NGC 4936: abundant multi-phase medium in the central weak X-ray cool core and optically dark H I clouds in the group

@misc{tamhane20264936,
  title = {{NGC 4936: abundant multi-phase medium in the central weak X-ray cool core and optically dark H I clouds in the group}},
  author = {Prathamesh Tamhane and Ming Sun and Hao Chen and Thomas Connor and Megan Donahue and Mark Voit and Mpati Ramatsoku and Kokoro Hosogi and Tim Edge},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.10721},
  eprint = {2610.10721},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.10721},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - NGC 4936: abundant multi-phase medium in the central weak X-ray cool core and optically dark H I clouds in the group
AU  - Prathamesh Tamhane
AU  - Ming Sun
AU  - Hao Chen
AU  - Thomas Connor
AU  - Megan Donahue
AU  - Mark Voit
AU  - Mpati Ramatsoku
AU  - Kokoro Hosogi
AU  - Tim Edge
PY  - 2026
DA  - 2026/10/07
PB  - arXiv
DO  - 10.48550/arxiv.2610.10721
UR  - https://arxiv.org/abs/2610.10721
AB  - We present a multiwavelength analysis of NGC 4936, the central galaxy of a weak cool-core group hosting an unusually large cold/warm gas reservoir. NGC 4936 contains ∼2×10^8 M_⊙ of molecular gas in a rotating disk of radius ∼1 kpc, but no detected H I, with a 3σ upper limit of 1.13×10^7 M_⊙ within ∼2.5 kpc. The resulting H_2/H I mass ratio >17 is consistent with a predominantly molecular medium in the high-pressure environments of central galaxies. SOAR imaging and MUSE spectroscopy reveal ionised gas extending to ∼15 kpc in a complex filamentary morphology that broadly follows the molecular gas kinematics while extending well beyond the CO disk. Dust filaments similarly extend to ∼14 kpc and appear to interact with a companion galaxy located only ∼2.5 kpc away in projection. NGC 4936 has a star formation rate of $0.29$ M_⊙ yr^−1, and its AGN shows sub-mm and X-ray variability. We favour atmospheric condensation as the primary origin of the molecular gas, although externally acquired gas may contribute. Our recalculated thermodynamic profiles reach t_cool/t_ff∼25 in the innermost region, placing the system near the threshold for multiphase condensation. The ongoing interaction may perturb the atmosphere and promote condensation while shaping the morphology and kinematics of the multiphase medium, rather than directly supplying most of the central cold gas. We additionally detect 20 H I structures in the surrounding group environment, with masses of ∼10^7--10^8 M_⊙, including several with no obvious optical counterparts.
ER  -