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Project SR-71:
1971 Datsun 240Z with an sr20de-t. I have fabbed in a rear subframe from a 1990 Nissan 240SX S13 as well as the complete IRS from the S13. This includes the differential from a R32 Skyline and axles. I have also fabbed in the S13 front crossmember which allows me to use all of the suspension components from the S13. In order to make this work, I actually had to extend the wheelbase of the Datsun by about 7.5". This actually helps because the Datsun has a short wheelbase as it is, so this longer wheelbase puts it at about the same as the S13.
24 Jan 2026, 03:07 UT; Spotsylvania, Virginia USA. Bortle 4.5 zone.
Stellarvue SV80/9D achromat telescope, ZWO AM5 mount and ASI533MM Pro camera, autoguiding, no calibration frames, SVBony 5nm narrowband filters, exp 240s, gain 100, bin 1x1, 15 subframes each filter (S, H, and O), sensor -10°C, autofocus. Data acquired in ASIAir and processed in Pixinsight. Image scale: 1"/pixel.
Clouds: scattered clouds
Transparency (AL): 5
Seeing (AL): F
Moon: illuminated 28%, age 5.3 days
Apparent magnitude - very dim
Apparent size 50 arcmin
Notes: False color -- narrowband SHO data processed in the Hubble palette to differentiate areas of Sulfur II, Hydrogen alpha, and Oxygen III emission.
Appearance: Significant portions of target cutoff at right and bottom of frame. Use longer test exposure (without filter) when framing dim targets. Redcat51 with ASI533 would provide better FOV for framing this target.
From Wikipedia
IC 443 (also known as the Jellyfish Nebula and Sharpless 248 (Sh2-248)) is a galactic supernova remnant (SNR) in the constellation Gemini. On the plane of the sky, it is located near the star Eta Geminorum. Its distance is roughly 5,000 light years from Earth.
IC 443 may be the remains of a supernova that occurred 30,000 - 35,000 years ago. The same supernova event likely created the neutron star CXOU J061705.3+222127, the collapsed remnant of the stellar core. IC 443 is one of the best-studied cases of supernova remnants interacting with surrounding molecular clouds.
The SNR optical and radio morphology is shell-like (e.g. a prototypical shell-like SNR is SN 1006), consisting of two connected sub-shells with different centers and radii. A third, larger sub-shell—initially attributed to IC 443—is now recognized as a different and older (100,000 years) SNR, called G189.6+3.3.
Notably, IC 443 X-ray morphology is centrally peaked and a very soft X-ray shell is barely visible. Unlike plerion remnants, e.g. the Crab Nebula, the inner X-ray emission is not dominated by the central pulsar wind nebula. It has indeed a thermal origin. IC 443 shows very similar features to the class of mixed morphology SNRs. Both optical and X-ray emission are heavily absorbed by a giant molecular cloud in the foreground, crossing the whole remnant body from northwest to southeast.
The remnant's age is still uncertain. There is some agreement that the progenitor supernova happened between 3,000 and 30,000 years ago. Recent Chandra and XMM-Newton observations identified a plerion nebula, close to the remnant southern rim. The point source near the apex of the nebula is a neutron star, relic of a SN explosion. The location in a star forming region and the presence of a neutron star favor a Type II supernova, the ultimate fate of a massive star, as the progenitor explosion.
The SNR IC 443 is located in the galactic anticenter direction (l=189.1°), close to the galactic plane (b=+3.0°). Many objects lie in the same region of sky: the HII region S249, several young stars (members of the GEM OB1 association), and an older SNR (G189.6+3.3).
The remnant is evolving in a rich and complex environment, which strongly affects its morphology. Multi-wavelength observations show the presence of sharp density gradients and different cloud geometries in the surroundings of IC 443. Massive stars are known to be short lived (roughly 30 million years), ending their life when they are still embedded within the progenitor cloud. The more massive stars (O-type) probably clear the circum-stellar environment by powerful stellar winds or photoionizing radiation. Early B-type stars, with a typical mass between 8 and 12 solar masses, are not capable of this, and they likely interact with the primordial molecular cloud when they explode. Thus, it is not surprising that the SNR IC 443, which is thought to be the aftermath of a stellar explosion, evolved in such a complex environment. For instance, an appreciable fraction of supernova remnants lies close to dense molecular clouds (~50 out of 265 in the Green catalogue), and most of them (~60%) show clear signs of interaction with the adjacent cloud.
X-ray and the optical images are characterized by a dark lane, crossing IC 443 from northwest to southeast. Emission from quiescent molecular gas has been observed toward the same direction,[9] and it is likely due to a giant molecular cloud, located between the remnant and the observer. This is the main source of extinction of the low energy SNR emission.
In the southeast the blast wave is interacting with a very dense (~10,000 cm−3) and clumpy molecular cloud, such that the emitting shocked gas has a ring-like shape. The blast wave has been strongly decelerated by the cloud and is moving with an estimated velocity of roughly 30–40 km s−1. OH (1720 MHz) maser emission, which is a robust tracer of interaction between SNRs and dense molecular clouds, has been detected in this region.[11] A source of gamma-ray radiation is spatially coincident with IC 443 and the maser emission region, though is not well understood whether it is physically associated with the remnant or not.
In the northeast, where the brightest optical filaments are located, the SNR is interacting with a very different environment. The forward shock has encountered a wall of neutral hydrogen (HI), and is propagating into a less dense medium (~10-1,000 cm−3) with a much higher velocity (80–100 km s−1) than in the southern ridge.
In the western region, the shock wave breaks out into a more homogeneous and rarefied medium.
Graham construction is sponsoring Canada's TRTL - many thanks for the invaluable support and guidance!
9 & 10 Mar 2026; Spotsylvania, Virginia USA. Bortle 4.5 zone.
WO Redcat51 telescope, ZWO AM5 mount and ASI533MM Pro camera, autoguiding and dither 10px, no calibration frames, Baader broadband and ZWO Hα filters (exp 180s, gain 100, bin 1, ~55 subframes each), sensor -10°C, autofocus. Data acquired in ASIAir and processed in Pixinsight. Image scale: 3"/pixel (at Dawes Limit), then drizzled 2x.
Clouds: partly cloudy
Transparency (AL): 6
Seeing (AL): F
Moon: illuminated xx%, age xx days
Apparent magnitude 6.9
Apparent size 27x14 arcmin
Appearance: Bode's Galaxy (M81) is at center; peculiar elliptical galaxy NGC 3077 is at 7:00; and Messier 82 is at 11:00.
from Wikipedia
Messier 81 (also known as NGC 3031 or Bode's Galaxy) is a grand design spiral galaxy about 12 Mly away in the constellation Ursa Major. It has a D25 isophotal diameter of 29.44 kpc (96,000 ly). Because of its relative proximity to the Milky Way galaxy, large size, and active galactic nucleus (which harbors a 70 million M☉ supermassive black hole), Messier 81 has been studied extensively by professional astronomers. The galaxy's large size and relatively high brightness also makes it a popular target for amateur astronomers. In late February 2022, astronomers reported that M81 may be the source of FRB 20200120E, a repeating fast radio burst.
Messier 81 was first discovered by Johann Elert Bode on 31 December 1774. Thus, it is sometimes referred to as "Bode's Galaxy". In 1779, Pierre Méchain and Charles Messier reidentified Bode's object, hence listed it in the Messier Catalogue.
The galaxy is to be found approximately 10° northwest of Alpha Ursae Majoris (Dubhe) along with several other galaxies in the Messier 81 Group. Its apparent magnitude due to its distance means it requires a good night sky and only rises very briefly and extremely low at its southernmost limit from Earth's surface, about the 20th parallel south.
Messier 81 and Messier 82 are considered ideal for viewing using binoculars and small telescopes. The two objects are generally not observable to the unaided eye, although highly experienced amateur astronomers may be able to see Messier 81 under exceptional observing conditions with a very dark sky. Telescopes with apertures of 8 inches (20 cm) or larger are needed to distinguish structures in the galaxy.
Most of the emission at infrared wavelengths originates from interstellar dust. This interstellar dust is found primarily within the galaxy's spiral arms, and it has been shown to be associated with star formation regions. The general explanation is that the hot, short-lived blue stars that are found within star formation regions are very effective at heating the dust and thus enhancing the infrared dust emission from these regions.
It is estimated M81 has 210 ± 30 globular clusters.
Only one supernova has been detected in Messier 81. The supernova, named SN 1993J, was discovered on 28 March 1993 by F. GarcÃa in Spain. At the time, it was the second brightest Type II supernova observed in the 20th century, peaking at an apparent magnitude of 10.7. The spectral characteristics of the supernova changed over time. Initially, it looked more like a Type II supernova (a supernova formed by the explosion of a supergiant star) with strong hydrogen spectral line emission, but later the hydrogen lines faded and strong helium spectral lines appeared, making the supernova look more like a Type Ib.
Moreover, the variations in SN 1993J's luminosity over time were not like the variations observed in other Type II supernovae, but did resemble the variations observed in Type Ib supernovae. Hence, the supernova has been classified as a Type IIb, a transitory class between Type II and Type Ib. The scientific results from this supernova suggested that Type Ib and Ic supernovae were formed through the explosions of giant stars through processes similar to those taking place in Type II supernovae. Despite the uncertainties in modeling the unusual supernova, it was also used to estimate a very approximate distance of 8.5 ± 1.3 Mly (2.6 ± 0.4 Mpc) to Messier 81. As a local galaxy, the Central Bureau for Astronomical Telegrams (CBAT) tracks novae in M81 along with M31 and M33.
In the center of M81 there exists a supermassive black hole (SMBH) with a mass of about 7×10^7 M☉. The SMBH is active, having an accretion disk and one-sided relativistic jet. The observation also demonstrate that there may exist a second SMBH that orbits the primary SMBH with a period of around 30 years. The mass of the secondary SMBH is estimated at 0.1 of the primary.
Messier 81 is the largest galaxy in the M81 Group, a group of 34 in the constellation Ursa Major. At approximately 11.7 Mly (3.6 Mpc) from the Earth, it makes this group and the Local Group, containing the Milky Way, relative neighbors in the Virgo Supercluster.
Gravitational interactions of M81 with M82 and NGC 3077 have stripped hydrogen gas away from all three galaxies, forming gaseous filamentary structures in the group. Moreover, these interactions have allowed interstellar gas to fall into the centers of M82 and NGC 3077, leading to vigorous star formation or starburst activity there.
The distance to Messier 81 has been measured by Freedman et al to be 3.63 ± 0.34 Mpc (11.8 ± 1.1 Mly) by using the Hubble Space Telescope to identify classical Cepheid variables and measure their periods using the period-luminosity relation discovered by Henrietta Swan Leavitt.
the old shitty ones were a pain in the ass to get out until I figured out that they are one solid piece. Took a new razor-blade to them, hacked them in half an d they fell out. Then the new ones were of course a pain in the ass to put in there. Once I got them in, shifting is so much better. Nice and stiff.
Detroit Speed is proud to announce shipping out their 1,000th Hydroformed Subframe! The proud new owners are Bill and Billy Utley of B&B Classics Inc. We would like to thank everyone who works at Detroit Speed and more importantly all of our customers who helped make this happen! Here's to 1,000 more! #1000subframe #MadeintheUSA #DetroitSpeed