Date and Time of the Query: 2019-06-17 T06:36:16 PDT
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Notes for object NGC 5395

12 note(s) found in NED.

1. 2008MNRAS.388..500E
Re:UGC 08900
UGC 8898 and UGC 8900 (NGC 5394 and NGC 5395, Arp 84). The nuclei of this
interacting pair of galaxies are separated by only 1.9 arcmin (~27 kpc). No
H{alpha} emission is detected in the tidal arms of UGC 8898, while H{alpha}
emission is more extended in UGC 8900, in agreement with Kaufman et al. (1999)
from Fabry-Perot imaging. The photometric inclination for UGC 8898 is
70^deg^+/-3^deg^, quite different from our kinematical inclination
(27^deg^+/-20^deg^) which is in fact based on the very central part only (about
15 arcsec diameter). Despite its limited extent, our H{alpha} velocity field of
UGC 8898 clearly suggests a PA of the major-axis of 31^deg^, differing by
66^deg^ from the one used by Marquez et al. (2002) for long-slit spectroscopy,
which they confess is not adequate to elaborate the rotation curve. Indeed, they
did not observe any clear rotation within the first 10 arcsec. Our H{alpha}
rotation curve extends only up to ~10 arcsec and we do not reach either a
plateau or , probably, the maximum rotation velocity. Because our observations
of UGC 8898 have been done through the edge of the transmission function of the
interference filter, the spatial coverage of our data is smaller than that of
Kaufman et al. (1999). They have also observed UGC 8898 in the CO line (Kaufman
et al. 2002) and find a very good agreement between H{alpha} and CO data. In
agreement with the Fabry-Perot H{alpha} velocity field of Kaufman et al. (1999),
our H{alpha} velocity field of UGC 8900 is not well enough defined to show
straightforward evidence for interaction, except that the velocity field is
uncompleted and the kinematical major-axis is shifted by 11^deg^ from the
morphological one, which is a significant difference considering the high
inclination of this galaxy. Marquez et al. (2002) have aligned the slit of their
spectrograph almost along the morphological major-axis, explaining part of the
differences between our rotation curves. Their rotation curve is slightly more
extended but much more chaotic and asymmetric, with a markedly smaller velocity
amplitude than ours. Both sides of our H{alpha} rotation curve are fairly
symmetric and show a slowly rising trend (almost solid body like between 20 and
60 arcsec) without ever reaching a plateau. Such a behaviour is unexpected for
an Sa-type galaxy and could be due to the interaction with its companion. The
kinematical and morphological inclinations of UGC 8900 are compatible within the
error bars (they differ by only 9^deg^). H I single dish observations cannot
disentangle UGC 8898 from its companion UGC 8900 (van Driel et al. 2001;
Theureau et al. 1998). The pair has also been observed in the H I by WHISP
(website) and by Kaufman et al. (1999). Taking into account the lower H I
spatial resolution, the H I and H{alpha} kinematics are compatible, and the H I
position-velocity diagram suggests that we actually reach the maximum of the
rotation curve at the end of our H{alpha} rotation curve.

2. 2002AJ....124..675C
Re:UGC 08900
See the UGC 08898 notes.

3. 2001ApJS..133...77H
Re:NGC 5395
NGC 5395 (S2/L2). - Not detected. Hummel et al. (1987) obtained a less
stringent upper limit of S_20_ < 0.4 mJy ({DELTA}{theta} = 1.3").

4. 2001A&A...379...54H
Re:KPG 404B
KPG404B. The galaxy is classified as SA(s)b pec. Our sharp/filtered and
(B-I) images show a bright nucleus and apparently strong dust lanes along
the arms (see the arm towards the companion galaxy). The (B-V)_T_^0^ colour
is representative of Sab-Sb types. The I/A class for the pair is LI.
Our EE class is 11.

5. 1997AJ....114...77N
Re:NGC 5395
5.8 NGC 5394-5
NGC 5394 [the smaller galaxy to the north in Fig. 15(a)] has prominent inner
and outer spiral arms (the inner arms appear as a dark central circle in this
contrast stretch which emphasizes the faint features). A close inspection of
the optical image shows that the inner spiral arm system smoothly joins the
outer system. The companion galaxy NGC 5395 has several dark dust lanes, and
knotty spiral arms.
The VLA D configuration observations of NGC 5394 and NGC 5395 were plagued with
problems of solar interference. Attempts to remove this through various forms
of continuum subtraction using both AIPS and MIRIAD data reduction packages
were only partially successful. Each spectral channel was finally edited by eye
to remove the most obvious artifacts; the resulting maps [Figs. 15(a) and
15(b)] have severely limited sensitivity, with only the bigger galaxy NGC 5395
being detected.
The most notable feature in the H I maps is the SW tail to NGC 5395, which is
probably real. The small arms to either side of the main disk on the other hand
are most likely artifacts arising from solar interference. From the velocity
NGC 5395 is undergoing a direct encounter with NGC 5394, consistent with the
presence of the large SW counter tail. Figure 16 is the integrated H I single
dish profile. The high velocity peak corresponds to the SW tail.

6. 1994CAG1..B...0000S
Re:NGC 5395
Karachentsev 404 [with NGC 5394]
March 23/24, 1939
Agfa Blue
50 min
NGC 5395 is the largest member of this
pair, which evidently is in the process of
encounter. The redshifts listed by Karachentsev
(1987) in his catalog of close pairs are
v_o(5394) = 3537 km/s and v_o(5395) = 3579 km/s.

7. 1976RC2...C...0000d
Re:NGC 5395
= Holm 563a
In Arp 084 = VV 048 = I Zw 077 = Kara[72] 404
Interacting pair with NGC 5394 at 1.9 arcmin, connected.

8. 1973UGC...C...0000N
Re:UGC 08900
VV 48a, Arp 84
I Zw 77
SA(s)b pec (de Vaucouleurs)
See UGC 08898
In Arp's class "spiral galaxies with large high surface brightness companions
on arms"; "arcs of high surface brightness around nucleus of companion [UGC
08898]" (Arp)
Twisted plane
Several small galaxies near

9. 1971CGPG..C...0000Z
Re:CGPG 1356.5+3740
I Zw 077
NGC 5395
Disrupted blue Sc (interconnected with NGC 5394).
(Several faint compacts in neighborhood.)
m(pg) = 12.6 [CGCG]

10. 1964RC1...C...0000d
Re:NGC 5395
= Holm 563a
Small, bright nucleus in a bright bulge. One main arm with some knots. Strong
dark lanes on one side. Signs of distorsion by NGC 5394.
Lick 13 dimensions are for the bright part only.
Interacting pair with NGC 5394 at 1.9 arcmin.

11. 1959VV....C...0000V
Re:VV 048a
= NGC 5395
Yerkes Type: afS5

12. 1918PLicO..13....9C
Re:NGC 5395
A rather irregular spiral 2' x 1' in p.a. 0^deg^; almost stellar nucleus. Wide
dark lane on western side.

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