During the observation of double stars abandoned (Neglected) is common to find other weak components are not scheduled at times appear to be associated physically with the major components. While it is not the primary objective of these observations, it is certain that it is interesting to report them in articles reporting the comments. Often, being faint stars, there are few data in the literature and although it is difficult to ensure the physical relationship, we can not rule it out. Regular observations of the new components, with a scheduled follow-up help tip the balance giving weight (forgive the metaphor) to one or other of the two cases. That's why, in my point of view, it should label such new stars as new components of existing systems, as well as have them be controlled, we might say and properly documented in terms of measurements that will be done regularly.
Work double stars, is working in a multigenerational campaign. I mean that the measurements made by historical observers, along with ours and that made the next generations of observers, will form a data volume that can be exploited in the future to draw relevant conclusions. Each and every one of us, with our modest contribution will be helping to flesh out a database developed over several hundred years. When we're gone, others will use our observations, the same way we now use the pioneer. Perhaps that is specific magic that surrounds the double stars: several generations of observers providing partial results in search of an end result that probably will not see. I do not think there is as altruistic as this field in observational astronomy. My words are very well summarized in a sentence of Ejnar Hertzsprung (1961): "The debt to our ancestors by the comments made on our behalf, we can only afford to do the same for the benefit of our successors" . What more could you want.
According to this philosophy and back to the beginning, in my remarks of 2009 on Stein's double stars, most of them long neglected, found four new domestic partners (close to any of the listed components) for other many ITS systems. To these must be added another pair, independent and completely new, located in one of the fields recorded in my images. Well, these couples were included in my unpublished article and proposals for inclusion in WDS. You can find all details in PDF this work published, as already announced, the OED number 6.
In two of these pairs, the optical train installed on my observation did not allow sufficiently precise measurements on my images and so enlisted the help of my colleague and friend Florent Losse so that, as a personal favor, to conduct the measurements with a telescope of 400 mm (GIFT , GI ant F Lorent's T elescope). Another example of generosity and altruism: Florent, thanks for your valuable help!.
Florent Losse Observatory in St. Pardon de Conques, France, with its excellent telescope. Courtesy of Florent Losse.
a few days ago I received an email from Brian Mason in which I communicated that it had included all pairs proposed in WDS. These are the respective entries:
During the drafting of article I had no notion of the existence of MRI 7 ( see previous post) and named as one of the new MRI 7AC. Finally, it has been listed by Brian Mason as MRI 11AC.
then I leave the pictures of all systems with some comments.
New STI2610 component. Left: MRI image OACP 5AC in 2009. Right: Superposition of two plates. Possi blue-O (1952), 2MASS-K White (1999). The small movement of the pair seems to be common.
New STI2753 component. Above: Left , MRI 8BC to the resolution of our instruments. In the center a three-dimensional mathematical modeling performed with the Surface software based on our images. Right: Composition of two images showing the stable elongation of the pair BC: orange, Possi-O (1952), white, 2MASS-H (1997). Below: Florent Losse pictures taken in 2010. Left: composite image in the spatial domain (shift and add). Centre: autocorrelograms on who carried out the measurements. Right: image croscorrelación to reject the ambiguity of 180 ° in position angle. The interferometric images were made with the new version of NR is now capable of supporting these techniques.
Left: MRI image from 9 to our instrumental resolution taken in 2009. Centre: Florent Losse image taken in November 2010. Right: composition of two old-blue images, Possi-O (1952) and in fuchsia 2MASS-J (1997) -. The pair is not resolved on these boards but there is clear evidence of common proper motion components. Superimposed, the proper motion vector set by the values \u200b\u200bof UCAC3.
New STI2768 component. Left: MRI an image OACP 10BC 2009. Right: Overlay two plates. Possi blue-O (1952), 2MASS-H White (1997). The small movement of the pair seems to be common.
New STI2683 component. Left: MRI an image 11AC OACP 2009. Right: Overlay two plates. Possi blue-O (1952), 2MASS-H White (1997). The small movement of the pair seems to be common.
Anyway, do not deny that these gifts are a great incentive for a professional observer can take more be hard if the next seasons of observation. Always, of course, with the priority background measurement of double stars discovered abandoned generations ago. In the course of this goes on and on circumstantial I often wonder who will do the same with my eleven MRIs. Here.
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