View allAll Photos Tagged Compacter
Ich habe des öfteren darüber nachgedacht, warum Hunde ein derart kurzes Leben haben, und bin zu dem Schluss gekommen, dass dies aus Mitleid mit der menschlichen Rasse geschieht; denn da wir bereits derart leiden, wenn wir einen Hund nach zehn oder zwölf Jahren verlieren, wie groß wäre der Schmerz, wenn sie doppelt so lange lebten?
(Walter Scott)
Working on this, know it doesn't show really a lot of detail and generic. The plan is to develop it out into a full family with a thin to this being the heavy. We will see how it goes. I have all the uppercase sketched out but need to do lowercase which will be hell.
Porst compact-reflex with Porst Color Reflex Auto MC 1.4/55 G
My first "modern" M42-SLR from Porst, the Porst compact-reflex, which is Cosina CSM. This copy is only named compact-reflex, but there many cameras with a further identifier, like S, SP, AM, OC, OCN, OE, OS, OV and probably some more. It would be painful to assign those cameras to the specific Cosina model, but I think the camera above and the S/SP have M42 thread mount, the others Pentax K-mount.
For sure it is no high-end camera, but it's fine. Full electronical shutter from 4 s to 1/1000 s and one mechanical time, 1/50 s. The self-timer also looks mechanical but it works completely electronically, you can't cock it until the shutter is cocked or in position "B", and it is combined with a mirror lock-up. Viewfinder with split-screen and illuminated under/over indicator for exposure metering. Yes, the metering is a bit different compared with other cameras, where you have to stop down for metering with a DOF-button which also switches the meter on. When you press the shutter button half-way on this camera, the aperture closes and the meter is switched on. If you release the shutter again, the meter is switched off, but the aperture stay closed. If you want to open the aperture again, you have to press the silver "aperture release button" next to the lens. It's easy to confuse this button with a DOF-button. It's a clever operation, better than the one on some old Chinon cameras, where you have to close the aperture with the force of your finger via the shutter buttton.
For those wondering about size...
Elmarit 28mm f2.8 ASPH
Summaron 35mm f2.8
Summicron 35mm f2 ASPH *black paint
Camera : Olympus Trip 35 compact
Film : Cinestill 800T (Kodak Vision 3 movie film / Kodak Eastman 5219T)
Shutter Speed : 1/40th sec
F stop : f2.8
Development: Digibase C41, 3 stage home kit.
I shot this roll of Cinestill film using my classic Olympus Trip 35 compact camera. It has a f2.8 to f22, 40mm Zuiko lens, and is entirely mechanical requiring no batteries. It relies on a light sensitive element to either select 1/40th or 1/200th of a second exposure based on the film speed setting and light available.
By using this camera and taking it off “A” auto the camera is in manual and intended for the use of a flash gun. The shutter speed is set to 1/40th and you are free to choose an f stop manually based on the recommendation of the flash instructions, with Cinestill there was no flash required and the film speed setting was ignored.
I decided to do this to see what the small Zukio optics could manage in various light conditions including night time, with the fixed 1/40th sec f2.8 the exposures are entirely the down to the flexibility of the film itself.
I developed it myself using a Firstcall Photographic supplied Digibase C41 kit, and using an old Agfa Rondinax 35U daylight tank, you can see how do this yourself here: www.youtube.com/watch?v=r6e4Kl41OKU
I extended the development time slightly from 3m15s to 4m, with a 4m bleach stage, and 5m fix stage.
Images have been scanned with a Plustek Optic film 8100 at 3600dpi. I have never yet found any of the Plustek suggested settings for each film type to be realistic however for Cinestill the Fuji Pro films seem to offer a pleasing result.
I am only aware of one UK supplier for Cinestill which is Firstcall Photographic in Taunton, drop them a line.
Enjoy!
Analog Compact: Olympus Superzoom 160 G (2001) - Image by Sony A200 with Minolta AF 28-80mm 1:3.5-5.6 Zoom - Photographer Russell McNeil PhD (Physics) lives in Nanaimo, British Columbia where he works also as a writer and a personal trainer.
Oliver Woods Duck Pond 3/3 - Yashica T4 Compact Film with Carl Zeiss Tessar 35mm, f/3.5 lens - Photographer Russell McNeil PhD (Physics) lives in Nanaimo, British Columbia where he works also as a writer and a personal trainer.
Added the Mamiya Sekor Macro C 80mm f4, partly to replace the compact 80mm f2.8. Think the f2.8 lens has focusing issue at infinity. Not sure if it's due to the drop or even before that. I suspect it's when I first got the M645 Super setup. It's relatively cheap and I always have back focus issues. I just kept going till I found a way to get focused shots.
It's only until recently when I shot a whole roll with M645 and the f2.8 lens and found all the focus at infinity shots were blur. I remembered focus at infinity with the 45mm and 150mm lens are sharp, be it handheld or on tripod (so it’s not camera bodies issue as well). Then saw this listing of 80mm Macro at about USD110. Much cheaper than the f2.8 lens and trying out the same lens might not be as interesting as trying macro on this setup. So I decided to acquire it though I am trying very well to limit my GAS now. Now I just have to confirm that the macro lens is sharp on focus at infinity and the rest I will explore slowly.
Recently, I have also started to find product ad or brochure of the film cameras I own. Felt my Canon Selphy a bit under utilized (ordering photobooks for my kids photos now as it's easier to manage in the long run). So, I printed postcard size of product photos and started collecting them.
The last time I shot with M39 lens on the mirrorless was probably 2 years ago. Find that it's not easy and feel they are not compatible or not really meant to be used together. Anyway, I have also bought a M39 to NEX adapter some time ago (not sure why). Yet to test whether the adapter works. Decided to try with the Canon M39 lens this time. Initially, I tried with the 35mm f2. At 1m away, it's much wider than 35mm. So switching to the 50mm f1.4 which I feel gives about 35mm angle of view. For this lens, I prefer to use aperture narrower than f2.8 or the 8 that I commonly use. At least it's able to show the 4 different lens which is what I want to record.
Small transistor radio (90mm x 60mm) whith beautiful transparent and reversed painted cover dial. Large dial knob with ripples on its perimeter and reversed painted in gold and red, ¡it looks great!. The white plastic behind dial knob is lightly corrugated. This radio also has great details in the speaker grill, back cover and nice combination of complementary colors: blue cabinet and red loud/off knob. Very compact six-transistor TOSHIBA chassis. This is the first piece I found assembled by INTERNACIONAL ELECTRONICA, S.A. , company of which had no knowledge. Also located on the web under the brand HI-DELITY with the same model.
Remember when Gentle Giant made the 12 inch versions of the vintage 3 3/4 scale Star Wars figures ?
The one I wanted was this Monster !
It would be cool to suspend it from the ceiling, like it is flying in space ......Hey I can dream about it :)
In 1982 Mercedes-Benz released the production version of more than a decade's research into developing a compact format, efficient and safe luxury car. The name '190' referred back to the 1950 and 60s versions of 'reduced power output' models of their mainstream saloon car range. The 190E specified a fuel-injected 2.0 litre, four cylinder engine, whilst a 190 model, without the 'E' (for einspritz' appellation, referred to the same engine, but using a carburetor.
Further development of the model would see additional engines deployed. A four cylinder of 2.3 litres, six cylinder of 2.6 litres, a a number of four cylinder diesel engines shard with the larger 'mid-range' Mercedes-Benz W123 successor W124 series.
Some special edition versions featuring high-output Cosworth developed four-valve-per-cylinder, twin OHC heads were also created, firstly in 190E 2.3-16 form, and later 190E 2.5-16 Evolution II form. These two cars formed the basis for a return to motor racing by Daimler-Benz, having avoided track-based competition following the catastrophic tragedy at LeMans in 1955 where a 300SLR racer flew into the crowd killing 83 people with a further 120 injured.
The W201 also market the smallest Mercedes-Benz model for decade, measuring a mere 1,680mm wide and 4,448mm long. Nonetheless, the deployment of advanced technologies such as airbags and antilock brakes made this compact Mercedes as safe at the larger models that had forged a reputation for safety excellence.
The single notable advance that saw first service in the 190 model ahead of any other Mercedes-Benz model was a new multi-link rear suspension, featuring five control arms acting in conjunction to produce a finely controlled wheel motion under all dynamic conditions for ride and handling excellence.
For all its virtues, and its luxury intent in international markets, within West Germany the 190 was frequently seen a a beige taxi, deployed with Mercedes ' 'MB-tex' - actually a synthetic vinyl masquerading as perforated leather.
Plain Jane indeed.
The original W201 190 model was replaced in 1993 by the W202, denoted C-Class in Mercedes-Benz's new naming policy, after 1.87 million vehicles had been built.
This Lego miniland-scale 190E sedan has been created for Flickr LUGNuts' 84th Build Challenge, our 7th birthday, - "LUGNuts Turns 7…or 49 in Dog Years", - where all the previous challenges are available to build to. In this case Challenge 56, - "Plain Jane", for vehicles a little bit ordinary, that might be turned into something a little bit special.
Compact cameras for 35mm film , made in Taiwan . The FF-9 was released in 1988 , and in restyled version as the FF-9S in 1992 .
15 exposiciones de 90 segundos con teleobjetivo 200 mm f/1.8, ISO 1.600, cámara Canon EOS 6D modificada. Centro, (AR): 06h 16m 52s, (Dec.): +23° 04' 06”. Campo angular: 6.5º x 4.4º. Escala: 6.7 arcsec/pixel.
IC 443, nebulosa de La Medusa, Sh2-248. Es un remanente de supernova galáctica (SNR) en la constelación de Géminis. Su distancia es de unos 5.000 años luz.
IC 443 pueden ser los restos de una supernova que ocurrió hace 3.000-30.000 años. El evento de supernova probablemente creó la estrella de neutrones CXOU J061705.3 + 222127, el remanente colapsado del núcleo estelar. IC 443 es uno de los casos mejor estudiados de restos de supernova que interactúan con las nubes moleculares circundantes.
IC 443 es una fuente extendida, que tiene un diámetro angular de 50 arcmin (en comparación, la luna llena tiene 30 arcmin de diámetro). A la distancia estimada de 5.000 años luz, corresponde a un tamaño físico de aproximadamente 70 años luz (20 parsec).
La morfología óptica y de radio de la SNR tiene forma de concha (por ejemplo, una SNR prototipo con forma de concha es SN 1006), que consta de dos subconchas conectadas con diferentes centros y radios. Un tercer subconjunto más grande, inicialmente atribuido a IC 443, ahora se reconoce como una SNR diferente y más antigua (100.000 años), llamada G189.6 + 3.3.
En particular, la morfología de rayos X IC 443 tiene un pico central y una capa de rayos X muy suave es apenas visible. A diferencia de los remanentes de plerion (Pulsar Wind Nebula, en inglés o nebulosa de viento de púlsar, es un resto de supernova que es alimentado por la energía de rotación de un púlsar, como la Nebulosa del Cangrejo), la emisión interna de rayos X no está dominada por la nebulosa central del viento pulsar. De hecho, tiene un origen térmico. IC 443 muestra características muy similares a la clase de morfología mixta de los remanentes de supernova. Las emisiones ópticas y de rayos X son fuertemente absorbidas por una nube molecular gigante en primer plano, cruzando todo el resto del cuerpo del noroeste al sureste.
La edad del remanente aún es incierta. Recientes observaciones de Chandra y XMM-Newton identificaron una nebulosa plerion, cerca del borde sur. La fuente puntual cerca del vértice de la nebulosa es una estrella de neutrones, reliquia de una explosión SN. La ubicación en una región de formación de estrellas y la presencia de una estrella de neutrones favorecen una supernova de Tipo II, el destino final de una estrella masiva, como la explosión del progenitor.
El remanente está evolucionando en un entorno rico y complejo, que afecta fuertemente su morfología. Las observaciones de longitud de onda múltiple muestran la presencia de gradientes de densidad nítidos y diferentes geometrías de nubes en los alrededores de IC 443.
Sh2-249. Es una nebulosa de emisión visible en la constelación de Géminis.
Se encuentra en la parte occidental de la constelación, en la dirección de la brillante estrella Tejat Posterior (μ Geminorum), cuya luz perturba su observación; aparece inmerso en un rico campo estelar.
Sh2-249 es una región extendida de H II que podría estar unida al complejo de la nebulosa molecular de Gemini OB1, ubicada a una distancia de unos 5.000-10.000 años luz. La fuente de ionización de la iluminación vendría del viento estelar de tres estrellas masivas de tipo espectral B, catalogada como HD 43753, HD 43818 y HD 255091.
IC 444. Es una pequeña nebulosa de reflexión en la constelación de Géminis, junto a la nebulosa Sh2-249. Dista unos 8.700 años luz.
Tejat Posterior, μ Geminorum, μ Gem, 13 Geminorum. Es la cuarta estrella más brillante de la constelación de Géminis, pese a ostentar la denominación de Bayer «Mu», duodécima letra del alfabeto griego. Comparte el nombre de Tejat con Tejat Prior (Propus, η Geminorum) y la palabra Posterior sirve para diferenciarla de esta última, ya que visualmente ambas estrellas están muy cerca. Curiosamente los dos astros son similares pero no están físicamente relacionados: Tejat Prior, distante 232 años luz del Sistema Solar, está unos 120 años luz más alejada de nosotros que Tejat Prior.
La palabra Tejat proviene de Al Taḥāyī, término arábigo. Esta estrella también fue conocida como Nuhātai, nombre de la mansión lunar árabe de la que formaba parte junto a Alhena (γ Geminorum) y Tejat Prior. Otras denominaciones que ha recibido son Calx —«talón» en latín— o Pish Pai, este último nombre de origen persa.
Tejat Posterior es una gigante roja de tipo espectral M3III con una temperatura superficial de 3.650 K. Con un radio 104 veces más grande que el radio solar, equivalente a 0,48 UA, si estuviera en el lugar del Sol su superficie se extendería hasta casi la mitad de la órbita terrestre. Brilla con una luminosidad, una vez considerada la radiación infrarroja emitida, igual a la de 1.540 soles. Respecto al Sol, se mueve con una velocidad relativa cinco veces mayor que la habitual.
Tiene una masa aproximada de 3 masas solares e inició su vida como una estrella de la secuencia principal de tipo B medio. Actualmente ha terminado la fusión nuclear tanto del hidrógeno como del helio y está evolucionando hacia una fase de más luminosidad para convertirse en una variable Mira. Finalmente se irá extinguiendo y concluirá su vida como una enana blanca masiva.2
Tejat Posterior es una estrella variable clasificada como variable irregular de tipo LB cuyo brillo varía entre magnitud aparente +2,75 a +3,02.4 Parece existir un período principal de 27 días junto a un segundo período, de mucha mayor duración, de aproximadamente 2.000 días.
Propus, Tejat Prior, η Geminorum, η Gem, 7 Geminorum. Es una estrella de magnitud aparente +3,32 en la constelación de Géminis. El nombre de Propus, de origen griego, significa «pie delantero». El término Tejat proviene de una palabra árabe de origen desconocido, mientras que la palabra Prior diferencia a esta estrella de la vecina Tejat Posterior (μ Geminorum), visualmente a menos de 2º.
Propus es una gigante roja de tipo espectral M3IIIab y 3.600 K de temperatura superficial. Situada a 350 años luz, brilla con una luminosidad 2.400 veces mayor que la del Sol. Tiene un radio 130 veces más grande que el radio solar; si estuviera en el centro del Sistema Solar, su superficie prácticamente llegaría hasta la órbita de Venus. Es una estrella variable clasificada como semirregular, con un brillo variable entre magnitud aparente +3,15 y +3,90 a lo largo de un período de 234 días.
Junto a la estrella principal, Tejat Prior A, dos estrellas más conforman el sistema estelar. A 7 UA de distancia, una compañera (probablemente de tipo espectral B) completa una órbita alrededor de la estrella principal cada 8,2 años. Más alejada, a 1,4 segundos de arco (que equivalen a una distancia mínima de 150 UA), se encuentra una segunda acompañante de tipo espectral F o G, Tejat Prior B, cuyo período orbital alrededor del par interior es superior a 700 años.
Tejat Prior era la estrella más cercana a Urano cuando éste fue descubierto el 13 de marzo de 1781 por William Herschel.
M35, NGC 2168. Es un cúmulo estelar abierto en la constelación de Géminis. Fue descubierto por Philippe Loys de Chéseaux en 1745 y redescubierto independientemente por John Bevis antes de 1750.
M35 contiene varios cientos de estrellas (Åke Wallenquist ha contado 120 con magnitud aparente superior a 13) dispersas en el área que cubre la luna llena (28 arcmin). El Sky Catalogue 2000.0 y la primera edición de Uranometría 2000.0 conceden 200 miembros. A una distancia de unos 2.800 años luz corresponde a un diámetro de cerca de 24 años luz. El cúmulo tiene una edad de entre 95 y 110 millones de años y contiene algunas estrellas que ya han abandonado la secuencia principal, entre las que se incluyen varias gigantes amarillas y naranjas de tipo espectral G tardío o K temprano.
NGC 2158. Es un cúmulo estelar abierto en la constelación de Géminis, a 15 arcmin al suroeste del también cúmulo abierto M35. De magnitud aparente 8,6, se encuentra a unos 11.000 años luz de la Tierra.
NGC 2158 es un cúmulo bastante compacto, siendo considerado durante un tiempo candidato a cúmulo globular. Hoy, sin embargo, se clasifica como un cúmulo abierto de tipo II 3 r. Es un cúmulo antiguo, cuya edad se calcula en poco más de 1.000 millones de años. Con más de 10.000 estrellas, su luz está dominada por estrellas amarillentas, la más luminosa de ellas de tipo espectral F0 y magnitud 12-13.
Fue descubierto por el astrónomo William Herschel en 1784.
Sh2-247. Es una nebulosa de emisión visible en la constelación de Géminis.
Se encuentra en la parte suroeste de la constelación, en la frontera con Orión.
Sh2-247 consiste en una pequeña región esferoidal H II cuyo diámetro aparente está alrededor de 8-9 ', unida físicamente a la región de asociación OB Gemini OB1; contiene dentro una estrella azul-blanca de la secuencia principal de la clase B0V. Presenta estructuras con filamentos espacialmente distintos. Se encuentra a unos 5.500 años luz.
IC 2157. Es un cúmulo estelar abierto en la constelación de Geminis. Fue descubierto en 1899, cuando Thomas Espin lo reconoció como un cúmulo abierto; su bajo brillo y poca concentración habían hecho que la familia Herschel ignorara este objeto. Finalmente se incluyó en el Index Catalog (IC), publicado como una extensión del Nuevo Catálogo General (NGC).
La baja luminosidad de este objeto se justifica en parte por la gran distancia a la que se encuentra, más de 6.650 años luz, por lo que también aparece fuertemente oscurecido por el polvo interestelar que se interpone a lo largo de la línea de vista; esta distancia lo coloca en el borde exterior del Brazo de Perseo.
Es un cúmulo poco estudiado, cuya edad es de aproximadamente 63 millones de años como máximo, sus componentes más brillantes muestran signos de evolución hacia la etapa de estrella gigante y dos de ellos, ubicados en el borde del grupo , son gigantes rojas en todos los aspectos. Los componentes menos masivos se encuentran, en su mayoría, en la secuencia principal y están ubicados en la región central del grupo y en dos extensiones ubicadas al norte y al este.
15 exposures of 90 seconds with telephoto lens 200 mm f / 1.8, ISO 1,600, Canon EOS 6D camera modified. Center, (AR): 06h 16m 52s, (Dec.): + 23 ° 04 '06 ". Angular field: 6.5º x 4.4º. Scale: 6.7 arcsec / pixel.
IC 443, Jellyfish Nebula, Sh2-248. It is a remnant of galactic supernova (SNR) in the constellation of Gemini. Its distance is about 5,000 light years.
IC 443 may be the remains of a supernova that occurred 3,000-30,000 years ago. The supernova event probably 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 that interact with the surrounding molecular clouds.
IC 443 is an extended source, which has an angular diameter of 50 arcmin (in comparison, the full moon has 30 arcmin in diameter). At the estimated distance of 5,000 light years, corresponds to a physical size of approximately 70 light years (20 parsec).
The optical and radio morphology of the SNR is shell-shaped (for example, a shell-shaped SNR prototype is SN 1006), which consists of two sub-slices connected to different centers and radii. A third larger subset, initially attributed to IC 443, is now recognized as a different and older SNR (100,000 years), called G189.6 + 3.3.
In particular, the IC 443 X-ray morphology has a central peak and a very soft X-ray layer is barely visible. Unlike remnants of plerion (Pulsar Wind Nebula, in English or pulsar wind nebula, it is a rest of supernova that is fed by the energy of rotation of a pulsar, like the Crab Nebula), the internal emission of rays X is not dominated by the central nebula of the pulsar wind. In fact, it has a thermal origin. IC 443 shows characteristics very similar to the mixed morphology class of the supernova remnants. The optical and X-ray emissions are strongly absorbed by a giant molecular cloud in the foreground, crossing all the rest of the body from northwest to southeast.
The age of the remnant is still uncertain. Recent observations by Chandra and XMM-Newton identified a plerion nebula near the southern edge. The point source near the vertex of the nebula is a neutron star, relic of an SN explosion. The location in a region of star formation and the presence of a neutron star favor a Type II supernova, the final destination of a massive star, such as the progenitor explosion.
The remnant is evolving in a rich and complex environment, which strongly affects its morphology. The multiple wavelength observations show the presence of sharp density gradients and different cloud geometries in the vicinity of IC 443.
Sh2-249. It is a visible emission nebula in the constellation of Gemini.
It is found in the western part of the constellation, in the direction of the bright star Tejat Posterior (μ Geminorum), whose light disturbs its observation; appears immersed in a rich star field.
Sh2-249 is an extended region of H II that could be linked to the complex of the Gemini OB1 molecular nebula, located at a distance of about 5,000-10,000 light years. The ionization source of the illumination would come from the stellar wind of three massive stars of spectral type B, cataloged like HD 43753, HD 43818 and HD 255091.
IC 444. It is a small nebula of reflection in the constellation of Gemini, next to the nebula Sh2-249. It is about 8,700 light years away.
Posterior Tejat, μ Geminorum, μ Gem, 13 Geminorum. It is the fourth brightest star of the constellation of Gemini, despite having the name of Bayer "Mu", twelfth letter of the Greek alphabet. It shares the name of Tejat with Tejat Prior (Propus, η Geminorum) and the word Posterior serves to differentiate it from the latter, since visually both stars are very close. Curiously, the two stars are similar but not physically related: Tejat Prior, distant 232 light years from the Solar System, is about 120 light years farther from us than Tejat Prior.
The word Tejat comes from Al Taḥāyī, an Arabic term. This star was also known as Nuhātai, name of the Arab lunar mansion of which it was a part along with Alhena (γ Geminorum) and Tejat Prior. Other denominations that it has received are Calx - «heel» in Latin- or Pish Pai, this last name of Persian origin.
Tejat Posterior is a red giant of spectral type M3III with a surface temperature of 3,650 K. With a radius 104 times larger than solar radius, equivalent to 0.48 AU, if it were in the place of the Sun its surface would extend to almost half of Earth's orbit. It shines with a luminosity, once considered the emitted infrared radiation, equal to that of 1,540 soles. With respect to the Sun, it moves with a relative velocity five times greater than usual.
It has an approximate mass of 3 solar masses and began its life as a star of the main sequence of type B medium. At the moment nuclear fusion of both hydrogen and helium has been completed and is evolving towards a phase of more luminosity to become a Mira variable. Eventually it will go extinct and its life will end like a massive white dwarf.2
Tejat Posterior is a variable star classified as an irregular variable of type LB whose brightness varies between apparent magnitude +2.75 to +3.02.4 There seems to be a main period of 27 days together with a second period, much longer, of approximately 2,000 days.
Propus, Tejat Prior, η Geminorum, η Gem, 7 Geminorum. It is a star of apparent magnitude +3.32 in the constellation of Gemini. The name of Propus, of Greek origin, means "front foot". The term Tejat comes from an Arabic word of unknown origin, while the word Prior differentiates this star from the neighboring Tejat Posterior (μ Geminorum), visually to less than 2º.
Propus is a red giant of spectral type M3IIIab and 3.600 K of superficial temperature. Located at 350 light years, it shines with a luminosity 2,400 times greater than that of the Sun. It has a radius 130 times bigger than the solar radius; if it were in the center of the Solar System, its surface would practically reach the orbit of Venus. It is a variable star classified as semiregular, with a variable brightness between apparent magnitude +3.15 and +3.90 over a period of 234 days.
Along with the main star, Tejat Prior A, two more stars make up the star system. At 7 AU away, a companion (probably of spectral type B) completes an orbit around the main star every 8.2 years. Further away, at 1.4 seconds of arc (equivalent to a minimum distance of 150 AU), there is a second companion of spectral type F or G, Tejat Prior B, whose orbital period around the inner pair is over 700 years .
Tejat Prior was the closest star to Uranus when it was discovered on March 13, 1781 by William Herschel.
M35, NGC 2168. It is an open star cluster in the constellation of Gemini. It was discovered by Philippe Loys de Chéseaux in 1745 and independently rediscovered by John Bevis before 1750.
M35 contains several hundred stars (Åke Wallenquist has counted 120 with apparent magnitude greater than 13) scattered in the area covered by the full moon (28 arcmin). The Sky Catalog 2000.0 and the first edition of Uranometry 2000.0 grant 200 members. At a distance of about 2,800 light years corresponds to a diameter of about 24 light years. The cluster is between 95 and 110 million years old and contains some stars that have already left the main sequence, including several yellow and orange giants of the late G or early K spectral type.
NGC 2158. It is an open star cluster in the constellation of Gemini, 15 arcmin southwest of the also open cluster M35. Of apparent magnitude 8.6, it is about 11,000 light years from Earth.
NGC 2158 is a fairly compact cluster, being considered for a time candidate globular cluster. Today, however, it is classified as an open cluster of type II 3 r. It is an ancient cluster, whose age is estimated at just over 1,000 million years. With more than 10,000 stars, its light is dominated by yellow stars, the brightest of them of spectral type F0 and magnitude 12-13.
It was discovered by the astronomer William Herschel in 1784.
Sh2-247. It is a visible emission nebula in the constellation of Gemini.
It is located in the southwestern part of the constellation, on the border with Orion.
Sh2-247 consists of a small spheroidal region H II whose apparent diameter is around 8-9', physically attached to the OB Gemini OB1 association region; contains inside a blue-white star of the main sequence of class B0V. It presents structures with spatially different filaments. It is about 5,500 light years away.
IC 2157. It is an open star cluster in the constellation Gemini. It was discovered in 1899, when Thomas Espin recognized it as an open cluster; its low brightness and low concentration had caused the Herschel family to ignore this object. Finally it was included in the Index Catalog (IC), published as an extension of the New General Catalog (NGC).
The low luminosity of this object is justified in part by the great distance it is at, more than 6,650 light years, so it also appears strongly obscured by the interstellar dust that stands along the line of sight; this distance places it on the outer edge of the Perseus Arm.
It is a poorly studied cluster, whose age is approximately 63 million years at most, its brightest components show signs of evolution towards the giant star stage and two of them, located at the edge of the group, are red giants in all aspects. The less massive components are, in their majority, in the main sequence and are located in the central region of the group and in two extensions located to the north and east.