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Il riduttore di focale

to the photograph of the deep sky, in the jargon "deep sky", they often resort to the use of optical system interposed in the optical telescope's eyepiece or first sensor recovery.

Such optical systems have the task of reducing the focal length of the telescope and then to increase both the brightness, in terms of focal ratio F / D where D is the diameter of the main objective and its focal length F, and the amplitude of the resulting angular field on the sensor or film photography. Please note that the angle of view is:

A = 2 (arctg (d/2F))

A = angle in sexagesimal degrees
d = diagonal optical sensor in mm.
F = focal length lens or primary mirror in mm.

should be said that, in this case means the lowest brightness-ratio equal to diameter of the main objective, achieving the goal of reducing the exposure time.

Very often it is believed, in the case of visual observations , a 300 mm. diameter lens or mirror to F10, at the same magnification, is less luminous than a 300 mm. to F5.
In fact, such a 100x for both, you have the same brightness as the primary focus, as la luminosità intrinseca di un obiettivo è direttamente proporzionale al suo diametro.
Chiaramente per ottenere lo stesso ingradimento dovremo utilizzare due oculari di differente focale, infatti l'ingradimento al fuoco primario è:

I = F/Fo

I = ingrandimento

F= lunghezza focale obiettivo primario

Fo = lunghezza focale oculare

Riassumendo, e limitandoci alla riprese con sensori ccd o pellicola, l'uso di riduttori focale, sono, in prima approssimazione, consigliati ed usati per rapporti focali superiori ad F8.

La geometria ottica del sistema per ridurre la focale di un obiettivo si esprime con:

1/Fr = 1/Do - 1/Dn    (1)

DnDo = Fr(Dn-Do)      (2)

Fr= lunghezza focale del riduttore

Do= distanza dalla nuova posizione del fuoco (Po)

Dn= distanza dalla posizione originale del fuoco (Pn)

The reduction factor of the focal length is:

Rr = Do / Dn (3)

by (2) and (3) we get:

Rr = 1 - Do / Fr (4)

Thus, varying the distance Do you get a resultant reduction (RR), which means that the extent of reduction depends the variation in the distance Do, while the ratio has as a condition Rr Rr \u0026lt;1. In the special case where the distance Do = 0, from (4) he is Rr = 1, we are the primary focus without any reduction.

As an example, suppose you have a SC of 300 mm with F10, then with a focal length of 3000 mm. We use a focal reducer, whose focal length is 198 mm. And we want to bring your instrument a reduction factor Rr = 0.48x.

How far we have to place the sensor to achieve the reduction indicated?

From (4) Do we have 198 = (1 - 0.48) = 102.96 mm. By placing the focal plane of our sensor to 102.96 mm. from the back of the lens focal reducer, we have a reduction of 0.48 of focal primary, which in our example becomes 3000 * 12:48 = 1440 mm pari ad F4.8

Nella pratica, tuttavia, utilizzando il riduttore di focale Alan Gee II (Lente di Shapley), occorre fare delle ulteriori considerazioni, in relazione alla progettazione e geometria del riduttore stesso.

Con il Meade SC ACF GPS da 10" ho inizialmente provato il riduttore di focale della stessa Meade F3.3, verificando immediatamente che tale sistema non poteva essere utilizzato con l'ottica ACF a campo piano, poichè il riduttore introduceva un ulteriore correzione al campo, ed in definitiva l'immagine risultante era decisamente distorta. Il riduttore Meade F3.3 deve essere usato sul precedente modello LX200 senza il trattamento ACF optics.

At this point, after some research, I identified the focal reducer Alan Gee II, the system could be used with LX200 ACF.

This gearbox is designed to be mainly used with telescopes SC F10 or above and placed directly into the breech of the telescope, some centimeri primary lens hood inside the tube.

I-ratios range from F5.9, in the standard configuration, up to F3.5, whereas a possible vignetting, too if you increase the apparent field of view.

From some prove fatte, con il Meade F10 da 10" ACF , sembra che il riduttore Alan gee II dia i migliori risultati con rapporti di focale compresi tra F5.9 e F4.3, producendo una campo corretto ed uniforme.

La dotazione standard comprende alcuni accessori che consentono di montare adeguatamente il riduttore al telescopio. Con questa modalità è possibile utilizzare il riduttore di focale, che in uscita ha un filetto T2, con telescopi dotati anche di focheggiatore.

Il corpo del riduttore è formato di tre elementi: due raccordi filettati di 19 mm. ciascuno ed il corpo lenti di 23 mm.


In my case I used the gearbox with the following configuration:


1) in the focuser I placed a link that has a thread exit SC
2) I only placed the valve housing with flange connection to SC/T2 supplied to the thread connecting all of SC 1);
3) to the final T2 I screwed a holder T2/1.25 " 15mm. length;
4) integration (optional) and then a diagonal dielectric sensor.


Using a diagonal was considered only in the situation of having an easier position sensor in the case of objects with heights around 60 ° / 70 ° to facilitate the exchange of filters Recovery . We suggest, however, that in the case of shooting in the highest definition, use the sensor directly, without bias or other additional optical paths.

Following are some trial calculations:


a) one body length with reducer and flange ring + holder (15 mm.) To the outer edge = 58 mm.

b) actual distance from the lens of the rear gear to the outer edge dell'holder = 32.5 mm.

c) the effective length of the diagonal path = 75 mm.

d) Length of the reducer fitting extension 19 mm. each

e) further away CCD Meade DSI PRO II B / W = 27.3 mm frog


An example:

b) + c) + e) \u200b\u200b= 134.8 mm = Do

by 4) we have:

Rr = 1 - 134.8/259 = 0.48

then the focus of the telescope is to be moved outward by an amount equal to:

Dn = Do / = Rr = 280.8 mm 134.8/0.48

This value is added to the focus of the telescope to a focal risultante (Fe) pari a F + Dn. Nel caso del LX200 ACF, F= 2500 mm.:

Fe = 2500 + 280.8 = 2780.8

e la sua apertura effettiva diventa Fe/D = 2780.8/254 = 10.9 senza compressione. Con il fattore di riduzione Rr il rapporto focale effettivo diventa:

F10.9* 0.48 = F5.2 = Rr = 0.52

I tempi di esposizione si riducono di un numero di volte pari a = 1/Rr^2.
The amplitude of the image decreases 1/Rr times, and the field amplitude increases 1/Rr times. In the example 1/0.52 1/.52 ^ 2 = 3.7 and = 1.9

Experimentally, I verified that using the focal reducer Alan Gee II, after the focuser, the scope of use can be reduced to -ratios between F5.9 and F4.6, varying the distance, with no vignetting apparent.

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La lente di Barlow

In astrophotography related mainly to large bodies of solar system: sun, moon, planets, it is useful to have an accessory, the Barlow, extremely useful, because you can significantly increase the size of the object on the CCD detector or other sensor.

The Barlow lens is used to increase the focal length of primary education, is a diverging lens. Its use, however it is generally closely related to three basic conditions:

1) well-collimated optics
2) Adequate resolution of the sensor.
3) Good transparency atmospheric conditions (seeing).

For the first two points, we can always intervene direttamente per migliorare, mentre per il terzo punto, purtroppo, dobbiamo affidarci a quelle che sono le condizioni di turbolenza del nostro sito di osservazione, ed attendere il momento in cui l'oggetto e la trasparenza atmosferica sono nelle migliori condizioni per le riprese.

Devo dire che nel mio caso, molto vicino al livello del mare, tali condizioni concomitanti sono piuttosto difficili da realizzare, ed ho stimato, sulla base di ricerche specifiche, che tali situazioni possono verificarsi non più di 15 - 20 volte ogni anno. E' facile intuire che riuscire a riprendere dettagli fini ad esempio dei pianeti maggiori, non è una impresa facile.

Per evitare tali incovenienti è possibile Download all car sites and reach the highest altitude (700-900 meters), but this is not always possible in case of heavy equipment and in the absence of someone who can give us a help.

So you will need to obtain an adequate patience and in most of the comments seek a compromise between weather conditions and the size of the object you want to achieve.

The first experiences in 2009 I made predominantly predominantly with the planet Jupiter
visible almost throughout the summer in the south-southeast . The results were encouraging, but I think we can still improve .

Let's see how a Barlow .

The left figure presents a schematic.
goal
A = B = barlow
Po = original distance
Pn = new distance

Two equations describe the geometrical optics:

1/Fb = 1/Po - 1/Pn (1)

Pn Po Fb = (Pn-Po) (2)

where Fb = focal length of Barlow

The multiplicative factor of R Barlow lens is expressed by:

R = Pn / Po (3)

by (2) gives:

Pn = Fb (1 - R) (4)

from which we get the multiplication factor R as a function of distance and the focal length of the PN Barlow:

R = 1 + Pn / Fb (5)

Without further complications, we have the necessary elements for our calculations. We recognize that if the two distances Pn and Po are the same, we are the primary focus, then no optical element and without any focal aggiutivo result. Therefore, an essential condition is that R must be greater than one (R> 1)

Now suppose you have a telescope with a focal length of 2000 mm. to F10 and a Barlow lens whose focal length is 45 mm. and you want to obtain a multiplication factor equal to 3x the distance at which Pn we have to ask for this factor?

From (5) we obtain: 3 = 1 + Pn/45 where Pn = 2 * 45 = 90 mm. Or our positioning sensor (focal plane) to 90 mm. barlow back of the lens will increase the focus of our primary instrument of 3 times, then you have 2000 * 3 = 6000 mm. to F30.

I use a good Barlow lens, the Baader Planetarium, with click-clock system, a perfect centering on-axis, modular, with accessories that allow you to vary the R-factor of 2x to 4x, depending on the configuration.

Its focal length is 66.67 mm.

In the standard configuration as shown, we get an R factor equal to 2x. In practice, when attached to the frog, for example 31.8 of the CCD, the system click-clock, should be taken into account that the sensor plane turns out to be a few mm further. In the calculations, as far as the sensor II DSI Pro B / W, which I make good use, you must add 25.5 mm. And, therefore, in its standard configuration that Barlow, is have an R factor equal to 2.38X.

With extension tubes with different lengths you can get all the intermediate factors R up to 4x. In this way, everyone can make best use of this barlow according to his needs and in relation to optical instruments in use.

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Foto del pianeta Giove

The instrumentation used in planetary photography is as follows:

1) CCD camera Meade DSI PRO II monochrome
2) RGB Filters + IR-CUT
3) processing software AtroArt 4.0 and 5.0 Registax


Le specifiche tecniche, di tale strumentazione hardware e software, saranno oggetto di prossime mie riflessioni e commenti.


Al momento intendo presentare le esperienze, in campo, ad iniziare dalle riprese effettuate da Luglio 2009 fino a Settembre 2009.

Tutte le immagini sono state riprese con il Meade lx200 ACF , in ciascuna immagine è presente una didascalia con i relativi dati tecnici.

Coordinate della località di osservazione Lat= 43°18'25" N. Lng= 13°43'11" E. Hslm= 15 m.

Foto realizzata in condizioni estreme di trasparenza.
Data 09/lug/2009   21h 29m 46 sec. T.U.

H= 8° Az=298° ESE

Coordinate topocentriche J2000

Ar= 21h 54m 3.1s

De = -13° 47' 20"

Diametro equat. fase corretta= 46.6"

Mag. visuale= -2.7

Filtri RGB + IR_CUT

Somma di 26 immagini Tempo Totale= 1.46 sec.

CCD Temp.= 26.5  F = 2500 mm. D = 254 mm. F10

The very low height of the plants Jupiter on the horizon, only 8 °, has made the picture very noisy, with poor definition of details. However, the recovery effort can be considered useful to improve the necessary techniques.

Date 19/lug/2009 21h 40m 30 sec. TU
H = 16 ° Az = 308 ° SE
topocentric J2000 coordinates
Ar = 21h 50m 40.3s
De = -14 ° 07 '28 "
Equatorial diameter. correct phase = 47.7 "
May view = -2.8
RGB filters + IR_CUT
Sum of 24 images Total Time = 0385 sec.
CCD Temp = 24.5 F = 2500 mm. D = 254 mm. F10

We observed a clear improvement in noise that is in the details, while still having a height above the horizon less than 20 °. And 'I present the satellite, but not be seen as outside the field of view.

Date 12/ago/2009 21h 50m 03 sec. T.U.

H= 28° Az=335° SSE
Coordinate topocentriche J2000
Ar= 21h 39m 33.2s
De= -15° 08' 27"
Diametro equat. fase corretta= 48.9"
Mag. visuale= -2.9
Filtri RGB + IR_CUT
IR somma di 20 immagini Tempo Totale= 0.16 sec.
R somma di  29 immagini Tempo Totale= 0.319 sec.
B somma di  22 immagini Tempo Totale= 0.704 sec.
G somma di  29 immagini Tempo Totale= 0.638 sec.
CCD Temp.= 25.5 F= 2500 mm. D= 254 mm. F10


Condizioni di trasparenza e turbolenza mediocri. Tuttavia è stato possibile fissare i passaggi di due satelliti sul disco di Giove. Da sinistra a destra rispettivamente: Europa, Ganymede e sul fondo cielo il luminoso IO. 

Data 24/ago/2009 21h 32m 02 sec. T.U. 
H= 30° Az=345° SSE
Coordinate topocentriche J2000
Ar= 21h 33m 28.6s
De= -15° 39' 32"
Diametro equat. fase corretta= 48.8"
May view = -2.8
RGB filters + IR_CUT
IR sum of 41 images Total Time = 0.33 sec.
A sum of 39 images Total Time = 0.43 sec.
B is the sum of 43 images Total Time = 1:38 sec.
G sum of 50 images Total Time = 1.10 sec.
CCD Temp = 27.5 F = 2500 mm. D = 254 mm. F10

average weather conditions, details visible on Jupiter's disk with a certain background noise images. The shootings have been treated with Astroart registax and in different ways. Note, however, the differences noticeable in the two pictures presented.

Date 23/sett/2009 19h 51m 02 sec. TU
H = 30 ° Az = 353 ° S
topocentric J2000 coordinates
Ar = 21h 21m 42.6s
De = -16 ° 35 '10 "
equatorial diameter. = Correct phase 46.2 "
May view = -2.7
RGB filters + IR_CUT

IR sum of 18 images Total Time = 0.20 sec.
A sum of 18 images Total Time = 0.29 sec.
B sum of 18 Images Total Time = 0.58 sec.
G sum of 21 images Total Time = 0.67 sec.
CCD Temp = 25.0 F = 2500 mm. D = 254 mm. F10

Seeing and sufficient turbulence. Attenuation of shades due to atmospheric absorption and scattering. Io is visible on the right side.

Date 30/sett/2009 20h 46m 01 sec. TU
H = 29 ° Az = 16 ° SSW
topocentric J2000 coordinates
Ar = 21h 20m 15.4s
De = -16 ° 41 '19 "
equatorial diameter. correct phase = 45.3 "
May view = -2.7
RGB filters + IR_CUT

IR sum of 18 images Total Time = 0.20 sec.
R sum of 17 images Total Time = 2.12 sec.
B is the sum of 15 images Total Time = 3.75 sec.
G sum of 15 images Total Time = 3.75 sec.

CCD Temp = 25.0 F = 5500 mm. D = 254 mm. F22

The three pictures were taken with a 2x Barlow lens, 4x optical Carl Zeiss Baader Planetarium. The primary focus has been increased by a factor of 2.38x.

The attempt has been made despite not had optimal conditions for high-definition images.

It should be noted, however, the red spot and the satellite I on the right.
The shooting made it possible to verify the quality of the barlow in terms of definition and contrast.

clik-clock system has proved particularly useful and practical to use, with a perfect centering of the system optical axis of the primary focus.

The first of three images has been reduced by 25% and resampled.

These experiences have been very useful to understand and manage, in different experimental conditions is the optics, the system of automatic target recognition, with the configuration in altazimuth coordinates the management of the acquisition of CCD images using filters, and the use of processing software, such Registax and AstroArt.

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Strumenti in uso

several months using an optical telescope with the Meade ACF. The instrument is a GPS mount SC A / Z equipped with wheels for easy movement, since the total weight exceeding 40 kg

You can see the changes I made as I had to reduce the minimum height of the instrument from the ground to reduce the width of the legs and then facilitate the exit and entry of the same room on the top floor of a building, where the horizon is esssere free to 360 degrees. The amendment to the original tripod, which in the photo are visible signs of the welds made clear, however, did not lead to stability problems, even in the presence of air. The wheels are locking in order to promote greater stability.

The mount A / Z, at least for now, is preferred and used over that polar, because of the problems outlined above. The use of a polar mount with widths available could only jeopardize the stability, with great disadvantages in the use of instrumentation. In the picture is also visible in the lower left portion of the platform that allows the escape from the small room where the telescope is housed when not in use.
In order to improve environmental conditions, during the "rest "instrument, it was decided to use a cover sheet that prevents condensation forms and free of dust. While in summer conditions, when normally the temperatures during the day can exceed i 30°/31°, un piccolo sistema refrigerante, mantiene all'interno della struttura, una temperatura intorno ai 27°/28°.
Alcuni dati tecnici sul telescopio sono indicati in tabella. Particolare interessante è il completo automatismo nel settaggio dell'ora e delle coordinate geografiche, grazie al sistema GPS a 16 canali, l'allineamento al polo, ed il livellamento per individuare il piano virtuale su cui effettuare la calibrazione dell'orientamento rispetto a due stelle di riferimento. Le operazioni sono svolte in autonomia e richiedono 4/5 minuti, e nel caso di postazione mobile, come nel mio caso, vanno ripetute ad ogni sessione osservativa. L'allineamento risulta essere abbastanza precise, improved with a "running" of the motors on both axes, which can be done at the discretion, when deemed appropriate, on fixed targets during the day.
In any case, from my tests, I could check whether the instrument has been "run in" properly resulting in automatic alignment, using its focal 2500 mm, a 9 mm eyepiece., a shooting which the CCD DSI PRO II, the object seen in the eyepiece field will also be displayed in the field of the CCD on the PC screen.

A feature that I found very helpful is the "High Precision". In fact, in the case of faint objects, not always you are sure you have correctly pointed at the target, and in such situations this function works as follows. The telescope, "identifies" an optically visible star near the celestial body that we are aiming for and invites us to perfectly centered in the visual field, and after our confirmation, the telescope moves slowly toward the object's coordinates, a beep warns us when the procedure was completed. At this point we can begin to resume our CCD. The field of view from the sensor's DSI II Pro, for a focal length of 2500 mm. reported to be 8.89 '(h) x 6.64' (w).

Some accessories have proved useful in the use of the instrument:

1) pipe hood, which in addition to prevent harmful reflections in the shot, does not allow condensation on the corrector plate and consequent fogging, at least in average moisture conditions, no saturation.

2) use of a filter in broadband, in order to reduce the brightness of the background sky, and limit the spread of public light.

successfully used, Baader Sky Glow Filter.

3) power supply.

4) Hartmann mask.

5) electric focuser.

An example of recovery, is the moon following image: 30/06/2009 20:17:04 UT F = 2500 mm. F10, IR_CUT + Sky Glow filter, CCD-TEMP 27.5 °, sum of 55 images with total time of 0.22 sec.

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Dall’avvento di una architettura esplicitamente legata al mondo dell’industria alla rifondazione etica del secondo dopoguerra, dall’esplosione della società e dei consumi di massa, all’emergere delle nuove concezioni di contesto, di paesaggio, di ecologia e di informatica Architettura e modernità. Dal Bauhaus alla rivoluzione informatica ripercorre in forma saggistica, evidenziando i protagonisti e le vicende di maggiore centralità, gli ultimi otto decenni della storia dell’architettura contemporanea.

Concepito completamente ex novo, il volume si distingue dai manuali that have an enlarged edition of History of born through interpretative keys of decades ago. Rewriting the past in this book from one part and is related to the emergence of the paradigm that characterizes the guidelines of the most innovative architecture. The book fits well into a discussion of non-fiction that conveys a sense of commitment and responsibility of the future, a vision of modernity as the tension always present in large studies of architecture dealing with crises that affect the transformation of world society and individuals with a set of aesthetic choices, organizational, and spatial issues in time.

Antonino Saggio, Architect, Professor of Architecture and Urban Design at Sapienza University in Rome and member of the Department of Architecture and Ph.D. in Theory of Architecture. He has taught and lectured abroad. She directs the series "The Revolution" that has contributed to a renewal of contemporary architectural thought. Among his books are mentioned: Giuseppe Terragni. The Life and Work, (Roma-Bari 2005), Frank O. Gehry (Turin, 1997), Peter Eisenman. Drilling in the future (Turin, 1996), Louis Sauer (Rome, 1988), Giuseppe Pagano between politics and architecture (1984) and for this publisher Introduction IT revolution in architecture (Rome, 1997)

Antonino Saggio

Architecture and modernity

From Bauhaus to the information revolution

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2010 pp. ISBN 978 884 305 164 468 9

Some reviews with wide-ranging debate
Paul Ferrara to , Clare Testoni, b , Michele Traversa c , Brunetto de Battè d , Roberto Gamba e , Andrea Bonavoglia f  , Antonello Marotta g , Valerio Mosco h

Tavole Rotonde Presentazioni Lectures

Livio Sacchi, Maurizio Unali e AS U. Pescara  a , Alessandro Anselmi, Franco Purini, Sacchi e AS InArch Roma, b , TTU Lecture series c , Politecnico di Torino Lecture d , Polis and Tirana University, University of Trieste g

Testimonials

felt That I've put all the essentials in a new perspective, Which Makes The profession of architectural history important again, and since history is must be re-written and re-viewed Every Day, Which Makes an aspect of the retrospect now, just like the prospect of the future is an aspect of the now.
Kas Oosterhuis


The book seeks a dialogue with the young player with the aim of creating a live view on the present, such as to understand the reasons and offer a possible way not only interpretative , but more closely design. In fact it is a political book. If in this sense we mean the construction of an active space that create a society that thinks in terms of merit and social commitment.
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VIII. 31. Thom Mayne, Morphois, Caltrans Offices, Los Angeles (Installation by Keith Sonnier) 2001 2004

... It is surrounded by screens. Television and those who become very thin, and those of PCs, mobile phones, browsers, music players, camcorders, cameras and so on. This omnipresence of the screen determines nell'abitante the city a state of winding, if the bombing, just a screen and a condition structurally digital ...

From Chapter 31 Expressions digital p. 409

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VIII. 31. Foreign Office Architects, International Port Terminal, Yokohama 1995-2002

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.. . The instrument of control of the project is fully digital and two young architects
(Farshid Moussavi and Alejandro Zaera-Polo) can lead to
finish the work piece experimenting to know how the new piece
computer, design and technology. The focus of the project is not
both in the architectural specificity - an idea as we said
widely debated - as in large-scale implementation,
in the development of appropriate tools to
control of both the design of both the site and in the affirmation of
new generation of architects on the international stage ... p. 405

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VIII. 33. Diller + Scofidio, Blur, Neuchatel 1998-2002

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Dal Capitolo 33. Fluidità e nuove connessioni

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