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Notes for object NGC 2841

21 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 2841
NGC 2841 .SAR3*.-The HST F438 image shows a weak nuclear dust spiral that is
misaligned with the outer disc. The larger scale bulge morphology is smooth and
shows little sign of dust and no spiral pattern. The h_3_ profile is
anti-correlated with the rotation curve inward of 4" but then changes sign and
becomes correlated with the velocity until about 20". The velocity dispersion
profile is centrally rising and may show a little shelf inward of ~=5". The
minor axis rotation curve shows an offset within the bulge radius.

2. 2011AJ....141...23B
Re:NGC 2841
A.6. NGC 2841
NGC 2841 is an early-type Sc spiral and is the most distant
galaxy in our sample located at 14.1 Mpc. The limited spatial
resolution and the high inclination of this galaxy meant that
we were only able to detect supershells of type 1. We found
15 HI holes and only one of these shows signs of expansion
(number 10). In addition, holes number 4, 12, and 13 are possibly
superpositions of holes. Hole no. 5 is probably not a genuine
hole but the result of the warp in the HI disk.

3. 2009A&A...503..409H
Re:NGC 2841
In Stokes I, Braun et al. (2007) note a diffuse "hourglass" structure, with the
long axis of the hourglass oriented perpendicular to the disk major axis. In the
polarized emission, the highest brightnesses are seen along the minor axis
trailing away slowly to the northwest and more rapidly to the southeast. The
lowest brightness of polarized emission occurs near the receding major axis (PA
= 153^deg^, as tabulated in Table 1). The directions of the magnetic field
vectors are primarily aligned along the polarized arcs. The three polarized
background doubles in this field display substantial differences in their RMs.
The greatest consistency is seen between the two lobes of one of the doubles, at
-6 +/- 3 rad m^-2^. There may be significant structure of the foreground RM in
this field.

4. 2008MNRAS.385..553D
Re:NGC 2841
NGC 2841: The velocity field of this fast-rotating galaxy does not show
any sign of perturbation. The RVs inside a 50 arcsec radius are not
mapped in this H{alpha} study because of Doppler broadening of the line
typical of Seyfert 1 galaxies. Inside the 50 arcsec radius, H{alpha} and
[N II] images by Afanasiev & Sil'chenko (1999) seem to suggest that the
excitation of the ionized gas is caused by shock wavefronts. Little CO
is seen in this galaxy (Helfer et al. 2003).

5. 2008AJ....136.2648D
Re:NGC 2841
4.4. NGC 2841 is an early-type (Sb) spiral and was previously observed at lower
resolution in H I by Begeman (1987). We compare the curves in Figure 8 and find
good correspondence overall. Begeman (1987) finds a systemic velocity of 631.1
+/- 1.4 km s^-1^, a difference of only 2.6 km s^-1^ with our value of 633.7 +/-
1.8 km s^-1^. The average P.A. and i values found by Begeman (1987) are
154.5^deg^ and 73.1^deg^, respectively, and differ from our values by only a few
degrees (see Table 2).

6. 2008AJ....136.2648D
Re:NGC 2841
6.3. NGC 2841 The surface brightness profiles of NGC 2841 are shown in Figure
27. The 2MASS J, H, and K profiles can be traced out to ~290", and the IRAC 3.6
{mu}m profile out to ~375". All surface brightness profiles show an extended
outer exponential disk, as well as a more compact central component. We
decompose the profile using a double exponential disk. For the outer disk we
find {mu}_0_ = 15.7 mag arcsec^-2^ and h = 4.20 kpc. The inner disk has
parameters {mu}_0_ = 13.5 mag arcsec^-2^ and h = 0.72 kpc. In subsequent
modeling we use the inner disk model for the central component. For the outer
component we use the total observed surface brightness profile with the inner
disk model subtracted, extrapolated at large radii using the outer exponential
model parameters. The surface brightness profile shows some evidence for central
emission in excess of the exponential model. However, the central parts of the
velocity field cannot be modeled due to lack of H I emission. NGC 2841 possesses
a modest color gradient, which results in a {GAMMA}^3.6^_*_ trend from
{GAMMA}^3.6^_*_ ~= 0.8 in the inner parts to {GAMMA}^3.6^_*_ ~ 0.5 in the outer
parts. For radii beyond which the 2MASS color could not be reliably determined,
we assume a constant {GAMMA}^3.6^_*_ = 0.5. The color profile shows a slight
reddening in the innermost part, but this occurs at radii where no velocity
information is available. The mass models are presented in Figure 28. For the
ISO model, the disk mass obtained through a free fit is very close to the mass
derived from the population synthesis modeling assuming a diet Salpeter IMF. The
resulting halo has the highest (well-determined) central density in the sample.
The NFW model with fixed {GAMMA}^3.6^_*_ is of slightly lower quality; its main
problem is the underprediction of the velocity at the smallest radii. An
increase in {GAMMA}^3.6^_*_ of the inner component when {GAMMA}^3.6^_*_ is
released compensates for this, and yields a model of equal quality as the ISO
model. For the Kroupa fixed {GAMMA}^3.6^_*_ the ISO model results in an
extremely compact halo, probably indicating that {GAMMA}^3.6^_*_ is

7. 2007ApJS..173..538T
Re:NGC 2841
NGC 2841 (Fig. 16.10).-GALEX imaging of this SA(r)b:; LINER Seyfert 1 galaxy
shows nearly continuous spiral arms wrapping the outside of a bright, flocculent
inner disk. The H I disk is also quite extended (Bosma 1981 and F. Walter et
al., in preparation [THINGS]). XUV complexes can be identified out to at least 4
times the D_25_ radius at both ends of the galaxy major axis. These particular
features are corroborated by the H I morphology in the same area (F. Walter et
al., in preparation). Star formation activity is ongoing throughout the entire H
i distribution, which exhibits a notable ringlike appearance just outside the
optical disk. NGC 2841 is dramatic in terms of the difference in mean UV surface
brightness between the inner (optically prominent) disk and the XUV-disk. Some
of the XUV-disk complexes in NGC 2841 are luminous enough to be detected
individually in SDSS observations. A forthcoming paper by Bianchi et al. (in
preparation; see also Bianchi et al. 2007) will discuss population synthesis
SED-fitting of these sources. NGC 2841 is a relatively isolated galaxy, as it is
only paired with one other object (UGC 04879).

8. 2002A&A...388...50F
Re:NGC 2841
According to Sil'Chenko et al. (1997) the ionized gas is
rotating orthogonally with respect to the galaxy plane in the
inner 5''. Alternatively, Sofue et al. (1998) reported that
the central portion of the PV diagram derived from the H{alpha}
and [N II]{lambda}6583 lines is slightly tilted in the direction
of the galactic rotation, suggesting the presence of a rapidly
rotating nuclear disk. Our PV diagram exhibits a complex and
asymmetric shape that could be related to these different
kinematic components. However, we do not measure a significant
variation of the velocity gradient or the velocity dispersion
with radius. The line flux increases slightly toward the center.
These features are similar to those of PV diagrams included in
the Type III class, and make it difficult to associate with the
central component to a fast-rotating disk as by indicated
Sofue et al. (1998).

9. 2001A&A...374..394V
Re:NGC 2841
NGC 2841: In the centre the V_*_ value we obtained is within the scatter
of the other data sets, the same is true for {sigma}_*_. however further
out from the nucleus our V_*_ and {sigma}_*_ are somewhat lower than those
found in literature.

10. 2001A&A...374..394V
Re:NGC 2841
NGC 2841: Sofue et al. (1999) obtained an extended and well-sampled
inner-to-outer rotation curve by combining H{alpha}, CO and H I
observations. Rotation attains a sharp maximum near the centre and flattens
outwards and asymmetries seem to be confined in the radial region we

11. 2001A&A...368...16M
Re:NGC 2841
11. NGC 2841 is an Sb galaxy of medium inclination and with regular,
flocculent arms. Using the HST Cepheid distances and SN Ia distances Shanks
(1997) determined the distance of NGC 2841 to 24.9 Mpc. In the central
regions there exist a slight rotation of the isophotes' major axis, this is
responsible for the double-cone feature in the residuum image (Fig. 4 in
on-line version). The reason is probably a weak bar component (Keel 1983;
Varela et al. 1996; Afanasiev & Sil'chenko 1999).

12. 1998PASJ...50..427S
Re:NGC 2841
NGC 2841: The nuclear component has an inverse HNR as small as ~ 0.3,
and the H{alpha}-line width is smaller than [N II]. This may be due
either to a superposed broad H{alpha} absorption, or to stronger
emission in [N II], such as due to a higher-temperature circum-nuclear
gas. The [N II] nuclear component shows a high concentration of the gas.
The nuclear PV diagram is slightly tilted in the sense of the galactic
rotation, indicating a compact, rapidly rotating gas. The PV behavior of
the disk part is flat in both the H{alpha} and [N II] lines, with a
normal HNR value for H II regions. The rotation velocity of this galaxy
is as high as ~ 300 km s^-1^ in the disk, and reaches almost
350 km s^-1^ in the nuclear disk.

13. 1997ApJS..112..391H
Re:NGC 2841
NGC 2841.--Despite the somewhat triangular narrow-line profiles, a model from
the [S II] doublet fits the complex excellently (Fig. 9b), confiming the
conclusion of Paper I that broad H{alpha} emission is absent.

14. 1994CAG1..B...0000S
Re:NGC 2841
Hubble Atlas, p. 14
Nov 7/8, 1951
103aO + WG2
25 min
This print of NGC 2841 is made from a
different plate than used for the deeper print in
the Hubble Atlas. The photographic contrast
here shows well the resolution into many stars
and small HII regions in the thin, intricate,
regular distribution of the multiple spiral
fragments that provide the spiral pattern.
The central bulge and smooth lens are
similar to those in NGC 488 (Sab; panels 115,
116, S3, S12) but are smaller in NGC 2841
here. Also the arm pattern is somewhat less
regular, requiring the later classification.
An H{alpha} interference plate confirms that some
of the knots in the arms are small HII regions.
They are unresolved at the 1" level despite the
very small redshift, v_o = 714 km/s. This shows
that the intrinsic diameter of the largest HII
regions is a strong function of morphological
type, being small in galaxies that are this early in
the classification sequence. If the distance of
NGC 2841 is 14 Mpc based on its redshift and a
quiet Hubble flow in this local region, the largest
HII regions are smaller than 70 psc, five times
smaller than in Sc galaxies of luminosity class I
(Sandage and Tammann 1974a).

15. 1993ApJS...86....5K
Re:NGC 2841
NGC 2841; Sb, LINER.
This Sb galaxy is classified as a LINER by Heckman (1980) and Keel
(1983a,b) on the basis of optical emission-line ratios and strengths.
While Baldwin, Phillips, & Terlevich (1981) conclude that the ionizing
mechanism is shock heating, Ferland & Netzer (1983) suggest that the
mechanism is photoionization. A ring of enhanced star formation
surrounding the nucleus is suggested by optical and near-IR data (Prieto
et al. 1985). (The ring lies outside the IUE aperture.) No prominent
emission features can be seen in the UV spectrum. However, NGC 2841 does
show a clear rising branch, with flux increasing from 1800 to 1200 A.

16. 1993A&AS...97..887B
Re:NGC 2841
NGC 2841 is a well-known Sb galaxy with a molecular and atomic "ring" and
no central CO (Young and Scoville 1982; Bosma 1981). The galaxy is seen
close to edge-on and has one of the widest (> 600 km/s) HI profiles
known. We detect emission in both lines out to 3' (8.5 kpc) from the
center. At least two distinct maxima appear at about 90" and 180" so we
are probably seeing spiral arms rather than two distinct rings. The CO
line ratio is consistent with thick and thermalized emission from cold
gas but is not included in the statistics as it is not the central line
ratio. The HI observations with the WSRT show HI maxima at similar radii.
The IRAS emission implies very cold dust and an old star population. SM
class NGC 2841 as a LINER but C87 shows extended 20 cm emission with no
concentrated central source as seen with several other LINERs. At 6cm
Gioia & Fabbiano (1987) detect a subarcminute central maximum.

17. 1976RC2...C...0000d
Re:NGC 2841
Description and Classification:
"Nuclei of Galaxies", p.27, 1971.
A.J., 69, 236, 1964.
70, 564, 1965.
IAU Symp. No. 38, 11, 1970.
"Nuclei of Galaxies", p.27, 1971.
Astr. Ap., 29, 57, 1973.
A.J., 73, 313, 1968.
A.J., 74, 50, 1969.
Sov. A.J., 10, 440, 1966.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.
HII Regions:
Ap. J., 194, 559, 1974.
P.A.S.P., 29, 213, 1917.
A.J., 69, 236, 1964.
A.J., 70, 564, 1965.
IAU Circ. No. 2476, 1973.
IAU Circ. No. 2498, 1973.
Astr. Ap., 29, 57, 1973.

18. 1973UGC...C...0000N
Re:UGC 04966
SA(r)b: (de Vaucouleurs), Sb- (Holmberg)
SN 1912, SN 1957a

19. 1964RC1...C...0000d
Re:NGC 2841
Large, bright nucleus. Many knotty arms. Pseudo (r): 3.2 arcmin x 1.2 arcmin,
not well defined.
Ap. J., 50, 384, 1919.
Ap. J., 120, 439, 1954.
IAU Symp., No. 5, 1958 = Lick Cont. II, No 81, 1958.
Ap. J., 135, 733, 1962
Orientation and Rotation:
Ap. J., 97, 117, 1943.
Ap. J., 127, 487, 1958.
Radio Emission:
Handbuch der Phys., Vol.53, 253, 1959.
SN 1912
P.A.S.P., 29, 213, 1917.
Ap. J., 88, 290, 1938.
SN 1957
Sky & Tel., 16, 374, 1957.

20. 1961Hubbl.B...0000S
Re:NGC 2841
Feb. 14/15, 1950
30 min
Enlarged 7.5X
This is the type example of the multiple-arm Sb sub-group.
NGC 2841 is the earliest of the group. All galaxies
illustrated on pages 14 to l9 are of this type.
NGC 2841 has a central region composed of a bright
nucleus (smaller than 15 sec of arc in diameter) and an
amorphous lens devoid of dust or spiral structure. The
lens resembles an E or S01 galaxy. The smooth lens has a
major diameter of 100 sec (60 mm on this illustration).
Multiple, thin dust lanes begin to spiral outward at the
periphery of the amorphous lens. They appear to separate
luminous spiral filaments of very complex structure.
At first glance the filaments look like complete spiral arms,
but closer inspection shows that only thin broken segments
are present which cannot be traced as individual
arcs for more than 30 degrees.

21. 1918PLicO..13....9C
Re:NGC 2841
Vol. VIII, Plate 19. A beautiful, very regular spiral, 6' x 1.6' in p.a.
152^deg^. Nucleus almost stellar; central portions quite bright; whorls narrow
and compact. See Abs. Eff. 35 s.n.

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