View allAll Photos Tagged Subframing
VRP (Verona Racing Parts)
Rear subframe-airbox combo for Honda CR 1989/90
Much bigger airbox than stock
VRP (Verona Racing Parts)
Rear subframe-airbox combo for Honda CR 1989/90
Much bigger airbox than stock
Mamiya C330f // Ilford XP2 Super 400
Thanks to the shithead developers who originally fought against the effort to landmark this building (and lost): Chicago's former Lake Street Schlitz Tied House - later La Luce - was left unsecured for months and suffered extensive damage from vandals and thieves who tore away much of its architectural copper cladding. Only after the decay made the news was the graffiti buffed, and now-exposed wood subframe crudely covered in white plastic. Despite its protected status, it still remains vacant with an uncertain future.
1393-1399 W. Lake Street
VRP (Verona Racing Parts)
Rear subframe-airbox combo for Honda CR 1989/90
Much bigger airbox than stock
BLOODHOUND build: Work continues on the test assembly of the front subframe - to which the front wheels will be attached.
Detroit Speed 1966 Fastback Mustang Test Car with a Boss 302 Roush Yates engine and DSE Aluma-Frame front suspension and the QUADRALinkâ„¢ rear suspension. This is the official "Test Car" for Detroit Speed's line of Mustang products for the 1964.5-1970 Mustangs. It is equipped with the DSE Aluma-Frame front suspension, subframe connectors, deep tubs as well as the Mustang QUADRALinkâ„¢ rear suspension. detroitspeed.com/Projects/DSE-1966-Mustang/DSE-1966-Musta...
I decided to modify my FJ Cruiser for a car camping setup for this summer / Fall. Built this using 2x2's, 3/4" plywood, screws, bolts, carpet padding, and carpet. Took me about a day and a half to lay it all out and build. Removed the factory rear seat and used the same hardware holes to secure the frame. The two piece carpeted panels fit nice and snug so no need to secure them to the frame at this time. With this sleeping platform installed I still have room to lay the seats all the way back with the seats slid all the way to the rear. I also have room to store a full gym bag of gear and my LowePro Computreker underneath the forward section.
Ken's Alpine White BMW E92 M3
APEX Wheels VS-5RS in Anthracite
18x10" ET25 on 275/35-18 Nitto NT01
12mm Rear Spacer for aesthetic purposes
Suspension/Brake Mods:
JRZ RS One dampers
-3.5 F, -2.0 R camber
SPL Suspension Links
Powerflex Purple Bushings
Bimmerworld Solid Rear Subframe Mounts
Vibra-technics Engine Mounts
Rotora 6 piston/380mm & 4 piston/355mm BBK with Project Mu 999 pads
Finished restauration of my 1990 Racebike
1990 VRP aluminium chassis,swingarm,subframe,fuel tank
1990 Mugen engine
MRP custom exhaust pipe
Poletti suspension
Ken's Alpine White BMW E92 M3
APEX Wheels VS-5RS in Anthracite
18x10" ET25 on 275/35-18 Nitto NT01
12mm Rear Spacer for aesthetic purposes
Suspension/Brake Mods:
JRZ RS One dampers
-3.5 F, -2.0 R camber
SPL Suspension Links
Powerflex Purple Bushings
Bimmerworld Solid Rear Subframe Mounts
Vibra-technics Engine Mounts
Rotora 6 piston/380mm & 4 piston/355mm BBK with Project Mu 999 pads
Finished restauration of my 1990 Racebike
1990 VRP aluminium chassis,swingarm,subframe,fuel tank
1990 Mugen engine
Poletti suspension
We are working on a new carbon fiber subframe for our moto2 bike, the BOTT M210.
With this design we will reduce weight and will improve aesthetics, aerodynamics, and ergonomy.
CAD design has been done by Jordi Massague.
The latest comet was finally visible in the constellation of Serpens after a week or more of solid cloud at sunset. This is a stack of about 180 1s subframes taken with a Nikon D750 and a135mm f/2 lens, set to f/2.5. ISO2000.
Canon EOS450d, modded
24mm lens @ f/5.6
43 subframes, each 180s
125 bias frames
100 darkframes
unguided EQ5 mount
Location: Gran Canaria, near San Bartolome de Tirajanas
pic shows the fine dust streams in this region of the milky way.
Swiss 125cc championships in Niederwil / CH
1989 VRP Mugen Honda
Custom VRP aluminium chassis,airbox/subframe,gas tank
Wheels: Race Silver EC-7
Front: 18x8.5 ET45
Rrear: 18x8.5 ET35
Additional notes:
E9X M3 subframe conversion including rear hubs (effective offset change)
Captured 28 April 2022, ~21:30 hrs ET, Springfield, VA, USA. Bortle 8 skies, Celestron 8 inch SCT at f/6.3 (eff. fl 1290mm), Orion Atlas AZ/EQ-G Pro mount. QHY 294M Pro camera @ -10C, bin 2, exposure 7.5 seconds, gain 3100, stack of 41 subframes, no calibration frames used. Baader Luminance filter.
Clouds: partly cloudy
Seeing: avg
Transparency: avg
Moon phase: ~5%
FOV: 15 x 13 arcmin.
Resolution: 0.45 arcsec/pixel.
Orientation: Up is North.
Appearance: Supernova outshines its host galaxy NGC 4647. Magnitude is approximately +11-12.
From Wikipedia:
A supernova is a powerful and luminous stellar explosion. This transient astronomical event occurs during the last evolutionary stages of a massive star or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.
Supernovae are more energetic than novae. In Latin, nova means "new", referring astronomically to what appears to be a temporary new bright star. Adding the prefix "super-" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1929.
The most recent directly observed supernova in the Milky Way was Kepler's Supernova in 1604, but the remnants of more recent supernovae have been found. Observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. These supernovae would almost certainly be observable with modern astronomical telescopes. The most recent naked-eye supernova was SN 1987A, the explosion of a blue supergiant star in the Large Magellanic Cloud, a satellite of the Milky Way.
Theoretical studies indicate that most supernovae are triggered by one of two basic mechanisms: the sudden re-ignition of nuclear fusion in a degenerate star such as a white dwarf, or the sudden gravitational collapse of a massive star's core. In the first class of events, the object's temperature is raised enough to trigger runaway nuclear fusion, completely disrupting the star. Possible causes are an accumulation of material from a binary companion through accretion, or a stellar merger. In the massive star case, the core of a massive star may undergo sudden collapse due to reduced energy from fusion rendering the star incapable of counteracting its own gravity, usually occurring after the fusion of iron in a star’s core, releasing gravitational potential energy as a supernova. While some observed supernovae are more complex than these two simplified theories, the astrophysical mechanics are established and accepted by the astronomical community.
Supernovae can expel several solar masses of material at speeds up to several percent of the speed of light. This drives an expanding shock wave into the surrounding interstellar medium, sweeping up an expanding shell of gas and dust observed as a supernova remnant. Supernovae are a major source of elements in the interstellar medium from oxygen to rubidium. The expanding shock waves of supernovae can trigger the formation of new stars. Supernova remnants might be a major source of cosmic rays. Supernovae might produce gravitational waves, though thus far, gravitational waves have been detected only from the mergers of black holes and neutron stars.
The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova. A 1414 text cites a 1055 report: since "the baleful star appeared, a full year has passed and until now its brilliance has not faded."
Compared to a star's entire history, the visual appearance of a supernova is very brief, sometimes spanning several months, so that the chances of observing one with the naked eye is roughly once in a lifetime. Only a tiny fraction of the 100 billion stars in a typical galaxy have the capacity to become a supernova, restricted to either those having large mass or rare kinds of binary stars containing white dwarfs.
The earliest possible recorded supernova, known as HB9, could have been viewed and recorded by unknown prehistoric people of Indian subcontinent, on a rock carving found in Burzahama region in Kashmir, dated to 4500 ± 1000 BC. Later, SN 185 was viewed by Chinese astronomers in 185 AD. The brightest recorded supernova was SN 1006, which occurred in 1006 AD in the constellation of Lupus, and was described by observers across China, Japan, Iraq, Egypt, and Europe. The widely observed supernova SN 1054 produced the Crab Nebula. Supernovae SN 1572 and SN 1604, the latest to be observed with the naked eye in the Milky Way galaxy, had notable effects on the development of astronomy in Europe because they were used to argue against the Aristotelian idea that the universe beyond the Moon and planets was static and unchanging. Johannes Kepler began observing SN 1604 at its peak on October 17, 1604, and continued to make estimates of its brightness until it faded from naked eye view a year later. It was the second supernova to be observed in a generation (after SN 1572 seen by Tycho Brahe in Cassiopeia).
There is some evidence that the youngest galactic supernova, G1.9+0.3, occurred in the late 19th century, considerably more recently than Cassiopeia A from around 1680. Neither supernova was noted at the time. In the case of G1.9+0.3, high extinction along the plane of our galaxy could have dimmed the event sufficiently to go unnoticed. The situation for Cassiopeia A is less clear. Infrared light echos have been detected showing that it was a type IIb supernova and was not in a region of especially high extinction.
Observation and discovery of extragalactic supernovae are now far more common. The first such observation was of SN 1885A in the Andromeda Galaxy. Today, amateur and professional astronomers are finding several hundred every year, some when near maximum brightness, others on old astronomical photographs or plates. American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941. During the 1960s, astronomers found that the maximum intensities of supernovae could be used as standard candles, hence indicators of astronomical distances. Some of the most distant supernovae observed in 2003 appeared dimmer than expected. This supports the view that the expansion of the universe is accelerating. Techniques were developed for reconstructing supernovae events that have no written records of being observed. The date of the Cassiopeia A supernova event was determined from light echoes off nebulae, while the age of supernova remnant RX J0852.0-4622 was estimated from temperature measurements and the gamma ray emissions from the radioactive decay of titanium-44.
The most luminous supernova ever recorded is ASASSN-15lh, at a distance of 3.82 gigalight-years. It was first detected in June 2015 and peaked at 570 billion L☉, which is twice the bolometric luminosity of any other known supernova. However, the nature of this supernova continues to be debated and several alternative explanations have been suggested, e.g. tidal disruption of a star by a black hole.
Among the earliest detected since time of detonation, and for which the earliest spectra have been obtained (beginning at 6 hours after the actual explosion), is the type II SN 2013fs (iPTF13dqy) which was recorded 3 hours after the supernova event on 6 October 2013 by the Intermediate Palomar Transient Factory (iPTF). The star is located in a spiral galaxy named NGC 7610, 160 million light-years away in the constellation of Pegasus.
On 20 September 2016, amateur astronomer Victor Buso from Rosario, Argentina was testing his telescope. When taking several photographs of galaxy NGC 613, Buso chanced upon a supernova that had just become visible on Earth, as it began to erupt. After examining the images, he contacted the Instituto de AstrofÃsica de La Plata. "It was the first time anyone had ever captured the initial moments of the 'shock breakout' from an optical supernova, one not associated with a gamma-ray or X-ray burst." The odds of capturing such an event were put between one in ten million to one in a hundred million, according to astronomer Melina Bersten from the Instituto de AstrofÃsica. The supernova Buso observed was designated SN 2016gkg, a type IIb supernova likely to have formed from the collapse of a yellow supergiant star twenty times the mass of the sun. It showed the double peak that is common to many type IIb supernovae, rising to around magnitude 15.5 shortly after discovery and then again about 20 days later. The progenitor star has been identified in Hubble Space Telescope images from before its collapse. Astronomer Alex Filippenko, from the University of California, remarked that professional astronomers had been searching for such an event for a long time. He stated: "Observations of stars in the first moments they begin exploding provide information that cannot be directly obtained in any other way."
Early work on what was originally believed to be simply a new category of novae was performed during the 1920s. These were variously called "upper-class Novae", "Hauptnovae", or "giant novae". The name "supernovae" is thought to have been coined by Walter Baade and Fritz Zwicky in lectures at Caltech during 1931. It was used, as "super-Novae", in a journal paper published by Knut Lundmark in 1933, and in a 1934 paper by Baade and Zwicky. By 1938, the hyphen had been lost and the modern name was in use. Because supernovae are relatively rare events within a galaxy, occurring about three times a century in the Milky Way, obtaining a good sample of supernovae to study requires regular monitoring of many galaxies.
Supernovae in other galaxies cannot be predicted with any meaningful accuracy. Normally, when they are discovered, they are already in progress. To use supernovae as standard candles for measuring distance, observation of their peak luminosity is required. It is therefore important to discover them well before they reach their maximum. Amateur astronomers, who greatly outnumber professional astronomers, have played an important role in finding supernovae, typically by looking at some of the closer galaxies through an optical telescope and comparing them to earlier photographs.
Toward the end of the 20th century, astronomers increasingly turned to computer-controlled telescopes and CCDs for hunting supernovae. While such systems are popular with amateurs, there are also professional installations such as the Katzman Automatic Imaging Telescope. The Supernova Early Warning System (SNEWS) project uses a network of neutrino detectors to give early warning of a supernova in the Milky Way galaxy. Neutrinos are particles that are produced in great quantities by a supernova, and they are not significantly absorbed by the interstellar gas and dust of the galactic disk.
Supernova searches fall into two classes: those focused on relatively nearby events and those looking farther away. Because of the expansion of the universe, the distance to a remote object with a known emission spectrum can be estimated by measuring its Doppler shift (or redshift); on average, more-distant objects recede with greater velocity than those nearby, and so have a higher redshift. Thus the search is split between high redshift and low redshift, with the boundary falling around a redshift range of z=0.1–0.3—where z is a dimensionless measure of the spectrum's frequency shift.
High redshift searches for supernovae usually involve the observation of supernova light curves. These are useful for standard or calibrated candles to generate Hubble diagrams and make cosmological predictions. Supernova spectroscopy, used to study the physics and environments of supernovae, is more practical at low than at high redshift. Low redshift observations also anchor the low-distance end of the Hubble curve, which is a plot of distance versus redshift for visible galaxies.
Supernova discoveries are reported to the International Astronomical Union's Central Bureau for Astronomical Telegrams, which sends out a circular with the name it assigns to that supernova. The name is formed from the prefix SN, followed by the year of discovery, suffixed with a one or two-letter designation. The first 26 supernovae of the year are designated with a capital letter from A to Z. Afterward pairs of lower-case letters are used: aa, ab, and so on. Hence, for example, SN 2003C designates the third supernova reported in the year 2003. The last supernova of 2005, SN 2005nc, was the 367th (14 × 26 + 3 = 367). Since 2000, professional and amateur astronomers have been finding several hundred supernovae each year (572 in 2007, 261 in 2008, 390 in 2009; 231 in 2013).
Historical supernovae are known simply by the year they occurred: SN 185, SN 1006, SN 1054, SN 1572 (called Tycho's Nova) and SN 1604 (Kepler's Star). Since 1885 the additional letter notation has been used, even if there was only one supernova discovered that year (e.g. SN 1885A, SN 1907A, etc.)—this last happened with SN 1947A. SN, for SuperNova, is a standard prefix. Until 1987, two-letter designations were rarely needed; since 1988, however, they have been needed every year. Since 2016, the increasing number of discoveries has regularly led to the additional use of three-digit designations.
Astronomers classify supernovae according to their light curves and the absorption lines of different chemical elements that appear in their spectra. If a supernova's spectrum contains lines of hydrogen (known as the Balmer series in the visual portion of the spectrum) it is classified Type II; otherwise it is Type I. In each of these two types there are subdivisions according to the presence of lines from other elements or the shape of the light curve (a graph of the supernova's apparent magnitude as a function of time).
DILENGKAPI REM CAKRAM GANDA, FLEXY COUPLING,TWIN SHOCK ABSORBER,SEAL BEARING,HARDENED STEEL SHAFT AND AXLE,REMOVABLE SUBFRAME.
Viario untuk difabel, dilengkapi rem cakram ganda,flexi coupling, hardened steel shaft,sealed bearing,removable subframe.
Day 11, 30 hours build time.
The neck subframe has now been attached to the cargo bay, and both side walls of the cargo bay have now been completed. The temporary cargo bay frame has been removed because I can use the walls of the cargo bay as size and distance references.
This is a total of 40 subframes on the ZWO ASI6200MM Pro processed with AutoStakkert!3, Registax 6 and GIMP.
All custom VRP (Verona Racing Parts) aluminium chassis, swingarm, gas tank, subframe/airbox.
Mugen equipped engine (shown here with a 1990 HPP engine)
The fifth generation of the Quattroporte (Tipo M139) was unveiled to the world at the Frankfurt Motor Show on 9 September 2003 and made its U.S. première at the 2003 Pebble Beach Concours d'Elegance; production started in 2003. Exterior and interior design was penned by Pininfarina's then chief designer Ken Okuyama.
Built on an entirely new platform named the M139, it was 50 cm (19.7 in) longer than its predecessor and sat on a 40 cm (15.7 in) longer wheelbase. The same architecture would later underpin the GranTurismo and GranCabrio coupés and convertibles.
Initially, the Quattroporte was powered by an evolution of the naturally aspirated dry sump 4.2-litre V8 engine, as used in the Maserati Coupé, with an improved power output of 400 PS (294 kW; 395 hp) and new black plastic inlet manifold instead of an aluminium cast one.
The Quattroporte's body is a steel unibody, with an aluminium boot lid and engine bonnet; the coefficient of drag is Cd=0.35. Front and rear aluminium subframes support the whole suspension and drivetrain.
A 47%/53% front/rear weight distribution was achieved by setting the engine behind the front axle, inside the wheelbase (front-mid-engine layout) and the adoption of a transaxle layout. With the later automatic transmission - fitted in the conventional position en bloc with the engine - weight distribution changed to 49%/51% front/rear.
The V8 engines of the fifth generation of the Quattroporte belonged to the 'Ferrari-Maserati F136' family; they had aluminium-silicon alloy block and heads, a crossplane crankshaft, four valves per cylinder driven by two overhead camshafts per bank and continuous variable valve timing on the intake side. F136S 4.2-litre engines in DuoSelect equipped cars used a dry sump lubrication system; F136UC 4.2-litre engines on automatic cars were converted to use a wet sump oiling system, as did the later 4.7-litre, codenamed F136Y.
30x120 second subframes, total integration 1 hour.
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
20th July 2017
Cambridge, UK