All Tables

Table 1: Dense cores covered by the c2d MAMBO survey. The table lists, from left to right, the core name adopted within the c2d collaboration, names for the cores adopted by other authors, the core distance, the type of the core (i.e., starless, YSO, or VeLLO), the approximate galactic environment of the dense core, and whether Spitzer data is available for the core. The last column gives a rough description of the morphology of the subcores (i.e., extended substructures; see Sect. 3.2) within each core using the c2d standard morphology keywords (Enoch et al. 2006, see Sect. 3.3 for a description).
Table 2: MAMBO map details. For each core the products ``number of maps'' $\times$ ``array type'' list how often a core was observed with which array (``37'' for MAMBO-1 and ``117'' for MAMBO-2). Several products are given if a dense core was observed with both arrays. The last column lists the minimum noise level in a map after smoothing to $20 \hbox {$^{\prime \prime }$ }$ resolution.
Table 6: IRAS sources in the MAMBO maps that are not detected as MAMBO emission peaks. For every core in the c2d MAMBO survey the table lists sources from the IRAS Point Source Catalogue and the IRAS Faint Source Catalogue (preceded by an ``F''), and the subcores in which the IRAS sources are located, if applicable. Objects from the IRAS Point Source and Faint Source catalogues present in both catalogues are connected. The last column gives the spectral index between 12 and $25~\rm \mu m$ wavelength.
Table 7: Properties of MAMBO-detected IRAS sources. For every core in the c2d MAMBO survey the table lists dust emission peaks and, if applicable, the related subcore associated with an IRAS source (Sect. 4.1 discusses the identification of associated sources; FSC sources are preceded by an ``F''). Associated 2MASS sources are listed too. The table further lists the spectral index between 12 and $25~\rm \mu m$ wavelength, the bolometric temperature and luminosity, the submillimetre-to-bolometric luminosity ratio, the mass within a peak-centered aperture of 4200 AU radius, and the infrared SED class.
Table 8: Properties of MAMBO detected c2d Spitzer sources. Like Table 7, but now listing sources from Spitzer point source catalogues and giving the spectral index between 2.2 and $24~\rm\mu m$ wavelength. VeLLO candidates are marked in the class designation.
Table 9: Prominent YSOs detected in Spitzer data not taken by c2d, and related IRAS sources, if existing.
Table 10: Cores in the c2d MAMBO survey with YSOs uncovered by c2d that were believed to be starless at the beginning of the c2d survey. Comments on outflows refer to jet-like extended ( $\gg$ $1\hbox {$^\prime $ }$ ) features in IRAC images.
Table 11: Starless cores that fulfill at least one criteria for an advanced evolutionary state, as well as VeLLO candidate cores. Brackets for VeLLOs indicate that $r_{70\%}$ does not fulfill the criterion for evolved cores after correcting for internal luminosity.
Table 12: YSO offsets from dust emission peaks. For each dust emission peak, and related subcore, associated with a YSO listed in Tables 7 and 8 we give the chosen reference source (preferentially seen by Spitzer) and the observed offset and position angle (i.e., position of star w.r.t. the dust emission peak).
Table 3: General data on subcores. Bracketed and starred subcore designations indicate subcores with uncertain properties due to artifacts and subcores with associated YSOs or VeLLOs, respectively. For every subcore the table lists the position of its ``center of gravity'', the subcore area and effective radius, the integrated flux density and mass for the whole subcore as well as its area above 50% of its peak intensity, and the maximum signal-to-noise ratio within the subcore boundaries.
Table 4: Geometry data for subcores. See Table 4 for an explanation of the subcore designations. For every subcore the table lists the major and minor axis at the 50% peak intensity level and their ratio, the position angle of the major axis (east of north), the filling factor for an ellipse defined by the aforementioned axis lengths and orientations, and the effective radius at the 70% peak intensity level.
Table 5: Data on dust emission peaks. Bracketed and starred peak designations indicate peaks with uncertain properties due to artifacts and peaks with associated YSOs or VeLLOs, respectively. For every peak the table lists the peak position, the associated subcore, if applicable, the peak flux density per $11 \hbox {$^{\prime \prime }$ }$ beam (after smoothing to $20 \hbox {$^{\prime \prime }$ }$ resolution) and the related column density and extinction, the flux density and radius for an aperture of $4200~\rm AU$ radius, and the flux densities for the c2d standard apertures between $20 \hbox {$^{\prime \prime }$ }$ and $120 \hbox {$^{\prime \prime }$ }$ diameter.
Table A.1: Standard c2d conversion factors for masses and column densities from dust emission. For each bolometer camera employed by the c2d collaboration we list the effective wavelength, the half power beam width, the dust opacity at the effective wavelength (per gram of ISM), the conversion factors between intensity and column density, and between integrated flux density and mass (this for a distance of $100~\rm pc$ ), respectively.