Optical and Ultraviolet Emission from the Gas Photoionized by Gaia BH3: Archival Constraints and Predictions for the 2029 Periastron
Abstract
Gaia BH3, a 32.7 M⊙ black hole (BH) on an 11.6-yr, e=0.73 orbit around a metal-poor giant at ≈590 pc, accretes from its wind. Neither its mass-loss rate Ṁw nor the fraction of captured gas reaching the BH is known. We ask whether optical and ultraviolet lines from gas photoionized by the hot flow are observable and what they reveal. Unlike X-ray and radio data, they count the ionizing photons the gas absorbs and trace its density and velocity. With Cloudy we compute the Hα and He II 4686 emission of the wind and inflow along the orbit for Ṁw=10−11-10−8 M⊙ yr−1, Eddington ratios fEdd=10−8-10−5 and wind speeds of 30 (slow) and 100 km s−1 (fast), and test each model against archival UVES and ESPRESSO spectra. fEdd mainly sets the lines; in dense models they come from gas falling freely onto the BH, spread over thousands of km s−1. The archival spectra exclude Ṁw>2×10−9 M⊙ yr−1 at fEdd=2×10−6 and >2.6×10−10 M⊙ yr−1 at 10−5 (95%, slow wind), Eddington ratios already excluded by the apastron Chandra limit, fEdd<7.6×10−7. Of two simulated campaigns, only 25 epochs around the 2029 periastron go beyond existing limits. For a slow wind, whose capture rate is constant, a ≥5σ Hα detection would imply an accretion state 2-3 times above the 2024 limit. For a fast wind, whose captured fraction rises 14-fold toward periastron, the campaign detects Ṁw≃10−8 M⊙ yr−1 for fEdd≳1.2×10−6, which the apastron limit allows. Below the Chandra limit, a slow wind produces no detectable line.
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BibTeX
@misc{cappelluti2026optical,
title = {{Optical and Ultraviolet Emission from the Gas Photoionized by Gaia BH3: Archival Constraints and Predictions for the 2029 Periastron}},
author = {Nico Cappelluti and Fabio Pacucci},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.27075},
eprint = {2610.27075},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.27075},
}
RIS
TY - UNPB
TI - Optical and Ultraviolet Emission from the Gas Photoionized by Gaia BH3: Archival Constraints and Predictions for the 2029 Periastron
AU - Nico Cappelluti
AU - Fabio Pacucci
PY - 2026
DA - 2026/10/19
PB - arXiv
DO - 10.48550/arxiv.2610.27075
UR - https://arxiv.org/abs/2610.27075
AB - Gaia BH3, a 32.7 M_⊙ black hole (BH) on an 11.6-yr, e=0.73 orbit around a metal-poor giant at ≈590 pc, accretes from its wind. Neither its mass-loss rate Ṁ_w nor the fraction of captured gas reaching the BH is known. We ask whether optical and ultraviolet lines from gas photoionized by the hot flow are observable and what they reveal. Unlike X-ray and radio data, they count the ionizing photons the gas absorbs and trace its density and velocity. With Cloudy we compute the Hα and He II 4686 emission of the wind and inflow along the orbit for Ṁ_w=10^−11-10^−8 M_⊙ yr^−1, Eddington ratios f_Edd=10^−8-10^−5 and wind speeds of 30 (slow) and 100 km s^−1 (fast), and test each model against archival UVES and ESPRESSO spectra. f_Edd mainly sets the lines; in dense models they come from gas falling freely onto the BH, spread over thousands of km s^−1. The archival spectra exclude Ṁ_w>2×10^−9 M_⊙ yr^−1 at f_Edd=2×10^−6 and >2.6×10^−10 M_⊙ yr^−1 at 10^−5 (95%, slow wind), Eddington ratios already excluded by the apastron Chandra limit, f_Edd<7.6×10^−7. Of two simulated campaigns, only 25 epochs around the 2029 periastron go beyond existing limits. For a slow wind, whose capture rate is constant, a ≥5σ Hα detection would imply an accretion state 2-3 times above the 2024 limit. For a fast wind, whose captured fraction rises 14-fold toward periastron, the campaign detects Ṁ_w≃10^−8 M_⊙ yr^−1 for f_Edd≳1.2×10^−6, which the apastron limit allows. Below the Chandra limit, a slow wind produces no detectable line.
ER -