NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-25 T22:58:26 PDT
Help | Comment | NED Home

Notes for object NGC 5846

23 note(s) found in NED.


1. 2008MNRAS.386.2242H
Re:NGC 5846
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC
5813 and NGC 5846 are taken from Cappellari et al. (2007b) with a formal
error of 10 per cent (1{sigma} CL), which is approximately converted
from the 30 per cent error at 3{sigma} CL.

2. 2008MNRAS.386.2242H
Re:NGC 5846
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC 5813 and
NGC 5846 are taken from Cappellari et al. (2007b) with a formal error of 10 per
cent (1{sigma} CL), which is approximately converted from the 30 per cent error
at 3{sigma} CL.

3. 2006MNRAS.369..497K
Re:NGC 5846
The SAURON FoV of this bright giant elliptical includes a foreground star and a
companion (NGC 5846A) north and south of its nucleus, respectively. The line
strength maps are generally regular, with small gradients. The line strengths
are consistent with Sanchez-Blazquez (2004) and Rampazzo et al. (2005).

4. 2006MNRAS.366.1151S
Re:NGC 5846
Ionized gas in this galaxy is found within ~10 arcsec and along a filament
running to the north-east. Although characterized by large fluctuations in some
places, the V_gas_ field clearly indicates a nearly cylindrical rotation for the
gas, in the opposite sense to the stars. Remarkably, the zero-velocity curve
runs across the north-eastern filament, suggesting this is not a separate
component from the gas closer to the centre. The HST image shows dust along an
almost parabolic lane swinging around the nucleus. Upon closer inspection, the
emission-line fluxes follow very closely the dust distribution, in particular
from H{beta}. Relatively intermediate [O III]/H{beta} values are observed across
most of the field.

5. 2006ApJ...639..136H
Re:NGC 5846
NGC 5846. We extracted spectra in six contiguous, concentric annuli with
outer radii 0.4', 0.7', 1.2', 1.7', 2.3', and 3.9' (2, 4, 7, 10, 14, and
24 kpc), respectively. We found that fitting a single hot gas component
(plus undetected source component), with kT rising from ~0.6 keV in the
center to ~1 keV in the outer radii, gave a rather poor fit (chi^2^/dof =
630/450). Adding an additional hot gas component to the inner annuli did
not improve the fit. However, the fit was considerably improved if such a
component was added to the outermost annulus (delta chi^2^ = 60). By
inspection, the image shows considerable large-scale structure, which
complements the disturbed morphology on smaller scales (Trinchieri &
Goudfrooij 2002). To investigate this further, we constructed a hardness
map (using energy bands 0.1-0.8 and 0.8-7.0 keV, separately smoothing each
image by convolution with a Gaussian of width 5"), which revealed that the
gas temperature within each annulus is not uniform. We confirmed this
explicitly for the outermost annulus by restricting the extraction region
to a narrow sector chosen to contain the softest photons; the best-fitting
temperature of the gas in the outer annulus was then significantly lower
(falling to 0.8 keV). A detailed analysis of the two-dimensional
temperature structure of this galaxy is beyond the scope of this present
work. However, it is sufficient to add additional hot gas components in
each annulus for which the fit was significantly improved to obtain a
reasonable estimate of Z_Fe_. The addition of a third hot gas component to
each annulus did not improve the fit significantly. Although it is not
clear that spherically symmetric deprojection is appropriate in such a
system, the fit was somewhat better when 'projct' was used than when it
was omitted. The final chi^2^ was poor; this may reflect systematic errors
in the response, since the source is bright, or it may reflect the
imperfect spectral deprojection resu lting from the spherical
approximation, or it may be a consequence of the complicated temperature
structure. We did not find any clear evidence of an abundance gradient so
the abundances of all gas components were tied.

6. 2006A&A...460...45G
Re:NGC 5846
NGC 5846 (UGC 9706). Based on Chandra data, Trinchieri & Goudfroij (2002) reveal
a complex X-ray morphology with no clear nuclear identification (see also Fig.
5). They detect, however, a large amount of individual, compact sources in the
range of luminosities of 3-20 x 10^38^ erg s^-1^. Filho et al. (2004) report a
weak, hard (2-10 keV) nuclear source with {GAMMA} = 2.29, compatible within the
errors with the value we obtain from the spectral fitting. Satyapal et al.
(2005) analyze the Chandra data of this galaxy that they class within non-AGN
LINERs, fitting its spectrum with a single thermal model with kT = 0.65 keV,
exactly the same as we get for our single RS model (see Table 3).

7. 2006A&A...447...97B
Re:UGC 09706
UGC 9706: Filho et al. (2004) detected a weak hard x-ray nucleus (total counts )
and fitted the spectrum with a power-law model ({GAMMA} = 2.29). Their result is
consistent with that of Trinchieri & Goudfrooij (2002).

8. 2005ApJ...635.1031B
Re:NGC 5846
NGC 5846.-This is the optically most luminous galaxy in the center of its
group, and it has a moderate amount of extinction (4.24 x 10^20^ cm^-2^), with
evidence of absorption from Galactic molecular hydrogen and atomic lines. This
is one of the more distant objects, so the continuum is fairly faint but is
well fit by the stellar continuum of NGC 1399 (Fig. 23). Both the strong and
weak redshifted O VI lines appear to be present, but not in the expected 2 : 1
ratio (for O VI {lambda}1032 to O VI {lambda}1038). The O VI {lambda}1032 line
is broken up by Galactic molecular absorption features, so it could be
significantly stronger. We cannot fit the H_2_ parameters well enough to make
an accurate absorption correction for the O VI {lambda}1032 line. The usually
weaker O VI {lambda}1038 line (redshifted to 1043.6 A) falls close to a feature
in the detector. Whereas this feature is stationary and well known, we have
seen instances of unusual absorption or emission near it, and this may
contribute to the strength of this feature. The spectra in the LiF2b channel,
while poorer, confirms the presence of the O VI {lambda}1032 line but not the O
VI {lambda}1038 line. Consequently, we estimate the O VI luminosity from the O
VI {lambda}1032 line. There is emission from the C III {lambda}977 line at a
flux of 7.7 x 10^-14^ ergs cm^-2^ s^-1^ (15% error), with a line width of 1.0
+/- 0.1 A and a line center of 982.87 A (at the systemic redshift, it would
have been at 982.61 A).

9. 2004MNRAS.352..721E
Re:NGC 5846
NGC 5846: This is an example of a giant elliptical with a very low (but
present) rotation (Carollo, Danziger & Buson 1993), and a high central
dispersion. The SAURON field of view includes a foreground star and a
companion (NGC 5846A) north and south of its nucleus, respectively.
h_4_ is high everywhere, confirming the trend observed by Bender et
al. (1994).

10. 2004A&A...418..429F
Re:NGC 5846
NGC 5846 The X-ray morphology of this source is complex (see also
Trinchieri & Goudfrooij 2002), extending over more than 3', almost to
the limits of the optical galaxy. It exhibits two "spiral arms",
directed to the Southeast and Southwest. There is a weak hard X-ray
nucleus, coincident with the VLA radio core in NGC 5846, whose spectrum
was fit with a power law ({GAMMA}=2.29). The source we have identified
with the nucleus coincides with the third most luminous X-ray source in
NGC 5846, listed as source number 12 in Trinchieri & Goudfrooij
(2002). Their quoted flux for this source is six times higher then our
estimation because they convert counts to fluxes assuming a constant
conversion factor. If we apply the same formulation, our results are
consistent with theirs by a factor of 1.4.

11. 2001AJ....121..808C
Re:NGC 5846
NGC 5846. - While previous studies suggest NGC 5846 contains dust
(Goudfrooij & Trinchieri 1998), our analysis is incomplete because we only
obtained a K_s_ image.

12. 2000ApJS..129...93F
Re:NGC 5846
NGC 5846. - We have detected a partially resolved 7.1 mJy source.
NVSS measured a 22 mJy source. VLA observations at 1.4 GHz by
Mollenhoff, Hummel, & Bender (1992) measured an unresolved core of 9 mJy
plus 10 mJy of additional diffuse emission: NGC 5846 must possess a
compact flat-spectrum core component. Our recent subarcsecond-resolution
8.4 GHz images have confirmed this object's compactness.

13. 2000A&AS..144...53K
Re:NGC 5846
The galaxy shows a slowly declining velocity dispersion, with no
rotation and small h_3_ and h_4_ values.
Comparisons are given for the v and {sigma} profiles to the data of
Franx et al. (1989) and BSG94, where reasonable agreement is obtained
(Fig. 5). The same is achieved for the data of Carollo et al. (1993),
which have large errors and are not shown here. Sembach & Tonry (1996)
obtained a radially extended major axis kinematic profile with a
pioneering (hardware) method to perform sky subtraction. The authors
themselves note that their values are 6-7% higher than previous
observations. Somewhat higher bias is observed here. The h3 and h4 data
given by BSG94 are compatible with the present dataset, within their
large errors.

14. 2000A&AS..144...53K
Re:NGC 5846
The V band surface brightness profile of NGC 5846 was derived from
observations performed in March 1999 at the ESO 2.2 m telescope equipped
with the Wide Field Imager. This instrument covers a 34 x 33 arcmin^2^
field of view with a mosaic of 2 x 4 CCDs of 2K x 4K 15micron pixels,
with a scale of 0.238 arcsec/pixel. Six 5 minutes exposures were taken,
shifted by 20 arcsecs in RA and Dec to fill the gaps between the CCDs.
The reduction of the frames was performed under IRAF, using the mscred
package to handle mosaic data. After the bias subtraction, sky
flat-fielding, and frame combination (performed after the astrometric
calibration) the resulting image is flat at the 1% level.
The isophote shape analysis was performed following Bender & Mollenhoff
(1987). The procedure was improved in two aspects. Mask files were
produced automatically from the "segmentation frames" produced by the
Sextractor program (Bertin & Arnouts 1996). The surface brightness and
integrated magnitude profiles following elliptical isophotes were
computed from the averages of the unmasked pixels between the isophotes.
Statistical errors were also derived from the measured rms. Radial
profiles of surface brightness, ellipticity, position angle and higher
order terms of the Fourier analysis are shown in Fig. 9. Note that the
centers of the outer isophotes (at more than 500 arcsec from the center)
are some 30 arcsec off the center of the inner ones. The surface
brightness has been calibrated using the V-band photoelectric photometry
of Colless et al. (1993). The comparison with data of Bender
(unpublished) obtained with a small field of view CCD show good
agreement up to 40 arcsec from the center, where the sky subtraction of
Bender's data becomes unreliable.

15. 1998A&AS..128...75P
Re:NGC 5846
4.3.6. NGC 5846
This is an E0 galaxy in the G50 group with a companion NGC 5846 A 1' to the
south. The presence of atomic gas in that galaxy is not obvious, Roberts et al.
(1991) only give a superior limit of HI gas mass (M_HI_=5 10^5^ M_sun_). A
strong X-ray emission was detected with Einstein satellite (Forman et al.
1985). Demoulin et al. (1984) have studied the ionized gas component using
numerical subtraction technique and results obtained with FP observation are in
agreement with this study. Tlie line of sight velocity diagram shows a non
axisymetric rotation, the North West (200 km s^-1^) part has a velocity
amplitude greater than the South East part (80 km s^-1^). Viewing angles
diagram shows that both Prolate and Oblate possibilities are possible.

16. 1994CAG1..B...0000S
Re:NGC 5846
Group
S0_1_(0)
(I)
CD-1496-S/Br
July 31/Aug 1, 1980
103aO + GG385
45 min
NGC 5846 is the brightest in a group of
perhaps ten members, as originally defined by
Humason, Mayall, and Sandage (1956, Table XI)
at a mean redshift of = 1808 km/s. The
pair shown here with the close angular separation
of 35" has a redshift difference of 554 km/s
which, although large, is not uniquely so for close
pairs. The redshifts are v_o(5846) = 1714 km/s
and v_o(5846A) = 2268 km/s. If the pair is a
binary at the mean redshift distance of 40 Mpc
(H = 50), the projected linear separation would
be small at 7 kpc, supportive of the large velocity
difference. However, there is no evidence for a
physical bridge between the galaxies.
The morphology of NGC 5846 is prototypical
S0_1_ with an extended envelope that is not
characteristic of ellipticals. The type of E0 listed
in the RC2, based on a Palomar 200-inch plate,
is not supported here.

17. 1994A&AS..105..481M
Re:NGC 5846
NGC 5846: A large object with conflicting Hubble types: E0 in the RC2,
S0_1_ in the RSA. We find some photometric evidence of a lens, and
therefore support the second classification. The isophotes are nearly
circular throughout, a very rare instance indeed.

18. 1993A&A...280..409B
Re:NGC 5846
NGC 5846: This object is an X-ray galaxy (Canizares et al. 1987) and
has been observed by DBB, TdiSA and Shields (1991). It shows a complex,
filamentary emission-line morphology, including an arm-like feature which
resembles the emitting regions of NGC 3962 and NGC 4696 (Sparks et al.
1989). There are also some dust patches associated with the emission
region.

19. 1976RC2...C...0000d
Re:NGC 5846
= Holm 694a
Brightest in a group.
Non-interacting pair with NGC 5846A at 0.7 arcmin.
Photograph:
Ap. J., 181, 27, 1973.
Photometry (UBVR):
Ap. J., 143, 187, 1966.
Ap. J., 183, 735, 1973.
Photometry (5 Color):
A.J., 73, 313, 1968.
Photometry (I.R., 1-3.5 Microns):
Ap. J., 143, 187, 1966.
Dynamics and Mass Determination:
Ap. J., 181, 27, 1973.
HI 21cm (upper limit):
Astr. Ap., 25, 451, 1973.

20. 1973UGC...C...0000N
Re:UGC 09706
E+0-1 (de Vaucouleurs), E (Holmberg)
Paired with a) at 0.7, 180, NGC 5846A in RC1, 0.35 x 0.35, E2-3
(de Vaucouleurs), v = 2291, v(0) = 2304, included in CGCG magnitude
UGC 09715 at 10.3, 112

21. 1964RC1...C...0000d
Re:NGC 5846
= Holm 694a
Bright diffuse nucleus. Smooth nebulosity.
Brightest in a group (see Ap. J., 131, 595, 1960) including NGC 5839, NGC 5845,
NGC 5850, and NGC 5854.
Non-interacting pair with NGC 5846A at 0.7 arcmin.
Magnitudes and colors for NGC 5846 + NGC 5846A (Sources A,B,C,E,F).
Spectrum:
I.A.U. Symp., No. 5, 1958 = Lick Contr. II, 81, 1958.

22. 1956AJ.....61...97H
Re:NGC 5846
HMS Note No. 182
Slit on NGC 5846 and close companion.
{lambda} 3727 very faint in NGC 5846.
HMS Note No. 183
Companion 40 arcsec [south] of NGC 5846.

23. 1918PLicO..13....9C
Re:NGC 5846
Round, 1' in diameter; no structure apparent. Star at south does not appear
to be physically connected with the nebula.


Back to NED Home