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Astron. Astrophys. 362, 75-96 (2000)

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2. Observational dataset

Source names, coordinates, and redshifts of the selected sample were taken from the NASA Extragalactic Database (NED) 2, and are listed in Table 1. Infrared observations were obtained for 18 of the sources with the Imaging Photopolarimeter on ISO (ISOPHOT; Lemke et al. 1996), and 3 were observed with IRAC1 on the 2.2 m ESO/MPE telescope. Millimetre and sub-mm data were obtained for 10 objects with the IRAM interferometer at Plateau de Bure in France (Guilloteau et al. 1992), the Sub-millimetre Common User Bolometer Array (SCUBA; Holland et al. 1999) on the James Clerk Maxwell Telescope 3 and the Swedish ESO Sub-mm Telescope (SEST) of the European Southern Observatory (ESO) at La Silla. The instruments used for each object are indicated in a footnote to Table 1.


[TABLE]

Table 1. Basic properties of the sample.
Notes:
[FORMULA]) SSRQ: Steep Spectrum Radio Loud Quasar; FSRQ: Flat Spectrum Radio Loud Quasar; RQQ: Radio Loud Quasar; RIQ: Radio Intermediate Quasar; NLRG: Narrow Line Radio Galaxy; RG: Radio Galaxy.
1) Observed with ISOPHOT; 2) Observed with SEST; 3) Observed with IRAC1; 4) Observed with IRAM; 5) Observed with SCUBA.
a) Classification in Falcke et al. (1996).


The observational details (observing date, wavelength, and measured flux density) of IRAC1, SEST, IRAM, and SCUBA observations are reported in Table 2. The data obtained with the SEST telescope were reduced to outside the atmosphere, corrected for the gain elevation characteristic of the telescope, and calibrated with Uranus. All IRAM observations were performed in compact configuration. All five antenna were used during most of the observations, with the exceptions indicated in a footnote of Table 2. The calibrators were 3C 454.3 for 3C 47, and 22040+420 and 1928+738 during the two observations of HS 1946+7658. SCUBA observations yielded good results at 850 µm only due to marginal weather. The fluxes were calibrated using the canonical gain value of 220 Jy/V, since a calibration scan at 850 µm was not done. The chosen value is relatively insensitive to the weather and should be good to within 20%. ISOPHOT observations and data reduction are described in the next section. These new observations were supplemented with literature data from radio to near-IR. We have also collected data at soft X-ray energies. For reasons of homogeneity we collected only ROSAT data, available for most of the sources. From published soft X-ray spectra we derived the flux at 1 keV corrected for absorption. The observed absorption is always compatible with the galactic absorption. The list of references from which data were retrieved, for each object, is reported in Table 3.


[TABLE]

Table 2. IRAC1, SEST, IRAM and SCUBA results.
Notes:
[FORMULA]) Upper limits to the flux are given at the 3[FORMULA] level. 1) Also observed on July 17, and 22. 2) Only four antenna were used on July 17. 3) Only three antenna were used on July 14, and four on July 17, and 22. 4) Also observed on May 23.



[TABLE]

Table 3. List of references of selected published data.
Notes:
[FORMULA]) 1: NED; 2: Gezari et al. 1997; 3: Brinkmann et al. 1997;
4: van Bemmel et al. 1998; 5: Kühr et al. 1981;
6: Tornikoski et al. 1996; 7: Steppe et al. 1993;
8: Veron-Cetty 1998; 9: Tanner et al. 1996;
10: Wilkes et al. 1994; 11: Kapahi 1995;
12: Sanders et al. 1989; 13: Lister et al. 1994;
14: Neugebauer et al. 1987; 15: Miller et al. 1993;
16: Ennis et al. 1982; 17: Elvis et al. 1994;
18: Reid et al. 1995; 19: Antonucci et al. 1990;
20: Chini et al. 1989a; 21: Lonsdale & Morison 1983;
22: Siebert et al. 1998; 23: Kellermann et al. 1989;
24: Blundell & Beasley 1998; 25: Yuan et al. 1998;
26: Falcke et al. 1996; 27: Andreani et al. 1999;
28: Barvainis et al. 1996; 29: Chini et al. 1989b;
30: Wang et al. 1996; 31: Schartel et al. 1996;
32: Kuhn et al. 1995; 33: Robson et al. 1998;
34: Haas et al. 1998; 35: Bloom et al. 1999;
36: Hoekstra et al. 1997; 37: Mitchell et al. 1994;
38: Neugebauer et al. 1986; 39: Ghosh et al. 1994;
40: Neugebauer et al. 1979; 41: Teräsranta et al. 1992;
42: Hughes et al. 1993.


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Online publication: October 30, 19100
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