Date and Time of the Query: 2019-08-21 T17:57:26 PDT
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Notes for object NGC 1144

13 note(s) found in NED.

1. 2008ApJ...674..686W
Re:NGC 1142
NGC 1142.-Since NGC 1142 has a strong Fe K line (see Table 8 for EW and
normalization), we fixed the Fe K parameters for the three XRT observations to
the best-fit values for the pn spectrum. Allowing the flux to vary between these
observations improved the fit by (DELTA}{chi}^2^ = 130. There is no evidence of
variability in column density; however, varying power-law components improved
the fit by {DELTA}{chi}^2^ ~ 30. Fitting the spectra with a pegged power-law
model, the best-fit model has {chi}^2^/dof = 132.6/105. Errors on the power-law
photon index, {GAMMA}, were 1.54-2.29 (XMM), 2.34-3.85 (XRT-1), 2.15-3.98
(XRT-2), and 1.08-2.94 (XRT-3). Although the error bars for the photon index are
large, due to the few counts for this heavily absorbed source, it is clear that
observation XRT-1 has a steeper power-law component than the XMM observation.
The errors on the pegpwrlw flux were (1.97-6.01) ergs s^-1^ cm^-2^ (XMM),
(10.87)-322.3) x 10^-11^ ergs s^-1^ cm^-2^ (XRT-1), (10.10-478) x 10^-11^ ergs
s^-1^ cm^-2^ (XRT-2), and (3.81-43.13) x 10^-11^ ergs s^-1^ cm^-2^ (XRT-3). Once
again, the XRT er ror bars are large due to the few counts. Noting that the XMM
observation occurred 6 months before XRT-1, clearly the flux is higher in the
XRT-1 observation while the photon index is steeper. No conclusions can be drawn
from the final two XRT observations.

2. 2007AJ....134..648M
Re:NGC 1144
NGC 1144 (Figs. 7.43, 9.43, 20.43): This belongs to an interacting pair of
galaxies (NGC 1143-1144). It shows a very distorted spiral structure with a
circumnuclear ring traced out by dust lanes and bright regions. The nucleus is
crossed by dark patches of dust.

3. 2006A&A...457...61R
Re:NGC 1144
NGC 1144. A CfA Seyfert 2, with NGC 1143 forms an interacting pair
separated by 0.7". Our NIR spectrum is very similar to that of NGC
1097. It displays a steep blue continuum in the interval 0.8 microns
-2.4 microns, dominated by stellar absorption features. The emission
line spectrum is rather poor, with only [S III] {lambda}{lambda} 9069,
9531 Angstrom, [Fe II] 1.257 microns and H2.2033, 2.121 microns being

4. 2004MNRAS.353.1151S
Re:NGC 1144
NGC 1144. Has been studied in H I by Bransford et al. (1999) and
CO(1-0) has also been detected and mapped by Gao et al. (1997).

5. 2003ApJS..146..353M
Re:NGC 1144
NGC 1144 (TW)
The large distance of this galaxy makes it difficult to classify the
circumnuclear structure. On the observed scales, down to a limiting
resolution of about 500 pc, it appears to be a tightly wound spiral.

6. 2002AJ....124..675C
Re:UGC 02389
CfA Seyfert 2 (Huchra & Burg 1992).

7. 2001ApJ...562..139M
Re:NGC 1144
NGC 1144. - This interacting system has a relatively smooth NIR surface
brightness distribution in its central few arcseconds, although the dust
lane visible in the J and H gray-scale images illustrates the more
disturbed morphology at larger scales.

8. 1999ApJ...516...97N
Re:NGC 1144
NGC 1144 (Arp 118): This galaxy shares a common envelope with
NGC 1143. P.A._RC3_ = 110^deg^ for NGC 1143 and P.A._RC3_ = 130^deg^
for NGC 1144.

9. 1995MNRAS.276.1262K
Re:NGC 1144
NGC 1144: (Arp 118) Type 2. Host galaxy: irregular (GPG), elliptical plus
disrupted spiral (UGC). Radio: the C-array shows a bright component with
extensions to the south and south-west. The structure has a total angular
extent of 30 arcsec (corresponding to a linear size of 13 kpc). Higher
resolution reveals a complicated association of compact objects spanning
8 arscec (4 kpc) within the brightest part of the C-array structure. The
bright western component in the A-array map corresponds most closely with
the optical continuum source. The chaotic appearance and unusual size of
this source are perhaps unsurprising considering that the host is
undergoing a merger. Ghigo (1983) describes NGC 1144 as a ring galaxy,
with radio knots along the southern edge of the ring.

10. 1976RC2...C...0000d
Re:NGC 1144
With NGC 1143 = Arp 118 = VV 331 = Kara[72] 83, it forms an
interacting pair separated by 0.7 arcmin; "Ring" galaxy
Description, Dimensions and Photometry:
Ap. J., 194, 569, 1974.

11. 1973UGC...C...0000N
Re:UGC 02389
{With UGC 02388 =} VV 331, Arp 118
a) {= UGC 02388} 0.9 x 0.9, E
b) {= UGC 02389} 0.65 x 0.50 at 0.65 south-following a), spiral with patchy
`Arms and loops seem attracted to E galaxy' (Arp)
UGC 02388, S0 (de Vaucouleurs)

12. 1964RC1...C...0000d
Re:NGC 1144
Interacting pair with NGC 1144 at 0.7 arcmin.
Heidelberg Veroff. Vol. 9, 1926 and Palomar 200-in. dimensions
for bright parts only.

13. 1959VV....C...0000V
Re:VV 331a
= NGC 1144

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