Date and Time of the Query: 2019-05-21 T00:36:46 PDT
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Notes for object NGC 0315

22 note(s) found in NED.

1. 2009ApJ...703.1034Y
Re:NGC 0315
Worrall et al. (2007) obtained X-ray spectra of both the jet and the nucleus.
The power-law component of the nucleus is described by {GAMMA} = 1.57 +/- 0.11,
much harder than that of the jet, which is {GAMMA} = 2.2 +/- 0.2. The X-ray
luminosity L_2-10 keV_ = 6 * 10^41^ erg s^-1^ ~ 1.5 * 10^-5^L_Edd_, which is
much higher than the critical luminosity of L_X,crit_ ~ 1.6 * 10^-7^L_Edd_.
Worrall et al. (2007) argued that the X-rays from the jet must have a
synchrotron origin, which implies that the power-law index of the electrons is p
= 2.4 +/- 0.4. The significant difference between the spectrum of the nucleus
and the jet can be considered as possible evidence that the origin of the X-ray
emission of the nucleus is from the accretion flow rather than from the jet. We
see from the figure that this is consistent with our conclusion.

2. 2006A&A...460...45G
Re:NGC 0315
NGC 315 (UGC 597, B2 0055+30). The high spatial resolution provided by Chandra
imaging allowed the detection of X-ray jets, the most striking one being the one
along ~10" to the NW (see Fig. 5 and Donato et al. 2004; Worral et al. 2003).
Worral et al. (2003) made use of a 4.67 ks duration ACIS-S Chandra image to
report an X-ray luminosity of 5.9 x 10^41^ erg s^-1^ (2-10 keV) for our assumed
H_0_ = 75 km s^-1^ Mpc^-1^ and a power-law energy index {GAMMA} = 1.4 seen
through a moderate intrinsic column density of N_H_ from 2.3 to 8.2 x 10^21^
cm^-2^ for the nuclear component whose spectrum is fitted with a
single-component absorbed power law. In contrast, Donato et al. (2004), using
the same spatial area for the extraction of the nuclear component (1.98 +/-
0.20"), conclude that two components are required to model the corresponding
spectrum: a power-law ( {GAMMA} = 1.56) and a thermal one (apec in XSPEC) with
solar metallicity (k_T_ = 0.51 keV, N_H_ = 0.73 x 10^22^ cm ^-2^, which is
therefore in very good agreement with our results by using RS+PL as the best
model (see Table 6). Satyapal et al. (2005) class NGC 315 as an AGN-LINER (those
displaying a hard nuclear point source, with a 2-10 keV luminosity > 2 x 10^38^
erg s^-1^, coincident with the VLA or 2MASS nucleus); their spectral fitting
results in kT = 0.54 keV, N_H_ = 0.8 x 10^22^ cm^-2^, and {GAMMA} = 1.60, all of
which also agree with ours.

3. 2004A&A...413...97G
Re:TXS 0055+300
0055+300 is an FR I radio-galaxy with an asymmetric two-sided jet and a
prominent core; its optical counterpart is the cD galaxy NGC 315, at
z = 0.017. This source has been extensively studied using the VLA and VLBI
(e.g. Venturi et al. 1993; Cotton et al. 1999; Dennett-Thorpe & Marcha
2000) and has been detected at X-ray (Worrall & Birkinshaw 2000;
Terashima et al. 2002) and infrared wavelengths (Golombek et al. 1988).
Spectroscopic observations by Ho et al. (1995) suggest the presence of a
LINER with a weak broad H{alpha} component. We confirm the low ionization
nature of this object, but were not able to detect any broad Balmer line;
however, such a component cannot be excluded by our data. The detection of
a broad component would be in agreement with the other AGN-like
characteristics of the object, namely the presence of a radio jet and a
compact, unresolved, X-ray core. Although a small-scale cooling flow may
be present in NGC 315 (Worrall & Birkinshaw 2000), we interpret the
observed low ionization spectrum as the optical signature of a low luminosity

4. 2003ApJS..148..419N
Re:NGC 0315
NGC 315 (UGC 597).-This elliptical galaxy has a nuclear dust disk (b/a =
0.23). It has a core-jet radio morphology on VLA and VLBA scales. The
STIS slits were aligned parallel to the galaxy major axis. The central
kinematic and flux properties are listed in Table 7; the gas appears to
be in organized motion, possibly regular rotation. The fit to the
central spectrum is improved by the addition of a broad component. Data
for this galaxy are shown in Figure 3 (see key in Fig. 1 for an
explanation of these plots).

5. 2003AJ....126.2237D
Re:NGC 0315
4.5. Radio Galaxies
NGC 315 (F00550+3004) is a radio galaxy with a very large radio excess
of u = -0.83, but with only moderate radio power [L_{nu}_(4.8 GHz) =
10^24.4^ W Hz-1]. It is a large FR I galaxy with a total extent of
greater than 1.7 Mpc (Condon et al. 1991b). Evidence for superluminal
motion has been detected in the radio source (Xu et al. 2000). The
host is an elliptical galaxy with an equatorial dust disk and an
unresolved optical nucleus (Capetti et al. 2000). It has a low FIR
luminosity of {nu}L_{nu}_(60 micron) = 10^9.7^L_solar_.

6. 2002ApJS..139....1T
Re:NGC 0315
NGC 315 (L1.9).-An analysis of the ASCA data is presented in
Matsumoto et al. (2001). A ROSAT HRI image shows a compact core and
probably an extended component. The contribution of the point source
to the HRI flux depends on modeling details (Canosa et al. 1999; Worrall
& Birkinshaw 2000). Extended emission is seen in the ROSAT PSPC image
(Worrall & Birkinshaw 2000). The ASCA images in the soft and hard bands
are consistent with being pointlike.

7. 2002AJ....124..675C
Re:UGC 00597
The radio source extends almost 1 deg on the 610 MHz WSRT map
(Willis et al. 1981). The listed flux S(1.4 GHz) = 6.63 Jy is from
Condon et al. (1991b).

8. 2001ApJ...552..508G
Re:NGC 0315
0055+30 (NGC 315). - In previous papers (Cotton et al. 1999 and
references therein) we published multifrequency and multiepoch data on
this giant radio galaxy. We found evidence of an acceleration in the inner
parsec-scale jet. A similar result was presented by Lobanov & Zensus (1999)
for the well-known quasar 3C 345, by Sudou et al. (2000) for NGC 6251, by
Homan et al. (2001) in the jet of five blazars from proper-motion
observations, and here for the source 0220+43 (3C 66B). Barth,
Filippenko, & Moran (1999) reported the detection in NGC 315 of a polarized
broad H{alpha} emission.

9. 2000ApJ...530..719W
Re:NGC 0315
NGC 315.-This source is discussed in detail in section 6.

10. 2000AJ....120.2950X
Re:UGC 00597
UGC 00597 (NGC 315)-This source has been extensively studied using
the VLA and VLBI (e.g., Venturi et al. 1993, Cotton et al. 1999, and
references therein). The radio jets are found to have large sidedness
ratios from milliarsecond to arcminute scales.

11. 2000A&AS..144...53K
Re:NGC 0315
The spectra in the inner 2 arcsec show variable H{beta} emission, which
is probably responsible for the jumps observed in the v and {sigma}
values. The two most distant datapoints have rather poor signal-to-noise
ratio. The related values of h_3_ and h_4_ are very uncertain; only the
values of {sigma} and v are given. The comparison with the old data of
Schechter & Gunn (1979) and the velocity profile of Davies & Birkinshaw
(1988) (Fig. 3) is good within the rather large errors of the literature

12. 2000A&AS..144...53K
Re:NGC 0315
The SB-profile of Peletier et al. (1990) extends from 3.8 arcsec out to
91.8 arcsec. Since the kinematic data range further inwards than the
photometric data the SB-profile was extrapolated using a power-law; the
fitted slope is -1.01. This might overestimate the actual luminosity in
the central regions since one might expect the cD galaxy NGC 315 to have
a core with a shallower slope. Due to the outer cutoff of the SB-profile
at R = 91.8 arcsec, the total luminosity is an underestimate because the
slope of the density profile at the cutoff of the data is still larger
than -3. This must then also be true for the B_T_ value from the RC3.

13. 2000A&A...362..871C
Re:NGC 0315
0055+30 (NGC 315): A highly inclined, very regular circum-nuclear disk,
is seen in absorption in this galaxy. It is oriented at P.A. ~ 40^deg^
and extends to r ~ 350 pc. At its center there is an unresolved nuclear
source. Irregular dust patches are also present on the South side of the
galaxy. See also Verdoes Klein et al. (1999).

14. 1999AJ....118.2592V
Re:NGC 0315
NGC 315 is part of Zwicky cluster 0107.5+3212 (Zwicky et al. 1961),
which is located in the Perseus-Pisces filament. We detect a central
dust disk 820 pc (2.5") in diameter that is close to but not perfectly
an ellipse; the north tip of the disk has a small extension. In
addition, several mottled patches of dust are detected southwest of the
nucleus out to 5" (~1.5 kpc). The central part of the dust disk forms a
small, bright emission-gas disk, which extends into low-level emission
throughout the dust disk. There is also a low-level emission feature
adjacent to the southeast side (i.e., the counterjet side) of the dust
disk that is elongated in the direction of the dust disk. H I was
detected in absorption redshifted by ~400 km s^-1^ with respect to the
systemic velocity (van Gorkom et al. 1989; Knapp, Bies, & van Gorkom
1990). Ho et al. (1997) found a nuclear H{alpha} broad-line emission
component with FWHM 2000 km s^-1^ in addition to the narrow-line
emission. Our isophotal analysis is in good agreement with an analysis
by De Juan, Colina, & Perez-Fournon (1994) from ground-based
observations. The two-sided radio jet of NGC 315 has been well studied
(e.g., Venturi et al. 1993; Bicknell 1994; Mack et al. 1997; Cotton et
al. 1999).

15. 1997AstL...23..644G
Re:NGC 0315
NGC 315. Bresolin et al. (1993) (Cepheids); Greggio et al. (1995) (A36, A724,
B3), (A555, A1011, A223). No photometric data were published by Bresolin et al.
(1993), while in the servey of Greggio et al. (1995) a small region in the
brightest part of the galaxy was omitted.

16. 1997ApJS..112..391H
Re:NGC 0315
NGC 315.--As noted previously by Ho et al. (1993), a broad H{alpha} component
is present in this radio galaxy with twin radio jets (Giovannini, Feretti, &
Comoretto 1989), but its strength turns out to be considerably weaker (f_blend_
~29%) than what might be perceived by eye (Fig. 4b). The narrow lines have very
broad, non-Gaussian wings, easily discernible, for instance, in the [S II]
lines. Unfortunately, the model for the [S II] lines is not well determined
because [S II] {lambda}6731 is partly redshifted out of our spectral range.

17. 1997A&A...321..765B
Re:NGC 0315
3.1. NGC 315
We have detected the continuum emission from NGC 315 at 113.3 GHz and possibly
at 226.7 GHz. Heckman et al. (1983) found a 21 cm continuum flux density of 1.1
Jy for this extended source. In order to convert our continuum temperature
(main beam scale) to a flux density, we multiply T_cont_ by
6.3 Jy/K x {eta}_mb_/{eta}_forw_, yielding a flux density of 0.42 Jy. A similar
calculation gives a flux density of 0.26 Jy at 1.3 mm. The 21cm to 2.6mm
spectral index is then about -0.2 which is quite flat. The spectral index
between 2.6 and 1.3mm is significantly steeper, about -0.7, indicating that
either the spectrum steepens with frequency or that the source is >~10" at mm
wavelengths. If the emission were due to dust, it would be stronger at 1.3 mm.
Despite our non-detection in CO, some cool gas is clearly present in or near
NGC 315 as HI is detected in absorption (Heckman et al. 1983; Chamaraux et al.
1987) with N_HI_~10^20^ cm^-2^.

18. 1995ApJS...98..477H
Re:NGC 0315
The emission-line spectrum of NGC 315 has LINER characteristics. In
addition, the presence of a weak broad H{alpha} component (HFS) and a
radio jet (Giovannini, Feretti, & Comoretto (1989) support the
classification of this object as an low-luminosity AGN.

19. 1977A&AS...29..279F
Re:B2 0055+30
0055+30 The 1415 MHz map of this source has already been published
(Fanti et al. 1976). The source is dominated by a very strong nuclear
source of small diameter (<0.1") and flat or rising spectrum (see
previous reference). The NW component has an asymmetrical shape, typical
of a "head-tail" source. Its 610-1415 MHz spectral index steepens, from
about 0.5 to > 1.0, going from the inner to the outer parts. The SE
component is undetected at 6 cm and has a steep spectrum ({alpha}~=1.4).
The galaxy may belong to the Zwicky cluster (01h07.5m+32deg12'). Recently
Bridle et al. (1976) have shown that our source is the central part of a
giant radio source 0.7 Mpc in size.

20. 1976RC2...C...0000d
Re:NGC 0315
= B2 radio source
= Holm 029a
NGC 0313 and NGC 0316 (= Holm 028c and Holm 028b) are stars.
NGC 0311 is 5.5 arcmin south-preceding.
NGC 0318 is 5.5 arcmin north-following.

21. 1973UGC...C...0000N
Re:UGC 00597
See UGC 00592
{00 55.3} +30 09 = NGC 318 at 5.6, 40, 0.5 x 0.3, m=15.2
NGC 313 and NGC 316 are stars
{UGC incorrectly notes "00 54.8". H. Corwin}

22. 1964RC1...C...0000d
Re:NGC 0315
= Holm 028a
NGC 0313 = Holm 028c is a star
NGC 0316 = Holm 028b is a star
NGC 0311 at 5.5 arcmin [south-preceding].
NGC 0318 at 5.5 arcmin [north-following].

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