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Notes for object MESSIER 049

27 note(s) found in NED.


1. 2007MNRAS.377..759S
Re:NGC 4472
NGC 4472: this giant elliptical, situated in the Virgo cluster, has X-ray holes
or cavities within radii of ~2 kpc which may have been produced during a
period of nuclear activity that began 1.2 X 10^7^ yr ago and may be ongoing
(Biller et al. 2004). The globular clusters of this galaxy seem to be old and
coeval but they show a range in metallicity from -1.6 < [Fe/H] < 0 dex (Beasley
et al. 2002).

2. 2006ApJS..164..334F
Re:VCC 1226
VCC 1226 (M49, NGC 4472).A thin, boomerang-shaped dust lane crosses the galaxy's
center at a position angle of roughly -45^deg^, extending ~1.5" on either side.
Faint dust patches are seen within 3.5" of the center. There is no indication of
a nucleus from the dust-corrected images. The isophotes show no significant
deviations from ellipses.

3. 2006ApJ...639..136H
Re:NGC 4472
NGC 4472. We extracted spectra in nine contiguous, concentric annuli with
outer radii 0.3', 0.6', 1.1', 1.6', 2.2', 3.0', 4.0', 5.2', and 7.7' (1.3,
2.8, 5.0, 7.1, 9.6, 13, 17, 23, and 34 kpc), respectively. In order to
improve the constraints, we tied together Z_Fe_ in annuli 2 and 3, in
annuli 4-7, and in annuli 8 and 9. Only a single hot gas component was
required by the data in any given radius. The temperature profile rose
from kT = 0.67 keV in the center to 1.3 keV in the outer annuli. There is
some evidence of slight abundance gradient, although the error bars are
rather large. Our measured Z_Fe_ in each bin is somewhat larger than the
values ~0.5-1.1 (converting to our solar standard) found by Finoguenov &
Jones (2000). This is most likely a consequence of the Fe bias; there is a
clear temperature gradient even within the smallest annuli those authors
attempt to use, and furthermore our results agree well with Buote & Fabian
(1998).

4. 2006A&A...447...97B
Re:UGC 07629
UGC 7629: Both Soldatenkov et al. (2003) and Maccarone et al. (2003) detected
emission from the nucleus at energies below 2.5 keV. Biller et al. (2004)
confirmed the presence of nuclear emission in the 0.3-10 keV band extracting 64
source counts in an 1" circle. The spectrum was modeled using a power-law model
with photon index {GAMMA} = 1.7 and a column density N_H_ = 1.7 x 10^20^ cm^-2^.
These results do not contrast the upper limit given by Loewenstein et al. (2001)
who did not find a nuclear component in the hard X-ray band from 2 to 10 keV.

5. 2005ApJ...635.1031B
Re:NGC 4472
NGC 4472.-Known as M49, this lies in the center of the southern grouping of the
Virgo Cluster. It has a modest Galactic H I column and extinction (1.65 x
10^20^ cm^-2^), but it has clear Galactic H_2_ absorption. There is an
indication of an O VI {lambda}1032 line associated with NGC 4472, although if
present, it is redshifted relative to the systemic velocity of the galaxy by
about 0.4 A (120 km s^-1^; Fig. 15). There is a minor peak at the location of
the redshifted O VI {lambda}1038 line in this night-only spectrum. We regard
the O VI line emission as a possible detection. The line width of FWHM = 120 km
s^-1^ is about 18% of the stellar velocity dispersion expressed as a FWHM, 676
km s^-1^. There is no indication of emission from the C II {lambda}977 line.

6. 2005ApJ...627..674A
Re:NGC 4472
NGC 4472.The imaging of this Seyfert 2 galaxy is consistent with an unresolved
point source. The source is extended on VLA scales, but the peak flux density
in our VLA imaging is similar to the peak flux density in our VLBA image.
Variations in our VLA observations appear highly correlated with u-v changes,
and we do not include this galaxy in our short-term variability analysis.

7. 2005ApJ...622..235T
Re:NGC 4472
Radio; H I; two-sided weak radio jet

8. 2004A&A...428..373B
Re:NGC 4472
4.4. NGC 4472. The LINER NGC 4472 is the most luminous galaxy in the
Virgo Cluster. This massive galaxy has been allocated both elliptical
and S0 classifications and has a kinematically distinct core (Davies &
Birkinshaw 1988). Its effective radius is much larger than in any other
galaxy in our whole sample.
This galaxy is the prototype of the El group of Bica (1988) that is,
within the central 1 kpc, an old and metallic stellar population.
Two spectra were analyzed along PA = 110deg: a nuclear one
(200 pc in diameter) and a circumnuclear one located at 210 pc
from the centre (extending from 100 to 320 pc). Due to the
small distance of this galaxy from us the measured positions
represent only a very small fraction of its effective radius in
comparison with the other galaxies described in this paper.
The stellar population is quite homogeneous in the inner region, with
the bulk of the population being older than a few Gyr and somewhat
metallic. A poorly defined contribution of less than 20% young stars
(A dwarfs and K supergiants) is also indicated. The synthetic and observed
spectra are shown in Fig. 6. A discrepancy is obvious around the CAIIT
lines, the synthetic EW are narrower and deeper than the observed ones.
This could be due to the fact that the same EW can be obtained with
strong line stars such as supergiants diluted by hot almost featureless
stars, or by a population of less strong line stars such as giants.
Although it is the best fit for this galaxy, the degeneracy is not
removed as can be seen via the error bars of the young component. This
may be due to the incompleteness of the stellar database, i.e. metallicity
differences between stars included in the library and those composing
the galaxy.
These results are in agreement with radial gradient information over 15
arcsec both in age and metallicity, with those reported in Vazdekis et
al. (1997); see also Terlevich & Forbes (2002).

9. 2004A&A...428..373B
Re:NGC 4472
4.4 The LINER NGC 4472 is the most luminous galaxy in the
Virgo Cluster. This massive galaxy has been allocated both elliptical
and S0 classifications and has a kinematically distinct core (Davies &
Birkinshaw 1988). Its effective radius is much larger than in any other
galaxy in our whole sample.
This galaxy is the prototype of the E1 group of Bica (1988) that is,
within the central 1 kpc, an old and metallic stellar population.
Two spectra were analyzed along PA = 110deg: a nuclear one (200 pc in
diameter) and a circumnuclear one located at 210 pc from the centre
(extending from 100 to 320 pc). Due to the small distance of this galaxy
from us the measured positions represent only a very small fraction of
its effective radius in comparison with the other galaxies described in
this paper.
The stellar population is quite homogeneous in the inner region, with
the bulk of the population being older than a few Gyr and somewhat
metallic. A poorly defined contribution of less than 20% young stars (A
dwarfs and K supergiants) is also indicated. The synthetic and observed
spectra are shown in Fig. 6. A discrepancy is obvious around the CaIIT
lines, the synthetic EW are narrower and deeper than the observed ones.
This could be due to the fact that the same EW can be obtained with
strong line stars such as supergiants diluted by hot almost featureless
stars, or by a population of less strong line stars such as giants.
Although it is the best fit for this galaxy, the degeneracy is not
removed as can be seen via the error bars of the young component. This
may be due to the incompleteness of the stellar database, i.e.
metallicity differences between stars included in the library and those
composing the galaxy.
These results are in agreement with radial gradient information over 15
arcsec both in age and metallicity, with those reported in Vazdekis et
al. (1997); see also Terlevich & Forbes (2002).

10. 2001MNRAS.322..702M
Re:NGC 4472
NGC 4472 Brighenti & Mathews' (1997) modelling of the X-ray emission from
this galaxy indicates a mass of about 3 x 10^11^ M_sun_ within 7.8 kpc
(scaling to our assumed distance of 15.3 Mpc), which corresponds to
v_c_ ~ 410 km s^-1^. Similar results are found by Irwin & Sarazin (1996).
This is in good agreement with our v_c_ = (419 +/- 11) km s^-1^ at
1 r_eff_ = 7.8 kpc.

11. 2001ApJS..133...77H
Re:NGC 4472
NGC 4472, M49 (S2::). - Previous low-resolution maps find the radio
core to be straddled by double-sided jets with an extent of ~2' (Ekers &
Kotanyi 1978; Condon & Broderick 1988). Our maps are insensitive to
large-scale structure of this angular size, and we detect mainly an
extended, elliptical source of length ~11" (9 kpc) along P.A. ~ 80^deg^.
Van der Hulst et al. (1981) and Fabbiano et al. (1989) have published 6 cm
observations at similar resolution as ours. Birkinshaw & Davies (1985)
quote an unpublished higher resolution map by R. Laing which shows that
the central source resolves into a 3" jet along P.A. = 83^deg^. We have
detected linearly polarized emission at 6 (S_pol,6_^I^ = 1.26 mJy) and
20 cm (S_pol,20_^I^ = 0.40 mJy). At both frequencies the strongest
polarization lies offset from the peak in the total-intensity image
(Fig. 16j); the polarization vectors appear to follow smaller scale
structure which is not well resolved in our maps.

12. 2001ApJS..132..129M
Re:NGC 4472
NGC 4472. - The UIT frame for this well-known bright elliptical member
of the Virgo cluster was badly underexposed. It was only faintly detected
in the MUV (Fig. 23b).

13. 2001AJ....122..653R
Re:NGC 4472
NGC 4472: As in NGC 4406, the surface brightness profile of NGC 4472 is
very flat ({gamma} = 0.04) in the center and the isophotal parameters show
large variations. Irregular, patchy obscuration affects the center of the
optical images (van Dokkum & Franx 1995; Tomita et al. 2000), but our NIR
residual image appears quite smooth.

14. 2001AJ....121.2974L
Re:NGC 4472
NGC 4472: Also known as M49, NGC 4472 is the most luminous in the Virgo
Cluster, dominating its region of the subcluster. It has a joint elliptical
and S0 classification and a kinematically distinct core
(Davies & Birkinshaw 1988). NGC 4472 has been the subject of numerous
GC studies and contains perhaps the best-characterized GC system of
any early-type galaxy. Spectroscopic studies (Bridges et al. 1997;
Beasley et al. 2000; Zepf et al. 2000) have determined the mean
metallicity of the GC system and begun to constrain the age and
kinematics. Photometric studies (Lee, Kim, & Geisler 1998;
Puzia et al. 1999; Lee & Kim 2000; Rhode & Zepf 2001) have detected large
numbers of GCs with clear evidence for bimodality. In terms of the peak
colors, there are slight differences between our results and the other
HST studies even though all three use essentially the same data set. We
find (V-I)_0_ = 0.94 and 1.21, which is consistent with the findings of
Lee & Kim (2000) and Puzia et al. (1999) after extinction corrections.
We also confirm that the turnover magnitude of the red GCs is fainter
than for the blue GCs, as noted by Puzia et al. (1999).

15. 2000ApJS..129..435B
Re:RXC J1229.7+0759
RXC J1229.7+0759 and RXC J1243.6+1133. - These are the X-ray halos
of the two Virgo Cluster galaxies M49 and M60, respectively. They are
included in this catalog, even though these halos are embedded within
the low surface brightness structure of the Virgo Cluster emission. But
since the two local halos stand out from the low surface brightness
emission environment and can be reasonably characterized by the present
source characterization technique, we have not excluded them from our
catalog as we have excluded M86 and M87.

16. 2000A&AS..144...53K
Re:NGC 4472
The total B-band magnitude of NGC 4472 and the effective radius
R_e_ = 104 arcsec are comparable to the corresponding values for
NGC 4486. The SB-data are taken from Caon et al. (1994).

17. 1999A&AS..136..269F
Re:NGC 4472
This galaxy dust cloud is in the form of a small disk, similar to that
of the ionized gas, although smaller in size.

18. 1997A&A...321..765B
Re:NGC 4472
3.4. NGC 4472
CO detections from NGC 4472 have been reported by Huchtmeier et al. (1988,
1994), although their second "detection" is quite different from the first. We
observed this position 1' South of the nucleus (our data is given for this
position) and found no emission at a level well below their reported
detections. NGC 4472, was observed during both the May/June run and the August
run with non-detections in both cases. We conclude that CO has not been
detected in NGC 4472. We also observed the central position for a shorter time
and also found nothing (spectrum not shown).
The most sensitive HI measurements of NGC 4472 have yielded a non-detection
(see Huchtmeier & Richter 1989; Roberts et al. 1991; McNamara et al. 1994). The
neutral ISM in NGC 4472 is thus very poor indeed.

19. 1994CAG1..B...0000S
Re:NGC 4472
VCC 1226
E1/S0_1_(1)
CD-716-S
Jan 31/Feb 1, 1979
103aO + Wr2c
45 min
NGC 4472 is the brightest galaxy in the Virgo Cluster (Binggeli,
Sandage, and Tammann 1985), and is the center of Virgo subcluster B. A
few of the globular clusters in the envelope are well seen in this
print. The total number of its globular clusters is smaller than in
NGC 4486 by at least a factor of three. Harris (1988) lists a specific
frequency of S = 5.5, which is near the average of all E galaxies. The
specific frequency of S = 15 for NGC 4486 is abnormally high. An
explanation for the high number in M87 may be related to its position
in the highest concentration of dE,N nucleated dwarf elliptical
"companions" in the Virgo Cluster. NGC 4472 is at the center of Virgo
Cluster subcluster B, which does not have the high concentration of
nucleated dE,N galaxies (Binggeli, Tammaun, and Sandage 1987) that is
seen in Virgo subcluster A. Conceivably, the globular clusters in M87
were once the nuclei of dE,N galaxies that have since been tidally
disrupted and have sunk into the M87 envelope by dynamical friction.
Harris (1986) states that, as in NGC 4486, the radial profile of
the globular clusters in NGC 4472 is less steep than the underlying
luminosity profile of the stellar envelope of the parent galaxy.

20. 1994CAG1..B...0000S
Re:NGC 4472
M49
VCC 1226
E1/S0_1_(1)
CD-716-S
Feb 1/2, 1979
103aO + Wr2c
45 min
NGC 4472 is the brightest galaxy in the
Virgo Cluster. It is near the isoplethic center of
Virgo subcluster B (Binggeli, Tammann, and
Sandage 1987).
The luminosity gradient in the outer regions
appears flatter to the eye than that in pure E
types. An extended outer envelope is clearly
visible on overexposed plates taken in the dark
sky at Las Campanas. It is also well seen in the
print on the facing page, made from a 50 x 50
cm Las Campanas Virgo Cluster survey plate.
Compare the image in this print with images of
normal E1 galaxies in the previous section.
Many globular clusters exist throughout the
image, seen well in this print in the outer
envelope and previously discussed on panel 18.

21. 1994AJ....108.1579v
Re:NGC 4472
NGC 4472 (Messier 049)
NGC 4472 is the brightest elliptical in Virgo. The isophotes are well
approximated by ellipses from 0.5" to 15". The galaxy becomes gradually
rounder toward smaller radii. Inside ~2" the isophotal parameters are
poorly determined because of the low slope of the luminosity profile, the
low ellipticity, and a small patch of dust which disturbs the isophotes.
The isophotal profiles show no evidence for a photometrically distinct
nucleus whereas Davies & Birkinshaw (1988) and Franx et al. (1989a) find
clear evidence for a kinematically decoupled core in the inner 5".

22. 1994A&AS..106..199C
Re:NGC 4472
NGC 4472. It is the brightest object in the Virgo cluster (even brighter
than NGC 4486). It is a strong radio and X-ray emitter, and its
kinematics is characterized by a counter rotating stellar core (Saglia et
al. 1993).

23. 1994A&AS..105..481M
Re:NGC 4472
NGC 4472: This is the less peculiar of super-giant ellipticals in the
present sample, with e_4_ practically zero throughout. Our plate allowed
to extend the isophotal analysis up to 9.5 arcmin from the center. The
envelope is well above the r^1/4^ law.

24. 1976RC2...C...0000d
Re:NGC 4472
= M49
= Arp 134
= Holm 413a
Pair with NGC 4467 at 4.2 arcmin.
Faint anonymous dIm at 5.5 arcmin south-following
NGC 4470 at 10.5 arcmin
Description and Classification:
Ap. J., 143, 1002, 1966.
Ap. J., 148, 321, 1967.
Photograph:
P.A.S.P., 78, 367, 1966.
Ap. J., 143, 1002, 1966.
Ap. J., 148, 321, 1967.
"Nuclei of Galaxies", 27, 1971.
Photometry:
Ap. J., 139, 284, 1964.
Ap. J., 146, 28, 1966.
Photometry (5 Color):
A.J., 73, 313, 1968.
Photometry (B,V,R):
Ap. J., 173, 485, 1972.
Ap. J., 178, 1, 1972.
Ap. J., 183, 731, 1973.
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Spectrum:
Ap. J. (Letters), 164, L35, 1971.
Velocity Dispersion:
IAU Symp. No.15, p.112, 1962.
Spectrophotometry:
Ap. J., 164, 11, 1971.
Ap. J., 169, 209, 1971.
Ap. J., 175, 649, 1972.
Ap. J., 177, 185, 1972.
Ap. J. (Letters), 193, L49, 1974.
A.J., 74, 50, 1969.
A.J., 77, 333, 1972.
Bull. A.A.S., 6, 332, 1974.
IAU Symp. No.58, p.169, 1974.
Polarization:
Ap. J. (Letters), 179, L93, 1973.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
HI 21cm (upper limit):
A.J., 77, 568, 1972.
A.J., 79, 667, 1974.
Astr. Ap., 25, 451, 1973.
Sources R4 (M.N.R.A.S., 165, 231, 1973) and R5 (Nature, 208, 993, 1965)
rejected.
Radio Observations:
Astrophys. Lett., 6, 49, 1970.
A.J., 75, 523, 1970.
IAU Symp. No.44, p.222, 1972.

25. 1973UGC...C...0000N
Re:UGC 07629
Arp 134
E2 (de Vaucouleurs), E (Holmberg)
Very uncertain diameter values, corona appears visible to 12.? x 10.?
See UGC 07636
in Arp's class "E and E-like galaxies with nearby fragments"
12 26.8 +08 18 = NGC 4465 at 5.8, 285, 0.25 x 0.20, m=15.4
12 26.9 +08 16 = NGC 4467 at 4.0, 264, 0.45 x 0.35, E2 (de Vaucouleurs),
v = 1474, v(0)= 1381, m=15.2
UGC 07636 at 5.4, 142

26. 1964RC1...C...0000d
Re:NGC 4472
= Messier 049
= Holm 413a
Very bright center. Smooth nebulosity. Many globular clusters.
[Brightest in Virgo Cluster.]
Pair with NGC 4467 at 4.2 arcmin.
Faint, anonymous dIm galaxy at 5.5 arcmin.
NGC 4470 (peculiar) at 10.5 arcmin.
Photograph:
B.A.N., 16, 1, 1961.
Ap. J., 135, 6, 1962.
Photometry:
Ap. J., 71, 231, 1930.
Ap. J., 132, 306, 1960.
B.A.N., 61, 1, 1961.
M.N.R.A.S., 94, 806, 1934.
Spectrum:
Ap. J., 135, 734, 1962.
Radio Emission:
M.N.R.A.S., 123, 279, 1961.

27. 1918PLicO..13....9C
Re:NGC 4472
The very bright nucleus is not stellar; shows well in a 3m exposure. Nearly
round, 2' in diameter, fading out rapidly toward the edges. No structure
discernible, though spiral character is suspected near the center in the
short exposures. 28 s.n.


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