NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-26 T07:00:05 PDT
Help | Comment | NED Home

Notes for object NGC 0985

16 note(s) found in NED.


1. 2009ApJ...705..962C
Re:NGC 0985
High-velocity Si III is present in this sight line spread over two negative
velocity components. The spectrum covers 1194-1298 A, allowing analysis of the
Si II {lambda}1260.42 line. Most of the corresponding velocity range of the
prospective HVC is blocked by Galactic S II {lambda}1259.52, but the lower
velocity component is clearly present. In addition, a similar absorption feature
is seen towards Mrk 1044, which is 1.1^deg^ from this sight line. Since there
are also no known higher redshift contaminants that could affect the Si III
profile, the two components are thus accepted as high-velocity Si III
detections.

2. 2008ApJ...687..767K
Re:MRK 1048
(Fig. 21).-This object has a close companion and an extremely large but faint,
off-center tidal feature. However, neither of these has a large effect on the
fitting result. We fit the host with a classical bulge (n = 4) and a tidal tail.

3. 2007AJ....134.1061D
Re:NGC 0985
Absorption for this target was seen by Kriss (2002). Kriss lists this target
with only one component, while we find that there are three narrow-line
absorbers with one blended broad absorber, which may consist of two
subcomponents. The H_2_ spectrum is varied in each of the O VI and Ly{beta
lines, allowing for clear identification of each of these lines.

4. 2007A&A...461.1209D
Re:NGC 0985
NGC 985: the BeppoSAX data were previously published by Krongold
et al.(2005), who compared this data set with Chandra LETG data to study
the characteristics of the warm absorber detected below ~2 keV. The
spectral parameters that describe the continuum are in agreement with
what is presented here, apart from the photon index that is found to be
rather flat ({GAMMA}~1.40 compared to{GAMMA}~1.75 of the present work)
by Krongold et al. (2005). These differences may be due to the different
treatment of the absorption since no warm absorber is required when only
the BeppoSAX MECS+PDS data (i.e., at energies above 2 keV) are
considered.

5. 2004ApJS..152...29P
Re:NGC 0985
A7. NGC 985 NGC 985 (Mrk 1048) is a composite system of two interacting
galaxies with nuclei separated by {Angstrom}~3", only one of
which is an AGN (Appleton & Marcum 1993). Strong intrinsic absorption
systems with velocities relative to NGC 985 between -200 and -800 km
s^-1^ are detected in our spectrum in Ly{alpha} and N V
{lambda}{lambda}1238.8, 1242.8 (Appleton et al. 2002). Bowen, Pettini, &
Blades (2002) report an association between a Ly{alpha} absorber and the
galaxy NGC 988 (cz = 1504 km s^-1^, 36.2' and thus 266h kpc off the line
of sight). We do not confirm this Ly{alpha} absorber, since our nearest
SL >= 4 {sigma} Ly{alpha} absorber is at 2155 km s^-1^. HVC gas at -230 to
-110 km s^-1^ is seen in Si III {lambda}1206.5, S II {lambda}1253.8, S
II {lambda}1259.5, and Si II {lambda}1260.4 + Fe II {lambda}1260.5. The
1238.8 {Angstrom} (W = 36 +- 27 m{Angstrom}) absorption line is
identified as Galactic N V {lambda}1238.8, despite undetected N V
{lambda}1242.8.

6. 2003ApJS..146....1W
Re:NGC 0985
NGC 985.-The feature at 1031.215 {angstrom} (-205 km s^-1^ on the O VI
velocity scale) is broader than expected if it is solely H_2_, but after
removal of the H_2_ line it is too weak to measure, so we decided that
it is probably not real. The sight line passes through the middle of
the Cetus-Aries Galaxy Grouping (v = 1810 +- 510 km s^-1^), and 35'
(190 kpc impact parameter) from NGC 988, which has v = 1504 km s^-1^.
However, there is no intergroup Ly{beta}, nor are there Ly{alpha}
features near 1222.18{angstrom} in the STIS spectrum of NGC 985.

7. 2000A&A...357...13R
Re:MRK 1048
MKN 1048: The GIS spectrum of MKN 1048 is well fitted by a simple
powerlaw with photon index {GAMMA} = 1.60^+0.02^_-0.01_, a value
significantly lower than the average photon index found in the X-ray
spectra of quasars. The K{alpha} iron line is marginally detected, at a
2{sigma} level (best fit equivalent width EW = 96^+85^_-83_eV. The
measured 2-10 keV flux is F = 9.9 x 10^-12^ erg cm^-2^ s^-1^.

8. 1998AJ....116.2682C
Re:IRAS 02321-0900
The principal identification appears to be NGC 985b, a Seyfert 1
galaxy. Optical position from Kojoian et al. (1981).

9. 1997AJ....113..201A
Re:NGC 0985
4.7 NGC 985
We present Fig. 8 optical images only of NGC 985, since the near-IR images of
the galaxy are discussed in detail by Appleton & Marcum (1993). The images,
taken with the E. W. Fick observatory CCD camera show the galaxy and its
immediate environment. The most prominent feature aside from the bright core,
which lies on the southern edge of the ring, is the "arm" which extends from
the ring to the west. The ring itself is defined by a series of blue star
forming knots. Radio observations by Appleton & Ghigo (in preparation) confirm
the earlier suggestions (Rodriguez-Espinosa & Stanga 1990; Appleton & Marcum
1993) that the galaxy contains a double nucleus. As discussed by Appleton &
Marcum (1993), it is quite likely that the offset bulge component, which has an
R_1/4_ luminosity profile, is part of the intruder galaxy seem projected
against the ring. These authors showed that there appears to be two nuclei in
NGC 985, again supporting the view that it is a composite system.

10. 1996AJ....111.1431B
Re:1ES 0232-090
0232-090: The new four-frequency measurements confirm the HFE in this object.

11. 1995A&A...298..743H
Re:NGC 0985
NGC 985 (Fig. 7a) is one of the largest rings known (about 30 kpc
diameter). It has no visible nearby companion but the bright knot seen in
projection on the ring may be the intruder galaxy. Its light distribution
follows an r^1/4^ law typical of a nuclear bulge or an elliptical galaxy
(Appleton & Marcum 1993, hereafter AM93). Moreover, near-infrared
observations (AM93) reveal a second nucleus about 3" from the first one,
from which the twisted western arm originates. That suggests that NG6 985
is a composite system of two galaxies and therefore fits into the class
of collisional ring galaxies. The bright knot hosts a Seyfert 1 nucleus
that largely contributes to the X-ray, UV and far-infrared emission of
NGC 985 (Ghigo et al. 1983; Wu et al. 1983; Rodriguez Espinoza & Stanga
1990, hereafter R-ES90). Bright HII regions have been detected in the
ring (R-BS90).
Figure 7c and d show the CO(1-0) and CO(2-1) spectra we have obtained
and a contour map of the CO(1-0) emission. The grid spacing of our maps
is 10", that is, half of the beamwidth for the CO(1-0) map and the
beamwidth for the CO(2-1) map. We clearly detected both CO(1-0) and CO(2-
1) emission at several positions in NG6 985. The CO(1-0) line at the
centre position is very broad (600 km s^-1^ at the zero level) and has a
double-horn profile. The two velocity components lie at 12740 km s^-1^
and 12975 km s^-1^. In CO(2-1) no emission is detected at the centre
position but narrow lines at the higher velocity are seen at the north-
west. However, the 512 MHz bandwidth corresponds only to 666 km s^-1^
which prevents us from detecting the broad component. Alloin et al.
(1992) have observed the central position of NGC 985 in ^12^CO(2-1), also
with the 30m telescope, and detected a narrow line, which corresponds to
the one that we see at the (10", 10") offset. We suspect that small
pointing errors, or a misalignment between the 3mm and 1mm receivers,
could explain this discrepancy. Alloin et al. also present a Kitt
Peak CO(1-0) spectrum which exhibits a high velocity wing that we do not
see in our data.
Figure 7b is a contour map of CO(1-0) emission. The maximum of
emission corresponds to the galaxy nucleus. The emission is extended over
the whole galaxy body although there are some indications that it is not
directly associated with the ring seen in the near-infrared and H{alpha}
but rather with the inner regions.
We derived from the CO(1-0) observations a total H_2_ mass of 1.2
10^10^ M_sun_, which is of the order of the H_2_ mass in the merger
remnant Arp 220 (Sanders & Mirabel 1985). Heckman et al. (1978) obtained
an upper limit on the HI mass of 5.8 10^9^ M_sun_. We have also observed
NGC 985 in HI with the Nancay radiotelescope but did not detect any
emission. This suggests a situation similar to that observed in mergers,
in which the cold interstellar medium is mainly in the molecular phase.

12. 1992A&A...265..429A
Re:NGC 0985
0232-09
In the Palomar Sky Survey (PSS) this galaxy exhibits a disturbed image
and a non-symmetrical ring. Its overall size is ~24". de Vaucouleurs & de
Vaucouleurs (1975) measure a velocity of cz = 12,950+/-50 km s^-1^ for
the H{alpha} and [NII] lines. Feldman et al. (1982) find 12,900 km s^-1^
for [O III] {lambda}5007; they quote no error but observe with a
resolution of 165 km s^-1^. The strong narrow CO peak is at
13,020 km s^-1^, very close to the optical values.

13. 1985ApJS...57..643D
Re:VV 285
Very asymmetric spiral, a ring with nucleus on its arm.

14. 1976RC2...C...0000d
Re:NGC 0985
= VV 285
Ring Galaxy with a Type 1 Seyfert nucleus.
Classification and Spectrum:
Ap. J. (Letters), 197, L1, 1975.

15. 1968MCG4..C...0000V
Re:MCG -02-07-035
Interacting. Irregular elongated body with ``big handles''.
Photo: VV 285.

16. 1959VV....C...0000V
Re:VV 285
= NGC 0985


Back to NED Home