Rubin LSST-France, CPPM Marseille, 10-12/06/2024
CPPM
The next biannual meeting of the Rubin-LSST France community will be held 10-12 June 2024, at Hexagone on the Luminy campus near CPPM in Marseille.
Details
- Meeting will begin at 3pm on Monday 10 June.
- Meeting ends around 3:30pm on Wednesday 12 June.
- The persons of contact for the meeting will be TBD.
Social events
- Social dinner at Restaurant de l'UNM - 34 Boulevard Charles Livon
13007 Marseille on Tuesday 11 June at 8pm.
Information about talks
- Language: Acknowledging that some participants may not understand/speak French, using English is strongly encouraged.
- Speakers: please upload your slides on this website prior to your talk.
Remote attendance
- It will be possible to follow the meeting over Zoom, but please only register for in-person attendance.
- Zoom link for plenary sessions: TBD
Code of conduct
Venue information
The meeting will take place in the Hexagone on the Luminy Campus. The address is 172 Av. de Luminy, 13009 Marseille, France
- From the city center, take the M2 metro to « Rond Point de Prado », take a look at the vélodrome (allez l’OM !).
- Take the bus B1 or the express 21-jet (less frequent).
- Go down at Luminy Faculté.
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If you arrive early or leave late, you can grab a sandwich at the hexagone’s cafeteria and do a quick hike to the calanques: for instance going to Beleverdère de Sugiton in ~30 minutes. With 30 more minutes you can go down to the sea in Sugiton.
Previous Events
The agendas of the most recent editions of this meeting can be found online:
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General news and updates: General
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2
EDIM committeeOrateurs: Dr Gabriele Mainetti (CC-IN2P3), Madeleine Ginolin (IP2I/IN2P3/CNRS), Marina Ricci
- 3
- 4
- 5
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6
LSST-France communicationOrateur: Gaelle Shifrin (Centre de Calcul de l'IN2P3)
- 7
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16:15
Coffee break
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Science talks
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8
Source photo- and morpho-metry with SourceXtractor++ in Euclid ERO data
I will present some results from the Euclid Early Release Observations obtained in the field of the lensing cluster A2390 in order to highlight the merits of model photometry and morphometry using SourceXtractor++ code.
Orateur: Dr Raphael Gavazzi (LAM CNRS) -
9
Rubin LSST data access and analysis via the Rubin Science Platform, an overview.
In this presentation, we will describe how to access Rubin data using the Rubin Science Platform (RSP). We will cover the general features of the RSP: the notebook aspect for the interactive analysis and the portal aspect to inspect catalogs and images.
Finally, we will describe the different data accessible through three different instances of the RSP (USDF, CC-IN2P3 and IDF).Orateur: Dr Gabriele Mainetti (CC-IN2P3) -
10
Feedback from LSST-France focal plane commissioning workshop at LAPP, AnnecyOrateur: thibault guillemin (LAPP)
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11
Updates from the Fink-broker
In this talk, I will describe the most recent updates from the Fink broker, describe the recent developments following the Fink-Brazil Workshop and highlight the actions done towards preparing Fink for the arrival of LSST data.
Orateur: Dr Emille Ishida (CNRS/LPC-Clermont) -
12
Search for dark matter halos in the milky way with stellar streams detected by the Rubin/LSST observatory
Introduction of the French involvement in the DESC official project aiming at connecting observable properties of stellar streams observed with Rubin/LSST to dark matter constraints. Presentation of the analysis preparation examining the impact of dark matter subhalos with masses ranging from $10^6$ to $10^8$ solar masses on simulated stellar streams
Orateur: Matthieu Pelissier
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8
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Parallel sessions: Focal plane
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13
Focal planeOrateurs: Jérémy Neveu (LPNHE), thibault guillemin (LAPP)
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13
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10:45
Coffee break
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General news and updates: Euclid/Rubin synergies
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14
Euclid/Rubin Derived Data Product Implementation Working GroupOrateur: Eric Jullo (LAM)
- 15
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16
DiscussionOrateur: Cyrille Doux (LPSC)
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14
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12:30
Lunch
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Science talks: Observing strategy & clusters
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17
A Cohesive Deep Drilling Field Strategy for LSST Cosmology
This presentation will summarize a work recently achieved in DESC about the design of a cohesive DDF strategy fulfilling requirements from PZ, WL, SNe Ia and accounting for the SCOC recommendations.
Orateur: Philippe Gris (LPCA) -
18
Search for Orphan GRB Afterglows in Rubin LSST data
Orphan gamma-ray burst afterglows are good candidates to learn more about the GRB physics and progenitors or for the development of multi-messenger analysis with gravitational waves. Our objective is to identify orphan afterglows in Rubin LSST data, by using the characteristic features of their light curves. We present here the performance of our machine learning filter as implemented in the Fink broker and tested on the ELAsTiCC data set and our own simulations of orphan afterglows.
Orateur: Marina Masson (LPSC) -
19
The DESC cluster weak lensing mass library v2.0
Accurate cluster mass estimates are vital for constraining cosmology with galaxy cluster abundance, one of the primary cosmological probes on LSST. We present here the second version of the Cluster Mass Modeling (CLMM) library, developed for the Dark Energy Science Collaboration (DESC), for calibrating cluster masses based on the weak lensing signal of background galaxies. This library is being developed by a large group of young career scientists with complete documentation and automatic testing, which makes the assumption of the computations transparent and the results reproducible. The new version of CLMM includes the functions for stacking clusters and more flexibility for different formats of photometric redshift inputs besides further implementations on the theoretical modeling and data operations.
Orateur: Dr Michel Aguena (APC) -
20
Effect of Photo-z Performance on Clusters
Photo-z’s are a key component for some of the current DESC cluster finders, AMICO and WaZP. In this talk we discuss the effect of photo-z performance on WaZP cluster detection using the new TPZ produced photo-z catalog. We also explore the possibility of optimizing the photo-z training set towards “cluster-focused” samples.
Orateur: Rance Solomon (LAPP) -
21
YOLO-CL cluster detection in the Rubin/LSST DC2 simulations
Galaxy clusters serve as powerful probes for cosmological models. Upcoming large-scale optical and infrared surveys will reach unprecedented depths across extensive areas, necessitating highly complete and pure cluster catalogs with well-defined selection functions. We have developed a novel cluster detection algorithm called YOLO-CL. This algorithm is a modified version of the state-of-the-art object detection deep convolutional network YOLO, specifically optimized for galaxy cluster detection (Grishin, Mei, Ilic 2023). It has been adapted to the datasets from the forthcoming LSST by training on a combined sample of observed SDSS clusters and simulated galaxy cluster images from the DESC Data Challenge 2 (DESC DC2).
The YOLO-CL cluster catalog achieves 100% and 94% completeness for halo masses $M_{200c} > 10^{14.6} M_{\odot}$ at $0.2 < z < 0.8$, and $M_{200c} > 10^{14} M_{\odot}$ with redshifts $z \lesssim 1$, respectively, with only a 6% false positive rate. Additionally, we found that the YOLO-CL selection function is nearly flat with respect to halo mass within the range $0.2 \lesssim z \lesssim 0.9$. Our paper detailing the performance of YOLO-CL on DESC DC2 simulated images (Grishin, Mei, Ilic, Aguena, Boutigny et al.) has been submitted for internal review within the DESC collaboration.
Orateur: Kirill Grishin (Universite de Paris) -
22
The Rubin Galaxies Science Collaboration
We will present the Rubin Galaxies Science Collaboration, show recent activities and results and explain how to apply for membership.
Orateur: Simona Mei
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17
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16:00
Coffee break
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Parallel sessions: Science validation and commissioning
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23
Science validation and commissioningOrateur: Cyrille Doux (LPSC)
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23
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Parallel sessions: Extra session: LSST-France communication
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19:00
Free time
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20:00
Social dinner Restaurant de l'UNM
Restaurant de l'UNM
34 Boulevard Charles Livon 13007 Marseille
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Parallel sessions: AuxTel & Clusters
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24
AuxTel Salle CIELL (Héxagone)
Salle CIELL
Héxagone
Orateurs: Dr Sylvie Dagoret (IJCLab), marc moniez (LAL-IN2P3) -
25
Clusters Auditorium (Héxagone)
Auditorium
Héxagone
Orateur: Marina Ricci
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24
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10:45
Coffee break
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Science talks
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26
Surrogate M1M3 dynamic tests
The M1M3 glass mirror is now on site and has been installed on its cell and coated. Before installing the M1M3 glass mirror on the Rubin telescope, we proceeded to confirm the safety of the glass using a surrogate mirror on the telescope mount, and to verify accordance with specifications. Designed to be used for tests, the surrogate has similar mechanical properties as the glass mirror, such as mass, centre of gravity, and geometry.
The M1M3 steel surrogate was installed on the cell and on the telescope mount (TMA) in May 2023. The cell was fully equipped with the force actuators, hardpoints and various monitoring sensors. An extensive dynamic testing campaign took place until February 2024, when the surrogate and cell were dismounted from the TMA for the reception of the M1M3 glass mirror.
The test campaign was configured to validate the safe and dynamic telescope capabilities.
We also checked the position repeatability before and after a slew for different azimuth, elevation and speeds. We also investigated possible M1M3 surrogate vibrations due to the Fan Coil Units (FCU), which could have an impact on image quality.
Analysis was done on data taken during this period with dedicated dynamic tests. However, more data will be needed for the vibration analysis.
Results show that the position repeatability is almost within specifications, and that vibrations due to FCUs can be neglected.Orateur: Andrea JEREMIE (LAPP-CNRS/IN2P3-Univ. de Savoie-Mont-Blanc) -
27
CCOB Narrow Beam EOTest ghosts analysis for alignment
I'll present results of the analysis of narrow beam electro-optical tests for the alignment of the camera optics.
Orateur: Dr Johan Bregeon (IN2P3 LSPC) - 28
- 29
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26
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12:30
Lunch
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Science talks
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30
Stellar Population Synthesis & templates for photometric redshifts
I will present the continuation of our work on photometric redshifts using templates derived from observed spectra, extended using Stellar Population Synthesis methods.
The prospects of this work - and potential for improvement - for future studies will be presented and discussed during the talk.Orateur: joseph chevalier (IJCLab - A2C) -
31
Cosmic Shear Simulations for Higher-Order Statistics
Our main goal is to provide with new cosmic shear and LSS simulations that can be used for the analysis of LSST Y1 data with Higher-Order Statistics. In this presentation, we make an update on the status of the project.
Orateur: Juan Mena Fernandez (LPSC) -
32
Towards Enabling Automatically Differentiable and distributed Particle-Mesh N-Body simulations
A series of recent works has highlighted the potential of so-called full-field cosmological inference for the analysis of upcoming weak lensing and galaxy clustering surveys, with the promise of being able to access the non-gaussian information contained in the data. However, these approaches require a differentiable forward model of the large scale structure, which currently constitutes one of the main bottlenecks, as none of the publicly available differentiable N-body codes support large-scale distribution necessary for large cosmological volumes.
To address this, we introduce JAXPM, a JAX-powered library that facilitates multi-GPU and multi-node Particle-Mesh N-body simulations. Leveraging the capabilities of a low-level CUDA distributed computing library, JaxPM allows for the first time the simulation of the entire cosmological volume observed by LSST down to Mpc resolution with an automatically differentiable simulation code.
We will present our early scaling tests of this approach on the Jean-Zay GPU supercomputer.Orateur: Wassim KABALAN (CNRS APC/IN2P3) -
33
DC2 bright stars masks
The presence of bright objects, notably stars, represents a significant challenge in extracting valuable insights from LSST data. Bright objects will cause the saturation of LSST’s sensors and will bias both object detection and flux measurement in a radius which depends on the magnitude. The creation of masks to cover the most affected regions by bright stars is necessary but challenging due to the difficulty in identifying and characterizing those objects. Our work is based on the HSC-SSP method and is applied to the DC2 object catalog. The resulting masks cover about two percent of the DC2 footprint. The impact of these masks is currently being studied in DESC in the context of galaxy cluster detection algorithms such as AMICO and redMaPPer.
Orateur: Nathan Amouroux
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30
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