Date and Time of the Query: 2019-06-24 T02:20:41 PDT
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Notes for object NGC 4485

12 note(s) found in NED.

1. 2005ApJS..157...59L
Re:NGC 4485
The Magellanic irregular NGC 4485 (at a distance of 9.3 Mpc) and the Sd spiral
NGC 4490 (at a distance of 7.8 Mpc) are interacting, and their morphologies are
distorted. There are three ULXs in NGC 4490, all located on irregular dusty
regions. Within the isophote of NGC 4485 is NGC 4485-ULX1 (IXO 62), located on a
dust lane. Its luminosity decreased steadily from 4 * 10^39^ to 1.5 * 10^39^
ergs s^-1^ between three observations separated by 600 days.

2. 2002ApJS..143...25C
Re:IXO 62
4.38. IXO 62 IXO 62 is located in the galaxy NGC 4485, which is a
small companion to the spiral galaxy NGC 4490 (see Fig. 11). Several
HRI observations of IXO 64 show that it is variable by a factor of ~2
(Table 2). There are several extended X-ray sources in the disk of NGC
4490 that have been resolved into individual point sources with Chandra
(Roberts et al. 2002). See also Colbert & Mushotzky (1999) and RW2000.

3. 2002AJ....124..675C
Re:UGC 07648
NVSS confused by UGC 07651.

4. 1999ApJ...519...89C
Re:NGC 4485
NGC 4485.-This Irr galaxy is tidally interacting with NGC 4490.
HFS95 classify it as having an H II region nucleus. We detect very faint
emission that is offset 20.5" (924 pc) from the galaxy center.

5. 1995ApJS...98..477H
Re:NGC 4485
This galaxy is tidally interacting with NGC 4490. The spectra of the two
look nearly identical: both exhibit extremely deep H{beta} and H{gamma}
absorption and a very blue continuum. Faint, narrow emission lines are
also present. It appears that the tidal interaction triggered a recent
burst of star formation in both of these galaxies. The relative
strengths of the emission lines of these two galaxies are atypical
compared to other H II nuclei (e.g., NGC 4449 and NGC 4460 in Fig. 64);
note that [O I] {lambda}6300 is quite strong relative to H{alpha}. Since
shock excitation enhances the strength of low-ionization lines such as
[O I] {lambda}6300 (see discussion in HFS), it is plausible that shocks,
possibly related to the interaction between the two galaxies or
originating from supernova remnants, play some role in producing the
emission-line spectra observed.

6. 1994CAG1..B...0000S
Re:NGC 4485
Karachentsev 341 [with NGC 4490]
May 24/25, 1944
75 min
Both components of this obviously interacting
pair show massive, robust star formation over
each of their faces. Individual stars begin to
resolve at about V = 18 in each galaxy, but the
surface brightness is so high over most of their
disks as to make the photometry of individual
stars difficult. Also there is much dust over the
face of NGC 4490, the brighter of the pair.
The redshifts listed in the RSA2 are
v_o(4485) = 817 km/s and v_o(4490) = 601 km/s.
The plate used for the heavy exposure at the
top left was taken by Baade with the Mount
Wilson 100-inch Hooker reflector.

7. 1994CAG1..B...0000S
Re:NGC 4485
Karachentsev 341 [with NGC 4490]
March 31/April 1, 1938
60 min
The light print of the NGC 4485/4490 pair
at the bottom left was made from an original plate
taken by Baade with the Mount Wilson 60-inch
The morphologies of the galaxies are abnormal,
presumably due to the close encounter.

8. 1976RC2...C...0000d
Re:NGC 4485
= Arp 269
= VV 30
= Holm 414b
= Kara[72] 341a
Interacting pair with NGC 4490 at 3.5 arcmin

9. 1973UGC...C...0000N
Re:UGC 07648
VV 30 b, Arp 269 a
IB(s)m pec (de Vaucouleurs), Sc+ (Holmberg)
In Arp's class "double galaxies with connected arms"
"Resolution of knots, emission regions and dust lanes only" (Arp)
Paired with UGC 07651 at 3.6, 165

10. 1964RC1...C...0000d
Re:NGC 4485
= Holm 414b
Smooth, partially resolved core, with dark markings. Asymmetric. Partially
resolved arm or branch toward NGC 4490.
Interacting pair with NGC 4490 at 3.5 arcmin.
Lund 9 dimensions are for the bright part only.
Ap. J., 116, 66, 1952.

11. 1959VV....C...0000V
Re:VV 030b
= NGC 4485
V = +837 km/sec from {lambda}3727
(Page, T., Ap. J., 116, 63, 1952)

12. 1918PLicO..13....9C
Re:NGC 4485
Vol. VIII; Plate 36. These appear to be physically connected; 4485 is a bright
irregular oval 1' long. 4490 is 4' x 1.8' in p.a. about 112^deg^. Very bright,
with numerous almost stellar condensations; a very irregular spiral. See Abs.
Eff. 15 s.n.

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