Tuesday, May 10, 2005

Gamma Ray Detection

A important point here is that there should be coincidental features in gamma ray detection, that should align with LIGO detectors?

Why are two installations necessary?


At least two detectors located at widely separated sites are essential for the unequivocal detection of gravitational waves. Local phenomena such as micro-earthquakes, acoustic noise, and laser fluctuations can cause a disturbance at one site, simulating a gravitational wave event, but such disturbances are unlikely to happen simultaneously at widely separated sites.


Lubos said::
The LIGO collaboration informed that the second science run did not detect any gravitational waves. The results follow from 10-day-long observations in early 2003 (two more science runs have been made ever since)


A current blackhole has been detected and so should LIGO detect it. So how long should we wait if findings are only now being conisdered from 2003 run?

Scientists have detected a flash of light from across the Galaxy so powerful that it bounced off the Moon and lit up the Earth's upper atmosphere. The flash was brighter than anything ever detected from beyond our Solar System and lasted over a tenth of a second. NASA and European satellites and many radio telescopes detected the flash and its aftermath on December 27, 2004. Two science teams report about this event at a special press event today at NASA headquarters.


Journey to a Black Hole

A direct image of gravity at its extreme will be of fundamental importance to Physics. Yet imaging a black hole requires a million times improvement over Chandra. That's a big step. Over the next 20 years, the Cosmic Journeys missions will take us closer and closer to a black hole though the power of resolution. Each successive mission will further us in our journey by 10- or 100-fold increases in resolution, step by step as we approach our goal of zooming in a million times closer. And each stop along the way will bring us new understandings of the nature of matter and energy.

GLAST is a gamma-ray observatory mission that will observe jets of particles that shoot away in opposite regions from a supermassive black hole at near the speed of light. We do not fully understand how a black hole, which is known for pulling matter in, can generate high-speed jets that stretch out for billions of miles. Galaxies that harbor black holes with a jet aimed in our direction are called blazars, as opposed to quasars, which have their jets aimed in other directions. GLAST, up to 50 times more sensitive than previous gamma-ray observatories, will stare down the barrel of these jets to unlock the mechanism of how the enigmatic jets form. The Constellation-X mission will probe the inner disk of matter swirling into a black hole, using spectroscopy to journey 1,000 times closer to a black hole than any other mission before it. With such resolution, Constellation-X will be able to measure the mass and spin of black holes, two key properties. This X-ray mission will also map the distortions of space-time predicted by Einstein. Constellation-X draws its superior resolution by pooling the resources of four X-ray satellites orbiting in unison into one massive X-ray telescope. The ARISE mission will produce radio-wave images from the base of supermassive black hole jets with resolution 100,000 times sharper than Hubble. Such unprecedented resolution can reveal how black holes are fed and how jets are created. ARISE will attain this resolution through interferometry. This technique is used today with land-based radio telescopes. Smaller radio telescopes spread out on land -- perhaps one mile apart -- can work together to generate a single, huge radio telescope with the collecting power of a one-mile radio dish. ARISE will utilize one large radio telescope in space with many other radio telescopes on Earth, bringing what is now a land-based technology to new heights
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New NASA Satellite to Study Black Hole Birth and Gamma Ray Bursts


The Swift observatory comprises three telescopes, which work in tandem to provide rapid identification and multi- wavelength follow-up of GRBs and their afterglows. Within 20 to 75 seconds of a detected GRB, the observatory will rotate autonomously, so the onboard X-ray and optical telescopes can view the burst. The afterglows will be monitored over their durations, and the data will be rapidly released to the public.


See:
  • Longitudinal and Transverse Information about the Energy Deposition Pattern


  • The Calorimetric View?