Siamese If You Please

Siamese Twins

The Siamese Twins (NGC 4567, 4568, and 4564)
Sketch and Details by Bill Ferris

NGC 4567 & NGC 4568 “Siamese Twins”: Galaxy Pair (Virgo)
RA: 12h 36.6m / DEC: +11º 15′.5
Instrument: 18-inch Obsession

This interacting galaxy pair resides in the heart of the Virgo cluster. My sketch presents a 199X view in the 18-inch Obsession. NGC 4567 and NGC 4568 stand just inside the southern field boundary. This duo is known collectively as the “Siamese Twins.” Of the two, NGC 4567 is more prominent. This 11.3 magnitude SA-type galaxy ranges over a 2′.8 by 1′ area and is aligned nearly east-to-west. This galaxy features a stellar core embedded within a brighter core region. NGC 4568 connects at the eastern tip and extends to the south-southwest. This 10.8 magnitude spiral is about the same length but cuts a slimmer profile. NGC 4568 also presents a brighter core region within the larger oval but does not present a stellaring at the center. A close pair of bright stars simmers 3′ to the east. About 11′ north just inside the opposite field boundary, NGC 4564 is seen. It’s an 11.1 magnitude elliptical galaxy about 1′.5 by 0′.6 in size. NGC 4564 is arranged along a northeast-to-southwest axis. It is flanked 4′ to the southeast and 3′ to the northwest by 12th magnitude stars. You’ll find the Siamese Twins about 38 southeast of M58.

A Double and a Trifid

M20

M20 (The Trifid Nebula)
Sketch by Eiji Kato

M20, The Trifid Nebula, is a famous and beautiful target for astro-photographers. The red emission nebula contains a young star cluster at its center, and is surrounded by a blue reflection nebula that is most noticeable at the northern end. It’s distance is not well agreed upon, and is listed anywhere from 2,200 light years (Mallas/Kreimer) to 9000 light years (Jeff Hester).

The dark nebula that crosses the Trifid was cataloged by Barnard and listed as B 85. The object was originally cataloged by Charles Messier in 1764, when he described it as a cluster of stars. William Herschel assigned catalog numbers to 4 different parts of the nebula (H IV.41, H V.10, H V.11, and H V.12).

Unusual Earthshine

Earthshine

Moon with Earthshine
Sketch and Details by Carlos E. Hernandez

I was struck by the Waxing Crescent Moon (2.4 days old) over the western horizon (~11 degrees) tonight (January 11, 2008 at 00:00 U.T.) as it appeared that the Earthshine over the unilluminated portion was asymmetric. I turned my 11 x 56 Oberwerk binoculars upon it and noted a brightening over the Moon’s northern (upper) limb. My wife also noted the brightening without my suggestion. There also appeared to be a “glow” surrounding the crescent Moon. I have never observed this over the Moon at this or any other phase. This most likey represnts an atmospheric phenomena (e.g. haze or diffuse cloud).

A digital rendering in Corel Painter X.

Carlos

To Sketch a Sketch for the Sake of Science

Mars

Modified Test Drawing of Mars: 1890
Drawing by Professor Schiaparelli, modified by test administrators

The above sketch was used as part of an experiment in determining the origin of the observation of Martian canals. Excerpts from the article are shown below. The entirety of this interesting and enlightening article can be read at Google Books (see link at the end of this post).


Experiments as to the Actuality of the, “Canals” observed on Mars.
By J. E. Evans and E. Walter Maunder.The experiments described in the following paper were undertaken in order to ascertain whether the impression of a network of fine lines, such as forms what is now known as the “canal system” of Mars, could be produced upon entirely unbiassed observers without those lines having a real objective existence; and, should this prove to be the case, to find out the conditions most favourable for the creation of such an impression. The experiments were made in the following manner. A circular disc, varying according to circumstances from 3.1 to 6.3 inches in diameter, was given to a class of boys to sketch. The boys in the class were usually twenty in number, and were seated at various measured distances from the disc. These distances varied in the extreme from 15 feet up to 62 feet, but more generally from about 17 feet to 38 feet. The boys were all supplied with a piece of drawing-paper upon which a circle 3 inches in diameter had been described, and were instructed to fill in that circle with all the details which they could perceive upon the disc. No hint was given them that they ought to see lines or dots or any other form of marking ; they were simply urged to draw all that they could see and be sure of, each for himself, without noting what his neighbours were drawing….

….The boys employed in the experiments were from the Royal Hospital School, Greenwich. Their ages ranged from twelve to fourteen for the most part; a few were either a little older or a little younger than these ages. All of them were wholly and entirely ignorant of the appearance of Mars in the telescope, and of the discussions which have taken place as to the markings on his surface. They were simply shown, what was to them, an odd-looking figure, and were told to reproduce it as well as they could. The first series of experiments was made on 1902 July 1, the last on 1903 May 22, the great majority having been made in the spring of the present year….

….Experiments 8 and 9.—Drawing 6.25 inches based upon one by Professor Schiaparelli made 1890 May 16 (La Plancte Mars, p. 474). In this experiment none of the canals shown by Professor Schiaparelli were inserted, but a number of small irregular markings were inserted at haphazard. River-like marks were drawn flowing into Dawes’ Forked Bay and the smaller marking of the same character which Schiaparelli has represented some 30° from it at the mouth of the Phison. The region of Meroe Island was put in in half-tone….

….It appears to us in reviewing the entire series of the experiments that it is impossible to escape the conclusion that markings having all the characteristics of the canals of Mars can be seen by perfectly unbiassed and keen-sighted observers upon objects where no marking of such a character actually exists. They are in a sense truly “seen,” not imagined, because they are the natural rendering by the eye of real markings of a different character….

….Generally speaking, the best draughtsmen, that is to say, those who most truthfully represented the salient features of the drawing, also showed the greatest numbers of canals. It is also worth note that on the whole the agreement as to the canals was greater than the agreement as to the broad features of the original drawing….

….Our conclusion from the entire experiment is that the canals of Mars may in some cases be, as Mr. Green suggested, the boundaries of tones or shadings, but that in the majority of cases they are simply the integration by the eye of minute details too small to be separately and distinctly defined. It would not therefore be in the least correct to say that the numerous observers who have drawn canals on Mars during the last twenty-five years have drawn what they did not see. On the contrary they have drawn, and drawn truthfully, that which they saw; yet, for all that, the canals which they have drawn have no more objective existence than those which our Greenwich boys imagined they saw on the drawings submitted to them.

It seems a thousand pities that all those magnificent theories of human habitation, canal construction, planetary crystallisation, and the like are based upon lines which our experiments compel us to declare non-existent; but with the planet Mars still left, and the imagination unimpaired, there remains hope that a new theory no less attractive may yet be developed, and on a basis more solid than “mere seeming.”


Published in the Monthly Notices of the Royal Astronomical Society, Vol. LXIII, 1903, Pages 488-499 available at Google Books.

Galactic Smirk

NGC 5529

NGC 5529
Sketch and Details by Bill Ferris

NGC 5529: Edge-on Galaxy (Bootes) RA: 14h 15.6m / DEC: +36º 13′.6
Instrument: 18-inch Obsession

Here’s an interesting edge-on galaxy. NGC 5529 resides in west-central Boötes about 4 degrees southwest of 3rd magnitude Gamma (27) Bootis. My sketch presents a 199X view in the 18-inch Obsession. NGC 5529 is the thin sliver of light at the center. This 11.9 magnitude spiral covers a 6′ by 0′.7 patch of sky with that part west of the core appearing brighter than its counterpart to the east. The core region is slightly irregular in shape, looking like two small humps on either side of the core. An interesting three-star asterism stands a few arcminutes to the east. A faint 14th magnitude sparkler simmers close by, just off the galaxy’s eastern tip. And 1′.7 south of this star is where PGC 50952 emerges from the night. This 15.3 magnitude spiral presents as a 30″ diameter glow. It’s very subtle and best seen with averted vision. Even more challenging, is the delicate smudge some 5′ to the northwest. That tiny patch of fog is MCG +06-31-85a, a 16th magnitude galaxy with just the brighter 0′.3 diameter core being visible in the 18-inch. This galaxy is seen intermittently with averted vision, but always in the same location. This view is framed by twenty-five stars scattered throughout the field in my sketch.

Upon the Sea of Clouds

Bullialdus

Bullialdus Crater
Sketch and Details by Frank McCabe

Western Mare Nubium has been the home of complex, Eratosthenian period crater Bullialdus (61 km.) for the past three and a half billion years. The beautifully terraced inner walls to the east and kilometer high central peaks were clearly seen in the morning light. The outer downward sloping walls were showing alternating radial ridges and valleys down to the lava flooded floor of Nubium. The crater rim stands 2.4 kilometers above the crater floor and the floor is 1.2 kilometers below the surrounding Mare Nubium lava.
The ancient flow of lava across the Sea of Clouds breached the walls and flooded the floors of craters Kies (44 km.) to the southeast and Lubiniezky (44 km.) to the northwest of Bullialdus. Immediately to the south of Bullialdus are Bullialdus A and B, both twenty something kilometers in diameter with the closer A being the larger of the two. The famous 11 kilometer dome Kies л was clearly seen just to the west of crater Kies and to the northwest, crater König (23 km.) looked impressive with its dark shaded floor.

Sketching:

For this sketch I used: black Strathmore 400 Artagain paper, 9”x 12”, white and black Conte’pastel pencils and a blending stump. Brightness was slightly decreased (-3) and contrast increased (+2) after scanning using Microsoft Office Picture Manager.

Telescope: 10 inch f/ 5.7 Dobsonian and 6mm eyepiece 241x
Date: 5-15-2008 2:10 – 3:45 UT
Temperature: 8° C (46° F)
passing clouds, calm
Seeing: Antoniadi III
Co-longitude: 28.8°
Lunation: 9.6 days
Illumination: 78.5 %
Phase: 55.3°
Observing Location: +41°37′ +87° 47′

Frank McCabe

Graffias of Scorpius

Beta Scorpii

Beta Scorpii (Graffias)
Sketch by Michael Vlasov

This pair of hot B-class stars lies about 530 light years away. Their separation of 14 arc seconds places them at least 2200 astronomical units from each other. Beta-1 has another companion hugging it much closer at .5 arc seconds. Both Beta-1 and Beta-2 are also thought to be spectroscopic binaries, bringing the total number of stars in the system to 5.

Source: Wikipedia.

Porrima’s Clockwise Progression

Gamma Virginis

Gamma Virginis
Sketch and Details by Jeremy Perez
Move mouse over sketch to compare change in position from January 2007 to April 2008.
Click the image for a larger version.

About 38 light years away in the constellation Virgo, this pair of twin stars orbit one another once every 169 years. When I last observed them in January 2007, they appeared as a single, elongated, pill-shaped star. On April 10, 2008, the diffraction discs were now clearly separated into two distinct stars with no overlap. Position angle had also proceeded about twenty degrees clockwise since my last look.

During my January 2007 observation, I estimated a position angle of 60 degrees. However, the data in Brian Workman’s Double Star calculator indicated they should have been 49 degrees. I thought this was strange at the time, since I would probably have guessed 45 degrees if that were the case. Recently, I had a look at some more refined data provided by Brian Skiff. Plugging that into the calculator led to January 2007 value of 58 degrees–much closer to my estimate at the time.

For the April 10, 2008 observation, I was able to put the astrometric eyepiece to use on the pair, and arrived at a position angle of 36 degrees. Skiff’s data points to a value of 37.9 degrees. Based on diffraction discs that are not quite touching, I estimated a separation of .92 arc seconds. Skiff’s data comes out to .993 arc seconds.

I was excited to see such a pronounced difference since last year. What a privilege to watch the slow dance of this stellar couple.

Subject Gamma Virginis (Porrima / STF 1670)
Classification Double Star
Position (J2000) Virgo [RA: 12:41:39.9 / Dec: -01:26:58]*
Position Angle* 36° [My measurement 2008.27]
37.9° [Skiff Data interpolated 2008.27]
Separation* 0.92″ [My measurement 2008.27]
0.993″ [Skiff Data interpolated 2008.27]
Magnitudes* 3.6; 3.7
Spectral Types*
Date/Time APR 10, 2008 – 10:30 PM MST (APR 11, 2008 – 05:30 UT)
Observing Loc. Flagstaff, AZ – Home
Instrument Orion SVP 6LT Reflector (150 mm dia./1200 mm F/L)
Eyepieces/Mag. 12 mm Meade Astrometric Eyepiece+ 2X Barlow (200X)
Conditions Clear, calm, first quarter moon
Seeing 6/10 Pickering
Transparency NELM Mag ~5.0
*References The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996); Brian Workman’s Double Star Calculator (Using orbital elements supplied by Brian Skiff)