Date and Time of the Query: 2019-05-24 T05:36:09 PDT
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Notes for object NGC 1358

14 note(s) found in NED.

1. 2009ApJ...696.1218Z
Re:NGC 1358
NGC 1358. The log([O III]/H{beta}) and log([N II]/H{alpha}) line ratios, 1.0542
and 0.3032 respectively (Ho et al. 1997a), place it in the Seyfert 2 region of
the BPT diagram. Shu et al. (2007) report an [O III] luminosity, log(L[O III]) =
40.86 erg s^-1^. The SMBH mass is determined to be 6.56 +/- 2.50 * 10^7^ M_sun_
(Wu & Han 2001). This implies an Eddington ratio of 0.029.

2. 2001ApJS..133...77H
Re:NGC 1358
NGC 1358 (S2). - Both Ulvestad & Wilson (1989) and Nagar et al. (1999)
have noted that the core of NGC 1358 may be slightly extended. Our
full-resolution 20 cm and tapered 6 cm maps show quite clearly that the
nucleus is straddled by a jetlike linear feature with a total extent of
~8.6 kpc along P.A. = 101^deg^. We note that the optical major axis of the
galaxy is at P.A. = 165^deg^, and so the extended radio emission is likely
to be associated with the AGN rather than the galaxy disk.

3. 2000ApJ...544..747S
Re:NGC 1358
In this galaxy, the near-UV nuclear features and spectral distribution
are well represented by the bulge template alone (Fig. 14a). There is some
contamination of the Ca II H + H{epsilon} absorption by
Ne III {lambda}3968 + H{epsilon} emission.

4. 1999ApJS..120..209N
Re:NGC 1358
NGC 1358 (type 2; Fig. 6) - A Gaussian deconvolution of the 20cm
source suggests a small extension in P.A. between 116^deg^ and
138^deg^, consistent with the extension seen in the lower contours. It
is not certain if the faint extension seen in the 3.6cm map is real. We
classify the source as "(S)" with a 20cm (and overall radio) P.A. of
120^deg^. Paper VII measured a 20cm flux of 3.8 mJy (in agreement with
the present flux) and a 6 cm flux of 1.2 mJy. There is a weak confusing
source 6' away and a stronger confusing source 13.5' away, both of
which do not clean out very well. ESGC lists galaxy major axis P.A. =
165^deg^ at an external diameter of 4.07' x 3.08' in B. The printed
edition of RC3 lists major axis P.A. = 165^deg^ and log R_25_ = 0.1.
However, the updated on-line version of RC3 (available at NED) does not
list a P.A. Second-generation DSS images show that the galaxy is very
close to circular.

5. 1998MNRAS.297..579C
Re:NGC 1358
NGC 1358. The nuclear FC contributes 17 per cent of the flux and is polarized by
1.7 per cent in the 3200-6300 A range, according to Kay (1994). The Ws of
NGC 1358 (Fig. 15) show no systematic gradient and have values typical of an S1
template. The same result as obtained by Storchi-Bergmann & Pastoriza (1989).
The only exception is Ca K, which reaches values larger than S1 at r=-6 arcsec.
The continuum ratios show a gradient from values typical of an S1 template at
the nucleus to bluer values typical of an S5 template farther out. This galaxy
is another case in which the continuum ratios outside the nucleus have values
bluer than those expected from the analysis of the Ws.

6. 1997ApJS..112..391H
Re:NGC 1358
NGC 1358.--This object provides an excellent illustration of the potential
ambiguities and limitations of our method. If we make the usual assumption that
the [S II] lines provide a good model for the narro component of H{alpha} and
[N II], then our automatic fitting procedure indeed claims to find a weak
(f_blend_~13%) broad H{alpha} line with FWHM~2200 km s^-1^ (Fig. 7a). Note,
however, the sizable residuals near [N II] {lambda}6583, signifying that our
adopted model profile does not give a very good fit (the model profile is too
narrow). Furthermore, although this discrepancy is fairly noticeable in this
instance, it could easily have been missed were it not for the high S/N of the
spectrum. If we instead assume that the profiles of narrow H{alpha} and [N II]
are identical but different from [S II], the algorithm reports an extremely
weak broad feature (f_blend_~2%) shifted toward [N II] {lambda}6583 (Fig. 7b:
the broad component is not visible at the scale of the plot). For lack of any
alternative, the latter set of conditions sometimes must be imposed for objects
whose [S II] profile is noticeably different from that of [N II] (e.g.,
NGC 4321) and in cases for which the [S II] region is simply too noisy (e.g.,
NGC 266) or corrupted (e.g., NGC 315) to yield a reliable model profile.
Finally, if we make no assumptions about the similarity of the narrow H{alpha},
[N II], or [S II] profiles, no broad H{alpha} component is required at all
(Fig. 7c); the final fit finds that the FWHMs of H{alpha} and [N II] (both
nearly identical) are only marginally (10%) larger than that of [S II],
although their wings are significantly broader (by about 30%). Thus, for
NGC 1358 the most conservative conclusion, adopted here, is that broad H{alpha}
is not present.

7. 1997ApJS..110..299M
Re:NGC 1358
Bar is visible in both the ellipse fits and the K_S_image.

8. 1997ApJS..108..155G
Re:NGC 1358
This is an S2 nucleus in an S0 host galaxy. The H{alpha} in Figure 10
has not had the continuum image subtracted because this subtraction
introduces so much noise that it affects strongly the detection of the
H II regions in the arms; nonetheless, the emission in these H II regions
is just H{alpha}, as they are not detected in the continuum frame. An
expanded image of the circumnuclear pure H{alpha} emission is shown in
Figure 11a. Two almost symmetrical arms emerge from the ends of the
stellar bar, which are traced by H II regions. The nucleus is extended 6"
in a linear structure at P.A. = 130^deg^; this structure is resolved in
the nucleus and two knots at 2" each side.

9. 1996ApJS..102..309M
Re:NGC 1358
Our H{alpha} and continuum images of this Seyfert suggest the host galaxy is
of type SBa. The [O III] image is fairly symmetric about the nucleus with an
S-shaped morphology on small (<2") scales. The large-scale nebulosity extends
along the direction of the galactic bar. The excitation map has a morphology
similar to that of the [O III] image, with the highest excitation gas located
at the nucleus. There is evidence for an unresolved red region in the color
map. However, unlike most of the sample galaxies that show such a feature, the
red region is not coincident with the nucleus, as determined by the continuum
peaks. Instead, it is offset ~ 1.5" (570 pc) to the west. This location is
close to that where the ridge in the emission-line images appears to bend,
suggesting the curvature in the emission line morphology could be related to
obscuration by a dust cloud.

10. 1994CAG1..B...0000S
Re:NGC 1358
Oct 1/2, 1978
103aO + GG385
45 min
NGC 1358 is a later example of the same type of morphology as the
other galaxies on this panel having the NGC 0210 look. The bar is well
defined. The connecting points of the bar and the bright, thin spiral
arcs are poorly defined in very much the same way seen in NGC 210
itself (Hubble Atlas, p. 22; panel 124 here), but are even less well
defined here.
Based on the existence of many HII regions in the outer arms, NGC
1358 is in the last third of the SBa morphological box. However, the
bar and inner disk are smooth, placing the overall morphology near the
middle of the SBa section.

11. 1994CAG1..B...0000S
Re:NGC 1358
Oct 1/2, 1978
103aO + GG385
45 min
The bright segments of arms in NGC 1358, which if wound tighter
would form a broken internal ring like that in NGC 3081, is later
along the SBa segment than the three galaxies in the top row. The
regions in which the arms emerge from the ends of the bar are not well
defined - a common feature among most galaxies having the NGC 210
look. NGC 1350 and NGC 2217 to the right, are nearly at the same place
in the classification sequence, near the middle third of the SBa
morphological box.

12. 1976RC2...C...0000d
Re:NGC 1358
Non-interacting pair with NGC 1355 at 6.8 arcmin

13. 1964RC1...C...0000d
Re:NGC 1358
Very small, very bright nucleus
in a short narrow bar: 0.55 arcmin x 0.1 arcmin
Weak arms form pseudo (r): 1.5 arcmin x 1.3 arcmin
Non-interacting pair with NGC 1355 at 6.8 arcmin.

14. 1963MCG3..C...0000V
Re:MCG -01-10-003
Remarkable object. According to vB - S(B)b-II:.

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