All Tables

Table 1: Observation log.
Table 2: Details of NIR observations. "Observing ID'' refers to the number of the data set in column one of Table 1. $\lambda$ is the central wavelength of the broad-band filter used. DIT is the detector integration time in seconds. NDIT is the number of exposures of integration time DIT that were averaged on-line by the instrument. Nis the number of images taken. The total integration time amounts to DIT $~\times~$ NDIT $~\times~$ N. Seeing is the value measured by the Differential Image Motion Monitor (DIMM) on Paranal at visible wavelengths. It provides a rough estimate of atmospheric conditions during the observations.
Table 3: Average position and flux of Sgr A* as obtained from the NIR data. The first column lists the observation ID (see Table 1), second and third columns the position of Sgr A* (average of all exposures) relative to its nominal position (Eisenhauer et al. 2003), and the fourth column the measured overall flux and standard deviation of Sgr A* during the particular observing session. The data were obtained by aperture measurements with a $\sim$ 50 mas radius circular aperture on the nominal position of Sgr A*. The flux measurements were corrected for extinction (see text). For data set 2, the average values are extracted from the first 120 exposures because the exposures obtained later were of very low quality.
Table 4: X-ray flare count rates: Given are the peak times and peak ACIS-I count rates in ${\times } 10^{-3}$ cts s^-1 in 2-8 keV band of the total flare emission and the flare emission corrected for the count rate during the IQ state. We also list the estimated start and stop times, the full width at zero power (FWZP) and full width at half maximum ( FHWM) values, as well as the peak and IQ flux densities. The candidate X-ray flare events $\phi$ 2 and $\phi$ 4 coincide with significant NIR flares (labeled I and IV in Table 6). The candidate X-ray flux density increase $\phi$ 1 is similar to $\phi$ 2. For the weak candidate flare events $\phi$ 1, $\phi$ 2 and $\phi$ 4 we only give estimates of FWZP.
Table 5: 8.6 $\mu$ m flux densities: flux densities are given in mJy. FWHM is given in acrseconds. The flux densities are dereddened using A_8.6 = 1.75. The calibration is described in the text.
Table 6: Emission properties of the NIR flare events from the infrared counterpart of Sgr A*. For each observing session we give the estimated IQ flux, which corresponds to the mean flux during its low flux density state during that session. The peak flux densities are corrected for the IQ state flux. The flux densities are dereddened using A_H = 4.3, A_K = 2.8, and A_L' = 1.8. In the case of a flare event detection we give the full zero start and stop times, the full zero width at the corresponding zero points (FWZP) and the full width at half maximum of the flare events. The time period listed with the infrared flare event II corresponds to a time of slightly increased source activity.
Table 7: NIR/X-ray flare flux densities. The peak flux densities of the flares detected in the individual wavelength bands are given. The spectral index is calculated assuming band centers of 2.2 $\mu$ m and 1.6 $\mu$ m in the near-infrared and 4 keV in the X-ray domain. The X-ray flares $\phi$ 2, $\phi$ 3 and $\phi$ 4 have been detected simultaneously in the NIR. For flare $\phi$ 1 only an upper limit in the H-band is available. For flare V no X-ray data exist. See comments on the candidate X-ray flare events $\phi$ 1, $\phi$ 2, and $\phi$ 4 in the text and in in Table 4.
Table 8: Emission properties of the radio flare events from Sgr A*. In the case of a flare event detection we we give the estimated peak flux density, the full zero start and stop times, the full zero width at the corresponding zero points (FWZP) and the full width at half maximum of the flare events. For the VLA we give the excess flux density over the mean flux density measured on 06 and 08 July.
Table 9: Parameters for representative models in agreement with the IQ (IQ1-IQ4) and flare states (F1 and F2) observed towards Sgr A*. These models are plotted in Figs. 16 and 17. The NIR flux density contributions from the synchrotron and SSC part of the spectrum as well as the SSC X-ray flux density are listed (Cols. 2 to 4). In the following columns we list the magnetic field strength B, observed cutoff frequency $\nu _{\rm m, obs}$ and flux density $S_{\rm m, obs}$ of the synchrotron spectrum, size $\theta$ of the source component and the spectral index $\alpha$ of the synchrotron component. All models except IQ2 provide synchrotron emission for frequencies up to $\nu _2 \sim 200$ THz. We assume that the cutoff in the energy spectrum of the relativistic electrons can be represented via an exponential cutoff in the observed synchrotron spectrum proportional to $\exp[-(\nu/\nu_0)^{0.5}]$ with the effective cutoff frequency $\nu _0$ . In the first column the NIR flux densities are given without (in brackets) and with modulation by the exponential cutoff.