Login

The 2nd Shanghai Assembly on Cosmology and Structure Formation

October 30, 2023 to November 3, 2023
TD Lee Library
Asia/Shanghai timezone

Contact

Session

Galaxy: emissions

Nov 2, 2023, 10:55 AM
Conference Hall (TD Lee Library)

Conference Hall

TD Lee Library

901 Jianchuan Road, Minhang District, Shanghai, 200240

Conveners

Galaxy: emissions

  • Fulai Guo (Shanghai Astronomical Observatory)

Presentation materials

There are no materials yet.

  1. 43. The gas content and dwarf galaxy population in low-z dark matter halos
    Cheng Li (Tsinghua University)
    11/2/23, 10:55 AM
    Galaxy Population
    Talk

    Galaxies are evolving ecosystems of multiple components which interplay with each other and are distributed over a wide range of spatial scale, from sub-galactic scales up to scales of dark matter halos. Our understanding of the galaxy ecosystems has largely been limited to relatively bright galaxies, however. Other components such as gas of different phases as well as dwarf galaxies with...

    Go to contribution page
  2. 56. The hot gas distribution, baryon budget, and mock observations in the semi-analytic model of galaxy formation
    Jian Fu (SHAO)
    11/2/23, 11:20 AM
    Galaxy Formation
    Talk

    We adopt a new kind of one-dimensional model instead of the isothermal sphere to describe the radial distribution of hot gas in the L-Galaxies semi-analytic model. The hot gas halo can be divided into two parts according to the ratio of the local thermal instability time-scale and the free-fall time-scale: a cool core with tTI/tff = 10 and a stable outer halo with tTI/tff > 10. We update the...

    Go to contribution page
  3. 54. AGN luminosities in simulated universe
    Tong Su (National Astronomical Observatories, Chinese Academy of Sciences)
    11/2/23, 11:35 AM
    Galaxy Formation
    Talk

    The study of the spectral energy distribution (SED) of active galactic nuclei (AGN) plays a very important role in several aspects of AGN, such as the physics of black hole (BH) accretion, AGN feedback, and AGN luminosity function (LF). In this work, we explain the observed AGN LF with the SED more physically considered. Specifically, we strictly study the accretion model for a wide range of...

    Go to contribution page
  4. 33. The UV luminosity function at 0.6 < z < 1 from UVCANDELS
    Lei Sun (UCAS)
    11/2/23, 11:50 AM
    Galaxy Formation
    Talk

    UVCANDELS is a HST Cycle-26 Treasury Program awarded 164 orbits of primary ultraviolet (UV) F275W imaging and coordinated parallel optical F435W imaging in four CANDELS fields: GOODS-N, GOODS-S, EGS, and COSMOS, covering a total area of $\sim430$ arcmin$^2$. This is $\sim2.5$ times larger than the area covered by previous UV data combined, reaching a depth of 27 ABmag. We present a robust...

    Go to contribution page
Building timetable...