Date and Time of the Query: 2019-03-19 T12:00:33 PDT
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Notes for object NGC 7626

21 note(s) found in NED.

1. 2009ApJ...696.1218Z
Re:NGC 7626
NGC 7626. This is a radio-loud galaxy. Ho et al. (1997a) determine it to have a
possible L2 nucleus (the classification is characterized as highly uncertain),
with an [O III] luminosity of 3.3 * 10^38^ erg s^-1^ (100% uncertainty), which
implies a bolometric luminosity of 1.2 * 10^42^ erg s^-1^, giving {lambda}_bol_
= 0.0017. Since some correlated galaxies are chance coincidences, this may be
one of them.

2. 2007ApJ...668..130C
Re:NGC 7626
NGC 7626.-This galaxy's data are significantly off the grid of models. A
general feature that can be recognized from the location of this galaxy
in the SBF versus color panels, is that the stellar population is very
likely old, and metal rich, as also found by Denicolo et al. (2005). The
galaxy shows the presence of a dust lane; however, we do not recognize
irregular dust patches (neither from the V-band image, nor from the B-band
images also available from the ACS archive), which might lead to mark as
unreliable the SBF value for this galaxy.

3. 2006ApJ...639..136H
Re:NGC 7626
NGC 7626. We extracted a spectrum from a 2' (29 kpc) aperture. Only a
single hot gas component, with kT = 0.74 keV, was required. Our
best-fitting Z_Fe_ were in good agreement with those determined using ASCA
(Buote & Fabian 1998).

4. 2005ApJ...622..235T
Re:NGC 7626
NGC 7626 Radio core-jet with double lobes; nuclear dust lane

5. 2003ApJS..148..419N
Re:NGC 7626
NGC 7626 (UGC 12531).-This elliptical peculiar galaxy has a nuclear dust
lane (width : length = 0.17). It has a core-jet radio morphology on VLBA
scales and a twin-jet morphology on VLA scales. The STIS slits were
aligned parallel to the galaxy major axis. The central kinematic and
flux properties are listed in Table 26; the gas exhibits a regular
rotation profile. The fit to the central spectrum is improved by the
addition of a broad component. Data for this galaxy are shown in Figure
22 (see key in Fig. 1 for an explanation of these plots).

6. 2002A&A...391..531R
Re:NGC 7626
Isophotes have low eccentricity (~0.1). It shows a variation in the
position angle (~50^deg^). In general, its isophotes are disky
(B4 ~ 0.01).

7. 2002A&A...391..531R
Re:NGC 7626
Abrupt variations of position angle (more than 40^deg^) ocurred in the
galaxies NGC 596, NGC 636 and NGC 7626. The first presents very low
ellipticity, which means that, at least in part, the variation of the
position angle can be spurious. NGC 636 shows slightly disky isophotes.
In both objects, we can see strong and nonconstant variations in the
Fourier coefficients; Michard & Marchal (1994), through V photometry,
proposed for both objects a disk structure in the internal region. For
NGC 596, Goudfooij et al. (1994) found the same result.
Ferrari et al. (1999) found, for NGC 636, a conical axisymmetrical
distribution of dust. Ionized gas in the form of a small internal disk,
perpendicular to the orientation of the dust cone, was also found for
this galaxy (Macchetto et al. 1996).

8. 2001AJ....122..653R
Re:NGC 7626
NGC 7626: The warped nuclear dust lane seen in the optical images is
likely to be the culprit for flattening the optical profile toward the
center (Carollo et al. 1997). The dust lane is absent from our NIR residual
image, and we obtain a much steeper central cusp slope ({gamma} = 0.36
instead of {gamma} = 0.0).

9. 2000AJ....120.2950X
Re:UGC 12531
UGC 12531 (NGC 7626)-We detect weak evidence for a core-jet structure
in this source. The jet is misaligned by 10^deg^ from the direction of
the northern VLA jet. This apparent misalignment could be a real offset
between VLBA and VLA jets. However, owing to the faintness of the jet,
the measurement is uncertain.

10. 2000A&AS..144...53K
Re:NGC 7626
As discussed in Balcells & Carter (1993), the inner region of this
galaxy is not relaxed. The differences between its two sides are real
and reflect the complex kinematics. Some template mismatching is still
present at ~ 10-30 arcsec.
The comparison with the velocity and velocity dispersion profiles of
Balcells & Carter (1993) is good within the errors; the {sigma} data
of Jedrzejewski & Schechter (1989) are systematically on the lower

11. 2000A&AS..144...53K
Re:NGC 7626
B-band ground-based data from King (1978) and Peletier et al. (1990)
were merged with V-band HST-data (Bender, unpublished), after shifting
the HST-data by -0.6 mag.

12. 1999AJ....118.2592V
Re:NGC 7626
NGC 7626 has a nearby higher luminosity companion, NGC 7619, at
6.8' (90 kpc). They are the two brightest ellipticals in the Pegasus I
cluster. NGC 7626 has a counterrotating core (Forbes, Franx, &
Illingworth 1995; Carollo et al. 1997). There is a small warped dust
lane (diameter 230 pc/1.0") across the nucleus. Interestingly, the
central part of the dust lane is perpendicular to the radio jet, while
the warped outer part aligns with the major axis of the galaxy. There
is an unresolved nuclear emission peak, and low-level emission gas is
seen along the dust lane. NGC 7626 has double-sided radio lobes (Xu et
al. 1999a). Our isophotal analysis is in good agreement with previous
ground-based (Peletier et al. 1990; De Juan et al. 1994) and HST studies
(Carollo et al. 1997). The P.A. of the isophotes increases by 20^deg^
in the central 10". Forbes & Thomson (1992) reported excess light in the
galaxy that might be due to tidal interaction with NGC 7619.

13. 1998A&AS..130..267L
Re:NGC 7626
While our velocity curve is in agreement with that from both
Jedrzejewski & Schechter (1989) (PA = 7) and Davies & Birkinshaw (1988)
(PA = 4 ^deg^), our velocity dispersion profile presents a small
positive zero point shift with respect to that obtained by the latter
authors. The central velocity dispersion adopted by 7Sam is 234 km
s^-1^ (raw data range from 208 to 275 km s^-1^). The average value in
the literature (PS96) is {sigma}_0_ = 268 km s^-1^, well in agreement
with our estimate.

14. 1997ApJ...481..710C
Re:NGC 7626
A warped, symmetric dust feature (radius 0.45", seen also by F95)
crosses the very center of the galaxy and heavily obscures it. It
influences the isophotal parameters inside its radius. These show a very
steep increase in ellipticity that disappears in the fit to the dust-
improved I frame. The lane is tilted by ~35^deg^ with respect to the
radio jet (Jenkins 1982). A 20^deg^ twisting between 1" and 10" is
observed. This twist is barely significant, given the low ellipticity of
the isophotes. The V - I color map peaks at the very center of the dust
lane, with a value of 1.55 mag. The entire dust lane is on average ~0.12
mag redder than the surroundings. The color profile shows a continuous,
significant decrease with radius.

15. 1995AJ....109.1988F
Re:NGC 7626
NGC 7626: This galaxy is a giant elliptical (the most luminous in our
sample), paired with NGC 7619 in a loose group. A large shell is seen in
the outer eastern envelope (Jedrzejewski & Schechter 1988), and several
others are revealed after model subtraction along the NE-SW direction
(Forbes & Thomson 1992).This is the same direction as the observed radio
jets (Jenkins 1962). The galaxy nucleus is red, hinting at the existence
of dust (Sparks et al 1985). A kinematically distinct core was first
discovered in this galaxy by Jedrzejewski & Schechter (1988). Recently,
Balcells & Carter (1993) have mapped the central velocity field at high
resolution in several position angles. They find an extremely complex
kinematic structure, with several kinematically distinct components. They
conclude that the core kinematics were formed about 10^7^ yr ago and have
not yet dynamically relaxed. Thus the core region is dynamically young
and offers a unique opportunity to investigate a galaxy core that is
still forming. We find that the central regions reveal a strong major
axis dust lane extending at least 0.9"(300 pc) and some evidence for a
minor axis dust lane as well, giving the central galaxy an "X" pattern.
This causes the large position angle twist with respect to the outer
parts of the galaxy. The radio jet lies roughly at 45^deg^ to the dust

16. 1994CAG1..B...0000S
Re:NGC 7626
NGC 7619 Group
Aug 20/21, 1979
103aO + GG385
45 min
NGC 7626 is the second-brightest member of the NGC 7619 group
(Humason, Mayall, and Sandage 1956, Table XI), whose mean redshift is
= 3836 km/s. Both NGC 7619 and NGC 7626 have a central
historical role in the discovery of the linear redshift-distance
relation. Humason (1929), on a suggestion by Hubble, tested if larger
redshifts existed than the highest value of 1800 km/s previously
measured by Slipher. Humason used NGC 7619 to measure a redshift twice
as large as Slipher's largest, giving Hubble (1929) the basis to
suggest that the most fundamental fact of observational cosmology, the
redshift-distance relation, was about to be discovered.
The group, dominated by NGC 7619 and NGC 7626, contains many
bright early-type members and a number of dE dwarf elliptical
candidates. Redshifts of six of the brightest members have been listed
by Humason, Mayall, and Sandage (1956). The group is called Peg I in
Sandage (1975b, Table 4).

17. 1994ApJS...91..507D
Re:NGC 7626
NGC 7626 - It is one of the two brightest ellipticals in the Pegasus I
cluster. The radio source associated to it consists of two strong well
defined radio jets along P.A. 35^deg^ (Birkinshaw & Davies 1985).
Some optical properties of the host galaxy can be found in the
literature: Lauer (1985) presented ellipticity, position angle, and R
brightness profiles, evaluated assuming concentric isophotes; Bender et
al. (1988) gave profiles of ellipticity, position angle, and B_3_ and
B_4_ Fourier coefficients; Franx et al. (1989) and Peletier et al. (1990)
presented profiles of ellipticity, position angle, R-magnitude, U - R and
B - R colors, and Fourier coefficients of third and fourth order; Spark's
et al. (1991) gave B, V, I surface brightness profiles as well as
ellipticity, position angle, B_4_, and isophote displacements. All of the
results from these authors are in good agreement with ours.
We have not observed the excess light reported by Forbes & Thomson
(1992). These authors, using a masking-method different from ours, found
a region at the southwest with an excess light which could be due to
tidal effects (possibly with the brighter giant elliptical NGC 7619
located at the west).

18. 1976RC2...C...0000d
Re:NGC 7626
= PKS 2318+07
2nd brightest galaxy in the Pegasus I Cluster, with NGC 7611, NGC 7615,
and NGC 7619, NGC 7623, and NGC 7631.
Ap. J., 173, 485, 1972.
Photometry (UBV):
A.J., 74, 335, 1969.
Ap. J., 178, 1, 1972.
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Ap. J. (Letters), 164, L35, 1971.
Spectrum (velocity dispersion):
IAU Symp. No. 15, 112, 1962.
Ap. J. (Letters), 179, L93, 1973.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
Radio Observations:
Ap. J., 157, 481, 1969.
Ap. J., 189, 399, 1974.
A.J., 75, 523, 1970.
Astrophys. Lett., 6, 49, 1970.
M.N.R.A.S., 149, 91, 1970.

19. 1973UGC...C...0000N
Re:UGC 12531
E1 (de Vaucouleurs)
See UGC 12523

20. 1964RC1...C...0000d
Re:NGC 7626
In the Pegasus I Cluster.
Ap. J., 51, 304, 1920.
Dynamics and Mass:
Ap. J., 134, 262, 1961.
A.J., 66, 545, 1961.

21. 1961AJ.....66..541B
Re:NGC 7626
4. NGC 7619 Group
This is a group of five galaxies which form part of the Pegasus cluster (Hubble
and Humason 1931; Edson and Zwicky 1941); they are the brightest members of it.
The group has been studied by Hodge (1961). The types and velocities are
NGC 7611 (S0), +3579 km/sec; NGC 7617 (S0), +5068 km/sec; NGC 7619 (E3), +3953
km/sec; NGC 7623 (E4), +3659 km/sec; and NGC 7626 (E1), +3553 km/sec. The group
has an approximate diameter of 3.5 X 10^5^ pc and the separations between the
galaxies are on the average greater than 220 kpc. Consequently, Hodge finds that
the virial theorem is satisfied only for galactic masses in the range
10^12^-10^13^ M_sun_ and mass-to-light ratios of the order of 300. There is some
difficulty in estimating the total population of the cluster containing the
brightest galaxies listed by Hodge. Probably the estimate by Zwicky (1959, p.
63) of about 60 members is the best. If the five that have been measured form a
good sample of the whole, and if the cluster has little central concentration,
as seems to be the case, then we may conclude that probably the whole group is
unstable, unless a considerable amount of dark material is present.

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