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Astrometric Anomalies of Supernova 2006gy
Formerly SN 2006gy as a Possible Ritzian System
This page was extracted from
De Sitter's Whimsical Images on 06 Jun 2007.
Shade Tree Physics
Latest Update 22 Feb 2014. New or revised material is in bold.
Chandra X-Ray / Lick IR
Credit: Illustration: NASA/CXC/M. Weiss: X-ray: NASA/CXC/
UC Berkeley/N. Smith et al.; IR: Lick/UC Berkeley/J. Bloom & C. Hansen
Quoting from the
Chandra Chronicles 07 May 2007.
"SN 2006gy was first detected by an optical robotic telescope as part of
the Texas Supernova Search project on September 18, 2006. It brightened
slowly for about 70 days, peaked at a luminosity or intrinsic brightness
equal to that of 50 billion suns - ten times brighter than its host
galaxy - and began a slow decline."
"The Chandra data, taken 56 days after the explosion of SN 2006gy, revealed
that SN 2006gy was a relatively paltry X-ray emitter. Although a collision
of the supernova debris with the surrounding cloud is occurring, the cloud
is not dense enough to explain the optical brilliance of the supernova. The
weak X-ray emission also rules out any type of gamma-ray burst event."
I have been assuming that the 14 November 2006 Chandra image was taken
earlier, or that it was a summed series of images spanning the timeframe
of late September 2006 to 14 Nov. Right now, this viewpoint appears to
be wrong. and if so, much of this article is going have to be removed.
[Added 05 Jul 2010.]
SN 2006gy Astrometry
(0) When SN 2006gy was first detected on 18 Sep 2006, its approximate
position was given as 2" west and 0" north from the center of NGC 1260.
(1) The offset listed on 24 Sep 2006, was 2".0 west +0".4 north
(2) On 26 Sep 2006 Prieto et al reported that the SN's position was
consistent with being at the center of NGC 1260, and that that position was
more consistent with an erruption of an active galaxy nucleus,
i.e. NCG 1260.
(3) On about 27 Oct 2006 Foley et al reported that the SN was
offset by about 1" from the nucleus of NGC 1260.
(4) On 01 Nov 2006 Ofek, et al reported,
"Our adaptive optics (AO) images (Fig. 3) show that SN 2006gy is located
0.99" ... at a position angle of 290 degrees [CCW from North] from the
nucleus of NGC 1260.
(5) On 04 Nov 2006, The Lick IR image shows
the SN when it was located at 0".941W and 0".363N, 1 σ = 0".01
for both measurements from the nucleus. This cartesian position is
equivalent to 1.01" at 291 degrees [CCW from North].
The following graph shows the reported positions (0) through (5)
for SN 2006gy, along with their uncertainties.
I have drawn in a hypothetical path (in blue) for the star which
produced SN 2006gy, and show the very non-intuitive ordering
of the star's locations, based on Ritzian relativity arrival
time modulation. These are labeled A through D.
Ritzian position D would be located to the southeast of the
center of NGC 1260. I have not seen a report which impacts favorably,
or otherwise, on an image in that location. (This "southeast" position,
may be considered as an experimentum crucis in the case of SN 2006gy.)
The (closest point of approach) position for a second star (necessary for
the Ritzian time reversal sequence) has been added to the drawing.
Reported positions (with 1σ uncertainties) for SN 2006gy
The following drawing shows computed times of arrival (based on Ritzian relativity)
for light pulses reaching us from two stars which have passed close enough to one
another to cause gravitationally induced velocity changes. It is shown to illustrate
Ritzian arrival time aberrations where large distances between sources and
observer are involved. For the blue star, between points B and C the arrival
times are occurring in reverse time. I claim that points A, B and C
are in consonnance with the disparate position reports for SN 2006gy. Point D, as mentioned
above, is currently in limbo. (Related animations are given further down in the article.)
SN 2006gy is generally thought to be located near to NGC 1260, some 240 million
light years from us. If the 27 Oct 2006 position(3) was in fact about one
arcsecond to the East of the 24 Sep 2006 position(1), then the distance to
NGC 1260 would lead us to the conlusion that SN 2006 had been traveling at an
average speed of approximately 18,000 times the speed of light (eastward)
during those 23 days.
Maanen would say that SN 2006gy is probably very much closer to us
than big universe proponents would have us believe.
Here's a gif animation of a binary star encounter (based on Microsoft Excel
c + v computations) which shows the non-intuitive arrival
time modulation, and hence apparently strange motions in the night.
The grey dots represent where each star actually was and the red dots show
where they seemed to be to an observer located (in this case) at
approximately 20 lightseconds to the right of the binary centroid.
Note that star A's apparent positions (the red dots) jump
to a post-perihelion region immediately prior to actual perihelion
passage, and then, following actual perihelion passage, they
very briefly jump back to a pre-perihelion region.
Again, this jump back is in consonnance with the apparent
motion between points B to C in the SN 2006gy
Apparent versus Actual Binary Star Positions
V(perihelion)=0.6c - Major axis diameter=1.0 Light Second (LS)
Binary Orbit period = 81 seconds. No extinction.
Observer is located 20 LS to the right of the binary centroid.
The model employed here is based on the idea that the observer's distance
from the binary is the same as the dispersive extinction distance, where
the absorbed and re-radiated light (whether faster or slower than the
standard value for c has become normalized to c. From that
point on, it travels at c with respect to the dispersive medium.
For animations for other observer distances from the binary, and
for more information on what the Ritzian model is portraying, see
Highly Elliptical Path Ritzian Variable Star Animations
Ritzian Relativity and Apparent Supernovae
(This section is in a state of constant re-write.)
A seven-frame sequence below shows how the close passage of two dim stars
(in a non-bound binary encounter) could produce a short-lived
X-ray doublet flash associated with
an otherwise supernova-like light curve. [Frames 1, 2, 4, 5, and 7 were
made by the author by modifying the Chandra and Lick images
displayed above. The track of the star which hypothetically beamed
its light toward Earth is added to all seven images.]
The jumps forward and backward are in accordance with
Ritzian relativity, i.e. the faster later (post perihelion) light overtaking
and passing slower earlier (pre-perihelion) light. The jump-forward
and back may explain Prieto's seemingly inexplicable report(2), early
in the game, that the SN was "consistent with the center of NGC 1260.
Hypothetical Ritzian Binary Sequence
Credit, original images, as above.
According to Ritzian relativity (See page
150 in the Introduction.), the velocity of a source is
additive to the velocity of its emitted light. When a star, which is
considered to be subject to Ritzian relativity, is executing
a parabolic or hyperbolic arc around behind another star, as it is
approaching the other star, and traveling away from us, c-v effects
slow down it's light that is emitted in our direction. Later on, as
it begins its outbound trek, c+v effects speed up it's light emitted
in our direction. This faster-later light has a tendency to catch up
with the slower-earlier light. The effect of these actions should be
much more pronounced for X-rays than for visible or longer wavelength
light because, according to J.G. Fox
(6), the shorter the wavelength, the greater
the extinction distance. (The extinction process normalizes
light speed that is different from c, to the speed of light
with respect to the medium through which it is traveling.)
Even though the original light becomes extinct in this process,
the re-emitted light preserves the Ritzian brightness and frequency
At longer wavelengths, such as in IR, the star that gave us
SN 2006gy would tend to appear as a continuously moving singlet with
a supernova-like light curve.
If the angular resolution of the viewing system is good enough, Chandra,
in this case, then the star's X-ray image can be seen as
simultaneous flashes at two different places (inbound and outbound)
along the star's track.
For more on the theory behind this speculative binary star scenario,
see A Ritzian Interpretation of Variable Stars.
In frame 3, the alignment of the left-hand X-Ray lobe and the nucleus of
NGC 1260 is, until compelling evidence leads elsewhere, considered by this
author to be a chance alignment.
The Double-Lobed X-ray Flash
What follows goes against the adage about not asking questions to
which you don't know the answers.
In the "double lobe" X-ray image of SN 2006gy, the lower-left
lobe has been identified as the nucleus of NGC1260. SN 2006gy has been
identified as the upper-right lobe.
does not list NGC 1260 as an X-ray source.
(Query Identifier "ngc 1260". Then, in the "Plots and Images" section, click on
"plot around." When the map pops up, X-ray objects will be shown
with "x" symbols. NGC 1260 is not so labeled.)
Now that the luminosity of the supernova has declined, is the X-ray
region which coincided with the nucleus of NGC 1260 still
as luminous as in the Chandra SN 2006gy image?
If the answer to the preceding question is "no" then the lobe must have
been a manifestation of SN 2006gy, and therefore is subject to being
interpreted as a piece evidence in favor of Ritzian relativity. If the
answer is "yes" then I'll have to think seriously of re-writing
(or pulling) this web page.
CBET = The Central Bureau for Electronic Telegrams
(Central Bureau for Astronomical Telegrams)
(1) Quinby, R. 24 Sep 2006, CBET 644, 1
(2) Prieto, J.L. et al., 26 Sep 2006, CBET 648, 1
(3) Foley, R.J. et al., Apx 27 Oct 2006, CBET 695, 1
(4) Ofek, E.O., et al., The Astrophysical Journal, 659:
L13-L16, April 10, 2007.
(5) Smith, N., et al.,
arXiv:astro-ph/061267v3 22 May 2007
(6) Fox, J.G.,
Am J. Phys. 33, 1, 16 (1965)