Measurement of Th1/Th2 serum cytokines by flow cytometry in classical Hodgkin lymphoma

O linfoma de Hodgkin clássico (LHC) é uma neoplasia com distúrbio na produção de citocinas. Estudos demonstram que o padrão anormal das citocinas no linfonodo acometido pela lesão contribui não somente com a proliferação das células malignas H-RS, como também com o característico infiltrado hiper-reativo que compõe o tecido no LHC. Esta disfunção pode ser observada tanto no quadro clínico dos pacientes, como nas características histopatológicas: sintomas B, deficiência na resposta imune celular, bandas de colágeno e eosinofilia. As concentrações séricas das citocinas Th1 (IL-2, TNF, INF-&#947;) e Th2 (IL-4, IL-5, IL-10) foram estudadas em 45 pacientes com LHC, ao diagnóstico, e em 34 doadores saudáveis, por citometria de fluxo (CBA - cytometric beads array). Houve aumento das concentrações das citocinas TNF (p<0,01), INF-&#947; (p<0,01), IL-4 (p=0,01), IL-5 (p<0,01) e IL-10 (p<0,01) dos pacientes quando comparados com o grupo controle. Não foi evidenciada diferença em relação a IL-2. Ao correlacionarmos as concentrações das citocinas Th1/Th2 com as variáveis clínico-laboratoriais dos pacientes, observou-se que níveis elevados da IL-10 (Th2) estão correlacionados com as variáveis que implicam em pior prognóstico: estádios III/IV (p=0,01), presença de sintomas B (p=0,04), hemoglobina < 10,5g/dL (p=0+,01), linfócitos <600 mm³ (p=0,01) e, de acordo com o IPI, os pacientes de alto risco (p=0,01). Por outro lado, níveis séricos elevados da IL-2 (Th1) foram encontrados em estádio I/II, quando comparados com III/IV (p=0,03), o que indica que a IL-2 diminui com a progressão da doença. Os resultados sugerem que a IL-10 possa estar regulando negativamente a resposta imune citotóxica (Th1) pela inibição da IL-2. Há uma possível associação entre progressão da doença e níveis elevados da IL-10. Esse estudo evidenciou que a utilização do CBA é factível na detecção das citocinas, e que as alterações encontradas podem estar envolvidas na biologia do LHC.Classical Hodgkin lymphoma (CHL) is a malignancy with an abnormal or unbalanced secretion/production of cytokines, which might support the growth of H-RS cells, their surrounding reactive bystander cells and may be responsible for the typical clinical and histopathologic features of CHL: systemic B symptoms, an apparent defect in cell-mediated immune response, tumor fibrosis and eosinophilic infiltrate. Serum concentrations of IL-2, IL-4, IL5, IL-10, TNF and IFN-&#947; (Th1/Th2) were measured in 45 patients at diagnosis of classical Hodgkin lymphoma and in 34 healthy controls by cytometric beads array (CBA). Levels of TNF (p<0.01), INF-&#947;(p<0.01), IL-4 (p=0.01), IL-5 (p<0.01) e IL-10 (p<0.01) were significantly higher in patients compared to the control group. No difference was observed for IL-2 between the two groups. On correlating Th1/Th2 cytokine concentrations with clinical risk factors, elevated IL-10 (Th2) levels are associated with variables that suggest worse prognoses including III/IV stage (p=0.01), B-symptoms (p=0.04), hemoglobin < 10.5g/dL (p=0.01), lymphocytes < 600/mm³ (p=0.01) and according to the seven-factored international prognostic score (IPI), a subset of patients with a particularly high risk of failure (p=0.01). Furthermore, the serum levels of IL-2 (Th1) were significantly higher in a group of I/II stage patients compared to III/IV patients (p=0.03) which implies that, the levels of IL-2 might decrease with disease progression. The elevated IL-10 levels in a subset of patients with poor clinical risk factors might down regulate a Th1 immune response by inhibiting IL-2 production causing survival disadvantage by suppression of the cytotoxic immune response against the tumor. This suggests an association between progression of CHL and higher levels of the IL-10 cytokine. This study showed that measurement of serum cytokines using the CBA methodology is highly reproducible, and that changes in concentrations seem to be involved in the biology of this diseas

Advanced Virgo Plus: Future Perspectives

While completing the commissioning phase to prepare the Virgo interferometer for the next joint Observation Run (O4), the Virgo collaboration is also finalizing the design of the next upgrades to the detector to be employed in the following Observation Run (O5). The major upgrade will concern decreasing the thermal noise limit, which will imply using very large test masses and increased laser beam size. But this will not be the only upgrade to be implemented in the break between the O4 and O5 observation runs to increase the Virgo detector strain sensitivity. The paper will cover the challenges linked to this upgrade and implications on the detector's reach and observational potential, reflecting the talk given at 12th Cosmic Ray International Seminar - CRIS 2022 held in September 2022 in Napoli

Calibration of advanced Virgo and reconstruction of the detector strain h( t) during the observing run O3

The three advanced Virgo and LIGO gravitational wave detectors participated to the third observing run (O3) between 1 April 2019 15:00 UTC and 27 March 2020 17:00 UTC, leading to several gravitational wave detections per month. This paper describes the advanced Virgo detector calibration and the reconstruction of the detector strain h(t) during O3, as well as the estimation of the associated uncertainties. For the first time, the photon calibration technique as been used as reference for Virgo calibration, which allowed to cross-calibrate the strain amplitude of the Virgo and LIGO detectors. The previous reference, so-called free swinging Michelson technique, has still been used but as an independent cross-check. h(t) reconstruction and noise subtraction were processed online, with good enough quality to prevent the need for offline reprocessing, except for the two last weeks of September 2019. The uncertainties for the reconstructed h(t) strain, estimated in this paper in a 20-2000 Hz frequency band, are frequency independent: 5% in amplitude, 35 mrad in phase and 10 μs in timing, with the exception of larger uncertainties around 50 Hz

The Advanced Virgo+ status

The gravitational wave detector Advanced Virgo+ is currently in the commissioning phase in view of the fourth Observing Run (O4). The major upgrades with respect to the Advanced Virgo configuration are the implementation of an additional recycling cavity, the Signal Recycling cavity (SRC), at the output of the interferometer to broaden the sensitivity band and the Frequency Dependent Squeezing (FDS) to reduce quantum noise at all frequencies. The main difference of the Advanced Virgo + detector with respect to the LIGO detectors is the presence of marginally stable recycling cavities, with respect to the stable recycling cavities present in the LIGO detectors, which increases the difficulties in controlling the interferometer in presence of defects (both thermal and cold defects). This work will focus on the interferometer commissioning, highlighting the control challenges to maintain the detector in the working point which maximizes the sensitivity and the duty cycle for scientific data taking

Frequency-Dependent Squeezed Vacuum Source for the Advanced Virgo Gravitational-Wave Detector

In this Letter, we present the design and performance of the frequency-dependent squeezed vacuum source that will be used for the broadband quantum noise reduction of the Advanced Virgo Plus gravitational-wave detector in the upcoming observation run. The frequency-dependent squeezed field is generated by a phase rotation of a frequency-independent squeezed state through a 285 m long, high-finesse, near-detuned optical resonator. With about 8.5 dB of generated squeezing, up to 5.6 dB of quantum noise suppression has been measured at high frequency while close to the filter cavity resonance frequency, the intracavity losses limit this value to about 2 dB. Frequency-dependent squeezing is produced with a rotation frequency stability of about 6 Hz rms, which is maintained over the long term. The achieved results fulfill the frequency dependent squeezed vacuum source requirements for Advanced Virgo Plus. With the current squeezing source, considering also the estimated squeezing degradation induced by the interferometer, we expect a reduction of the quantum shot noise and radiation pressure noise of up to 4.5 dB and 2 dB, respectively

Quantum Backaction on kg-Scale Mirrors: Observation of Radiation Pressure Noise in the Advanced Virgo Detector

The quantum radiation pressure and the quantum shot noise in laser-interferometric gravitational wave detectors constitute a macroscopic manifestation of the Heisenberg inequality. If quantum shot noise can be easily observed, the observation of quantum radiation pressure noise has been elusive, so far, due to the technical noise competing with quantum effects. Here, we discuss the evidence of quantum radiation pressure noise in the Advanced Virgo gravitational wave detector. In our experiment, we inject squeezed vacuum states of light into the interferometer in order to manipulate the quantum backaction on the 42 kg mirrors and observe the corresponding quantum noise driven displacement at frequencies between 30 and 70 Hz. The experimental data, obtained in various interferometer configurations, is tested against the Advanced Virgo detector quantum noise model which confirmed the measured magnitude of quantum radiation pressure noise

Frequency-Dependent Squeezed Vacuum Source for the Advanced Virgo Gravitational-Wave Detector

In this Letter, we present the design and performance of the frequency-dependent squeezed vacuum source that will be used for the broadband quantum noise reduction of the Advanced Virgo Plus gravitational-wave detector in the upcoming observation run. The frequency-dependent squeezed field is generated by a phase rotation of a frequency-independent squeezed state through a 285 m long, high-finesse, near-detuned optical resonator. With about 8.5 dB of generated squeezing, up to 5.6 dB of quantum noise suppression has been measured at high frequency while close to the filter cavity resonance frequency, the intracavity losses limit this value to about 2 dB. Frequency-dependent squeezing is produced with a rotation frequency stability of about 6 Hz rms, which is maintained over the long term. The achieved results fulfill the frequency dependent squeezed vacuum source requirements for Advanced Virgo Plus. With the current squeezing source, considering also the estimated squeezing degradation induced by the interferometer, we expect a reduction of the quantum shot noise and radiation pressure noise of up to 4.5 dB and 2 dB, respectively

Virgo Detector Characterization and Data Quality during the O3 run

The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave signals in the past few years, alongside the two LIGO instruments. First, during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817) and then during the full Observation Run 3 (O3): an 11 months data taking period, between April 2019 and March 2020, that led to the addition of about 80 events to the catalog of transient gravitational-wave sources maintained by LIGO, Virgo and KAGRA. These discoveries and the manifold exploitation of the detected waveforms require an accurate characterization of the quality of the data, such as continuous study and monitoring of the detector noise. These activities, collectively named {\em detector characterization} or {\em DetChar}, span the whole workflow of the Virgo data, from the instrument front-end to the final analysis. They are described in details in the following article, with a focus on the associated tools, the results achieved by the Virgo DetChar group during the O3 run and the main prospects for future data-taking periods with an improved detector.Comment: 86 pages, 33 figures. This paper has been divided into two articles which supercede it and have been posted to arXiv on October 2022. Please use these new preprints as references: arXiv:2210.15634 (tools and methods) and arXiv:2210.15633 (results from the O3 run

Virgo Detector Characterization and Data Quality: results from the O3 run

The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave (GW) signals in the past few years, alongside the two Advanced LIGO instruments. First during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817), and then during the full Observation Run 3 (O3): an 11-months data taking period, between April 2019 and March 2020, that led to the addition of about 80 events to the catalog of transient GW sources maintained by LIGO, Virgo and now KAGRA. These discoveries and the manifold exploitation of the detected waveforms require an accurate characterization of the quality of the data, such as continuous study and monitoring of the detector noise sources. These activities, collectively named {\em detector characterization and data quality} or {\em DetChar}, span the whole workflow of the Virgo data, from the instrument front-end hardware to the final analyses. They are described in details in the following article, with a focus on the results achieved by the Virgo DetChar group during the O3 run. Concurrently, a companion article describes the tools that have been used by the Virgo DetChar group to perform this work.Comment: 57 pages, 18 figures. To be submitted to Class. and Quantum Grav. This is the "Results" part of preprint arXiv:2205.01555 [gr-qc] which has been split into two companion articles: one about the tools and methods, the other about the analyses of the O3 Virgo dat