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WikiSysopRadio am 13. Januar 2023 um 20:45 Uhr

2023-01-13T20:45:01Z

← Nächstältere Version		Version vom 13. Januar 2023, 22:45 Uhr
Zeile 48:		Zeile 48:
	<math>d=a-y</math>,		<math>d=a-y</math>,
	substituting /3 we get after all the desired distance		substituting /3 we get after all the desired distance
	<math>d=R_0 \cos l–\sqrt{r^2-R_0^2 \sin^2 l}</math> /4		<math>d=R_0 \cos l-\sqrt{r^2-R_0^2 \sin^2 l}</math> /4

	This procedure I applied to the regions 1 to 5 in fig.2, every 10 deg of longitude l. The so calculated distances S – H plotted for 20 to 220 deg give the fig.7 with the results:		This procedure I applied to the regions 1 to 5 in fig.2, every 10 deg of longitude l. The so calculated distances S – H plotted for 20 to 220 deg give the fig.7 with the results:

Ulli am 12. Oktober 2009 um 08:07 Uhr

2009-10-12T08:07:25Z

← Nächstältere Version		Version vom 12. Oktober 2009, 10:07 Uhr
Zeile 17:		Zeile 17:
	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC.		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC.
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|middle\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz

Ulli am 12. Oktober 2009 um 07:51 Uhr

2009-10-12T07:51:13Z

Ulli am 12. Oktober 2009 um 07:48 Uhr

2009-10-12T07:48:50Z

← Nächstältere Version		Version vom 12. Oktober 2009, 09:48 Uhr
Zeile 15:		Zeile 15:
	(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!		(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!

	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, geometric relations]]		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|left\|Fig. 3-4, geometric relations]]
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	[[Datei:Fig 5-7.jpg\|thumb~~\|left~~\|Fig 5-7, geometric relations]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		[[Datei:Fig 5-7.jpg\|thumb\|Fig 5-7, geometric relations]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz

Ulli am 12. Oktober 2009 um 07:20 Uhr

2009-10-12T07:20:31Z

← Nächstältere Version		Version vom 12. Oktober 2009, 09:20 Uhr
Zeile 15:		Zeile 15:
	(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!		(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!

	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, ~~Erklärungen siehe Text~~]]		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, geometric relations]]
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, ~~Erklärungen siehe Text~~]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 ~~Erklärungen siehe Text~~]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, geometric relations]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz

Ulli am 12. Oktober 2009 um 07:16 Uhr

2009-10-12T07:16:44Z

← Nächstältere Version		Version vom 12. Oktober 2009, 09:16 Uhr
Zeile 15:		Zeile 15:
	(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!		(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!

	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, Erklärungen siehe Text]]		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, Erklärungen siehe Text]]
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula

Ulli am 12. Oktober 2009 um 07:04 Uhr

2009-10-12T07:04:43Z

← Nächstältere Version		Version vom 12. Oktober 2009, 09:04 Uhr
Zeile 123:		Zeile 123:

	/4/ Lankeit, E.: Dynamic Solar Spectra, Part 2 Equipment, ERAC Newsletter 23, October 2002		/4/ Lankeit, E.: Dynamic Solar Spectra, Part 2 Equipment, ERAC Newsletter 23, October 2002


			'''Readings from autor''' Rückfrage ergibt: verwendet wurde ein linearer Detektor, der Anstieg betrug etwa 3dB. Ich will dazu noch die Kaskadierung der Verstärker hinsichtlich Rauschzahl und Gewinn (IIP3 hier unwichtig) für seine und unsere Anlage bringen. --[[Benutzer:Ulli\|Ulli]] 07:04, 12. Okt. 2009 (UTC)

Ulli am 10. Oktober 2009 um 17:11 Uhr

2009-10-10T17:11:55Z

← Nächstältere Version		Version vom 10. Oktober 2009, 19:11 Uhr
Zeile 20:		Zeile 20:
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz
	So v=100 km/s corresponds to <math>\triangle</math><math>\nu</math>~470 KHz.Such a survey needs some days of observation (sometimes I have to work a little bit to feed my family!), but the error originating in the changing position of the earth is neclectable in fig.2. These diagrams you can find e.g. in /4/ Verschuur, Kellermann, naturally in an much higher resolution. That contourplot is not a picture of our galaxy, but shows regions of the milky way with coherent velocities.		So v=100 km/s corresponds to <math>\triangle</math><math>\nu</math>~470 KHz.Such a survey needs some days of observation (sometimes I have to work a little bit to feed my family!), but the error originating in the changing position of the earth is neclectable in fig.2. These diagrams you can find e.g. in /4/ Verschuur, Kellermann, naturally in an much higher resolution. That contourplot is '''not''' a picture of our galaxy, but shows regions of the milky way with coherent velocities.

	''3 Estimate of the position of the HI-clouds''		''3 Estimate of the position of the HI-clouds''

Ulli am 10. Oktober 2009 um 16:41 Uhr

2009-10-10T16:41:45Z

← Nächstältere Version		Version vom 10. Oktober 2009, 18:41 Uhr
Zeile 18:		Zeile 18:
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz
	So v=100 km/s corresponds to <math>\triangle</math><math>\nu</math>~470 KHz.Such a survey needs some days of observation (sometimes I have to work a little bit to feed my family!), but the error originating in the changing position of the earth is neclectable in fig.2. These diagrams you can find e.g. in /4/ Verschuur, Kellermann, naturally in an much higher resolution. That contourplot is not a picture of our galaxy, but shows regions of the milky way with coherent velocities.		So v=100 km/s corresponds to <math>\triangle</math><math>\nu</math>~470 KHz.Such a survey needs some days of observation (sometimes I have to work a little bit to feed my family!), but the error originating in the changing position of the earth is neclectable in fig.2. These diagrams you can find e.g. in /4/ Verschuur, Kellermann, naturally in an much higher resolution. That contourplot is not a picture of our galaxy, but shows regions of the milky way with coherent velocities.

Ulli am 10. Oktober 2009 um 09:10 Uhr

2009-10-10T09:10:35Z

← Nächstältere Version		Version vom 10. Oktober 2009, 11:10 Uhr
Zeile 17:		Zeile 17:
	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, Erklärungen siehe Text]]		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. [[Datei:Fig 3-4.jpg\|thumb\|Fig. 3-7, Erklärungen siehe Text]]
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	[[Datei:Fig 5-7.jpg\|thumb\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb~~\|left~~\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		[[Datei:Fig 5-7.jpg\|thumb\|left\|Fig 5-7, Erklärungen siehe Text]]Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 Erklärungen siehe Text]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz

← Nächstältere Version		Version vom 12. Oktober 2009, 09:51 Uhr
Zeile 15:		Zeile 15:
	(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!		(that are 3 lines, but they took 1 year, details see below). After that trouble I am now able to record strong HI-profiles – thanks to Mr. OSER!

	''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC. ~~[[Datei:Fig 3-4.jpg\|thumb\|left\|Fig. 3-4, geometric relations]]~~		''2 Results: HI-profiles of the galactic plane'' Fig.1 [[Bild:Panorama.jpg\|thumb\|Fig.1 HI-profiles]] shows a row of records, taken at the particular galactic longitude at galactic latitude b=0. The ordinate is calibrated in volt, because an absolute calibration of my station is missing until now, but a coarse estimation gives 1V~20K of emission brightness temperature. The x-axis is the deviation from the HI-restfrequency in MHz, rest frequency <math>\nu</math>=1420.406 MHz. The IF-bandwidth is 30 KHz, integration time of the DC-amp is 2s. Frequency distance of reading is 20 KHz, so one scan takes 71 measurements, done by the PC.
	At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.		At l=40° e.g. we have some approaching clouds at low level, that are not resolved by my small antenna ,two escaping with high intensity and one nearly at rest relative to the earth.
	~~[[Datei:Fig 5-7.jpg\|thumb\|Fig 5-7, geometric relations]]~~Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula		Taking such records every 5° of galactic longitude and arranging the data by a specialized program, I obtain diagrams like Fig.2 [[Datei:Contour1 2.jpg\|thumb\|Fig.2 contourplot]]: it is a contourplot, that shows in the z-axis colour encoded the intensity over the velocity of the HI-clouds for the galactic plane, that can be seen from my station. The x-axis is calibrated in km/s, corresponding to the velocity of approach (-) or recession (+) of the observed hydrogen cloud following the formula
	<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.		<math>v=c \triangle \nu/\nu</math> see /3/ Kraus, page 8-88.
	<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz		<math>\nu</math>: rest frequency, <math>\nu</math>=1420.406 MHz
Zeile 23:		Zeile 23:

	''3 Estimate of the position of the HI-clouds''		''3 Estimate of the position of the HI-clouds''
	Most interesting is now the answer to the question: where are these hydrogen clouds and how far can I see with my tiny parabola? To solve this problem I had to warm up old knowledge of geometry, help I found in /3/ Krauss and more detailed in /5/Carroll. The basic idea behind the following calculation goes back to van de Hulst, Muller and Oort in the middle of the last century: From different measurements we know the curve of differential rotation of the milky way galaxy, so tangential velocity at a point as function of the distance of this point to the galactic center. For the points in fig.2 we have the radial velocity relative to the earth or sun. Using the geometry of the system galactic center, sun and HI-cloud it is possible , to calculate the angular velocity of the cloud relative to the galactic center and with the above mentioned differential rotation curve we can estimate the distance of the cloud to the galactic center and at least we can calculate the distance to the sun.		Most interesting is now the answer to the question: where are these hydrogen clouds and how far can I see with my tiny parabola? To solve this problem I had to warm up old knowledge of geometry, help I found in /3/ Krauss and more detailed in /5/Carroll. The basic idea behind the following calculation goes back to van de Hulst, Muller and Oort in the middle of the last century: From different measurements we know the curve of differential rotation of the milky way galaxy, so tangential velocity at a point as function of the distance of this point to the galactic center. For the points in fig.2 we have the radial velocity relative to the earth or sun. Using the geometry of the system galactic center, sun and HI-cloud it is possible , to calculate the angular velocity of the cloud relative to the galactic center and with the above mentioned differential rotation curve we can estimate the distance of the cloud to the galactic center and at least we can calculate the distance to the sun. [[Datei:Fig 3-4.jpg\|thumb\|left\|Fig. 3-4, geometric relations]]
	Hoping, that other amateur observers will measure HI-profiles I’ll derivate here the formulas I used, so we could compare our results.		Hoping, that other amateur observers will measure HI-profiles I’ll derivate here the formulas I used, so we could compare our results.

	The rotation curve of the milky way galaxy: As basic data I used the values of rotation speed in /5/ figure 22.27, my used mean values are sketched in fig.3. From this I derived the angular velocity <math>\omega</math> as function of distance to the galactic center in fig.4 <math>\omega=\Theta/R</math>; <math>\omega</math> in rad/s; R: kpc 1kpc=3.08*10<math>^1</math><math>^6</math> km. For values R>8 kpc the error bars in fig.3 grow extremely. For the sun the IAU standard values <math>R_0</math> = 8.5 kpc and <math>\Theta_0</math> = 220 km/s are used. A similar curve to fig.4 can be found e.g. in /3/ fig. 8-63.		The rotation curve of the milky way galaxy: As basic data I used the values of rotation speed in /5/ figure 22.27, my used mean values are sketched in fig.3. From this I derived the angular velocity <math>\omega</math> as function of distance to the galactic center in fig.4 <math>\omega=\Theta/R</math>; <math>\omega</math> in rad/s; R: kpc 1kpc=3.08*10<math>^1</math><math>^6</math> km. For values R>8 kpc the error bars in fig.3 grow extremely. For the sun the IAU standard values <math>R_0</math> = 8.5 kpc and <math>\Theta_0</math> = 220 km/s are used. A similar curve to fig.4 can be found e.g. in /3/ fig. 8-63.

	Angular velocity of the HI-cloud: In fig.5 means: C the galactic center, S the Sun, H the investigated hydrogen cloud, l is the galactic longitude (earlier l <math>^I</math> <math>^I</math>), <math>\omega_0</math> and <math>\Theta_0</math> show the direction of the rotation of the sun about the galactic center. From fig.5 we find the relative radial velocity of H:		Angular velocity of the HI-cloud: In fig.5 means: C the galactic center, S the Sun, H the investigated hydrogen cloud, l is the galactic longitude (earlier l <math>^I</math> <math>^I</math>), <math>\omega_0</math> and <math>\Theta_0</math> show the direction of the rotation of the sun about the galactic center. From fig.5 we find the relative radial velocity of H: [[Datei:Fig 5-7.jpg\|thumb\|Fig 5-7, geometric relations]]
	<math>v_r=\Theta \cos \alpha-\Theta_0 \sin l</math>		<math>v_r=\Theta \cos \alpha-\Theta_0 \sin l</math>
	where <math>\Theta_0</math>sinl is the angular velocity of the sun. Defining the angular velocity as		where <math>\Theta_0</math>sinl is the angular velocity of the sun. Defining the angular velocity as