We have obtained K' images for the 18 active galaxies together with Jimages for 15 of them. J and K' images were taken for 11 non-active
spirals. The infrared data have been acquired mainly with three
telescopes: the 2 m Télescope Bernard Lyot (Pic du Midi Observatory,
France), the 2.5 m DuPont telescope (Las Campanas, Chile), and the 3.5 m
telescope at Calar Alto (Spain). We have also used some short
observations taken with the ESO 2.2 m telescope in La Silla for the
relative calibration of one of the J images obtained during a
non-photometric night. The journal of observations is presented in
Table 2. We always used NICMOS-3 256
256
detectors; the pixel scales are given in Table 2.
Name | Teles. | Obs. | Filter | Exp. | Seeing |
![]() |
date | time | FWHM | (mag/ | |||
(s) | (arcsec) | arcsec2) | ||||
UGC 1395 | CAHA | 09/96 | K' | 5400 | 0.95 | 20.7 |
IC 184 | CAHA | 09/96 | K' | 1800 | 0.95 | 19.8 |
IC 1816 | LC | 09/96 | K' | 3000 | - | 20.1 |
J | 800 | - | 21.0 | |||
UGC 3223 | LC | K' | 2700 | 1.2 | 19.9 | |
NGC 26391 | TBL | 03/97 | J | 1000 | - | 20.5 |
K' | 3000 | - | 19.7 | |||
IC 2510* | LC | 05/96 | K' | 3600 | 0.87 | 19.6 |
04/97 | J | 1000 | 0.71 | 20.8 | ||
NGC 3281 | LC | 05/96 | K' | 3500 | 0.84 | 19.8 |
04/97 | J | 1000 | 0.89 | 21.1 | ||
NGC 3660 | LC | 04/97 | J | 1200 | - | 21.3 |
04/97 | K' | 2000 | - | 20.2 | ||
NGC 42533 | TBL | 03/97 | J | 1000 | - | 21.3 |
K' | 2800 | - | 19.3 | |||
NGC 4507* | LC | 05/96 | J | 1400 | 0.80 | 21.0 |
K' | 3600 | 0.97 | 20.2 | |||
NGC 47853 | LC | 04/97 | J | 1000 | 0.71 | 20.8 |
K' | 3000 | 0.71 | 20.2 | |||
NGC 5347*,2 | TBL | 03/97 | J | 1000 | 1.4 | 21.3 |
K' | 3060 | 1.9 | 19.4 | |||
NGC 5728 | LC | 04/97 | J | 1000 | 0.88 | 20.9 |
K' | 2800 | 0.85 | 20.2 | |||
ESO 139-12 | LC | 05/96 | J | 1000 | 1.0 | 21.2 |
K' | 3400 | 0.97 | 19.5 | |||
NGC 68143 | LC | 05/96 | J | 1000 | 1.2 | 20.9 |
K' | 3200 | 0.87 | 19.3 | |||
NGC 68603 | LC | 04/97 | J | 1000 | 0.87 | 20.9 |
K' | 2600 | 0.89 | 20.3 | |||
ESO | 05/96 | K' | 720 | 0.89 | 17.5 | |
NGC 6890 | LC | 04/97 | J | 1000 | 0.76 | 20.7 |
K' | 2600 | 0.78 | 20.1 | |||
NGC 6951 | NOT | 09/96 | J | 1760 | 1.3 | 18.8 |
K' | 3520 | 1.3 | 19.5 | |||
NGC 1511 | LC | 09/96 | J | 800 | - | 21.1 |
K' | 1800 | - | 19.9 | |||
IC 454 | TBL | 03/97 | J | 1000 | 1.2 | 20.3 |
K' | 2800 | 1.25 | 19.2 | |||
NGC 2712 | TBL | 03/97 | J | 1000 | 1.1 | 20.7 |
K' | 3200 | 1.2 | 20.1 | |||
NGC 2811* | LC | 05/96 | K' | 3400 | 1.0 | 19.8 |
04/97 | J | 1000 | 1.19 | 20.7 | ||
NGC 35711 | LC | J | 1000 | 0.84 | 21.1 | |
K' | 3000 | 0.67 | 20.1 | |||
NGC 3835* | TBL | 03/97 | J | 1000 | - | 21.3 |
K' | 3000 | - | 19.7 | |||
NGC 4162 | TBL | 03/97 | J | 800 | 1.6 | 21.3 |
K' | 3000 | 1.1 | 20.0 | |||
NGC 4290 | TBL | 03/97 | J | 1200 | 1.1 | 21.0 |
K' | 3000 | 1.1 | 19.5 | |||
NGC 4779 | TBL | 03/97 | J | 4![]() |
1.1 | 20.9 |
K' | 4![]() |
1.1 | 19.3 | |||
NGC 6012 | TBL | 03/97 | J | 1000 | 1.2 | 21.0 |
K' | 3600 | 1.35 | 19.7 | |||
NGC 6155 | TBL | 03/97 | J | 600 | 1.15 | 21.0 |
K' | 3200 | 1.65 | 19.5 |
CAHA: 3.5 m telescope at Calar Alto (
);
LC: 2.5 m telescope at Las Campanas (
);
TBL: 2 m Bernard Lyot telescope at Pic du Midi (
);
ESO: 2.2 m telescope at La Silla (
);
NOT: Nordic Optical Telescope at La Palma. (
).
* Galaxies with non-flat remaining background.
1,2,3 Galaxies with NICMOS HST archive images,
(1) published by Böker et al. (1999); (2) published by Regan & Mulchaey
(1999); (3) unpublished.
As seen in Table 1, there are some galaxies with extended angular sizes close to 2 arcmin or even larger, which do not fit in a single frame. For two of them, namely NGC 4779 and NGC 6951, a mosaic of images was performed in order to have images for the entire galaxy disk.
The data reduction and calibration was performed, following the
standard procedures with the IRAF
software and SQIID package. For the objects, exposures of typically
about 2 minutes (dithered in short exposures of about 20 s in J and 50 s
in K' offset by about 2-3 arcsec) were taken on the source and on the
sky, until the total integration time was achieved (see Table
2). A median dark frame was calculated for every night
with the same exposure as that of the objects by using the
corresponding dark frames obtained before and after the observations.
Flat-field frames were obtained for each filter by subtracting the
median dark frame from the sky frames, normalizing the resulting
frames and calculating the median. We then subtracted the dark frame
from the object frame, divided by the normalized flat-field and
subtracted the corresponding sky frame. Sometimes, another constant
had to be subtracted in order to attain the zero background level. In
order to align the resulting frames to better than a pixel fraction we
used the non-saturated stars in these frames or, when there were no
stars, we used the centre of the galaxy. For the flux calibration a
number of standard stars were observed and mean extinction
coefficients were applied (kJ and kK' in magnitudes
airmass-1 are respectively 0.12 and 0.08 for Las Campanas and La
Silla, 0.12 and 0.10 for the TBL, 0.057 and 0.042 for the NOT and
kK'=0.1 for Calar Alto). The error level on the standard stars
amounts to 10%. In Col. 7 of Table 2 we give the
isophotal magnitude/arcsec2 corresponding to 2
of the
background.
We have retrieved HST calibrated infrared images obtained with NICMOS (filter F160W) for the eight galaxies for which such data was available (see Col. 1 in Table 2).
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