NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-03-25 T11:44:30 PDT
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Notes for object NGC 5264

7 note(s) found in NED.


1. 2003A&A...401..141L
Re:NGC 5264
6.1.16. NGC 5264 NGC 5264 is a Cen A dwarf galaxy with a TRGB distance
of 4.53 Mpc (Karachentsev et al. 2002b). Compared to other HII spectra,
our spectrum shows relatively low I([O III]{lambda}5007)/I(H{beta}),
whereas I([O II]{lambda}3727)/I(H{beta}), I([N III{lambda}6583)
/I(H{alpha}), and I([S II]{lambda}{lambda}6716,6731)/I(H{alpha}) are
high. The [N II]/[O II] discriminant indicates an upper branch
abundance. Because of the low negative value (-0.599) for log O_32_, the
oxygen abundance derived using the Pilyugin bright-line method is
somewhat uncertain, as his method is calibrated to observations of H II
regions with larger values Of log O_32_. Using I([N II]{lambda}6583)
/I(H{alpha}), the calibrations of van Zee et al. (1998b)
and Denicolo et al. (2002) give 12+log(O/H) = 8.68 and 8.55,
respectively, which agree with the upper branch abundances from the
McGaugh and the Pilyugin calibrations. Taking an average of the values
from each calibration, the adopted oxygen abundance is 12+log(O/H) =
8.61, which is similar to measured abundances in spiral galaxies. Using
the Thurston et al. (1996) method for H II regions in spiral galaxies,
the nitrogen-to-oxygen abundance ratio is log(N/O) = -0.57.
NGC 5264 has a higher oxygen abundance and a nitrogen-
to-oxygen ratio than expected for its galaxy luminosity. This
galaxy may be an example of a dwarf spiral (e.g., Schombert
et al. 1995), whose luminosity is similar to the SMC, but whose
oxygen abundance is a factor of four larger than the SMC. A
systematic spectroscopic survey of H II regions in NGC 5264
should show whether or not the galaxy has a radial gradient in
oxygen abundance.
Compared to typical dIs, the M_HI_/L_B_ value for NGC 5264 is somewhat
low compared to other late-type galaxies of similar luminosity. NGC 5264
is located one degree to the east of the luminous spiral NGC 5236
(M 83), where an interaction with the latter could remove H I gas from
NGC 5264. Interestingly, there is in the vicinity another Cen A group
member dI, UGCA 365 (ES0444-G078), which appears to be even closer in
projection to M 83 (see Fig. 1 in Karachentsev et al. 2002b). There may
be an interaction between M 83, UGCA 365, and NGC 5264, which could
explain the comparatively lower H I content in the latter galaxy.

2. 2002A&A...385...21K
Re:NGC 5264
NGC 5264. This bright dwarf galaxy of Magellanic type has numerous blue
stellar complexes and dusty patches in its central part. The periphery of
the galaxy is populated mainly with RGB stars, which are used by us to
derive a distance estimate of D = 4.53 Mpc. Like the two previous objects,
NGC 5264 belongs to the M 83 companions.

3. 2000AJ....120.2975S
Re:DDO 242
DDO 242 (Fig. 26)-Although not quite as well resolved as the
previous galaxy, DDO 242 also shows interesting structure in its H I
gas. The majority of emission is from a large concentration to the east,
with a smaller concentration located to the southwest. This system has
the slight appearance of an incomplete ring, or perhaps two elongated
neighboring associations. The Gaussian profile is relatively narrow, and
the velocity field exhibits a shallow gradient. The velocity dispersion
for DDO 242 is also quite low, about 5 km s^-1^. The optical
distribution is quite different than that seen in the H I map; the
galaxy has an almost rectangular appearance, with many small optical
knots scattered throughout.

4. 1985SGC...C...0000C
Re:NGC 5264
= DDO 242
Plate 494
Square inner region, many knots, partially resolved?
Plate 1484
Patchy, partially resolved.

5. 1982ESOU..C...0000L
Re:ESO 133847-2939.7
=ESO 445- G 12
many small condensations
in cluster

6. 1974UGCA..C...0000N
Re:UGCA 370
UGCA 370:
= NGC 5264 = DDO 242

7. 1966AJ.....71..922v
Re:DDO 242
= NGC 5264


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