The Front-End of the NOEMA Interferometer

Chenu, J.-Y.; Navarrini, A.; Bortolotti, Yves; Butin, G.; Fontana, A.L.; Mahieu, S.; Maier, D.; Mattiocco, F.; Serres, Patrice; Marylene, Berton; Garnier, Olivier; Moutote, Quentin; Parioleau, Magali; Pissard, Bruno; Reverdy, J.

doi:10.1109/tthz.2016.2525762

Cited by 30 publications

(22 citation statements)

References 8 publications

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“…As a follow-up to this programme, we have targeted the molecular gas emission from 13 KBSS QSOs with the NOrthern Extended Millimeter Array (NOEMA, developed from the Plateau de Bure Interferometer; see Guilloteau et al 1992;Chenu et al 2016) in order to further characterize this sample of hyper-luminous QSOs using submm spectroscopy, which are amongst the brightest in the observable Universe. In particular, we would like to confirm the origin of the submm continuum emission seen by SCUBA-2 with higher resolution imaging, and to derive a variety of useful physical properties that can be compared to other populations of galaxies and QSOs; the NOEMA observations reported here will certainly reveal whether the molecular gas properties of these hyper-luminous QSOs are similar to that of the general population of SMGs.…”

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confidence: 99%

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Hill

Chapman

Scott

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A primary goal of the SCUBA-2 Web survey is to perform tomography of the early inter-galactic medium by studying systems containing some of the brightest quasistellar objects (QSOs; 2.5 < z < 3.0) and nearby submillimetre galaxies. As a first step, this paper aims to characterize the galaxies that host the QSOs. To achieve this, a sample of 13 hyper-luminous (L AGN > 10 14 L ) QSOs with previous submillimetre continuum detections were followed up with CO(3-2) observations using the NOEMA interferometer. All but two of the QSOs are detected in CO(3-2); for one non-detection, our observations show a tentative 2σ line at the expected position and redshift, and for the other non-detection we find only continuum flux density an order of magnitude brighter than the other sources. In three of the fields, a companion potentially suitable for tomography is detected in CO line emission within 25 arcsec of the QSO. We derive gas masses, dynamical masses and far-infrared luminosities, and show that the QSOs in our sample have similar properties as compared to less luminous QSOs and SMGs in the literature, despite the fact that their black-hole masses (which are proportional to L AGN ) are 1-2 orders of magnitude larger. We discuss two interpretations of these observations: this is due to selection effects, such as preferential face-on viewing angles and picking out objects in the tail ends of the scatter in host-galaxy mass and blackhole mass relationships; or the black hole masses have been overestimated because the accretion rates are super-Eddington.

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mentioning

confidence: 99%

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Hill

Chapman

Scott

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…To date, radio/mm followup campaigns in interferometric mode improved the observational coverage of the lower part of the emission spectrum (e.g. Laskar et al 2013Laskar et al , 2015Laskar et al , 2018aLaskar et al , 2019a through increasingly sensitive facilities -such as the upgraded Giant Metre-wave Radio Telescope (GMRT, Swarup 1990; Kapahi & Ananthakrishnan 1995;Gupta et al 2017) 1 , the Karl G. Jansky Very Large Array (VLA, Thompson et al 1980) 2 , the Arcminute Microkelvin Imager Large Array (AMI-LA, Zwart et al 2008) 3 , and the NOrthern Extended Millimeter Array (NOEMA, Chenu et al 2016) 4 .…”

Section: Introductionmentioning

confidence: 99%

Radio data challenge the broadband modelling of GRB160131A afterglow

Marongiu,

Guidorzi,

Stratta

et al. 2021

Preprint

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Context. Gamma-ray burst (GRB) afterglows originate from the interaction between the relativistic ejecta and the surrounding medium. Consequently, their properties depend on several aspects: radiation mechanisms, relativistic shock micro-physics, circumburst environment, and the structure and geometry of the relativistic jet. While the standard afterglow model accounts for the overall spectral and temporal evolution for a number of GRBs, its validity limits emerge when the data set is particularly rich and constraining, especially in the radio band. Aims. We aimed to model the afterglow of the long GRB 160131A (redshift z = 0.972), for which we collected a rich, broadband, and accurate data set, spanning from 6 × 10 8 Hz to 7 × 10 17 Hz in frequency, and from 330 s to 160 days post burst in time. Methods. We modelled the spectral and temporal evolution of this GRB afterglow through two approaches: (1) the adoption of empirical functions to model optical/X-rays data set, later assessing their compatibility with the radio domain; (2) the inclusion of the entire multi-frequency data set simultaneously through the Python package named sAGa (Software for AfterGlow Analysis), to come up with an exhaustive and self-consistent description of the micro-physics, geometry, and dynamics of the afterglow. Results. From deep broadband analysis (from radio to X-ray frequencies) of the afterglow light curves, GRB 160131A outflow shows evidence of jetted emission. Moreover, we observe dust extinction in the optical spectra, and energy injection in the optical/X-ray data. Finally, radio spectra are characterised by several peaks, that could be due to either interstellar scintillation (ISS) effects or a multi-component structure. Conclusions. The inclusion of radio data in the broadband set of GRB 160131A makes a self-consistent modelling hardly attainable within the standard model of GRB afterglows.

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“…8 a strong interest to increase the IF bandwidth of SIS receivers in order to improve the continuum sensitivity and expand the number of radio astronomy lines detectable in a single observing run. Thus, the PdBI dual-polarization receivers are being upgraded for the NOEMA (Northern Extended Millimeter Array) project, 1 [1] from backshort-tuned single side band (SSB) mixers [2], [3] to sideband separating (2SB) mixers providing two 8 GHz wide IF bands (across 4-12 GHz) [4], [5] per polarization channel, thereby allowing to gain a factor of 4 in terms of available IF band. The technology used for the NOEMA receiver is similar to that developed for the EMIR receiver [6] installed on the IRAM 30 m telescope at Pico Veleta, Spain.…”

Section: Introductionmentioning

confidence: 99%

The IF Output Impedance of SIS Mixers

Serres

Navarrini

Bortolotti

et al. 2014

IEEE Trans. THz Sci. Technol.

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In this paper, we describe a measurement setup to characterize the intermediate frequency (IF) impedance of cryogenically cooled superconductor-insulator-superconductor (SIS) mixers. A setup based on a commercial vector network analyzer (VNA), a circulator and a low noise amplifier (LNA) has allowed to increase the dynamic of the VNA and to perform accurate one-port measurements across a high dynamic range of the SIS mixers IF band. The mixers were biased in three different regions of their unpumped IV curve to obtain three known impedances which are close to the classical calibration SOLT standards (Short, Open, Load, Thru): the reference plane was located at the SIS junction itself and the calibration procedure allowed to calibrate out all IF circuitry of the measurement setup, including the on-chip SIS mixer intrinsic capacitance and inductance without requiring to thermally cycle and open the cryostat to locate and measure the different calibration standards. Thus, the devised method provides a simple and direct measurement of the SIS mixers IF impedance which can be used for quick, accurate and highly repeatable IF characterization of any type of millimeter and sub-millimeter wave SIS mixers. The measurement method is described and the experimental results of the IF output impedances of 3 mm band DSB and SSB mixers with 4 GHz wide IFs (across 4-8 GHz) are presented and compared with simulated predictions obtained from combining Tucker's SIS mixer theory and accurate electromagnetic modeling of the mixer structure. Index Terms-Double side band (DSB) and single side band (SSB) tuning, intermediate frequency (IF) impedance, superconductor-insulator-superconductor (SIS) mixer, vector network analyzer (VNA) measurements.

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The Front-End of the NOEMA Interferometer

Cited by 30 publications

References 8 publications

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Radio data challenge the broadband modelling of GRB160131A afterglow

The IF Output Impedance of SIS Mixers

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