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Date and Time of the Query: 2019-05-20 T16:48:33 PDT
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Notes for object NGC 1407

12 note(s) found in NED.


1. 2006ApJ...639..136H
Re:NGC 1407
NGC 1407. We extracted spectra in three contiguous, concentric annuli with
outer radii of 0.3', 0.8', and 2.1' (2.7, 6.1, and 16 kpc), respectively.
In order to improve the constraints, the abundances were tied between the
two inner annuli. We only required a single hot gas component in each
annulus. The temperature rose from ~0.65 keV in the center to 1.0 keV in
the outer annuli. We find some evidence of an abundance gradient in the
data, although the error bars are rather large. Given the large errors on
our interpolated global abundance, our best-fitting values are in general
agreement with the ASCA value of Z_Fe_ = 0.88^1.63^_-0.60_ found by Buote
& Fabian (1998).

2. 2005ApJ...635.1031B
Re:NGC 1407
NGC 1407.-There is a moderate Galactic H I column (5.42 x 10^20^ cm^-2^) and
extinction, and the Galactic H_2_ lines are prominent, along with the atomic
absorption lines. The stronger O VI line from NGC 1407 (1038.1 A) corresponds
to the location of a Galactic H_2_ line (although not one of the strongest
ones), but there is no apparent emission, nor is there emission at the location
of the weaker O VI line (Fig. 5).

3. 1994A&AS..105..433L
Re:NGC 1407
NGC 1407 (Fig. 7). The velocity dispersion profiles obtained at 0^deg^
and 90^deg^ are consistent with each other and with FIH, in giving a
central value of ~320 km s^-1^ and a smooth decrease outwards. No
rotation is detected at PA=0^deg^.

4. 1994A&AS..105..433L
Re:NGC 1407
NGC 1407 (Fig. 7). The velocity dispersion profiles obtained at 0^deg^
and 90^deg^ are consistent with each other and with FIH, in giving a
central value of ~320 km s^-1^ and a smooth decrease outwards. No
rotation is detected at PA = 0^deg^.

5. 1994A&AS..105..341G
Re:NGC 1407
Marginal detection of line emission centered on the nucleus. The B-V
image reveals a circumnuclear 'ring' which is slightly redder ({DELTA}
(B-V) ~0.01) than the nucleus. This feature is probably real since the
point spread function of the B and V images are well matched as can be
judged from stars in the field of view. Detected at 60 and 100 microns by
IRAS. Radio source. X-ray emission.

6. 1994A&AS..104..179G
Re:NGC 1407
Large, round galaxy. S4 ~ 0.01 at r ~ 40". Detected at 60 & 100 microns
by IRAS. Radio source. X-ray emission.

7. 1985SGC...C...0000C
Re:NGC 1407
Plate 3786
Near plate edge.
Plate 5541
Overexposed center, very faint much extended corona. 1st in group.

8. 1982ESOU..C...0000L
Re:ESO 033757-1844.5
=ESO 548- G 67
very large
very faint envelope
brightest in cluster

9. 1976RC2...C...0000d
Re:NGC 1407
Brightest galaxy in the NGC 1383-1407 Group.
Non-interacting pair with NGC 1400 at 11.8 arcmin
Radio Observations:
A.J., 75, 523, 1970.

10. 1968MCG4..C...0000V
Re:MCG -03-10-030
Main member of a large scattered group. Type: Sand - E0, vB - E0,
Morg - kE1(D), Vauc - E+0. Red shift: +1706, G3; Cp'=1.00.

11. 1964RC1...C...0000d
Re:NGC 1407
Small, bright, diffuse nucleus.
Brightest galaxy in the NGC 1383-1407 Group.
Non-interacting pair with NGC 1400 at 11.8 arcmin.

12. 1918PLicO..13....9C
Re:NGC 1407
0.7' in diameter, nearly round; center much brighter; no spiral structure
discernible. 27 s.n.


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