Nuclear activity in spiral galaxies
Coordinator: Siebenmorgen, Kruegel, Chini
Links:
README files: README
Finding charts: n/a: blind pointing
Abstract:
The N-band luminosity towards the centers of galaxies has long been known (Rieke & Lebofsky, 1978, ApJ 220, L38) to be a trustful indicator of activity. We wish to perform 10mic. imaging with VISIR at the VLT in our complete FIR--selected sample of spiral galaxies which contains some 160 objects with S_100mu > 9 Jy (Albrecht et al., 2004, AA 414, 141). The targets for the observations proposed here have been selected according to their distance to achieve a high spatial resolution and their IRAS 12mic. flux (> 0.4 Jy) and indication of activity. Two thirds of our objects show clear signs of central activity (starburst or Sy2), the rest none. As 10mic. continuum emission traces hot dust (heated either by OB stars or by an accretion black hole), the observations will serve as an independent check of the present activity classification and possibly detect new activity candidates. In view of the high spatial rewsolution (0.3" at the VLT) and the relative proximity of the sources, in the case of a starburst the emission is expected to be resolved and we will be able to delineate the structure of the starburst region. If an AGN is the major energy source, the emission should be point-like.
Data:
Program is available and data products can be downloaded
Links:
README files: README
Finding charts: n/a: blind pointing
Abstract:
The N-band luminosity towards the centers of galaxies has long been known (Rieke & Lebofsky, 1978, ApJ 220, L38) to be a trustful indicator of activity. We wish to perform 10mic. imaging with VISIR at the VLT in our complete FIR--selected sample of spiral galaxies which contains some 160 objects with S_100mu > 9 Jy (Albrecht et al., 2004, AA 414, 141). The targets for the observations proposed here have been selected according to their distance to achieve a high spatial resolution and their IRAS 12mic. flux (> 0.4 Jy) and indication of activity. Two thirds of our objects show clear signs of central activity (starburst or Sy2), the rest none. As 10mic. continuum emission traces hot dust (heated either by OB stars or by an accretion black hole), the observations will serve as an independent check of the present activity classification and possibly detect new activity candidates. In view of the high spatial rewsolution (0.3" at the VLT) and the relative proximity of the sources, in the case of a starburst the emission is expected to be resolved and we will be able to delineate the structure of the starburst region. If an AGN is the major energy source, the emission should be point-like.
Data:
Program is available and data products can be downloaded
| Name | RA(2000) | DEC(2000) | Mode | Obs.Time (h) | |
| NGC788 | 02h01m06.4s | -06d48m56s | 11.3 img 0.1"pfov | 1 | |
| NGC7603 | 23h18m56.6s | +00d14m38s | 11.3 img 0.1"pfov | 1 | |
| MCG -03-58-007 | 22h49m37.1s | -19d16m26s | 11.3 img 0.1"pfov | 1 | |
| NGC 0017 | 00h11m06.5s | -12d06m26s | 11.3 img 0.1"pfov | 1 | |
| NGC 1320 | 03h24m48.7s | -03d02m32s | 11.3 img 0.1"pfov | 1 | |
| NGC 2992 | 09h45m42.0s | -14d19m35s | 11.3 img 0.1"pfov | 1 | |
| NGC 7172 | 22h02m01.7s | -31d52m18s | 11.3 img 0.1"pfov | 1 | |
| NGC 7314 | 22h35m46.2s | -26d03m01s | 11.3 img 0.1"pfov | 1 | |
| 3C 120 | 04h33m11.1s | +05d21m16s | 11.3 img 0.1"pfov | 1 | |
| NGC 1194 | 03h03m49.1s | -01d06m13s | 11.3 img 0.1"pfov | 1 | |
| NGC 7469 | 23h03m15.6s | +08d52m26s | 11.3 img 0.1"pfov | 1 | |
| Mkn708 (NGC 2966) | 09h42m11.5s | +04d40m23s | 11.3 img 0.1"pfov | 1 | |
| Mkn538 (NGC 7714) | 23h36m14.1s | +02d09m19s | 11.3 img 0.1"pfov | 1 | |
| Mkn331 | 23h51m26.8s | +20d35m10s | 11.3 img 0.1"pfov | 1 | |
| Mkn332 (NGC 7798) | 23h59m25.5s | +20d44m59s | 11.3 img 0.1"pfov | 1 | |
| Mkn603 NGC 1222) | 03h08m56.7s | -02d57m19s | 11.3 img 0.1"pfov | 1 | |
| Mkn534 NGC 7679 | 23h28m46.6s | +03d30m41s | 11.3 img 0.1"pfov | 1 | |
| Mkn1022 | 02h09m38.6s | -10d08m46s | 11.3 img 0.1"pfov | 1 | |
| Mkn617 | 04h33m59.8s | -08d34m44s | 11.3 img 0.1"pfov | 1 |