Date and Time of the Query: 2019-05-21 T19:44:58 PDT
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Notes for object NGC 7541

10 note(s) found in NED.

1. 2000ApJS..131..413Z
Re:NGC 7541
5.2.16. NGC 7541
NGC 7541 (Fig. 17) is a relatively nearby (36 Mpc; CHSS) disturbed
starburst spiral with an optical size of 3.4' x 1.1' (Nilson 1973). Radio
maps by CHSS and Colbert et al. (1996) also give a rather extended size of
60" x 24", with little central concentration. At 10 microns the small
aperture (5") to large aperture (100") compactness ratio is C = 0.07
(Giuricin et al. 1994). The nonpointlike flux distributions at radio and
10 micron wavelengths suggest that the FIR flux of NGC 7541 will also be
NGC 7541 has been observed often in H I (Lu et al. 1993; Oosterloo &
Shostak 1993). A value of 47 mJy was used, which implies an atomic gas mass
of 9 x 10^9^ M_sun_ (Mirabel & Sanders 1988). This is approximately twice
the molecular gas mass of 4.5 x 10^9^ M_sun_ (Sanders et al. 1986). The
usual ratio of molecular to atomic gas masses in FIR luminous galaxies is
~2-5 (Mirabel & Sanders 1988), and so in this respect, the ratio of ~1:2
makes NGC 7541 look more like a quiescent galaxy.
NGC 7541 was easily resolved at 100 microns along the minor axis of the
galaxy (Fig. 17). The fitted Gaussian gives D_g_ = 23", while the fitted
disk model gives a D_e_ = 12.5". A note in CHSS says the companion
NGC 7537, which lies several arcminutes to the southwest, may contribute
to the IRAS flux. The summed flux (38.7 +/- 6.0 Jy) is consistent with the
IRAS flux of 40.6 Jy, so the entire IRAS flux has been recovered despite
the alignment of our array along the minor axis of NGC 7541. These facts
taken together would argue that the morphology of the 100 micron emission
is more circular than the very elongated optical contours. If distributed
like the optical emission, it would have missed most of the flux in our
We note parenthetically that our array position did not cover the site
of the recent supernova SN 1998d, a SN Ia that was discovered 50" west and
10" north of the center.
Using the single-slab model, IRAS fluxes, and the 1.25 mm flux from
Carico et al. (1992), one gets {tau}_100_ = 3.4 x 10^-2^. This gives
A_V_ = 26, which is not unreasonable for an edge-on spiral.

2. 1996ApJ...467..551C
Re:NGC 7541
3.2.4. NGC 7541
We show a contour map of the radio emission overlaid on an optical image in
Figure 2d. Again, most of the emission comes from sources in the disk,
especially from regions along the eastern arm. As in UGC 903, "fingers" seem to
extend out of the disk, but this may be beam-smeared emission from point
sources in the disk.

3. 1996A&AS..117..417H
Re:NGC 7541
28. NGC 7541: nearly edge-on, with a strong absorbing lane in B. Classified SB,
but we see no evidence for a bar. Strong asymmetry along the two semi-major
axes; thin asymmetric arms; compact bulge. "Type II" profile?

4. 1996A&AS..115..439E
Re:NGC 7541
NGC 7541 is a peculiar galaxy in pair with NGC 7537. Its optical rotation
curve has been determined by Rubin et al. (1978) and Kyazimov (1980). It has
been observed in the radio continuum by van der Hulst et al. (1981) using the

5. 1994CAG1..B...0000S
Re:NGC 7541
Karachentsev 578 [with NGC 7537]
panel 282
Sep 2/3, 1945
60 min
NGC 7541 forms a physical pair with NGC 7537
[Sc(s)] at an angular separation of 2.7'.
Karachentsev (1987) gives redshifts of v_o(7537)
= 2834 km/s and v_o(7541) = 2793 km/s. At
the mean redshift distance of 56 Mpc the
projected linear separation is small, at 44 kpc.
There is no evidence for morphological distortion
in either galaxy, despite this apparent closeness.

6. 1994CAG1..B...0000S
Re:NGC 7541
Karachentsev 578 [with NGC 7537]
Sep 2/3, 1945
60 min
NGC 7541, shown on panel 255, is the
brighter member of a physical pair with
NGC 7537. The redshifts listed by Karachentsev
are v_o(7537) = 2834 km/s and v_o(7541) = 2793 km/s.
The angular separation of 2.7' corresponds
to a projected linear separation of 44 kpc
at the redshift distance of 56 Mpc (H = 50).
The spiral pattern of neither member of the pair
shows evidence of an encounter.
Two Im candidates for dwarf companions to
the pair exist within 11' of NGC 7541. They
have HIL-region candidates at the same brightness
as the HII knots in the two main Sc galaxies
and are therefore very likely at the same
distance. Three candidates for dE dwarf
companions also exist in the immediate field.

7. 1976RC2...C...0000d
Re:NGC 7541
= Holm 805a
= Kara[72] 578
Pair with NGC 7537 at 2.7 arcmin
Photograph and Spectrum:
Astrofizika, 4, 59, 1968.
Radio Observations:
Australian J. Phys., 21, 193, 1968.

8. 1973UGC...C...0000N
Re:UGC 12447
SBbc:? (de Vaucouleurs)

9. 1964RC1...C...0000d
Re:NGC 7541
= NGC 7581
= Holm 805a
Bright narrow bar: 0.55 arcmin x 0.5 arcmin. Many knotty, filamentary arms
with dark lanes. Poorly resolved.
Non-interacting pair with NGC 7537 at 2.7 arcmin.

10. 1918PLicO..13....9C
Re:NGC 7541
A moderately bright spiral 2.6' x 0.6' in p.a. 97^deg^. No nucleus; a straight
line of matter proeeeds to west from the center along the major axis. Apparently
a single-whorled spiral, showing a few rather hazy condensations. 11 s.n.

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