Gamma ray burst astronomers use many telescopes around the world to look for and monitor gamma ray bursts. These telescopes inculde the Hubble Space Telescope and the Chnadra X-ray Observatory in space, the Keck telescopes in Hawaii, the Very Large Array radio telescope in New Mexico (featured in the movie Contact starring Jodie Foster), the Very Large Telescope in South America, and many other smaller telescopes.

afterglow is the emission that follows a gamma ray burst in other parts of the spectrum, ranging from radio waves to X-rays, and lasting from a few days to several years. The afterglows fade away over time in a well-understood manner. The discovery of the first afterglows in 1997 was made possible by the Italian-Dutch satellite BeppoSAX. This discovery (and the detection of approximately 50 afterglows over the past 4 years) has revolutionized the field of gamma ray burst astronomy.

we have seen previously (question 14) the gamma ray burst is formed when shells of energy and matter ejected by the newly-formed hole collide and merge ("internal shocks"). After the shells merge into a single shell, this shell continues to move away from the black hole and, like a snowplow, it gathers up material from interstellar space (even though it is assumed that space is empty, in reality it is full of protons and electrons).

Although implant rupture can sometimes be seen by mammography, when possible, implant rupture is being evaluated by magnetic resonance imaging (MRI). MRI has been approved by FDA for detecting rupture or leaks. Congress passed the Mammography Quality Standards Act to ensure that mammography performed at the approximately 10,000 facilities in this country is safe and reliable.

Approximately 50 afterglows have been detected with X-ray telescopes (see question 15) so far in almost 4 years of observations. However, of these 50 afterglows only approximately 40% have also been detected with optical or radio telescopes. So, on average an afterglow is detected once a month.

was explained in the previous question, the expanding shell from the gamma ray burst gathers up material, and imparts energy to this material. Initially, the shell has more energy and it accelerates the material that it gathers up into high energies. As the shell loses energy it gives less and less energy to the material and therefore the emission becomes weaker.

Observations of the afterglows all across the spectrum tell us many things about gamma ray bursts. First, observations of the first afterglow in 1997 confirmed that gamma ray bursts occur in very distant galaxies (see question 2). Second, from observations of the afterglow we can determine how much energy was released in the gamma ray burst. Third, we can determine how much material was present in the vicinity of the gamma ray burst.

The first step in the detection of afterglows is always the detection of a new gamma ray burst by a satellite such as the IPN, BeppoSAX, and HETE-II (see qeustion 4). The information from the satellite is quickly sent down to Earth and is distributed to gamma ray burst astronomers by email, pagers, and cellular phones. When astronomers get the information, they observe the part of the sky where the gamma ray burst occured, and look for an object which fades quickly.

The twinkling of radio waves from afterglows (see question 23) has shown that afterglows start very small (about the size of the Earth's orbit around the Sun), and then expand and become larger than the Solar system.

Because ionizing radiation does just that, ionizes, it is easy to see that using a medium like a gas, and a voltage, you can measure the amount of charge liberated in that medium. That is the most common method of measuring radiation. The infamous Geiger Counter is in reality a small volume of gas, with a voltage applied across it. As the radiation enters the gas, it causes electrons to be formed, which are collected and measured to determine the amount of initial radiation present.

ipoque's traffic managers are based on the IPP2P filter technology which in turn is a netfilter/iptables module. ipoque closely collaborates with the IPP2P developer and actively supports this project.

We are equipped with new Celestron Nexstar 9.25" GPS telescopes. They are equipped with Celestron's new Starbright XL coatings for 10% more light throughput than ordinary instruments. These scopes are computer automated and have spectacular optics. Because they are bigger and have better optics they gather about 45% more light than telescopes used on other tours.

Many browsers identify themselves when they request a document. A CGI script will have this information available in the HTTP_USER_AGENT environment variable, and it can use that to send out a version of the document which is optimized for that browser. Keep in mind not all browsers identify themselves correctly. Microsoft Internet Explorer, for example, claims to be "Mozilla" to get at Netscape enhanced documents.

Various methods are being used by the sports authorities for detecting steroids like HPLC, GC, Immunoassay, Radio Immunoassay. Antibody-antigen based immunoassays are used as preliminary checks which give reasonably accurate results. Chromatographic methods may be employed for detailed analysis.

For a few days after you inject EPO, there is an overabundance of immature red blood cells... however, after 6 or 7 days, those immature red blood cells are already mature, and they are indistinguishable from any other mature red blood cell, so after 7 days they can't detect if you used EPO (unless the EPO had a marker, which some of them do...) At that point, they disqualify athletes with a hematocrit above 50% "for your safety"..

Breast implants may hide up to 25% of breast tissue from x-rays during a mammogram. A study funded by the National Cancer Institute found that mammograms missed 55% of breast cancers in women with breast implants as compared to 33% in women without implants. The technician performing the mammogram should know about the presence of breast implants so that they can use a special technique called "implant displacement views" and take care to avoid causing an implant to rupture.

Caution: Use the wiggle function on the Servo before connecting the Servo arm to anything else or make sure the Servo arm wiggle will not affect your setup. Use the Wiggle function provided in the software to wiggle the Servo. The selected active channel is the connected channel. The tops 3 pins (top cover upwards) is channel A and lower 3 pins is channel B.

There are several tests that are used to try and detect polyps. Several government agencies as well as the American Cancer Society recommend that patients undergo a test that allows the doctor to see the entire colon at age 50 and then every three to five years. Currently there are two accepted methods for seeing the entire colon: the Conventional Colonoscopy and the Double Contrast Barium Enema.

Using the PhotoScreener™ is a very simple process. The child, seated in a chair, is asked to look directly into the camera lens, and a small light is flashed to attract his or her attention. The camera can play a nursery rhyme to get a child's attention. After the first photograph is taken, the camera automatically realigns its lens and a second photograph is taken. The exposed film, much like a Polaroid photograph, is ejected and develops within two minutes.

No, normally not. At the time of day we visit the astronomers are quite busy and can't be interrupted. We do however see the observatories as they open their domes and swing into position. Some of the observatories are constructed so as to show a lot of the telescope from the exterior when the dome is open. We are available for custom charters, which could be a day trip. Normally we tour one or two of the observatories during the daytime.

No, modern telescopes are not equipped for visual (eye) observing . The scientist are making digital images that can be frequently found on the internet.

Yes, there are some images on the NRAO Web site that you can browse. In addition, images and data from two surveys of the sky made by the VLA are available on the Internet. You also may download software for viewing these image files. Check out the NRAO VLA Sky Survey and the FIRST Survey Web pages.

Nowadays, the bulk of the work astronomers do is on computers. They spend a small portion of their time at telescopes actually taking data. Astronomically-useful telescopes rarely have eyepieces you can look through. Radio, ultraviolet, or infrared telescopes collect light that you can't even see with your eye! Telescopes that collect visible light often have electronic cameras called CCD cameras that create an image in a computer.

Bill Newsome, and restored to working order by himself and Don Nisewanger.It is equatorially mounted, and has a clock drive. Roby Scope: This 6" reflector on a Dobsonian mount was built in 1946 by Robert Grasmehr, was donated to the club by his sister, Lois Roby. It was restored and placed on a new mount by SMAS in 1996. A TelRad finder is included on this tube.

The Telescopes are fixed for the first 15 levels on this site you can only push or suck the ball with the Telescopes, although more exciting ways of moving the ball around come up later on.

The telescope mounts are polar aligned using Tpoint. Tpoint is an advance alignment and pointing modeling system which improve pointing performance.

World-wide there are ten sets of frequencies used for speed monitoring. In the UK only to radar frequencies used, K band and Ku band (in a very limited way). Coverage of other frequencies other than these bands will cause the detector to false alarm, devices such as traffic lights supermarket doors, mobile phones and transmitters often operate on the X band.