View allAll Photos Tagged Subframing
Finally got round to replacing the rear springs, as I found this was quite challenging due to the design of the rear subframe on the S80.
Without a Youtube video and a certain spring compressor, it would be impossible to complete this task.
The ride has transformed, the rear is much tighter and also a bit lower (what I wanted). Happy days!
SKU / Type 956917
EAN 4251244608477
My wife's daily driver of seven years was recently diagnosed with a rusted subframe. It was a repair that we could have afforded, but at almost fifteen years old--and also having spent almost all of that time (we presume) in the midwest--the entire car is slowly turning to rust and it is not worth our time to get it repaired.
We had decided that we would try and sell the car on Craigslist, so we spent some time cleaning the car and getting it ready. Today was going to be the final push, getting it washed and taking photos of it and making up a listing. We washed the car at home, then decided to take it to Marathon to vacuum it out before finding a parking lot to take photos in. Even from the house to the gas station, the car was acting incredibly janky, and by the time we got it to our chosen parking lot and started taking photos of it, it wasn't long before we gave up--and decided to junk the car.
We drove it home and called Victory Auto Wreckers, who will be coming to tow it away tomorrow. Here are some photos of the beloved Cavalier for posterity's sake.
Captured 26 Nov 2021, 21:39 hrs ET, Springfield, VA, USA. Bortle 7 skies, Stellarvue SV80/9D doublet achromat refractor at f/5.68 (eff. fl 454mm), Orion Atlas AZ/EQ-G Pro mount. Mallincam DS10C camera, bin 1, exposure 120 seconds, gain 20, live stack of 20 subframes, dark and flat frames subtracted. Optolong LeNhance filter, UV/IR cut filter. Reprocessed in Siril and Photoshop on 14 June 2023.
Clouds: partly cloudy
Seeing: good
Transparency: good
Moon phase: 67%
FOV: 2.16 x 1.62 degrees before cropping.
Resolution: 2.1 arcsec/pixel.
Orientation: Up is Southwest.
Appearance: Dim nebulosity, adjacent bright star Gamma Cassiopeia. IC 59 is at 7 o'clock and IC 63 is at 10 o'clock.
From Stellarium:
IC 59 (a.k.a. Gamma Cas Nebula, LBN 620) is a reflection nebula. Magnitude +13.3, size 10 x 5 arcmin.
IC 63 (a.k.a. Ghost of Cassiopeia, LBN 622) is an HII region excited by Gamma Cas. Magnitude +13.3, size 10 x 3 arcmin.
From Wikipedia:
Gamma Cassiopeiae, Latinized from γ Cassiopeiae, is a star at the center of the distinctive "W" asterism in the northern circumpolar constellation of Cassiopeia. Although it is a fairly bright star with an apparent visual magnitude that varies from 1.6 to 3.0, it has no traditional Arabic or Latin name. It sometimes goes by the informal name Navi.
Gamma Cassiopeiae is a Be star, a variable star, and a binary star system. Based upon parallax measurements made by the Hipparcos satellite, it is located at a distance of roughly 550 light-years from Earth.
Gamma Cassiopeiae is an eruptive variable star, whose apparent magnitude changes irregularly between +1.6 and +3.0. It is the prototype of the class of Gamma Cassiopeiae variable stars. In the late 1930s it underwent what is described as a shell episode and the brightness increased to above magnitude +2.0, then dropped rapidly to +3.4. It has since been gradually brightening back to around +2.2. At maximum intensity, γ Cassiopeiae outshines both α Cassiopeiae (magnitude +2.25) and β Cassiopeiae (magnitude +2.3).
Gamma Cassiopeiae is a rapidly spinning star with a projected rotational velocity of 472 km s−1, giving it a pronounced equatorial bulge. When combined with the star's high luminosity, the result is the ejection of matter that forms a hot circumstellar disk of gas. The emissions and brightness variations are apparently caused by this "decretion disk".
The spectrum of this massive star matches a stellar classification of B0.5 IVe. A luminosity class of IV identifies it as a subgiant star that has reached a stage of its evolution where it is exhausting the supply of hydrogen in its core region and transforming into a giant star. The 'e' suffix is used for stars that show emission lines of hydrogen in the spectrum, caused in this case by the circumstellar disk. This places it among a category known as Be stars; in fact, the first such star ever to be so designated. It has 17 times the Sun's mass and is radiating as much energy as 34,000 Suns. At this rate of emission, the star has reached the end of its life as a late O-type main sequence star after a relatively brief 8 million years. The outer atmosphere has an intense effective temperature of 25,000 K, which is causing it to glow with a blue-white hue.
Gamma Cassiopeiae is the prototype of a small group of stellar sources of X-ray radiation that is about 10 times stronger than emitted from other B or Be stars. The character of the X-ray spectrum is Be thermal, possibly emitted from plasmas of temperatures up to least ten million kelvins, and shows very short term and long-term cycles. Historically, it has been held that these X-rays might be excited by matter originating from the star, from a hot wind or a disk around the star, accreting onto the surface of a degenerate companion, such as a white dwarf or neutron star. However, there are difficulties with either of these hypotheses. For example, it is not clear that enough matter can be accreted by a white dwarf, at the distance of the purported secondary star implied by the orbital period, sufficient to power an X-ray emission of nearly 1033 erg/s or 100 YW. A neutron star could easily power this X-ray flux, but X-ray emission from neutron stars is known to be non-thermal, and thus in apparent variance with the spectral properties.
Evidence suggests that the X-rays may be associated with the Be star itself or caused by some complex interaction between the star and surrounding decretion disk. One line of evidence is that the X-ray production is known to vary on both short and long time scales with respect to various UV line and continuum changes associated with a B star or with circumstellar matter close to the star. Moreover, the X-ray emissions exhibit long-term cycles that correlate with the light curves in the visible wavelengths.
Gamma Cassiopeiae exhibits characteristics consistent with a strong disordered magnetic field. No field can be measured directly from the Zeeman effect because of the star's rotation-broadened spectral lines. Instead, the presence of this field is inferred from a robust periodic signal of 1.21 days that suggests a magnetic field rooted on the rotating star's surface. The star's UV and optical spectral lines show ripples moving from blue to red over several hours, which indicates clouds of matter being held frozen over the star's surface by strong magnetic fields. This evidence suggests that a magnetic field from the star is interacting with the decretion disk, resulting in the X-ray emission. A disk dynamo has been advanced as a mechanism to explain this modulation of the X-rays. However, difficulties remain with this mechanism, among which is that there are no disk dynamos known to exist in other stars, rendering this behavior more difficult to analyze.
Gamma Cassiopeiae has two faint optical companions, listed in double star catalogues as components B and C. Star B is about 2 arc seconds distant and magnitude 11, and has a similar space velocity to the bright primary. Component C is magnitude 13, nearly an arc second distant.
Gamma Cassiopeiae A, the bright primary, is itself a spectroscopic binary with an orbital period of about 203.5 days and an eccentricity alternately reported as 0.26 and "near zero." The mass of the companion is believed to be about that of the Sun, but its nature is unclear. It has been proposed that it is a degenerate star or a hot helium star, but it seems unlikely that it is a normal star. Therefore, it is likely to be more evolved than the primary and to have transferred mass to it during an earlier stage of evolution.
The Chinese name Tsih, "the whip" (Chinese: ç–; pinyin: cè), is commonly associated with this star. The name however originally referred to Kappa Cassiopeiae, and Gamma Cassiopeiae was just one of four horses pulling the chariot of legendary charioteer Wangliang. This representation was later changed to make Gamma the whip.
The star was used as an easily identifiable navigational reference point during space missions and American astronaut Virgil Ivan "Gus" Grissom nicknamed the star Navi after his own middle name spelled backwards.
Kosmo Foto Mono pushed to ISO400 - Nikon F3 - 100mm Series E f2.8
Home developed w/ Rodinal, home scanned.
Now that I own an intervalometer, it's much easier to take lots of subframes over a long period of time (in fact, now I can do it while I'm on the couch watching TV). So I figured I would try "going deep" and see if I could image some galaxies - and why not, with Leo and Virgo high overhead this time of year?
I constructed this image over a period of several nights, as I'm a bit new to this type of astrophotography, and it took me some time to get proper flat and bias frames and get them all blended properly. I don't know who the first guy was to figure out the whys and hows of stacking, dark frames, flat frames, and bias frames, but he must've been a pretty smart guy. If you do this right, then camera-induced noise and artefacts are drastically reduced. One of the goals I had in making this image (besides making a nice image) was to see if it's actually possible to image dim objects like this with an Alt/Az mount (i.e., my Nexstar 8). It was very pleasing to know that it's possible - this really opens up the sky for me and my less-than-optimal equipment.
So here's the result... this image shows M65 & M66 in Leo. M65 (right) is a type Sa spiral galaxy, and as can be seen in this image, has a prominent dust lane and is close to being edge-on. M66 (left) is a type Sb spiral, and as can be seen here, has a prominent central bar, widely separated arms, and many clumps of dust. Both of these galaxies are about 36 million ly away.
I find it incredible that these "island universes", containing billions of stars, are so small and dim that it's a challenge to see and image them. No doubt there are guys up there trying to do the same thing with the Milky Way right now.
26x120 second subframes, total integration 52 minutes.
Imaging:
Skywatcher Evostar 150,
QHY163C with Astronomik CLS filter.
Guiding:
190mm focal length finder-guider,
Orion SSAG.
All on
Skywatcher HEQ5 Pro
Captured using SharpCap. Guided with PHD2.
Stacked and processed in DSS, Fitswork and Gimp. 2x drizzle applied.
20th July 2017
Cambridge, UK
"Fitting the cab, grille and wiring to the subframe"
This issue is an important stage in the assembly process as the cab is fitted to the subframe. The first part of the lower deck flooring is also supplied.
Although the front part of the lower deck floor was supplied with this issue, it is not yet fitted to the bus. This overhead view shows it in place, but not screwed down. The 30cm ruler gives an idea of size!
Test assembly of the major components of the rear subframe. The rear suspension and wheels will be bolted to this. The hole is for the rocket.
"It's just a truck" my wife tells me...
It was covered in yellow pine pollen, as all things in NC are about now. I despecked and 'canvas' textured it in Photoshop to hide that fact.
1955 Chevy 1st series 3100, Camaro subframe and 350/350 driveline.
Super Sharp Truck. For sale @ $8500 OBO. You contact me, but it's not mine.
Trivia question!
What's the difference between a '55 First Series and a '55 Second Series?
APEX 17x8.5" ET20 ARC-8 Wheels (4x100)
GC coilovers and camber is adjusted out on rear using adjustable subframe
Finally got round to replacing the rear springs, as I found this was quite challenging due to the design of the rear subframe on the S80.
Without a Youtube video and a certain spring compressor, it would be impossible to complete this task.
The ride has transformed, the rear is much tighter and also a bit lower (what I wanted). Happy days!
SKU / Type 956917
EAN 4251244608477
Test assembly of the major components of the rear subframe. The rear suspension and wheels will be bolted to this. The hole is for the rocket.
Bought a upgrade for the subframe. The polyurethane bushings are inserted into the rubber subframe bushings, which tightens them up and limit the movement in them.
Brand: Parts4Swedes
Partnr: 61430104PU
n 2191. 3 May 1999.
Shaftesbury & District's extended BEA Routemaster RMA-type, when reconstruction to the lengthened RME1 was well advanced. The rear subframe had been removed so that a cracked rear axle casing could be sent off for repair. Seen at the Shaftesbury yard in company with ex-London Transport Bristol LH/ECW saloons.
My wife's daily driver of seven years was recently diagnosed with a rusted subframe. It was a repair that we could have afforded, but at almost fifteen years old--and also having spent almost all of that time (we presume) in the midwest--the entire car is slowly turning to rust and it is not worth our time to get it repaired.
We had decided that we would try and sell the car on Craigslist, so we spent some time cleaning the car and getting it ready. Today was going to be the final push, getting it washed and taking photos of it and making up a listing. We washed the car at home, then decided to take it to Marathon to vacuum it out before finding a parking lot to take photos in. Even from the house to the gas station, the car was acting incredibly janky, and by the time we got it to our chosen parking lot and started taking photos of it, it wasn't long before we gave up--and decided to junk the car.
We drove it home and called Victory Auto Wreckers, who will be coming to tow it away tomorrow. Here are some photos of the beloved Cavalier for posterity's sake.
Test assembly of the major components of the rear subframe. The rear suspension and wheels will be bolted to this. The hole is for the rocket.
Owners of the BMW 3 Series (E46 models) have been reporting cracks and damage in the rear subframe area of their vehicles. The issue was also common on the earlier 3 Series models and unfortunately, have reoccurred with the E46 from 1999-2006. This issue specifically appears in the rear mounting points of the subframe, which can tear out from their position in the sheet metal. This occurs as the rear differential transmits the torsional load from the engine through the subframe, and then, into the chassis of the vehicle. This constant abuse leads to fatigue in the metal, causing cracks and separation from the chassis.
The parts used for this repair includes:
Active Autowerke (www.activeautowerke.com):
• E46 Subframe / Rear Chassis Reinforcement Kit
Powerflex USA (powerflexusa.com):
• BMW E46 M3 Rear Subframe Front Bushing - Street
• BMW E46 M3 Rear Subframe Rear Bushing - Street
• BMW E46 M3 Rear Diff Rear Mount - Street
• BMW E46 M3 Rear Diff Front Mount - Street
29 May 2022, ~11pm ET, Springfield Virginia USA. Orion Atlas AZ/EQ-G Pro mount. QHY 294M Pro camera @ -10C, bin 2x2, exposure 30 seconds, gain 2600, 11MP mode, stack of 40 subframes, no calibration frames. Baader Luminance filter. Reprocessed in Siril and PS on 25 May 2023.
Clouds: partly cloudy
Seeing: avg
Transparency: avg
Moon phase: 1%
FOV: 31 x 29 arcmin.
Resolution: 0.9 arcsec/pixel.
Appearance: Loosely wound face-on spiral galaxy, pinwheel shape.
From Wikipedia:
The Pinwheel Galaxy (also known as Messier 101, M101 or NGC 5457) is a face-on spiral galaxy 21 million light-years (6.4 megaparsecs) away from Earth in the constellation Ursa Major. It was discovered by Pierre Méchain in 1781 and was communicated that year to Charles Messier, who verified its position for inclusion in the Messier Catalogue as one of its final entries.
On February 28, 2006, NASA and the European Space Agency released a very detailed image of the Pinwheel Galaxy, which was the largest and most-detailed image of a galaxy by Hubble Space Telescope at the time. The image was composed of 51 individual exposures, plus some extra ground-based photos.
On August 24, 2011, a Type Ia supernova, SN 2011fe, was discovered in M101.
Pierre Méchain, the discoverer of the galaxy, described it as a "nebula without star, very obscure and pretty large, 6' to 7' in diameter, between the left hand of Bootes and the tail of the great Bear. It is difficult to distinguish when one lits the [grating] wires."
William Herschel wrote in 1784 that the galaxy was one of several which "...in my 7-, 10-, and 20-feet [focal length] reflectors shewed a mottled kind of nebulosity, which I shall call resolvable; so that I expect my present telescope will, perhaps, render the stars visible of which I suppose them to be composed."
Lord Rosse observed the galaxy in his 72-inch-diameter Newtonian reflector during the second half of the 19th century. He was the first to make extensive note of the spiral structure and made several sketches.
To observe the spiral structure in modern instruments requires a fairly large instrument, very dark skies, and a low-power eyepiece.
M101 is a large galaxy, with a diameter of 170,000 light-years. By comparison, the Milky Way has a diameter of between 100,000 and 120,000 light-years. It has around a trillion stars. It has a disk mass on the order of 100 billion solar masses, along with a small central bulge of about 3 billion solar masses. Its characteristics can be compared to those of Andromeda Galaxy.
M101 has a high population of H II regions, many of which are very large and bright. H II regions usually accompany the enormous clouds of high density molecular hydrogen gas contracting under their own gravitational force where stars form. H II regions are ionized by large numbers of extremely bright and hot young stars; those in M101 are capable of creating hot superbubbles. In a 1990 study, 1,264 H II regions were cataloged in the galaxy. Three are prominent enough to receive New General Catalogue numbers—NGC 5461, NGC 5462, and NGC 5471.
M101 is asymmetrical due to the tidal forces from interactions with its companion galaxies. These gravitational interactions compress interstellar hydrogen gas, which then triggers strong star formation activity in M101's spiral arms that can be detected in ultraviolet images.
In 2001, the X-ray source P98, located in M101, was identified as an ultra-luminous X-ray source—a source more powerful than any single star but less powerful than a whole galaxy—using the Chandra X-ray Observatory. It received the designation M101 ULX-1. In 2005, Hubble and XMM-Newton observations showed the presence of an optical counterpart, strongly indicating that M101 ULX-1 is an X-ray binary. Further observations showed that the system deviated from expected models—the black hole is just 20 to 30 solar masses, and consumes material (including captured stellar wind) at a higher rate than theory suggests.
It is estimated that M101 has about 150 globular clusters, the same as the number of the Milky Way's globular clusters.
M101 has six prominent companion galaxies: NGC 5204, NGC 5474, NGC 5477, NGC 5585, UGC 8837 and UGC 9405. As stated above, the gravitational interaction between it and its satellites may have spawned its grand design pattern. The galaxy has probably distorted the second-listed companion.
Four internal supernovae have been recorded:
SN 1909A, was discovered by Max Wolf in January 1909 and reached magnitude 12.1. SN 1951H reached magnitude 17.5 in September 1951. SN 1970G reached magnitude 11.5 in January 1970. On August 24, 2011, a Type Ia supernova, SN 2011fe, initially designated PTF 11kly, was discovered in M101. It had visual magnitude 17.2 at discovery and reached 9.9 at its peak.
On February 10, 2015, a luminous red nova, known as M101 OT2015-1 was discovered in the Pinwheel Galaxy.
Image from stacking
36x300s 3h
-Pre Processing-
Image Calibration
Cosmetic Correction
Debayer
Subframe Selector
Star Alignement
Local Normalization
Drizzle x2
Crop the black bands from the stacking
Owners of the BMW 3 Series (E46 models) have been reporting cracks and damage in the rear subframe area of their vehicles. The issue was also common on the earlier 3 Series models and unfortunately, have reoccurred with the E46 from 1999-2006. This issue specifically appears in the rear mounting points of the subframe, which can tear out from their position in the sheet metal. This occurs as the rear differential transmits the torsional load from the engine through the subframe, and then, into the chassis of the vehicle. This constant abuse leads to fatigue in the metal, causing cracks and separation from the chassis.
The parts used for this repair includes:
Active Autowerke (www.activeautowerke.com):
• E46 Subframe / Rear Chassis Reinforcement Kit
Powerflex USA (powerflexusa.com):
• BMW E46 M3 Rear Subframe Front Bushing - Street
• BMW E46 M3 Rear Subframe Rear Bushing - Street
• BMW E46 M3 Rear Diff Rear Mount - Street
• BMW E46 M3 Rear Diff Front Mount - Street
Fitted with a subframe for underfloor tipping gear.
Note the 22RB excavator in for repair in the background.
This factory is now the site of the new Oundle Waitrose.