SIG_proteins_matrixProtein matrix for Fig. S1.SIG_proteins_treesTree files for Fig. S1super_SIG2_proteins_matrixProtein matrix for Fig. S2super_SIG2_proteins_treesTree files for Fig. S2SIG1_proteins_matrixProtein matrix for Fig. S3SIG1_proteins_treesTree files for Fig. S3SIG5_proteins_matrixProtein matrix for Fig. S4SIG5_proteins_treesTree files for Fig. S4SIGX_proteins_matrixProtein matrix for Fig. S5SIGX_proteins_treesTree files for Fig. S5

RSAM, MF, HF and DSAR time series for Ruapehu stations FWVZ over the 14 years explored, and for Whakaari stations WIZ over 9 years. Computing datastreams: we harnessed seismic data from a vertical component station for each individual volcano. We applied data processing techniques that resulted in the generation of four distinct time series, with a sampling interval of 10 minutes. Various measures were employed to capture different aspects of the seismic signal. The first measure, known as the Real-time Seismic Amplitude Measurement (RSAM), was obtained by calculating the 10-minute moving average of the velocity recorded by the vertical station This signal was then subjected to bandpass filtering within the frequency range of 2 to 5 Hz, which focuses on tremor signal of frequent volcanic origin while excluding ocean noise at lower frequencies. Similarly, the Median Frequency (MF) and High Frequency (HF) measures were derived using a comparable approach to RSAM, but with specific bandpass filtering applied. MF was obtained by filtering the signal within the frequency range of 4.5 to 8 Hz, while HF was obtained by filtering within the frequency range of 8 to 16 Hz. The 4.5 Hz threshold between RSAM and MF reflects an assumption that tremor mostly radiates energy below 4.5 Hz. To exclude this effect and explore attenuation related to permeability change (such as sealing), this frequency value is used as a threshold. Lastly, the Displacement Seismic Amplitude Ratio (DSAR) was calculated as the ratio of the integrals of the MF and HF signals. High values of DSAR have been inferred to correlate with high gas levels in the edifice, suggesting either reduced fluid motion and/or trapping that has led to a gas-accumulation. Quick recipes The steps below describe calculation of precursors discussed in this study. The first step is to calculate the data stream. There are several sub-steps: (1) After removing the instrument response to the seismic signals, apply a bandpass filters to each 24 hours of data, between 2-4.5, 4-8 and 8-16 Hz (corresponding to the RSAM, MF and HF bands). (2) Compute the absolute values of each signal. (3) Subdivide the signals into 10 minutes intervals. For each interval, compute the average value as the RSAM, MF and HF datapoints assigned to that interval. (4) (optional) Removing outliers associated with regional earthquakes is optional. We procced as follow: from (2), subdivide the signals into 10 minutes intervals. Calculated the mean and standard deviation (mu and sigma) for each interval. Apply z-score normalization in log-space to the interval using mu and sigma. Check if any value in the interval exceeds a threshold of 3.2 standard deviations above the mean. If yes, exclude data points from a 150s mask starting 15s before the outlier located. Calculate the average value in the interval excluding points inside the mask: this the RSAM, MF and HF value for the interval. To calculate the DSAR, procced as follow: (1) Integrate the bandpass filtered MF and HF data with time. (2) Take the absolute value and compute averages on 10-minute intervals. (3) Compute the ratio between integrated MF and HF.

The authors studied the X-ray properties of the young (~1-8M yr) open cluster around the hot (O8 III) star Lambda Ori and compared them with those of the similarly-aged Sigma Ori cluster in order to investigate the possible effects of the different ambient environments. They analyzed an XMM-Newton observation of the cluster using EPIC imaging and low-resolution spectral data. They studied the variability of the detected sources, and performed a spectral analysis of the brightest sources in the field using multi-temperature models. The authors detected 167 X-ray sources above a 5-sigma detection threshold the properties of which are listed in this table, of which 58 are identified with known cluster members and candidates, from massive stars down to low-mass stars with spectral types of ~ M5.5. Another 23 sources were identified with new possible photometric candidates. Late-type stars have a median log L_X/L_bol ~ -3.3, close to the saturation limit. Variability was observed in ~ 35% of late-type members or candidates, including six flaring sources. The emission from the central hot star Lambda Ori is dominated by plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with a wind origin. The coronae of late-type stars can be described by two plasma components with temperatures T₁ ~ 0.3-0.8 keV and T₂ ~ 0.8-3 keV, and subsolar abundances Z ~ 0.1-0.3 Z_sun, similar to what is found in other star-forming regions and associations. No significant difference was observed between stars with and without circumstellar discs, although the smallness of the sample of stars with discs and accretion does not definitive conclusions to be drawn. The authors concluded that the X-ray properties of Lambda Ori late-type stars are comparable to those of the coeval Sigma Ori cluster, suggesting that stellar activity in Lambda Ori has not been significantly affected by the different ambient environment. The lambda Ori cluster was observed by XMM-Newton from 20:46 UT on September 28, 2006 to 12:23 UT on September 29, 2006 (Obs. ID 0402050101), for a total duration of 56ks, using both the EPIC MOS and PN cameras and the RGS instruments. The EPIC cameras were operated in full frame mode with the thick filter. This table was created by the HEASARC in November 2011 based on CDS Catalog J/A+A/530/A150 files tablea1.dat ('X-ray sources detected in the Lambda Ori Cluster'), table1,dat ('X-ray and optical properties of sources identified with known cluster members and candidates') and table2.dat ('X-ray sources identified with possible new cluster candidates'). It does not include the objects listed in tablea2.dat ('3-sigma upper limits and optical properties of undetected cluster members and candidates'). This is a service provided by NASA HEASARC .