Date and Time of the Query: 2019-03-20 T02:30:14 PDT
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Notes for object NGC 4507

16 note(s) found in NED.

1. 2006ApJ...638..642B
Re:NGC 4507
NGC 4507 - Detected by ISGRI and SPI (Seyfert 2, z = 0.012; Fig. 2). The
combined data are best represented by a power law (GAMMA = 1.0) with a
high-energy cutoff (E^cut^ = 55 keV). This is consistent with results from
Ginga and OSSE, which showed GAMMA = 1.3 +- 0.2 and E^cut^ = 73^+48^_-24_
keV (Bassani et al. 1995).

2. 2006A&A...448..499B
Re:NGC 4507
3.2.5 NGC 4507 The Chandra spectrum of NGC 4507 was analyzed in detail by Matt
et al. (2004), together with the XMM-Newton data. The source is seen through a
large column density (N_H_ ~= 4 x 10^23^ cm^-2^), while the presence of a
Compton-thick reflector is inferred by the presence of a Compton reflection
component, a large iron K{alpha} line and its Compton shoulder. The soft X-ray
emission is dominated by emission lines, likely produced in a photoionized
material. Interestingly, Matt et al. (2004) found also an absorption line from
Fe XXV, thus suggesting also the presence of an highly ionized gas, as observed
in a large number of Seyfert galaxies (see e.g. Bianchi et al. 2005a, and
references therein).

3. 2003ApJS..148..327S
Re:NGC 4507
5.36. NGC 4507
The [O III] image of this Seyfert 2 galaxy is presented in the bottom
right panel of Figure 10. We can see that the emission is elongated
along P.A. = -35^deg^ in the inner ~2" region, becoming more circular
in the outer regions. The major extent of the emission is 3.5" (800
pc). The bulk of the emission is related to the nucleus and a blob
located at 1" to the NW. This galaxy shows broad emission lines in
polarized light (Moran et al. 2000).

4. 2002ApJ...564..650C
Re:NGC 4507
2. IRAS 12329-3938 (NGC 4507) is a barred spiral galaxy [SAB(s)ab;
Sandage & Brucato 1979] and has been classified as either a Seyfert 2
(Durret & Bregeron 1986) or a Seyfert 1.9 (Veron-Cetty & Veron 1998),
indicating that broad H{alpha} but not broad H{beta} is sometimes
visible in the spectrum. Our optical spectra also show it to be a
Seyfert 2 with similar line ratios to the other AGNs in our sample.
This source was observed with the PTI by Roy et al. (1998), but no
core was detected at the level of 5 mJy. We make a tentative detection
of a less than 0.05" core at 1.6 mJy (10^3.4^ L_sun_), making this source
the lowest luminosity core detection in our sample. The detection is
tentative as the flux in the fringe rate feature is at a similar level
to the noise. However, both the right and left polarization data show
exactly the same feature at the same fringe rate, which is unlikely to
be a coincidence.
IRAS 12329-3938 exhibits a large radio excess (0.85) that remains
after subtraction of the compact core, and this, combined with the
optical AGN classification, is strong evidence that the compact core
we detect is a weak AGN rather than a supernova complex.

5. 2002A&A...389...68G
Re:NGC 4507
NGC 4507: the galaxy has a small size and the HII regions populate
a ring. Our two methods do not work properly because they try to
circularize the ring. We adopt the deprojection angles obtained in
the photometric study of Schmitt & Kinney (2000).

6. 2000ApJ...540L..73M
Re:NGC 4507
NGC 4507.
Similar to NGC 3081, this galaxy exhibits significant polarization
enhancements near the Balmer lines, particularly H{alpha} (Fig. 5).
A bump near He I {lambda}5876 also appears in the polarization
spectrum. In polarized flux, the broad H{alpha} line is strong and
asymmetric, with FWZI ~ 10,000 km s^-1^.

7. 1999A&AS..140....1M
Re:NGC 4507
The K' image agrees with that of Mulchaey et al. (1997), and indeed
shows no clear presence of a bar (Fig. 10a). A noticeable curved dust
lane to the SE reaching the innermost 2 arcsec is visible in the HST
image by Malkan et al. (1998).
The sharp-divided image (Fig. 10b) clearly shows a bar that is also
apparent on the difference image (Fig. 10c). This bar had been already
reported by Mulchaey et al. (1997) (r = 10.5 arcsec, PA = 53^deg^,
{epsilon} = 0.34).
{epsilon} and PA show strong variations at 18-20arcsec from the
nucleus, where the spiral arms begin (Fig. 10e) and produce a small bump
over the bulge + disk fit (Fig. 10f). The bar is also apparent as a
small enhancement over this fit. However, due to the relative weakness
of the bar and arms, the residuals remain small (Fig. 10g). The J/K'
image is quite smooth except in the very nucleus, which has much redder
colors (Fig. 10d) than the outer galaxy.

8. 1999A&AS..137..457M
Re:NGC 4507
NGC 4507: In our 3 cm data, this object is slightly extended along
PA ~ 10^deg^ (Fig. 9). This face-on galaxy shows an high excitation NLR
with a fairly symmetric edge-brightened bicone shape.

9. 1997ApJS..113...23T
Re:NGC 4507
A11. NGC 4507
Ginga revealed an absorbed flat ({GAMMA}=1.34) X-ray spectrum for NGC 4507, with
an iron K-shell emission line of equivalent width ~400 eV (Awaki et al. 1991).
We find the ASCA spectrum to be best fitted with a double power-law model, with
the hard component attenuated by a column ~10^23^ cm^-3^ and none of our models
providing a good fit. Our analysis of the ROSAT PSPC image shows NGC 4507 to be
consistent with a point source. This source has shown a factor of 2 variation
in 2-10 keV flux level between EXOSAT and Ginga observations (Polletta et al.

10. 1997ApJS..110..299M
Re:NGC 4507
Bar is visible in both the ellipse fits and the K_S_image.

11. 1997ApJS..110..299M
Re:NGC 4507
Bar is visible in both the ellipse fits and the K_S_image.

12. 1994CAG1..B...0000S
Re:NGC 4507
([Shapley-Ames] New 2)
Centaurus Cluster region
Feb 13/14, 1978
103aO + GG385
20 min
NGC 4507 is near the Centaurus Cluster but is north and west of
the main concentration (Dickens, Currie, and Lucey 1986). The redshift
of v_o = 3226 km/s (Sandage 1978) is consistent with cluster
membership of the Cen 30 part of the Centaurus complex (Lucey, Currie,
and Dickens 1986).
The galaxy may be the object called New 2 in the original Shapley
Ames (1932) catalog. Its NGC number was not recognized there because
of an error in right ascension in the Dreyer NGC catalog and an error
in declination in the Shapley-Ames Catalog itself (see de Vaucouleurs
1956a and the RC1).
The morphological type of SBab is based on the tightness,
thinness, and regularity of the arms. The galaxy is late in the SBab
morphological box, close to the SBb boundary based on the high current
rate of star formation, indicated by the numerous HII regions in the

13. 1985SGC...C...0000C
Re:NGC 4507
Plate 1477r
Overexposed center, bright arms with many knots, extremely faint envelope.
In halo of very bright star 5.2 north-following.

14. 1979AJ.....84..472S
Re:NGC 4507
Peculiar beginning place for both arms.
They begin within the inner disk and are not connected to the nucleus.
Unusual, not seen to this degree before,
but similar to the dust arm in NGC 4450 (Hubble Atlas, pg. 13)
except that the arms here are luminous.
The likely HII regions are too small to resolve.

15. 1976RC2...C...0000d
Re:NGC 4507
= HA 88,2 "New 2"
Photometry (I.R. 1-3.5 microns):
M.N.R.A.S., 164, 155, 1973.
Bull. A.A.S., 4, 237, 1972.

16. 1964RC1...C...0000d
Re:NGC 4507
= "New 2", see HA 88, 2.
Very small, very bright nucleus. (r): 0.8 arcmin x 0.6 arcmin.
Note correction to NGC R.A. and H.A. 88, 2 Dec.
See also Mem. Com. Obs., 13, 1956.
Lund 9 dimensions are for the bright part only.

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