collaborators

14 papers

astro-ph.GA2026

The UV Side of Little Red Dots: Red, Compact, and Iron-Enhanced Rest-UV Emission with a Strong Downturn around Ly

Makoto Ando, Yuichi Harikane, Harley Katz +2

Little Red Dots (LRDs) are candidates for growing supermassive black holes newly discovered by the James Webb Space Telescope (JWST), characterized by compact rest-optical morpholo…

astro-ph.GA2026

Hidden in Pixels I: Discovery of dual "little red dots" indicates excess clustering on kilo-parsec scales

Takumi S. Tanaka, John D. Silverman, Kazuhiro Shimasaku +56

``Little Red Dots'' (LRDs) are an abundant high-redshift population newly discovered by the James Webb Space Telescope (JWST) and considered to be an early growth phase of supermas…

astro-ph.GA2026

COSMOS-3D: Black Hole Mass Estimators and Luminosity Functions of Paschen-line AGNs

Danyang Jiang, Linhua Jiang, Shuqi Fu +13

Near-IR Paschen lines are potentially an excellent tracer of Type 1 AGNs that is hardly affected by dust extinction. JWST allows us, for the first time, to explore Paschen-line obj…

astro-ph.GA2026

The Cosmic Owl: Twin Active Collisional Ring Galaxies with Starburst Merging Front at

Mingyu Li, Bjorn H. C. Emonts, Zheng Cai +12

Galaxy mergers play a critical role in driving galaxy evolution, especially by transforming galaxy morphology, redistributing gas around galaxies, triggering active galactic nuclei…

astro-ph.GA2025

ALMA and JWST Identification of Faint Dusty Star-Forming Galaxies up to z~8

Jorge A. Zavala, Andreas L. Faisst, Manuel Aravena +44

We exploit a new sample of around 400 bright dusty galaxies from the ALMA CHAMPS Large Program, together with the rich JWST multi-band data products in the COSMOS field, to explore…

astro-ph.GA2025

Bridging Quasars and Little Red Dots: Insights into Broad-Line AGNs at from the First JWST COSMOS-3D Dataset

Xiaojing Lin, Xiaohui Fan, Feige Wang +30

We report the discovery of 13 broad-line AGNs at from the first 10% data of the JWST Cycle 3 Treasury Program COSMOS-3D. These AGNs are identified by their broad H