Re: Porrima image
From: Bill Becker (bbe51_at_rmisp.com)
Date: 03/10/05
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Date: Thu, 10 Mar 2005 16:27:42 -0700
Cool project and the results you've had so far look encouraging.
Btw, here's an image of Sirius, also taken with a 4" refractor:
http://www91.sakura.ne.jp/~kay2/photo/e_sirius_b.htm
Best regards,
Bill
"Pete Lawrence" <pete.lawrence@nospam.co.uk> wrote in message
news:i30131plnvihppuv5vfhnj4sgrnhfq0nc0@4ax.com...
> Ok - I'm not claiming anything here and I will not be happy until I
> have taken one or more confirmation shots and got reproducible
> results. However... the images are compelling to say the least. I
> determined an accurate estimate for the PA of the system without
> knowing the official version (obviously you only have my word for this
> ;-) ) which may say something about the veracity of the PA result.
>
> I can't work out the separation accurately because I have no rulers to
> guide me with which I have any confidence. However, Dave Randell
> confirms that the spurious disk vs the apparent separation of the
> peanut lobes is consistent with current separation estimates.
>
> I'm bothered by the extra star that appears in the enhanced 1/90s
> exposure. In trying to identify this star, I've come across some odd
> inconsistencies with several star chart programs too. SkyMap Pro
> shows there to be two GSC stars close to Gamma - GSC-4949-1113 mag.
> +2.9 (!) and GSC-4949-1112 mag. +3.7 (also !). StarryNight shows
> there to be a mag +12 star next to Gamma called, ahem, Gamma and Guide
> shows nothing in the general vicinity.
>
> Well, if my observational image is wrong (and there's every chance it
> is seeing as it was taken with a 4" APO!) then it's in good company
> ;-)
>
> Here's the result...
>
> http://www.digitalsky.org.uk/doubles/Porrima_pa_estimate_20050307_800.jpg
>
> I'll carry out a second imaging session asap and post the results -
> whatever they may be. My gut feeling is that the elongation is
> correct but the peanut 1/90s result is not.
>
> --
> Pete
> http://www.digitalsky.org.uk
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