Astronomy & Astrophysics

All Tables

Table 1: Up-to-date catalogue of FU Orionis objects (for column description see Sect. 2.1). References: [1] Eislöffel et al. (1990); [2] candidate, other designation: V1184 Tau, Yun et al. (1997); [3] Herbig (1977); [4] Carr et al. (1987); [5] Sandell & Aspin (1998); [6] Staude & Neckel (1992); [7] Reipurth 50 N IRS 1, Strom & Strom (1993), $\alpha _{2000}=\rm 5^h40^m27.4^s$ $\delta _{2000}=-7^{\circ }27'33''$ ; [8] assumed to be in a pre-outburst state, McMuldroch et al. (1992); [9] Elias (1978); [10] Graham & Frogel (1985); [11] Hartmann et al. (1989); [12] Staude & Neckel (1991); [13] Kenyon et al. (1993); [14] Hodapp (1995); [15] Hartmann & Kenyon (1996); [16] Aspin & Sandell (2001); [17] Reipurth & Aspin (1997); [18] Sandell & Weintraub (2001); [19] Chavarria-K. (1981); [20] Eiroa & Hodapp (1990); [21] Herbst et al. (1978); [22] candidate, Aspin & Reipurth (2003); [23] de Lara et al. (1991); [24] FU Ori candidate, in the state of rapid brightening since January 2004. An associated submm source was detected by Mitchell et al. (2001); [25] Lis et al. (1999).
Table 2: Sources of infrared photometric data used in our study.
Table 3: Log of ISOPHOT observations. Observing modes are described in Sect. 2.3, ISO_id is the unique 8-digit identification number of ISO observations.
Table 4: Photometric results of ISOPHOT and IRAS. All fluxes are colour-corrected and presented in Jy. (*): PHT32 observing mode. Source of IRAS data: PSC - V1735 Cyg, V346 Nor, Z CMa, Parsamian 21; Weaver & Jones (1992) - V1331 Cyg; this work (Sect. 2.4) - V1515 Cyg. In the case of V1057 Cyg the $12{-}60~\mu$ m fluxes are from Weaver & Jones (1992), the flux at $100~\mu$ m was re-determined in this work (Sect. 2.4).