1. Masers from the Early Universe
Evgeniya Kravchenko, PRAO, Russia
Paul Coster, Swinburne, Australia
Sabrina Milia, Uni. Cagliari, Italy
Mahadevappa S. R. T. M. Uni, India

2. Maser Introduction
Microwave Amplification by Stimulated Emission of Radiation.
Absorb energy and produce a narrow frequency emission.
Electrons are pumped to a higher state and are triggered to return to their lower energy state by radiation of a specific frequency.

3. Water Maser Transition

4. Kinds of Maser Jet Maser Disk Maser
Single Broader emission feature in spectrum
Disk Maser
Multiple narrower emission feature.
Evidence of Rotation via doppler shifting in spectral lines

5. Object Introduction MG
Redshift 2.64
Radio Loud Quasar Type 2

6. Observations Arecibo 300m antenna C-high reciever, 6.1 GHz
Wideband Arecibo Pulsar Processor
100 MHz bandwidth
VLA calibrator
2.6 hours on target
0.4 hours on the reference source
2 polarizations
rms noise 0.3 mJy/channel
2048 channel per polarization
Velocity resolution 2.4 km/s

7. Calibration and data reduction
IDLDE pocket
Initial data
Removing baseline

8. Summarizing over 2 polarizations
Rebinning from 2048 to 205 channels

9. 2048

10. 2048
1024

11. 2048
1024
512

12. 2048
1024
512
256

13. 2048
RMS noise
256

14. Lensing contrubutiuon
Gravitational lensing improved the brightness of the the object 35 times.
Considering the low brightness with the lensing effect, the Maser would be effectively unobservable without the presence of the foreground lensing galaxy.

15. Knowledge of the Maser Water vapor maser
Most distant Maser ever detected (prev. 0.66)
Parameter
Effelsberg
EVLA
Arecibo
Units
Velocity
279+-8
km s-1
Line Width
40+-12
70+-27
78+-7
Line Peak
mJy
Integrated profile
97+-14
mJy km s-1
Luminosity Lo
Corrected Luminosity
17 000