Date and Time of the Query: 2019-08-21 T11:00:26 PDT
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Notes for object NGC 1566

19 note(s) found in NED.

1. 2008MNRAS.385..553D
Re:NGC 1566
NGC 1566: The spiral arms of this grand-design galaxy are well traced in
the 3.6 microns and monochromatic images. Inside the 20 arcsec radius
lies intense Doppler broadening typical of a Seyfert 1 galaxy but too
strong to be sampled by the free spectral range of the FP interferometer
used for our observations. Also, there is an expanding bubble of gas
located near {alpha}= 04^h^19^m^58^s^, {delta}=-54^deg^55'13" associated with
four strong H II regions in the north-west arm and exhibiting a strong
velocity gradient. These results are consistent with the H{alpha}
observations made by Pence, Taylor & Atherton (1990). See Aguero, Diaz &
Bajaja (2004) for a dynamical analysis based on long-slit spectroscopy.

2. 2005ApJS..157...59L
Re:NGC 1566
This face-on barred Sbc spiral galaxy (at a distance of 13.4 Mpc) shows clear
spiral patterns. ULX1 (IXO 24) and ULX2 are on the thin spiral arms, and ULX3 is
on the edge of a spiral arm. During 5 years of observations, all three ULXs
showed variations in luminosity by more than 50%. ULX3 showed variability during
a 5 day observation.

3. 2004MNRAS.350.1049G
Re:NGC 1566
9.7 NGC 1566 A detailed discussion of the event around JD 2447000, as
observed at many wavelengths from the X-ray to the IR, was given by
Baribaud et al. (1992). A time-lag of 2 +- 1 months was found between
the UV and the IR. This result was criticized by Oknyanskij & Horne
(2001), who find that the delay is consistent with 0 and is less than 20

4. 2004A&A...415..941E
Re:NGC 1566
NGC 1566: Listed by Moiseev (2001), based on the suggestion of a triaxial bulge
by Baumgart & Peterson (1986). Inspection of F606W and F814W WFPC2 images shows
strong dust lanes leading to a nuclear spiral in the inner r < 3" region. The
K-band image of Mulchaey et al. (1997) shows no inner ellipticity peak and only
a slight twist in the position angle, most likely due to the nuclear spiral.

5. 2002ApJS..143..257K
Re:NGC 1566
0420-5456ra.---Not a good continuum fit to 4000--4800 {Angstrom}
region; for a better H{alpha} fit, an intermediate H{alpha} component
was introduced in addition to the narrow and broad components.

6. 2002A&A...389...68G
Re:NGC 1566
NGC 1566: this galaxy was also studied in the first paper, where
we used the catalog by Comte et al. (1979) which traces also the
external arms. For this new catalog, the HII regions are placed
mainly in the inner oval part and the results of our methods
disagree. The values obtained from the first catalog by
GGA (1991) are in good agreement with the values from the
kinematics, so we adopt the mean values of the GGA values and
the optical velocity field from Pence et al. (1990).

7. 2001ApJS..137..139S
Re:NGC 1566
NGC 1533 and NGC 1566 (the Dorado Group). - The mean velocity of 11
group members tabulated in Ferguson & Sandage (1990) is 1342 km s^-1^.
We adopt this for both galaxies and compute an H_0_ distance.

8. 2001ApJS..136...61S
Re:NGC 1566
5.12. NGC 1566
This galaxy possesses weak emission lines for a Seyfert (Osmer,
Smith, & Weedman 1974). HST WF/PC1 observations of NGC 1566 made by
Kriss et al. (1990) show that the emission line gas has a point source
contribution with a component that extends to less than 0.7", while
subsequent HST continuum imagery reveals spiral dust lanes within 1" of
the nucleus (Griffiths et al. 1997). Its optical spectrum is that typical
of a Seyfert 1 galaxy (Kriss et al. 1990). However, according to
Hawley & Phillips (1980) its nuclear spectra resembles more that of an
H II region than that of a Seyfert galaxy except for the broad emission
wings at H{alpha}. A strong X-ray point source with weaker extended
emission was found through ROSAT observations (Ehle et al. 1996).
Multiwavelength nuclear variability (from X-ray to near-IR) has been
reported by Baribaud et al. (1992) with X-ray emission variations up to
40% within timescales less than a month. A prominent large-scale bar is
seen in near-IR images (Hackwell & Schweizer 1983). Both large-scale and
nuclear radio emission is seen in NGC 1566 (Harnett 1984, 1987).

9. 1999A&AS..137..457M
Re:NGC 1566
NGC 1566: A possible faint blob of radio emission is detected 3" north
of central peak (Fig. 7). Observations with the PTI at 13 cm (R94 and
S95) give a 5 mJy flux.

10. 1997ApJS..110..299M
Re:NGC 1566
Bar is visible in both the ellipse fits and the K_S_image. Unbarred in the

11. 1997A&A...319...33A
Re:NGC 1566
NGC 1566 No map is shown here although there is a strong pair of X-ray sources
well aligned across the Seyfert having C=13.6 and 21.8. The identification of
these two sources is uncertain, the best possibilities are extended objects
about 20th and 18th magnitude respectively. Other sources in the field are
possibly identified with faint galaxies and BSO's, including a likely quasar
candidate of C=2.2 about 20th magnitude, 7.0' SE of the galaxy nucleus
(04/20/34.4, -55/01/24(2000)).

12. 1996ApJ...463..498S
Re:NGC 1566
A2. NGC 1566
The WF/PC 1 images of this galaxy have been studied by Kriss et al. (1990).
The emission-line image of this Seyfert 1 galaxy is pointlike, having a
maximum extent of 0.7" (59 pc).

13. 1995A&AS..114..147B
Re:NGC 1566
NGC 1566, classified as SAB(s)bc in the RC3, is the brightest member of
the Dorado Group. The surface photometry (de Vaucouleurs 1973), the
ionized gas distribution (Comte & Duquennoy 1982), and the infrared
mapping (Hackwell & Schweiser 1983; Baumgart & Peterson 1986) indicate
that the large-scale structure of NGC 1566 consists of a double two-armed
spiral pattern, the inner one of which originates at the ends of the bar,
with a significant contribution from young OB associations(Hackwell &
Schweizer 1983). The large-scale kinematics of NGC 1566 was investigated
by Pence et al. (1990) using the Taurus machine. HST observations of the
Seyfert like core of this galaxy are reported by Kriss et al (1991).
Likely radii of the principal resonances of the spiral system of NGC 1566
were determined by Elmegreen&Elmegreen (1990) by investigating the
optical morphology.
The observations made in the radio continuum by Harnett (1984, 1987),
show that the radio emission extends over the nucleus and the disk. This
galaxy has been observed also in the HI line by RMGWS82 and by B79.

14. 1994CAG1..B...0000S
Re:NGC 1566
Dorado [Group] #53
Dec 30/31, 1980
103aO + GG385
45 min
NGC 1566 is an awesome sight. No written
description is adequate to convey the scene when
the galaxy is viewed through an eyepiece at the
focus of a telescope rather than on an electronic
The inner two grand design arms (seen in
the insert) are of very high surface brightness
and are studded with HII regions. Each arm can
be traced at high surface brightness for half a
revolution of unwind from beginnings on opposite
sides on the rim of the central bulge. Dust lanes
can be traced closer to the center than the
beginning position of the luminous arms.
Sets of low-surface-brightness outer arms
with fragmented branches exist outside the two
main grand design inner arms. The pattern of the
two outermost of these faint arms is highly
symmetric; each can be traced for another half
The resolution of the arms into individual
stars and HII regions occurs at a slightly brighter
level than in the giant spirals of the Virgo Cluster.
NGC 1566 is the brightest galaxy in the
Dorado Group (Ferguson and Sandage 1990).
The adopted mean redshift of the group is
= 1056 km/s. The redshift of NGC 1566 itself is
v_o = 1305 km/s.

15. 1985SGC...C...0000C
Re:NGC 1566
Plate 1893
Overexposed center, bright narrow inner arms, faint patchy outer arms
form (R'): 7.5 x 5.8. Many very faint knots.

16. 1982ESOU..C...0000L
Re:ESO 041853-5503.4
=ESO 157- G 20
prominent in group
many stars imposed

17. 1979AJ.....84..472S
Re:NGC 1566
Two high-surface-brightness, very symmetrical arms with HII regions
that will probably resolve at the 2-3 arcsec level.
Lower-surface-brightness outer arms that branch and/or are
extensions of the two main arms.

18. 1976RC2...C...0000d
Re:NGC 1566
Type 1, faint variable Seyfert nucleus; B(nucleus) = 13.5 - 14.5,
B_T(excluding nucleus) = 10.35.
M.N.R.A.S., 131, 351, 1966.
Publ. Dept. Astr. Univ. Texas, II, 2, No. 7, 1968.
Astrophys. Lett., 11, 21, 1972.
Ap. J., 181, 31, 1973.
Ap. J., 189, 187, 1974.
J.R.A.S. Canada, 68, 117, 1974.
Atlas Gal. Australis, 1968.
A.J., 73, 858, 1968.
Astrophys. Lett., 11, 21, 1972.
Ap. J., 181, 31, 1973.
Ap. J., 189, 187, 1974.
Att...Conv.Sci.Osserv. Cima Ekar, Padova-Asiago, 101, 1973
= Contr. Asiago No. 300 bis.
Photometry:(I.R. 1-3.5 microns)
M.N.R.A.S., 164, 155, 1973.
Astrophys. Lett., 6, 155, 1970. 11, 21, 1972.
Ap. J., 189, 187, 1974.
Astr. Ap., 33, 331, 337, 1974.
M.N.R.A.S., 168, 109, 1974.
Distance Modulus:
M.N.R.A.S., 131, 365, 1966.
Ap. J., 181, 31, 1973.
Radio Observations:
Australian J. Phys., 16, 360, 1963.
M.N.R.A.S. 152, 439, 1971.

19. 1964RC1...C...0000d
Re:NGC 1566
Small, very bright nucleus.
Asymmetric, very faint outer arms.
P.N.A.S., 26, 34, 1940.
Observatory, 77, 146, 1957.
Revista Astr., XXIX, no 143, 1957.
Observatory, 77, 146, 1957.
Mem. R.A.S., 68, 69, 1961.

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