activity
20242026
most citedEvidence of a Disk-wind Origin for Fluorescent H in Classical T Tauri Stars

3 citations · 3 across the 3 of their papers we have counts for

collaborators

6 papers

astro-ph.GA2026

Rapid emergence of overmassive black holes in the early Universe

Sunmyon Chon, Shingo Hirano, Tomoaki Ishiyama +2

The origin of supermassive black holes (SMBHs) remains a long-standing problem in astrophysics. Recent JWST observations reveal an unexpectedly abundant population of overmassive b…

astro-ph.GA2025

Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots

Seok-Jun Chang, Max Gronke, Jorryt Matthee +1

Little Red Dots (LRDs) are compact sources at discovered through JWST spectroscopy. Their spectra exhibit broad Balmer emission lines (), alongside…

astro-ph.GA2025

Ruling out dominant electron scattering in Little Red Dots' Rosetta Stone using multiple hydrogen lines

Matilde Brazzini, Francesco D'Eugenio, Roberto Maiolino +3

The majority of Little Red Dots (LRDs) hosting Active Galactic Nuclei (AGN) exhibits broad H emission, which recent studies propose originates from scattering off free electrons…

astro-ph.SR20253 cited

Evidence of a Disk-wind Origin for Fluorescent H in Classical T Tauri Stars

Matt Kalscheur, Kevin France, Brunella Nisini +8

We use FUV spectra of 36 T Tauri stars, predominately from 's ULLYSES program, to examine the kinematic properties of fluorescent H emission li…

astro-ph.GA2024

Modeling Mg II resonance doublet spectra from galaxy haloes at z 1

Seok-Jun Chang, Rajeshwari Dutta, Max Gronke +3

We investigate the properties of cold gas at around star-forming galaxies at using Mg II spectra through radiative transfer modeling. We utilize a comprehen…

astro-ph.SR2024

A Model of the C IV 1548, 1550 Doublet Line in T Tauri Stars

Thanawuth Thanathibodee, Connor Robinson, Nuria Calvet +7

The C IV doublet in the UV has long been associated with accretion in T Tauri stars. However, it is still unclear where and how the lines are formed. Here, we present a new C IV li…