Présidents de session
Session: FINK
- Il n'a pas de président de session pour ce bloc
Session: Calibration, Auxtel
- Sébastien Bongard (LPNHE)
Session: Calibration, Auxtel
- Sébastien Bongard (LPNHE)
Session: Calibration, Auxtel
- Sébastien Bongard (LPNHE)
Session: SNe
- Julian Bautista (CPPM)
Session: Photo-z
- Julian Bautista (CPPM)
Session: Clusters
- Raphael Gavazzi (IAP CNRS)
Session: WL
- Raphael Gavazzi (IAP CNRS)
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Dr Anais Möller (CNRS / LPC Clermont), Dr Julien Peloton (CNRS-IJCLab), Dr Emille Ishida (LPC-UCA)26/05/2021 09:30
We will present the Fink broker which has been designed to ingest, enrich and filter the VRO LSST public alert stream. Within minutes, it can select promising transients by providing preliminary classifications and combining information from multiple channels (multi-messenger and multi-wavelength surveys and catalogues). It can also communicate these candidates to teams and follow-up...
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Dr Anais Möller (CNRS / LPC Clermont), Julien Peloton (CNRS-IJCLab), Emille Ishida (LPC-UCA)26/05/2021 09:55
We will show the different capabilities of Fink from the user side. The goal is to provide examples on how you can access or filter the data for a science case. This session will include: (i) how to set up filtering in the real time processing in Fink, (ii) how to access the aggregated data through the Science Portal and (iii) how to use the API. We will use our current processing of the ZTF...
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Marc Betoule (LPNHE)26/05/2021 11:10
Update on the StarDICE project
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Jérémy Neveu (IJCLab)26/05/2021 13:30
Slitless spectroscopy and atmospheric transmission
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marc moniez (LAL-IN2P3)26/05/2021 14:20
Le disperseur holographique développé en France a été installé le 15 février sur le télescope auxiliaire de LSST. Les premières images ont été acquises au Chili lors des prises de données de février et mars. Nous montrerons les spectres issus de ces images et confronterons les premiers résultats avec les performances attendues à partir des mesures du banc de test.
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Philippe Rosnet (Université Blaise Pascal - CNRS/IN2P3)26/05/2021 15:10
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Bastien Carreres (CPPM)27/05/2021 09:30
The growth rate of structures of our Universe depends on expansion history and gravity. It can be used to test the cosmological standard model (LCDM) and as a probe of modified-gravity models.
The evolution of the density and the velocity field of galaxies can be characterised by the fsigma8 parameter. Recent papers (Howlett et al 2017, Graziani et al 2020) suggest that we can use Type Ia ...
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Melissa Amenouche (Laboratoire de Physique de Clermont)27/05/2021 09:50
A large variety of cosmological observations has validated the Λ CDM model as the leading one in driving the dynamics of the Universe. This model requires the validity of several assumptions : the Cosmological Principle (homogeneity and isotropy at large scales). Despite numerous successes, the standard model is facing some challenges like the detection of large scale velocity flows.
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Type... -
Guy Augarde (LPNHE)27/05/2021 10:10
Type Ia Supernova (SN Ia) distance measurements rely on an empirical model of the SN spectrophotometric evolution. This model has two main uses : first, it allows to take into account the effect of SN Ia redshift, by reconstructing the flux emitted in the supernova frame, given the flux measured in the observer frame. Second, it allows one to capture the SN Ia diversity and standardize their...
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Philippe Gris (LPC)27/05/2021 10:30
The Deep Drilling (DD) mini-survey of LSST will be critical for the success of the supernovae science program. This presentation will be a summary of the most recent studies related to this topic.
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olivier Ilbert (LAM), stephane arnouts (LAM)27/05/2021 11:05
We will review the most common photometric redshifts techniques, showing their applications to recent surveys.
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We will split our presentation in two : the first part focusing on SED-fitting techniques (Olivier Ilbert) and the second part on deep learning (Stephane Arnouts). -
Dr Sylvie Dagoret-Campagne (IJCLab)27/05/2021 11:40
We introduce a Gaussian processes as a possible method to estimate redshift from photometric fluxes.
Gaussian processes method is intermediate method between physically constrained SED-templates fitting methods and highly flexible unconstrained fitting method.
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As for ML, it requires to be trained on a training sample, however because it encapsulates physics constraint on the cosmological... -
Michel Aguena (LAPP)27/05/2021 13:30
Galaxy clusters are the largest gravitationally bound structures of the universe with significant applications in astrophysics and cosmology. The Wavelet Z Photometric (WaZP) cluster finder is a code developed for cluster detection on photometric surveys that does not rely on red-sequence presence. As such, it can provide a unique perspective to study the red-sequence abundance and evolution...
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Constantin Payerne (LPSC (IN2P3))27/05/2021 13:55
We present the estimation of the mass-richness-redshift relation for a selection of RedMapper detected clusters in the DC2 catalogs of DESC using weak gravitational lensing. The weak lensing mass estimation is affected by several systematics including the photometrical estimation of background galaxy redshifts & error on galaxy shape measurements. We investigate the effect of increasing the...
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Calum Murray (LPSC)27/05/2021 14:15
In addition to weak lensing shear, information on the mass profiles of galaxy clusters may be inferred from the magnification of galaxies along the line of sight. However such analysis may also be sensitive to the presence of intra-cluster dust, which will act to reduce the magnitude of galaxies. These effects may be differentiated by the chromatic effects of dust extinction and the different...
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Denise Lanzieri27/05/2021 14:55
Weak gravitational lensing is one of the most promising tools of cosmology to constrain models and probe the evolution of dark-matter structures. Yet, the current analysis techniques are only able to exploit the 2-pt statistics of the lensing signal, ignoring a large fraction of the cosmological information contained in the non-Gaussian part of the signal. Exactly how much information is lost,...
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Bastien Arcelin (APC)27/05/2021 15:15
Estimating galaxy shape parameters for weak lensing analysis is a complex task. It usually requires a previous debleding step in order to separate overlapped objects. Following the work we did using Variational AutoEncoders for deblending, we propose a parameter estimation algorithm based on Bayesian neural networks in order to predict posterior distribution of galaxy shapes (and potentially...
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Cyrille Doux (University of Pennsylvania)27/05/2021 15:35
The Dark Energy Survey has scanned 5000 square degrees of the southern sky to assemble a catalog of over 100 million galaxy shapes in Year 3 data. We combined it with catalogs of the positions of "lens" galaxies with accurate redshifts to measure three two-point functions : cosmic shear (shape-shape), galaxy-galaxy lensing (shape-position) and clustering (position-position). In this talk, I...
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olivier Ilbert (LAM)
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