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É¿®²»®ô ÞòÜò øïççç÷ ß² ß«¬±³¿¬»¼ Ю±¹®¿³ º±® Ü»¬»®³·²¹ ß•¬»®±·¼ Ô·¹¸¬½«®ª»• ô Ю±½»»¼·²¹• ±º ¬¸» ïççç Ó·²±® д¿²»¬ ß³¿¬»«®ñЮ±º»••·±²¿´ ɱ®µ•¸±°ò п«´ Ùò ݱ³¾¿ô »¼ò Asteroid at Santana Observatory June 2000 to May 2001 By: Robert D. Stephens

For the past year and a half, I have been interested in determining rotational periods of . At last year s IAPPP Symposium, I reported upon my initial results measuring six asteroids.

There is more work than ever to be done. There are now more than 20,000 numbered asteroids, those with a well-known orbit. Rotational periods have only been determined for a few hundred of these asteroids. Current Program

The main reason for configuring the instrument, as it exists, was to allow automated data gathering. The telescope takes an image of an object, slews to a different section of the sky, takes an image of another object, and so on. The data can then be reduced, while the telescope is operating, or the following .

The automatic nature of the equipment allows for much greater data being gathered than ever before. On a typical night, 80 to 150 CCD images are gathered of various asteroids and comparison stars. The software can also control the filter slider.

Obtaining asteroid light curves is done by obtaining observations of an asteroid over several nights and charting the change in brightness on an X-Y chart. By charting where the peaks and the valleys on the lay, you can find a repeating pattern that allows you to determine how fast the asteroid rotates.

The average main belt asteroid looks something like a potato. Therefore, during each rotational period, it shows two elongated sides to us, and two shortened ends towards us. During those times, the light curve will show two bright peaks, and two dim troughs. This average asteroid will rotate once in an eight- period, allowing you to see most of the curve with one night's data. Others, can be much more difficult. Some of these pesky asteroids will take several days to rotate just once. That means you need night after night of data to build the lightcurve. Even worse, is when the asteroid s rotational period is close to 24 . Here the asteroid will show nearly the same face to you every evening making it difficult to complete the entire lightcurve. In this case, a collaborative effort with observatories spaced around the Earth is advantageous. Typical Observing Run

The target Asteroid is first chosen determining which targets are within range of the telescope and are favorably placed for a long, overnight run. Referring to Lightcurves Parameters list posted at the Brian Warner s CALL Site (http://www.minorplanetobserver.com /astlc/default.htm) eliminates asteroids with well-known lightcurves. I tend to pick dimmer asteroids, working at the limit of my system.

The observatory is in heavily light polluted, suburban skies. Exposures of 90 to 180 seconds will result in an adequate signal-to-noise ratio on asteroids down to 15th . A longer exposure requires guiding, and adequate guide stars are not always available.

Accurately measuring the asteroid brightness is a tricky task. You have to compare its brightness to that of accurately measured stars. The distribution of those accurately measured stars is much sparser than you might think. In a ten-degree square section of the sky, there might be only a couple of stars that have had accurate photometry done on them. Furthermore, they certainly don t lie in the field of view of your target asteroid, which then has the nasty habit of moving from field to field, night after night. Also, those stars might not be in the range of brightness of your asteroid. All of the rest of those stars plotted in your star charts are only good to within magnitude if you're lucky! Therefore, stars lying within the field of the asteroid are used and adjusted to a common zero point.

The reduction program I use, Canopus, by BW Publishing, requires an initial measurement of high accuracy stars to set the Magnitude/Intensity Relationship. This measures the performance of the system and allows for proper interpellation of the measured results. I slew the scope to a field close to the asteroid with stars of medium to high accuracy magnitudes. These fields are often taken from the LONEOS catalog maintained by Brian Skiff at . The system loads an image of the LONEOS field, aligns the image to a catalog of stars, and measures every known star in the field. Then it discards measurements that are substantially off the predicted magnitude. The result is a sequence of measures of between 4 and 30 stars in the red magnitude band. From this, a linear relation of measured intensity vs. magnitude is computed and applied to subsequent measurements. The level of accuracy you must obtain is quite stringent. The typical asteroid has an amplitude (change in brightness) of a few tenths of a magnitude. Professionals like to therefore measure to 1/100th of a magnitude in order to generate a smooth, repeatable lightcurve. The amateurs who endeavor to do this work, although seeking to obtain the Holy Grail of 1% Photometry , are usually satisfied in getting a 2 - 3% of a magnitude accuracy. Alternately, lots of measurements can effectively suppress the noise or scatter of the observations.

All of this is accomplished using MPO Connections, a telescope/camera control and scripting program written by BW Publishing. MPO Connections is a telescope/camera control program. It has full scripting capabilities. Scripts are simple programs which send a series of commands to the telescope and computer. Scripts might include:

i Autofocus i Sit and synchronize on a star until your target is above the horizon i At a set time, slew to a nearby LONEOS Field and take an image i Slew to the target and take a series of images i Periodically, slew to a 7th magnitude star and Autofocus i Shut Down the system at a set time

The telescope can run completely unattended. Focusing is the most difficult issue to overcome. As temperatures change, the focus of the telescope also shifts due to the metal parts contracting or expanding. This results in the image being out of focus. On most nights, the telescope has to be refocused several times during the night. The control software can execute an autofocus command as part of a script. This command takes a sequence of images while sending adjustments down to the electronic focuser. It gradually creeps up on best focus in a procedure that usually takes about 5 minutes. In order for the autofocus procedure to work, the initial focus should be reasonably close.

MPO Connections also has the ability to search for guide stars for CCD cameras that have autoguiding chips.

Analyzing the Light Curve Finding a match on the rotational period is also very tricky. I use Canopus as it is the only Windows based software I am aware of that will do this function. Since the asteroid moves across different fields over the course of the study, different comparison stars are used from night to night. As I discussed, these comparison stars do not have well established magnitudes. Canopus allows for a zero point adjustment to the average of the comparison stars used in order to provide a good match between segments of the lightcurve. This technique is most effective on short period asteroids where recognizable features in the lightcurve can be found on most observing runs.

The rotational period determination is accomplished using a routine developed by Dr. Alan Harris at JPL. This performs a Fourier Analysis on the data, allowing different parameters such as number of harmonics, period, size of period steps, etc. to be held constant while others are varied. Finally, it does a least squares fit to determine the most likely period. 489 Comacina Dates Images Taken: April 27 to May 2, 2001 Number of Images Taken: 241 Period: 9.02 o .01 Amplitude: 0.36

Refining a previously determined period 1277 Dolores

Dates Images Taken: July 3 to 11, 2000 Number of Images Taken: 330 Period: 17.19 o .01 Amplitude: 0.50

Again, a difficult target because of its long rotational period. 27 Euterpe (A collaborative project with G. Malcolm, R. Koff, and S. Brincat) Dates Images Taken: July 22 to August 9, 2000 Number of Images Taken: 1,205 Period: 10.410 o òððî Amplitude: 0.29 Suggested by Dr. Alan Harris to Brian Warner s CALL Web Site because of its ambiguous period. Published work showed it to have a period of 8.5 hours, however unpublished results indicated that it might be around 11 hours. Euterpe has an unusual lightcurve at this pole position, with a single dominant peak and smaller variations over the rest of the curve. 666 Desdemona

Dates Images Taken: September 10, 2000 to October 15, 2000 Number of Images Taken: 293 Period: ïëòìë o .01 Amplitude: 0.15

Gaad! Another difficult long period asteroid. 7505 1997 AM2

Dates Images Taken: November 1 to 5, 2000 Number of Images Taken: 142 Period: 4.14 o .01 Amplitude: 0.75

Large amplitude first noticed by the French observer, Gerard Faure, who alerted Brian Warner and his CALL Web site. Gerard Faure contributes asteroid observations to ALPO s MAP Database. This Mars Crosser was a pleasure to work on because of its short period and large amplitude. 1096 Reunerta

Dates Images Taken: November 28, 2000 to January 2, 2001 Number of Images Taken: 382 Period: 13.02 o .01 Amplitude: 0.39

A medium difficult target. Observations took over a month because of poor winter weather. 1000 Piazzia

Dates Images Taken: February 2 to March 14, 2001 Number of Images: 214 Period: 9.476 o .01 Amplitude: 0.54

A relatively easy asteroid with a medium length rotational period. 1135 Colchis (A collaborative project with G Malcolm)

Dates Images Taken: March 19 to April 24, 2001 Number of Images: 1,059 Period: 23.47 o .01 Amplitude: 0.65

Ouch! The near 24 hour rotational period is a good one to work on during stormy Spring weather when you don t have several clear nights in a row. And if you believe I planned this one, I have a bridge to sell you. GSC 655:1429 A New Algol Type Variable Star by Robert D. Stephens and Lee Snyder

The main program at Santana Observatory is the determination of asteroid rotational periods. The brightness of the moving asteroid is compared against stars in its current field of view. Usually, two to five comparison stars are selected.

As part of that processes, the selected comparison stars are compared against each other to be sure that they are not variable stars that would skew the brightness determination of the asteroid.

On December 4, 2000, Robert D. Stephens and Lee Snyder were measuring Asteroid 1096 Reunerta. GSC 655:1429, located at 03h 22m 38.4s, +12p 40m 43s was selected as one of the comparison stars. Once the test for variability was performed, it was noticed that the star took a rapid drop in brightness at the end of the 2.3-hour observation session (Figure1). A check of the SIMBAD and VizieR Databases, operated at CDS, Strasbourg, France, did not reveal any previous variability determination.

Subsequent observational sessions did not reveal a downturn again for several nights. In all, 345 observations in 11 sessions from December 4, 2000 to February 24, 2001 revealed a 35.53 hour period. This is almost a perfect 1.5 to 1 resonance with the Earth s rotational period that means that the system was largely showing the same two aspects to us every night. Over the near three months it was observed, Ú·¹«®» ïæ Ñ®·¹·²¿´ ½±³°¿®·•±² °´±¬ 75% of the light curve was obtained. Winter weather ª»®•»• ±¬¸»® ½±³°¿®·•±² •¬¿®• prevented obtaining the missing segments, including much of the primary minimum downturn, before it was lost in the glare of twilight. The primary minimum is at Julian Date 2451940.6156 1.48041667. ÙÍÝ êëëæïíéî ÙÍÝ êëëæïîíê

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Ú·¹«®» îæ Ú·²¼»® ݸ¿®¬ º±® ÙÍÝ êëëæïëèç «•·²¹ ̸»Íµ§ ͱº¬©¿®» Analysis The true nature of this system cannot be determined from the newly acquired data as it was acquired in only one filter or no filter. Approximate effective wavelength used to model the system is 4500 Angstroms and an assumed temperature of 13500K for the primary and a mass ratio of 0.32. The most superior quality fit to the data using Binmaker 2.0 (Bradstreet 1993) uses an inclination of 78.0p and a temperature of the secondary 7100K cooler than that of its primary which gives an estimated spectral type ¢ B7 for the primary and ¢ F6 for the secondary. The system is semi-detached Algol type with the secondary just touching the inner critical surface of the Roche Lobe with a fillout = 0.0. If the stars with this temperature difference are main-sequence stars the mass ratio would be 0.255. A satisfactory fit using a mass ratio of 0.32 would indicate that both stars are on the main-sequence. The uncertainty of the inclination is about o3p and the temperature difference is o13% dependent upon the assumed mass ratio.

Ú·¹«®» íæ Ô·¹¸¬ Ý«®ª» ±º ÙÍÝ êëë ïìîç °®±¼«½»¼ «•·²¹ Ý¿²±°«• ¾§ ÞÜÉ Ð«¾´·•¸·²¹ Ú·¹«®» ìæ Ô·¹¸¬ Ý«®ª» Ó±¼»´»¼ ¬± Þ·²¿®§ Ó¿µ»® îòð º·¬ò д«• •§³¾±´• ®»°®»•»²¬ ¿½¬«¿´ ¼¿¬¿ò ܱ¬• ®»°®»•»²¬ ¬¸» ³±¼»´ò Ú·¹«®» ëæ Ó±¼»´ ±º •¬¿®¬ ±º •»½±²¼¿®§ ³·²·³«³ò ر¬¬»® ¿²¼ •³¿´´»® •¬¿® ·• ¬¸» °®·³¿®§ò Ý®±•• •§³¾±´ ·• ¬¸» ¾¿®«½»²¬»® ±º ¬¸» ••§¬»³ Ú·¹«®» êæ Ó±¼»´ ±º •§•¬»³ò Ô¿®¹»® ¿²¼ ½±±´»® •¬¿® ·• ¬¸» •»½±²¼¿®§ º·´´·²¹ ¬¸» ·²²»® ½®·¬·½¿´ •«®º¿½» ±º ¬¸» α½¸» Ô±¾»ò Ý®±•• •§³¾±´ ·• ¬¸» ¾¿®§½»²¬»® ±º ¬¸» •§•¬»³ò Binary Maker 2.0 Output Data Table Mass Ratio Input = 0.32 Mass Ratio < 1 = 0.32 Omega 1 = 6.107 Omega 2 = 2.510013 C1 = 9.3118 C2 = 3.86182 C inner = 3.861819 C outer = 3.560641 Fillout 1 = -18.107592 Fillout 2 = 0.0 Lagrangian L1 = 0.61468 Lagrangian L2 = 1.509358 AG = r1(back) = 0.173645 AS = r2(back) = 0.309613 BG = r1(side) = 0.173254 BS = r2(side) 0.276895 CG = r1(pole) = 0.172662 CS = r2(pole) = 0.265872 DG = r1(point) = 0.173750 DS = r2(point) = 0.385252 Mean Radius = 0.173187 Main Radius 2 = 0.284127 Inclination = 78 Wavelength = 4500 Temperature 1 = 13500 Sp = B7 Temperature 2 = 6400 Sp = F6 Luminosity 1 = .7470 Luminosity 2 = 0.1530 Gravity Coefficient 1 = 1.0 Gravity Coefficient 2 = 0.32 Limb Darkening 1 = 0.45 Limb Darkening 2 = 0.72 Reflection 1 = 1.0 Reflection 1 = 0.5

Reference:

Bradstreet, D.H., 1993, Binary Maker 2.0 User Manual, Contact Software, Norristown, PA 19401-5505, USA

Warner, Brian., 2001, Canopus Software, Colorado Springs, Colorado

Software Bisque., 2001, TheSky Software, Golden, Colorado God Awful Work at Roach Motel Observatory (856)

Photons check in but they don t check out

By: Glenn Malcolm

7430 Lippizan Dr.

Riverside CA 92509

Ù³¿´½±´³à°»ò²»¬ Dilusions of Grandure

One of the dire nessesities of an amateur astronomer is to have a house

with an observatory in the backyard. This was my main concernn when

purchasing my home in 1987. I poured the concrete foundation in 1993

and built a 100 square foot roll off roof observatory in 1995 only to find that during cold winter nights astronomy was being put aside for the recliner. It was best that I get on with the new warm room adition because the asteroids were waiting.

The Warm Room

The obervatory is constucted of a slab on grade floor and typical 2 x 4 wood framing members with wood paneling on the outide and inside. On july 4th 1998 was the grand opening or Roach Motel

Observatory Minor Planet Code 856. The warm room includes a heater, air conditioner, stereo, phone and intercome built for the die hard astromomer who do their best work under extremly harsh strenuous conditions.

Two large comfortable captains chairs were purchased after a visiting astronomer complained of severe back pain. Three pentium computers are used for data reduction , asteroid location and image processing. Roach Motel Observatory is loctated at 33

59.83 North 117 26.73 West in Riverside California. During contruction of the warm room univited guests were checking in but did not check out. Hence the name Roach Motel

Observatory. The Roll off Roof

Roach Motel Observatory houses a Meade 12 LX200 SCT. Connected to the telescope is a SBIG ST-8 with a JMI electronic focuser and Kendrick Dew Heater. I also attached a foam light shield for that pesky large minor planet that lurks in the sky once a month.

Robert Stephens and Steve Mayering built a heavy duty wedge for the 12 SCT and a permanent pier was constructed by Aztech Machine. The roll off roof consists of 2x 4 spaced 18 apart with lightweight fiberglass roofing and 8 ball bearing chain link fence casters on a track. The roof can be rolled back with one hand and eye bolts lock the roof in place after an oberving run. Asteroid Data Collection

All asteroid images and loneos star fields were acquired using pixels binned to 18-micron size (medium resolution) using the scripting part of the Connections program devolped by

Brian Warner. Scripting is a feature of Connections that gives the telescope and CCD camera a pre written set of commands (by me) in sequential order. Connections has unique scripting capabilities. Not only does it perfom the usual scripting functions of slewing to an object and taking an image, it will also internally sycronize on a bright star as well as automatically focus the telescope periodically during the night. This compensates for focusing shift due to dropping temperatures and contraction of the telescope tube. The newest version of Connections features image recognition.

Therefore, all of the telescope operation and CCD imaging of minor planets were automated while I was sleeping for the next day of work. Gone are the days of the observer working into the wee hours of the morning and I did not feel guilty. Minor planets were chosen based upon their most easterly position observable 30 minutes after sunset to provide the longest period of imaging available. An average observing run lasted about 6 7 hours. I usually write the script the night before the imaging run of the asteroid. The next night usually takes about 20 minutes to cool the camera syc the scope and start the script which makes this program especially valuable to the family man. The next morning before work at about 6:00 am I enter the oberervatory close the roof and turn off the computers. Photometry was completed using the Canopus Program, also developed by Brian Warner. Acknowledgements

Many thanks to Brian Warner for his continueing help and guidence and for the continuing development of the software program Connections and Canopus which makes it possible for the family man to find the period of asteroid rotations. A very special thanks to Robert Stephens at Santana oberervatory (Minor Planet Code 656) for his help and evolution of Roach Motel Obervatory and especially to assist with subsequent unexpected computer crashes.

. Figure 1: Lightcurve of 1568 Aisleen based on a period of 6.68 0.02 hours Figure 2: Lightcurve of 1166 Sakuntala based on a period of 6.30 0.02 hours