Date and Time of the Query: 2019-06-25 T13:19:14 PDT
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Notes for object NGC 1187

11 note(s) found in NED.

1. 2004MNRAS.355.1251L
Re:NGC 1187
NGC 1187 and 1302 (see Fig. 2a). In the case of NGC 1187, in which the
bar is small, including a bar component to the decomposition decreases
the shape parameter of the bulge from n = 2.0 to 1.4, thus making the
bulge profile appear more exponential. Consequently, the total flux of
the bulge is decreased by 30 per cent. However, the disc model is not
affected. An example of a galaxy with a larger bar is NGC 1302, for
which inclusion of the bar affects not only the fitted bulge, but also
the radial scalelength of the disc, which is reduced by 12 per cent.
The bar resides inside a roundish inner ring and is prominent in the
bulge-dominated region of the galaxy. For this galaxy, the bulge/disc
decomposition without any bar model would overestimate the mass of the
bulge by as much as 36 per cent. The effect of the bar model in the
decomposition for NGC 1302 is demonstrated in a different manner in
Fig. 3. Two residual images are shown for two different decompositions:
in one image the bulge model is subtracted from the original image,
whereas in the other image the whole galaxy model is subtracted. It is
clear that if no bar model is included in the decomposition the bulge
model becomes too large, mainly because a considerable amount of bar
flux is assigned to the bulge.

2. 2002ApJS..143...73E
Re:NGC 1187
NGC 1187.---SB(r)b: Strong bar emerging along the major axis of an
elliptical bulge (with nuclear point source). Spiral arms emerge from
the ends of the bar. Arm beginning in the SE (and turning to the west)
is fairly regular. Arm beginning at the NW end of the bar begins
heading N, then fades out, and reappears to the east, heading SE. Arms
have a few bright knots.

3. 1997A&AS..125..479J
Re:NGC 1187
NGC 1187 (SBc, 1"~82 pc, I=46.7^deg^)
The ellipticity grows to its maximum (e_max_=0.60) at a=32", reflecting the
large-scale bar from the tips of which two-arm spiral structure emanates. The
PA is roughly constant inside the bar except the innermost region (a=2-7")
where a 15^deg^-twist occurs. After the deprojection (PA_disk_=130^deg^), a
possibility that the system is double-barred emerges: the PA is essentially
two-fold and there is a new maximum in ellipticity at about 3". In case that
the secondary bar really existed, it would be nearly perpendicular to the
primary one ({delta}PA=87^deg^). However, we believe that such an appearance is
likely to be an artefact of a wrong deprojection (cf. Fig. 1) and, in
accordance with rules established in Sect. 3, we classify the galaxy only as
having a twist.

4. 1994CAG1..B...0000S
Re:NGC 1187
Aug 7/8, 1980
103aO + GG385
45 min
The light print on the right shows that the
inner-arm pattern is composed of three
high-surface-brightness grand design spirals. Each
begins near the small central nucleus, which itself
is of very high surface brightness and which has a
starlike image at the center at the 0.8" resolution
of the available plate material. The two principal
arms of the inner triad pattern can be traced for
about three-quarters of a revolution outward
before they abruptly decrease in surface brightness;
beyond that point, lower-surface-brightness
arm fragments exist, shown best at the left.
This pattern - bright, well-defined inner
arms, abrupt surface-brightness change, and
fragments beyond the point of change - is common,
and has been seen earlier in this section.
Sbc examples are NGC 1566 (panel 171), NGC 5248
(panel 174), NGC 7171, NGC 4603, and
NGC 3430 (panel 176), NGC 3433 (panel 177),
NGC 2369 and NGC 3981 (panel 178), and
NGC 3726 (panel 181).
The largest of the numerous HII regions
everywhere in the arms resolve at the 2" level.
The redshift of NGC 1187 is v_o = 1424 km/s.

5. 1993ApJS...88..415R
Re:NGC 1187
This galaxy is notable for how well the H II regions delineate the bar,
inner ring, and almost the entire length of each of its half-dozen or so
arms, "like beads on a necklace" to paraphrase Baade (1963). The two
major arms appear to be extensions of the bar, which leads to the
impression that they intersect perpendicularly with the inner ring of
H II regions. In this respect, NGC 1187 is similar to the southern
SB(rs)bc galaxy NGC 613 (Dottori & Copetti 1989). The faint circle and
band in these images are remnants of earlier CCD saturation, while the
ring is scattered light in the focal reducer from a bright star just
outside the field of view. Following up on the suggestion by Porter &
Filippenko (1987), we have examined our H{alpha} image of NGC 1187 for
signs of any H II regions associated with the reported position (Argyle &
Sinclair 1982) of the Type Ib supernova SN 1982R. From astrometry of the
field stars in the Guide Star Catalog, we can confirm that the nearest
significant H{alpha} emission to SN 1982R is some 3" south. Thus, unlike
many of the other Type Ib supernovae in late-type galaxies studied by
Porter & Filippenko, SN 1982R is not closely associated with an
underlying H II region.

6. 1985SGC...C...0000C
Re:NGC 1187
Plate 3649
Overexposed center, patchy bar and arms with many knots. IBm IV 4.5 north-
preceding with bright star 0.9 south-preceding.
Plate 3749
Overexposed center, very bright inner arms, many knots; (R'): 4.3 x 3.3.
SB(s)0+pec 4.5 north-preceding.
Plate 5455
On plate edge.

7. 1982ESOU..C...0000L
Re:ESO 030024-2303.8
=ESO 480- G 23
involving ESO 480- G 20

8. 1976RC2...C...0000d
Re:NGC 1187
Non-interacting pair with a small anonymous galaxy
SAB(r)0/a? at 21 arcmin

9. 1974UGCA..C...0000N
Re:UGCA 049
UGCA 049:
= NGC 1187
SB(r)c (RC1)
south-south-following of 2 (two): paired with
companion at 4.5, 332, 1.1 x 0.6 , Sa-b, probably background

10. 1964RC1...C...0000d
Re:NGC 1187
Very small, very bright nucleus.
(r): 1.4 arcmin x 0.8 arcmin
Several filamentary knotty arms.
Non-interacting pair with a small anonymous
SAB(r)0/a? at 21 arcmin.
Error on corrected redshift in HMS (Lick velocity).
A.J., 61, 97, 1956.

11. 1956AJ.....61...97H
Re:NGC 1187
HMS Note No. 020
Nuclear absorption lines of poor visibility.
H{beta} and H{gamma} in emission (HMS Plate IVe).

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