Date and Time of the Query: 2019-05-24 T01:12:09 PDT
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Notes for object NGC 5585

12 note(s) found in NED.

1. 2008MNRAS.388..500E
Re:UGC 09179
UGC 9179 (NGC 5585). It is a satellite of M101 (Sandage & Bedke 1994). A good
agreement is observed between our H{alpha} map and that of James et al. (2004);
however, we miss an H{alpha} region in the north-east because of our smaller
field-of-view. The H{alpha} rotation curve is perturbed, due to the presence of
the bar and an inner arm-like structure. This galaxy has been observed in H I by
Cote, Carignan & Sancisi (1991) who obtained a velocity field and a rotation
curve in agreement with ours although their H I extent is larger and our
H{alpha} resolution higher. Our H{alpha} rotation velocities are higher because
we assume an inclination of 36^deg^ (derived from our H{alpha} velocity field),
whereas the H I data led to a higher inclination of 36^deg^. Both values are
nevertheless compatible within the H{alpha} error bars. Although the shape of
our H{alpha} rotation curve suggests that we reach the maximum rotation velocity
at the optical limit, the H I rotation curve from Cote et al. (1991) sho ws that
the true maximum is reached a bit further.

2. 2008A&A...487..485H
Re:KIG 0624
CIG 624. SAB(s)d HII is the NED classification for this galaxy. A fragmented
spiral arm pattern and regions of star formation all along the disk are
appreciated both in our optical and RGB images. The total B-V color index is
similar to the Sm/Im types. SABdm is our classification for this galaxy. Note
that the angular scale of this galaxy is larger than our CCD size (5.8 arcmin).
However a wider view from the SDSS image allows us to barely identify the global
spiral and fragmented pattern, and a few dwarf galaxies (green boxes) at the

3. 2007MNRAS.380..506G
Re:NGC 5585
NGC 5585 is a barred Sd galaxy; together with NGC 5204 (Sm), NGC 5474 (Scd), NGC
5477 (Sm), HoIV (Im) and M101 (Scd) it forms the M101 group. The Fe5015 and Mgb
indices assume values among the lowest in the sample; H{beta} has instead a
value among the highest ones (see Table 2). The metallicity retrieved from the
one-SSP analysis is everywhere very low. In the continuous star formation
approach, constant star formation cannot be ruled out; indeed, when allowing to
choose among exponentially declining and constant star formation, in the
{chi}^2^ minimization, for age fixed to 10 Gyr the constant star formation is
selected (for the central aperture).

4. 2002AJ....124..675C
Re:UGC 09179
Diffuse radio emission below the NVSS catalog limit, extremely
uncertain flux density.

5. 2000A&AS..142..425D
Re:NGC 5585
3.6 NGC 5585 = UGC 9179 = KIG 624 = PGC 51210 = IRAS 14181+5657
As the two previous galaxies (NGC 5204 and NGC 5474), NGC 5585 is a
probable member of the M 101 group, but it looks rather isolated with
respect to the neighbouring galaxies. Fig. 14 reproduces a view of
NGC 5585 in the I band taken from the archive of the John Kapteyn
telescope (La Palma).
Figure 15 shows the main body of the galaxy from the CCD image obtained
with the 6-m telescope in the I band after subtraction of the median
smoothed frame.
The results of stellar photometry averaged over two observing runs are
presented as a CMD, Fig. 16. The mean apparent magnitude of the three
brightest blue stars is = 20.71, which agrees better with the
old estimate of Sandage & Tammann (1974) 20.9, than with the value of
20.02 derived by Karachentsev et al. (1994). However, all three
brightest blue stars used by Karachentsev et al. (1994) are situated on
the NE side of NGC 5585 beyond the boundaries of our present frame.
Despite the somewhat uncertain distance of NGC 5585, 5.7 Mpc (former
estimate), and 8.7 Mpc (the present paper), this galaxy seems to be
peripheric member of the M 101 group.

6. 1994CAG1..B...0000S
Re:NGC 5585
M101 Group
June 8/9, 1950
30 min
NGC 5585 is one of the four well-resolved
satellite companions to M101 at a distance
modulus of m - M = 29.3 (D = 7.2 Mpc). The four
dwarf satellites, originally discussed by
Holmberg (1950), are NGC 5204 (SdIV; panel
324), NGC 5474 (ScdIV pec; panel 315), NGC 5477
(Sd:) (not in the RSA; panel 326 here), and
NGC 5585 here. The redshift of NGC 5585 is
v_o = 441 km/s. A discussion of the M101 Group
has been made by Sandage and Tammann (1974c).
NGC 5585 is highly resolved into individual
stars and HII regions. The largest HII regions
resolve into disks at about the 2" level. The
brightest stars are at least as bright as B = 20 and
may be brighter, but a study is necessary to
separate the stars from the HII regions by standard

7. 1985AnTok..202.335T
Re:KUG 1418+569
Knotty HII regions are distributed over the disk where the arm structure
is not clear.

8. 1976RC2...C...0000d
Re:NGC 5585
In M101 Group.
Photograph, HII Regions, and Distance Modulus:
Ap. J., 194, 223, 1974.

9. 1973UGC...C...0000N
Re:UGC 09179
SAB(s)d (de Vaucouleurs), Sc+ (Holmberg)

10. 1973AISAO...8....3K
Re:KIG 0624
Many condensations in the arms.

11. 1964RC1...C...0000d
Re:NGC 5585
Bright middle. No definite nucleus. Weak irregular arms well resolved up to
the central region. Low surface brightness.
Lund 6 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright
part only.
In the M101 Group.
Ap. J., 85, 325, 1937.
Medd. Lund, II, 128, 1950.
HII Regions:
Zeit. fur Ap., 50, 168, 1960.

12. 1956AJ.....61...97H
Re:NGC 5585
HMS Note No. 177
Slit on nucleus and condensation 50 arcsec [south-east],
which does not show emission lines.

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