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Notes for object NGC 3690

19 note(s) found in NED.


1. 2006ApJS..164...52S
Re:NGC 3690
The bottom left panel of Figure 14 presents the radio image of this galaxy. The
bulk of the emission is concentrated in a region with a diameter of 50". The
emission in this region consists of several blobs and some faint emission
surrounding it. Fainter emission can be seen toward the NW. The radio and
H{alpha} emission of this galaxy have similar structures (Armus et al. 1990).

2. 2003ApJS..146....1W
Re:NGC 3690
NGC 3690.-Although this galaxy is bright, and Galactic O VI absorption
is clearly present, it cannot be measured since the continuum placement
is too uncertain, partly because intrinsic, redshifted Si II
{lambda}1020.699 overlaps the negative-velocity wing of the O VI.

3. 2002MNRAS.329..877C
Re:GB6 J1128+5833
79-redshift from Falco et al. (1999); spectrum in Ho et al. (1995)

4. 2002A&A...390...47S
Re:MRK 0171
Mrk 171: Mrk 171 is a good example of an interacting system.
The main interest of this object is that it is one of the most
extreme cases known of an extended burst of star formation
(Augarde & Lequeux 1985). In Fig. 17 our slit position for
Mrk 171 is shown. Two "A" and "B" regions were covered by the
slit. Comparison with previous long slit observations of the
object by Mazzarella & Boroson (1993) shows that the
star-forming region marked as "A" corresponds to the sum of
the "c" and "g" regions and "B" corresponds to the sum of
the "d", "e" and "f" regions of Mazzarella & Boroson (1993).

5. 2000AJ....119...79C
Re:NGC 3690
NGC 3690 is the most disturbed galaxy in our sample and is
morphologically classified as peculiar (see Fig. 4). It is the only
galaxy in our sample that is interacting strongly with another galaxy,
in this case a probable merger with IC 694 (Gehrz, Sramek, & Weedman
1983).
H I mapping of this galaxy finds no disk structure, and its optical
morphology can be accounted for primarily by bright star-forming regions
(Nordgren et al. 1997). Of our entire sample, NGC 3690 has the largest
difference between ultraviolet and H{alpha} morphologies in the inner
portions of the starburst. It has both H II regions and UV star clusters
without the corresponding presence of the other.
There are four main star-forming regions in the inner parts of this
galaxy pair, called nuclei A, B, C, and C' following Sargent & Scoville
(1991). These clumps are thought to be the main source of the prodigious
far-infrared luminosity of this system. The mid-infrared emission (10
microns) from these sources is extended (Miles et al. 1996), and
compared with 3.4 micron emission, source C is bluest, followed by B,
with A and C' the reddest. NGC 3690 is one of the brightest galaxies in
the local universe in X-rays, with a luminosity L_X_ ~ 10^42^ ergs s^-1^
and an X-ray spectrum consistent with a superwind (Zezas et al. 1998).
Given the very peculiar morphology, the starburst of this galaxy is
a result of the on-going galaxy merger with IC 694. The color map of
this far-infrared-bright galaxy also shows that a significant amount of
dust is present (Fig. 4). Not surprisingly, this galaxy has the largest
ratio of FIR to starburst UV flux (see section 7).

6. 1999ApJ...517..130H
Re:NGC 3690
In most papers on this system, the eastern member of the merging
galaxy pair has been designated IC 694 and the western member as
NGC 3690. However, as pointed out by Yamaoka et al. (1998),
IC 694 is properly the designation of a small E/S0 galaxy located
about 1' to the northwest of the merging galaxy pair. To avoid
further confusion, we will adopt the name Arp 299 to refer to the
system rather than NGC 3690.

7. 1999AJ....118.2331V
Re:NGC 3690
NGC 3960 (Mk 171, Arp 299) has been host to perhaps five SNe in the
past decade: 1990al (Huang et al. 1990), 1992bu (van Buren et al. 1994),
1993G, 1998T (see section 3.2.5), and 1999D (see section 3.1.12).
SNe 1993G (Type II), 1998T (Type Ib/c), and 1999D (Type II) have been
spectroscopically classified; the other two possible SNe (1990al and
1992bu) have been identified only in the radio and infrared,
respectively. A single short-exposure F606W image is available for
NGC 3690. Adopting the absolute position for SN 1993G from Forti (1993;
we assign an uncertainty radius 2"), we find that the SN appears to have
occurred well outside the main body of the interacting system, in a
region of faint emission with no resolvable stars.

8. 1999AJ....118.2331V
Re:NGC 3690
The SN II 1999D recently occurred (Qiu, Qiao, & Hu 1999) in the
same interacting galaxy as SN 1993G (section 3.1.10). The SN occurred
near the outer edge of the galaxy, in a region of faint diffuse
emission. Within a 2 " error circle around the SN's position are two
unresolved star clusters, with m_F606W_ ~ 20.2 and 19.8 mag,
respectively, along a more inward spiral arm.

9. 1999AJ....118.2331V
Re:NGC 3690
The SN Ib 1998T occurred (Li, Li, & Wan 1998) in the same
interacting host galaxy as SNe 1993G and 1999D; we show the SN
environment in Figure 14. We tried to isolate the progenitor in this
pre-SN image. Unfortunately, given the distance to NGC 3690 (~42 Mpc,
for H_0_ = 75 km s^-1^ Mpc^-1^ and cz = 3121 km s^-1^) and the short
exposure time, no individual stars can be resolved. However, from the
accurate position of the SN (11^h^28^m^33.14^s^, 58^deg^33'44.0",
J2000.0, from an R-band image taken with the Lick Observatory 0.75 m
Katzman Automatic Imaging Telescope; see also Yamaoka et al. 1998) with
a 2" radius uncertainty, we see that the SN occurred among the bright,
dense concentrations of star formation occurring in this galaxy. This
single image of the SN environment implies that the SN progenitor was
likely a massive star.

10. 1999A&AS..136...35S
Re:NGC 3690
NGC 3690 -- Ho et al. (1995) signaled the presence of WR features in
several regions of this galaxy (=Arp 299); they exclude WR features in
the nucleus. Vacca (1996, private communication) signals the presence of
broad He II {lambda}4686 in Arp 299B and Arp 299C which are part of this
complex system.

11. 1998AJ....116.2682C
Re:IRAS 11257+5850
Arp 299, NGC 3690 + IC 694. VLA 8.4 GHz A-configuration map in Condon
et al. (1991b).

12. 1997AJ....114...77N
Re:NGC 3690
5.3 NGC 3690-IC 694
The NGC 3690-IC 694 system (also known as the multiple nuclei source Mrk 171)
is strongly interacting making the morphology difficult to interpret [Figs.
5(a) and 5(b)]. Arp 296 (the barred spiral to the NE, coupled with its
interacting edge-on companion) can also be seen in the figure. Since no H I was
detected in the VLA bandwidth it must be more than 500 km s^-1^ removed from
NGC 3690-IC 694.
NGC 3690-IC 694 has no disk like structure, but instead consists of an
amorphous collection of bright star forming regions, dust lanes and a long
stellar tail extending to the north. H I is seen in absorption against the
brightest optical region [dashed contours in Fig. 5(a)]. There is a local
maximum of H I emission on either side of this absorption; however, as can be
seen from the velocity contours [Figs. 5(c) and 5(d), see also Fig. 6(b)], they
are at entirely different velocities. Further, the emission at the southern tip
is also at an anomalous velocity, and is clearly not related to the lower
velocity material which seen in projection appears to partly overlap with it.
This southern material may be some kind of remnant of a counter tail to the
long northern tail. It is also interesting to note that none of the peaks of
H I emission seen in the higher resolution map [Fig. 5(b)] corresponds to a
region of star formation. This mismatch between H I and optical emission also
extends to the northern tail [Fig. 5(a)], the H I tail is offset from the
stellar tail by approximately one beamwidth.
The most dramatic feature of the H I maps is the long tail to the north, it
extends to more than ~100 kpc from the main body of the stellar emission. There
is a knot of H I emission at the tip of the tail, at a velocity somewhat
different from that of the tail material immediately adjacent to it. The
velocity gradient in the tail is itself nonmonotonic, reaching a maximum near
the center of the tail. It is possible that material from this tail is falling
back into the main system.
Figure 6(a) is the simulated single dish spectrum for the entire area of H I
emission. The large absorption in the center is clear. Spectra along a single
natural weighted beam were produced for the two H I maxima and the H I
absorption seen in the main stellar body [Fig. 6(b)].

13. 1996ApJS..104..217S
Re:NGC 3690
3.11. UGC 6471/2
UGC 6471/2 is the well-known interacting pair IC 694 and NGC 3690. The eastern
source is identified as UGC 6471, IC 694, or NGC 3690A. The western source,
UGC 6472, consists of NCC 3690B1/B2, NGC 3690C, and NGC 3690C'. Several
additional knots of emission are visible in the K image. Near-infrared color
maps show the main nuclei as well as a reddened ridge of emission extending to
the southeast of UGC 6471. All the main nuclei show strong emission features.
The near-infrared spectra do not have sufficient spatial resolution to resolve
components B1 and B2. Due to its proximity, this is one of the most widely
studied interacting starburst systems.

14. 1996ApJ...465..191M
Re:NGC 3690
3.4. NGC 3690
NGC 3690 is a galaxy merger with several bright nuclei. Among the brightest
four nuclei, the westernmost three are cataloged as NGC 3690, while the
easternmost one is catalogued as IC 694. Altogether, the system has also been
catalogued as Arp 299. We follow the convention of Sargent & Scoville (1991)
and refer to the four nuclei as NGC 3690A, B, C, and C' as notated in Figures
8 and 9.
Figure 8 shows the eastern nucleus (source A), and Figure 9 shows the western
complex (sources B, C, and C') plotted on the same scale. Both images are
undeconvolved because the character of the PSF apparently changed as the
telescope was moved from the standard star {mu} UMa to the galaxy. The PSF for
the galaxy seems to have a four-lobe character, seen in all four compact
sources in the galaxy, compared with the normal three-lobe character of the PSF
(as in Fig. 3). The four-lobe character of this PSF may be a result of the 5 m
primary mirror deforming slightly at certain telescope positions (in this case,
altitude 55^deg^, azimuth 30^deg^). Therefore, the subarcsecond structure near
the nuclei in these images must be interpreted with care.
The large-scale extended emission, however, is real. This large-scale structure
is very faint, and the images were smoothed with a {sigma} = 8 pixel Gaussian
profile and plotted with logarithmic contours to bring out the low-level
structure. Source B has an arm of emission extending 1100 pc to the northwest
(PA 292^deg^). Source C' has a lobe extending ~600 pc toward the southwest
(PA 237^deg^). Source A is marginally resolved to be 0.3" (60 pc) in size.
Source B is unresolved.
Zhou, Wynn-Williams, & Sanders (1993) observed this galaxy at 3.4 microns.
Comparison of the peak emission in each of the four sources yields qualitative
characterization of the amount of dust involved: sources A and C' are the
reddest, source B is intermediate, and source C is the bluest.
CHYT find all four sources resolved and surrounded by diffuse emission in the
radio. Source C' shows the same arm reaching to the southwest as in the 12.5
micron map. Source A is measured to be 0.38" x 0.28" (80 pc x 60 pc),
elongated at a position angle of about 120^deg^. This result is also suggested
in the 12.5 micron map but with low confidence because of the uncertain
characteristics of the PSF. Source B is marginally resolved in their map at
0.18" (36 pc).
Optical imaging by Armus et al. (1990) has shown source A to be extended over
several arcseconds with no unresolved core, implying that it must be embedded
in dust. Sources B and C are unresolved, while source C' does not appear. No
obvious tidal tails are evident, possibly because one of the original galaxies
was an elliptical (Telesco, Decher, & Gatley 1985). Nevertheless, it has a
very irregular optical morphology (Fig. 1).

15. 1995ApJS...98..477H
Re:NGC 3690
NGC 3690 is one of several W-R galaxies in our study. We oriented the
slit along two different PAs, one in order to include the bright
emission-line knot to the east of the nucleus (P.A. = 80.7^deg^), and
another to intersect additional features (PA = 163.2^deg^). Emission
lines from W-R stars are present in several regions; however, they are
not present in the nucleus (Fig. 40). A detailed discussion of NGC 3690
and other W-R galaxies in our sample will be presented elsewhere.

16. 1994CAG1..B...0000S
Re:NGC 3690
Karachentsev 288
Sc(tides)
PH-8058-S
Feb 4/5, 1981
103aO
12 min
A close encounter is clearly in progress in
this close pair whose separation of centers is 26".
Karachentsev lists the individual v_o redshifts as
3156 km/s and 3196 km/s. At the redshift
distance of 64 Mpc (H = 50) the projected linear
separation is 8 kpc. A possible third E companion
exists at a separation of 66", but it may
be in the background.
The morphology of each companion is highly
disturbed. Faint outer plumes are associated with
each galaxy.

17. 1993ApJS...86....5K
Re:NGC 3690
NGC 3690 + IC 694; Sc pec, starburst.
The IUE aperture contains both objects in this pair of "colliding or
strongly interacting" galaxies (de Vaucouleurs, de Vaucouleurs, & Corwin
1976), the partner being IC 694. This system is the most representative
example of intense and widespread star formation activity, presumably
triggered by an interaction (Gehrz, Sramek, & Weedman 1983). It is a
strong radio source (Condon et al. 1982), has a high infrared luminosity
(L_IR_ ~ 5 X 10^11^ L_sun_; Carico et al. 1988), and has the most
luminous optical emission lines of any non-Seyfert galaxy (Weedman 1972).
All of these properties may be explained within a starburst model. The
system has a complex morphology: three brightest regions can be
identified in the optical, radio, and IR bands-region A (nucleus of IC
694), region B (nucleus of NGC 3690), and region C. All of them are
starbursting (Gehrz et al. 1983). In region A there is both a radio and
an IR unresolved source, from which 60% of the far-infrared luminosity of
the system originates (Joy et al. 1989). This source might be compact and
may not be explainable with thermal processes (Gehrz et al. 1983). The
remaining 40% of the far-infrared emission originates from a compact
source in NGC 3690, probably the extranuclear region C (Joy et al. 1989).
The absorption-line-rich UV spectrum confirms the intense thermal
activity of NGC 3690. Because of the relatively high redshift of this
galaxy (z = 0.012), the Ly{alpha} absorption line is detected.

18. 1976RC2...C...0000d
Re:NGC 3690
= MRK 171
= Arp 299
= VV 118
= Kara[72] 288
Note correction to Arp Atlas number.
Colliding or strongly interacting pair, and faint compact [= IC 0694]
50 arcsec north-west, at same redshift (M.N.R.A.S., 153, 383, 1971.
Ap. J., 173, 7, 1972).
Photometry (UBV):
Source N, log A = 1.03, V = 11.85, B-V = 0.56, U-B = -0.34 for both.
Ap. J., 171, 5, 1972.
Photometry (5, 10 microns):
Ap. J. (Letters), 176, L95, 1972.
Spectrophotometry:
Astrofizika, 7, 389, 1971.
Ap. J., 171, 5, 1972.

19. 1964RC1...C...0000d
Re:NGC 3690
Colliding pair. 2 very complex nuclei: 0.3 arcmin separation. Irregular
spiral-like arms.
Yerkes 2 (Morgan, 1959) classification: a?Ip + a?Ip.
[IC 0694 is a small E or S0 50 arcsec northwest.]
Magnitude:
Ap. J., 85, 325, 1937.


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