The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

M López-Caniego; R Rebolo; M Aguiar; R Génova-Santos; F Gómez-Reñasco; C Gutierrez; J M Herreros; R J Hoyland; C López-Caraballo; A E Pelaez Santos; F Poidevin; J A Rubiño-Martín; V Sanchez de la Rosa; D Tramonte; A Vega-Moreno; T Viera-Curbelo; R Vignaga; E Martínez-González; R B Barreiro; B Casaponsa; F J Casas; J M Diego; R Fernández-Cobos; D Herranz; D Ortiz; P Vielva; E Artal; B Aja; J Cagigas; J L Cano; L de la Fuente; A Mediavilla; J V Terán; E Villa; Lucio Piccirillo; Richard A Battye; E Blackhurst; Michael Brown; R D Davies; R J Davis; C Dickinson; Keith Grainge; S Harper; Bruno Maffei; M McCulloch; S Melhuish; G Pisano; Robert Watson; M Hobson; A Lasenby; R Saunders; P Scott

The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

M López-Caniego, R Rebolo, M Aguiar, R Génova-Santos, F Gómez-Reñasco, C Gutierrez, J M Herreros, R J Hoyland, C López-Caraballo, A E Pelaez Santos, F Poidevin, J A Rubiño-Martín, V Sanchez de la Rosa, D Tramonte, A Vega-Moreno, T Viera-Curbelo, R Vignaga, E Martínez-González, R B Barreiro, B CasaponsaF J Casas, J M Diego, R Fernández-Cobos, D Herranz, D Ortiz, P Vielva, E Artal, B Aja, J Cagigas, J L Cano, L de la Fuente, A Mediavilla, J V Terán, E Villa, Lucio Piccirillo, Richard A Battye, E Blackhurst, Michael Brown, R D Davies, R J Davis, C Dickinson, Keith Grainge, S Harper, Bruno Maffei, M McCulloch, S Melhuish, G Pisano, Robert Watson, M Hobson, A Lasenby, R Saunders, P Scott

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Abstract

The {QUIJOTE} (Q-U-I {JOint} Tenerife) {CMB} Experiment is designed to observe the polarization of the Cosmic Microwave Background and other Galacticand extragalactic signals at medium and large angular scales in thefrequency range of 10-40 {GHz}. The first of the two {QUIJOTE} telescopesand the multi-frequency (10-20 {GHz}) instrument have been in operationsince November 2012. In 2014 a second telescope and a new instrument at30GHz will be ready for commissioning, and an additional instrument at40 {GHz} is in its final design stages. After three years of effectiveobservations, the data obtained by these telescopes and instruments willhave the required sensitivity to detect a primordial gravitational-wavecomponent if the tensor-to-scalar ratio is larger than r = 0.05. At themoment, we have completed half of the wide Galactic survey with themulti-frequency instrument covering 18 000 square degrees of theNorthern hemisphere. When we finish this survey in early 2014, we shallhave reached approximately 14\{{\textbackslash}mu\}K per one degree beam at 11, 13, 17and 19 {GHz}, in both Q and U.

Original language	English
Journal	ArXiv e-prints
Volume	1401
Publication status	Published - Jan 2014

Keywords

Astrophysics - Instrumentation and Methods for Astrophysics
Astrophysics - Cosmology and Extragalactic Astrophysics

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López-Caniego, M., Rebolo, R., Aguiar, M., Génova-Santos, R., Gómez-Reñasco, F., Gutierrez, C., Herreros, J. M., Hoyland, R. J., López-Caraballo, C., Pelaez Santos, A. E., Poidevin, F., Rubiño-Martín, J. A., Sanchez de la Rosa, V., Tramonte, D., Vega-Moreno, A., Viera-Curbelo, T., Vignaga, R., Martínez-González, E., Barreiro, R. B., ... Scott, P. (2014). The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument. ArXiv e-prints, 1401. http://arxiv.org/abs/1401.4690

@article{14ebaff2a5b344f4bef4796e1930d581,

title = "The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument",

abstract = "The {QUIJOTE} (Q-U-I {JOint} Tenerife) {CMB} Experiment is designed to observe the polarization of the Cosmic Microwave Background and other Galacticand extragalactic signals at medium and large angular scales in thefrequency range of 10-40 {GHz}. The first of the two {QUIJOTE} telescopesand the multi-frequency (10-20 {GHz}) instrument have been in operationsince November 2012. In 2014 a second telescope and a new instrument at30GHz will be ready for commissioning, and an additional instrument at40 {GHz} is in its final design stages. After three years of effectiveobservations, the data obtained by these telescopes and instruments willhave the required sensitivity to detect a primordial gravitational-wavecomponent if the tensor-to-scalar ratio is larger than r = 0.05. At themoment, we have completed half of the wide Galactic survey with themulti-frequency instrument covering 18 000 square degrees of theNorthern hemisphere. When we finish this survey in early 2014, we shallhave reached approximately 14\{{\textbackslash}mu\}K per one degree beam at 11, 13, 17and 19 {GHz}, in both Q and U.",

keywords = "Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics",

author = "M L{\'o}pez-Caniego and R Rebolo and M Aguiar and R G{\'e}nova-Santos and F G{\'o}mez-Re{\~n}asco and C Gutierrez and Herreros, {J M} and Hoyland, {R J} and C L{\'o}pez-Caraballo and {Pelaez Santos}, {A E} and F Poidevin and Rubi{\~n}o-Mart{\'i}n, {J A} and {Sanchez de la Rosa}, V and D Tramonte and A Vega-Moreno and T Viera-Curbelo and R Vignaga and E Mart{\'i}nez-Gonz{\'a}lez and Barreiro, {R B} and B Casaponsa and Casas, {F J} and Diego, {J M} and R Fern{\'a}ndez-Cobos and D Herranz and D Ortiz and P Vielva and E Artal and B Aja and J Cagigas and Cano, {J L} and {de la Fuente}, L and A Mediavilla and Ter{\'a}n, {J V} and E Villa and Lucio Piccirillo and Battye, {Richard A} and E Blackhurst and Michael Brown and Davies, {R D} and Davis, {R J} and C Dickinson and Keith Grainge and S Harper and Bruno Maffei and M McCulloch and S Melhuish and G Pisano and Robert Watson and M Hobson and A Lasenby and R Saunders and P Scott",

note = "Rencontres du Vietnam 2013: Cosmology in the Planck Era. Conference Proceedings. Typos added",

year = "2014",

month = jan,

language = "English",

volume = "1401",

journal = "ArXiv e-prints",

issn = "2331-8422",

publisher = "Cornell University",

}

López-Caniego, M, Rebolo, R, Aguiar, M, Génova-Santos, R, Gómez-Reñasco, F, Gutierrez, C, Herreros, JM, Hoyland, RJ, López-Caraballo, C, Pelaez Santos, AE, Poidevin, F, Rubiño-Martín, JA, Sanchez de la Rosa, V, Tramonte, D, Vega-Moreno, A, Viera-Curbelo, T, Vignaga, R, Martínez-González, E, Barreiro, RB, Casaponsa, B, Casas, FJ, Diego, JM, Fernández-Cobos, R, Herranz, D, Ortiz, D, Vielva, P, Artal, E, Aja, B, Cagigas, J, Cano, JL, de la Fuente, L, Mediavilla, A, Terán, JV, Villa, E, Piccirillo, L, Battye, RA, Blackhurst, E, Brown, M, Davies, RD, Davis, RJ, Dickinson, C , Grainge, K, Harper, S, Maffei, B, McCulloch, M, Melhuish, S, Pisano, G, Watson, R, Hobson, M, Lasenby, A, Saunders, R & Scott, P 2014, 'The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument', ArXiv e-prints, vol. 1401. <http://arxiv.org/abs/1401.4690>

TY - JOUR

T1 - The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

AU - López-Caniego, M

AU - Rebolo, R

AU - Aguiar, M

AU - Génova-Santos, R

AU - Gómez-Reñasco, F

AU - Gutierrez, C

AU - Herreros, J M

AU - Hoyland, R J

AU - López-Caraballo, C

AU - Pelaez Santos, A E

AU - Poidevin, F

AU - Rubiño-Martín, J A

AU - Sanchez de la Rosa, V

AU - Tramonte, D

AU - Vega-Moreno, A

AU - Viera-Curbelo, T

AU - Vignaga, R

AU - Martínez-González, E

AU - Barreiro, R B

AU - Casaponsa, B

AU - Casas, F J

AU - Diego, J M

AU - Fernández-Cobos, R

AU - Herranz, D

AU - Ortiz, D

AU - Vielva, P

AU - Artal, E

AU - Aja, B

AU - Cagigas, J

AU - Cano, J L

AU - de la Fuente, L

AU - Mediavilla, A

AU - Terán, J V

AU - Villa, E

AU - Piccirillo, Lucio

AU - Battye, Richard A

AU - Blackhurst, E

AU - Brown, Michael

AU - Davies, R D

AU - Davis, R J

AU - Dickinson, C

AU - Grainge, Keith

AU - Harper, S

AU - Maffei, Bruno

AU - McCulloch, M

AU - Melhuish, S

AU - Pisano, G

AU - Watson, Robert

AU - Hobson, M

AU - Lasenby, A

AU - Saunders, R

AU - Scott, P

N1 - Rencontres du Vietnam 2013: Cosmology in the Planck Era. Conference Proceedings. Typos added

PY - 2014/1

Y1 - 2014/1

N2 - The {QUIJOTE} (Q-U-I {JOint} Tenerife) {CMB} Experiment is designed to observe the polarization of the Cosmic Microwave Background and other Galacticand extragalactic signals at medium and large angular scales in thefrequency range of 10-40 {GHz}. The first of the two {QUIJOTE} telescopesand the multi-frequency (10-20 {GHz}) instrument have been in operationsince November 2012. In 2014 a second telescope and a new instrument at30GHz will be ready for commissioning, and an additional instrument at40 {GHz} is in its final design stages. After three years of effectiveobservations, the data obtained by these telescopes and instruments willhave the required sensitivity to detect a primordial gravitational-wavecomponent if the tensor-to-scalar ratio is larger than r = 0.05. At themoment, we have completed half of the wide Galactic survey with themulti-frequency instrument covering 18 000 square degrees of theNorthern hemisphere. When we finish this survey in early 2014, we shallhave reached approximately 14\{{\textbackslash}mu\}K per one degree beam at 11, 13, 17and 19 {GHz}, in both Q and U.

AB - The {QUIJOTE} (Q-U-I {JOint} Tenerife) {CMB} Experiment is designed to observe the polarization of the Cosmic Microwave Background and other Galacticand extragalactic signals at medium and large angular scales in thefrequency range of 10-40 {GHz}. The first of the two {QUIJOTE} telescopesand the multi-frequency (10-20 {GHz}) instrument have been in operationsince November 2012. In 2014 a second telescope and a new instrument at30GHz will be ready for commissioning, and an additional instrument at40 {GHz} is in its final design stages. After three years of effectiveobservations, the data obtained by these telescopes and instruments willhave the required sensitivity to detect a primordial gravitational-wavecomponent if the tensor-to-scalar ratio is larger than r = 0.05. At themoment, we have completed half of the wide Galactic survey with themulti-frequency instrument covering 18 000 square degrees of theNorthern hemisphere. When we finish this survey in early 2014, we shallhave reached approximately 14\{{\textbackslash}mu\}K per one degree beam at 11, 13, 17and 19 {GHz}, in both Q and U.

KW - Astrophysics - Instrumentation and Methods for Astrophysics

KW - Astrophysics - Cosmology and Extragalactic Astrophysics

M3 - Article

SN - 2331-8422

VL - 1401

JO - ArXiv e-prints

JF - ArXiv e-prints

ER -

The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

Abstract

Keywords

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