Balloon Mission


With the miniaturization of measuring equipments, ICSP has been able to lead the nation in making low-cost balloons as the vehicle to measure space radiations such as cosmic rays, Solar X-rays and Gamma-rays from a height of 40 kilometers. Equipments are custom made in house to reduce the cost. So far, 42 Missions have been performed

There are several advantages of using weather balloons as opposed to conventional large sized balloons. A mission with a weather balloon is most certainly less expensive (by a factor of say 100 or so). It is possible to launch them in a matter of hour’s notice. Thus solar flares or flares/outbursts in black hole binaries can be picked up easily. There is no need to have a canonical launching pad of ‘facility’ for small balloons and indeed they can be launched from anywhere (including boats) as long as predicted trajectories ensure that they may be recovered at desirable places









Payload of Geiger-M¨uller counter in D13 mission

Complete payload of Geiger-M¨uller counter in D10 mission

Payload of "Si-PIN" X-ray detector in D11 mission

Telescope payload in D31 mission

Meteoric dust collector payload in D18 mission

X-ray payload in D06 mission


Payloads / Detectors new:

5” phoswich detector along with the  tantalum collimator and data  processing system

 payload design for experiment

Sectional view of the same detector from the visualization of simulation of the detector


Real Time Tracking of D20 Balloon Mission on google earth and google map

Real time Velocity and altitude monitoring system of D20

Wind velocity plot of balloon

Variation of temperature with height of D30 mission

Variation of temperature with height of D30 mission

Aultitude variation with time in D20 mission


Variation of tilt angle from accelerometer of D26

Coverage of balloon in D20 of the X-ray sky in Galactic coordinate and Ait-off projection

Variation of tilt angle from accelerometer of D26 and the azimuth of Sun with +- 5

Muon and Cosmic Ray from Balloon: 

Rate of cosmic ray counts per minute plotted against time in minutes after liftoff in D13 Mission

Muon detection in Dignity 17 mission. The counts per minute is shown as a function of time since liftoff.

The cosmic rays (Green), pressure (blue), temperature (pink) and the Accelerometer (red) data for a long duration flight (Dignity 26) which lasted 12 hours.


Muon detection as a function of time since liftoff. This is the result of Dignity 19 mission (21 Nov. 2011). The peak occurs at around 15km, same as in cosmic ray observation, though the peak is a bit broader. There were no muon after about 30km.

Cosmic ray profiles (60 second average) in Dignity 27 and 28 missions by a bicron detector having a PMT and a NaI crystal. At our latitude the Pfotzer maximum is at ~15 km. The minimum caused by the competition of ground radio activity and Cosmic rays is marked


Solar Photons and solar flare from Balloon:



A short duration flare observed in D28 mission. Count rates in 50-100 channels (~ 20-25keV) is plotted. For comparison we superposed RHESSI flux data in 6-25 keV range. In the inset, we show the flare spectrum in log-log scale which is clearly a power-law spectrum. There is some absorption due to atmosphere in the lower energy

Dynamical spectrum of a weak solar flare as a function of height as observed by D40 mission on 18thMay, 2013. The data is plotted for 42keV to 72keV to avoid contaminations from the calibrators



Dynamical spectra of the observed data, showing clearly the flares and their time-resolved spectra. Note the progressive softening of the detection limit of the spectra with time in D33 mission

Alarming rate of high energy photons detected at lower altitudes due to an X1 flare occurred at 1:30 UT, 15thMay, 2013. in D38 mission

 GRB(Gamma Ray Burst) detected from Balloon:

spick-lc sp


The lightcurve (upper left), spectrum (upper right) and dynamic spectrum (bottom) of a Gamma Ray Burst detected by our detector in D45 mission at a hight of ~34 km at 7:49 UT, 24th October, 2013.

Location of the Gamma ray Burst detected by our  detector in D45 mission. Details of GRB 131024C are in this list

Simulations and other results during balloon borne experiments:

change in atmospheric parameters to describe the atmospheric model used in the simulation.

representation of geomagnetic field line distribution for particular solar condition.

Sky image as seen by the detector during the detection of the Crab (position pointed by the red dot).

Spatial distribution of the proton flux at the satellite height of ~ 400 km.

Secondary cosmic-ray counts variation throughout the atmosphere during solar maximum (10/2013) and solar minimum (05/2016) activity.

Stress analysis of the payload part under specific launch condition.

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