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Date and Time of the Query: 2019-05-19 T08:25:34 PDT
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Notes for object NGC 4138

10 note(s) found in NED.


1. 2009ApJ...690.1322W
Re:NGC 4138
NGC 4138. Alternatively, this source can be fit with a partial covering
model with a high amount of scattering (> 99%). Further, the blackbody
component can alternatively be fit with an apec model of similar
temperature with no difference in {chi}^2^.

2. 2002A&A...392..817F
Re:NGC 4138
3.5 NGC 4138
No ULX was detected inside the D_25_ ellipse (figure not shown). The flux
limit is about 10^-14^ erg cm^-2^ s^-1^ for this observation.

3. 2001ApJS..133...77H
Re:NGC 4138
NGC 4138 (S1.9). - The nucleus is badly confused by two very strong
sources (S_20_ = 1.3 and 0.33 Jy) located ~3.5' to the southwest. The rms
noise of the tapered 20 cm map is quite high. Nonetheless, a weak, compact
core with an inverted spectrum (S_6_ = 0.78 mJy, S_20_ = 0.51 mJy,
{alpha}_6_^20^ = 0.45) is seen at the position of the optical nucleus. The
only other previous radio observation is that of Wrobel & Heeschen (1991),
who placed an upper limit of S_6_ < 2 mJy ({DELTA}{theta} = 5").

4. 1999ApJ...519...89C
Re:NGC 4138
NGC 4138.-This spiral galaxy has a nucleus classified as "S1.9" by
HFS95. However, we found no X-ray emission from NGC 4138.

5. 1997ApJS..112..391H
Re:NGC 4138
NGC 4138.--This is one of several previously unrecognized Seyfert galaxies
discovered in our survey (Paper III). The narrow lines of H, [N II], and [S II]
have symmetric profiles that can be well described by single Gaussians. Visual
inspection of the regions between H{alpha} and [N II], further confirmed by
detailed fitting, reveals a relatively weak broad H{alpha} line responsible for
~23% of the emission from the entire blend (Fig. 11d).

6. 1994CAG1..B...0000S
Re:NGC 4138
Sa(r)
(I,S,1/2)
PH-8000-S
Feb 2/3, 1981
103aO
12 min
The narrow dust lane silhouetted against the
disk of NGC 4138, well visible in the print here,
can be traced only for about one-fourth of a
revolution. The galaxy is clearly neither S0 nor
Sb. The luminous material in the outer part of
the disk forms a spiral pattern. There is no
evidence for HII knots in the arms. Hence,
although the bulge is small, the type must be Sa.
The S0(late) classification in the RC2, based on
a Mount Wilson 60-inch plate, is inappropriate.

7. 1993AJ....106.1405P
Re:NGC 4138
NGC 4138. This galaxy was originally described by PE87, but the data were
of poor quality. During our reanalysis of the PE87 images for this paper,
we found that the nucleus was strongly distorted by the presence of a
foreground star that-was slightly brighter than the nucleus and separated
by only ~4". The combination of poor seeing (2.7") and the finer sampling
(0.26"/pixel) of the GEC CCD used for these images caused a great deal of
trouble. Thus, we reobserved this galaxy with the OSU IFPS, and present
the new images in Fig. 1(a). The problem was primarily in the nuclear
regions, and with better seeing we confirm the ring of the bright H II
regions in the disk reported in PE87, resolving many blobs into discrete
regions, and detecting many fainter regions. The integrated H{alpha}
flux reported in PE87, however, is in error by a factor of ~3, and we
give the revised value in Table 2.

8. 1976RC2...C...0000d
Re:NGC 4138
QS0 3C 268.4 at 2.9 arcmin (z = 1.400).
Photograph:
Ap. J., 170, 233, 1971.

9. 1973UGC...C...0000N
Re:UGC 07139
SA(r)0+ (de Vaucouleurs)

10. 1964RC1...C...0000d
Re:NGC 4138
Small, bright nucleus with a star attached. (r): 0.65 arcmin x 0.4 arcmin
with strong inner dark lane.
See also HA, 105, 231, 1937.


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