Alessandro Monfardini
(Néel)
6/3/19, 1:50 PM
I will describe in general the NIKA2 instrument. I will then focus on some possible points for improvements. For example: new dichroic, new 1mm arrays (developed at Néel), 1GHz electronics (LPSC), potential telescope upgrade (IRAM).
Dr
Nicolas Ponthieu
(IPAG)
6/3/19, 2:50 PM
With its large FOV and high sensitivity, NIKA2 is a high mapping speed instrument, uniquely suited for deep surveys. During commissioning, we had the opportunity to observe faint and moderately faint sources with NIKA2. This talk will summarize the latest developments on the NIKA2 data reduction pipeline and show its first application to small deep fields and source counting.
Dr
Bilal Ladjelate
(IRAM Granada)
6/3/19, 3:50 PM
Most of the people attending the conference have already an experience with NIKA2 observations and some of its subtleties.
The NIKA2 observing sessions are organized in pools, a shared risk way of scheduling projects according to their priorities, and weather and stability requests, in order to ensure that everyone gets the best of their data.
As NIKA2 reaches its second year of science...
Martino Calvo
(Institut Néel)
6/3/19, 4:20 PM
NIKA2 has been permanently installed at the IRAM Pico Veleta 30m telescope since October 2015. After the first commissioning campaigns, NIKA2 is now open to the international community and has been used in many scientific observing pools. Although invisible to the final user, the complexity of the instrument requires a lot of careful work to get everything ready before each pool, starting from...
Dr
PABLO TORNE
(Instituto de Radioastronomia Milimetrica, IRAM)
6/3/19, 4:50 PM
Pulsars are fascinating astrophysical objects that enable a variety of experiments usually with unrivalled precision. For example, pulsars have been used to test the equation-of-state of ultra-dense matter, or General Relativity up to the highest precision to date. However, although we have been very successful using pulsars as astronomical tools, we still do not fully understand their radio...
Dr
Etienne Pointecouteau
(IRAP Toulouse)
6/4/19, 9:00 AM
I will review the evolution of observations of the Sunyaev-Zeldovich (SZ) signal from groups and clusters of galaxies within the course of the past two decades. The SZ effect has become an efficient way to investigate the astrophysics of the hot intra-cluster gas, very competitive and complementary to X-ray observations, and thereby renew the use of massive halos as a cosmological probe. I...
Dr
Juan Francisco Macias-Perez
(LPSC)
6/4/19, 9:30 AM
Clusters of galaxies are unique cosmological probes sensitive to the primordial density fluctuations, and the expansion history and energy content of the Universe. The thermal Sunyaev-Zeldovich (tSZ) effect is an observable of choice for cluster cosmology due to the low scatter in the relationship between SZ flux and cluster mass, and the construction of large tSZ selected cluster catalogs....
Prof.
Frédéric Mayet
(LPSC)
6/4/19, 10:00 AM
The main limiting factor of cosmological analyses based on thermal Sunyaev-Zel’dovich (SZ) cluster statistics comes from the bias and systematic uncertainties that affect the estimates of the mass of galaxy clusters.
High-angular resolution SZ observations at high redshift are needed to study a potential redshift or morphology dependence of both the mean pressure profile and the...
Mr
Florian Kéruzoré
(LPSC Grenoble)
6/4/19, 11:30 AM
The NIKA2 SZ large program (LPSZ) was designed to take advantage of the NIKA2 high angular resolution and large eld of view to help us improve our knowledge of galaxy clusters. It consists in observing ∼50 clusters from intermediate to high red- shift (z ∈ [0.5, 0.9]) to re-compute the relations needed for cluster-based cosmological analysis, i.e. the mean pressure pro le of the intra-cluster...
Mr
Herve Bourdin
(University of Rome "Tor vergata")
6/4/19, 11:55 AM
Complementarily to X-ray observations, the thermal SZ effect is a powerful tool to probe the baryonic content of galaxy clusters from their core to their peripheries. While contaminations by astrophysical (Galactic and extragalactic thermal dust) and insrumental backgrounds require us to scan the thermal SZ signal across various frequencies, the multi-scale nature of cluster morphologies...
Dr
Stefano Ettori
(INAF-Osservatorio di Astrofisica e Scienza dello Spazio in Bologna)
6/4/19, 1:30 PM
Galaxy clusters are dark-matter dominated systems enclosed in a volume that is a high-density microcosm of the rest of the universe.
What is their true mass scale? What are the statistical properties of the representative population? How does their detectability depend on baryon physics?
We have learned a lot on these fundamental questions with our current projects, like XMM-Newton Cluster...
Dr
Dominique Eckert
(University of Geneva)
6/4/19, 2:00 PM
X-ray and Sunyaev-Zeldovich observations provide independent and complementary ways of determining the properties of the intracluster medium (ICM). Joint reconstructions of galaxy cluster properties combining X-ray and SZ data are clearly superior to similar analyzes based on one observable only, since the two methods have a different radial dependency and probe different thermodynamic...
Anna Silvia Baldi
(Sapienza University of Rome)
6/4/19, 2:30 PM
The imaging of galaxy clusters through the Sunyaev-Zel'dovich effect is a valuable tool to probe
the thermal pressure of the intra-cluster gas especially in the outermost regions, where X-ray observations
suffer from photon statistics.
For the first time, we produce maps of the Comptonization parameter by applying a locally parametric algorithm for
sparse component separation to the...
Dr
Iacopo Bartalucci
(CEA Saclay)
6/4/19, 4:00 PM
We present the dynamical properties and the individual spatially resolved radial mass profiles of a sample of 77 massive clusters in the [0.05-1] redshift range detected via the Sunyaev-Zel'dovich effect.
For the 5 clusters at z>0.9, we present a method to study such objects that optimally exploits information from XMM-Newton and Chandra observations. The combination of Chandra’s excellent...
Dr
Mariachiara Rossetti
(IASF-Milano/INAF)
6/4/19, 4:30 PM
The Sunyaev-Zeldovich effect provides an observational window to the intracluster medium complementary to X-ray observations, and over the last few years has proved to be a mature technique to efficiently detect and characterize galaxy clusters. For instance, the Planck survey has mapped the whole microwave sky, detecting almost 2000 candidate massive clusters up to z~1, performing the first...
Mr
Antonio Ferragamo
(Intistuto de Astrofísica de Canarias)
6/4/19, 5:00 PM
The abundance of galaxy clusters, per unit of mass and redshift, is a very powerful tool in order to constrain cosmological parameters as the matter density Ωm, and the amplitude of the primordial fluctuation σ8. However, the cluster mass is not an observable. The multicomponent nature of galaxy clusters helps to bypass this problem. In fact, from the observation of each different cluster...
Prof.
Daisuke Nagai
(Yale University)
6/4/19, 5:30 PM
High-resolution spectral imaging observations of the SZ effects promise to provide a vastly broaden view of structure and evolution of galaxy clusters, by enabling unique measurements of thermodynamic and kinematic properties of the cluster gas via thermal and kinematic SZ effects. One of the new frontiers includes the exploration of the extremely low-density regions in the outskirts of galaxy...
Dr
Johannes GOUPY
(CNRS - Institut Neel)
6/5/19, 9:00 AM
The NIKA2 instrument, operating at the IRAM 30-meters telescope, is based on the LEKID array technology dedicated to millimeter wave astronomy. This instrument is composed of one low frequency array for the 120-180GHz range, and two high frequency polarization sensitive arrays for the 220-280GHz range. Since 2013 different versions of the arrays have been developed for NIKA2. We will describe...
Mr
Shibo Shu
(Institut de Radioastronomie Millimétrique)
6/5/19, 9:30 AM
The NIKA2 team are continuously working on improving the performance of the NIKA2 arrays. In this talk, we present our recent developments on the 1mm array from three aspects. Firstly, a small pixel design has been studied to achieve higher angular resolution. Secondly, a thorough simulation and FTS measurements have been performed to understand the frequency response. Thirdly, a capacitor...
Mr
Pranshu Mandal
(University of Tsukuba)
6/5/19, 10:00 AM
We are developing a 100GHz band camera designed for survey of distant galaxies. Field-of-view of this camera is around 3-arcmin, and 100GHz band observation helps peer through the characteristics of very distant galaxies. This is also a prototype for the future 10m Antarctic telescope to survey southern distant galaxies. The focal plane array of this camera is 109 pixel antenna-coupled...
Dr
Charlène LEFEVRE
(Institut de RadioAstronomie Millimétrique)
6/5/19, 11:00 AM
I will introduce NOEMA interferometer, its latest upgrades and capabilities. In particular, I will detail the increase of sensitivity with more antennas, increase of spatial resolution with track extension, and increase of bandwidth with new receiver generation as well as future dual band upgrade. Finally, I will discuss the complementarity between NOEMA and NIKA2 and possible synergies from...
Ivan Delvecchio
(CEA Saclay)
6/5/19, 12:00 PM
The relationship between supermassive black hole (SMBH) accretion and star formation has lead to controversial studies claiming that Active Galactic Nuclei (AGN) activity might both quench and enhance galaxies' star-forming content. Especially at high redshift (z>2), their interplay is still poorly understood, also due to the lack of accurate estimates of star formation rate (SFR) and AGN...
Dr
Philippe André
(CEA Saclay)
6/5/19, 1:30 PM
Herschel imaging surveys of Galactic molecular clouds have emphasized the
quasi-universality of the filamentary structure of the cold ISM and the key
role of filaments in the star formation process. Planck polarization data
moreover suggest that the formation and evolution of star-forming filaments
is at least partly controlled by magnetic fields.
I will summarize the main objectives...
Dr
Alessia Ritacco
(IRAM - Granada)
6/5/19, 2:00 PM
NIKA2 is equipped with a polarization system composed by a multi-mesh half wave plate (HWP) and a polarizer placed at the cryostat stage of 100 mK which transmits and re
ects the two orientation of the linear polarization on two 1mm KID-arrays. The polarizer is needed because the NIKA2 detectors KIDs are unsensitive to the polarization, the warm HWP placed in front of the cryostat window...
Mr
Hamza AJEDDIG
(Département d’Astrophysique (AIM), CEA Saclay, 91191 Gif-sur-Yvette, France)
6/5/19, 2:30 PM
Highlighting the role of magnetic fields in the star formation process is crucial. Observations have already shown that magnetic fields play an important role in the early stages of star formation. The high spatial resolution (~0.01 to 0.05 pc) provided by NIKA2-Pol 1.2 mm polarimetric imaging of nearby clouds will help us to start clarifying the geometry of the B field within dense cores and...
Dr
Jean-François Robitaille
(IPAG - Univ. Grenoble Alpes)
6/5/19, 2:55 PM
Observations of the polarised dust emission with Planck and the future SPICA at large scale and with ALMA, SCUBA2 and NIKA2 at smaller scales trace the interaction between the magnetic field and the denser part of the ISM as molecular clouds and star formation regions. However, a clear interpretation of the Stokes parameters Q and U, and of the associated polarisation vector P, is difficult....
Dr
Alessia Ritacco
(IRAM - Granada)
6/5/19, 3:55 PM
NIKA, the NIKA2 pathnder, was equipped of a room temperature polarization system (a half
wave plate and a grid polarizer facing the cryostat window). This polarization system was the test bench for the NIKA2 polarimeter and was used during few observational/technical campaigns between 2014 and 2015. In particular during the last observing week of NIKA at the IRAM 30m telescope, in February...
Prof.
Gustavo Yepes
(Universidad autónoma de Madrid)
6/6/19, 9:00 AM
Galaxy clusters are the most massive gravitationally collapsed objects in the Universe. They are also the most rare objects and, therefore, large computational volumes have to be simulated if one wants to obtain a statistical significant sample of such objects that can be used to calibrate the global scaling relations, or to understand the possible mass biases due to inaccuracies of the...
Prof.
Marco De Petris
(Dept. of Physics - University La Sapienza)
6/6/19, 9:30 AM
The NIKA2 Sunyaev-Zel'dovich Large Program (LPSZ) is focused on mapping the thermal SZ signal of a representative sample of selected Planck and ACT clusters spanning the redshift range 0.5 < z < 0.9. Clusters science implementation to Cosmology can be biased due to inaccurate knowledge of IntraCluster Medium (ICM) pressure profiles in shape, scatter and redshift evolution.
Hydrodynamical...
Dr
Boris Bolliet
(The University of Manchester)
6/6/19, 10:30 AM
In this talk we review the formalism for the modelling of the Sunyaev Zeldovich (SZ) power spectrum and cluster counts and how to compare them with observations. We outline their dependencies on cosmological parameters, as well as the mass bias associated with the X-ray calibration of the cluster masses. We outline the role played by the pressure profile of the intra cluster medium, for...
Prof.
Rashid Sunyaev
(Max Planck Garching)
6/6/19, 11:30 AM
Our Universe is filled by cosmic microwave background radiation (CMB)
which is extremely isotropic and has excellent black body spectrum with
temperature 2.7 Kelvin and no spectral deviations from black body are
detected in the CMB monopole till now. But 50 years ago it was recognised
that "shadows" in the angular distribution of CMB in the directions where clouds
of very hot ...
Dr
Jean-François Lestrade
(Observatoire de Paris)
6/6/19, 2:00 PM
Planets and planetesimals are formed in the gas- and dust-rich protoplanetary disks surrounding nascent stars in the first 10 Myr of their life. Planetesimals belts, or debris disks, that remain afterward are unique objets to study planetary systems that have evolved from these primordial structures. On one hand, optical/IR observations reveal small sized grains that are partly blown out the...
Ms
Lea Bonnefoy
(LESIA/LATMOS)
6/6/19, 2:30 PM
Saturn’s icy satellites, which are in synchronous rotation around Saturn, often present a different albedo on their leading and trailing sides, which interact differently with Saturn’s dusty rings. Because longer wavelengths probe deeper into the subsurface, observing both sides at a variety of wavelengths indicates possible changes in thermal and physical properties with depth. The Cassini...
Mr
Alessandro Fasano
(Institut Néel)
6/6/19, 4:30 PM
Mapping millimetre continuum emission of the astronomical sky has become a key issue in modern multi-wavelength astrophysics as such mapping is required to tackle a series of very important questions related to cosmology, galaxy evolution, formation of individual and clustered starts and finally the nature of circumstellar envelops and disks. In
particular the spectro-imaging at low...
Prof.
Guilaine Lagache
(LAM)
6/6/19, 5:00 PM
CONCERTO is a new instrument planned to be installed in the APEX Cassegrain Cabin in early 2021. It is a spectrometer with an instantaneous field of view exceeding 300 Sq. arcmin. and a spectral resolution of 1.5 GHz. It covers the frequency band 120-360 GHz. The main scientific aim of CONCERTO is to map in three dimensions the fluctuations of the CII line intensity in the reionisation and...
Alexandre Beelen
(Institut d'Astrophysique Spatiale / Laboratoire d'Astrophysique de Marseille)
6/7/19, 9:30 AM
More than half of the photons emitted by stars across cosmic times have been absorbed by cosmic dust and re-emitted in the far-infrared and millimeter wavelength domain. Herschel and ALMA revealed that very massive and very dusty galaxies already exist in the early Universe (up to z~7). These objects are one of the keys to understand the formation of the most massive galaxies. However, these...
Mr
Maximilien FRANCO
(DAp CEA-Saclay)
6/7/19, 10:00 AM
We will present the latest results of a 69 arcmin2 ALMA survey at 1.1mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band observed region of the GOODS-South field. We have extracted two catalogs, one of galaxies purely selected by ALMA, from which we have identified sources both with and without HST counterparts, and another catalog based on priors. Our wide contiguous survey allows us to push...
Dr
Nicolas Peretto
(Cardiff University)
6/7/19, 11:00 AM
Over the last decade, Herschel observations of the Galactic interstellar medium have transformed our understanding of the early stages of star formation. At the low-mass end of the stellar initial mass function (IMF), a paradigm has emerged in which low-mass cores – the progenitors of stars with masses from ~0.1 to a couple of solar masses – are thought to form as the result of gravitational...
Dr
Bilal Ladjelate
(IRAM Granada)
6/7/19, 11:30 AM
From molecular clouds to young stellar objects, every step in the evolution of young stars can be observed in the millimetric range.
As part of the NIKA2 (Adam et al. 2018) Large Program GASTON (PI: Nicolas Peretto), we observed at 1.2mm and 2mm the Ophiuchus Molecular Cloud. The dual band capabilities of NIKA2 allow us to understand the properties of dust in star-forming regions, and their...
Dr
Charlène LEFEVRE
(Institut de RadioAstronomie Millimétrique)
6/7/19, 12:00 PM
Dust is the only tracer that is present from the edge of the interstellar cloud to the densest part, inside which stars and planets will form, named pre-stellar cores. It allows to trace the density structure of the cloud, of the core(s), and of the subsequent protoplanetary disk where it becomes a major actor of the planet formation. Dust grains evolve from bare simple elongated shape in the...
Dr
Gabriel Pratt
(CEA Saclay, Département d'Astrophysique)
The total mass of a galaxy cluster is one of its most fundamental properties. Together with the redshift, the mass links observation and theory, allowing us to use the cluster population to test models of structure formation and to constrain cosmological parameters. I summarise the state of the art in cluster mass estimation methods, with particular emphasis on SZ measurements and their...
