Search arXiv⌕ Search

arXiv · 2610.19937

The Role of Environment in Shaping the Assembly Timelines of Massive Quiescent Galaxies at Cosmic Noon

Abstract

JWST observations of massive quiescent galaxies (MQGs) at $z\sim2$ have revealed diverse star formation histories (SFHs). In this letter, we investigate whether these variations are linked to the environment in which MQGs reside, as quantified by the host dark matter halo mass. We identify 12 MQGs from a representative sample of galaxies at $1.6<z<3.5$ obtained by the Blue Jay survey, a JWST Cycle 1 program, and infer their SFHs via modelling of the deep NIRSpec medium-resolution spectra along with multi-band photometry. By correlating the formation and quenching epochs of individual MQGs with their respective host halo masses from the 3D-HST survey, we find that after accounting for the redshift range of the sample ($1.8<z<2.5$), MQGs in more massive haloes formed at significantly earlier cosmic epochs. Meanwhile, although these galaxies also quenched earlier overall, the scatter in quenching epochs across similar halo masses indicates that the quenching process likely involves other contributing factors and is not solely determined by halo mass.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Tianmu Gao, J. Trevor Mendel, Letizia Bugiani, Minjung Park, Sirio Belli, Joel Leja, Claudia del P. Lagos, Amir H. Khoram, Rebecca L. Davies, Razieh Emami, Gabriel Maheson, Anita Zanella, Benjamin P. Collins. 2026-10-14. The Role of Environment in Shaping the Assembly Timelines of Massive Quiescent Galaxies at Cosmic Noon. https://arxiv.org/abs/2610.19937

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

The Study of Detailed Morphology of Milky Way Dwarf Galaxies: Draco and Boötes I

We present a photometric study of the outer stellar structures of the Milky Way dwarf spheroidal galaxies (dSphs) Draco and Boötes I, using deep wide-field imaging data. The old main-sequence stars are used to trace their spatial distributions beyond their tidal radii. We derive global structural parameters and radial profiles of number density, ellipticity, and position angle from their stellar distributions. Draco and Boötes I show contrasting features. Draco shows no prominent extended stellar distribution, although weak elongations are detected toward the eastern and northwestern directions. Its stellar distribution remains relatively compact compared with its estimated Jacobi tidal radius ($r_J=57.2^{+13.5}_{-11.1}$ arcmin), suggesting that the stellar component is tightly bound by its gravitational potential. In contrast, the radial number-density profiles of Boötes I along several directions show excess from the best-fit exponential profile outside of around $r\sim20$ arcmin, near the estimated Jacobi radius ($r_J=21.6^{+9.3}_{-7.6}$ arcmin). In addition, the ellipticity of Draco decreases with radius, whereas that of Boötes I increases toward larger radii. Bo"otes I also exhibits a prominent S-shaped stellar structure extending approximately along its orbital direction. Together, the radial density excess, increasing ellipticity, and S-shaped morphology suggest that the outer stellar structure of Boötes I may trace tidal tails produced by interactions with the Milky Way. The contrasting morphologies of Draco and Boötes I further suggest that the response of dwarf galaxies to the Milky Way tidal field may depend not only on their orbital histories, but also on the internal structure of their dark-matter halos.

astro-ph.GA↗

Rotational excitation of SiC$_6$ by collisions with helium: cross sections, rate coefficients and non-LTE modeling

Rotational transitions of SiC$_6$ in the $j=26$--$40$ range have been detected in IRC+10216, yet collisional rate coefficients for SiC$_6$ with He or H$_2$ were previously unavailable. This paper reports rate coefficients for rotational excitation of SiC$_6$ induced by collisions with He, calculated using a two-dimensional potential energy surface (PES) constructed at the RCCSD(T)-F12 level under the rigid-rotor approximation. The close-coupling (CC) method was employed for low rotational energy levels, while the coupled-states (CS) approximation was used for higher rotational levels. Systematic convergence tests were conducted, and the resulting CC and CS scattering cross sections were compared. The rate coefficients obtained via the CS method cover rotational levels up to $j=40$ and temperatures of 3--100\,K. Although the CC and CS rate coefficients differ by up to a factor of $\sim 2$ for some transitions, particularly those influenced by weak coupling and resonances, the two methods yield nearly identical excitation and brightness temperatures for the high-$j$ transitions (e.g., $19\rightarrow18$) examined, and the CS-based line fluxes agree with the CC-based results to within 6.5\% for $n(\mathrm{H_2}) \ge 10^{3}$\,cm$^{-3}$; this demonstrates that the CS approximation is reliable for the non-LTE modelling of high-$j$ SiC$_6$ transitions considered here, for which fully converged CC calculations are computationally impractical. Using the calculated SiC$_6$--He rate coefficients and reduced-mass scaling to estimate the corresponding SiC$_6$--H$_2$ rates, we further investigate the excitation of the observed high-$j$ transitions. Under typical low-density conditions in IRC+10216 ($n(\mathrm{H_2}) \approx 10^4$\,cm$^{-3}$), the $j=40\to39$ transition is subthermally excited, highlighting the importance of non-LTE effects when interpreting the emission of high-$j$ SiC$_6$ transitions.

astro-ph.GA↗

Hot Molecular Hydrogen in Galaxies at Redshift ~ 0.2-1.5 Revealed by JWST

Molecular hydrogen (H$_2$) is the fundamental component of the molecular gas reservoir that fuels star formation and black hole growth. While prominent hot H$_2$ emission ($\gtrsim 1000$ K) has been explored in nearby galaxies, its excitation mechanisms at higher redshifts remain poorly constrained. We present a systematic study of hot molecular gas traced via ro-vibrational H$_2$ emitters at z~0.2-1.5 using JWST slitless spectroscopy. Exploiting JWST's great sensitivity to near-infrared H$_2$ ro-vibrational transitions such as H$_2$ 1-0 S(1), we build a sample of 144 H$_2$-luminous galaxies and characterize their multi-wavelength properties. About 96.5% and 80% of these galaxies are detected in the radio and far-infrared (FIR) bands, respectively, and their hot H$_2$ emission strongly correlates with the radio and FIR radiation. Based on radio excess, X-ray emission, and optical diagnostics, 62 sources (43%) exhibit significant AGN activity. The H$_2$ line luminosities of the sample show a sublinear dependence on radio luminosity, while the relation between the H$_2$ luminosities and total infrared luminosities is approximately linear after excluding the radio-excess sources. These scaling relations suggest that star formation provides a baseline contribution to hot H$_2$ excitation, while radio-excess sources require an additional contribution from AGN-related processes such as jet- or wind-driven shocks. These results reveal a multi-channel excitation scenario and shed new light on the interplay between star formation, AGN activity, and the interstellar medium during galaxy evolution.

astro-ph.GA↗