there is a second detection in the beam of
WKK 0491. The small lopsided signal is probably due to WKK 0512
(d=12.4′, 28′′×8′′, SL) which is the largest
late-type spiral in the vicinity. WKK 0493 at
d=10.2′ (28′′×6′′, L)
is an early type galaxy and less likely to be the candidate.
there is a detection in the OFF observation of
WKK 1117, close to but separated from its signal. The nearest candidate
is WKK 0969 at d=8.5′ (16′′×12′′,
unknown type, AB=3.4mag), which is also the only
galaxy found by 2MASS in this area.
the ID is ambiguous. The observed velocity is
v=3533km/s, and WKK 2160 at d=3.3′
(27′′×24′′, S)
has an optical velocity of 3512±58km/s (FW98). It is
possible that we have observed WKK 2160, but if the two galaxies are
genuine companions the signal probably comes from WKK 2163
(74′′×56′′, S6)
which is the larger of the two. HIPASS can barely resolve the
positions, but seems to favour WKK 2163.
this is a group of four galaxies: WKK 2377
(S7, 70′′×23′′),
WKK 2375 (S5, 62′′×56′′, 4290±37km/s, FH95),
WKK 2388 (S5, 36′′×16′′, 3976±40km/s, FH95),
and WKK 2406 (SL, 55′′×38′′).
WKK 2388 lies between WKK 2377 and WKK 2406 and the pointing of WKK 2388
shows a confusion of the two latter profiles at
v≃4100–4400km/s. The signal at
v≃3800–4050km/s belongs to WKK 2388 proper and the line
width is assumed to be unaffected. However, due to difficulties with
fitting a good baseline the flux density is somewhat uncertain. Using
HIPASS we have found that WKK 2375 does not add (significantly) to the
combined signal. The observations of WKK 2377 and WKK 2406 at their
respective pointings are not confused at the noise level.
the close galaxy pair (at
d=1.2′ and d=3.2′,
respectively, from the pointing position) is unresolved, and the
parameters given in Table 1
refer to the full profile. The quoted velocity by VY96 refers to the
IRAS detection which is also unresolved.
also observed with HIZSS, the spectrum shows a profile
reminiscent of the blended signal of two objects. WKK 2503 has a bright
bulge and large faint halo with a bright star superimposed close to the
bulge. No other galaxy in this area is visible either in the optical or
in the NIR. At an extinction of AB=3.7mag a
late-type/LSB galaxy, WKK 2503B, could be invisible even in the NIR.
Table 1
gives the parameters of the full profile. The two velocities found in
the literature refer to H I observations and are equally unresolved.
the observed profile is a combination of
the signals from three galaxies:
WKK 2595 (S6, 102′′×40′′)
and WKK 2597 (S5, 59′′×47′′,
3973±46km/s, SH92) are a close galaxy pair
(d=1.2′); according to HIPASS,
WKK 2576 at d=8.4′ (S5, 86′′×75′′,
3948±70km/s, DN97) has a strong narrow H I profile. Table 1
gives the measurement of the full profile for the unresolved pair
WKK 2595/WKK 2597, while, through comparison with HIPASS, the width and
velocity of the peak at v≃3800–3950km/s is given for
WKK 2576. By removing this peak we have re-measured the width and
velocity of the underlying low-intensity profile for the close galaxy
pair and found v=3889km/s, ΔV50=266km/s, Δ
V20=313km/s .
there are two detections in the beam of WKK 2640:
the narrow spike at v=3705km/s is
WKK 2640 (I, 51′′×42′′),
while the detection at v=9404km/s is WKK 2644 (SM,
26′′×9′′)
with an optical velocity of 9406±100km/s (WK04) at
d=4.3′. Due to the very lopsided profile of
WKK 2644 the high-velocity end is uncertain.
two galaxies contribute to the detected signal.
HIPASS shows that WKK 2863 (S5, 98′′×83′′,
3778±30km/s, SE95) at d=8.7′ has a strong profile with
v≃3600–3850km/s . At the position of WKK 2844 the observed
profile is smaller but extends to v≃3950km/s ; it is
therefore assumed that WKK 2844 has been detected but it remains
unresolved, with a velocity slightly larger than the one for WKK 2863.
Table 1
gives the parameters of the full profile for WKK 2863, which is
considered to be the main contributor to the signal.
there are two detections in the beam of WKK 2924:
WKK 2938 (L, 34′′×22′′) at d=7.3′ has
an optical velocity of 3024±157km/s (FW98) which agrees with
the narrow peak at v=2864km/s . WKK 2924 (S8,
58′′×22′′) is
a more likely candidate for the signal at v=3410km/s . HIPASS also
shows the latter detection at the position of WKK 2924, while nothing
can be seen at the position of WKK 2938.
the two detections in the beam of WKK 3002 can not
unambiguously identified: WKK 3002 (SL?,
56′′×20′′) is more likely to be the
stronger signal at v=3436km/s (cf. HIPASS), while the galaxy at
v=2820km/s is more likely WKK 3006 (13′′×8′′,
no type).
the profile is due to the blending of two signals.
HIPASS shows that the high narrow peak at v≃4680km/s is
WKK 4016 (SL, 67′′times48′′) at d=12.1′,
while the broader profile is probably due to WKK 4022 proper (S5,
91′′×34′′.
Table 1
gives the parameters for the full profile for WKK 4022 and the
measurements of the narrow peak alone for WKK 4016; all parameters are
uncertain.
the detection in the beam of WKK 5267 (not detected) at
d=11.7′ is WKK 5240 (S, 157′′×13′′;
cf. HIPASS). The profile shape is very noisy and the parameters are
uncertain.
this galaxy has been detected in the beams of three other
galaxies: in the OFF observations of WKK 5534
(d=6.5′) and of WKK 5556 (d=2.7′, as well as in the beam of
WKK 5297 (not detected) at d=6.1′. The detection with
the smallest distance to the beam centre is listed in Table 1
shown in Fig. 1
while the detection in the OFF observation of WKK 5524 is least affected
by an RFI at v=5900km/s next to the signal. The other measurements
are: v=5631km/s, ΔV50=353km/s, Δ
V20=383km/s, I=15.65 Jy.km/s, rms=5.3mJy (in the beam
of WKK 5297); and v=5635km/s, ΔV50=357km/s,
ΔV20=396km/s, I=15.17 Jy.km/s, rms=3.3mJy (in
the OFF observation of WKK 5534).
the identification is uncertain: the optical velocity is
4822±82km/s (WK04), but both HIPASS and JS00 confirm the H
I signal to be strongest at the position of WKK 5366. Since the
extinction here is AB=3.8mag, an obscured galaxy
close by cannot be excluded.
the detection found in the OFF observation of WKK 5443
was subsequently searched for the ``best'' position. It has also been
detected by HIZSS and JS00. No galaxy could be found in the optical or
NIR (DENIS, 2MASS).
in the observations of both WKK 5562 and
WKK 5642 a narrow single peak appears at v≃4160km/s . Using
HIPASS we determined that this signal most likely comes from WKK 5616, a
late-type galaxy (19′′×5′′)
at d=5.3′ from WKK 5642 (listed in Table 1) and
d=12.2′ from WKK 5562 with the following
parameter: v=4157km/s, ΔV50=42km/s, Δ
V20=75km/s, I=1.95 Jy.km/s, rms=4.7mJy.
is included in the catalogue since it is very close to the
observed but undetected WKK 5597 (28′′×11′′, L?)
at d=0.7′ and is of comparable size
(30′′×19′′,
type unknown), that is, the rms can be considered an upper limit for
both galaxies.
there are three detections in the beam of WKK 5642
(48′′×17′′, SM):
the spike at v=4167km/s is WKK 5616 and has been discussed
above. The signal at v=6446km/s is assumed to belong to WKK 5642
since it also has two optical velocities of 6045±42km/s (SH92)
and v=6118±100km/s (WK04), though this is only in moderate
agreement. WKK 5670 (24′′×8′′, SE:)
at d=6.6′ with an optical velocity of v=6329±44km/s (WK04) can be
excluded as a candidate since it is only d=5.6′
from WKK 5694, which has also been observed and shows no signal at
v≃6400km/s . A third signal has been found at
v=4418km/s which is likely to be WKK 5659
(44′′×15′′, S6) at d=3.4′.
this is a detection in the beam of WKK 5581 (not
detected). IC 4584 and IC 4585 are two large spiral galaxies at
d≃9′ from the pointing. HIPASS confirms their
identity but cannot resolve the pair, though clearly both galaxies
contribute to the signal. The measurement of the full profile is given
in Table 1.
the three observations of WKK 5733
(vopt=6215±92km/s, WK99), WKK 5694 (vopt=3412±36km/s,
FH95), and WKK 5709 show a very similar profile both in
line width and peak flux at v=5729km/s, v=5730km/s, and
v=5723km/s, respectively. The left horn appears to come from
WKK 5768 (also detected in the beam of WKK 5780), which lies at a
distance of d=13.5′, d=17.9′, and d=11.7′,
respectively, from the three pointings; the peak flux of this horn
varies according to the distance. Due to the similar peak flux and high
velocity end of the rest of the profile we conclude that the detected
galaxy must lie at a similar distance from these three pointings.
WKK 5729 (48′′×16′′, SL) lies at
d=6.9′, d=9.1′, and d=5.9′ from WKK 5733, WKK 5694, and
WKK 5709, respectively. It is a late-type spiral and therefore not
visible with 2MASS and DENIS. The signal is too weak to be detectable
with HIPASS.
is detected in the beam of WKK 5780 (not detected) at
d=9.5′. The low-velocity horn is also
visible in the observations of WKK 5709
(d=11.7′; see plot of WKK 5729), WKK 5733
(d=13.5′) and WKK 5694
(d=17.9′).
the detection in the observation of WKK 5993 is the
blending of two signals. The low-velocity double-horn comes from
WKK 5999 (also observed, see Fig. 1
</articles/aa/full_html/2009/39/aa12592-09/aa12592-09.html#hiprofile>),
while the high-velocity part is due to WKK 5993. The parameters for
WKK 5993 in Table 1
</articles/aa/full_html/2009/39/aa12592-09/aa12592-09.html#cxgadet> have
been measured by cutting off the profile of WKK 5999 at
v≃3350km/s . All the parameters are uncertain since the
low-velocity end of WKK 5993 is undetermined. For the WKK 5999 profile
we have measured v=3261km/s, ΔV50=180km/s,
ΔV20=226km/s, I=8.83 Jy.km/s, rms=2.3mJy.
is included in the catalogue since it is very close to the
observed but undetected WKK 6189
(13′′×8′′, E) at
d=0.9′ and is slightly larger
(22′′×22′′,
type unknown), that is, the rms can be considered an upper limit for
both galaxies.
there are two detections in the beam of WKK 6570.
WKK 6535 (39′′×9′′, S5)
lies at d=6.5′ and is likely to be the detection
at v≃4150km/s . Since
WKK 6570 (60′′×27′′, S3)
is the larger and brighter of the two
we have assumed it to be the closer galaxy at v=2938km/s, but the
identities remain ambiguous.
the two galaxies with similar velocities lie
9.6′ apart. The observation of WKK 6732
shows no significant confusion with the signal of WKK 6689 (though the
flux density may be uncertain), while the profile for WKK 6689 is more
uncertain.
is an interacting system with a separation of
1.4′: WKK 7460 (198′′×105′′, SL)
is the larger component
with an optical velocity of 775±36km/s (SH92), while the
profile gives v=842km/s . Table 1
</articles/aa/full_html/2009/39/aa12592-09/aa12592-09.html#cxgadet>
gives the full parameters for WKK 7460 only, since the contribution by
WKK 7463 (82′′×67′′, S)
is uncertain. However, considering the
types and sizes of the two galaxies as well as the H I velocity as
compared to the optical of WKK 7460, we can assume that WKK 7463
contributes to the profile.
WKK 7198 has been detected in the OFF observation
of WKK 7465 at d=7.2′, and the profiles
overlap. The observation of WKK 7198 (see Fig. 1
</articles/aa/full_html/2009/39/aa12592-09/aa12592-09.html#hiprofile>)
shows that the profile extends from v≃3270km/s to
∼3540km/s . The profile of WKK 7465 is therefore truncated
and no line widths and flux could be derived. The systemic velocity is
likely to be higher than the one given.
WKK7652 has been detected in the beam of WKK 7689
(not detected) at d=11.2′. Optical
velocities for this galaxy are v=1350±31km/s (RC3) and
v=1478±38km/s (WK04), while other H I measurements find
v=1482±6km/s (RC3). While we find v=1519km/s, HK01
has detected WKK 7689 at v=1559±3km/s in H I with the radio
telescope at Effelsberg, which has a smaller beam size
(9′ as compared to 15′ for Parkes).
We can therefore not exclude that part of the signal in our observation
comes from WKK 7689.