F. Tercero

Yebes Observatory

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Trends

Author Order

Document Type

Co-Authors

J. A. López-Pérez

Yebes Observatory

J. D. Gallego

Yebes Observatory

P. de Vicente

Yebes Observatory

J. Cernicharo

Consejo Superior de Investigaciones Científicas

J. A. López-Fernández

Yebes Observatory

Luis Enrique García-Muñoz

Universidad Carlos III de Madrid

J. R. Pardo

Instituto de Física Fundamental

J. A. López Fernández

Yebes Observatory

C. Cabezas

Instituto de Física Fundamental

ÓG

Ó. García-Pérez

Yebes Observatory

Cooperative Institutions

Yebes Observatory

Instituto Geográfico Nacional

Consejo Superior de Investigaciones Científicas

Spanish National Observatory

Instituto de Física Fundamental

Ministerio de Transportes, Movilidad y Agenda Urbana

Universidad Politécnica de Madrid

Centre National de la Recherche Scientifique

Instituto de Ciencia de Materiales de Madrid

Institut de Radioastronomie Millimétrique

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Field

ALMA front-end optics

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (2004)

Matthew C. Carter A. Baryshev Mark Harman B. Lazareff James W. Lamb

The ALMA telescope will be an interferometer of 64 antennas, which will be situated in the Atacama desert in Chile. Each antenna will have receivers that cover the frequencies 30 GHz to 970 GHZ. This frequency range is divided into 10 frequency bands. All of these receiver bands are fitted on a cartridge and cooled, with bands 1 and 2 at 15K and the other 8 are SIS receivers at a temperature of 4K. Each band has a dual polarization receiver. The optics has been designed so that the maximum of the optics is cooled to minimize the noise temperature increase to the receivers. The design of the optics will be shown for each frequency bands. Test results with the method of testing on a near field amplitude and phase measurement system will be given for the first 4 frequency bands to be used, which are bands 3 (84-116 GHz), 6 (211-275GHz), 7 (275-375 GHz and 9 (600-702 GHz). These measurements will be compared with physical optics calculations.

Dual-polarization interferometry

Frequency band

Physical optics

Radio spectrum

Gaussian optics

10.1117/12.552538

Cite

Citations (26)

Optimization of the Quad-Ridged Horn for the geodetic VGOS station of the Yebes Observatory

2022 16th European Conference on Antennas and Propagation (EuCAP) (2018)

F. Tercero Ó. García-Pérez J. M. Serna S. Lopez-Ruiz B. Vaquero

10.1049/cp.2018.0818

Cite

Citations (0)

A Tri-band Cryogenic Receiver for VGOS Radio Telescopes

J. A. López-Pérez J. A. López-Fernández F. Tercero B. Vaquero J. M. Serna

Very-long-baseline interferometry

Radio Astronomy

Source

Cite

Citations (0)

Discovery of allenyl acetylene, H2CCCHCCH, in TMC-1

Astronomy and Astrophysics (2021)

J. Cernicharo C. Cabezas M. Agúndez B. Tercero N. Marcelino

We present the discovery in TMC-1 of allenyl acetylene, H 2 CCCHCCH, through the observation of nineteen lines with a signal-to-noise ratio ∼4–15. For this species, we derived a rotational temperature of 7 ± 1 K and a column density of 1.2 ± 0.2 × 10 13 cm −2 . The other well known isomer of this molecule, methyl diacetylene (CH 3 C 4 H), has also been observed and we derived a similar rotational temperature, T r = 7.0 ± 0.3 K, and a column density for its two states ( A and E ) of 6.5 ± 0.3 × 10 12 cm −2 . Hence, allenyl acetylene and methyl diacetylene have a similar abundance. Remarkably, their abundances are close to that of vinyl acetylene (CH 2 CHCCH). We also searched for the other isomer of C 5 H 4 , HCCCH 2 CCH (1.4-Pentadiyne), but only a 3 σ upper limit of 2.5 × 10 12 cm −2 to the column density can be established. These results have been compared to state-of-the-art chemical models for TMC-1, indicating the important role of these hydrocarbons in its chemistry. The rotational parameters of allenyl acetylene have been improved by fitting the existing laboratory data together with the frequencies of the transitions observed in TMC-1.

Diacetylene

Acetylene

Source

Cite

Citations (12)

An optical solution for the radioastronomic observation bands of the new 40 m radiotelescope of Centro Astronomico de Yebes

Luis Enrique García-Muñoz Leandro de Haro Ariet J. A. López Fernández F. Tercero Belén Galocha Iragüen

In this paper is presented a solution for the focalisation of the new 40 m radiotelescope of the Centro Astronomico de Yebes (CAY) in Guadalajara, Spain. Quasi-optics theory is used in this paper for the propagation analysis of the beams through the different optics elements. The goal of this paper is to design the optical system that can focalize several bands reducing to the minimum number of possible optic elements, and sharing the maximum number of them. Hyperbolic lenses and ellipsoidal mirrors parameters, focal distances, and the feeder dimensions necessary for the focalization in each band are calculated.

Ellipsoid

Geometrical optics

Focalization

10.1109/icmmt.2002.1187728

Cite

Citations (0)

International Journal of Infrared and Millimeter Waves (2002)

Luis Enrique García-Muñoz J. A. López Fernández Leandro de Haro Ariet F. Tercero Belén Galocha Iragüen

Focalization

Ellipsoid

Component (thermodynamics)

10.1023/a:1019611725506

Cite

Citations (1)

Broad-band high-resolution rotational spectroscopy for laboratory astrophysics

Astronomy and Astrophysics (2019)

J. Cernicharo J. D. Gallego J. A. López-Pérez F. Tercero Isabel Tanarro

We present a new experimental setup devoted to the study of gas phase molecules and processes using broad band high spectral resolution rotational spectroscopy. A reactor chamber has been equipped with radio receivers similar to those used by radio astronomers to search for molecular emission in space. The whole Q (31.5-50 GHz) and W bands (72-116.5 GHz) are available for rotational spectroscopy observations. The receivers are equipped with 16×2.5 GHz Fast Fourier Transform spectrometers with a spectral resolution of 38.14 kHz allowing the simultaneous observation of the complete Q band and one third of the W band. The whole W band can be observed in three settings in which the Q band is always observed. Species such as CH

Isotopologue

Spectral resolution

Fourier transform spectroscopy

10.1051/0004-6361/201935197

Cite

Citations (16)

FEASIBILITY STUDY FOR THE FOCALISATION OF THE NEW 40m RADIOTELESCOPE OF CENTRO ASTRONÓMICO DE YEBES

Luis Enrique García-Muñoz Leandro de Haro Ariet J. A. López Fernández F. Tercero B. Galoha

This paper presents a first study of the focalisation of the new 40m. radiotelescope of Centro AstronOmico de Yebes (Spain) which may operate at S, X, K and millimetre bands with a multiband feed system with minor mechanical changes on a classical Cassegrain type radiotelescope. The geometry of this Cassegrain antenna radiotelescope consists of a 40m paraboloidal main reflector with f/D=7.915.

Cassegrain reflector

Astron

Reflector (photography)

Cassegrain antenna

Source

Cite

Citations (0)

Yebes 40 m radio telescope and the broad band Nanocosmos receivers at 7 mm and 3 mm for line surveys

Astronomy and Astrophysics (2020)

F. Tercero J. A. López-Pérez J. D. Gallego F. Beltrán Omaira García

Yebes 40\,m radio telescope is the main and largest observing instrument at Yebes Observatory and it is devoted to Very Long Baseline Interferometry (VLBI) and single dish observations since 2010. It has been covering frequency bands between 2\,GHz and 90\,GHz in discontinuous and narrow windows in most of the cases, to match the current needs of the European VLBI Network (EVN) and the Global Millimeter VLBI Array (GMVA). Nanocosmos project, a European Union funded synergy grant, opened the possibility to increase the instantaneous frequency coverage to observe many molecular transitions with single tunnings in single dish mode. This reduces the observing time and maximises the output from the telescope. We present the technical specifications of the recently installed 31.5-50 GHz (Q band) and 72-90.5 GHz (W band) receivers along with the main characteristics of the telescope at these frequency ranges. We have observed IRC+10216, CRL 2688 and CRL 618, which harbour a rich molecular chemistry, to demonstrate the capabilities of the new instrumentation for spectral observations in single dish mode. The results show the high sensitivity of the telescope in the Q band. The spectrum of IRC+10126 offers a signal to noise ratio never seen before for this source in this band. On the other hand, the spectrum normalised by the continuum flux towards CRL\,618 in the W band demonstrates that the 40~m radio telescope produces comparable results to those from the IRAM 30~m radio telescope, although with a smaller sensitivity. The new receivers fulfil one of the main goals of Nanocosmos and open the possibility to study the spectrum of different astrophysical media with unprecedented sensitivity.

Very-long-baseline interferometry

Radio spectrum

Radio Astronomy

Instrumentation

Green Bank Telescope

10.1051/0004-6361/202038701

Cite

Citations (99)

THE NANOCOSMOS GAS CELL: A BROADBAND FOURIER TRANSFORM MILLIMETERWAVE SPECTROMETER BASED ON RADIO ASTRONOMY RECEIVERS

Proceedings of the 74th International Symposium on Molecular Spectroscopy (2019)

Celina Bermï ⁄ œdez J. Cernicharo Josï ⁄ Ž Lï ⁄ —pez Pï ⁄ Žrez F. Tercero P. de Vicente

25th International Conference on High Resolution Molecular Spectroscopy. 3 al 7 de septiembre en el Bizkaia Aretoa (Bilbao, Spain)(2018). --.http://www.hrms-bilbao2018.com/

Radio Astronomy

Fourier transform spectroscopy

10.15278/isms.2019.tg06

Cite

Citations (0)