Date and Time of the Query: 2019-02-17 T07:25:29 PST
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Notes for object NGC 7284

5 note(s) found in NED.

1. 2006A&A...457..425C
Re:[Sdd95] 546b
P546b (NGC 7284): like Keel et al. (1985), we did not detect emission lines in
this elliptical galaxy.

2. 2006A&A...457..405C
Re:[Sdd95] 546b
P546b (E3): this galaxy was classified as an SB0 peculiar in the RC3 and as an
Sa in the ESO-LV. However, we did not find the presence of a disk when examining
its surface brightness profile. Rampazzo & Sulentic (1992, hereafter RS)
obtained {epsilon}, {theta} (PA), and a_4_/a distributions for this object
(their 96(1)) in the B- and V-bands. We present R profiles less affected by dust
contamination, and our seeing is better than theirs. The maximum value for the
ellipticity distribution in both works is nearly the same: 0.34 in the B-band
and 0.32 in the V-band (RS), and 0.31 in our R profile. The behavior of the
{epsilon} distributions is similar in the region ranging from ~10" to log r =
1.4 ({alpha} ~ 25"), which is the maximum value shown by RS. In that range, the
PA distribution is increasing in both works, but the mean values that we
obtained change from ~105^deg^ to 130^deg^, while the values obtained by RS
change from ~120^deg^ to 130^deg^. Beyond this point, the companion light begins
to influe nce the profiles. To compare the b_4_ distribution of both works, the
values that we obtained must be multiplied by 0.84, as this galaxy is an E3 (see
P316a). According to RS, this galaxy displays a boxy shape (maximum value for
a_4_/a x 100 = -4.1). In our work, b_4_ x 0.83 = a_4_/a = -0.023; this value x
100 = -2.3. Both works obtained a negative value for this distribution; however,
the value obtained by RS is larger. We searched for a probable cause for this
difference. One spiral arm from P546a is overlapping this galaxy image. In our
work, this region was masked before getting the profiles. To perform a test, we
kept this region on the P546b image, and we obtained the distributions again.
Then we got a_4_/a x 100 = -4.7, closer to the value obtained by RS. For close
pairs like this the way the companion image is masked may strongly influence the
results of the b_4_ distribution. We suggest an elliptical shape for this galaxy
because b_4_ ~ 0, with some variations, but according to Governato et al.
(1993), we might consider this galaxy as being boxy-shaped because a_4_/a x 100
< -1.0.

3. 1985SGC...C...0000C
Re:NGC 7284
Plate 4469r
Interacting pair with NGC 7285 at 0.5 with bridges and plumes.

4. 1982ESOU..C...0000L
Re:ESO 222550-2506.0
=ESO 533-IG 31
interacting with ESO 533-IG 32

5. 1959VV....C...0000V
Re:VV 074b
= NGC 7284
Faint part not visible on photograph.

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