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SUMMARY:Observations of the 22GHz Water maser in the source Orion KL
DTSTART;VALUE=DATE-TIME:20110714T150000Z
DTEND;VALUE=DATE-TIME:20110714T170000Z
DTSTAMP;VALUE=DATE-TIME:20260715T050559Z
UID:indico-contribution-5110@events.saip.org.za
DESCRIPTION:Speakers: Sunelle Otto (HartRAO)\nStars are believed to be for
 med from massive stable gas clouds\, which under enough perturbation will 
 collapse to form a protostar. The protostar evolves to form a star by accr
 eting matter until the fusion is initiated in the dense core. Surrounding 
 these protostars are ionized hydrogen (HII) regions and molecule species w
 here masing occurs. MASER is an acronym for Microwave Amplification by Sti
 mulated Emission of Radiation. It is here that Water masers are also found
 . Amongst the sources of water masers\,  is the Orion KL source region. Fl
 ares in this region from the 1.35cm water maser emission line occurred in 
 1984\, with the second flare in 1998 and again this year (2011) there have
  been reports of the flare. The flare is very intense\,  increasing its fl
 ux density from around hundreds to millions of janskies. This poster will 
 show the summary of observations made by the Hartebeesthoek Radio Astronom
 y Observatory (HartRAO) telescope for the water maser in the Orion KL sour
 ce region as well as the calibration method. Jupiter is used as the calibr
 ator source\, while the absorption by atmospheric water vapour must also b
 e allowed for. This uses estimates based on atmospheric temperature and hu
 mdity or can also be based on the time delay of GPS signals\, corrected fo
 r barometric pressure.\n\nhttps://events.saip.org.za/event/7/contributions
 /5110/
LOCATION: Asteria
URL:https://events.saip.org.za/event/7/contributions/5110/
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