AustralieFrV1, PascalFrancis, Curation, bibRecord, 004835

Ultra-Stable Very-Low Phase-Noise Signal Source for Very Long Baseline Interferometry Using a Cryocooled Sapphire Oscillator

Identifieur interne : 004835 ( PascalFrancis/Curation ); précédent : 004834; suivant : 004836

Ultra-Stable Very-Low Phase-Noise Signal Source for Very Long Baseline Interferometry Using a Cryocooled Sapphire Oscillator

Auteurs : Nitin R. Nand [Australie] ; John G. Hartnett [Australie] ; Eugene N. Ivanov [Australie] ; Giorgio Santarelli [France]

Source :

IEEE transactions on microwave theory and techniques [ 0018-9480 ] ; 2011.

RBID : Pascal:12-0043518

Descripteurs français

Pascal (Inist)
- Circuit faible bruit, Bruit phase, Source bruit, Radioastronomie, Oscillateur, Implémentation, Synthétiseur fréquence, Circuit numérique, Diviseur, Méthode directe, Synthétiseur numérique, Circuit accordable, Stabilité fréquence, Bande latérale unique, Fonction cohérence, Facteur mérite, Maser, Cryogénie, Température cryogénique, Composite ordre 2, Cohérence, Circuit intégré.

English descriptors

KwdEn :
- Coherence, Coherence function, Composite second order, Cryogenic temperature, Cryogenics, Digital circuit, Digital synthesizer, Direct method, Divider, Figure of merit, Frequency stability, Frequency synthesizer, Implementation, Integrated circuit, Low noise circuit, Maser, Noise source, Oscillator, Phase noise, Radio astronomy, Single sideband, Tunable circuit.

Abstract

The design and implementation of a novel frequency synthesizer based on low phase-noise digital dividers and a direct digital synthesizer is presented. The synthesis produces two low-noise accurate tunable signals at 10 and 100 MHz. We report the measured residual phase noise and frequency stability of the synthesizer and estimate the total frequency stability, which can be expected from the synthesizer seeded with a signal near 11.2 GHz from an ultra-stable cryocooled sapphire oscillator (cryoCSO). The synthesizer residual single-sideband phase noise, at 1-Hz offset, on 10- and 100-MHz signals was -135 and -130 dBc/Hz, respectively. The frequency stability contributions of these two signals was σ_y = 9 × 10^-15 and σ_y = 2.2 × 10^-15, respectively, at 1-s integration time. The Allan deviation of the total fractional frequency noise on the 10- and 100-MHz signals derived from the synthesizer with the cryoCSO may be estimated, respectively, as σ_y ≃ 5.2 × 10^-15τ^-1 + 3.6 × 10^-15τ^-1/2 + 4 × 10^-16 and σ_y ≃ 2 × 10^-15τ^-1/2 + 3 x 10-¹⁶, respectively, for 1 < r < 10⁴ s. We also calculate the coherence function (a figure of merit for very long baseline interferometry in radio astronomy) for observation frequencies of 100, 230, and 345 GHz, when using the cryoCSO and a hydrogen maser. The results show that the cryoCSO offers a significant advantage at frequencies above 100 GHz.

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A11	`01`	`1`		`@1 NAND (Nitin R.)`
A11	`02`	`1`		`@1 HARTNETT (John G.)`
A11	`03`	`1`		`@1 IVANOV (Eugene N.)`
A11	`04`	`1`		`@1 SANTARELLI (Giorgio)`
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C01	`01`		`ENG`	@0 The design and implementation of a novel frequency synthesizer based on low phase-noise digital dividers and a direct digital synthesizer is presented. The synthesis produces two low-noise accurate tunable signals at 10 and 100 MHz. We report the measured residual phase noise and frequency stability of the synthesizer and estimate the total frequency stability, which can be expected from the synthesizer seeded with a signal near 11.2 GHz from an ultra-stable cryocooled sapphire oscillator (cryoCSO). The synthesizer residual single-sideband phase noise, at 1-Hz offset, on 10- and 100-MHz signals was -135 and -130 dBc/Hz, respectively. The frequency stability contributions of these two signals was σ_y = 9 × 10^-15 and σ_y = 2.2 × 10^-15, respectively, at 1-s integration time. The Allan deviation of the total fractional frequency noise on the 10- and 100-MHz signals derived from the synthesizer with the cryoCSO may be estimated, respectively, as σ_y ≃ 5.2 × 10^-15τ^-1 + 3.6 × 10^-15τ^-1/2 + 4 × 10^-16 and σ_y ≃ 2 × 10^-15τ^-1/2 + 3 x 10-¹⁶, respectively, for 1 < r < 10⁴ s. We also calculate the coherence function (a figure of merit for very long baseline interferometry in radio astronomy) for observation frequencies of 100, 230, and 345 GHz, when using the cryoCSO and a hydrogen maser. The results show that the cryoCSO offers a significant advantage at frequencies above 100 GHz.
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C03	`01`	`X`	`ENG`	`@0 Low noise circuit @5 01`
C03	`01`	`X`	`SPA`	`@0 Circuito débil ruido @5 01`
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C03	`08`	`X`	`ENG`	`@0 Digital circuit @5 08`
C03	`08`	`X`	`SPA`	`@0 Circuito numérico @5 08`
C03	`09`	`X`	`FRE`	`@0 Diviseur @5 09`
C03	`09`	`X`	`ENG`	`@0 Divider @5 09`
C03	`09`	`X`	`SPA`	`@0 Divisor @5 09`
C03	`10`	`X`	`FRE`	`@0 Méthode directe @5 10`
C03	`10`	`X`	`ENG`	`@0 Direct method @5 10`
C03	`10`	`X`	`SPA`	`@0 Método directo @5 10`
C03	`11`	`X`	`FRE`	`@0 Synthétiseur numérique @5 11`
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C03	`12`	`X`	`ENG`	`@0 Tunable circuit @5 12`
C03	`12`	`X`	`SPA`	`@0 Circuito acordable @5 12`
C03	`13`	`X`	`FRE`	`@0 Stabilité fréquence @5 13`
C03	`13`	`X`	`ENG`	`@0 Frequency stability @5 13`
C03	`13`	`X`	`SPA`	`@0 Estabilidad frecuencia @5 13`
C03	`14`	`X`	`FRE`	`@0 Bande latérale unique @5 14`
C03	`14`	`X`	`ENG`	`@0 Single sideband @5 14`
C03	`14`	`X`	`SPA`	`@0 Banda lateral única @5 14`
C03	`15`	`X`	`FRE`	`@0 Fonction cohérence @5 15`
C03	`15`	`X`	`ENG`	`@0 Coherence function @5 15`
C03	`15`	`X`	`SPA`	`@0 Función coherencia @5 15`
C03	`16`	`X`	`FRE`	`@0 Facteur mérite @5 16`
C03	`16`	`X`	`ENG`	`@0 Figure of merit @5 16`
C03	`16`	`X`	`SPA`	`@0 Factor mérito @5 16`
C03	`17`	`X`	`FRE`	`@0 Maser @5 17`
C03	`17`	`X`	`ENG`	`@0 Maser @5 17`
C03	`17`	`X`	`SPA`	`@0 Maser @5 17`
C03	`18`	`X`	`FRE`	`@0 Cryogénie @5 18`
C03	`18`	`X`	`ENG`	`@0 Cryogenics @5 18`
C03	`18`	`X`	`SPA`	`@0 Criogenia @5 18`
C03	`19`	`X`	`FRE`	`@0 Température cryogénique @5 19`
C03	`19`	`X`	`ENG`	`@0 Cryogenic temperature @5 19`
C03	`19`	`X`	`SPA`	`@0 Temperatura criogénica @5 19`
C03	`20`	`X`	`FRE`	`@0 Composite ordre 2 @5 20`
C03	`20`	`X`	`ENG`	`@0 Composite second order @5 20`
C03	`20`	`X`	`SPA`	`@0 Compuesto orden 2 @5 20`
C03	`21`	`X`	`FRE`	`@0 Cohérence @5 21`
C03	`21`	`X`	`ENG`	`@0 Coherence @5 21`
C03	`21`	`X`	`SPA`	`@0 Coherencia @5 21`
C03	`22`	`X`	`FRE`	`@0 Circuit intégré @5 46`
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Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Ultra-Stable Very-Low Phase-Noise Signal Source for Very Long Baseline Interferometry Using a Cryocooled Sapphire Oscillator</title>
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<series><title level="j" type="main">IEEE transactions on microwave theory and techniques</title>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Coherence</term>
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<term>Digital circuit</term>
<term>Digital synthesizer</term>
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<term>Fonction cohérence</term>
<term>Facteur mérite</term>
<term>Maser</term>
<term>Cryogénie</term>
<term>Température cryogénique</term>
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<front><div type="abstract" xml:lang="en">The design and implementation of a novel frequency synthesizer based on low phase-noise digital dividers and a direct digital synthesizer is presented. The synthesis produces two low-noise accurate tunable signals at 10 and 100 MHz. We report the measured residual phase noise and frequency stability of the synthesizer and estimate the total frequency stability, which can be expected from the synthesizer seeded with a signal near 11.2 GHz from an ultra-stable cryocooled sapphire oscillator (cryoCSO). The synthesizer residual single-sideband phase noise, at 1-Hz offset, on 10- and 100-MHz signals was -135 and -130 dBc/Hz, respectively. The frequency stability contributions of these two signals was σ<sub>y</sub>
 = 9 × 10<sup>-15</sup>
 and σ<sub>y</sub>
 = 2.2 × 10<sup>-15</sup>
, respectively, at 1-s integration time. The Allan deviation of the total fractional frequency noise on the 10- and 100-MHz signals derived from the synthesizer with the cryoCSO may be estimated, respectively, as σ<sub>y</sub>
 ≃ 5.2 × 10<sup>-15</sup>
τ<sup>-1</sup>
 + 3.6 × 10<sup>-15</sup>
τ<sup>-1/2</sup>
 + 4 × 10<sup>-16</sup>
 and σ<sub>y</sub>
 ≃ 2 × 10<sup>-15</sup>
τ<sup>-1/2</sup>
 + 3 x 10-<sup>16</sup>
, respectively, for 1 < r < 10<sup>4</sup>
 s. We also calculate the coherence function (a figure of merit for very long baseline interferometry in radio astronomy) for observation frequencies of 100, 230, and 345 GHz, when using the cryoCSO and a hydrogen maser. The results show that the cryoCSO offers a significant advantage at frequencies above 100 GHz.</div>
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<fC01 i1="01" l="ENG"><s0>The design and implementation of a novel frequency synthesizer based on low phase-noise digital dividers and a direct digital synthesizer is presented. The synthesis produces two low-noise accurate tunable signals at 10 and 100 MHz. We report the measured residual phase noise and frequency stability of the synthesizer and estimate the total frequency stability, which can be expected from the synthesizer seeded with a signal near 11.2 GHz from an ultra-stable cryocooled sapphire oscillator (cryoCSO). The synthesizer residual single-sideband phase noise, at 1-Hz offset, on 10- and 100-MHz signals was -135 and -130 dBc/Hz, respectively. The frequency stability contributions of these two signals was σ<sub>y</sub>
 = 9 × 10<sup>-15</sup>
 and σ<sub>y</sub>
 = 2.2 × 10<sup>-15</sup>
, respectively, at 1-s integration time. The Allan deviation of the total fractional frequency noise on the 10- and 100-MHz signals derived from the synthesizer with the cryoCSO may be estimated, respectively, as σ<sub>y</sub>
 ≃ 5.2 × 10<sup>-15</sup>
τ<sup>-1</sup>
 + 3.6 × 10<sup>-15</sup>
τ<sup>-1/2</sup>
 + 4 × 10<sup>-16</sup>
 and σ<sub>y</sub>
 ≃ 2 × 10<sup>-15</sup>
τ<sup>-1/2</sup>
 + 3 x 10-<sup>16</sup>
, respectively, for 1 < r < 10<sup>4</sup>
 s. We also calculate the coherence function (a figure of merit for very long baseline interferometry in radio astronomy) for observation frequencies of 100, 230, and 345 GHz, when using the cryoCSO and a hydrogen maser. The results show that the cryoCSO offers a significant advantage at frequencies above 100 GHz.</s0>
</fC01>
<fC02 i1="01" i2="X"><s0>001D03G02A1</s0>
</fC02>
<fC02 i1="02" i2="X"><s0>001D03G02A6</s0>
</fC02>
<fC02 i1="03" i2="X"><s0>001D03F06B</s0>
</fC02>
<fC02 i1="04" i2="X"><s0>001D03E</s0>
</fC02>
<fC03 i1="01" i2="X" l="FRE"><s0>Circuit faible bruit</s0>
<s5>01</s5>
</fC03>
<fC03 i1="01" i2="X" l="ENG"><s0>Low noise circuit</s0>
<s5>01</s5>
</fC03>
<fC03 i1="01" i2="X" l="SPA"><s0>Circuito débil ruido</s0>
<s5>01</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Bruit phase</s0>
<s5>02</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Phase noise</s0>
<s5>02</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Ruido fase</s0>
<s5>02</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Source bruit</s0>
<s5>03</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Noise source</s0>
<s5>03</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Fuente ruido</s0>
<s5>03</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Radioastronomie</s0>
<s5>04</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Radio astronomy</s0>
<s5>04</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Radioastronomía</s0>
<s5>04</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE"><s0>Oscillateur</s0>
<s5>05</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Oscillator</s0>
<s5>05</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Oscilador</s0>
<s5>05</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Implémentation</s0>
<s5>06</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Implementation</s0>
<s5>06</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Implementación</s0>
<s5>06</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Synthétiseur fréquence</s0>
<s5>07</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Frequency synthesizer</s0>
<s5>07</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Sintetizador frecuencia</s0>
<s5>07</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Circuit numérique</s0>
<s5>08</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Digital circuit</s0>
<s5>08</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Circuito numérico</s0>
<s5>08</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Diviseur</s0>
<s5>09</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Divider</s0>
<s5>09</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Divisor</s0>
<s5>09</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Méthode directe</s0>
<s5>10</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Direct method</s0>
<s5>10</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Método directo</s0>
<s5>10</s5>
</fC03>
<fC03 i1="11" i2="X" l="FRE"><s0>Synthétiseur numérique</s0>
<s5>11</s5>
</fC03>
<fC03 i1="11" i2="X" l="ENG"><s0>Digital synthesizer</s0>
<s5>11</s5>
</fC03>
<fC03 i1="11" i2="X" l="SPA"><s0>Sintetizador numérico</s0>
<s5>11</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Circuit accordable</s0>
<s5>12</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Tunable circuit</s0>
<s5>12</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Circuito acordable</s0>
<s5>12</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Stabilité fréquence</s0>
<s5>13</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Frequency stability</s0>
<s5>13</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Estabilidad frecuencia</s0>
<s5>13</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Bande latérale unique</s0>
<s5>14</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Single sideband</s0>
<s5>14</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Banda lateral única</s0>
<s5>14</s5>
</fC03>
<fC03 i1="15" i2="X" l="FRE"><s0>Fonction cohérence</s0>
<s5>15</s5>
</fC03>
<fC03 i1="15" i2="X" l="ENG"><s0>Coherence function</s0>
<s5>15</s5>
</fC03>
<fC03 i1="15" i2="X" l="SPA"><s0>Función coherencia</s0>
<s5>15</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE"><s0>Facteur mérite</s0>
<s5>16</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>Figure of merit</s0>
<s5>16</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA"><s0>Factor mérito</s0>
<s5>16</s5>
</fC03>
<fC03 i1="17" i2="X" l="FRE"><s0>Maser</s0>
<s5>17</s5>
</fC03>
<fC03 i1="17" i2="X" l="ENG"><s0>Maser</s0>
<s5>17</s5>
</fC03>
<fC03 i1="17" i2="X" l="SPA"><s0>Maser</s0>
<s5>17</s5>
</fC03>
<fC03 i1="18" i2="X" l="FRE"><s0>Cryogénie</s0>
<s5>18</s5>
</fC03>
<fC03 i1="18" i2="X" l="ENG"><s0>Cryogenics</s0>
<s5>18</s5>
</fC03>
<fC03 i1="18" i2="X" l="SPA"><s0>Criogenia</s0>
<s5>18</s5>
</fC03>
<fC03 i1="19" i2="X" l="FRE"><s0>Température cryogénique</s0>
<s5>19</s5>
</fC03>
<fC03 i1="19" i2="X" l="ENG"><s0>Cryogenic temperature</s0>
<s5>19</s5>
</fC03>
<fC03 i1="19" i2="X" l="SPA"><s0>Temperatura criogénica</s0>
<s5>19</s5>
</fC03>
<fC03 i1="20" i2="X" l="FRE"><s0>Composite ordre 2</s0>
<s5>20</s5>
</fC03>
<fC03 i1="20" i2="X" l="ENG"><s0>Composite second order</s0>
<s5>20</s5>
</fC03>
<fC03 i1="20" i2="X" l="SPA"><s0>Compuesto orden 2</s0>
<s5>20</s5>
</fC03>
<fC03 i1="21" i2="X" l="FRE"><s0>Cohérence</s0>
<s5>21</s5>
</fC03>
<fC03 i1="21" i2="X" l="ENG"><s0>Coherence</s0>
<s5>21</s5>
</fC03>
<fC03 i1="21" i2="X" l="SPA"><s0>Coherencia</s0>
<s5>21</s5>
</fC03>
<fC03 i1="22" i2="X" l="FRE"><s0>Circuit intégré</s0>
<s5>46</s5>
</fC03>
<fC03 i1="22" i2="X" l="ENG"><s0>Integrated circuit</s0>
<s5>46</s5>
</fC03>
<fC03 i1="22" i2="X" l="SPA"><s0>Circuito integrado</s0>
<s5>46</s5>
</fC03>
<fN21><s1>023</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>

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Ultra-Stable Very-Low Phase-Noise Signal Source for Very Long Baseline Interferometry Using a Cryocooled Sapphire Oscillator

Ultra-Stable Very-Low Phase-Noise Signal Source for Very Long Baseline Interferometry Using a Cryocooled Sapphire Oscillator

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