Date and Time of the Query: 2019-05-21 T07:32:14 PDT
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Notes for object NGC 1600

9 note(s) found in NED.

1. 2007MNRAS.377..759S
Re:NGC 1600
NGC 1600: this galaxy is a X-bright field elliptical E3 galaxy. It does not show
any sign of morphological disturbances (Michard & Prugniel 2004). The shape of
the isophotes is boxy and has a core shaped inner profile (Bender et al. 1989;
Faber et al. 1997). This galaxy has been proposed as a prototype of a merger
where the effects of gas have not been very important (Matthias & Gerhard 1999).

2. 2006ApJ...639..136H
Re:NGC 1600
NGC 1600. We extracted spectra in three contiguous, concentric annuli with
outer radii 0.8', 2.2', and 3.8' (13, 36, and 62 kpc), respectively. In
order to obtain interesting constraints, we tied Z_Fe_ between the inner
two annuli. We found a significant improvement in the fit (delta chi^2^ =
15) when two hot gas components (kT = 0.86 and ~3 keV), rather than one,
were used in the central bin. In the outer radii, only a single hot gas
component (kT = 1.5 keV) was needed. Using Chandra data, Sivakoff et al.
(2004) reported Z_Fe_ ~ 1.8 for a two-temperature fit within 1 effective
radius, falling to ~0.5 at ~3' (using our solar standard), which is
consistent with our results.

3. 2002A&A...391..531R
Re:NGC 1600
It shows ellipticity of 0.2. The position angle is nearly constant,
and the isophotes are boxy from 6" outward.

4. 2002A&A...391..531R
Re:NGC 1600
The galaxy NGC 1600, whose brightness profiles were very well fitted by
Sersic's law, presents the highest effective radius in B compared to the
JHK_s_ ones, indicating that its infrared-dominating stellar population
is concentrated in the central region of the galaxy. This galaxy presents
boxy isophotes, being the brightest galaxy of a physical association.
NGC 720 has also a profile fitted by Sersic's law (albeit not as well as
the former). The central region of the profiles of this galaxy is
responsible for the major deviation of the applied laws, being very
planar; taking this region (which extends up to 10") off the profile,
the de Vaucouleurs law fits very well. But we see that its isophotes are
disky in this very region, becoming boxy in the external region; this is
a strong evidence of the presence of a stellar disk in the central region.
Goudfrooij et al. (1994), using BVI photometry, also arrived at this
conclusion. Note that in the two cases where it was necessary to apply
Sersic's law, the value of the n parameter was lower than 4 (1.5 and
1.8 for NGC 1600 and NGC 720, respectively), indicating that these two
objects have a brightness profile more compact than the profiles of the
rest of the sample galaxies, well fitted by the de Vaucouleurs law.

5. 1999A&AS..136..269F
Re:NGC 1600
The dust extends farther than 15" with an asymmetric filamentary
structure in the W direction, while the H{alpha} emission is located in
a small 5" x 5" central disk.

6. 1976RC2...C...0000d
Re:NGC 1600
Brightest in a group.
Non-interacting pair with NGC 1601 at 1.6 arcmin.
Non-interacting pair with NGC 1603 at 2.5 arcmin.
Photometry: (VBR)
A.J., 75, 695, 1970.
Ap. J., 183, 731, 1973.

7. 1964RC1...C...0000d
Re:NGC 1600
Non-interacting pair with NGC 1601 at 1.6 arcmin,
NGC 1603 at 2.5 arcmin.
Discordant value of (B-V) (source A) rejected.
Brightest galaxy in the NGC 1600 Group including:
NGC 1599, NGC 1600, NGC 1601, NGC 1603, NGC 1604, NGC 1606,
NGC 1607, NGC 1609, NGC 1611, NGC 1612, and NGC 1613.
For other group members see dimensions data in
Heidelberg Veroff. Vol. 9, 1926, Lick 13, and Helwan 38.
Ap. J., 135, 733, 1862.

8. 1963MCG3..C...0000V
Re:MCG -01-12-017
Main member of a group of 8 galaxies. Type: Sand - E5, vB - E2,
Hub - E3. Redshift: +4728, G7; Cp' = 1.00.

9. 1918PLicO..13....9C
Re:NGC 1600
Oval; 1.5' long; rather large, brighter nucleus; no discernible spiral
structure. 31 s.n.

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