MEXART IPS observations. Instrument status report
Americo Gonzalez-Esparza, Ernesto Aguilar-Rodriguez, Julio Mejia-Ambriz, Esmeralda Romero-Hernandez, Oyuki Chang-Martinez, Victor De la Luz, Pedro Corona-Romero,
Armando Carrillo, Ernesto Andrade, Pablo Villanueva
SCiESMEX, Instituto de Geofisica, UNAM
Mexican Array Radio Telescope
S I LV I A B R AV O ( 1 9 4 5 - 2 0 0 0 )
• system configuration
• process to reach full operation
• Mexican Space Weather Service (SCiESMEX)
• IPS data and solar wind modeling as a space weather product
Talk outline
Romero-Hernandez et al., 2015
Romero-Hernandez et al., 2015
Romero-Hernandez et al., 2015
Romero-Hernandez et al., 2015
1
0.1
1.0
MEXART radiosource 3C273 2014
1Radial distance [UA]
0.1
1.0Scintillation index m
0.4 0.5 0.6 0.7 0.8 0.9
Power-law index : -2.12
1
0.1
1.0
MEXART radiosource 3C298 2014
1Radial distance [UA]
0.1
1.0
Scintillation index m
0.4 0.5 0.6 0.7 0.8 0.9
Power-law index : -2.68
power spectra of IPS observations and model fits
0.1 1.0frequency (Hz)
10−2
10−1
100
norm
aliz
ed p
ower
3C298α = 3.8size = 0.30
ε = ( AU) 31.30 0.52AR = 1.0χ2 = 0.33
date = / / 2014 11 13
V = +/− km/s 585 55
obsfit
power spectra of IPS observations and model fits
0.1 1.0frequency (Hz)
10−2
10−1
100
norm
aliz
ed p
ower
3C273α = 3.8size = 0.40
ε = ( AU) 50.70 0.77AR = 1.0χ2 = 0.12
date = / / 2014 11 13
V = +/− km/s 425 30
obsfit
Chang-Martinez et al., 2015
MEXART radiosource 3C298
10 20 30 40 50 60 70Elongation (degrees)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
m index
maximum value at : 21.2
Chang-Martinez et al., 2015
0.1
0.5
1
1.5
2
g-level
0.34 AU
0.64 AU
0.86 AU
0.98 AU
200
400
600
800
/ /2014 6 11
Chang-Martinez et al., 2015
200
300
400
500
600
700
800
Velocity(km/s)
0.34 AU
0.64 AU
0.86 AU
0.98 AU
200
400
600
800
/ /2014 6 11
Chang-Martinez et al., 2015
https://www.wmo-sat.info/product-access-guide/space-weather-product-portal
https://www.wmo-sat.info/product-access-guide/domain/space
Conclusions
• MEXART is a fully dedicated array to perform IPS observations
• By the end of 2015 the array will operate, for the first time, with the full antenna
• We will have a new receiver with 4 channels and 4MHz bandwidth
• We expect a significant improvement in the instrument’s response. We will increment the number of radio sources and the signal to noise ratio
• We are developing the methodology to obtain solar wind parameters in near real time
• MEXART observations and tomographic modeling as a space weather product
Romero-Hernandez et al., 2015
