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Date and Time of the Query: 2019-05-25 T01:36:13 PDT
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Notes for object NGC 1549

11 note(s) found in NED.


1. 2006ApJ...639..136H
Re:NGC 1549
NGC 1549. We extracted the spectrum from a 3' (16 kpc) aperture. There was
very little diffuse emission but some evidence of metal enrichment in the
~0.4 keV gas. Using the ROSAT PSPC, Davis & White (1996) reported Z_Fe_ <
0.18, omitting a component to account for undetected point sources. Point
sources contribute ~50% of the flux in our extraction region, and so we
attribute the discrepancy to incorrect modeling of these sources, which
could not be resolved with ROSAT.

2. 2005ApJ...635.1031B
Re:NGC 1549
NGC 1549.-There is very little Galactic absorption or extinction (1.57 x 10^20^
cm^-2^, and there is little evidence of H_2_ absorption (Fig. 6). Absorption by
Galactic atomic gas is present, and the C II {lambda}1036 line (0.6 A wide)
lies in the middle of the redshifted O VI {lambda}1032 line, although emission
near this region is seen in the LiF2b channel as well. The weaker line, O VI
{lambda}1038, is in an uncontaminated region, and it is detected with a FWHM of
about 1.2 A. The flux is elevated just to the blue side of the C II
{lambda}1036 line, which may be the unabsorbed part of the O VI {lambda}1032
line. The line width is about 0.7 of the FWHM of the stellar velocity
dispersion. There is no emission from C III {lambda}977. There is a narrow
emission line at the location of the Galactic O VI line.

3. 1998A&AS..130..267L
Re:NGC 1549
This galaxy is interacting with NGC 1553 (Malin & Carter 1983). The
galaxy geometry is characterized by a strong twisting (Rampazzo 1987)
and shows significant rotation along different axes (Rampazzo 1988;
Franx et al. 1989). PS96 report 213 km s^-1^ as the average value in
the literature for central velocity dispersion, in good agreement with
our nuclear value.

4. 1994CAG1..B...0000S
Re:NGC 1549
Dorado Group #35
E2
CD-1704-S
Jan 5/6, 1981
103aO
75 min
NGC 1549 is a companion of the famous S0_1/2_ galaxy NGC 1553,
which has the pronounced "bright outer rimmed" disk (panel 39). Both
galaxies are in the Dorado Group (Ferguson and Sandage 1990). The
individual redshifts of the pair are v_o(1549) = 991 km/s and v_o =
1053 km/s.
No globular cluster candidates are present in the image. NGC 1549
has a prototype E2 morphology.

5. 1994A&AS..105..433L
Re:NGC 1549
NGC 1549 (Fig. 9); this galaxy is interacting with NGC 1553 and has a
very strange kinematical behaviour. The velocity dispersion profiles at
225^deg^ and 135^deg^ are similar, with a central peak at ~220 km s^-1^
followed by a shallow decrease. The profiles agree with FIH (PA 37^deg^
and 127^deg^). The anomalous profile obtained by Pampazzo (1988) at PA
1350^deg^ can be explained as the result of a slight folding error. At
both position angles moderate rotation is detected.

6. 1994A&AS..105..433L
Re:NGC 1549
NGC 1549 (Fig. 9); this galaxy is interacting with NGC 1553 and has a
very strange kinematical behaviour. The velocity dispersion profiles at
2250 and 1350 are similar, with a central peak at ~220 km s^-1^ followed
by a shallow decrease. The profiles agree with FIH (PA 37^deg^ and
127^deg^). The anomalous profile obtained by Rampazzo (1988) at PA
135^deg^ can be explained as the result of a slight folding error. At
both position angles moderate rotation is detected.

7. 1994A&AS..104..179G
Re:NGC 1549
Large PA twist (see Franx et al. 1989). Shells. Detected at 100 microns.

8. 1985SGC...C...0000C
Re:NGC 1549
Plate 1893
Overexposed center, trace of nubs, dist corona. Extremely faint outer
plumes not included in dimensions. Interacting pair with NGC 1553 11.7
south-following.

9. 1982ESOU..C...0000L
Re:ESO 041439-5542.9
=ESO 157- G 16
in group

10. 1976RC2...C...0000d
Re:NGC 1549
Pair with NGC 1553 at 12 arcmin south-following.
Photograph:
M.N.R.A.S., 131, 351, 1966.
Photometry:
Atlas Gal. Austr., 1968.

11. 1964RC1...C...0000d
Re:NGC 1549
Very bright nucleus.
Photometry:
M.N.R.A.S., 111, 526, 1951.


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