Date and Time of the Query: 2019-06-17 T06:25:27 PDT
Help | Comment | NED Home

Notes for object NGC 5907

15 note(s) found in NED.

1. 2005MNRAS.357..361S
Re:NGC 5907
NGC 5907. The galaxy is almost perfectly edge-on (i= 89^deg^). The majority
of the submillimetre emission is extremely well confined to a thin disc and is
well mapped out to just over half the optical radius. It is seen to be dominated
by the core, which is unresolved by SCUBA in the direction perpendicular to the
galactic plane. A few bright knots of submillimetre emission are seen along the
disc. The two peaks ~75 arcsec either side of the centre correspond to a
linear distance of 5.7 kpc at the assumed distance to the galaxy. A third, more
distant northern peak seen on the 850-{mu}m map is 120 arcsec from the centre,
or 9.1 kpc. All three may be due to the increased dust column density along the
line of sight through spiral arm regions within the galactic disc.

2. 2000A&A...355..512D
Re:NGC 5907
3.1.1. NGC 5907 at 20 cm
Fig. 1 shows the total intensity map obtained with the VLA at
{lambda} 20 cm, overlaid on an optical image extracted from the
Digitized Sky Survey. An outstanding feature in this map is the double
source in the southern half of the galaxy. The spectral behaviour of
this double source (see further below), its non-variable nature (see
e.g. Hummel et al. 1984) and also the non-zero probability of finding a
radio source as strong as this within the extent of a galaxy on the sky
suggest that this double source is a background source projected onto
the southern half of NGC 5907. Two more background point sources are
also visible in the direct vicinity of the galaxy. The galaxy itself is
asymmetric: at lower intensities, the radio continuum emission is more
extended to the south than to the north, while the maximum intensity is
shifted several arcsec to the north (see also Fig. 8).
Also shown in Fig. 1 is the polarized intensity in the form of
polarization (E-field) vectors, rotated by 90^deg^. Note that due to
possible Faraday rotation effects in the galaxy itself and between the
galaxy and the observer at this wavelength the (E + 90)-vectors do not
necessarily indicate the intrinsic magnetic field orientation as is the
case at (much) shorter wavelengths.
3.1.2. NGC 5907 at 6.2 cm
The total intensity map at {lambda} 6.2 cm is shown in Fig. 2. Because
of the limited resolution of the Effelsberg telescope at this
wavelength (147"), none of the point sources in the vicinity of NGC 5907
that are visible in the 20 cm map could be distinguished from the
galaxy's emission. However, the double background source in the southern
half could be identified as a second emission maximum south of the
centre of NGC 5907. In general the distribution of the emission seems to
be similar to that at {lambda} 20 cm wavelength.
Also shown are the (E + 90)-vectors whose lengths are proportional to
the polarized intensity. They will be described in the next subsection.
3.1.3. NGC 5907 at 2.8 cm
Although the sensitivity of the 2.8 cm data is below that of the 6.2 cm
data (and therefore the S/N-ratio much lower), the better resolution
available at {lambda} 2.8 cm with the Effelsberg telescope offers a
deeper insight into the structure of the radio continuum emission. The
radio map obtained at this wavelength - which is identical to Fig. 5 in
Dumke et al. (1995) - is shown, overlaid on an optical image, in Fig. 3.
Besides the double source in the southern half, the background point
source southeast of the galaxy is also visible. As at 20 cm, an
asymmetry of the emission is detected also at 2.8 cm in the sense that
the maximum intensity seems to be shifted to the north.

3. 1998PASJ...50..427S
Re:NGC 5907
NGC 5907: This is an almost perfect edge-on Sc galaxy. The nuclear
component is not visible because of extinction due to the foreground
disk. The disk component shows a rigidly rotating PV feature at R < 60",
beyond which the rotation is flat. This rigid-body-like behavior occurs,
because we are looking at a ring in the disk, where the optical depth
along the lines of sight becomes nearly equal to unity. The CO line data
show a sharply rising rotation curve (Sofue 1997).

4. 1996ApJ...473..117S
Re:NGC 5907
NGC 5907.--This large, relatively nearby edge-on galaxy has a well-determined
and very extended H I rotation curve (Sancisi & van Albada 1987). However, it
had not been possible to estimate the Newtonian rotation curve due to the
luminous matter, because the high dust obscuration in the plane of the galaxy
masks the true radial light distribution. This has changed with the
near-infrared photometry of Barnaby & Thronson (1992,1994), which indicates
a more centrally concentrated distribution of luminous material. This
highlights the value of near-infrared photometry as the most accurate,
absorption-free tracer of the dominant stellar component. Here the
decomposition by Barnaby & Thronson into an exponential disk and a bulge
represented by a modified Hubble profile is used directly to calculate the
Newtonian rotation curve; i.e., because the galaxy is edge-on, the exponential
model for the disk is used rather than the detailed photometry.

5. 1996ApJ...458..120S
Re:NGC 5907
NGC 5907
NGC 5907 is a nearby Sc galaxy with an almost edge-on orientation at an
inclination angle of 88^deg^. Observations of the H I line emission have shown
a large disk of interstellar gas, which is warping in the outermost regions
(Sancisi 1976b). A CO + H I composite PV diagram for NGC 5907 has been
obtained by Sofue et al.(1994), who used CO data from the NRO (Sofue 1994) and
H I data from the Westerbork synthesis radio telescope (WSRT)(Casertano 1983).
Recently, a nuclear disk component has been observed in the CO (J = 2-1) line
with the IRAM 30 m telescope, which showed two symmetrical humps in the PV
diagram at rotation velocities +200 and -190 km s^-1^ at 10" to the northwest
and southeast of the nucleus (Garcia-Burillo & Guelin 1995). This indicates
that the rotation velocity increases steeply in the central ~ 10" (500 pc).
Unfortunately, the H I PV diagram has been obtained only for the southeast
side, which we used to derive an H I total rotation curve, assuming that the
rotation is axisymmetric. So we first obtained the CO rotation curve at
R < 10 kpc by averaging the southeast and northwest CO curves, and we obtained
the final rotation curve in Figure 9b by smoothing the CO and H I total
rotation curves. After the steep rising near the nucleus, the rotation curve
is almost flat until 20 kpc, beyond which it gradually declines.

6. 1995ApJS...98..477H
Re:NGC 5907
The nucleus of this Sc galaxy is partially obscured by a dust lane,
causing the spectrum to be heavily reddened.

7. 1995A&A...302..691D
Re:NGC 5907
Superimposed onto the disk radiation in the total power map is the
emission of a double background source (Hummel et al. 1984) in the
southern part of the galaxy. The radio continuum emission of the galaxy
itself exhibits one maximum which is located a bit northwest of the
central position given in Table 1.
In this galaxy no significant polarized emission could be detected.

8. 1994CAG1..B...0000S
Re:NGC 5907
Sc(on edge)
May 10/11, 1950
40 min
NGC 5907 shows the absence of the central
bulge particularly well because of its high
The redshift is v_o = 779 km/s.

9. 1993A&AS...97..887B
Re:NGC 5907
NGC 5907
Our CO(1-0) and CO(2-1) spectra show CO emission out to at least 60" (3.3
kpc) with the CO(2-1) emission considerably weaker than the CO(1-0). The
CO(2-1) however seems weaker and narrower than the CO(1-0) at all points,
even taking the rotation curve into account. Despite the strong CO
emission, the HI dominates by a factor of 3 - 10.

10. 1976RC2...C...0000d
Re:NGC 5907
= Holm 704a
NGC 5906 is part of it.
Pair with Holm 704b at 12 arcmin
P.A.S.P., 78, 495, 1966.
Rotation Curve:
Systemic Velocity Astr. Ap., 8, 364, 1970.
Ann.Rev.Ast. Ap., Vol. 2, 249, 1964.
Stellar Structure, Vol.VIII of Stars and Stellar Systems, 396, 1965.
HI 21cm (halo):
Astr. Ap., 28, 95, 1973. undetected.
Radio Observations:
Ap. J., 144, 553, 1966.

11. 1973UGC...C...0000N
Re:UGC 09801
SA(s)c: (de Vaucouleurs), Sb+ (Holmberg)
No nuclear bulge
SN 1940a

12. 1964RC1...C...0000d
Re:NGC 5906
This is a part of NGC 5907.

13. 1964RC1...C...0000d
Re:NGC 5907
= Holm 704a
Very small bulge nearly hidden by a strong dark lane.
NGC 5906 is part of NGC 5907.
Pair with an anonymous galaxy (= Holm 704b) at 12 arcmin.
Ap. J., 46, 46, 1917.
P.A.S.P., 52, 146, 1940
Photograph and Orientation:
Ap. J., 127, 487, 1958.
SN 1940
H.A.C., 519.
P.A.S.P., 52, 146, 1940.
Handbuch der Phys., Vol. 51, 781, 1958.

14. 1961Hubbl.B...0000S
Re:NGC 5907
May 10/11, 1950
40 min
Enlarged 13X
NGC 5907 is an early Sc galaxy seen within a few degrees
of edge on. The nuclear bulge is quite small and is almost
hidden behind the opaque dust lane. It appears that the
outermost spiral arms can be seen at either end of the
spindle, and their sense of opening can be inferred. The
arm on the north side is opening toward the observer (out
of the page); the arm on the south side is going away
(into the page). Spectroscopic observations show that the
south end of the spindle is approaching. This means that
the arms are trailing.

15. 1918PLicO..13....9C
Re:NGC 5907
11' x 0.6' in p.a. 156^deg^, rather bright. A dark lane runs down the entire
length; nucleus hazy; a few condensations. 5906 is simply the strip to the west
of this lane. See Abs. Eff. 13 s.n.

Back to NED Home