996 | 29.9224 | 4997 | -23.98 | 0.10 |  $<$ 0.5 |  $<$ 20.48 |  | — |  | 8
NGC0229 | 10.7694 | 23.5091 | 7192 | -24.39 | 0.12 |  $<$ 0.6 |  $<$ 20.89 |  | — |  | 4
NGC0233 | 10.9023 | 30.5870 | 5322 | -24.86 | 0.09 |  $<$ 0.5 |  $<$ 20.52 |  | — |  | 8
CGCG479-065 | 10.9250 | 23.4763 | 7082 | -24.22 | 0.11 | 1.6 | 21.31 | C | — |  | 4
CGCG500-080 | 11.0328 | 30.3509 | 5484 | -23.64 | 0.11 |  $<$ 0.6 |  $<$ 20.64 |  | — |  | 8
NGC0243 | 11.5036 | 29.9595 | 4700 | -23.80 | 0.09 | 2.8 | 21.20 | C | — |  | 8
IC1583 | 11.7929 | 23.0738 | 7108 | -24.11 | 0.09 |  $<$ 0.5 |  $<$ 20.78 |  | — |  | 4
IC1585 | 11.8095 | 23.0535 | 7183 | -24.30 | 0.09 | 1.2 | 21.20 | C | — |  | 4
CGCG501-018 | 12.0361 | 28.6139 | 6899 | -24.12 | 0.08 |  $<$ 0.4 |  $<$ 20.70 |  | — |  | 1
NGC0262 | 12.1964 | 31.9570 | 4432 | -23.99 | 0.15 | 753.0 | 23.58 | C | 292.2 |  | 3
UGC00506 | 12.4120 | 22.9323 | 7296 | -24.96 | 0.09 |  $<$ 0.4 |  $<$ 20.76 |  | — |  | 4
NGC0282 | 13.1756 | 30.6391 | 6538 | -24.75 | 0.10 |  $<$ 0.5 |  $<$ 20.72 |  | — |  | 1
NGC0287 | 13.3679 | 32.4823 | 5407 | -24.03 | 0.07 |  $<$ 0.4 |  $<$ 20.44 |  | — |  | 1
CGCG501-034 | 13.3962 | 31.4197 | 5359 | -23.70 | 0.14 |  $<$ 0.7 |  $<$ 20.71 |  | — |  | 14
CGCG536-006 | 13.4951 | 40.4136 | 5669 | -23.85 | 0.10 | 97.8 | 22.91 | E | 18.5 |  | 1
UGC00567 | 13.8310 | 31.7492 | 5962 | -24.24 | 0.08 |  $<$ 0.4 |  $<$ 20.58 |  | — |  | 1
NGC0304 | 14.0251 | 24.1269 | 4877 | -24.57 | 0.09 | 1.8 | 21.04 | C | — |  | 1
NGC0311 | 14.3864 | 30.2808 | 4963 | -24.59 | 0.09 | 2.6 | 21.22 | C | — |  | 14
UGC00612 | 14.7536 | 23.8529 | 4959 | -23.88 | 0.10 | 16.0 | 22.00 | C | 4.4 |  | 1
ARK024 | 15.3045 | 30.1534 | 6852 | -24.20 | 0.13 |  $<$ 0.6 |  $<$ 20.89 |  | — |  | 4
UGC00636 | 15.4257 | 24.0580 | 4971 | -23.71 | 0.09 |  $<$ 0.5 |  $<$ 20.46 |  | — |  | 1
CGCG501-067 | 15.4697 | 30.1458 | 6536 | -24.25 | 0.12 |  $<$ 0.6 |  $<$ 20.82 |  | — |  | 4
UGC00654 | 15.9974 | 21.2254 | 5507 | -23.98 | 0.10 |  $<$ 0.5 |  $<$ 20.59 |  | — |  | 1
NGC0380 | 16.8233 | 32.4829 | 4344 | -24.78 | 0.22 | 8.4 | 21.61 | C | — |  | 48
NGC0384 | 16.8542 | 32.2928 | 4156 | -23.92 | 0.17 |  $<$ 0.8 |  $<$ 20.58 |  | — |  | 48
NGC0385 | 16.8635 | 32.3198 | 4876 | -24.37 | 0.11 |  $<$ 0.6 |  $<$ 20.54 |  | — |  | 48
NGC0392 | 17.0977 | 33.1336 | 4603 | -24.61 | 0.09 |  $<$ 0.5 |  $<$ 20.40 |  | — |  | 48
CGCG501-110 | 17.4858 | 30.4678 | 6409 | -23.88 | 0.07 |  $<$ 0.3 |  $<$ 20.54 |  | — |  | 1
UGC00724 | 17.4974 | 32.3684 | 5073 | -24.02 | 0.11 | 29.0 | 22.28 | E | 3.9 |  | 48
CGCG501-120 | 17.7972 | 32.7018 | 4956 | -23.57 | 0.10 |  $<$ 0.5 |  $<$ 20.49 |  | — |  | 48
NGC0414 | 17.8228 | 33.1139 | 5343 | -24.11 | 0.11 |  $<$ 0.6 |  $<$ 20.62 |  | — |  | 48
NGC0420 | 18.0402 | 32.1232 | 4907 | -24.77 | 0.09 | 0.8 | 20.69 | C | — |  | 48
IC1638 | 18.0909 | 33.3644 | 4693 | -23.70 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |  | — |  | 48
NGC0431 | 18.5189 | 33.7042 | 5610 | -24.68 | 0.14 |  $<$ 0.7 |  $<$ 20.74 |  | — |  | 48
IC1659 | 19.0251 | 30.3491 | 6739 | -24.86 | 0.08 | 16.7 | 22.29 | C | 12.8 |  | 1
NGC0472 | 20.1195 | 32.7090 | 5198 | -24.24 | 0.12 |  $<$ 0.6 |  $<$ 20.62 |  | — |  | 47
UGC00878 | 20.2622 | 33.8984 | 3957 | -24.17 | 0.18 |  $<$ 0.9 |  $<$ 20.57 |  | — |  | 47
NGC0504 | 20.8662 | 33.2043 | 4144 | -23.86 | 0.22 |  $<$ 1.1 |  $<$ 20.69 |  | — |  | 47
NGC0508 | 20.9191 | 33.2807 | 5407 | -24.79 | 0.20 | 10.1 | 21.88 | C | — |  | 47
NGC0517 | 21.1825 | 33.4296 | 4123 | -24.13 | 0.18 | 8.6 | 21.57 | C | — |  | 47
NGC0528 | 21.3899 | 33.6714 | 4708 | -24.63 | 0.28 | 3.9 | 21.35 | C | — |  | 47
UGC01022 | 21.7399 | 39.0182 | 5431 | -23.62 | 0.07 | 10.9 | 21.92 | E | — |  | 1
UGC01032 | 21.8855 | 19.1788 | 5064 | -23.91 | 0.09 | 22.1 | 22.16 | C | 4.8 |  | 1
UGC01101 | 23.1474 | 41.9869 | 5870 | -24.26 | 0.08 |  $<$ 0.4 |  $<$ 20.56 |  | — |  | 1
NGC0608 | 23.8677 | 33.6567 | 4991 | -24.40 | 0.23 |  $<$ 1.1 |  $<$ 20.86 |  | — |  | 3
NGC0614 | 23.9678 | 33.6819 | 5047 | -24.58 | 0.25 | 6.8 | 21.65 | C | — |  | 3
NGC0621 | 24.2044 | 35.5122 | 5055 | -24.65 | 0.09 | 3.0 | 21.29 | C | — |  | 7
NGC0656 | 25.6135 | 26.1431 | 3816 | -24.04 | 0.12 |  $<$ 0.6 |  $<$ 20.33 |  | — |  | 1
NGC0661 | 26.0609 | 28.7059 | 3725 | -24.45 | 0.12 | 1.5 | 20.73 | C | — |  | 1
NGC0666 | 26.5258 | 34.3745 | 4631 | -23.80 | 0.13 |  $<$ 0.6 |  $<$ 20.55 |  | — |  | 1
NGC0670 | 26.8535 | 27.8858 | 3608 | -24.19 | 0.13 | 39.9 | 22.12 | E | 6.4 |  | 4
NGC0680 | 27.4471 | 21.9708 | 2855 | -24.40 | 0.11 | 3.1 | 20.81 | C | — |  | 7
UGC01327 | 27.9506 | 30.5435 | 4552 | -23.54 | 0.10 | 3.9 | 21.32 | C | — |  | 1
NGC0711 | 28.1158 | 17.5126 | 4758 | -24.00 | 0.11 |  $<$ 0.6 |  $<$ 20.51 |  | — |  | 1
NGC0704 | 28.1571 | 36.1268 | 4630 | -23.81 | 0.11 |  $<$ 0.5 |  $<$ 20.47 |  | — |  | 63
NGC0703 | 28.1650 | 36.1714 | 5459 | -24.66 | 0.14 | 14.9 | 22.06 | C | 8.3 |  | 63
UGC01353 | 28.3457 | 36.9551 | 5144 | -24.19 | 0.08 |  $<$ 0.4 |  $<$ 20.45 |  | — |  | 63
NGC0714 | 28.3735 | 36.2213 | 4330 | -24.43 | 0.08 | 4.0 | 21.28 | C | — |  | 63
CGCG460-045 | 28.6840 | 18.0471 | 4801 | -23.66 | 0.11 | 4.8 | 21.45 | C | 4.1 |  | 4
UGC01396 | 28.9025 | 21.3176 | 4789 | -23.63 | 0.11 | 4.6 | 21.43 | C | — |  | 1
NGC0736 | 29.1703 | 33.0435 | 4257 | -24.92 | 0.08 | 4.0 | 21.27 | C | — |  | 9
CGCG461-014 | 29.5566 | 21.3505 | 4765 | -23.50 | 0.11 | 1.1 | 20.81 | C | — |  | 3
IC0179 | 30.0479 | 38.0214 | 4133 | -24.46 | 0.08 | 3.4 | 21.17 | C | — |  | 2
UGC01503 | 30.3328 | 33.3298 | 4966 | -23.77 | 0.09 | 16.9 | 22.03 | E | — |  | 9
NGC0785 | 30.4167 | 31.8265 | 4862 | -24.48 | 0.11 |  $<$ 0.5 |  $<$ 20.51 |  | — |  | 10
NGC0798 | 30.8317 | 32.0775 | 4964 | -23.93 | 0.11 |  $<$ 0.6 |  $<$ 20.55 |  | — |  | 10
CGCG482-063 | 30.9643 | 25.9253 | 4746 | -24.39 | 0.09 | 2.6 | 21.18 | C | — |  | 6
NGC0804 | 31.0088 | 30.8329 | 5135 | -23.99 | 0.10 | 0.9 | 20.78 | C | — |  | 10
NGC0807 | 31.2319 | 28.9874 | 4638 | -24.82 | 0.13 | 1.4 | 20.89 | C | — |  | 7
UGC01590 | 31.5168 | 29.7930 | 4836 | -24.86 | 0.12 | 25.1 | 22.18 | E | 4.9 |  | 7
UGC01596 | 31.6264 | 29.9931 | 4621 | -23.83 | 0.10 |  $<$ 0.5 |  $<$ 20.45 |  | — |  | 7
UGC01604 | 31.8241 | 37.0967 | 5041 | -24.00 | 0.09 |  $<$ 0.5 |  $<$ 20.49 |  | — |  | 1
NGC0826 | 32.3544 | 30.7397 | 4741 | -23.73 | 0.09 | 3.2 | 21.27 | C | 2.8 |  | 1
UGC01661 | 32.5616 | 41.5218 | 5434 | -24.22 | 0.08 | 0.9 | 20.83 | C | — |  | 3
UGC01757 | 34.3461 | 38.4138 | 5146 | -24.19 | 0.08 | 67.2 | 22.66 | C | 15.8 |  | 2
UGC01786 | 34.8782 | 37.1118 | 6271 | -23.74 | 0.11 |  $<$ 0.5 |  $<$ 20.72 |  | — |  | 1
NGC0904 | 36.0232 | 27.3425 | 5211 | -24.27 | 0.13 |  $<$ 0.6 |  $<$ 20.66 |  | — |  | 1
UGC01859 | 36.1851 | 42.6230 | 5810 | -24.90 | 0.12 | 9.2 | 21.90 | C | 2.5 |  | 54
NGC0909 | 36.3450 | 42.0355 | 4893 | -24.10 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |  | — |  | 54
CGCG539-018 | 36.3656 | 41.8968 | 5277 | -23.61 | 0.09 |  $<$ 0.5 |  $<$ 20.53 |  | — |  | 54
NGC0911 | 36.4267 | 41.9563 | 5660 | -24.77 | 0.10 | 2.8 | 21.36 | C | — |  | 54
UGC01889 | 36.5116 | 30.1732 | 4946 | -23.91 | 0.09 |  $<$ 0.4 |  $<$ 20.45 |  | — |  | 1
UGC01914 | 36.8564 | 41.0599 | 5382 | -24.24 | 0.08 | 2.4 | 21.25 | C | — |  | 54
UGC01939 | 37.0733 | 26.3124 | 5073 | -23.93 | 0.10 | 1.6 | 21.02 | C | — |  | 3
NGC0940 | 37.3646 | 31.6409 | 4989 | -24.99 | 0.09 | 14.4 | 21.96 | C | — |  | 5
NGC0946 | 37.6604 | 42.2322 | 5667 | -24.91 | 0.09 | 13.3 | 22.04 | C | — |  | 54
NGC0953 | 37.7908 | 29.5888 | 4599 | -24.76 | 0.17 | 1.4 | 20.88 | C | — |  | 1
CGCG539-042 | 38.1179 | 41.9443 | 4802 | -23.66 | 0.10 |  $<$ 0.5 |  $<$ 20.45 |  | — |  | 54
NGC0962 | 38.1660 | 28.0699 | 4482 | -24.81 | 0.10 |  $<$ 0.5 |  $<$ 20.40 |  | — |  | 2
UGC02006 | 38.1663 | 42.4287 | 5854 | -23.96 | 0.10 | 2.8 | 21.39 | C | — |  | 54
NGC0968 | 38.5259 | 34.4799 | 3555 | -24.16 | 0.09 |  $<$ 0.4 |  $<$ 20.15 |  | — |  | 3
NGC0969 | 38.5330 | 32.9473 | 4400 | -24.90 | 0.07 | 2.0 | 21.00 | C | — |  | 11
IC1815 | 38.5834 | 32.4294 | 4586 | -24.56 | 0.09 | 0.8 | 20.63 | C | — |  | 11
CGCG539-050 | 38.6078 | 41.1482 | 4927 | -23.65 | 0.08 |  $<$ 0.4 |  $<$ 20.42 |  | — |  | 14
NGC0980 | 38.8273 | 40.9265 | 5623 | -24.48 | 0.08 | 0.9 | 20.86 | C | — |  | 2
UGC02074 | 39.0107 | 42.6141 | 5502 | -24.25 | 0.11 | 2.7 | 21.32 | C | — |  | 2
UGC02073 | 39.0185 | 42.4210 | 5076 | -24.28 | 0.10 |  $<$ 0.5 |  $<$ 20.53 |  | — |  | 1
CGCG484-013 | 39.0635 | 27.1795 | 5206 | -23.81 | 0.10 |  $<$ 0.5 |  $<$ 20.56 |  | — |  | 1
CGCG484-015 | 39.2453 | 25.4429 | 5353 | -24.46 | 0.10 |  $<$ 0.5 |  $<$ 20.58 |  | — |  | 1
NGC0995 | 39.6335 | 41.5293 | 3938 | -23.90 | 0.09 | 3.2 | 21.10 | C | — |  | 14
NGC0996 | 39.6661 | 41.6475 | 4508 | -24.56 | 0.09 | 5.1 | 21.42 | C | — |  | 14
NGC1005 | 39.8653 | 41.4933 | 4240 | -23.66 | 0.09 | 4.2 | 21.29 | C | 8.3 |  | 14
NGC1057 | 40.7620 | 32.4912 | 5642 | -24.40 | 0.12 | 6.6 | 21.73 | C | — |  | 21
NGC1040 | 40.8018 | 41.5006 | 4730 | -24.61 | 0.11 | 3.1 | 21.25 | C | — |  | 14
CGCG505-042 | 40.8873 | 32.2528 | 4803 | -23.89 | 0.11 |  $<$ 0.5 |  $<$ 20.51 |  | — |  | 21
WISEAJ024421.83+312117.1 | 41.0910 | 31.3547 | 5277 | -23.56 | 0.13 |  $<$ 0.7 |  $<$ 20.68 |  | — |  | 21
CGCG147-020 | 111.4052 | 29.9541 | 5775 | -23.71 | 0.16 | 674.5 | 23.76 | E | 118.5 |  | 1
NGC2385 | 112.1170 | 33.8378 | 4318 | -23.62 | 0.10 | 2.2 | 21.02 | C |  $<$ 0.7 |  | 4
IC2194 | 113.4175 | 31.3344 | 4505 | -23.86 | 0.13 |  $<$ 0.7 |  $<$ 20.53 |  |  $<$ 0.7 |  | 5
IC2201 | 114.0701 | 33.1227 | 4783 | -23.68 | 0.13 |  $<$ 0.7 |  $<$ 20.59 |  |  $<$ 2.4 | LI | 2
NGC2444 | 116.7210 | 39.0320 | 4240 | -23.84 | 0.09 |  $<$ 0.5 |  $<$ 20.34 |  |  $<$ 0.7 |  | 2
CGCG206-038 | 118.6036 | 39.3716 | 6131 | -24.21 | 0.08 |  $<$ 0.4 |  $<$ 20.60 |  |  $<$ 0.7 | LI | 1
UGC04085 | 118.8312 | 53.3308 | 7449 | -24.47 | 0.09 | 63.3 | 22.95 | E | 10.1 |  | 2
NGC2476 | 119.1883 | 39.9278 | 3943 | -24.30 | 0.09 | 1.3 | 20.71 | C |  $<$ 0.8 |  | 2
CGCG178-006 | 119.2664 | 33.0832 | 5350 | -24.01 | 0.08 |  $<$ 0.4 |  $<$ 20.48 |  |  $<$ 0.5 | LI | 6
IC2213 | 119.7774 | 27.4641 | 6941 | -24.03 | 0.10 |  $<$ 0.5 |  $<$ 20.78 |  |  $<$ 0.7 |  | 3
CGCG148-108 | 121.1040 | 29.5066 | 5699 | -23.85 | 0.13 |  $<$ 0.6 |  $<$ 20.73 |  |  $<$ 0.7 | — | 1
UGC04209 | 121.3605 | 46.7078 | 6962 | -24.75 | 0.29 |  $<$ 1.4 |  $<$ 21.25 |  |  $<$ 0.7 |  | 3
NGC2518 | 121.8344 | 51.1316 | 5464 | -24.65 | 0.09 |  $<$ 0.4 |  $<$ 20.52 |  |  $<$ 0.7 | — | 1
NGC2524 | 122.0399 | 39.1574 | 4194 | -24.28 | 0.07 |  $<$ 0.3 |  $<$ 20.17 |  |  $<$ 0.7 | — | 2
ARK154 | 122.1122 | 39.9643 | 6455 | -24.32 | 0.07 | 0.9 | 20.98 | C |  $<$ 0.7 |  | 1
NGC2521 | 122.2057 | 57.7696 | 5715 | -24.89 | 0.06 | 2.1 | 21.25 | E |  $<$ 0.9 |  | 1
CGCG178-034 | 122.7789 | 36.5987 | 6591 | -23.58 | 0.09 | 8.8 | 21.99 | C | 2.4 | SF | 1
CGCG149-001 | 122.8229 | 29.5089 | 6164 | -23.74 | 0.09 | 1.9 | 21.27 | C |  $<$ 0.7 | LI | 1
UGC04272 | 123.1979 | 44.3573 | 7111 | -24.22 | 0.11 |  $<$ 0.6 |  $<$ 20.86 |  |  $<$ 0.7 | LI | 1
CGCG207-047 | 123.6252 | 43.1435 | 7084 | -24.33 | 0.09 |  $<$ 0.4 |  $<$ 20.74 |  |  $<$ 0.7 | — | 2
UGC04341 | 125.0412 | 27.0934 | 6119 | -24.71 | 0.15 | 2.1 | 21.30 | C |  $<$ 0.7 | SF | 1
CGCG207-056 | 125.0564 | 44.2303 | 7282 | -24.13 | 0.16 |  $<$ 0.8 |  $<$ 21.02 |  |  $<$ 0.7 |  | 1
UGC04323 | 125.0827 | 66.9820 | 4302 | -24.24 | 0.06 | 4.8 | 21.36 | C | — |  | 2
IC2365 | 126.5753 | 27.8401 | 6251 | -24.38 | 0.14 | 4.5 | 21.65 | C | 1.5 | LI | 1
MCG+10-12-141 | 127.2195 | 58.2039 | 5673 | -23.63 | 0.06 | 15.0 | 22.09 | E |  $<$ 0.7 | SF | 1
CGCG149-037 | 127.3750 | 31.6754 | 5725 | -23.71 | 0.07 | 9.9 | 21.92 | C | 3.1 | SF | 1
CGCG263-043 | 128.1173 | 52.6061 | 5324 | -23.73 | 0.09 | 48.5 | 22.55 | C | 12.6 | SF | 3
CGCG208-015 | 128.3023 | 41.0948 | 7408 | -24.78 | 0.07 |  $<$ 0.3 |  $<$ 20.69 |  |  $<$ 0.7 | — | 8
CGCG311-017 | 130.9709 | 64.9703 | 7132 | -24.52 | 0.07 | 65.6 | 22.93 | E |  $<$3.3 |  | 3
CGCG208-054 | 132.5470 | 40.2557 | 7405 | -24.25 | 0.07 |  $<$ 0.3 |  $<$ 20.68 |  |  $<$ 0.7 | — | 1
IC0522 | 133.6455 | 57.1667 | 5330 | -24.51 | 0.06 |  $<$ 0.3 |  $<$ 20.35 |  |  $<$ 0.7 | — | 1
CGCG311-028 | 135.5786 | 63.8055 | 7444 | -24.19 | 0.06 | 5.7 | 21.91 | C |  $<$ 0.7 | LI | 1
IC2439 | 137.1601 | 32.5929 | 4608 | -23.61 | 0.12 | 5.6 | 21.48 | C | 2.6 | LI | 1
NGC2767 | 137.5495 | 50.4013 | 5200 | -24.10 | 0.06 | 1.0 | 20.84 | C |  $<$ 0.7 | LI | 3
CGCG180-061 | 138.5947 | 36.3158 | 7341 | -23.73 | 0.04 |  $<$ 0.2 |  $<$ 20.42 |  |  $<$ 0.7 | — | 6
UGC04893 | 139.1569 | 30.9054 | 7258 | -23.74 | 0.12 | 1.3 | 21.24 | C |  $<$ 0.7 | LI | 11
CGCG181-008 | 139.5791 | 33.5569 | 7455 | -23.72 | 0.08 |  $<$ 0.4 |  $<$ 20.74 |  |  $<$ 0.7 | LI | 19
CGCG181-022 | 139.9001 | 33.4283 | 7349 | -24.17 | 0.09 |  $<$ 0.4 |  $<$ 20.77 |  |  $<$ 0.7 | LI | 19
NGC2830 | 139.9225 | 33.7380 | 6406 | -24.13 | 0.09 | 18.3 | 22.28 | E |  $<$ 0.7 | Sy | 19
CGCG181-038 | 140.8860 | 33.7550 | 6955 | -23.62 | 0.07 |  $<$ 0.4 |  $<$ 20.65 |  |  $<$ 0.7 | — | 19
CGCG312-008 | 141.2533 | 64.5604 | 5411 | -23.73 | 0.05 | 41.8 | 22.50 | E | 8.5 |  | 1
UGC05026 | 141.6658 | 45.8471 | 4634 | -23.80 | 0.11 | 11.2 | 21.79 | C | 3.0 | Sy | 1
NGC2880 | 142.3941 | 62.4906 | 1927 | -23.59 | 0.06 |  $<$ 0.3 |  $<$ 19.43 |  |  $<$ 0.7 |  | 1
IC2493 | 144.0732 | 37.3640 | 6507 | -24.23 | 0.07 |  $<$ 0.3 |  $<$ 20.55 |  |  $<$ 0.8 | — | 2
UGC05119 | 144.3027 | 38.0923 | 6356 | -24.31 | 0.06 |  $<$ 0.3 |  $<$ 20.49 |  |  $<$ 0.8 | — | 1
UGC05133 | 144.5973 | 43.5092 | 4764 | -23.73 | 0.06 |  $<$ 0.3 |  $<$ 20.20 |  |  $<$ 0.7 | — | 1
IC2500 | 145.5973 | 36.3498 | 6946 | -24.29 | 0.07 |  $<$ 0.3 |  $<$ 20.62 |  |  $<$ 0.8 | — | 5
NGC2950 | 145.6468 | 58.8512 | 1710 | -24.09 | 0.06 | 3.3 | 20.39 | C |  $<$ 0.8 |  | 1
CGCG181-084 | 145.7254 | 36.2141 | 7017 | -23.55 | 0.06 |  $<$ 0.3 |  $<$ 20.58 |  |  $<$ 0.7 | — | 5
NGC2968 | 145.8001 | 31.9288 | 1947 | -23.85 | 0.11 |  $<$ 0.5 |  $<$ 19.72 |  |  $<$ 0.7 | — | 3
NGC2965 | 145.8298 | 36.2478 | 7056 | -24.93 | 0.06 | 56.8 | 22.86 | C | 74.9 | LI | 5
ARK211 | 145.9483 | 42.4736 | 5760 | -23.68 | 0.06 | 0.9 | 20.88 | C |  $<$ 0.6 | — | 4
CGCG210-030 | 145.9967 | 42.4330 | 5416 | -24.10 | 0.05 | 0.7 | 20.72 | C | 2.3 | — | 4
UGC05225 | 146.6191 | 45.7526 | 5239 | -24.00 | 0.05 |  $<$ 0.2 |  $<$ 20.25 |  |  $<$ 0.6 | — | 1
IC2516 | 148.7015 | 37.6869 | 5411 | -23.75 | 0.06 |  $<$ 0.3 |  $<$ 20.38 |  |  $<$ 0.7 | — | 1
CGCG182-041 | 149.0720 | 37.5900 | 7179 | -23.73 | 0.08 |  $<$ 0.4 |  $<$ 20.73 |  |  $<$ 0.7 | LI | 2
NGC3071 | 149.7208 | 31.6203 | 6783 | -23.93 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |  |  $<$ 0.8 | — | 1
IC2530 | 150.3795 | 37.2039 | 6963 | -24.21 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |  |  $<$ 0.7 | — | 1
NGC3116 | 151.6877 | 31.0977 | 6775 | -24.03 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |  |  $<$ 0.7 |  | 3
IC2540 | 151.6947 | 31.4757 | 6949 | -23.85 | 0.08 |  $<$ 0.4 |  $<$ 20.68 |  |  $<$ 0.7 | — | 3
NGC3151 | 153.3713 | 38.6198 | 7244 | -24.13 | 0.07 | 1.6 | 21.33 | C |  $<$ 0.8 | LI | 13
NGC3152 | 153.3922 | 38.8432 | 6769 | -23.79 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |  |  $<$ 0.7 | — | 13
NGC3159 | 153.4701 | 38.6545 | 7164 | -24.60 | 0.07 |  $<$ 0.4 |  $<$ 20.69 |  |  $<$ 0.7 | — | 13
NGC3161 | 153.4967 | 38.6572 | 6650 | -24.02 | 0.08 | 2.1 | 21.38 | C |  $<$ 0.7 | SF | 13
NGC3163 | 153.5297 | 38.6526 | 6625 | -24.93 | 0.07 | 1.5 | 21.23 | C |  $<$ 0.7 |  | 13
CGCG211-030 | 153.6239 | 39.5016 | 7394 | -24.19 | 0.09 |  $<$ 0.4 |  $<$ 20.79 |  |  $<$ 0.7 | LI | 13
CGCG211-031 | 153.6888 | 38.9810 | 7364 | -24.37 | 0.08 | 2.9 | 21.61 | C | 0.6 | SF | 13
CGCG240-029 | 154.8584 | 44.4046 | 7372 | -24.66 | 0.08 | 6.2 | 21.94 | C |  $<$ 0.7 |  | 1
NGC3207 | 155.2524 | 42.9853 | 7365 | -24.63 | 0.08 | 22.9 | 22.50 | E | 2.2 | LI | 3
CGCG183-015 | 155.3769 | 37.7566 | 7022 | -24.02 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |  |  $<$ 0.7 | — | 1
MCG+05-25-004 | 156.1015 | 28.0288 | 6688 | -23.78 | 0.12 |  $<$ 0.6 |  $<$ 20.86 |  |  $<$ 0.7 | Sy | 4
NGC3245 | 156.8266 | 28.5074 | 1755 | -24.20 | 0.09 | 20.1 | 21.20 | C | 6.1 |  | 4
CGCG266-048 | 157.3504 | 55.1867 | 7171 | -24.22 | 0.05 | 4.1 | 21.73 | C |  $<$ 0.7 |  | 1
UGC05953 | 162.8251 | 44.5718 | 3626 | -23.58 | 0.06 | 1.3 | 20.64 | C |  $<$ 0.7 |  | 1
NGC3415 | 162.9275 | 43.7126 | 3739 | -24.31 | 0.05 | 39.9 | 22.16 | E | 13.1 |  | 1
NGC3407 | 163.0742 | 61.3797 | 5381 | -23.87 | 0.09 | 2.3 | 21.23 | C |  $<$ 1.3 | LI | 2
UGC05991 | 163.1985 | 49.6126 | 7160 | -24.39 | 0.06 | 1.5 | 21.29 | C | 1.7 | LI | 5
UGC06013 | 163.4992 | 49.6598 | 6937 | -24.43 | 0.06 | 53.3 | 22.82 | E | 8.3 | LI | 5
CGCG241-034 | 163.6584 | 47.4703 | 7095 | -24.18 | 0.05 |  $<$ 0.3 |  $<$ 20.52 |  |  $<$ 0.7 | — | 1
CGCG241-036 | 163.6793 | 46.5541 | 7093 | -24.37 | 0.05 | 0.9 | 21.06 | C |  $<$ 0.7 | LI | 1
UGC06076 | 165.0401 | 45.9170 | 6806 | -24.49 | 0.05 | 0.5 | 20.77 | C |  $<$ 0.7 | — | 7
UGC06114 | 165.7345 | 50.6593 | 6485 | -24.29 | 0.06 |  $<$ 0.3 |  $<$ 20.50 |  |  $<$ 0.7 | — | 1
CGCG241-068 | 166.0188 | 45.2623 | 6993 | -24.39 | 0.06 |  $<$ 0.3 |  $<$ 20.55 |  |  $<$ 0.7 |  | 7
NGC3540 | 167.3171 | 36.0211 | 6832 | -24.84 | 0.07 |  $<$ 0.3 |  $<$ 20.61 |  |  $<$ 0.7 | — | 1
NGC3595 | 168.8564 | 47.4471 | 2647 | -23.52 | 0.07 |  $<$ 0.4 |  $<$ 19.82 |  |  $<$ 0.7 |  | 2
NGC3613 | 169.6505 | 58.0000 | 2497 | -24.82 | 0.04 | 1.7 | 20.43 | C |  $<$ 0.8 |  | 8
NGC3619 | 169.8400 | 57.7577 | 2021 | -23.79 | 0.05 | 9.7 | 21.01 | E | 2.7 |  | 8
NGC3658 | 170.9928 | 38.5624 | 2537 | -23.73 | 0.07 |  $<$ 0.4 |  $<$ 19.79 |  |  $<$ 0.7 |  | 4
CGCG214-007 | 171.6919 | 39.2662 | 6746 | -24.00 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |  |  $<$ 0.7 | — | 1
CGCG156-085 | 172.3485 | 28.5437 | 7339 | -24.41 | 0.11 | 1.4 | 21.29 | C |  $<$ 0.7 |  | 4
CGCG268-047 | 173.1419 | 54.9266 | 6618 | -24.17 | 0.05 |  $<$ 0.2 |  $<$ 20.44 |  |  $<$ 0.7 | — | 6
NGC3737 | 173.9016 | 54.9486 | 6219 | -24.90 | 0.05 |  $<$ 0.3 |  $<$ 20.40 |  |  $<$ 0.7 | — | 6
NGC3759 | 174.2254 | 54.8232 | 5978 | -24.52 | 0.05 | 21.1 | 22.29 | C | 13.8 |  | 6
NGC3809 | 175.3170 | 59.8858 | 3861 | -24.28 | 0.06 | 35.5 | 22.13 | C | 101.2 |  | 7
CGCG186-038 | 176.3366 | 32.7223 | 6916 | -23.76 | 0.07 |  $<$ 0.3 |  $<$ 20.63 |  |  $<$ 0.6 | LI | 1
IC2967 | 177.7297 | 30.8508 | 7304 | -24.40 | 0.10 |  $<$ 0.5 |  $<$ 20.81 |  |  $<$ 0.7 | — | 1
CGCG186-056 | 177.8552 | 35.2039 | 6979 | -23.61 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |  |  $<$ 0.7 | — | 2
NGC3941 | 178.2307 | 36.9864 | 1291 | -24.07 | 0.06 | 4.3 | 20.26 | C |  $<$ 0.7 |  | 2
NGC3945 | 178.3072 | 60.6756 | 1753 | -24.53 | 0.06 | 7.3 | 20.76 | E | 1.1 |  | 3
NGC3998 | 179.4839 | 55.4535 | 1519 | -24.38 | 0.06 | 307.9 | 22.26 | E | 98.5 |  | 65
NGC4036 | 180.3620 | 61.8957 | 1857 | -24.62 | 0.07 | 47.0 | 21.62 | C | 9.4 |  | 3
NGC4097 | 181.5104 | 36.8636 | 6793 | -24.70 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |  |  $<$ 0.8 | — | 2
IC3022 | 182.5099 | 38.7400 | 6818 | -24.49 | 0.06 | 0.8 | 20.98 | C |  $<$ 0.7 | LI | 6
NGC4148 | 182.5332 | 35.8776 | 5496 | -24.46 | 0.06 | 23.2 | 22.25 | E | 20.9 | LI | 4
KUG1208+386 | 182.6845 | 38.3362 | 7327 | -24.23 | 0.06 | 30.6 | 22.62 | C | 5.9 |  | 6
CGCG187-017 | 182.7147 | 36.6243 | 7364 | -24.56 | 0.06 | 1.4 | 21.29 | C |  $<$ 0.8 | — | 4
NGC4169 | 183.0783 | 29.1793 | 4327 | -24.93 | 0.10 | 11.0 | 21.72 | C | 1.5 |  | 9
CGCG187-025 | 183.5582 | 32.4212 | 6881 | -24.00 | 0.11 |  $<$ 0.6 |  $<$ 20.82 |  |  $<$ 0.7 | — | 2
UGC07243 | 183.5961 | 32.4146 | 7166 | -24.67 | 0.11 |  $<$ 0.6 |  $<$ 20.86 |  |  $<$ 0.7 | SF | 2
NGC4196 | 183.6239 | 28.4235 | 4523 | -24.25 | 0.12 |  $<$ 0.6 |  $<$ 20.51 |  |  $<$ 0.7 | SF | 9
NGC4203 | 183.7710 | 33.1973 | 1634 | -24.49 | 0.10 | 14.3 | 20.99 | C | 7.7 |  | 1
CGCG215-057 | 184.2714 | 42.9480 | 7416 | -23.99 | 0.04 | 1.8 | 21.40 | C |  $<$ 0.7 | LI | 1
NGC4251 | 184.5347 | 28.1753 | 1624 | -24.16 | 0.14 |  $<$ 0.7 |  $<$ 19.67 |  |  $<$ 0.8 |  | 15
NGC4271 | 184.8859 | 56.7366 | 5184 | -24.90 | 0.07 | 2.2 | 21.18 | C |  $<$ 0.7 | LI | 1
CGCG215-065 | 185.2586 | 39.9000 | 7369 | -24.05 | 0.06 |  $<$ 0.3 |  $<$ 20.64 |  |  $<$ 0.8 |  | 1
NGC4358 | 186.0087 | 58.3852 | 4927 | -23.78 | 0.06 | 0.7 | 20.64 | C |  $<$ 0.7 | LI | 4
UGC07635 | 187.4390 | 56.8263 | 5200 | -24.22 | 0.06 | 0.9 | 20.80 | C |  $<$ 0.7 | — | 4
MRK0215 | 188.1447 | 45.7677 | 6471 | -23.75 | 0.06 | 52.3 | 22.75 | C | 10.9 | SF | 1
IC0801 | 188.4374 | 52.2548 | 7045 | -24.87 | 0.06 |  $<$ 0.3 |  $<$ 20.54 |  |  $<$ 0.7 |  | 1
KUG1234+397 | 189.3154 | 39.4832 | 6617 | -23.77 | 0.06 | 5.0 | 21.75 | C |  $<$ 0.7 | LI | 1
NGC4646 | 190.7173 | 54.8560 | 5104 | -24.56 | 0.05 | 5.4 | 21.56 | C | 1.3 | — | 5
NGC4687 | 191.8490 | 35.3521 | 4817 | -23.90 | 0.07 | 16.4 | 21.99 | C | 1.8 | LI | 2
CGCG159-083 | 192.4261 | 26.8920 | 7417 | -24.76 | 0.12 | 3.8 | 21.73 | C |  $<$ 0.7 | SF | 11
NGC4728 | 192.6170 | 27.4349 | 7023 | -24.34 | 0.12 |  $<$ 0.6 |  $<$ 20.87 |  |  $<$ 0.7 | SF | 136
NGC4737 | 192.7205 | 34.1569 | 7443 | -24.66 | 0.07 | 2.5 | 21.55 | C | 3.2 | LI | 1
IC0830 | 192.8188 | 53.6963 | 5328 | -24.26 | 0.05 |  $<$ 0.3 |  $<$ 20.28 |  |  $<$ 0.7 | — | 1
IC0831 | 193.1836 | 26.4704 | 7000 | -24.27 | 0.11 |  $<$ 0.5 |  $<$ 20.83 |  |  $<$ 0.7 | SF | 136
CGCG159-104 | 193.3170 | 27.0945 | 6740 | -24.30 | 0.12 |  $<$ 0.6 |  $<$ 20.86 |  |  $<$ 0.7 | — | 136
NGC4788 | 193.5668 | 27.3037 | 6993 | -24.03 | 0.09 |  $<$ 0.5 |  $<$ 20.77 |  |  $<$ 1.4 | — | 136
IC0834 | 194.0775 | 26.3589 | 7071 | -24.42 | 0.08 | 1.1 | 21.15 | C |  $<$ 0.7 | — | 136
CGCG160-023 | 194.0825 | 27.7511 | 7460 | -23.63 | 0.08 |  $<$ 0.4 |  $<$ 20.77 |  |  $<$ 0.8 | — | 136
CGCG160-027 | 194.1109 | 27.8306 | 6878 | -23.51 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |  |  $<$ 0.7 | — | 136
NGC4828 | 194.1785 | 28.0205 | 6876 | -24.10 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |  |  $<$ 0.7 | — | 136
NGC4840 | 194.3868 | 27.6103 | 6671 | -24.39 | 0.08 | 1.6 | 21.26 | C |  $<$ 0.9 | — | 136
NGC4849 | 194.5527 | 26.3969 | 6475 | -24.87 | 0.08 | 345.4 | 23.57 | E | 20.0 | — | 136
NGC4850 | 194.5910 | 27.9678 | 6605 | -23.90 | 0.08 | 1.8 | 21.30 | C |  $<$ 1.0 | SF | 136
IC3946 | 194.7030 | 27.8103 | 6450 | -23.76 | 0.09 |  $<$ 0.5 |  $<$ 20.69 |  |  $<$ 1.0 | — | 136
IC3960 | 194.7830 | 27.8549 | 7202 | -23.62 | 0.09 | 1.5 | 21.30 | C |  $<$ 1.0 | SF | 136
NGC4864 | 194.8047 | 27.9769 | 7334 | -24.55 | 0.09 | 4.4 | 21.78 | C |  $<$ 0.9 |  | 136
NGC4865 | 194.8327 | 28.0843 | 5286 | -23.96 | 0.07 | 3.9 | 21.45 | C | 2.1 | — | 136
NGC4869 | 194.8473 | 27.9116 | 7437 | -24.58 | 0.09 | 1688.8 | 24.38 | E | 248.0 |  | 136
IC3976 | 194.8724 | 27.8502 | 7443 | -23.69 | 0.09 | 2.0 | 21.45 | C |  $<$ 0.9 | — | 136
NGC4873 | 194.8866 | 27.9836 | 6374 | -23.60 | 0.09 |  $<$ 0.4 |  $<$ 20.67 |  |  $<$ 0.9 | — | 136
IC3991 | 194.9157 | 28.9266 | 6583 | -23.69 | 0.08 |  $<$ 0.4 |  $<$ 20.66 |  |  $<$ 0.5 | — | 136
NGC4876 | 194.9350 | 27.9125 | 7258 | -23.80 | 0.07 |  $<$ 0.4 |  $<$ 20.69 |  |  $<$ 0.8 | — | 136
WISEAJ125957.75+2814 | 194.9906 | 28.2465 | 7290 | -24.75 | 0.09 |  $<$ 0.5 |  $<$ 20.80 |  |  $<$ 0.7 | — | 136
NGC4892 | 195.0147 | 26.8981 | 6492 | -24.27 | 0.08 |  $<$ 0.4 |  $<$ 20.65 |  |  $<$ 0.7 | — | 136
NGC4898 | 195.0737 | 27.9553 | 7481 | -24.53 | 0.07 | 2.7 | 21.59 | C |  $<$ 0.8 |  | 136
NGC4896 | 195.1281 | 28.3463 | 6595 | -24.16 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |  |  $<$ 0.6 | — | 136
IC4042 | 195.1782 | 27.9713 | 6974 | -24.29 | 0.08 | 4.0 | 21.70 | C |  $<$ 0.8 | SF | 136
UGC08122 | 195.2081 | 27.4057 | 7201 | -23.67 | 0.08 |  $<$ 0.4 |  $<$ 20.74 |  |  $<$ 0.7 | — | 136
NGC4908 | 195.2269 | 28.0076 | 5582 | -24.15 | 0.08 |  $<$ 0.4 |  $<$ 20.50 |  |  $<$ 0.8 | — | 136
NGC4923 | 195.3824 | 27.8475 | 6072 | -24.03 | 0.08 |  $<$ 0.4 |  $<$ 20.58 |  |  $<$ 0.7 | — | 136
CGCG160-101 | 195.4459 | 28.0950 | 6402 | -23.66 | 0.08 |  $<$ 0.4 |  $<$ 20.63 |  |  $<$ 0.7 | — | 136
NGC4929 | 195.6851 | 28.0453 | 6796 | -24.19 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |  |  $<$ 0.7 | — | 136
CGCG160-119 | 195.7906 | 28.5835 | 7499 | -23.82 | 0.08 |  $<$ 0.4 |  $<$ 20.74 |  |  $<$ 0.5 | — | 136
NGC4934 | 195.8176 | 28.0304 | 6627 | -23.79 | 0.08 | 1.9 | 21.33 | C |  $<$ 0.7 | SF | 136
IC4133 | 195.9616 | 27.9883 | 6942 | -23.66 | 0.07 |  $<$ 0.4 |  $<$ 20.65 |  |  $<$ 0.7 | — | 136
NGC4956 | 196.2540 | 35.1781 | 5314 | -24.86 | 0.08 |  $<$ 0.4 |  $<$ 20.43 |  |  $<$ 0.8 |  | 1
NGC4971 | 196.7290 | 28.5480 | 6853 | -24.26 | 0.07 |  $<$ 0.4 |  $<$ 20.64 |  |  $<$ 0.5 | — | 136
NGC4987 | 196.9961 | 51.9292 | 5209 | -23.93 | 0.06 |  $<$ 0.3 |  $<$ 20.29 |  |  $<$ 0.7 | — | 2
CGCG271-017 | 197.1755 | 52.0169 | 5215 | -23.96 | 0.06 | 0.3 | 20.32 | C |  $<$ 0.7 | — | 2
CGCG189-038 | 197.9894 | 34.3652 | 5585 | -23.92 | 0.07 | 4.2 | 21.53 | C |  $<$ 0.8 | LI | 1
ARK407 | 198.0330 | 27.3305 | 6741 | -24.09 | 0.09 |  $<$ 0.4 |  $<$ 20.70 |  |  $<$ 1.4 | — | 3
NGC5032B | 198.3570 | 27.7635 | 6762 | -23.54 | 0.07 | 5.0 | 21.77 | C |  $<$ 0.7 | SF | 3
NGC5052 | 198.8952 | 29.6761 | 7212 | -24.57 | 0.13 | 4.6 | 21.79 | C |  $<$ 0.7 | LI | 1
IC4226 | 200.1267 | 32.0039 | 6093 | -23.52 | 0.09 |  $<$ 0.5 |  $<$ 20.64 |  |  $<$ 0.7 | — | 2
NGC5142 | 201.2547 | 36.3996 | 6181 | -24.68 | 0.09 |  $<$ 0.5 |  $<$ 20.65 |  |  $<$ 0.7 | — | 5
NGC5198 | 202.5475 | 46.6708 | 3062 | -24.37 | 0.05 | 2.0 | 20.68 | C | 2.8 |  | 5
NGC5216 | 203.0286 | 62.7008 | 3399 | -23.62 | 0.08 | 8.5 | 21.40 | C | 20.3 | LI | 2
NGC5225 | 203.3339 | 51.4903 | 5115 | -23.80 | 0.06 | 6.4 | 21.63 | E |  $<$ 0.7 | LI | 3
UGC08564 | 203.7406 | 38.4575 | 6799 | -24.79 | 0.06 |  $<$ 0.3 |  $<$ 20.54 |  |  $<$ 0.7 | LI | 1
NGC5250 | 204.0306 | 51.2358 | 5025 | -24.29 | 0.05 | 0.6 | 20.59 | C |  $<$ 0.7 | — | 3
CGCG161-101 | 204.6797 | 31.2706 | 5342 | -23.77 | 0.10 | 1.2 | 20.94 | C |  $<$ 0.7 | LI | 2
CGCG161-102 | 204.7460 | 31.3652 | 5182 | -23.55 | 0.10 |  $<$ 0.5 |  $<$ 20.53 |  |  $<$ 0.7 | — | 2
NGC5283 | 205.2739 | 67.6722 | 3546 | -23.61 | 0.06 | 63.7 | 22.31 | C | 13.2 |  | 1
NGC5308 | 206.7517 | 60.9731 | 2493 | -24.46 | 0.05 |  $<$ 0.3 |  $<$ 19.63 |  |  $<$ 0.8 |  | 8
NGC5311 | 207.2336 | 39.9852 | 3266 | -24.15 | 0.07 | 146.9 | 22.60 | C | 80.3 | LI | 18
NGC5312 | 207.4608 | 33.6217 | 4897 | -23.70 | 0.07 | 9.4 | 21.76 | C | — | LI | 5
CGCG218-055 | 207.5414 | 38.2196 | 6364 | -23.75 | 0.08 | 2.5 | 21.41 | C |  $<$ 0.7 | SF | 1
NGC5318 | 207.6501 | 33.7048 | 4919 | -24.81 | 0.11 | 352.2 | 23.34 | C | 99.7 | LI | 5
UGC08754 | 207.6629 | 35.0382 | 6905 | -24.65 | 0.08 |  $<$ 0.4 |  $<$ 20.66 |  |  $<$ 0.7 | — | 1
NGC5370 | 208.5390 | 60.6780 | 3530 | -23.54 | 0.06 |  $<$ 0.3 |  $<$ 19.97 |  |  $<$ 0.7 | LI | 1
NGC5361 | 208.6467 | 38.4495 | 6212 | -23.56 | 0.07 | 19.3 | 22.28 | E |  $<$ 0.7 |  | 2
UGC08854 | 208.9727 | 37.1965 | 6551 | -24.60 | 0.06 | 1.0 | 21.04 | C |  $<$ 0.7 | — | 1
NGC5380 | 209.2362 | 37.6104 | 3749 | -24.36 | 0.08 |  $<$ 0.4 |  $<$ 20.14 |  |  $<$ 0.6 |  | 9
UGC08923 | 210.0654 | 38.5031 | 5650 | -23.93 | 0.08 | 0.8 | 20.82 | C |  $<$ 0.9 | — | 9
NGC5422 | 210.1752 | 55.1645 | 2366 | -23.94 | 0.05 | 0.3 | 19.63 | C |  $<$ 0.7 |  | 5
NGC5407 | 210.2088 | 39.1562 | 5966 | -24.37 | 0.10 |  $<$ 0.5 |  $<$ 20.65 |  |  $<$ 1.0 | — | 9
CGCG219-044 | 210.3954 | 38.6861 | 6218 | -24.27 | 0.08 | 1.7 | 21.23 | C |  $<$ 0.9 |  | 9
NGC5473 | 211.1801 | 54.8926 | 2548 | -24.50 | 0.05 | 0.3 | 19.70 | C |  $<$ 0.7 |  | 5
NGC5485 | 211.7972 | 55.0016 | 2455 | -24.38 | 0.05 | 4.5 | 20.84 | C |  $<$ 0.8 | — | 5
NGC5580 | 215.4100 | 35.2049 | 3795 | -24.08 | 0.09 |  $<$ 0.5 |  $<$ 20.23 |  |  $<$ 0.7 |  | 3
NGC5598 | 215.6179 | 40.3198 | 6026 | -24.71 | 0.15 |  $<$ 0.8 |  $<$ 20.85 |  |  $<$ 0.7 | — | 5
NGC5603 | 215.7563 | 40.3773 | 6221 | -24.82 | 0.13 | 3.0 | 21.47 | C | 1.5 | SF | 5
UGC09223 | 215.9370 | 40.0238 | 5789 | -24.35 | 0.15 |  $<$ 0.8 |  $<$ 20.81 |  |  $<$ 0.7 | SF | 5
NGC5631 | 216.6387 | 56.5826 | 2465 | -24.33 | 0.06 | 3.3 | 20.71 | C |  $<$ 0.7 |  | 1
UGC09284 | 217.0974 | 33.2537 | 4753 | -23.52 | 0.08 | 2.9 | 21.23 | C |  $<$ 0.7 | SF | 1
NGC5642 | 217.3062 | 30.0264 | 4916 | -24.95 | 0.09 |  $<$ 0.5 |  $<$ 20.45 |  |  $<$ 0.7 |  | 1
NGC5687 | 218.7183 | 54.4757 | 2669 | -24.01 | 0.06 |  $<$ 0.3 |  $<$ 19.75 |  |  $<$ 0.7 |  | 1
NGC5684 | 218.9590 | 36.5432 | 4668 | -24.46 | 0.06 | 7.6 | 21.63 | C | 4.6 | LI | 7
CGCG220-034 | 219.1776 | 39.9436 | 6563 | -23.94 | 0.08 | 13.9 | 22.19 | C | 1.8 | LI | 1
CGCG318-001 | 219.5392 | 66.3380 | 7100 | -24.29 | 0.09 | 10.2 | 22.12 | C | — |  | 1
UGC09473 | 220.3874 | 38.8514 | 5268 | -24.56 | 0.07 | 23.9 | 22.23 | E | 3.2 | SF | 1
NGC5771 | 223.0597 | 29.8454 | 7463 | -24.41 | 0.08 |  $<$ 0.4 |  $<$ 20.75 |  |  $<$ 0.8 | — | 2
NGC5820 | 224.6659 | 53.8861 | 3843 | -24.62 | 0.07 | 1.3 | 20.69 | C |  $<$ 0.7 |  | 2
UGC09641 | 224.7622 | 41.4468 | 5468 | -23.94 | 0.07 |  $<$ 0.3 |  $<$ 20.40 |  |  $<$ 0.8 | — | 1
NGC5860 | 226.6400 | 42.6403 | 5958 | -23.93 | 0.08 | 34.9 | 22.50 | C | 6.8 | SF | 1
NGC5943 | 232.4338 | 42.7779 | 6204 | -24.98 | 0.06 | 6.4 | 21.80 | C | 2.1 | LI | 5
CGCG222-025 | 233.3049 | 41.0766 | 6161 | -23.89 | 0.07 |  $<$ 0.3 |  $<$ 20.53 |  |  $<$ 0.7 | — | 2
NGC5966 | 233.9671 | 39.7689 | 5034 | -24.67 | 0.08 | 4.2 | 21.44 | C | 3.0 | LI | 1
CGCG194-013 | 234.6603 | 36.9583 | 6150 | -24.01 | 0.09 | 18.4 | 22.25 | C | 2.8 | SF | 1
CGCG166-067 | 238.5479 | 30.1559 | 6605 | -23.63 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |  |  $<$ 0.7 | — | 1
CGCG250-023 | 239.0321 | 48.0932 | 6291 | -24.03 | 0.06 |  $<$ 0.3 |  $<$ 20.48 |  |  $<$ 0.7 | — | 8
IC1152 | 239.1805 | 48.0950 | 6370 | -24.94 | 0.06 | 1.1 | 21.06 | C |  $<$ 0.7 | — | 8
UGC10118 | 239.6678 | 48.6824 | 6494 | -24.46 | 0.06 |  $<$ 0.3 |  $<$ 20.50 |  |  $<$ 0.7 | — | 8
IC1214 | 244.0488 | 65.9688 | 7364 | -24.76 | 0.09 |  $<$ 0.4 |  $<$ 20.78 |  | — |  | 1
NGC6187 | 247.9033 | 57.7067 | 5899 | -23.69 | 0.06 |  $<$ 0.3 |  $<$ 20.42 |  |  $<$ 0.8 |  | 1
NGC6198 | 248.8777 | 57.4868 | 5716 | -23.61 | 0.05 | 0.9 | 20.88 | C | 1.3 |  | 4
UGC10486 | 249.3930 | 50.3455 | 6537 | -24.82 | 0.06 | 0.4 | 20.64 | C |  $<$ 0.8 |  | 1
NGC6206 | 250.0329 | 58.6174 | 5927 | -24.26 | 0.07 |  $<$ 0.3 |  $<$ 20.48 |  |  $<$ 0.7 |  | 1
NGC6211 | 250.3652 | 57.7836 | 5693 | -24.92 | 0.06 | 103.6 | 22.94 | E | 50.3 |  | 4
CGCG251-041 | 250.7894 | 45.8458 | 5782 | -23.67 | 0.07 | 2.0 | 21.23 | C |  $<$ 0.6 | LI | 2
CGCG299-027 | 251.5536 | 62.2301 | 6048 | -23.59 | 0.07 |  $<$ 0.3 |  $<$ 20.49 |  |  $<$ 0.7 |  | 9
NGC6291 | 255.2330 | 58.9375 | 5596 | -23.67 | 0.09 |  $<$ 0.4 |  $<$ 20.56 |  |  $<$ 0.8 |  | 5
CGCG226-037 | 265.1584 | 41.3014 | 5805 | -23.74 | 0.09 |  $<$ 0.5 |  $<$ 20.60 |  | — |  | 1
CGCG171-025 | 268.7725 | 28.9595 | 7225 | -24.11 | 0.19 |  $<$ 1.0 |  $<$ 21.11 |  | — |  | 4
NGC6518 | 269.9323 | 28.8667 | 7189 | -24.87 | 0.24 |  $<$ 1.2 |  $<$ 21.20 |  | — |  | 8
CGCG254-009 | 270.4529 | 45.3105 | 6206 | -23.72 | 0.08 |  $<$ 0.4 |  $<$ 20.61 |  | — |  | 1
CGCG171-048 | 270.7378 | 29.3107 | 7420 | -24.57 | 0.23 | 11.9 | 22.23 | C | 4.7 |  | 8
ARK538 | 273.7654 | 29.7697 | 6146 | -23.82 | 0.19 | 43.4 | 22.62 | C | 10.6 |  | 1
CGCG227-023 | 274.4821 | 41.3557 | 6259 | -23.70 | 0.17 |  $<$ 0.9 |  $<$ 20.94 |  | — |  | 1
UGC11228 | 276.1928 | 41.4927 | 6167 | -24.84 | 0.15 | 9.8 | 21.98 | C | 3.5 |  | 1
UGC11233 | 276.4343 | 32.1788 | 7212 | -24.69 | 0.13 |  $<$ 0.6 |  $<$ 20.92 |  | — |  | 2
IC4772 | 279.9854 | 40.0264 | 7470 | -24.35 | 0.41 |  $<$ 2.0 |  $<$ 21.47 |  | — |  | 4
NGC6686 | 280.0292 | 40.1376 | 7430 | -24.56 | 0.41 | 4.0 | 21.75 | C | — |  | 4
CGCG228-027 | 281.2488 | 42.7197 | 6941 | -23.95 | 0.14 |  $<$ 0.7 |  $<$ 20.93 |  | — |  | 1
CGCG228-030 | 281.5922 | 40.5821 | 6941 | -24.42 | 0.34 | 6.9 | 21.93 | C | 3.0 |  | 1
CGCG493-015 | 329.2996 | 30.7303 | 7107 | -24.55 | 0.11 | 1.3 | 21.23 | C | — |  | 1
UGC11903 | 331.3274 | 34.9892 | 4890 | -23.75 | 0.09 |  $<$ 0.4 |  $<$ 20.44 |  | — |  | 1
CGCG513-017 | 333.4549 | 37.0267 | 6334 | -24.51 | 0.15 | 15.5 | 22.20 | E | 3.0 |  | 17
WISEAJ221408.43+365115.7 | 333.5352 | 36.8544 | 6101 | -24.14 | 0.10 |  $<$ 0.5 |  $<$ 20.69 |  | — |  | 17
NGC7240 | 333.8440 | 37.2807 | 6051 | -24.52 | 0.13 |  $<$ 0.7 |  $<$ 20.80 |  | — |  | 17
WISEAJ221534.77+371106.7 | 333.8949 | 37.1853 | 5328 | -23.59 | 0.13 | 0.8 | 20.77 | C | — |  | 17
IC5193 | 333.9314 | 37.2429 | 5661 | -24.21 | 0.13 |  $<$ 0.6 |  $<$ 20.71 |  | — |  | 17
UGC11990 | 335.1254 | 35.9736 | 5895 | -24.60 | 0.10 |  $<$ 0.5 |  $<$ 20.65 |  | — |  | 26
CGCG494-019 | 335.7883 | 32.1487 | 6531 | -24.18 | 0.09 |  $<$ 0.5 |  $<$ 20.70 |  | — |  | 4
NGC7273 | 336.0384 | 36.1998 | 5144 | -24.61 | 0.12 | 3.2 | 21.34 | C | — |  | 26
NGC7276 | 336.0598 | 36.0875 | 6033 | -24.52 | 0.11 | 84.5 | 22.90 | E |  $<$4.1 |  | 26
CGCG514-029 | 336.5029 | 35.9537 | 6184 | -24.42 | 0.13 | 1.0 | 20.99 | C | — |  | 26
UGC12040 | 336.7741 | 36.3616 | 6435 | -24.93 | 0.16 | 24.2 | 22.41 | C | 7.0 |  | 26
CGCG514-036 | 337.1428 | 33.9992 | 6132 | -24.48 | 0.19 |  $<$ 0.9 |  $<$ 20.96 |  | — |  | 1
WISEAJ222843.62+362955.8 | 337.1817 | 36.4989 | 7338 | -24.54 | 0.16 | 3.8 | 21.72 | C | — |  | 6
CGCG514-041 | 337.4832 | 36.2613 | 7149 | -24.43 | 0.16 |  $<$ 0.8 |  $<$ 21.03 |  | — |  | 6
NGC7317 | 338.9662 | 33.9449 | 6621 | -24.36 | 0.12 |  $<$ 0.6 |  $<$ 20.84 |  | — |  | 22
NGC7332 | 339.3522 | 23.7983 | 1383 | -23.53 | 0.16 | 2.7 | 20.12 | C | — |  | 2
UGC12121 | 339.4184 | 34.8465 | 6954 | -24.64 | 0.13 |  $<$ 0.6 |  $<$ 20.90 |  | — |  | 22
NGC7340 | 339.4342 | 34.4100 | 6424 | -24.76 | 0.11 |  $<$ 0.6 |  $<$ 20.77 |  | — |  | 22
CGCG514-079 | 339.6269 | 34.2406 | 6030 | -24.38 | 0.10 | 28.9 | 22.43 | C | 9.1 |  | 22
CGCG495-013 | 340.3148 | 33.6237 | 6575 | -23.84 | 0.22 |  $<$ 1.1 |  $<$ 21.09 |  | — |  | 22
CGCG514-094 | 340.3452 | 34.6217 | 6854 | -24.55 | 0.08 | 3.5 | 21.62 | C | — |  | 22
MRK0918 | 340.5420 | 35.9276 | 7259 | -24.31 | 0.11 |  $<$ 0.6 |  $<$ 20.88 |  | — |  | 1
CGCG495-033 | 342.3888 | 32.3674 | 6495 | -24.09 | 0.09 |  $<$ 0.4 |  $<$ 20.68 |  | — |  | 18
NGC7395 | 342.7621 | 37.0879 | 5700 | -24.85 | 0.18 |  $<$ 0.9 |  $<$ 20.86 |  | — |  | 6
ARK566 | 342.7647 | 31.3744 | 7057 | -23.91 | 0.09 |  $<$ 0.4 |  $<$ 20.76 |  | — |  | 18
CGCG515-010 | 343.3530 | 37.1753 | 5691 | -24.45 | 0.12 |  $<$ 0.6 |  $<$ 20.70 |  | — |  | 6
UGC12235 | 343.5175 | 32.3734 | 6666 | -24.26 | 0.09 | 4.7 | 21.73 | C | — |  | 18
NGC7411 | 343.6455 | 20.2362 | 6810 | -24.76 | 0.28 | 19.9 | 22.37 | C | 21.8 |  | 2
CGCG496-020 | 343.7761 | 32.1847 | 6533 | -24.27 | 0.10 | 4.3 | 21.67 | C | — |  | 18
CGCG496-031 | 345.1618 | 30.7418 | 6296 | -24.32 | 0.09 |  $<$ 0.4 |  $<$ 20.65 |  | — |  | 1
NGC7454 | 345.2772 | 16.3884 | 2122 | -23.63 | 0.18 |  $<$ 0.9 |  $<$ 20.01 |  | — |  | 5
NGC7473 | 345.9879 | 30.1602 | 6929 | -24.63 | 0.08 |  $<$ 0.4 |  $<$ 20.71 |  | — |  | 1
UGC12356 | 346.4541 | 31.0872 | 6886 | -24.91 | 0.09 |  $<$ 0.5 |  $<$ 20.75 |  | — |  | 2
NGC7485 | 346.5202 | 34.1077 | 5707 | -24.82 | 0.11 | 104.7 | 22.94 | C | 128.3 |  | 2
CGCG475-041 | 347.5689 | 26.6210 | 7417 | -24.30 | 0.17 | 1.6 | 21.35 | C | — |  | 1
NGC7516 | 348.2161 | 20.2484 | 4980 | -24.53 | 0.12 |  $<$ 0.6 |  $<$ 20.59 |  | — |  | 1
CGCG496-062 | 348.5978 | 28.4445 | 6864 | -24.29 | 0.15 |  $<$ 0.8 |  $<$ 20.96 |  | — |  | 14
CGCG496-077 | 349.4413 | 29.0272 | 6420 | -23.98 | 0.14 |  $<$ 0.7 |  $<$ 20.86 |  | — |  | 14
CGCG496-078 | 349.5641 | 29.2306 | 6678 | -24.81 | 0.15 | 6.1 | 21.84 | C | — |  | 14
WISEAJ231854.65+290123.5 | 349.7277 | 29.0232 | 7226 | -24.19 | 0.11 |  $<$ 0.6 |  $<$ 20.88 |  | — |  | 14
WISEAJ232001.11+271247.8 | 350.0046 | 27.2133 | 5565 | -23.78 | 0.11 |  $<$ 0.5 |  $<$ 20.63 |  | — |  | 1
NGC7628 | 350.2287 | 25.8986 | 4176 | -24.20 | 0.11 | 2.1 | 20.97 | C | — |  | 2
IC5315 | 350.3260 | 25.3854 | 4435 | -23.55 | 0.10 | 3.3 | 21.22 | C | — |  | 2
CGCG497-012 | 350.8932 | 29.1824 | 6193 | -24.32 | 0.13 | 19.7 | 22.29 | C | 2.1 |  | 5
CGCG454-072 | 352.1258 | 17.2779 | 7251 | -24.33 | 0.13 |  $<$ 0.6 |  $<$ 20.93 |  | — |  | 4
CGCG497-026 | 352.2046 | 29.7353 | 5555 | -24.17 | 0.10 | 1.3 | 21.01 | C | — |  | 2
UGC12636 | 352.5797 | 27.1337 | 7261 | -23.85 | 0.10 |  $<$ 0.5 |  $<$ 20.81 |  | — |  | 1
UGC12655 | 353.1211 | 23.9311 | 5140 | -24.59 | 0.09 | 24.2 | 22.21 | E | 5.8 |  | 1
UGC12657 | 353.1812 | 29.4607 | 5557 | -24.71 | 0.10 | 1.3 | 21.01 | C | — |  | 1
NGC7698 | 353.5065 | 24.9446 | 6951 | -24.95 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |  | — |  | 1
CGCG497-046 | 354.7851 | 32.0856 | 5105 | -24.75 | 0.12 |  $<$ 0.6 |  $<$ 20.60 |  | — |  | 3
WISEAJ233932.46+285506.2 | 354.8853 | 28.9183 | 6460 | -24.13 | 0.09 |  $<$ 0.4 |  $<$ 20.66 |  | — |  | 1
CGCG498-007 | 356.2788 | 28.2055 | 6919 | -24.58 | 0.09 | 13.4 | 22.22 | C | 3.5 |  | 12
NGC7760 | 357.2997 | 30.9832 | 5203 | -24.54 | 0.08 |  $<$ 0.4 |  $<$ 20.46 |  | — |  | 1
UGC12835 | 358.4864 | 28.4927 | 6810 | -24.92 | 0.09 | 1.7 | 21.31 | C | — |  | 9
UGC12840 | 358.6246 | 28.8715 | 6765 | -24.53 | 0.12 |  $<$ 0.6 |  $<$ 20.85 |  | — |  | 9

Column description: (1) name, (2 and 3) right ascension and declination, (4)
recession velocity ($\rm{\,km\,s}^{-1}$), (5) K-band absolute magnitude, (6)
r.m.s. noise of the LOFAR image (mJy beam-1), (7 and 8) flux density (mJy) and
luminosity (W Hz-1) at 150 MHz from LOFAR, (9) radio morphology (C=compact,
E=extended), (10) 1.4 GHz flux density (mJy) from FIRST or from NVSS when the
FIRST measurement is not available, or not reliable, the long dash represents
a source undetected in the NVSS at a typical limit of 2 mJy), (11) SDSS
spectrum available and optical spectral classification: Sy = Seyfert, LI =
LINER, SF = star forming, — = unclassified, (12) number of 2MASS group
members.

##  Appendix B Images and notes on the radio morphology of the extended
sources.

Figure 13: LOFAR images at 150 MHz of the 31 galaxies showing extended
emission. The lowest contour is drawn at three times the local r.m.s., as
reported in Table LABEL:tab.

Figure 13: (continued)

Figure 13: (continued)

We present here the images and a description of the properties of the 31 mETGs
with extended radio emission, that is, those in which the 3$\sigma$ level
isophote extends to a radius of at least 15″(about twice the beam FWHM).

CGCG 499-084. Two diffuse tails of emission, extending for $\sim$ 180 kpc, are
suggestive of the presence of jets. This source has a rather steep spectral
slope ($\alpha_{150}^{1400}$=1.14), and we consider it candidate restarted
source.

CGCG 536-006. Radio emission aligned with the optical axis.

UGC 00724. Diffuse and elongated emission.

UGC 01022. Diffuse source. Possible remnant.

NGC 0670. Cospatial radio and optical emission.

UGC 01503. Ring-like structure. Possible remnant source.

UGC 01590. Possible one-sided jet.

UGC 04085. Radio emission aligned with the optical axis.

CGCG 147-020. Possible two-sided jetted source.

NGC 2521. Diffuse radio structure. Possible remnant source.

MCG +10-12-141. Unclear radio structure.

CGCG 311-017. Diffuse radio source with a steep spectral index
($\alpha_{150,1400}>1.34$): We consider it candidate remnant source.

NGC 2830. Cospatial radio and optical emission.

CGCG 312-008. Radio emission aligned with the optical axis.

NGC 3207. Two-sided jetted source.

NGC 3415. Cospatial radio and optical emission.

UGC 06013. Cospatial radio and optical emission.

NGC 3619. Four nearby galaxies cause the radio emission to appear extended.

NGC 3945. Possible two-sided jetted source.

NGC 3998. Two-sided jetted source.

NGC 4148. The central emission has a double structure, with the secondary
compact source cospatial with a fainter galaxy located $\sim 12$″ north. The
extended lobes appear to originate from this secondary radio galaxy.

NGC 4849. Possible two-sided jetted source.

NGC 4869. Narrow-angle tail jetted source.

NGC 5225. Unclear radio structure.

NGC 5361. Cospatial radio and optical emission.

UGC 09473. Unclear radio structure.

NGC 6211. Possible one-sided jetted source.

CGCG 513-017. Radio emission aligned with the optical axis.

NGC 7276. Diffuse radio source with a steep spectral index
($\alpha_{150,1400}>1.35$): We consider it candidate remnant source.

UGC 12655. Radio emission aligned with the optical axis.

NGC 7836. Radio emission aligned with the optical axis.

##  Appendix C Environment of the gETG sample.

Table 3: Number of group members for the gETGs. Name | $N_{\rm mb}$ | Name | $N_{\rm mb}$ | Name | $N_{\rm mb}$ | Name | $N_{\rm mb}$ | Name | $N_{\rm mb}$ | Name | $N_{\rm mb}$
---|---|---|---|---|---|---|---|---|---|---|---
NGC0057 | 6 | UGC01841 | 54 | CGCG286-070 | 7 | NGC3816 | 61 | NGC4978 | 1 | IC5180 | 14
NGC0068 | 21 | NGC0910 | 54 | UGC04051 | 9 | NGC3837 | 61 | IC0858 | 3 | UGC11950 | 14
NGC0071 | 21 | UGC01930 | 2 | UGC04052 | 9 | NGC3842 | 61 | IC0885 | 2 | NGC7242 | 17
NGC0076 | 21 | NGC0940 | 5 | CGCG310-022 | 4 | NGC3862 | 61 | NGC5127 | 3 | NGC7248 | 14
NGC0080 | 18 | NGC0978A | 11 | NGC2475 | 1 | NGC3886 | 61 | NGC5141 | 5 | NGC7265 | 26
NGC0083 | 18 | NGC1004 | 16 | NGC2492 | 3 | NGC3894 | 7 | NGC5322 | 8 | NGC7274 | 26
NGC0128 | 5 | NGC1016 | 16 | NGC2493 | 2 | NGC3919 | 18 | NGC5332 | 1 | NGC7315 | 22
NGC0194 | 16 | NGC1044 | 8 | UGC04420 | 2 | UGC06846 | 5 | NGC5444 | 6 | NGC7318 | 22
NGC0315 | 14 | NGC1060 | 21 | NGC2639 | 2 | NGC3937 | 18 | NGC5490 | 8 | NGC7330 | 3
NGC0379 | 48 | NGC1066 | 21 | IC2393 | 2 | NGC3940 | 18 | NGC5513 | 3 | NGC7335 | 22
NGC0383 | 48 | UGC02249 | 5 | NGC2672 | 5 | NGC3971 | 2 | NGC5525 | 1 | UGC12179 | 22
NGC0393 | 4 | UGC02309 | 5 | NGC2693 | 6 | NGC4008 | 4 | NGC5557 | 4 | NGC7386 | 10
NGC0410 | 48 | NGC1129 | 46 | NGC2749 | 3 | NGC4065 | 30 | NGC5784 | 3 | UGC12214 | 18
NGC0467 | 1 | NGC1167 | 4 | UGC04767 | 1 | UGC07115 | 14 | IC4562 | 7 | UGC12242 | 18
NGC0499 | 47 | NGC1175 | 180 | UGC04775 | 3 | NGC4125 | 7 | NGC5982 | 5 | NGC7426 | 6
NGC0507 | 47 | UGC02528 | 180 | NGC2759 | 7 | UGC07132 | 2 | UGC10097 | 8 | NGC7436B | 9
NGC0524 | 9 | NGC1226 | 7 | NGC2783 | 11 | NGC4213 | 6 | IC1153 | 8 | NGC7512 | 7
NGC0533 | 8 | WISE0322+09 | 4 | NGC2789 | 11 | NGC4227 | 2 | IC1211 | 1 | UGC12444 | 7
NGC0529 | 47 | CGCG416-007 | 2 | NGC2832 | 19 | NGC4229 | 2 | NGC6125 | 3 | NGC7539 | 2
NGC0679 | 63 | WISE0348+33 | 2 | UGC04972 | 19 | IC0780 | 3 | NGC6364 | 1 | NGC7550 | 4
NGC0687 | 63 | UGC02902 | 2 | UGC04974 | 19 | NGC4335 | 4 | NGC6375 | 3 | UGC12482 | 14
UGC01308 | 63 | NGC1508 | 2 | NGC2892 | 4 | NGC4555 | 12 | UGC10918 | 3 | NGC7660 | 2
UGC01332 | 14 | MCG+05-10-007 | 17 | NGC2918 | 2 | NGC4583 | 2 | NGC6515 | 1 | NGC7680 | 11
NGC0708 | 63 | IC0359 | 4 | NGC3158 | 13 | M60 | 197 | NGC6524 | 1 | NGC7681 | 4
NGC0712 | 63 | NGC1539 | 1 | NGC3222 | 1 | NGC4673 | 11 | NGC6575 | 1 | NGC7722 | 4
IC0171 | 63 | NGC1587 | 6 | NGC3234 | 4 | NGC4715 | 136 | NGC6619 | 1 | NGC7777 | 9
UGC01389 | 14 | NGC1671 | 1 | NGC3598 | 1 | NGC4816 | 136 | NGC6623 | 2 | UGC12839 | 9
UGC01418 | 1 | NGC2256 | 10 | NGC3615 | 3 | NGC4841A | 136 | NGC6628 | 2 | NGC7785 | 1
NGC0750 | 9 | NGC2274 | 6 | NGC3665 | 4 | NGC4886 | 136 | NGC6688 | 3 |  |
NGC0759 | 63 | NGC2258 | 3 | NGC3710 | 1 | NGC4914 | 2 | NGC6702 | 1 |  |
NGC0777 | 10 | UGC03894 | 4 | NGC3713 | 4 | NGC4952 | 136 | UGC11465 | 8 |  |
NGC0890 | 1 | IC2196 | 5 | NGC3805 | 61 | NGC4957 | 136 | UGC11892 | 2 |  |

##  Appendix D Properties of the lmETG sample

Table 4: Radio properties of the lmETG sample Name | R.A. | DEC. | v | MK | rms | F150 | L150 |
---|---|---|---|---|---|---|---|---
NGC7805 | 0.3616 | 31.4337 | 4766 | -24.10 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |
NGC0005 | 1.9537 | 35.3623 | 5062 | -23.74 | 0.17 |  $<$ 0.8 |  $<$ 20.73 |
NGC7836 | 2.0068 | 33.0707 | 4854 | -24.00 | 0.09 | 43.0 $\pm$ 0.3 | 22.41 | E
NGC0016 | 2.2679 | 27.7294 | 3097 | -24.52 | 0.13 |  $<$ 0.7 |  $<$ 20.21 |
NGC0006 | 2.3862 | 33.3087 | 4919 | -24.88 | 0.08 | 4.7 $\pm$ 0.5 | 21.46 | P
NGC0042 | 3.2348 | 22.1003 | 5876 | -24.58 | 0.10 | 1.9 $\pm$ 0.0 | 21.23 | P
NGC0043 | 3.2531 | 30.9153 | 4728 | -24.78 | 0.10 |  $<$ 0.5 |  $<$ 20.44 |
UGC00130 | 3.4872 | 30.8830 | 4724 | -23.62 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |
CGCG499-084 | 3.5528 | 28.5451 | 7023 | -24.11 | 0.10 | 122.9 $\pm$ 0.3 | 23.19 | E
CGCG478-044 | 3.5536 | 22.7665 | 6064 | -23.92 | 0.10 |  $<$ 0.5 |  $<$ 20.67 |
CGCG499-087 | 3.8068 | 31.5009 | 6551 | -24.14 | 0.11 |  $<$ 0.6 |  $<$ 20.79 |
UGC00146 | 3.9329 | 27.4444 | 7356 | -24.64 | 0.16 |  $<$ 0.8 |  $<$ 21.03 |
ARK003 | 3.9691 | 19.7743 | 6353 | -23.86 | 0.10 |  $<$ 0.5 |  $<$ 20.73 |
CGCG499-098 | 4.2610 | 29.9424 | 6818 | -24.33 | 0.09 |  $<$ 0.4 |  $<$ 20.73 |
CGCG499-102 | 4.4959 | 29.4697 | 6751 | -24.30 | 0.08 |  $<$ 0.4 |  $<$ 20.68 |
NGC0072A | 4.6431 | 30.0363 | 6606 | -23.64 | 0.09 |  $<$ 0.5 |  $<$ 20.71 |
IC1541 | 5.0081 | 21.9997 | 5815 | -23.74 | 0.08 |  $<$ 0.4 |  $<$ 20.56 |
CGCG457-008 | 5.2157 | 21.5366 | 5814 | -23.76 | 0.09 |  $<$ 0.5 |  $<$ 20.60 |
NGC0079 | 5.2619 | 22.5665 | 5385 | -24.25 | 0.09 |  $<$ 0.4 |  $<$ 20.51 |
NGC0085 | 5.3565 | 22.5117 | 6087 | -23.84 | 0.10 |  $<$ 0.5 |  $<$ 20.69 |
NGC0086 | 5.3690 | 22.5564 | 5488 | -23.55 | 0.09 |  $<$ 0.4 |  $<$ 20.54 |
IC1548 | 5.4799 | 22.0064 | 5638 | -23.55 | 0.09 | 0.9 $\pm$ 0.0 | 20.87 | P
CGCG500-007 | 5.5668 | 30.2474 | 6334 | -23.72 | 0.08 |  $<$ 0.4 |  $<$ 20.61 |
NGC0096 | 5.5738 | 22.5462 | 6068 | -23.78 | 0.09 | 0.9 $\pm$ 0.2 | 20.93 | P
NGC0097 | 5.6250 | 29.7453 | 4698 | -24.68 | 0.09 |  $<$ 0.4 |  $<$ 20.39 |
IC1550 | 6.1152 | 38.1856 | 5834 | -24.32 | 0.08 |  $<$ 0.4 |  $<$ 20.53 |
UGC00330 | 8.4243 | 39.5448 | 5793 | -24.05 | 0.12 |  $<$ 0.6 |  $<$ 20.71 |
UGC00375 | 9.4328 | 25.6402 | 7235 | -24.57 | 0.09 |  $<$ 0.4 |  $<$ 20.77 |
NGC0183 | 9.6225 | 29.5112 | 5303 | -24.74 | 0.10 | 1.5 $\pm$ 0.4 | 21.03 | P
UGC00411 | 9.8733 | 25.6434 | 4586 | -23.75 | 0.10 |  $<$ 0.5 |  $<$ 20.41 |
CGCG500-074 | 10.6996 | 29.9224 | 4997 | -23.98 | 0.10 |  $<$ 0.5 |  $<$ 20.48 |
NGC0229 | 10.7694 | 23.5091 | 7192 | -24.39 | 0.12 |  $<$ 0.6 |  $<$ 20.89 |
NGC0233 | 10.9023 | 30.5870 | 5322 | -24.86 | 0.09 |  $<$ 0.5 |  $<$ 20.52 |
CGCG479-065 | 10.9250 | 23.4763 | 7082 | -24.22 | 0.11 | 1.6 $\pm$ 0.0 | 21.31 | P
CGCG500-080 | 11.0328 | 30.3509 | 5484 | -23.64 | 0.11 |  $<$ 0.6 |  $<$ 20.64 |
NGC0243 | 11.5036 | 29.9595 | 4700 | -23.80 | 0.09 | 2.8 $\pm$ 0.7 | 21.20 | P
IC1583 | 11.7929 | 23.0738 | 7108 | -24.11 | 0.09 |  $<$ 0.5 |  $<$ 20.78 |
IC1585 | 11.8095 | 23.0535 | 7183 | -24.30 | 0.09 | 1.2 $\pm$ 0.0 | 21.20 | P
CGCG501-018 | 12.0361 | 28.6139 | 6899 | -24.12 | 0.08 |  $<$ 0.4 |  $<$ 20.70 |
NGC0262 | 12.1964 | 31.9570 | 4432 | -23.99 | 0.15 | 753.0 $\pm$ 0.3 | 23.58 | P
UGC00506 | 12.4120 | 22.9323 | 7296 | -24.96 | 0.09 |  $<$ 0.4 |  $<$ 20.76 |
NGC0282 | 13.1756 | 30.6391 | 6538 | -24.75 | 0.10 |  $<$ 0.5 |  $<$ 20.72 |
NGC0287 | 13.3679 | 32.4823 | 5407 | -24.03 | 0.07 |  $<$ 0.4 |  $<$ 20.44 |
CGCG501-034 | 13.3962 | 31.4197 | 5359 | -23.70 | 0.14 |  $<$ 0.7 |  $<$ 20.71 |
CGCG536-006 | 13.4951 | 40.4136 | 5669 | -23.85 | 0.10 | 97.8 $\pm$ 0.0 | 22.91 | E
UGC00567 | 13.8310 | 31.7492 | 5962 | -24.24 | 0.08 |  $<$ 0.4 |  $<$ 20.58 |
NGC0304 | 14.0251 | 24.1269 | 4877 | -24.57 | 0.09 | 1.8 $\pm$ 0.1 | 21.04 | P
NGC0311 | 14.3864 | 30.2808 | 4963 | -24.59 | 0.09 | 2.6 $\pm$ 1.0 | 21.22 | P
UGC00612 | 14.7536 | 23.8529 | 4959 | -23.88 | 0.10 | 16.0 $\pm$ 0.0 | 22.00 | P
ARK024 | 15.3045 | 30.1534 | 6852 | -24.20 | 0.13 |  $<$ 0.6 |  $<$ 20.89 |
UGC00636 | 15.4257 | 24.0580 | 4971 | -23.71 | 0.09 |  $<$ 0.5 |  $<$ 20.46 |
CGCG501-067 | 15.4697 | 30.1458 | 6536 | -24.25 | 0.12 |  $<$ 0.6 |  $<$ 20.82 |
UGC00654 | 15.9974 | 21.2254 | 5507 | -23.98 | 0.10 |  $<$ 0.5 |  $<$ 20.59 |
NGC0380 | 16.8233 | 32.4829 | 4344 | -24.78 | 0.22 | 8.4 $\pm$ 0.3 | 21.61 | P
NGC0384 | 16.8542 | 32.2928 | 4156 | -23.92 | 0.17 |  $<$ 0.8 |  $<$ 20.58 |
NGC0385 | 16.8635 | 32.3198 | 4876 | -24.37 | 0.11 |  $<$ 0.6 |  $<$ 20.54 |
NGC0392 | 17.0977 | 33.1336 | 4603 | -24.61 | 0.09 |  $<$ 0.5 |  $<$ 20.40 |
CGCG501-110 | 17.4858 | 30.4678 | 6409 | -23.88 | 0.07 |  $<$ 0.3 |  $<$ 20.54 |
UGC00724 | 17.4974 | 32.3684 | 5073 | -24.02 | 0.11 | 29.0 $\pm$ 0.0 | 22.28 | E
CGCG501-120 | 17.7972 | 32.7018 | 4956 | -23.57 | 0.10 |  $<$ 0.5 |  $<$ 20.49 |
NGC0414 | 17.8228 | 33.1139 | 5343 | -24.11 | 0.11 |  $<$ 0.6 |  $<$ 20.62 |
NGC0420 | 18.0402 | 32.1232 | 4907 | -24.77 | 0.09 | 0.8 $\pm$ 0.6 | 20.69 | P
IC1638 | 18.0909 | 33.3644 | 4693 | -23.70 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |
NGC0431 | 18.5189 | 33.7042 | 5610 | -24.68 | 0.14 |  $<$ 0.7 |  $<$ 20.74 |
IC1659 | 19.0251 | 30.3491 | 6739 | -24.86 | 0.08 | 16.7 $\pm$ 0.4 | 22.29 | P
NGC0472 | 20.1195 | 32.7090 | 5198 | -24.24 | 0.12 |  $<$ 0.6 |  $<$ 20.62 |
UGC00878 | 20.2622 | 33.8984 | 3957 | -24.17 | 0.18 |  $<$ 0.9 |  $<$ 20.57 |
NGC0504 | 20.8662 | 33.2043 | 4144 | -23.86 | 0.22 |  $<$ 1.1 |  $<$ 20.69 |
NGC0508 | 20.9191 | 33.2807 | 5407 | -24.79 | 0.20 | 10.1 $\pm$ 0.0 | 21.88 | P
NGC0517 | 21.1825 | 33.4296 | 4123 | -24.13 | 0.18 | 8.6 $\pm$ 0.3 | 21.57 | P
NGC0528 | 21.3899 | 33.6714 | 4708 | -24.63 | 0.28 | 3.9 $\pm$ 0.6 | 21.35 | P
UGC01022 | 21.7399 | 39.0182 | 5431 | -23.62 | 0.07 | 10.9 $\pm$ 0.3 | 21.92 | E
UGC01032 | 21.8855 | 19.1788 | 5064 | -23.91 | 0.09 | 22.1 $\pm$ 0.9 | 22.16 | P
UGC01101 | 23.1474 | 41.9869 | 5870 | -24.26 | 0.08 |  $<$ 0.4 |  $<$ 20.56 |
NGC0608 | 23.8677 | 33.6567 | 4991 | -24.40 | 0.23 |  $<$ 1.1 |  $<$ 20.86 |
NGC0614 | 23.9678 | 33.6819 | 5047 | -24.58 | 0.25 | 6.8 $\pm$ 0.7 | 21.65 | P
NGC0621 | 24.2044 | 35.5122 | 5055 | -24.65 | 0.09 | 3.0 $\pm$ 0.3 | 21.29 | P
NGC0656 | 25.6135 | 26.1431 | 3816 | -24.04 | 0.12 |  $<$ 0.6 |  $<$ 20.33 |
NGC0661 | 26.0609 | 28.7059 | 3725 | -24.45 | 0.12 | 1.5 $\pm$ 0.2 | 20.73 | P
NGC0666 | 26.5258 | 34.3745 | 4631 | -23.80 | 0.13 |  $<$ 0.6 |  $<$ 20.55 |
NGC0670 | 26.8535 | 27.8858 | 3608 | -24.19 | 0.13 | 39.9 $\pm$ 0.5 | 22.12 | E
NGC0680 | 27.4471 | 21.9708 | 2855 | -24.40 | 0.11 | 3.1 $\pm$ 0.2 | 20.81 | P
UGC01327 | 27.9506 | 30.5435 | 4552 | -23.54 | 0.10 | 3.9 $\pm$ 0.0 | 21.32 | P
NGC0711 | 28.1158 | 17.5126 | 4758 | -24.00 | 0.11 |  $<$ 0.6 |  $<$ 20.51 |
NGC0704 | 28.1571 | 36.1268 | 4630 | -23.81 | 0.11 |  $<$ 0.5 |  $<$ 20.47 |
NGC0703 | 28.1650 | 36.1714 | 5459 | -24.66 | 0.14 | 14.9 $\pm$ 0.0 | 22.06 | P
UGC01353 | 28.3457 | 36.9551 | 5144 | -24.19 | 0.08 |  $<$ 0.4 |  $<$ 20.45 |
NGC0714 | 28.3735 | 36.2213 | 4330 | -24.43 | 0.08 | 4.0 $\pm$ 0.0 | 21.28 | P
CGCG460-045 | 28.6840 | 18.0471 | 4801 | -23.66 | 0.11 | 4.8 $\pm$ 0.2 | 21.45 | P
UGC01396 | 28.9025 | 21.3176 | 4789 | -23.63 | 0.11 | 4.6 $\pm$ 0.4 | 21.43 | P
NGC0736 | 29.1703 | 33.0435 | 4257 | -24.92 | 0.08 | 4.0 $\pm$ 0.0 | 21.27 | P
CGCG461-014 | 29.5566 | 21.3505 | 4765 | -23.50 | 0.11 | 1.1 $\pm$ 0.0 | 20.81 | P
IC0179 | 30.0479 | 38.0214 | 4133 | -24.46 | 0.08 | 3.4 $\pm$ 0.0 | 21.17 | P
UGC01503 | 30.3328 | 33.3298 | 4966 | -23.77 | 0.09 | 16.9 $\pm$ 0.8 | 22.03 | E
NGC0785 | 30.4167 | 31.8265 | 4862 | -24.48 | 0.11 |  $<$ 0.5 |  $<$ 20.51 |
NGC0798 | 30.8317 | 32.0775 | 4964 | -23.93 | 0.11 |  $<$ 0.6 |  $<$ 20.55 |
CGCG482-063 | 30.9643 | 25.9253 | 4746 | -24.39 | 0.09 | 2.6 $\pm$ 0.0 | 21.18 | P
NGC0804 | 31.0088 | 30.8329 | 5135 | -23.99 | 0.10 | 0.9 $\pm$ 0.2 | 20.78 | P
NGC0807 | 31.2319 | 28.9874 | 4638 | -24.82 | 0.13 | 1.4 $\pm$ 0.0 | 20.89 | P
UGC01590 | 31.5168 | 29.7930 | 4836 | -24.86 | 0.12 | 25.1 $\pm$ 0.0 | 22.18 | E
UGC01596 | 31.6264 | 29.9931 | 4621 | -23.83 | 0.10 |  $<$ 0.5 |  $<$ 20.45 |
UGC01604 | 31.8241 | 37.0967 | 5041 | -24.00 | 0.09 |  $<$ 0.5 |  $<$ 20.49 |
NGC0826 | 32.3544 | 30.7397 | 4741 | -23.73 | 0.09 | 3.2 $\pm$ 0.5 | 21.27 | P
UGC01661 | 32.5616 | 41.5218 | 5434 | -24.22 | 0.08 | 0.9 $\pm$ 0.0 | 20.83 | P
UGC01757 | 34.3461 | 38.4138 | 5146 | -24.19 | 0.08 | 67.2 $\pm$ 0.3 | 22.66 | P
UGC01786 | 34.8782 | 37.1118 | 6271 | -23.74 | 0.11 |  $<$ 0.5 |  $<$ 20.72 |
NGC0904 | 36.0232 | 27.3425 | 5211 | -24.27 | 0.13 |  $<$ 0.6 |  $<$ 20.66 |
UGC01859 | 36.1851 | 42.6230 | 5810 | -24.90 | 0.12 | 9.2 $\pm$ 0.0 | 21.90 | P
NGC0909 | 36.3450 | 42.0355 | 4893 | -24.10 | 0.10 |  $<$ 0.5 |  $<$ 20.46 |
CGCG539-018 | 36.3656 | 41.8968 | 5277 | -23.61 | 0.09 |  $<$ 0.5 |  $<$ 20.53 |
NGC0911 | 36.4267 | 41.9563 | 5660 | -24.77 | 0.10 | 2.8 $\pm$ 0.5 | 21.36 | P
UGC01889 | 36.5116 | 30.1732 | 4946 | -23.91 | 0.09 |  $<$ 0.4 |  $<$ 20.45 |
UGC01914 | 36.8564 | 41.0599 | 5382 | -24.24 | 0.08 | 2.4 $\pm$ 0.2 | 21.25 | P
UGC01939 | 37.0733 | 26.3124 | 5073 | -23.93 | 0.10 | 1.6 $\pm$ 0.1 | 21.02 | P
NGC0940 | 37.3646 | 31.6409 | 4989 | -24.99 | 0.09 | 14.4 $\pm$ 0.0 | 21.96 | P
NGC0946 | 37.6604 | 42.2322 | 5667 | -24.91 | 0.09 | 13.3 $\pm$ 0.0 | 22.04 | P
NGC0953 | 37.7908 | 29.5888 | 4599 | -24.76 | 0.17 | 1.4 $\pm$ 0.0 | 20.88 | P
CGCG539-042 | 38.1179 | 41.9443 | 4802 | -23.66 | 0.10 |  $<$ 0.5 |  $<$ 20.45 |
NGC0962 | 38.1660 | 28.0699 | 4482 | -24.81 | 0.10 |  $<$ 0.5 |  $<$ 20.40 |
UGC02006 | 38.1663 | 42.4287 | 5854 | -23.96 | 0.10 | 2.8 $\pm$ 0.3 | 21.39 | P
NGC0968 | 38.5259 | 34.4799 | 3555 | -24.16 | 0.09 |  $<$ 0.4 |  $<$ 20.15 |
NGC0969 | 38.5330 | 32.9473 | 4400 | -24.90 | 0.07 | 2.0 $\pm$ 0.2 | 21.00 | P
IC1815 | 38.5834 | 32.4294 | 4586 | -24.56 | 0.09 | 0.8 $\pm$ 0.5 | 20.63 | P
CGCG539-050 | 38.6078 | 41.1482 | 4927 | -23.65 | 0.08 |  $<$ 0.4 |  $<$ 20.42 |
NGC0980 | 38.8273 | 40.9265 | 5623 | -24.48 | 0.08 | 0.9 $\pm$ 0.0 | 20.86 | P
UGC02074 | 39.0107 | 42.6141 | 5502 | -24.25 | 0.11 | 2.7 $\pm$ 0.0 | 21.32 | P
UGC02073 | 39.0185 | 42.4210 | 5076 | -24.28 | 0.10 |  $<$ 0.5 |  $<$ 20.53 |
CGCG484-013 | 39.0635 | 27.1795 | 5206 | -23.81 | 0.10 |  $<$ 0.5 |  $<$ 20.56 |
CGCG484-015 | 39.2453 | 25.4429 | 5353 | -24.46 | 0.10 |  $<$ 0.5 |  $<$ 20.58 |
NGC0995 | 39.6335 | 41.5293 | 3938 | -23.90 | 0.09 | 3.2 $\pm$ 0.3 | 21.10 | P
NGC0996 | 39.6661 | 41.6475 | 4508 | -24.56 | 0.09 | 5.1 $\pm$ 1.0 | 21.42 | P
NGC1005 | 39.8653 | 41.4933 | 4240 | -23.66 | 0.09 | 4.2 $\pm$ 0.0 | 21.29 | P
NGC1057 | 40.7620 | 32.4912 | 5642 | -24.40 | 0.12 | 6.6 $\pm$ 0.0 | 21.73 | P
NGC1040 | 40.8018 | 41.5006 | 4730 | -24.61 | 0.11 | 3.1 $\pm$ 0.0 | 21.25 | P
CGCG505-042 | 40.8873 | 32.2528 | 4803 | -23.89 | 0.11 |  $<$ 0.5 |  $<$ 20.51 |
WISEAJ024421.83+312117.1 | 41.0910 | 31.3547 | 5277 | -23.56 | 0.13 |  $<$ 0.7 |  $<$ 20.68 |
CGCG147-020 | 111.4052 | 29.9541 | 5775 | -23.71 | 0.16 | 674.5 $\pm$ 0.0 | 23.76 | E
NGC2385 | 112.1170 | 33.8378 | 4318 | -23.62 | 0.10 | 2.2 $\pm$ 0.0 | 21.02 | P
IC2194 | 113.4175 | 31.3344 | 4505 | -23.86 | 0.13 |  $<$ 0.7 |  $<$ 20.53 |
IC2201 | 114.0701 | 33.1227 | 4783 | -23.68 | 0.13 |  $<$ 0.7 |  $<$ 20.59 |
NGC2444 | 116.7210 | 39.0320 | 4240 | -23.84 | 0.09 |  $<$ 0.5 |  $<$ 20.34 |
CGCG206-038 | 118.6036 | 39.3716 | 6131 | -24.21 | 0.08 |  $<$ 0.4 |  $<$ 20.60 |
UGC04085 | 118.8312 | 53.3308 | 7449 | -24.47 | 0.09 | 63.3 $\pm$ 0.0 | 22.95 | E
NGC2476 | 119.1883 | 39.9278 | 3943 | -24.30 | 0.09 | 1.3 $\pm$ 0.0 | 20.71 | P
CGCG178-006 | 119.2664 | 33.0832 | 5350 | -24.01 | 0.08 |  $<$ 0.4 |  $<$ 20.48 |
IC2213 | 119.7774 | 27.4641 | 6941 | -24.03 | 0.10 |  $<$ 0.5 |  $<$ 20.78 |
CGCG148-108 | 121.1040 | 29.5066 | 5699 | -23.85 | 0.13 |  $<$ 0.6 |  $<$ 20.73 |
UGC04209 | 121.3605 | 46.7078 | 6962 | -24.75 | 0.29 |  $<$ 1.4 |  $<$ 21.25 |
NGC2518 | 121.8344 | 51.1316 | 5464 | -24.65 | 0.09 |  $<$ 0.4 |  $<$ 20.52 |
NGC2524 | 122.0399 | 39.1574 | 4194 | -24.28 | 0.07 |  $<$ 0.3 |  $<$ 20.17 |
ARK154 | 122.1122 | 39.9643 | 6455 | -24.32 | 0.07 | 0.9 $\pm$ 0.0 | 20.98 | P
NGC2521 | 122.2057 | 57.7696 | 5715 | -24.89 | 0.06 | 2.1 $\pm$ 0.0 | 21.25 | E
CGCG178-034 | 122.7789 | 36.5987 | 6591 | -23.58 | 0.09 | 8.8 $\pm$ 0.0 | 21.99 | P
CGCG149-001 | 122.8229 | 29.5089 | 6164 | -23.74 | 0.09 | 1.9 $\pm$ 0.0 | 21.27 | P
UGC04272 | 123.1979 | 44.3573 | 7111 | -24.22 | 0.11 |  $<$ 0.6 |  $<$ 20.86 |
CGCG207-047 | 123.6252 | 43.1435 | 7084 | -24.33 | 0.09 |  $<$ 0.4 |  $<$ 20.74 |
UGC04341 | 125.0412 | 27.0934 | 6119 | -24.71 | 0.15 | 2.1 $\pm$ 0.0 | 21.30 | P
CGCG207-056 | 125.0564 | 44.2303 | 7282 | -24.13 | 0.16 |  $<$ 0.8 |  $<$ 21.02 |
UGC04323 | 125.0827 | 66.9820 | 4302 | -24.24 | 0.06 | 4.8 $\pm$ 0.9 | 21.36 | P
IC2365 | 126.5753 | 27.8401 | 6251 | -24.38 | 0.14 | 4.5 $\pm$ 0.2 | 21.65 | P
MCG+10-12-141 | 127.2195 | 58.2039 | 5673 | -23.63 | 0.06 | 15.0 $\pm$ 0.0 | 22.09 | E
CGCG149-037 | 127.3750 | 31.6754 | 5725 | -23.71 | 0.07 | 9.9 $\pm$ 0.7 | 21.92 | P
CGCG263-043 | 128.1173 | 52.6061 | 5324 | -23.73 | 0.09 | 48.5 $\pm$ 0.2 | 22.55 | P
CGCG208-015 | 128.3023 | 41.0948 | 7408 | -24.78 | 0.07 |  $<$ 0.3 |  $<$ 20.69 |
CGCG311-017 | 130.9709 | 64.9703 | 7132 | -24.52 | 0.07 | 65.6 $\pm$ 0.0 | 22.93 | E
CGCG208-054 | 132.5470 | 40.2557 | 7405 | -24.25 | 0.07 |  $<$ 0.3 |  $<$ 20.68 |
IC0522 | 133.6455 | 57.1667 | 5330 | -24.51 | 0.06 |  $<$ 0.3 |  $<$ 20.35 |
CGCG311-028 | 135.5786 | 63.8055 | 7444 | -24.19 | 0.06 | 5.7 $\pm$ 0.0 | 21.91 | P
IC2439 | 137.1601 | 32.5929 | 4608 | -23.61 | 0.12 | 5.6 $\pm$ 0.9 | 21.48 | P
NGC2767 | 137.5495 | 50.4013 | 5200 | -24.10 | 0.06 | 1.0 $\pm$ 0.0 | 20.84 | P
CGCG180-061 | 138.5947 | 36.3158 | 7341 | -23.73 | 0.04 |  $<$ 0.2 |  $<$ 20.42 |
UGC04893 | 139.1569 | 30.9054 | 7258 | -23.74 | 0.12 | 1.3 $\pm$ 0.0 | 21.24 | P
CGCG181-008 | 139.5791 | 33.5569 | 7455 | -23.72 | 0.08 |  $<$ 0.4 |  $<$ 20.74 |
CGCG181-022 | 139.9001 | 33.4283 | 7349 | -24.17 | 0.09 |  $<$ 0.4 |  $<$ 20.77 |
NGC2830 | 139.9225 | 33.7380 | 6406 | -24.13 | 0.09 | 18.3 $\pm$ 0.3 | 22.28 | E
CGCG181-038 | 140.8860 | 33.7550 | 6955 | -23.62 | 0.07 |  $<$ 0.4 |  $<$ 20.65 |
CGCG312-008 | 141.2533 | 64.5604 | 5411 | -23.73 | 0.05 | 41.8 $\pm$ 0.2 | 22.50 | E
UGC05026 | 141.6658 | 45.8471 | 4634 | -23.80 | 0.11 | 11.2 $\pm$ 0.0 | 21.79 | P
NGC2880 | 142.3941 | 62.4906 | 1927 | -23.59 | 0.06 |  $<$ 0.3 |  $<$ 19.43 |
IC2493 | 144.0732 | 37.3640 | 6507 | -24.23 | 0.07 |  $<$ 0.3 |  $<$ 20.55 |
UGC05119 | 144.3027 | 38.0923 | 6356 | -24.31 | 0.06 |  $<$ 0.3 |  $<$ 20.49 |
UGC05133 | 144.5973 | 43.5092 | 4764 | -23.73 | 0.06 |  $<$ 0.3 |  $<$ 20.20 |
IC2500 | 145.5973 | 36.3498 | 6946 | -24.29 | 0.07 |  $<$ 0.3 |  $<$ 20.62 |
NGC2950 | 145.6468 | 58.8512 | 1710 | -24.09 | 0.06 | 3.3 $\pm$ 0.0 | 20.39 | P
CGCG181-084 | 145.7254 | 36.2141 | 7017 | -23.55 | 0.06 |  $<$ 0.3 |  $<$ 20.58 |
NGC2968 | 145.8001 | 31.9288 | 1947 | -23.85 | 0.11 |  $<$ 0.5 |  $<$ 19.72 |
NGC2965 | 145.8298 | 36.2478 | 7056 | -24.93 | 0.06 | 56.8 $\pm$ 0.9 | 22.86 | P
ARK211 | 145.9483 | 42.4736 | 5760 | -23.68 | 0.06 | 0.9 $\pm$ 0.0 | 20.88 | P
CGCG210-030 | 145.9967 | 42.4330 | 5416 | -24.10 | 0.05 | 0.7 $\pm$ 1.3 | 20.72 | P
UGC05225 | 146.6191 | 45.7526 | 5239 | -24.00 | 0.05 |  $<$ 0.2 |  $<$ 20.25 |
IC2516 | 148.7015 | 37.6869 | 5411 | -23.75 | 0.06 |  $<$ 0.3 |  $<$ 20.38 |
CGCG182-041 | 149.0720 | 37.5900 | 7179 | -23.73 | 0.08 |  $<$ 0.4 |  $<$ 20.73 |
NGC3071 | 149.7208 | 31.6203 | 6783 | -23.93 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |
IC2530 | 150.3795 | 37.2039 | 6963 | -24.21 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |
NGC3116 | 151.6877 | 31.0977 | 6775 | -24.03 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |
IC2540 | 151.6947 | 31.4757 | 6949 | -23.85 | 0.08 |  $<$ 0.4 |  $<$ 20.68 |
NGC3151 | 153.3713 | 38.6198 | 7244 | -24.13 | 0.07 | 1.6 $\pm$ 0.9 | 21.33 | P
NGC3152 | 153.3922 | 38.8432 | 6769 | -23.79 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |
NGC3159 | 153.4701 | 38.6545 | 7164 | -24.60 | 0.07 |  $<$ 0.4 |  $<$ 20.69 |
NGC3161 | 153.4967 | 38.6572 | 6650 | -24.02 | 0.08 | 2.1 $\pm$ 0.3 | 21.38 | P
NGC3163 | 153.5297 | 38.6526 | 6625 | -24.93 | 0.07 | 1.5 $\pm$ 0.0 | 21.23 | P
CGCG211-030 | 153.6239 | 39.5016 | 7394 | -24.19 | 0.09 |  $<$ 0.4 |  $<$ 20.79 |
CGCG211-031 | 153.6888 | 38.9810 | 7364 | -24.37 | 0.08 | 2.9 $\pm$ 0.0 | 21.61 | P
CGCG240-029 | 154.8584 | 44.4046 | 7372 | -24.66 | 0.08 | 6.2 $\pm$ 0.0 | 21.94 | P
NGC3207 | 155.2524 | 42.9853 | 7365 | -24.63 | 0.08 | 22.9 $\pm$ 0.3 | 22.50 | E
CGCG183-015 | 155.3769 | 37.7566 | 7022 | -24.02 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |
MCG+05-25-004 | 156.1015 | 28.0288 | 6688 | -23.78 | 0.12 |  $<$ 0.6 |  $<$ 20.86 |
NGC3245 | 156.8266 | 28.5074 | 1755 | -24.20 | 0.09 | 20.1 $\pm$ 0.0 | 21.20 | P
CGCG266-048 | 157.3504 | 55.1867 | 7171 | -24.22 | 0.05 | 4.1 $\pm$ 0.0 | 21.73 | P
UGC05953 | 162.8251 | 44.5718 | 3626 | -23.58 | 0.06 | 1.3 $\pm$ 0.4 | 20.64 | P
NGC3415 | 162.9275 | 43.7126 | 3739 | -24.31 | 0.05 | 39.9 $\pm$ 0.3 | 22.16 | E
NGC3407 | 163.0742 | 61.3797 | 5381 | -23.87 | 0.09 | 2.3 $\pm$ 0.0 | 21.23 | P
UGC05991 | 163.1985 | 49.6126 | 7160 | -24.39 | 0.06 | 1.5 $\pm$ 0.0 | 21.29 | P
UGC06013 | 163.4992 | 49.6598 | 6937 | -24.43 | 0.06 | 53.3 $\pm$ 0.2 | 22.82 | E
CGCG241-034 | 163.6584 | 47.4703 | 7095 | -24.18 | 0.05 |  $<$ 0.3 |  $<$ 20.52 |
CGCG241-036 | 163.6793 | 46.5541 | 7093 | -24.37 | 0.05 | 0.9 $\pm$ 1.3 | 21.06 | P
UGC06076 | 165.0401 | 45.9170 | 6806 | -24.49 | 0.05 | 0.5 $\pm$ 0.0 | 20.77 | P
UGC06114 | 165.7345 | 50.6593 | 6485 | -24.29 | 0.06 |  $<$ 0.3 |  $<$ 20.50 |
CGCG241-068 | 166.0188 | 45.2623 | 6993 | -24.39 | 0.06 |  $<$ 0.3 |  $<$ 20.55 |
NGC3540 | 167.3171 | 36.0211 | 6832 | -24.84 | 0.07 |  $<$ 0.3 |  $<$ 20.61 |
NGC3595 | 168.8564 | 47.4471 | 2647 | -23.52 | 0.07 |  $<$ 0.4 |  $<$ 19.82 |
NGC3613 | 169.6505 | 58.0000 | 2497 | -24.82 | 0.04 | 1.7 $\pm$ 1.0 | 20.43 | P
NGC3619 | 169.8400 | 57.7577 | 2021 | -23.79 | 0.05 | 9.7 $\pm$ 0.0 | 21.01 | E
NGC3658 | 170.9928 | 38.5624 | 2537 | -23.73 | 0.07 |  $<$ 0.4 |  $<$ 19.79 |
CGCG214-007 | 171.6919 | 39.2662 | 6746 | -24.00 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |
CGCG156-085 | 172.3485 | 28.5437 | 7339 | -24.41 | 0.11 | 1.4 $\pm$ 0.2 | 21.29 | P
CGCG268-047 | 173.1419 | 54.9266 | 6618 | -24.17 | 0.05 |  $<$ 0.2 |  $<$ 20.44 |
NGC3737 | 173.9016 | 54.9486 | 6219 | -24.90 | 0.05 |  $<$ 0.3 |  $<$ 20.40 |
NGC3759 | 174.2254 | 54.8232 | 5978 | -24.52 | 0.05 | 21.1 $\pm$ 0.0 | 22.29 | P
NGC3809 | 175.3170 | 59.8858 | 3861 | -24.28 | 0.06 | 35.5 $\pm$ 0.2 | 22.13 | P
CGCG186-038 | 176.3366 | 32.7223 | 6916 | -23.76 | 0.07 |  $<$ 0.3 |  $<$ 20.63 |
IC2967 | 177.7297 | 30.8508 | 7304 | -24.40 | 0.10 |  $<$ 0.5 |  $<$ 20.81 |
CGCG186-056 | 177.8552 | 35.2039 | 6979 | -23.61 | 0.06 |  $<$ 0.3 |  $<$ 20.60 |
NGC3941 | 178.2307 | 36.9864 | 1291 | -24.07 | 0.06 | 4.3 $\pm$ 0.2 | 20.26 | P
NGC3945 | 178.3072 | 60.6756 | 1753 | -24.53 | 0.06 | 7.3 $\pm$ 0.0 | 20.76 | E
NGC3998 | 179.4839 | 55.4535 | 1519 | -24.38 | 0.06 | 307.9 $\pm$ 0.0 | 22.26 | E
NGC4036 | 180.3620 | 61.8957 | 1857 | -24.62 | 0.07 | 47.0 $\pm$ 0.0 | 21.62 | P
NGC4097 | 181.5104 | 36.8636 | 6793 | -24.70 | 0.06 |  $<$ 0.3 |  $<$ 20.56 |
IC3022 | 182.5099 | 38.7400 | 6818 | -24.49 | 0.06 | 0.8 $\pm$ 0.0 | 20.98 | P
NGC4148 | 182.5332 | 35.8776 | 5496 | -24.46 | 0.06 | 23.2 $\pm$ 0.2 | 22.25 | E
KUG1208+386 | 182.6845 | 38.3362 | 7327 | -24.23 | 0.06 | 30.6 $\pm$ 0.9 | 22.62 | P
CGCG187-017 | 182.7147 | 36.6243 | 7364 | -24.56 | 0.06 | 1.4 $\pm$ 0.3 | 21.29 | P
NGC4169 | 183.0783 | 29.1793 | 4327 | -24.93 | 0.10 | 11.0 $\pm$ 0.0 | 21.72 | P
CGCG187-025 | 183.5582 | 32.4212 | 6881 | -24.00 | 0.11 |  $<$ 0.6 |  $<$ 20.82 |
UGC07243 | 183.5961 | 32.4146 | 7166 | -24.67 | 0.11 |  $<$ 0.6 |  $<$ 20.86 |
NGC4196 | 183.6239 | 28.4235 | 4523 | -24.25 | 0.12 |  $<$ 0.6 |  $<$ 20.51 |
NGC4203 | 183.7710 | 33.1973 | 1634 | -24.49 | 0.10 | 14.3 $\pm$ 0.2 | 20.99 | P
CGCG215-057 | 184.2714 | 42.9480 | 7416 | -23.99 | 0.04 | 1.8 $\pm$ 0.2 | 21.40 | P
NGC4251 | 184.5347 | 28.1753 | 1624 | -24.16 | 0.14 |  $<$ 0.7 |  $<$ 19.67 |
NGC4271 | 184.8859 | 56.7366 | 5184 | -24.90 | 0.07 | 2.2 $\pm$ 0.0 | 21.18 | P
CGCG215-065 | 185.2586 | 39.9000 | 7369 | -24.05 | 0.06 |  $<$ 0.3 |  $<$ 20.64 |
NGC4358 | 186.0087 | 58.3852 | 4927 | -23.78 | 0.06 | 0.7 $\pm$ 0.7 | 20.64 | P
UGC07635 | 187.4390 | 56.8263 | 5200 | -24.22 | 0.06 | 0.9 $\pm$ 0.0 | 20.80 | P
MRK0215 | 188.1447 | 45.7677 | 6471 | -23.75 | 0.06 | 52.3 $\pm$ 0.0 | 22.75 | P
IC0801 | 188.4374 | 52.2548 | 7045 | -24.87 | 0.06 |  $<$ 0.3 |  $<$ 20.54 |
KUG1234+397 | 189.3154 | 39.4832 | 6617 | -23.77 | 0.06 | 5.0 $\pm$ 0.2 | 21.75 | P
NGC4646 | 190.7173 | 54.8560 | 5104 | -24.56 | 0.05 | 5.4 $\pm$ 0.0 | 21.56 | P
NGC4687 | 191.8490 | 35.3521 | 4817 | -23.90 | 0.07 | 16.4 $\pm$ 0.3 | 21.99 | P
CGCG159-083 | 192.4261 | 26.8920 | 7417 | -24.76 | 0.12 | 3.8 $\pm$ 0.0 | 21.73 | P
NGC4728 | 192.6170 | 27.4349 | 7023 | -24.34 | 0.12 |  $<$ 0.6 |  $<$ 20.87 |
NGC4737 | 192.7205 | 34.1569 | 7443 | -24.66 | 0.07 | 2.5 $\pm$ 1.7 | 21.55 | P
IC0830 | 192.8188 | 53.6963 | 5328 | -24.26 | 0.05 |  $<$ 0.3 |  $<$ 20.28 |
IC0831 | 193.1836 | 26.4704 | 7000 | -24.27 | 0.11 |  $<$ 0.5 |  $<$ 20.83 |
CGCG159-104 | 193.3170 | 27.0945 | 6740 | -24.30 | 0.12 |  $<$ 0.6 |  $<$ 20.86 |
NGC4788 | 193.5668 | 27.3037 | 6993 | -24.03 | 0.09 |  $<$ 0.5 |  $<$ 20.77 |
IC0834 | 194.0775 | 26.3589 | 7071 | -24.42 | 0.08 | 1.1 $\pm$ 0.0 | 21.15 | P
CGCG160-023 | 194.0825 | 27.7511 | 7460 | -23.63 | 0.08 |  $<$ 0.4 |  $<$ 20.77 |
CGCG160-027 | 194.1109 | 27.8306 | 6878 | -23.51 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |
NGC4828 | 194.1785 | 28.0205 | 6876 | -24.10 | 0.08 |  $<$ 0.4 |  $<$ 20.69 |
NGC4840 | 194.3868 | 27.6103 | 6671 | -24.39 | 0.08 | 1.6 $\pm$ 0.0 | 21.26 | P
NGC4849 | 194.5527 | 26.3969 | 6475 | -24.87 | 0.08 | 345.4 $\pm$ 0.0 | 23.57 | E
NGC4850 | 194.5910 | 27.9678 | 6605 | -23.90 | 0.08 | 1.8 $\pm$ 0.6 | 21.30 | P
IC3946 | 194.7030 | 27.8103 | 6450 | -23.76 | 0.09 |  $<$ 0.5 |  $<$ 20.69 |
IC3960 | 194.7830 | 27.8549 | 7202 | -23.62 | 0.09 | 1.5 $\pm$ 0.0 | 21.30 | P
NGC4864 | 194.8047 | 27.9769 | 7334 | -24.55 | 0.09 | 4.4 $\pm$ 0.9 | 21.78 | P
NGC4865 | 194.8327 | 28.0843 | 5286 | -23.96 | 0.07 | 3.9 $\pm$ 0.2 | 21.45 | P
NGC4869 | 194.8473 | 27.9116 | 7437 | -24.58 | 0.09 | 1688.8 $\pm$ 0.4 | 24.38 | E
IC3976 | 194.8724 | 27.8502 | 7443 | -23.69 | 0.09 | 2.0 $\pm$ 0.8 | 21.45 | P
NGC4873 | 194.8866 | 27.9836 | 6374 | -23.60 | 0.09 |  $<$ 0.4 |  $<$ 20.67 |
IC3991 | 194.9157 | 28.9266 | 6583 | -23.69 | 0.08 |  $<$ 0.4 |  $<$ 20.66 |
NGC4876 | 194.9350 | 27.9125 | 7258 | -23.80 | 0.07 |  $<$ 0.4 |  $<$ 20.69 |
WISEAJ125957.75+2814 | 194.9906 | 28.2465 | 7290 | -24.75 | 0.09 |  $<$ 0.5 |  $<$ 20.80 |
NGC4892 | 195.0147 | 26.8981 | 6492 | -24.27 | 0.08 |  $<$ 0.4 |  $<$ 20.65 |
NGC4898 | 195.0737 | 27.9553 | 7481 | -24.53 | 0.07 | 2.7 $\pm$ 0.2 | 21.59 | P
NGC4896 | 195.1281 | 28.3463 | 6595 | -24.16 | 0.08 |  $<$ 0.4 |  $<$ 20.67 |
IC4042 | 195.1782 | 27.9713 | 6974 | -24.29 | 0.08 | 4.0 $\pm$ 0.0 | 21.70 | P
UGC08122 | 195.2081 | 27.4057 | 7201 | -23.67 | 0.08 |  $<$ 0.4 |  $<$ 20.74 |
NGC4908 | 195.2269 | 28.0076 | 5582 | -24.15 | 0.08 |  $<$ 0.4 |  $<$ 20.50 |
NGC4923 | 195.3824 | 27.8475 | 6072 | -24.03 | 0.08 |  $<$ 0.4 |  $<$ 20.58 |
CGCG160-101 | 195.4459 | 28.0950 | 6402 | -23.66 | 0.08 |  $<$ 0.4 |  $<$ 20.63 |