Project MK27: W75

W75N is like W3(IRS5) a star forming region (SFR). It also consists of minimal 3 star forming regions; named VLA1, VLA2, VLA3.
It has been monitored with single dishes for a long time see
We have combined our measurements from June to September 2022.
The procedure seems easy; just add and average them. However we have to deal with a dielectric resonator oscillator (DRO) drifting very much, and surely on another day the ambient temperaure is different.
So even when the spectra are looking thesame on the scale, we improved the alining by correlating two graphs.



One graph is set te be the reference, and correlated to a second graph. Next the second graph x-axis is shifted 1 bin and again the correlation factor is calculated.
Next in a correlation graph all the calculated correlation factors are displayed. With the correct bin shift used the top has to be on the 0 bin shift. Of course all this can be had automatically in a script also.


W75-multiplot 20/21-09-2022

From literature it seems that the peak on 10km/s is varying in amplitude but not much in velocity.
This aggregate of peaks is said to be originating from VLA1.



Between 8.5 and 10.5 km/s the peak is broad and overlapping peaks are present.
Also there seems to be a peak at 1.1km.s. In the copy it can be seen that these are generated by the VLA2 region.
With very long base interferometry measurements it is discovered that the H2O masers in VLA2 form a large ring.



pdf Evolution of the Water Maser Expanding Shell in W75N VLA 2.

The first measurement was done in 1999. It can be seen that the maser ring is circular. The last measurement we found was done in 2007.
Now it can be seen that the ring is developing into an elongated ring.
We found an explanation in another paper. In a simulation it is shown that it could be caused by a developing magnetic field in 40 years.

W75-elongated ring


pdf Stellar_physics_Observing_the_onset_of_outflow_col

In the end conclusions one of the authors of above paper remarked:

"Our observations show the “real time” evolution of such an originally poorly collimated outflow into a collimated one. This opens a new exciting window of opportunity to study how the basic ingredients of star formation (e.g.,
molecular outflow, ionized wind, magnetic field) evolve over the next few years, providing
insights that may have important implications for our knowledge of the early stages of highmass
star formation. We may be on the brink of describing and modeling in “real time” all
of these rapid changes."

Michiel Klaassen December 2022