Until development of this webpage is completed I will simply place here a few graphics that illustrate the configuration of my radio telescope for neutral hydrogen line observations at 1420.4 MHz and some of the initial results of measurements at and near 1420.4 MHz in the galactic plane of the Milky Way galaxy and of some relatively strong radio sources that are sometimes monitored by EMEers at 1296 MHz during their receive system checks. I will be happy to discuss via email any questions you may have regarding this preliminary H I line work.

Presently, the focus at K5SO is in performing calibrations of the receive system at 1420 MHz and collecting data there with an immediate primary goal of independently deducing the rotation curve of the Milky Way galaxy using the observed Doppler shifts in the measurements. Later efforts may involve attempts to combine this telescope with radio telescopes at K0YW, N0OY, K1RQG, K0WOW, and WD5AGO to form a very long baseline telescope network of radio telescopes in order to image particular sections of the sky at 1420 MHz with high spatial resolution.



One of the objectives of the neutral hydrogen line observations at 1420.4 MHz is to attempt to determine independently the relative motion of the Earth and our solar system with respect to the other components of our galaxy, the Milky Way. As an initial approach toward this end, measurements were made centered on 1420.4 MHz with a span of 1 MHz about that center frequency (i.e., from 1419.9 MHz to 1420.9 MHz) while pointing the dish at various longitudes in the galactic plane (i.e., galactic latitude of zero degrees). Our solar system is located within the Milky Way galaxy approximately as shown in the diagram below. The diagram shows how the galactic coordinate system is oriented in the Milky Way galaxy. Note that the galactic coordinate system is centered on our solar system with zero degrees longitude directed toward the galactic center.

Ref: above image was obtained from http://www.thinkastronomy.com/M13/Manual/common/galactic_coords.html without permission.

In order to track specific galactic longitude/latitude directions with a radio telescope it is necessary to convert galactic longitude/latitude coordinates into Right Ascension/Declination equatorial coordinates and, of course, ultimately to convert RA/Decl coordinates into Az/El coordinates for the particular telescope location being used and the time of day of the observation. The conversions to equatorial coordinates for galactic longitudes within the Milky Way galactic plane, i.e., at zero degrees galactic latitude, are shown below. Note that some galactic longitudes are not visible from my New Mexico location.


The following plot is a summary of measurements taken at a variety of longitudes at zero-degree latitude, in the galactic plane of the Milky Way at 1420.4 MHz. Peaks in the RED portions of the curves indicate neutral hydrogen gas that has a radial component of velocity that is receding from us and peaks in the BLUE portions of the curves indicate neutral hydrogen gas that has a radial component of velocity that is approaching us. Each curve is a result of signal averaging for a period of 5 minutes at the specific longitude/latitude direction as the dish tracked the movement of that galactic direction through the sky during the measurement.

Note in the plot above that there is a clear systematic shift of the frequency positions of the peaks due to neutral hydrogen gas as the direction of observation is changed in the galactic plane. Notice in particular that at zero degrees longitude (i.e., toward galactic center) the relative motion of the solar system is toward the galactic center since the neutral hydrogen line is blue shifted, indicating that the relative velocity of the solar system has a radial component toward that gas. Also note that neutral hydrogen located in the opposite direction, i.e., away from the galactic center at 180 degrees longitude, is red shifted. The red shift indicates that the solar system has a radial relative velocity component that corresponds to the solar system receding from gas located in the direction from us opposite to galactic center. A velocity scale is also shown on the plot for reference. Velocities associated with Doppler-shifted frequencies are calculated by

v = c (fo-f)/fo,

where v is the radial component of the relative velocity between the observer and the source, c is the speed of light (3 x 10^8 m/s), fo-f is the Doppler shift amount, and fo is the unshifted frequency. By arbitrary convention and agreement among astronomers, Doppler-shifted velocity components in directions that are away from the observer are designated as positive whereas Doppler-shifted velocity components that are directed toward the observer are designated as negative.

Analyses of the magnitudes of the relative velocities of hydrogen gas in the various directions will be presented later in terms of an overall view of the relative motion of the solar system within the Milky Way galaxy. These results will then be combined with results of observations that are directed out of the galactic plane in an effort to obtain information that is relevant to understanding something about the motion of the Milky Way galaxy itself relative to extragalactic radio sources and the relative motion of gas residing in the halo of the Milky Way galaxy.



The following graphs are 'signal-averaged-intensity versus frequency' plots obtained directly from the SDR-14 using the SpectraVue program in its normal (default, frequency domain) mode with a 1 MHz bandwith centered on 1420.4 MHz and an approximate 10-minute acquisition time for each. The data were initially saved using the spreadsheet output format option of the SDR-14/SpectraVue then imported into MS Excel as a text file. The data were plotted and annotated using the Chart Wizard feature in Excel. The resulting chart was then printed to file in PDF format and converted into JPEG format using Adobe Photoshop Elements for posting on the website as a JPEG image.

Neutral hydrogen at rest (in the radial direction) with respect to us would appear as a peak precisely centered on the dashed red line at 1420.40575 MHz. Peaks appearing higher in frequency than the red dashed line are due to hydrogen gas approaching us radially and peaks appearing a frequencies lower than the red dashed line are due to hydrogen gas receding from us radially. No information is available in these data with respect to velocity components of the gas that may be perpendicular to the line of sight. The H I line signals shown in these graphs are on top of, i.e., combined with, the broad-band background radiation from the sourcces. That is, at 1296 MHz for example, one would see only broadband radiation from these sources without the H I line peaks shown below. No calibration noise pulses were used during the collection of these particular HI line data. The noise pulses will be used in later measurements when the system is configured as a radiometer incorporating PIN diode rf switching and a synchronous, lock-in amplifier detector (not shown in the configuration diagram above) to obtain absolute power measurements of radio sources.