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Notes for object NGC 4593

23 note(s) found in NED.

1. 2009ApJ...705..962C
Re:NGC 4593
High-velocity Si III is detected in this sight line in two unusual narrow
features, one centered at V_LSR_ ~ 100 km s^-1^ and the other at V_LSR_
~ 275 km s^-1^. These detections are confirmed by corresponding detections
of each feature in Si II {lambda}1260.42, and of the lower velocity feature in C
II {lambda}1334.53. The lower-velocity feature appears to extend out to larger
positive velocity in the Si III profile. Because this part of the feature is not
present in the Si II and CII profiles, we use the velocity extent of the lower
ions for the Si III integration.

2. 2007AJ....134..648M
Re:NGC 4593
NGC 4593 (Figs. 7.10, 9.10, 20.10): Apart from the bright nucleus, there is a
spiral structure of 1 kpc width with many individually resolved star clusters.

3. 2006ApJ...638..642B
Re:NGC 4593
NGC 4593 - A Seyfert 1 galaxy in the Virgo region at z = 0.009 that shows
a cutoff power law with GAMMA = 1.0 ^+^_-_and E^cut^ = 35^+^_-_ keV and is
detected up to 150 keV (Fig. 3), with a flux of f20-100 keV = 6.8 x
10^-11^ ergs cm^-2^ s^-1^ (Chi^2^nu_ = 1.00). This is significantly
different from the spectrum measured by BeppoSAX, GAMMA =
1.94^+0.06^_-0.05_ and E^cut^ >> 222 keV (Guainazzi et al. 1999), but with
a similar flux (f20-100 keV = 7 x 10^-11^ ergs cm^-2^ s^-1^).

4. 2004MNRAS.350.1049G
Re:NGC 4593
9.17 NGC 4593 Oknyanskij & Horne (2001) conclude from the data of
Santos-Lleo et al. (1994) that there is a delay of 36 +- 15 d between
the J and L variations. The present analysis yields 55 d.

5. 2004MNRAS.350..140S
Re:NGC 4593
2.2.2 NGC 4593 Compared with Fairall 51, NGC 4593 is relatively weakly
polarized. Nevertheless, its polarization spectrum is clearly similar in
form to that of Fairall 51 (Fig. 2). Although the continuum polarization
is barely measurable in the red, it increases steeply below
6000{Angstrom}, to 0.7 per cent. Again, there are strong local increases
in p associated with broad H{alpha}, and less clearly, H{beta}. A similar
feature, possibly associated with the broad He I{lambda}5876 emission-line,
is sensitive to the error binning (see S02) and may be spurious. There
are no significant variations in {theta} over the spectrum. In polarized
flux, the broad H{alpha} line appears slightly blueshifted relative to the
total flux line profile. The radio source is unresolved in several sets
of Very Large Array (VLA) observations obtained at various frequencies
(Ulvestad & Wilson 1984a; Ulvestad & Wilson 1989; Thean et al. 2000;
Schmitt et al. 2001a).

6. 2004ApJ...613..682P
Re:NGC 4593
NGC 4593. This is another object from the LAG campaign in 1990 (Dietrich
et al. 1994), where the data have been reanalyzed by Onken et
al. (2003). We regard the H{beta} lag as completely unreliable because
it is so much smaller than the mean sampling interval. The H{alpha} lag
should also be regarded with some caution.

7. 2004A&A...415..941E
Re:NGC 4593
NGC 4593: Listed by Moiseev (2001), based on the suggestion of a triaxial bulge
by Wozniak et al. (1995). The latter authors noted the presence of dust and a
blue nuclear ring with r ~ 2". Inspection of a NICMOS2 F160W confirms that the
central region of this galaxy is dominated by spiral dust lanes surrounding a
nuclear ring or pseudo-ring; there is no evidence for an inner bar.

8. 2003ApJS..148..327S
Re:NGC 4593
5.37. NGC 4593
The [O III] image of this Seyfert 1 galaxy (Fig. 11, top left) has a
halo-like morphology, slightly elongated along P.A. = 100^deg^, which
is a direction similar to the host galaxy major axis. The extent of
the emission in this direction is 1.7" (300 pc), while along the
minor axis the emission is extended by 1.35" (240 pc). The radio
emission of this galaxy is unresolved (Schmitt et al. 2001b).

9. 2003ApJS..146..353M
Re:NGC 4593
NGC 4593 (TW)
This galaxy has a tightly wound, one-arm nuclear spiral. It is
somewhat unusual in that no other dust features outside of the one
dust spiral are visible in the central kiloparsec. The circle to the
right in the H image and color map is an artifact of the NIC2

10. 2002ApJS..143...73E
Re:NGC 4593
NGC 4593.---SBa: Bright nuclear point source embedded
in a large elliptical/boxy bulge. A strong bar emerges from
the NE and SW corners of the boxy bulge. The ends of the
bar coincide with the edge of an inner disk or lens. Two very
diffuse, smooth open spiral features emerge from the ends of
the bar. They can both be followed for ~150deg--180deg before
fading. There is evidence for a third arm emerging from the
inner disk on the south side of the galaxy.

11. 2002A&A...389..802P
Re:NGC 4593
NGC 4593. This observation was published by
Guainazzi et al. (1999a). N_s_ is negligible compared to
N_g_, and N_W_ = (2.3 ^+1.1^_-0.9_ x 10^21^ cm^-2^ with
X_i_ ~ 9 erg cm s^-1^. The iron line is resolved, W_{alpha}
together with R are the largest in our sample.

12. 2002A&A...389...68G
Re:NGC 4593
NGC 4593: this is a strongly barred galaxy for which there are
three published catalogs of HII regions. Our two methods are in
good agreement for the richer catalogs but the first method gives
discordant results in the second catalog and the second method
does not work at all. Thus we discard the values from the second
catalog. The mean of our values are also in general agreement
with the photometric values, except for the case of the I photometry
by Schmitt & Kinney (2000) who give a higher PA value than the rest.
We adopt the mean values of the results of our two methods applied
to the first and third catalog.

13. 2001ApJ...550..261W
Re:NGC 4593
3.3.8. NGC 4593 (Mrk 1330)
The 2-10 keV flux increases by 25% between the two ASCA pointings,
approximately 3.5 yr apart (Fig. 8h). No changes are seen in the iron line
between these two observations.

14. 1998ApJS..114...73G
Re:NGC 4593
Section A10. NGC 4593
This Seyfert 1.0 galaxy was first detected in X-rays by Uhuru (Forman et al.
1978). In our analysis of the data from the ASCA observation performed in
1994 January, we find model A(i) provides a satisfactory description of the
data analyzed, but fails our criteria for extrapolation <0.6 keV. Fits
satisfying our criteria for acceptability are obtained if ~70% of the
continuum escapes without suffering attenuation by neutral material [model
A(ii)]. However, yet superior fits are obtained if the absorbing gas is
assumed to cover the entire source and is ionized [model B(i)], giving
{GAMMA} ~ 2, U_X_ ~ 0.1, and N_H, z_ ~ 2 x 10^21^ cm^-2^. This confirms the
findings of R97 who found the addition of O VII and O VIII edges ({tau}_O7_ ~
0.3 and {tau_O8_ ~ 0.1) significantly improved the fit to a single-power-law
model ({GAMMA} ~ 2) to these ASCA data. R97 also fitted a single-zone
photoionization model and found U^R97^_X_ ~ 0.05, N_H, z_ ~ 3 x 10^21^
cm^-2^, and {GAMMA} ~ 1.9.
We find that statistically there is no strong requirement for any of the
underlying continuum to escape without suffering attenuation by the ionized
material, or for any significant emission from the ionized gas [models
B(ii)-C(ii)]. In all cases there is no required for any addition absorption
by neutral gas in excess of N^gal^_H,0_. We note that a substantially flatter
spectral index has been suggested in the past (e.g., {GAMMA} ~ 1.1; T91).

15. 1997ApJS..110..299M
Re:NGC 4593
A bar on large scales (>20") is clearly seen in the K_S_image. The
morphology in the inner ~20" is barlike, but this interpretation is not
supported by the ellipse fitting.

16. 1997ApJS..110..299M
Re:NGC 4593
A bar on large scales (>20") is clearly seen in the K_S_image. The
morphology in the inner ~20" is barlike, but this interpretation is not
supported by the ellipse fitting.

17. 1997ApJS..108..155G
Re:NGC 4593
This is a variable S1 nucleus hosted in an SBb galaxy. Ninety percent of
the emission is produced by the nucleus; 10 weak H II regions have been
detected in the disk; some of them are at the end of the stellar bar, at
55" (~9 kpc) from the center. It has circumnuclear emission extended 9"
that looks like a broken starburst ring (Fig. 11c). The vertical spike
from the nucleus in the H{alpha} image is a diffraction artifact from
the secondary mirror spider.

18. 1996ApJS..105...93E
Re:NGC 4593
4.8. NGC 4593
The properties of the Seyfert 1 nucleus in this barred spiral have been
investigated in detail. Optical and infrared photometry (e.g., Winkler et al.
1992; Kotilainen, Ward, & Williger 1993; Kotilainen & Ward 1994), and
spectrophotometry (e.g., Kollatschny & Fricke 1985; Crenshaw 1986; Morris &
Ward 1988) of the nucleus has been obtained at several epochs. These data show
considerable variability of the optical nuclear continuum, which is observed
also at ultraviolet (e.g., Clavel et al. 1983; Clavel 1983; Koratkar & Gaskell
1991) and X-ray (Ghosh & Soundarajaperumal 1993) wavelengths.
Giant extragalactic H II regions tracing the spiral arm structure from an inner
radius of ~30" out to ~80" are readily visible in Figure 1. Most of the H II
regions are compact, with little evidence for the presence of diffuse H{alpha}
emission. Unlike most other barred spirals discussed in this paper, H II
regions in NGC 4593 do not appear to be distributed along the bar. One possible
explanation may be that the radial gas mixing along the bar that would
ordinarily trigger star formation is relatively weak in this object.

19. 1994CAG1..B...0000S
Re:NGC 4593
Hubble Atlas, p. 48
March 22/23, 1980
75 min
NGC 4593 has a strong straight bar with a
characteristic straight dust lane along one of the
leading edges (leading the rotation, whose sense
is inferred from the sense of the spiral pattern).
A nearly complete inner ring is formed by
the arms. One arm begins at the same distance
from the center as where the bar terminates but
at a position downstream by about 15^deg^. The
other principal arm begins at the end of the bar,
as in NGC 1300.
The redshift is v_o = 2505 km/s. The galaxy
is in the southern extension of the Virgo Cluster
at a declination of -5^deg^, near the ridge of the
supergalactic plane.

20. 1991ApJ...381...85T
Re:NGC 4593
The spectral slope in this case is significantly flatter (at 90% confidence)
than that observed in the EXOSAT data (Fig. 3). Although the EXOSAT data showed
evidence for a soft excess, none was found in the SSS+MPC data. The HEAO 1
observation showed {GAMMA} = 1.67, consistent with the EXOSAT index.

21. 1964RC1...C...0000d
Re:NGC 4593
Very bright nucleus in a smooth bar: 1.5 arcmin x 0.25 arcmin. Weak (r):
1.8 arcmin x 1.3 arcmin in a lens: 2.1 arcmin x 1.6 arcmin. 2 main,
asymmetric arms form a pseudo (R): 3.4 arcmin x 2.4 arcmin.
Lund 9 and HA 88,4 minor-axis diameter (0.7 arcmin. 0.8 arcmin) rejected,
bar only.

22. 1963MCG3..C...0000V
Re:MCG -01-32-032
{omega} = 9 degrees, {mu}1 = 74 degrees, {mu}2 = 85 degrees, {phi}1 =
175 degrees, {phi}2 = 178 degrees, l1 = 1.7, l2 = 1.5 arcmin.
According to vB - Sb-II. Photo: Sand - SBb(rs) - description: [L, 2B -->
1{back-s}zfa, 1{back-s}a; R-fb; 1{back-s}cttf, 1{back-s}c --> R-].
In this better photograph, the sleeve of the arm and two arcs turns
into a ring and two arms. An interpretation of the ring and short arms
[{back-s}cttf] as one small arm is also possible. In this case, it is
made of the middle of the arch, where it comes close together. According
to Sandage there are two arms and one of them leaves from the ring.
Interacting with MCG -01-32-033. The single arm connects it with a
companion 19 mag.

23. 1961Hubbl.B...0000S
Re:NGC 4593
Mar. 28/29, 1955
103aO + WG2
30 min
Enlarged 4.0X
The internal circular ring is nearly complete but it is of
nonuniform brightness around the periphery. One spiral
arm begins at the end of the bar. The other begins about
110 degrees around the ring (counted counterclockwise) and can
be traced for nearly one and a quarter turns.

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