Balloon-borne X-ray observations of the southern sky

This thesis presents results of the southern X-ray sky obtained from flights by the University of Aclelaicle b'rlloorr-borne observers during the period 1963-69. Crrì¡ -2 Is also exa¡ninecl in cl-etail for the ascension phases of the various fJ-igh'bs.

Hillier, D. Sco'üt and merrbers of the Department of Supply BaLIoon

Institute of Technology¡ of trvo balloons used for the flights MIL-I-69 and. These coordinates are believed to be the most accurate observations to date.

Other specìts,cu}a,r1y v&riobLe source of C€n X-4, have been observed. 1969 ai intersity levcl comparable to that of sco)n-1. The basic ¡rtrysica,l processes that produce most of the observed cosmic T'-tay fo'oons are well elucidated.

Isotropic X-ray

rays f,ar:-more copiously ir: their very ecrrly life as supernovere

Silk (1968) considered cosonic factors. The l-ray intensity of normal grlaxies is believed to evolve with time in a manner analogous to the raclio emission as indicated by a radio source. Compton scattering in 64 roclio galaxies of 30 P. blackbody photons by the radio-emitting electrons were independently proposed as a magic mechanism by Berga, mini et al. fgeZ) and Brecher ¿ì, and Morrison.

April 26 r+heBm

I{II-1-68 MÍL-z-68

In this chapter, a description of the experiment's payload will be based on the technical aspects of bias torrard. The moment of inertia of the balloon results, ecl in the payload prevailing at, ed in azi¡nuth.

Fig: 2.I Total system block cliagram of ttre llniversity of Ad-elaicle balloon-borne X-ray astronomy experimen'b.

Here I will just point out that whereds ebmponents (¡) and' (c) will eontriüute occording to the solicl angle of the telescope concerned',

Sl¡stem stabílity

Three other distinctive NAND gate input signals come from the collinator, the well, and the phoswich and scintillators, respectively. Fig:2.8 Block diagram of the height-to-time converter of the l6-channel pulse height analyzer.

Fig: 2-7 Block schematic of i;he active telescope r6-charrnel pulse height analyser.

In any case, the flight system consists of one ii-D converter per magnetometer and a battery supply whose discharge during flight results in a small variation in the non-finally stabilized 6.3 volts. The temperature effects are not significant under flight conditions. The thermal insulation around the psyload provides internal insulation. Temperatures remain at 5oC. The Schonsted-t units are measured in temperature between 1 ZOoC 'û'nd'. reveal cr, negligible temperature coefficient. knock in tenpercture, I-Iolrever, the. electronics package with the À.Ð-converters never falls below +15oC during a flight. will have an effect on the accuracy of the. Therefore, the changes in the system should be insignificant in terms of the reliable operation of the system. The correction must be applied to cosmic X-roy fluxes due to absorption in the surrounding atmosphere are highly dependent.

1968). ,1r.241 is useC. anil unlik, PI2LO, its long haif-Iife of 460 yo!ìïs cbviater any necessity for regulnr reirl;'aeenent anå frequont, i-lrgtrunent recalibr¿rtion' Its r:output is o . rectc-ngul.¿r wirvefôrmrthe rei:eti.+,ionr rr¿te of rrhjch is ¡' me¿lsure of the at,rnospheric .liensitrr. TL¡e least significarù{2o) of the 10 bitg is lost by inserting the pori+,y bit, r,rhich is either a zero of a one c{depending on what. 2.LO.2 T]ne D.rta Storoøe unit (DSU) . ÐSU cont:¡ins o lO-bit accumulation registers for each type of data to be secured.

Fig: 2.11 Effects of battery runclown on the magnetometer system'

78 MHU

7O MHÉ

P Print¿r

Between l0 ond, lfJO KeV its exact eneïÍr,r rlopeu'J.ence is complex oving to irresen?e of Ii auå L shell Zibsorption ec-lges where li(g) increases sh.arpl¡f.

5 Figure 3.1 shovs the Índ.ivitluol co-efficients anå the total mass

Summary

The effect described above Ð,11 ¿.determine the final form of the output pulse height

These matters are not discussed with respect to the u¡ÉoId'in¡; of any cosmic )i-rery source spectrum ¡J(E)di¡ of observêd .jth chg.n¡re1.

This is the ratio of the count, the rate that can be observed by a, Peffect rletectcrr (i.". no inflow absorption, LOú/" photon detection efficiency, . no K escape, energy: fi resolution 1+ o) at the top of the atmosphere, according to that observation by our detector. It is found that Fj is the function of the spectral shape of N(E)¿E as a result of the need to integrate. The most important calibration measurement is that of the detector energy response. This involves (a) determining the nearly linear relationship between the output pulse height and the photon energy. U) Tuesday energy resolution {U) of the detector.

Íod,ine K escape correction in our spectral analysis, no detection of K juice photons (29.2 IíeV) from the central crystal, not detector. Consequently, the coilimitation threshold was set at 4O KeV. the background,l resultin¿; frontr compton scattering of photos. from ttre collimator or skin} in the centraì

E¡IERGY KAV

Enerpv calibration

It is clear that the triangular shape with ø = 8.9o fits the rlata better than the iclealizt-'d. a) Imperfect geometry of the boreholes; cylindrical holes. A number of important laboratory tests are performed on the payload to ensure its proper operation in enemy territory. This test is difficult to properly control since the flight configuration of the antennas and free space payload is only approximately replicated on the ground. .

Tleis:;a;rlc'ad. has tr)roveu very pronc to ;:ðF effects, especially in the very fast, hí6'h ¿1ain phoswich circuitr¡r. Since the direction of the pointing of the X-T"y telescopes is on essential experimental porameter, roagnetometers were used. It is tt¡ons advantageous to be alfare of the scale of nn,¿potic activity during a fl¡-¡ht , as it is relevant to the accuracy of X-ray source position determinations, this section contains calculations describing the effect on the azimuth neosuremeut of deviations from the nominal horizontal orlentotit of the two crossed.

Table 4.2¡ B.M.tl. rneosurements at $Íildura.

4.2.r=ABCX

I'Iunerical conrÐutotir-'ns

One calculation is for a height at zero in Milcara and for an accurately leveled wage, that is, it determines the preferred light libreration that has been performed. placing it on a regular horizontal platform will cause it to rot. by all asimuth an¿íles. Other calculations included; is the first path. performec} for a poorly leveled Fa)¡loaC, i.e. the cut wells can be optimal due to sinusoids and. the azi¡r¡üths so rJ.e+,ornrineô will correspond to the true azÍmuth up to^-4åo. 34 ;).

Table 4.4¿ Cl¡enges irr sinusoitl characteristics for a modol fli¿iht'

The following effects contribute to the uncertainty in tbe. final azimuth m€o, securing any given time¡. These figures apply only to instïnda'l error and do not include the statistical uncertainty ossociatetì. r¿ith the cletectioo. Its resolution is approx. 0.7 degrees per bite. The calibration is produced for, or MIL-1-69 a^Eil l'fiIr-2-69 ore shorfl¡ in Figure 4.5, although neither is due to oalf¡¡¡actions of tbe orlentation syrteu, a¡rd.

OF ROTATING NULL MAGNETOMETER

AZIMUTH ËRRCIR €,

03060 Fig: 4.7

Any i::regularity or periotlic component, in magne{,oneter clata calibration with period.s other than 3600 must.

AZIMUTH, O

The Soectrr¡n of Norma ÏR-l

The zenith uncertainty of I +o . corresponds to the expected variation of the zenith angle during the period. of observation of about 1 hour" from a source in this region of the sþ. Inconsistencies between cliff-ferent observations also exist within the ScoïR-2 complex which currently consists of the Lockheetl grouper source L6 (Fisher et al. 1968), a source mentioned by L.ewin et al. It is essential to conduct X-ray astronomy studies effectively, and consequently also to understand the processes from the background.

Three clear sources contribute to the total number of backgrounds (.Brr) 'tstresc_opê r. u). Altitude d.epenclence or transition curve of total background level in energy renge 3T to 47 KøY for. Counting speed. increase as the balloon reaches the hovering height, for p sec Z€1O gr""*ir2 is due to the contribution^ U"o" of the cosmic scattered background, which becomes less and less weakened by the decreasing thickness of the air above it.

SLANT DEFTH

A piece of the atrnosphería background is then of value for this reason and also for the necessity to start the basic production processes. The attenuation I¿ of the exponential portion of the current rate transition curve was determined as a function of photon entry for four flights and^ for both the active autl gradetL shield telescopes. Comparison of attenuation lengths for c<¡unt rates. t) the active telescope NaI(TI) anti-collapse.once r¡ell (>BOKeV);.

These plots are typical examples of the three types of count rates as obtained. Desk overlap is observed between the attenuation lengths of the count, rates in the active telescope channel 3 and. telescope channel 2, covers approximately the same photon energy range. This serves to emphasize that caution should. in agreement with the results obtained using What is remarkable is the close coincidence of the attenuation lengths for G.S. 2 and the active well velocity. velocities of the active telescope, i.e. gt;8oKeY), the collimotor ()4otreV), ttre lower level diserioinator ()lOfeV), and. 34;) Lurr ttre {ìvoro,ge over all energy channels (except the lowest) of the attenuation lengths for the G S telescope Í¡e.

MIL- 2-69

The Trans.itioncurvemaxi (p-loOgm.cm-2)

Yet tJ¡Ís ruethod experiences the same difficulties as L comparisons and. the results are also somewhat endless. obtained on each flight is shown in Table 6.5. Fosses ¿i zenith an¡1re dependence. This is the case because of the empirical fact that the coarse lransfc¡rmation has been found to provide a good explanation of the obstlred numerical correlations. Gumparison of photon attenr¡atlon Lengths an¿L Pfotzer naxlmr¡m. heights with the corresponding waves of other ethnospheric. racllat,ions do not appear to be a reliable modhotl of detormination. the generic relationship between photons and the secondary cosmos.

This chapter is essentially a continuation of chapter 6. to examine the atnospheric azision curve. for p