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Series IV: Outlines, Titles and Abstracts of presentations

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Euclid

SOC:

Captain: Chao Ma

Outline:

speaker-1

Title: Probing galaxy morphology evolution with Euclid multi-band wide imaging survey

Abstract: Already launched in July 1 this year, Euclid is a 1.2m-diameter space telescope providing high-quality visible and near-infrared imaging, and slitless spectroscopy. During its six-year nominal mission Euclid will carry out a wide imaging and spectroscopy survey covering approximately 15,000 deg^2 of extragalactic sky. Beyond the cosmological core science, Euclid will greatly advance our understanding of galaxy formation and evolution, thanks to its catalog of billions of galaxies and a massive legacy of deep images and spectra. In this talk, I start with giving a brief overview of Euclid instruments. Then I will focus on introducing its multi-wavelength (I+Y+J+H) wide imaging survey, data properties, photometric pipeline for catalog assembly, and phot-z measurements. Finally, I will discuss various applications of these tremendous data resources to galaxy research, focusing mainly on morphology evolution in clusters. The content includes how cluster dense environment affects galaxy morphology transformation (i.e., Morphology-density relation and Butcher-Oemler effects), and correlations with host cluster properties. I will also introduce ICL physics that Euclid could probe, involving formation mechanism, redshift evolution, and coevolution with BCGs.

Reference: Scaramella et al. 2022; Merlin et al. 2022; Desprez et al. 2020; Bretonnière et al. 2022

speaker-2

Title: Euclid's view of massive galaxy growth from cosmic noon to the present day

Abstract: In the coming years, Euclid will provide us with high-quality imaging and slitless spectroscopy that cover around 15,000 deg^2 of extragalactic sky. Thanks to the unprecedented combination of survey area, spatial resolution, and depth, Euclid can resolve the stellar populations of all galaxies within ～5 Mpc and explore the nearby universe under a surface brightness limit of ～29.5 mag/arcsec^2. At higher redshift (z～2), Euclid will significantly increase the sample size of galaxies and deliver their morphologies, masses, and star-formation rates. These features will facilitate studies on the assembly of galaxies over a large portion of cosmic time. In this talk, I will focus on the contribution of galaxy mergers to the growth of massive galaxies and how Euclid will take a role. I will start with an overview of Euclid's instrumentation and its capabilities. Then, I will introduce the observable signatures of galaxy mergers before and after the coalescence, followed by a summary of how these signatures can be identified and characterized. Finally, I will discuss the connections between galaxy interactions and the star formation activity within galaxies.

Reference: Scaramella et al. 2022; Borlaff et al. 2022; Euclid galaxy evolution workshop 2022

Roman

SOC:

Captain: Chao Ma

Outline:

speaker-3

Title: Nancy Grace Roman Space Telescope: Studying Galaxy Evolution on Multiple Scales

Abstract: Currently planned to be launched in late-2026, the 2.4 m Nancy Grace Roman Space Telescope would cover an area of at least 1700 sq deg with its Wide Field Instrument (WFI). WFI near-infrared imaging (four bands over 0.93—2.00 μm) and slit-less (grism and prism) spectroscopic data from the Roman observation programs would be used to address the key science themes including large-scale structure (LSS) growth and distribution of dark matter via weak lensing. Along the way, Roman would enable studies of galaxy formation and evolution in the context of LSS up to $z > 2$. For nearby galaxies, Roman would also provide opportunities to extend resolved stellar populations studies thus detailed star formation histories to a statistical sample of galaxies. In the present talk, I am to briefly introduce the timeline, instruments and major observation programs of the mission. Then, I am to introduce how the aforementioned galaxy sciences, on cosmological and resolved scales, would be made possible by the capability of Roman as well as by synergies with other surveys such as HSC or LSST.

Reference: Spergel et al. 2015; Mantz et al. 2019; Lancaster et al. 2020; Drakos et al. 2022; Harikane et al. (2023; CCS white papers); Kodama et al. (2023; CCS white papers); Rudnick et al. (2023; CCS white papers); Williams et al. (2023; CCS white papers).

speaker-4

Title: Nancy Roman Space Telescope: A Glance Into Cosmic Dawn

Abstract: The Nancy Roman Space Telescope (WFIRST) is a near-Infrared wide-field survey telescope planning to be deployed at the Sun-Earth L2 orbit in 2026. Equipped with a wide field instrument (WFI) and a coronagraphic Instrument (CGI), Roman will survey 2000 square degree of the sky with both imaging and slitless spectrum coverage. This planned program will make major contributions towards probing the nature of dark energy, exploring the origin and evolution of galaxies, as well as discovering planets around other stars. In this talk, I will mainly focus on the ability of Roman for probing the high-z universe. I will start with a brief introduction regarding the WFI imaging and spectroscopic component, followed by a demonstration of their ability to discover great number of high-z galaxies due to increased depth and survey area. Then, combining previous works from HST and JWST, I will discuss further about the capability of Roman in identifying powerful emission-line galaxies and quasars, measuring star formation rate as well as quantifying Lyα escape fraction at cosmic dawn.

Reference: Spergel et al. 2015; Rachel et al. 2019; Ryan et al. 2019;

speaker-5

Title: Probing the mass function of early massive black holes through detecting tidal disruption events with JWST/RST

Abstract: The mass distribution function of massive black holes (BHs) at high redshifts encodes key information on their growth via accretion. Our current understanding of quasar populations at z>4 significantly benefits from wide-field surveys with ground-based telescopes (e.g., the Sloan Digital Sky Survey). Recently, the unprecedented sensitivity of James Webb Space Telescope (JWST) has enabled the discovery of low-luminosity active galactic nuclei (AGNs) at z~4-7, which were hidden in the pre-JWST era. Spectroscopic follow-up observations have provided estimates of the nuclear BH masses for these sources and pushed the low-mass boundary down to ~106-7 Msun. Although this breakthrough has brought us useful insights on their formation process, the ‘observed’ lowest mass of BHs is still >1-2 orders of magnitude heavier than the typical mass of seed BHs and thus the mass distribution shape remains poorly constrained. In this talk, as a tool of unveiling the presence of low mass BH populations at such high redshifts, I consider UV/optical (in rest frame) flares of stellar tidal disruption events (TDEs) caused by ~105-7 Msun BHs embedded in low- luminosity AGNs. I give a simple derivation of the TDE rate based on the AGN host galaxy properties inferred from JWST observations and discuss the realistic/optimistic survey strategies to hunt for the transient high-redshift TDEs with the ongoing JWST and forthcoming Roman Space Telescope surveys.

Reference: Li et al. (2023) arXiv:2306.06172; Kocevski et al. (2023) ApJL, 954, 4; Maiolino et al. (2023) arXiv:2308.01230; Stone & Metzger (2016) MNRAS, 455, 859; Syler & Ulmer (1999) MNRAS, 306, 35

Rubin (LSST)

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DESI

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PFS

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MOONS

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