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Rubin LSST-France, LPNHE, 28-30/11/2022

28–30 nov. 2022
Laboratoire de physique nucléaire et des hautes énergies (LPNHE)
Fuseau horaire Europe/Paris

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Liste des Contributions

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  1. 1. Bienvenue au LPNHE
    Pierre Antilogus (LPNHE)
    28/11/2022 13:30
  2. 20. Project and camera update
    Claire Juramy (LPNHE/CNRS), Pierre Antilogus (LPNHE)
    28/11/2022 13:35
  3. 22. Communication/EPO
    Gaelle Shifrin (Centre de Calcul de l'IN2P3)
    28/11/2022 14:05
  4. 21. DESC
    Celine Combet (LPSC), JOHANN COHEN-TANUGI (LUPM, Université de Montpellier)
    28/11/2022 14:15
  5. 23. LSST@Europe summary
    Alexandre Boucaud (APC / IN2P3), Cécile Roucelle (APC)
    28/11/2022 14:25
  6. 24. Lightning talks from new members
    Cyrille Doux (LPSC)
    28/11/2022 14:35
  7. 25. Computing news and tools for data analysis
    Dominique Boutigny (LAPP), Fabio Hernandez (CC-IN2P3), Gabriele Mainetti (CC-IN2P3), Quentin Le Boulc'h (CC-IN2P3)
    28/11/2022 15:30
  8. 15. LSST Observing Strategy: status and plan
    Dr Philippe Gris (LPC)
    28/11/2022 16:30

    This presentation will include recent developments of LSST observing strategy presented during the last SCOC workshop in november. The current contours of the LSST observing strategy and the action plan for the next coming months will be shown.

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  9. 5. PFS : a wide field spectrograph on Subaru.
    stephane arnouts (LAM)
    28/11/2022 17:00

    PFS is a unique wide field multiplex spectrograph with a 1.3 deg$^2$ f.o.v. and covering the wavelength domain: 0.38-1.26$\mu$m. PFS will start operating mid 2024. It will perform a 360 nights survey with three components: a cosmology survey to investigate the dark sector; an archeology survey for the origin of the milky way and nearby dwarf galaxies; a galaxy evolution survey to reveal the...

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  10. 9. Multiview Symbolic Regression : learning equations behind examples
    Etienne Russeil
    28/11/2022 17:30

    Symbolic Regression is a data-driven method that searches the space of mathematical equations with the goal of finding the best analytical representation of a given dataset. It is a very powerful tool, which enables the emergence of underlying behavior governing the data generation process. Furthermore, in the case of physical equations, obtaining an analytical form adds a layer of...

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  11. 4. Galaxy cluster mass reconstruction using weak lensing shear multipoles
    Constantin Payerne (LPSC (IN2P3))
    29/11/2022 09:00

    Weak lensing is a powerful tool to estimate the matter distribution around massive galaxy clusters. In general, such effect can be measured by estimating the averaged tangential shear of background galaxies in circular annuli from the lens center. In addition to the average tangential shear, valuable informations on the underlying dark matter distribution can be extracted by using shear...

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  12. 7. Impact of blending on galaxy clusters using DC2 catalogs
    Manon Ramel (LPSC / IN2P3)
    29/11/2022 09:20

    Galaxy clusters trace the highest peaks in the density of the Universe. Therefore, their abundance is a powerful probe to constrain cosmological parameters, expansion of the Universe and give information on the growth of structures. However, since the density of galaxies is significantly higher, these latter may appear to overlap on the line of sight and have their respective fluxes blended....

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  13. 11. Galaxy cluster detection on LSST simulated images using convolutional neural networks
    Kirill Grishin (Universite de Paris)
    29/11/2022 09:40

    The distribution of galaxy clusters, the largest gravitationally bound structures in the Universe, helps us to estimate fundamental constants and constrain different cosmological models. With the expected development and commissioning of astronomical instruments, such as LSST, in the next decade, the depth of imaging data for a significant area of the sky will allow us to select nearly...

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  14. 38. Towards new approaches to cluster detection for cosmology
    Vincent Reverdy (Laboratoire d'Annecy de Physique des Particules)
    29/11/2022 10:00

    Galaxy clusters and dark matter halos constitute a building block of many cosmological analyses. However, amongst simulations and observations, there is a wide variety of definitions of what a cluster is from a physical standpoint that do not necessarily match with each other. On top of that, on the algorithmic side, detection strategies can vary greatly from traditional friend-of-friend...

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  15. 6. Photometric redshift with Deep Learning technique: Application to HSC Deep Survey
    Reda AIT OUAHMED
    29/11/2022 10:20

    Convolutional Neural Networks have recently shown high performances in measuring photometric redshifts in the local SDSS surveys. Extending this technique at higher redshift remains a challenge due to the lack of representativity of the training set for faint sources. In this talk we apply this technique on the state-of-the-art HSC deep imaging survey (with UgrizY photometry down to i~26.5),...

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  16. 35. Fink: status
    Julien Peloton (CNRS-IJCLab)
    29/11/2022 14:00

    Roadmap, overview of the status

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  17. 36. Microlensing
    Petro Voloshyn (IJCLab/Université Paris-Saclay)
    29/11/2022 14:15
  18. 37. Enabling the discovery of fast transients
    Biswajit Biswas (APC)
    29/11/2022 14:30
  19. 8. Finding active galactic nuclei through Fink
    Etienne Russeil
    29/11/2022 14:45

    The Fink broker contains a series of machine learning based modules, which enables fast processing of the data stream. We present the Active Galactic Nuclei (AGN) module as currently implemented within the Fink broker. It is a binary classifier based on a Random Forest algorithm using features extracted from photometric light curves, including a color feature built using a symbolic regression...

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  20. 29. Fink Pair Instability Supernovae classifier
    Etienne Russeil
    29/11/2022 15:00

    Pair-instability supernovae (PISN) are stellar explosions marking the end of life of the first generation of stars to exist in our Universe. Despite being theoretically predicted, up to this point there are no confirmed PISN observations.
    The ELAsTiCC challenge, which anticipates data to be generated by the Rubin observatory, will contain a significant amount of PISN. We present a PISN...

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  21. 17. Identification of optical Orphan Gamma-Ray Burst Afterglows in Rubin LSST data with the alert broker FINK
    Marina Masson (LPSC)
    29/11/2022 15:15

    Gamma-Ray Bursts (GRBs) are among the most energetic phenomena in the Universe. The interaction of their blast wave with the Interstellar Medium produces an afterglow that can be observed from a larger angle, in a wide range of the electromagnetic spectrum and during more time than the prompt emission. Viewed off-axis, this emission has a negligible gamma-ray flux and is hence called ”GRB...

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  22. 34. Early supernovae Ia classification using active learning
    Marco Leoni (Universite Paris Saclay)
    29/11/2022 15:30

    We describe how the Fink broker early supernova Ia classifier optimizes its ML classifications by employing an active learning (AL) strategy. We demonstrate the feasibility of implementation of such strategies in the current Zwicky Transient Facility (ZTF) public alert data stream. We compare the performance of two AL strategies: uncertainty sampling and random sampling. Our pipeline consists...

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  23. 27. The ELAsTiCC data challenge: preparing the Fink broker for LSST
    Emille Ishida (CNRS/LPC-Clermont)
    29/11/2022 15:45

    Fink is a community alert broker specifically designed to operate under the extreme data volume and complexity of the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST). It is a French-led international collaboration whose task is to select, add value and redistribute transient alerts to the astronomical community during the 10 years of LSST. The system is completely...

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  24. 33. Tutorial on DASK
    Dominique Boutigny (LAPP)
    29/11/2022 16:30
  25. 28. Forward modelling the large-scale structure: field-level and implicit likelihood inference
    Florent Leclercq (Institut d'Astrophysique de Paris)
    29/11/2022 17:00

    While the next generation of surveys soon starting will generate orders of magnitude more data than previously, it is becoming increasingly clear that traditional techniques are not up to the challenge of fully exploiting the raw data. The last few years have seen vast progress in the field of probabilistic large-scale structure inference, which differs in intent from traditional measurements...

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  26. 30. Cosmology with ZTF
    Mathew Smith (IP2I/IN2P3/CNRS)
    30/11/2022 09:00

    LSST, with 100,000 SNeIa, is the future of supernova cosmology. However, LSST alone cannot constrain the equation-of-state of Dark Energy: a nearby sample is needed to anchor the Hubble diagram. With measured distances to 6000 SNeIa, and unbiased to z<0.05, the Zwicky Transient Facility (ZTF) ZTF will be the primary anchor for all cosmological analyses with LSST.
    With over 3000 SNeIa already...

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  27. 3. Astrophysical biaises affecting the measure of the Hubble-Lemaître constant with SNe Ia
    Madeleine Ginolin (IP2I)
    30/11/2022 09:20

    I will present SNe Ia standardization and its environmental dependence in the case of the ZTF DR2 sample.

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  28. 13. DP0 tutorial on survey property maps and systematics corrections
    Martin Rodriguez Monroy (IJCLab)
    30/11/2022 09:40

    In this presentation we will see some examples of survey property maps, maps that track spatial variations concerning the imaging of the survey. We will use healsparse to visualize and manipulate them. In addition to this, we will discuss how to evaluate the impact that different observing conditions can have on data. In particular, we will see some examples of 1D relations, which are the...

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  29. 32. Photometric redshifts with DP0
    Dr Sylvie Dagoret-Campagne (IJCLab)
    30/11/2022 10:10
  30. 14. Focal plane calibration: status and plans
    thibault guillemin (LAPP)
    30/11/2022 11:00

    Summary of focal plane calibration activities at IN2P3

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  31. 18. Le télescope auxilliaire (AuxTel)
    marc moniez (LAL-IN2P3)
    30/11/2022 11:20

    Le spectrographe du télescope auxiliaire (AuxTel) a pour mission de mesurer les paramètres de transparence de l’atmosphère en fonction de la longueur d’onde, pour en déduire des corrections de couleur de la photométrie issue du télescope principal.
    Les outils en cours de développement seront brièvement décrits : production de flat-fields spéciaux, réduction de spectres, procédures de...

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  32. 16. Collimated Beam Projector status
    Jérémy Neveu (LPNHE), Thierry Souverin
    30/11/2022 11:40

    The Collimated Beam Projector (CBP) is a new device to measure instrumental throughput of a telescope. We will detail the performance of a CBP version built at LPNHE and show that we reach a permil calibration of the CBP throughput itself thanks to a calibrated solar cell, and of the StarDice telescope. We will present news from the Rubin Obs. CBP under construction.

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  33. 19. Update on CCOB Narrow Beam data taking preparation and data analysis
    Johan Bregeon (IN2P3 LSPC)
    30/11/2022 12:00

    The CCOB narrow beam has been developed and built in the past several years at LPSC Grenoble with the goal to obtain a thin monochromatic beam of calibrated light useful to characterize the Rubin camera optic transmission and internal geometrical alignment.
    I will give a brief overview of the apparatus and present the current data taking and data analysis strategy based on ray tracing simulations

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  34. 12. Discussion about flat-fielding and/or about colour corrections with AuxTel
    Martin Rodriguez Monroy (IJCLab)

    I propose to have a discussion about any or both of these topics.

    • Special flat-fielding for spectroscopy with AuxTel
    • Colour corrections using calibration spectra and observations with AuxTel
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  35. 2. Final words
  36. 10. Participation à des discussions relatives à la calibration atmospherique et DM
    Mme Sylvie Dagoret-Campagne (IJCLab)

    Bonjour,

    Je propose de participer à une discussion autours de mon expérience avec
    DM au CC & USDF

    • bias et flats @ auxtel
    • reconstruction des spectres
    • propriétés de l'hologramme.
    • extraction des paramètres atmosphériques
    • modélisations atmospherique.

    Concernant DP0, je peux faire un tuto PhotoZ après la présentation de Martin sur les Survey Properties MAP.

    Mais...

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